FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Ramos-Madrigal, J Smith, BD Moreno-Mayar, JV Gopalakrishnan, S Ross-Ibarra, J Gilbert, MTP Wales, N AF Ramos-Madrigal, Jazmin Smith, Bruce D. Moreno-Mayar, J. Victor Gopalakrishnan, Shyam Ross-Ibarra, Jeffrey Gilbert, M. Thomas P. Wales, Nathan TI Genome Sequence of a 5,310-Year-Old Maize Cob Provides Insights into the Early Stages of Maize Domestication SO CURRENT BIOLOGY LA English DT Article ID ANCIENT; ADMIXTURE; HISTORY; ORIGIN; MEXICO; ARCHITECTURE; POPULATION; ANCESTRY; TEOSINTE; KERNELS AB The complex evolutionary history of maize (Zea mays L. ssp. mays) has been clarified with genomic-level data from modern landraces and wild teosinte grasses [1, 2], augmenting archaeological findings that suggest domestication occurred between 10,000 and 6,250 years ago in southern Mexico [3, 4]. Maize rapidly evolved under human selection, leading to conspicuous phenotypic transformations, as well as adaptations to varied environments [5]. Still, many questions about the domestication process remain unanswered because modern specimens do not represent the full range of past diversity due to abandonment of unproductive lineages, genetic drift, on-going natural selection, and recent breeding activity. To more fully understand the history and spread of maize, we characterized the draft genome of a 5,310-year-old archaeological cob excavated in the Tehuacan Valley of Mexico. We compare this ancient sample against a reference panel of modern landraces and teosinte grasses using D statistics, model-based clustering algorithms, and multidimensional scaling analyses, demonstrating the specimen derives from the same source population that gave rise to modern maize. We find that 5,310 years ago, maize in the Tehuacan Valley was on the whole genetically closer to modern maize than to its wild counterpart. However, many genes associated with key domestication traits existed in the ancestral state, sharply contrasting with the ubiquity of derived alleles in living landraces. These findings suggest much of the evolution during domestication may have been gradual and encourage further paleogenomic research to address provocative questions about the world's most produced cereal. C1 [Ramos-Madrigal, Jazmin; Moreno-Mayar, J. Victor; Gopalakrishnan, Shyam; Gilbert, M. Thomas P.; Wales, Nathan] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark. [Smith, Bruce D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, 10th & Constitut Ave, Washington, DC 20560 USA. [Smith, Bruce D.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. [Ross-Ibarra, Jeffrey] Univ Calif Davis, Ctr Populat Biol, Dept Plant Sci, 1 Shields Ave, Davis, CA 95616 USA. [Ross-Ibarra, Jeffrey] Univ Calif Davis, Genome Ctr, 1 Shields Ave, Davis, CA 95616 USA. [Gilbert, M. Thomas P.] Curtin Univ, Dept Environm & Agr, Trace & Environm DNA Lab, Perth, WA 6102, Australia. [Gilbert, M. Thomas P.] NTNU Univ Museum, N-7491 Trondheim, Norway. RP Ramos-Madrigal, J; Wales, N (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark. EM jramos@lcg.unam.mx; wales.nathan@gmail.com OI Wales, Nathan/0000-0003-0359-8450 FU Lundbeck Foundation [R52-A5062]; Danish Council for Independent Research [10-081390]; Danish National Research Foundation [DNRF94]; Consejo Nacional de Ciencia y Tecnologia (Mexico) FX This research was supported by the Lundbeck Foundation (R52-A5062), the Danish Council for Independent Research (10-081390), and the Danish National Research Foundation (DNRF94). We thank the Danish National High throughput Sequencing Centre for assistance in generating Illumina data. The Robert S. Peabody Museum kindly provided archaeological maize specimens for destructive DNA testing. We thank Thomas Sicheritz-Ponten and Bent Petersen (DTU) for additional computational support, as well as Rute R. da Fonseca and Filipe Garrett Vieira for their helpful discussions. We would also like to thank our colleagues at LANGEBIO for ongoing discussion. J.V.M.-M. was supported by a scholarship from Consejo Nacional de Ciencia y Tecnologia (Mexico). NR 36 TC 3 Z9 3 U1 9 U2 9 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD DEC 5 PY 2016 VL 26 IS 23 BP 3195 EP 3201 DI 10.1016/j.cub.2016.09.036 PG 7 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA EE4QS UT WOS:000389590500026 PM 27866890 ER PT J AU Spiegel, O Crofoot, MC AF Spiegel, Orr Crofoot, Margaret C. TI The feedback between where we go and what we know - information shapes movement, but movement also impacts information acquisition SO CURRENT OPINION IN BEHAVIORAL SCIENCES LA English DT Review ID ANIMAL MOVEMENT; SPATIAL MEMORY; CAPUCHIN MONKEYS; FOOD DETECTION; TRAVEL SPEED; SPACE-USE; ECOLOGY; EVOLUTION; BEHAVIOR; RESOURCES AB What animals know about their environment is crucial for understanding observed patterns of movement and space-use, but the feedback between information acquisition and movement is rarely considered. Animals can inherit spatial information or obtain it with their senses, via their social environment, or from direct experience. On one hand, this information affects decisions about when, where and how to move. On the other hand, movement itself shapes the information animals acquire due to effects of habitat sampling, speed-accuracy tradeoffs, and cognitive limitations. We suggest that simultaneously considering how the information animals have about their environment affects their movements and how these movements, in turn, shape the information they acquire about their habitat will provide useful insights to the field of movement ecology. C1 [Spiegel, Orr] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Crofoot, Margaret C.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Crofoot, Margaret C.] Univ Calif Davis, Anim Behav Grad Grp, Davis, CA 95616 USA. [Crofoot, Margaret C.] Smithsonian Trop Res Inst, Panama City, Panama. RP Spiegel, O (reprint author), Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. EM orr.spiegel@huji.ac.il OI Spiegel, Orr/0000-0001-8941-3175 FU NSF [DEB-1456730, BCS-1440755, IOS-1250895, III-1514174] FX We are grateful to T. Avgar and an anonymous reviewer for their valuable feedback on this manuscript; and to A. Sih and A. Kacelnik for their invitation to contribute to this special feature. OS was supported by the NSF grant (DEB-1456730) to A. Sih. MCC acknowledges support from the NSF (BCS-1440755, IOS-1250895 and III-1514174). NR 63 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2352-1546 EI 2352-1554 J9 CURR OPIN BEHAV SCI JI Curr. Opin. Behav. Sci. PD DEC PY 2016 VL 12 BP 90 EP 96 DI 10.1016/j.cobeha.2016.09.009 PG 7 WC Behavioral Sciences SC Behavioral Sciences GA EM5AK UT WOS:000395324100015 ER PT J AU Dame, K Gianninas, A Kilic, M Munn, JA Brown, WR Williams, KA von Hippel, T Harris, HC AF Dame, Kyra Gianninas, A. Kilic, Mukremin Munn, Jeffrey A. Brown, Warren R. Williams, Kurtis A. von Hippel, Ted Harris, Hugh C. TI New halo white dwarf candidates in the Sloan Digital Sky Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: atmospheres; stars: evolution; white dwarfs ID MODEL ATMOSPHERE ANALYSIS; SPECTROSCOPIC ANALYSIS; LUMINOSITY FUNCTION; COOLING SEQUENCE; SPY-PROJECT; 3D KINEMATICS; GALACTIC DISK; DEEP; ULTRACOOL; AGE AB We present optical spectroscopy and near-infrared photometry of 57 faint (g = 19-22) high proper motion white dwarfs identified through repeat imaging of approximate to 3100 deg(2) of the Sloan Digital Sky Survey footprint by Munn et al. We use ugriz and JH photometry to perform a model atmosphere analysis, and identify 10 ultracool white dwarfs with T-eff < 4000 K, including the coolest pure H atmosphere white dwarf currently known, J1657+ 2638, with T-eff = 3550 +/- 100 K. The majority of the objects with cooling ages larger than 9 Gyr display thick disc kinematics and constrain the age of the thick disc to >= 11 Gyr. There are four white dwarfs in our sample with large tangential velocities (nu(tan) > 120 km s(-1)) and UVW velocities that are more consistent with the halo than the Galactic disc. For typical 0.6 M-circle dot white dwarfs, the cooling ages for these halo candidates range from 2.3 to 8.5 Gyr. However, the total main sequence+white dwarf cooling ages of these stars would be consistent with the Galactic halo if they are slightly undermassive. Given the magnitude limits of the current large-scale surveys, many of the coolest and oldest white dwarfs remain undiscovered in the solar neighbourhood, but upcoming surveys such as Gaia and the Large Synoptic Survey Telescope should find many of these elusive thick disc and halo white dwarfs. C1 [Dame, Kyra; Gianninas, A.; Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Munn, Jeffrey A.; Harris, Hugh C.] US Naval Observ, Flagstaff Stn, 10391 W Naval Observ Rd, Flagstaff, AZ 86005 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Williams, Kurtis A.] Texas A&M Univ Commerce, Dept Phys & Astron, POB 3011, Commerce, TX 75429 USA. [von Hippel, Ted] Embry Riddle Aeronaut Univ, Phys Sci, 600 South Clyde Morris Blvd, Daytona Beach, FL 32114 USA. RP Dame, K; Gianninas, A; Kilic, M (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM kyra.c.dame-1@ou.edu; alex.gianninas@gmail.com; mukreminkilic@gmail.com FU NSF [AST-1312678]; NASA [NNX14AF65G] FX This study is based on observations obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. We gratefully acknowledge the support of the NSF and NASA under grants AST-1312678 and NNX14AF65G, respectively. NR 43 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 3 BP 2453 EP 2464 DI 10.1093/mnras/stw2146 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SC UT WOS:000393566000015 ER PT J AU Lund, MN Basu, S Aguirre, VS Chaplin, WJ Serenelli, AM Garcia, RA Latham, DW Casagrande, L Bieryla, A Davies, GR Viani, LS Buchhave, LA Miglio, A Soderblom, DR Valenti, JA Stefanik, RP Handberg, R AF Lund, Mikkel N. Basu, Sarbani Aguirre, Victor Silva Chaplin, William J. Serenelli, Aldo M. Garcia, Rafael A. Latham, David W. Casagrande, Luca Bieryla, Allyson Davies, Guy R. Viani, Lucas S. Buchhave, Lars A. Miglio, Andrea Soderblom, David R. Valenti, Jeff A. Stefanik, Robert P. Handberg, Rasmus TI Asteroseismology of the Hyades with K2: first detection of main-sequence solar-like oscillations in an open cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE asteroseismology; methods: data analysis; stars: individual: EPIC 210444167 (HIP 20357, vB 37); stars: individual: EPIC 210499243 (HIP 19877, vB 20); stars: rotation; galaxies: star clusters: individual: Hyades ID ACTIVITY-ROTATION RELATIONSHIP; HERTZSPRUNG-RUSSELL DIAGRAMS; STELLAR EVOLUTION DATABASE; GENEVA-COPENHAGEN SURVEY; SUN-LIKE STAR; M-CIRCLE-DOT; MAGNETIC ACTIVITY; RED GIANTS; NGC 6791; F-STARS AB The Hyades open cluster was targeted during Campaign 4 (C4) of the NASA K2 mission, and short-cadence data were collected on a number of cool main-sequence stars. Here, we report results on two F-type stars that show detectable oscillations of a quality that allows asteroseismic analyses to be performed. These are the first ever detections of solar-like oscillations in main-sequence stars in an open cluster. C1 [Lund, Mikkel N.; Chaplin, William J.; Davies, Guy R.; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Lund, Mikkel N.; Aguirre, Victor Silva; Chaplin, William J.; Davies, Guy R.; Miglio, Andrea; Handberg, Rasmus] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Basu, Sarbani; Viani, Lucas S.] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. [Serenelli, Aldo M.] Inst Space Sci CSIC IEEC, Campus UAB,Carrer Can Magrans S-N, E-08193 Cerdanyola Del Valles, Barcelona, Spain. [Garcia, Rafael A.] Univ Paris Diderot, CNRS, CEA DRF, Lab AIM,IRFU SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Latham, David W.; Bieryla, Allyson; Stefanik, Robert P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Casagrande, Luca] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Soderblom, David R.; Valenti, Jeff A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Lund, MN (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM mikkelnl@phys.au.dk OI Garcia, Rafael/0000-0002-8854-3776; Handberg, Rasmus/0000-0001-8725-4502; Lund, Mikkel Norup/0000-0001-9214-5642 FU Danish Council for Independent Research \ Natural Science [DFF-4181-00415]; European Community [312844]; Danish National Research Foundation [DNRF106]; ASTERISK project - European Research Council [267864]; UK Science and Technology Facilities Council (STFC); NASA [NNX13AE70G]; NSF [AST-1514676]; MINECO [ESP2014-56003-R, ESP2015-66134-R]; VILLUM FONDEN [10118]; ANR [ANR-12-BS05-0008]; CNES FX We acknowledge the dedicated team behind the Kepler and K2 missions, without whom this work would not have been possible. We thank Daniel Huber and Benoit Mosser for useful comments on an earlier version of the paper. MNL acknowledges the support of The Danish Council for Independent Research vertical bar Natural Science (Grant DFF-4181-00415). MNL was partly supported by the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312844 (SPACEINN), which is gratefully acknowledged. Funding for the Stellar Astrophysics Centre (SAC) is provided by The Danish National Research Foundation (Grant DNRF106). The research was supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no.: 267864). WJC, GRD, and AM acknowledge the support of the UK Science and Technology Facilities Council (STFC). SB acknowledges partial support from NASA grant NNX13AE70G and NSF grant AST-1514676. AMS is partially supported by grants ESP2014-56003-R and ESP2015-66134-R (MINECO). VSA acknowledges support from VILLUM FONDEN (research grant 10118). RAG acknowledges the support from the ANR program IDEE (n. ANR-12-BS05-0008) and the CNES. DWL acknowledges partial support from the Kepler mission under Cooperative Agreement NNX13AB58B with the Smithsonian Astrophysical Observatory. This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory; the WEBDA data base, operated at the Department of Theoretical Physics and Astrophysics of the Masaryk University; and the SIMBAD data base, operated at CDS, Strasbourg, France. NR 128 TC 3 Z9 3 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 3 BP 2600 EP 2611 DI 10.1093/mnras/stw2160 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SC UT WOS:000393566000025 ER PT J AU Mahony, EK Morganti, R Prandoni, I van Bemmel, IM Shimwell, TW Brienza, M Best, PN Bruggen, M Rivera, GC de Gasperin, F Hardcastle, MJ Harwood, JJ Heald, G Jarvis, MJ Mandal, S Miley, GK Retana-Montenegro, E Rottgering, HJA Sabater, J Tasse, C van Velzen, S van Weeren, RJ Williams, WL White, GJ AF Mahony, E. K. Morganti, R. Prandoni, I. van Bemmel, I. M. Shimwell, T. W. Brienza, M. Best, P. N. Brueggen, M. Rivera, G. Calistro de Gasperin, F. Hardcastle, M. J. Harwood, J. J. Heald, G. Jarvis, M. J. Mandal, S. Miley, G. K. Retana-Montenegro, E. Rottgering, H. J. A. Sabater, J. Tasse, C. van Velzen, S. van Weeren, R. J. Williams, W. L. White, G. J. TI The Lockman Hole project: LOFAR observations and spectral index properties of low-frequency radio sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies: active; radio continuum: galaxies ID COMPACT STEEP-SPECTRUM; SKY SURVEY; SOURCE CATALOG; DATA REDUCTION; SOURCE COUNTS; BOOTES FIELD; EXTRAGALACTIC SURVEY; MINI-SURVEY; GALAXIES; I. AB The Lockman Hole is a well-studied extragalactic field with extensive multi-band ancillary data covering a wide range in frequency, essential for characterizing the physical and evolutionary properties of the various source populations detected in deep radio fields (mainly star-forming galaxies and AGNs). In this paper, we present new 150-MHz observations carried out with the LOw-Frequency ARray (LOFAR), allowing us to explore a new spectral window for the faint radio source population. This 150-MHz image covers an area of 34.7 square degrees with a resolution of 18.6x14.7 arcsec and reaches an rms of 160 mu Jy beam(-1) at the centre of the field. As expected for a low-frequency selected sample, the vast majority of sources exhibit steep spectra, with a median spectral index of alpha(1400)(150) = -0.78 +/- 0.015. The median spectral index becomes slightly flatter (increasing from alpha(1400)(150) = -0.84 to alpha(1400)(150) = -0.75) with decreasing flux density down to S-150 similar to 10 mJy before flattening out and remaining constant below this flux level. For a bright subset of the 150-MHz selected sample, we can trace the spectral properties down to lower frequencies using 60-MHz LOFAR observations, finding tentative evidence for sources to become flatter in spectrum between 60 and 150 MHz. Using the deep, multi-frequency data available in the Lockman Hole, we identify a sample of 100 ultra-steep-spectrum sources and 13 peaked-spectrum sources. We estimate that up to 21 per cent of these could have z > 4 and are candidate high-z radio galaxies, but further follow-up observations are required to confirm the physical nature of these objects. C1 [Mahony, E. K.; Morganti, R.; Brienza, M.; Harwood, J. J.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Mahony, E. K.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Mahony, E. K.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Morganti, R.; Brienza, M.; Heald, G.] Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands. [Prandoni, I.] INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. [van Bemmel, I. M.] Joint Inst VLBI Europe, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Shimwell, T. W.; Rivera, G. Calistro; de Gasperin, F.; Mandal, S.; Miley, G. K.; Retana-Montenegro, E.; Rottgering, H. J. A.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Best, P. N.; Sabater, J.] Royal Observ, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Hardcastle, M. J.; Williams, W. L.] Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England. [Heald, G.] CSIRO Astron & Space Sci, 26 Dick Perry Ave, Kensington, WA 6151, Australia. [Jarvis, M. J.] Univ Oxford, Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Jarvis, M. J.] Univ Western Cape, Dept Phys & Astron, ZA-7535 Bellville, South Africa. [Tasse, C.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France. [Tasse, C.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [van Velzen, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [White, G. J.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0NL, Oxon, England. [White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. RP Mahony, EK (reprint author), Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands.; Mahony, EK (reprint author), Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia.; Mahony, EK (reprint author), ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. EM elizabeth.mahony@sydney.edu.au OI Sabater, Jose/0000-0003-1149-6294; van Weeren, Reinout/0000-0002-0587-1660; Harwood, Jeremy/0000-0003-0251-6126; Hardcastle, Martin/0000-0003-4223-1117 FU European Research Council under the European Union's Seventh Framework Programme (FP)/ERC Advanced Grant [RADIOLIFE-320745]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; UK STFC [ST/M001229/1]; UK Science and Technology Facilities Council [ST/M001008/1]; ERC Advanced Investigator programme NewClusters [321271]; Leverhulme Trust FX The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant RADIOLIFE-320745. Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. PNB is grateful for support from the UK STFC via grant ST/M001229/1, MJH and WLW acknowledge support from the UK Science and Technology Facilities Council [ST/M001008/1], TS acknowledges support from the ERC Advanced Investigator programme NewClusters 321271 and GJW gratefully acknowledges support from the Leverhulme Trust. NR 100 TC 3 Z9 3 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 3 BP 2997 EP 3020 DI 10.1093/mnras/stw2225 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SC UT WOS:000393566000056 ER PT J AU McKean, JP Godfrey, LEH Vegetti, S Wise, MW Morganti, R Hardcastle, MJ Rafferty, D Anderson, J Avruch, IM Beck, R Bell, ME van Bemmel, I Bentum, MJ Bernardi, G Best, P Blaauw, R Bonafede, A Breitling, F Broderick, JW Bruggen, M Cerrigone, L Ciardi, B de Gasperin, F Deller, A Duscha, S Engels, D Falcke, H Fallows, RA Frieswijk, W Garrett, MA Griessmeier, JM van Haarlem, MP Heald, G Hoeft, M van der Horst, AJ Iacobelli, M Intema, H Juette, E Karastergiou, A Kondratiev, VI Koopmans, LVE Kuniyoshi, M Kuper, G van Leeuwen, J Maat, P Mann, G Markoff, S McFadden, R McKay-Bukowski, D Mulcahy, DD Munk, H Nelles, A Orru, E Paas, H Pandey-Pommier, M Pietka, M Pizzo, R Polatidis, AG Reich, W Rottgering, HJA Rowlinson, A Scaife, AMM Serylak, M Shulevski, A Sluman, J Smirnov, O Steinmetz, M Stewart, A Swinbank, J Tagger, M Thoudam, S Toribio, MC Vermeulen, R Vocks, C van Weeren, RJ Wucknitz, O Yatawatta, S Zarka, P AF McKean, J. P. Godfrey, L. E. H. Vegetti, S. Wise, M. W. Morganti, R. Hardcastle, M. J. Rafferty, D. Anderson, J. Avruch, I. M. Beck, R. Bell, M. E. van Bemmel, I. Bentum, M. J. Bernardi, G. Best, P. Blaauw, R. Bonafede, A. Breitling, F. Broderick, J. W. Brueggen, M. Cerrigone, L. Ciardi, B. de Gasperin, F. Deller, A. Duscha, S. Engels, D. Falcke, H. Fallows, R. A. Frieswijk, W. Garrett, M. A. Griessmeier, J. M. van Haarlem, M. P. Heald, G. Hoeft, M. van der Horst, A. J. Iacobelli, M. Intema, H. Juette, E. Karastergiou, A. Kondratiev, V. I. Koopmans, L. V. E. Kuniyoshi, M. Kuper, G. van Leeuwen, J. Maat, P. Mann, G. Markoff, S. McFadden, R. McKay-Bukowski, D. Mulcahy, D. D. Munk, H. Nelles, A. Orru, E. Paas, H. Pandey-Pommier, M. Pietka, M. Pizzo, R. Polatidis, A. G. Reich, W. Rottgering, H. J. A. Rowlinson, A. Scaife, A. M. M. Serylak, M. Shulevski, A. Sluman, J. Smirnov, O. Steinmetz, M. Stewart, A. Swinbank, J. Tagger, M. Thoudam, S. Toribio, M. C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wucknitz, O. Yatawatta, S. Zarka, P. TI LOFAR imaging of Cygnus A - direct detection of a turnover in the hotspot radio spectra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radio continuum: galaxies ID HOT-SPOTS; RESOLUTION; GALAXIES; LOBES; ARRAY; GAS AB The low-frequency radio spectra of the hotspots within powerful radio galaxies can provide valuable information about the physical processes operating at the site of the jet termination. These processes are responsible for the dissipation of jet kinetic energy, particle acceleration, and magnetic-field generation. Here, we report new observations of the powerful radio galaxy Cygnus A using the Low Frequency Array (LOFAR) between 109 and 183 MHz, at an angular resolution of similar to 3.5 arcsec. The radio emission of the lobes is found to have a complex spectral index distribution, with a spectral steepening found towards the centre of the source. For the first time, a turnover in the radio spectrum of the two main hotspots of Cygnus A has been directly observed. By combining our LOFAR imaging with data from the Very Large Array at higher frequencies, we show that the very rapid turnover in the hotspot spectra cannot be explained by a low-energy cut-off in the electron energy distribution, as has been previously suggested. Thermal (free-free) absorption or synchrotron self-absorption models are able to describe the low-frequency spectral shape of the hotspots; however, as with previous studies, we find that the implied model parameters are unlikely, and interpreting the spectra of the hotspots remains problematic. C1 [McKean, J. P.; Godfrey, L. E. H.; Wise, M. W.; Morganti, R.; Bentum, M. J.; Blaauw, R.; Bonafede, A.; Cerrigone, L.; Deller, A.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; van Haarlem, M. P.; Heald, G.; Iacobelli, M.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Maat, P.; McFadden, R.; Munk, H.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Rowlinson, A.; Sluman, J.; Toribio, M. C.; Vermeulen, R.; Yatawatta, S.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [McKean, J. P.; Morganti, R.; Avruch, I. M.; Heald, G.; Koopmans, L. V. E.; Shulevski, A.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [Vegetti, S.; Ciardi, B.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Wise, M. W.; van Leeuwen, J.; Markoff, S.] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. [Rafferty, D.; Bonafede, A.; Brueggen, M.] Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Anderson, J.] Helmholtz Zentrum Potsdam, Deutsch GeoForschungsZentrum GFZ, Dept Geodesy & Remote Sensing 1, Telegrafenberg A17, D-14473 Potsdam, Germany. [Avruch, I. M.] SRON Netherlands Insitute Space Res, POB 800, NL-9700 AV Groningen, Netherlands. [Beck, R.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Bell, M. E.] CSIRO Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia. [van Bemmel, I.] Joint Inst VLBI Europe, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Bentum, M. J.] Univ Twente, POB 217, NL-7500 AE Enschede, Netherlands. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bernardi, G.; Smirnov, O.] SKA South Africa, 3rd Floor,Pk Rd, ZA-7405 Pinelands, South Africa. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. [Broderick, J. W.; Mulcahy, D. D.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [de Gasperin, F.; Garrett, M. A.; Intema, H.; Rottgering, H. J. A.; Toribio, M. C.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Engels, D.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Falcke, H.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Griessmeier, J. M.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Griessmeier, J. M.] Univ Orleans, OSUC, Stn Radioastron Nancay, Observ Paris,CNRS INSU,USR 704, Route Souesmes, F-18330 Nancay, France. [Hoeft, M.] Thuringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany. [van der Horst, A. J.] George Washington Univ, Dept Phys, 725 21st St NW, Washington, DC 20052 USA. [Intema, H.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA. [Juette, E.] Ruhr Univ Bochum, Astron Inst, Univ Str 150, D-44780 Bochum, Germany. [Karastergiou, A.; Pietka, M.; Stewart, A.] Univ Oxford, Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Profsoyuznaya Str 84-32, Moscow 117997, Russia. [Kuniyoshi, M.] Natl Astron Observ Japan, Tokyo 1818588, Japan. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Tahtelantie 62, FI-99600 Sodankyla, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Harwell Sci & Innovat Campus, Didcot OX11 0QX, Oxon, England. [Nelles, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Paas, H.] Univ Groningen, CIT, POB 72, NL-9700 AB Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, 9 Av Charles Andre, F-69561 St Genis Laval, France. [Scaife, A. M. M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Serylak, M.] Univ Western Cape, Dept Phys & Astron, Private Bag X17, ZA-7535 Bellville, South Africa. [Smirnov, O.] Rhodes Univ, Dept Phys & Elelctron, POB 94, ZA-6140 Grahamstown, South Africa. [Swinbank, J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Zarka, P.] Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France. RP McKean, JP (reprint author), Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. EM mckean@astron.nl OI Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660; Shulevski, Aleksandar/0000-0002-1827-0469; Hardcastle, Martin/0000-0003-4223-1117 FU South African SKA project (SKA SA); European Research Council under the European Union's Seventh Framework Programme (FP)/ERC Advanced Grant [RADIOLIFE-320745] FX We would like to thank Chris Carilli, Paul Nulsen, Lukasz Stawarz and in particular Dan Harris for useful discussions, and the anonymous referee for their valuable comments. LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. The financial assistance of the South African SKA project (SKA SA) towards this research is hereby acknowledged. Opinions expressed and conclusions arrived at are those of the authors and are not necessarily to be attributed to the SKA SA. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant RADIOLIFE-320745. NR 26 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 3 BP 3143 EP 3150 DI 10.1093/mnras/stw2105 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SC UT WOS:000393566000068 ER PT J AU Schiaffino, F Sander, SJ Bacares, MEP Barnes, KJ Kiupel, M Walsh, T Murray, S AF Schiaffino, Francesca Sander, Samantha J. Bacares, Marcia E. Pereira Barnes, Katie J. Kiupel, Matti Walsh, Timothy Murray, Suzan TI CEREBELLAR AND MESENCEPHALON NEOPLASIA IN A NILE HIPOPPOTAMUS (HIPPOPOTAMUS AMPHIBIOUS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Cerebellum; Hippopotamus amphibious; mesencephalon; neoplasia; Nile hippopotamus ID HEXAPROTODON-LIBERIENSIS; TUMORS AB A 52-yr-old female Nile hippopotamus (Hippopotamus amphibious) was presented for acute onset anorexia, depression, lethargy, instability, and weakness in the pelvic limbs. Clinical signs were rapidly progressive, despite empiric therapy with anti-inflammatory medications, resulting in the death of the animal. Gross necropsy evaluation revealed two tan, firm masses in the cerebellum and mesencephalon and a single mass in the right cranial adrenal gland. All three masses had a similar histologic morphology, and immunohistochemical investigation confirmed the general diagnosis of an adenocarcinoma, but the exact cell of origin remains unclear. In addition, there was evidence of neuroendocrine differentiation in the adrenal gland and not in the brain. These findings suggest either two distinct neoplastic populations or a metastasizing adenocarcinoma with focal endocrine differentiation. In dogs, anal sac and clitoral adenocarcinomas have been reported to undergo focal endocrine differentiation, and both can cause widespread metastasis while the primary lesion can be small. A small neoplasm of these glands may have been missed on gross examination. C1 [Schiaffino, Francesca] Univ Peruana Cayetano Heredia, Fac Vet Med, Urbanizac Ingn, Av Honorio Delgado 430, Lima 15102, Peru. [Sander, Samantha J.; Bacares, Marcia E. Pereira; Walsh, Timothy] MRC 5501 Vet Hosp, Wildlife Hlth Sci, Smithsonians Natl Zool Pk,POB 37012, Washington, DC 20013 USA. [Murray, Suzan] MRC 5501 Vet Hosp, Smithsonian Conservat Biol Inst, Smithsonian Global Hlth Program, POB 37012, Washington, DC 20013 USA. [Barnes, Katie J.; Kiupel, Matti] Diagnost Ctr Populat & Anim Hlth, Dept Pathobiol & Diagnost Invest, 4125 Beaumont Rd, Lansing, MI 48910 USA. [Schiaffino, Francesca] Johns Hopkins Bloomberg Sch Publ Hlth, 615 N Wolfe St, Baltimore, MD 21205 USA. [Sander, Samantha J.] Maryland Zoo Baltimore, 1876 Mans House Dr,Druid Hill Pk, Baltimore, MD 21217 USA. [Murray, Suzan] MRC 5501 Vet Hosp, Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012, Washington, DC 20013 USA. [Bacares, Marcia E. Pereira] Covance Labs Inc, 14500 Av Pkwy,Suite 125, Chantilly, VA 20151 USA. RP Schiaffino, F (reprint author), Univ Peruana Cayetano Heredia, Fac Vet Med, Urbanizac Ingn, Av Honorio Delgado 430, Lima 15102, Peru.; Schiaffino, F (reprint author), Johns Hopkins Bloomberg Sch Publ Hlth, 615 N Wolfe St, Baltimore, MD 21205 USA. EM fschiaffino@gmail.com NR 17 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD DEC PY 2016 VL 47 IS 4 BP 1093 EP 1096 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA EK3BE UT WOS:000393800200022 PM 28080901 ER PT J AU Holoien, TWS Kochanek, CS Prieto, JL Grupe, D Chen, P Godoy-Rivera, D Stanek, KZ Shappee, BJ Dong, S Brown, JS Basu, U Beacom, JF Bersier, D Brimacombe, J Carlson, EK Falco, E Johnston, E Madore, BF Pojmanski, G Seibert, M AF Holoien, T. W. -S. Kochanek, C. S. Prieto, J. L. Grupe, D. Chen, Ping Godoy-Rivera, D. Stanek, K. Z. Shappee, B. J. Dong, Subo Brown, J. S. Basu, U. Beacom, J. F. Bersier, D. Brimacombe, J. Carlson, E. K. Falco, E. Johnston, E. Madore, B. F. Pojmanski, G. Seibert, M. TI ASASSN-15oi: a rapidly evolving, luminous tidal disruption event at 216 Mpc SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; galaxies: nuclei ID MASSIVE BLACK-HOLE; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; ACTIVE GALACTIC NUCLEI; MAIN-SEQUENCE STAR; X-RAY OUTBURST; QUIESCENT GALAXY; LATE TIMES; SUPERNOVA; BRIGHT; DISCOVERY AB We present ground-based and Swift photometric and spectroscopic observations of the tidal disruption event (TDE) ASASSN-15oi, discovered at the centre of 2MASX J20390918-3045201 (d similar or equal to 216 Mpc) by the All-Sky Automated Survey for SuperNovae. The source peaked at a bolometric luminosity of L similar or equal to 1.3 x 10(44) erg s(-1) and radiated a total energy of E similar or equal to 6.6 x 10(50) erg over the first similar to 3.5 months of observations. The early optical/UV emission of the source can be fit by a blackbody with temperature increasing from T similar to 2 x 10(4) K to T similar to 4 x 10(4) K while the luminosity declines from L similar or equal to 1.3 x 10(44) erg s(-1) to L similar or equal to 2.3 x 10(43) erg s(-1), requiring the photosphere to be shrinking rapidly. The optical/UV luminosity decline during this period is most consistent with an exponential decline, L proportional to e(-(t-t0)/tau), with tau similar or equal to 46.5 d for t(0) similar or equal to 57241.6 (MJD), while a power-law decline of L proportional to (t - t(0))(-alpha) with t(0) similar or equal to 57 212.3 and alpha = 1.62 provides a moderately worse fit. ASASSN-15oi also exhibits roughly constant soft X-ray emission that is significantly weaker than the optical/UV emission. Spectra of the source show broad helium emission lines and strong blue continuum emission in early epochs, although these features fade rapidly and are not present similar to 3 months after discovery. The early spectroscopic features and colour evolution of ASASSN-15oi are consistent with a TDE, but the rapid spectral evolution is unique among optically selected TDEs. C1 [Holoien, T. W. -S.; Kochanek, C. S.; Godoy-Rivera, D.; Stanek, K. Z.; Brown, J. S.; Basu, U.; Beacom, J. F.] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA. [Holoien, T. W. -S.; Kochanek, C. S.; Stanek, K. Z.; Beacom, J. F.] Ohio State Univ, CCAPP, 191 W Woodruff Ave, Columbus, OH 43210 USA. [Prieto, J. L.] Univ Diego Portales, Fac Ingn, Nucleo Astron, Ave Ejercito 441, Santiago, Chile. [Prieto, J. L.] Millennium Inst Astrophys, Santiago, Chile. [Grupe, D.] Morehead State Univ, Dept Earth & Space Sci, 235 Martindale Dr, Morehead, KY 40351 USA. [Chen, Ping] Peking Univ, Dept Astron, Yi He Yuan Rd 5, Beijing 100871, Peoples R China. [Shappee, B. J.; Carlson, E. K.; Madore, B. F.; Seibert, M.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Yi He Yuan Rd 5, Beijing 100871, Peoples R China. [Basu, U.] Grove City High Sch, 4665 Hoover Rd, Grove City, OH 43123 USA. [Beacom, J. F.] Ohio State Univ, Dept Phys, 191 Woodruff Ave, Columbus, OH 43210 USA. [Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. [Brimacombe, J.] Coral Towers Observ, Cairns, Qld 4870, Australia. [Falco, E.; Johnston, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pojmanski, G.] Warsaw Univ Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Holoien, TWS; Kochanek, CS; Stanek, KZ (reprint author), Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA.; Holoien, TWS; Kochanek, CS; Stanek, KZ (reprint author), Ohio State Univ, CCAPP, 191 W Woodruff Ave, Columbus, OH 43210 USA. EM tholoien@astronomy.ohio-state.edu; ckochanek@astronomy.ohio-state.edu; kstanek@astronomy.ohio-state.edu OI Beacom, John/0000-0002-0005-2631 FU NSF [AST-1515927, AST-0908816, PHY-1404311]; Center for Cosmology and AstroParticle Physics at the Ohio State University; Mt Cuba Astronomical Foundation; George Skestos; DOE Computational Science Graduate Fellowship [DE-FG02-97ER25308]; FONDECYT [1151445]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Strategic Priority Research Program - Emergence of Cosmological Structures' of the Chinese Academy of Sciences [XDB09000000]; NSFC [11573003]; NASA through Hubble Fellowship by Space Telescope Science Institute [HST-HF-51348.001]; NASA [NAS 5-26555]; Marie Curie Actions of the European Commission (FP7-COFUND); NASA Swift programme [NAS5-00136]; 'Strategic Priority Research Program - The Emergence of Cosmological Structures' of the Chinese Academy of Sciences [XDB09000000]; Special Fund for Astronomy from Ministry of Finance; Robert Martin Ayers Sciences Fund; NASA; NSF; National Aeronautics and Space Administration; PESSTO (Public ESO Spectroscopic Survey for Transient Objects Survey) ESO programme [188.D-3003, 191.D-0935] FX ASAS-SN is supported by NSF grant AST-1515927. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Mt Cuba Astronomical Foundation, and by George Skestos.; TW-SH is supported by the DOE Computational Science Graduate Fellowship, grant number DE-FG02-97ER25308. Support for JLP is in part provided by FONDECYT through the grant 1151445 and by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. PC and SD are supported by 'the Strategic Priority Research Program - The Emergence of Cosmological Structures' of the Chinese Academy of Sciences (Grant No. XDB09000000) and Project 11573003 supported by NSFC. BJS is supported by NASA through Hubble Fellowship grant HST-HF-51348.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. JFB is supported by NSF grant PHY-1404311. EJ acknowledges support from the Marie Curie Actions of the European Commission (FP7-COFUND).; This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. At Penn State the NASA Swift programme is supported through contract NAS5-00136.; This research uses data obtained through the Telescope Access Program (TAP), which has been funded by the 'Strategic Priority Research Program - The Emergence of Cosmological Structures' of the Chinese Academy of Sciences (Grant No. XDB09000000) and the Special Fund for Astronomy from the Ministry of Finance.; This research was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund.; This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF.; This publication makes use of data products from the WISE, a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.; This work is based in part on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere, Chile as part of PESSTO, (the Public ESO Spectroscopic Survey for Transient Objects Survey) ESO programme 188.D-3003, 191.D-0935. NR 94 TC 3 Z9 3 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 4 BP 3813 EP 3828 DI 10.1093/mnras/stw2272 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SW UT WOS:000393568200030 ER PT J AU Elias-Rosa, N Pastorello, A Benetti, S Cappellaro, E Taubenberger, S Terreran, G Fraser, M Brown, PJ Tartaglia, L Morales-Garoffolo, A Harmanen, J Richardson, ND Artigau, E Tomasella, L Margutti, R Smartt, SJ Dennefeld, M Turatto, M Anupama, GC Arbour, R Berton, M Bjorkman, KS Boles, T Briganti, F Chornock, R Ciabattari, F Cortini, G Dimai, A Gerhartz, CJ Itagaki, K Kotak, R Mancini, R Martinelli, F Milisavljevic, D Misra, K Ochner, P Patnaude, D Polshaw, J Sahu, DK Zaggia, S AF Elias-Rosa, N. Pastorello, A. Benetti, S. Cappellaro, E. Taubenberger, S. Terreran, G. Fraser, M. Brown, P. J. Tartaglia, L. Morales-Garoffolo, A. Harmanen, J. Richardson, N. D. Artigau, E. Tomasella, L. Margutti, R. Smartt, S. J. Dennefeld, M. Turatto, M. Anupama, G. C. Arbour, R. Berton, M. Bjorkman, K. S. Boles, T. Briganti, F. Chornock, R. Ciabattari, F. Cortini, G. Dimai, A. Gerhartz, C. J. Itagaki, K. Kotak, R. Mancini, R. Martinelli, F. Milisavljevic, D. Misra, K. Ochner, P. Patnaude, D. Polshaw, J. Sahu, D. K. Zaggia, S. TI Dead or Alive? Long-term evolution of SN 2015bh (SNhunt275) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: evolution; supernovae: general; supernovae: individual: SN 2015bh; supernovae: individual: SN 2009ip; galaxies: individual: NGC 2770 ID SOUTHERN SPECTROPHOTOMETRIC STANDARDS; LUMINOUS BLUE VARIABLES; ETA-CARINAE ANALOG; MASSIVE STAR; SUPERNOVA IMPOSTOR; IIN SUPERNOVAE; CORE-COLLAPSE; INTERACTING SUPERNOVAE; 2012 OUTBURST; LIGHT CURVES AB Supernova (SN) 2015bh (or SNhunt275) was discovered in NGC 2770 on 2015 February with an absolute magnitude of M-r similar to -13.4 mag, and was initially classified as an SN impostor. Here, we present the photometric and spectroscopic evolution of SN 2015bh from discovery to late phases (similar to 1 yr after). In addition, we inspect archival images of the host galaxy up to similar to 21 yr before discovery, finding a burst similar to 1 yr before discovery, and further signatures of stellar instability until late 2014. Later on, the luminosity of the transient slowly increases, and a broad light-curve peak is reached after about three months. We propose that the transient discovered in early 2015 could be a core-collapse SN explosion. The pre-SN luminosity variability history, the long-lasting rise and faintness first light-curve peak suggests that the progenitor was a very massive, unstable and blue star, which exploded as a faint SN because of severe fallback of material. Later on, the object experiences a sudden brightening of 3 mag, which results from the interaction of the SN ejecta with circumstellar material formed through repeated past mass-loss events. Spectroscopic signatures of interaction are however visible at all epochs. A similar chain of events was previously proposed for the similar interacting SN 2009ip. C1 [Elias-Rosa, N.; Pastorello, A.; Benetti, S.; Cappellaro, E.; Terreran, G.; Tartaglia, L.; Tomasella, L.; Turatto, M.; Ochner, P.; Zaggia, S.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Taubenberger, S.] European Org Astron Res Southern Hemisphere ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Taubenberger, S.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Terreran, G.; Smartt, S. J.; Kotak, R.; Polshaw, J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Fraser, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Brown, P. J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA. [Morales-Garoffolo, A.] Inst Ciencies Espai CSIC IEEC, Campus UAB,Cami Can Magrans S-N, E-08193 Cerdanyola Del Valles, Barcelona, Spain. [Harmanen, J.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaisalantie 20, FI-21500 Piikkio, Finland. [Richardson, N. D.; Bjorkman, K. S.; Gerhartz, C. J.] Univ Toledo, Dept Phys & Astron, Ritter Observ, Toledo, OH 43606 USA. [Artigau, E.] Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. [Artigau, E.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Margutti, R.] Northwestern Univ, Dept Phys & Astrophys, Evanston, IL 60208 USA. [Margutti, R.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Dennefeld, M.] CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France. [Dennefeld, M.] Univ Paris 06, 98 Bis Blvd Arago, F-75014 Paris, France. [Anupama, G. C.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Arbour, R.] Pennell Obs, Winchester SO21 3HE, Hants, England. [Berton, M.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy. [Boles, T.] Coddenham Astron Observ, Peel House, Coddenham IP6 9QY, Suffolk, England. [Briganti, F.; Mancini, R.; Martinelli, F.] Gavena Observ, I-50050 Florence, Italy. [Briganti, F.; Mancini, R.; Martinelli, F.] Lajatico Astron Ctr, Via Mulini Vento, I-56030 Pisa, Italy. [Chornock, R.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, 251B Clippinger Lab, Athens, OH 45701 USA. [Ciabattari, F.] Osservatorio Astron Monte Agliale, Via Cune Motrone, I-55023 Borgo A Mozzano, Lucca, Italy. [Cortini, G.] Monte Maggiore Astron Observ, Via Montemaggiore, I-47016 Predappio, Forli, Italy. [Dimai, A.] Osservatorio Astron Col Drusci, I-32043 Cortina Dampezzo, Italy. [Itagaki, K.] Itagaki Astron Observ, Teppo Cho, Yamagata 9902492, Japan. [Milisavljevic, D.; Patnaude, D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Misra, K.] Aryabhatta Res Inst Observat Sci, Manora Peak, Naini Tal 263002, India. RP Elias-Rosa, N (reprint author), INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM nancy.elias@oapd.inaf.it OI Elias-Rosa, Nancy/0000-0002-1381-9125 FU European Union under 'Astronomy Fellowships in Italy' (AstroFIt) [267251]; PRIN-INAF (project 'Transient Universe: unveiling new types of stellar explosions with PESSTO'); MIUR PRIN; European Research Council under European Union/ERC [291222]; Spanish Ministerio de Economia y Competitividad (MINECO) [ESP2013-41268]; European Union FP7 programme through ERC grant [320360]; German Research Foundation [TRR 33]; University of Toledo; Helen Luedtke Brooks Endowed Professorship; NASA's Astrophysics Data Analysis Program [NNX13AF35G]; UK Science and Technology Facilities Council; Copernico Telescope [1.82-m]; INAF-Asiago Observatory [Schmidt 67/92 cm]; Galileo Telescope of Dipartimento di Fisica e Astronomia (Universita di Padova) at the Asiago Observatory [1.22 m]; Telescopi Joan Oro of the Montsec Astronomical Observatory; National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877, AST-1005313]; Universite de Montreal; Universite Laval; Natural Sciences and Engineering Research Council of Canada (NSERC); Fond quebecois de la recherche sur la Nature et les technologies (FQRNT); Canada Economic Development programme; NASA [NAS 5-26555]; NASA FX The research leading to these results has partially been funded by the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 267251 'Astronomy Fellowships in Italy' (AstroFIt). NER, AP, SB and LT are partially supported by the PRIN-INAF 2014 (project 'Transient Universe: unveiling new types of stellar explosions with PESSTO'). N.E.R. acknowledges financial support by MIUR PRIN 2010-2011, 'The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid'. GT and SJS acknowledges European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no. [291222]. AMG acknowledges financial support by the Spanish Ministerio de Economia y Competitividad (MINECO) grant ESP2013-41268. MF is supported by the European Union FP7 programme through ERC grant number 320360. ST is supported by TRR 33 'The Dark Universe' of the German Research Foundation. NDR acknowledges postdoctoral support by the University of Toledo and by the Helen Luedtke Brooks Endowed Professorship. The work made use of Swift/UVOT data reduced by P. J. Brown and released in the SOUSA. SOUSA is supported by NASA's Astrophysics Data Analysis Program through grant NNX13AF35G.; This research is based on observations made with: the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias; the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma; the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacin Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias; The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council; the 1.82-m Copernico Telescope and the Schmidt 67/92 cm of INAF-Asiago Observatory; the 1.22 m Galileo Telescope of Dipartimento di Fisica e Astronomia (Universita di Padova) at the Asiago Observatory; the Telescopi Joan Oro of the Montsec Astronomical Observatory, which is owned by the Generalitat de Catalunya and operated by the Institute for Space Studies of Catalunya (IEEC); the 2 m HCT, operated by the Indian Institute of Astrophysics. Observations reported here were also obtained at Haute-Provence Observatory, CNRS, France This paper includes data gathered with the 6.5 metre Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations obtained at the MDM Observatory, operated by Dartmouth College, Columbia University, Ohio State University, Ohio University, and the University of Michigan. Observations reported here were also obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant no. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE) and the Los Alamos National Laboratory. This work was based in part on observations obtained with CPAPIR at the Observatoire du Mont Megantic, funded by the Universite de Montreal, Universite Laval, the Natural Sciences and Engineering Research Council of Canada (NSERC), the Fond quebecois de la recherche sur la Nature et les technologies (FQRNT) and the Canada Economic Development programme. These results also made use of the Discovery Channel Telescope at Lowell Observatory.; Lowell is a private, non-profit institution dedicated to astrophysical research and public appreciation of astronomy and operates the DCT in partnership with Boston University, the University of Maryland, the University of Toledo, Northern Arizona University and Yale University. The Large Monolithic Imager construction was supported by a grant AST-1005313 from the National Science Foundation.; This paper is also based on observations made with the Swift telescope: we thank their staffs for excellent assistance; on data obtained from the Isaac Newton Group Archive which is maintained as part of the CASU Astronomical Data Centre at the Institute of Astronomy, Cambridge; and on observations made with the NASA/ESA HST, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This work has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 96 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 4 BP 3894 EP 3920 DI 10.1093/mnras/stw2253 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SW UT WOS:000393568200035 ER PT J AU Bertemes, C Trakhtenbrot, B Schawinski, K Done, C Elvis, M AF Bertemes, Caroline Trakhtenbrot, Benny Schawinski, Kevin Done, Chris Elvis, Martin TI Testing the completeness of the SDSS colour selection for ultramassive, slowly spinning black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTION; 7TH DATA RELEASE; X-RAY; ACCRETION DISCS; RADIATIVE EFFICIENCY; EDDINGTON RATIOS; EMISSION REGIONS; HOST GALAXIES AB We investigate the sensitivity of the colour-based quasar selection algorithm of the Sloan Digital Sky Survey (SDSS) to several key physical parameters of supermassive black holes (SMBHs), focusing on BH spin (a(*)) at the high BH-mass regime (M-BH >= 10(9) M-circle dot). We use a large grid of model spectral energy distribution (SED), assuming geometrically thin, optically thick accretion discs, and spanning a wide range of five physical parameters: BH mass M-BH, BH spin a(*), Eddington ratio L/L-Edd, redshift z, and inclination angle inc. Based on the expected fluxes in the SDSS imaging ugriz bands, we find that similar to 99.8 per cent of our models with M-BH <= 10(9.5) M-circle dot are selected as quasar candidates and thus would have been targeted for spectroscopic follow-up. However, in the extremely high-mass regime, >= 10(10) M-circle dot, we identify a bias against slowly/retrograde spinning SMBHs. The fraction of SEDs that would have been selected as quasar candidates drops below similar to 50 per cent for a(*) < 0 across 0.5 < z < 2. For particularly massive BHs, with M-BH similar or equal to 3 x 10(10) M-circle dot, this rate drops below similar to 20 per cent, and can be yet lower for specific redshifts. We further find that the chances of identifying any hypothetical sources with M-BH = 10(11) M-circle dot by colour selection would be extremely low at the level of similar to 3 per cent. Our findings, along with several recent theoretical arguments and empirical findings, demonstrate that the current understanding of the SMBH population at the high M-BH, and particularly the low-or retrograde-spinning regime, is highly incomplete. C1 [Bertemes, Caroline; Trakhtenbrot, Benny; Schawinski, Kevin] Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Done, Chris] Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Bertemes, C; Trakhtenbrot, B (reprint author), Swiss Fed Inst Technol, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM cberteme@phys.ethz.ch; benny.trakhtenbrot@phys.ethz.ch OI Trakhtenbrot, Benny/0000-0002-3683-7297 FU Swiss National Science Foundation [PP00P2_138979/1] FX We thank the anonymous referee, whose comments helped us to clarify some outstanding issues and improve the presentation of our results. KS gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. We thank Andrea Scanzio for providing us with his code recreating SDSS's colour selection algorithm, and for fruitful discussions. NR 61 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 4 BP 4041 EP 4051 DI 10.1093/mnras/stw2207 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SW UT WOS:000393568200042 ER PT J AU Loomis, RA Shingledecker, CN Langston, G McGuire, BA Dollhopf, NM Burkhardt, AM Corby, J Booth, ST Carroll, PB Turner, B Remijan, AJ AF Loomis, Ryan A. Shingledecker, Christopher N. Langston, Glen McGuire, Brett A. Dollhopf, Niklaus M. Burkhardt, Andrew M. Corby, Joanna Booth, Shawn T. Carroll, P. Brandon Turner, Barry Remijan, Anthony J. TI Non-detection of HC11N towards TMC-1: constraining the chemistry of large carbon-chain molecules SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: individual objects: TMC-1; ISM: molecules ID DIFFUSE INTERSTELLAR BANDS; SPECTRAL-LINE SURVEY; LABORATORY DETECTION; DARK CLOUDS; ASTRONOMICAL DETECTION; C-13 ISOTOPOMERS; COLOGNE DATABASE; TAURUS; ANIONS; HC7N AB Bell et al. reported the first detection of the cyanopolyyne HC11N towards the cold dark cloud TMC-1; no subsequent detections have been reported towards any source. Additional observations of cyanopolyynes and other carbon-chain molecules towards TMC-1 have shown a log-linear trend between molecule size and column density, and in an effort to further explore the underlying chemical processes driving this trend, we have analysed Green Bank Telescope observations of HC9N and HC11N towards TMC-1. Although we find an HC9N column density consistent with previous values, HC11N is not detected and we derive an upper limit column density significantly below that reported in Bell et al. Using a state-of-the-art chemical model, we have investigated possible explanations of non-linearity in the column density trend. Despite updating the chemical model to better account for ion-dipole interactions, we are not able to explain the non-detection of HC11N, and we interpret this as evidence of previously unknown carbon-chain chemistry. We propose that cyclization reactions may be responsible for the depleted HC11N abundance, and that products of these cyclization reactions should be investigated as candidate interstellar molecules. C1 [Loomis, Ryan A.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Shingledecker, Christopher N.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Langston, Glen] Natl Sci Fdn, Div Astron Sci, Arlington, VA 22230 USA. [McGuire, Brett A.; Dollhopf, Niklaus M.; Booth, Shawn T.; Turner, Barry; Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22904 USA. [McGuire, Brett A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dollhopf, Niklaus M.; Burkhardt, Andrew M.; Corby, Joanna; Booth, Shawn T.] Univ Viriginia, Dept Astron, Charlottesville, VA 22904 USA. [Carroll, P. Brandon] CALTECH, Div Chem & Chem Engn, Pasadena, CA 91125 USA. RP Loomis, RA (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM rloomis@cfa.harvard.edu FU National Science Foundation FX We would like to thank M. McCarthy, A. Vanderburg, and B. Montet for productive discussion and helpful comments on the manuscript. We also thank two anonymous referees for providing comments that greatly improved the quality of the manuscript. RAL gratefully acknowledges support from a National Science Foundation Graduate Research Fellowship. CNS wishes to thank the National Science Foundation for supporting the Astrochemistry programme at the University of Virginia. BAM and PBC are grateful to G. A. Blake for his support. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 75 TC 1 Z9 1 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 4 BP 4175 EP 4183 DI 10.1093/mnras/stw2302 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SW UT WOS:000393568200051 ER PT J AU Zhou, G Kedziora-Chudczer, L Bailey, J Marshall, JP Bayliss, DDR Stockdale, C Nelson, P Tan, TG Rodriguez, JE Tinney, CG Dragomir, D Colon, K Shporer, A Bento, J Sefako, R Horne, K Cochran, W AF Zhou, G. Kedziora-Chudczer, L. Bailey, J. Marshall, J. P. Bayliss, D. D. R. Stockdale, C. Nelson, P. Tan, T. G. Rodriguez, J. E. Tinney, C. G. Dragomir, D. Colon, K. Shporer, A. Bento, J. Sefako, R. Horne, K. Cochran, W. TI Simultaneous infrared and optical observations of the transiting debris cloud around WD 1145+017 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: individual: WD 1145+017; white dwarfs ID ANGLO-AUSTRALIAN TELESCOPE; WHITE-DWARF G29-38; DUST CLOUD; DATA RELEASE; SDSS; CANDIDATE; DISCOVERY; FREQUENCY; GRAINS; STARS AB We present multiwavelength photometric monitoring of WD 1145+017, a white dwarf exhibiting periodic dimming events interpreted to be the transits of orbiting, disintegrating planetesimals. Our observations include the first set of near-infrared light curves for the object, obtained on multiple nights over the span of 1 month, and recorded multiple transit events with depths varying between similar to 20 and 50 per cent. Simultaneous near-infrared and optical observations of the deepest and longest duration transit event were obtained on two epochs with the Anglo-Australian Telescope and three optical facilities, over the wavelength range of 0.5-1.2 mu m. These observations revealed no measurable difference in transit depths for multiple photometric pass bands, allowing us to place a 2 sigma lower limit of 0.8 mu m on the grain size in the putative transiting debris cloud. This conclusion is consistent with the spectral energy distribution of the system, which can be fit with an optically thin debris disc with minimum particle sizes of 10(-3)(+5) mu m. C1 [Zhou, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kedziora-Chudczer, L.; Bailey, J.; Marshall, J. P.; Tinney, C. G.] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia. [Kedziora-Chudczer, L.; Bailey, J.; Marshall, J. P.; Tinney, C. G.] Univ New South Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Bayliss, D. D. R.] Univ Geneva, Astron Observ, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. [Stockdale, C.] Hazelwood Observ, Melbourne, Vic, Australia. [Nelson, P.] Ellinbank Observ, Melbourne, Vic, Australia. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Rodriguez, J. E.] Vanderbilt Univ, Dept Phys & Astron, Stevenson Ctr 6301, Nashville, TN 37235 USA. [Dragomir, D.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Dragomir, D.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Colon, K.] NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. [Colon, K.] Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA. [Shporer, A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Bento, J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Sefako, R.] SAAO, POB 9, ZA-7935 Observatory, South Africa. [Horne, K.] Univ St Andrews, SUPA Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Cochran, W.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. RP Zhou, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM george.zhou@cfa.harvard.edu OI Tan, Thiam-Guan/0000-0001-5603-6895 FU UNSW Vice-Chancellor's Postdoctoral Fellowship; NASA - Space Telescope Science Institute [HST-HF2-51372.001-A]; NASA [NAS5-26555] FX GZ thanks insightful discussions with Andrew Vanderburg and Bryce Croll. JPM is supported by a UNSW Vice-Chancellor's Postdoctoral Fellowship. We thank the support staff at the AAO, who made the continued IRIS2 observations possible. This work makes use of observations from the LCOGT network. DD acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51372.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. NR 48 TC 6 Z9 6 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC PY 2016 VL 463 IS 4 BP 4422 EP 4432 DI 10.1093/mnras/stw2286 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ9SW UT WOS:000393568200068 ER PT J AU Strahan, D Tsukada, M AF Strahan, Donna Tsukada, Masahiko TI Measuring mercury emissions from cinnabar lacquer objects SO STUDIES IN CONSERVATION LA English DT Article DE Cinnabar; Handling; Health risk; Lacquer; Mercury; Storage; Vermilion ID HERBARIUM AB This paper presents the results of a study on mercury emissions from Asian lacquer objects containing the red pigment cinnabar, also known as vermilion, which is mercury (II) sulfide. Initial tests for mercury vapor emission from a variety of lacquer objects were carried out using mercury- indicating powder, while more accurate measurements were made with a mercury vapor meter. The emissions were compared to American Occupational Safety and Health Administration (OSHA) guidelines. The results revealed that cinnabar lacquer objects emitted a small amount of mercury vapor, that this could accumulate in enclosed spaces, and that under certain conditions, objects and storage containers housed near cinnabar lacquers may become contaminated. Recommended methods and guidelines for storing, treating, and handling cinnabar lacquers are provided. C1 [Strahan, Donna] Freer Gallery Art, Washington, DC USA. [Strahan, Donna] Arthur M Sackler Gallery, Washington, DC USA. [Tsukada, Masahiko] Tokyo Univ Arts, Tokyo, Japan. RP Strahan, D (reprint author), Smithsonian Inst, Freer Gallery Art, Dept Conservat & Sci Res, POB 37012,MRC 707, Washington, DC 20013 USA.; Strahan, D (reprint author), Smithsonian Inst, Arthur M Sackler Gallery, POB 37012,MRC 707, Washington, DC 20013 USA. EM strahand@si.edu NR 22 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0039-3630 EI 2047-0584 J9 STUD CONSERV JI Stud. Conserv. PD DEC PY 2016 VL 61 SU 3 BP 166 EP 172 DI 10.1080/00393630.2016.1227048 PG 7 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA EK1MS UT WOS:000393690400017 ER PT J AU Bold, U Crowley, JL Smith, EF Sambuu, O Macdonald, FA AF Bold, Uyanga Crowley, James L. Smith, Emily F. Sambuu, Oyungerel Macdonald, Francis A. TI Neoproterozoic to early Paleozoic tectonic evolution of the Zavkhan terrane of Mongolia: Implications for continental growth in the Central Asian orogenic belt SO LITHOSPHERE LA English DT Article ID U-PB GEOCHRONOLOGY; BAYANKHONGOR OPHIOLITE ZONE; NORTH CHINA CRATON; WESTERN MONGOLIA; DETRITAL ZIRCONS; SW MONGOLIA; SOUTHERN MONGOLIA; SIBERIAN CRATON; LAKE ZONE; SOUTHWESTERN MONGOLIA AB The Zavkhan terrane is a Proterozoic cratonic fragment in southwestern Mongolia that forms the core of the Central Asian orogenic belt. We provide new geologic and U-Pb zircon geochronologic constraints on the Neoproterozoic and early Paleozoic tectonic evolution of the terrane. Orthogneisses dated as ca. 1967 and ca. 839 Ma form the basement and are intruded and overlain by ca. 811-787 Ma arc-volcanic and volcaniclastic rocks that lack a gneissic fabric, suggestive of a mid-Neoproterozoic metamorphic event. Rifting and formation of the Zavkhan ribbon continent occurred from ca. 770-717 Ma and was followed by passive margin sedimentation between 717 and 580 Ma. During the latest Ediacaran to Cambrian, the southern margin of the Zavkhan terrane was reactivated with the obduction of the Lake terrane, slab break-off and reversal, and ca. 509-507 Ma magmatism. Metamorphosed Proterozoic and Cambrian units are cut by undeformed ca. 496 Ma gabbro, providing a tight constraint on the age of Cambrian metamorphism. Late Ordovician to Silurian rifting is marked by bimodal magmatism and deposition in narrow fault-bound basins. Our data indicate that the Zavkhan terrane traveled alone in the Neoproterozoic, collided with the Lake terrane in the late Ediacaran to Cambrian, accreted an unknown crustal block during Cambrian Epoch 2-Epoch 3, and then rifted away in the Ordovician. We suggest the majority of continental growth in Mongolia occurred through the trapping and oroclinal bending of ribbon continents rather than long-lived accretion on the margin of a major craton. C1 [Bold, Uyanga; Macdonald, Francis A.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Crowley, James L.] Boise State Univ, Dept Geosci, 1910 Univ Dr, Boise, ID 83725 USA. [Smith, Emily F.] Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. [Sambuu, Oyungerel] Mongolian Univ Sci & Technol, Sch Geol & Min Engn, 8th Khoroo,Baga Toiruu 34, Sukhbaatar Dist 14191, Ulaanbaatar, Mongol Peo Rep. RP Bold, U (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. FU Massachusetts Institute of Technology National Aeronautics and Space Administration Astrobiology Institute node FX We thank our field assistants Gerelt Sarantuya, Javzandulam Chuluunbaatar, Munkh-Erdene Delger, Munkh Jugder, Uchral Khuchitbaatar, Otgonbayar Dandar, Ariunsanaa Dorj, Odbayar Erdenebat, Dan Bradley, Tanya Petach, and Sarah Moon. We also thank Nicholas Swanson-Hysell and Taylor Kilian for insightful comments and discussions, and the Massachusetts Institute of Technology National Aeronautics and Space Administration Astrobiology Institute node for support. NR 103 TC 1 Z9 1 U1 2 U2 2 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 1941-8264 EI 1947-4253 J9 LITHOSPHERE-US JI Lithosphere PD DEC PY 2016 VL 8 IS 6 BP 729 EP 750 DI 10.1130/L549.1 PG 22 WC Geochemistry & Geophysics; Geology SC Geochemistry & Geophysics; Geology GA EJ2RP UT WOS:000393059000010 ER PT J AU Mayne, RG Smith, SE Corrigan, CM AF Mayne, Rhiannon G. Smith, Samantha E. Corrigan, C. M. TI Hiding in the howardites: Unequilibrated eucrite clasts as a guide to the formation of Vesta's crust SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID MAGMA OCEAN CRYSTALLIZATION; ASTEROID 4 VESTA; HED PARENT BODY; THERMAL HISTORY; DIOGENITES; GEOCHEMISTRY; METEORITES; DIFFERENTIATION; PETROGENESIS; METAMORPHISM AB 204 howardites in the National Meteorite Collection at the Smithsonian were examined for the presence of fine-grained eucrite clasts, with the goal of better understanding the formation of the uppermost crust of asteroid 4Vesta. Eight clasts were identified and characterized in terms of their textures and mineral chemistry, and their degree of thermal metamorphism was assessed. The paucity of fine-grained eucrites, both within the unbrecciated eucrites and as clasts within the howardites, suggests that they originate from small-scale units on the surface of Vesta, most likely derived from partial melting. Six of the eight clasts described were found to be unequilibrated, meaning that they preserve their original crystallization trends. The vast majority of eucrites are at least partially equilibrated, making these samples quite rare and important for deciphering the petrogenesis of the vestan crust. Biomodal grain populations suggest that eucrite melts often began crystallizing pyroxene and plagioclase during their ascent to the surface, where they were subject to more rapid cooling, crystallization, and later metasomatism. Pyroxene compositions from this study and prior work indicate that the products of both primitive and evolved melts were present at the vestan surface after its formation. Two howardite thin sections contained multiple eucrite composition clasts with different crystallization and thermal histories; this mm-scale diversity reflects the complexity of the current day vestan surface that has been observed by Dawn. C1 [Mayne, Rhiannon G.; Smith, Samantha E.] Texas Christian Univ, Sch Geol Energy & Environm, Monnig Meteorite Collect & Gallery, TCU Box 298830, Ft Worth, TX 76109 USA. [Corrigan, C. M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th & Constitut NW, Washington, DC 20560 USA. RP Mayne, RG (reprint author), Texas Christian Univ, Sch Geol Energy & Environm, Monnig Meteorite Collect & Gallery, TCU Box 298830, Ft Worth, TX 76109 USA. EM r.g.mayne@tcu.edu NR 48 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2016 VL 51 IS 12 BP 2387 EP 2402 DI 10.1111/maps.12730 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA EJ3US UT WOS:000393138200008 ER PT J AU Lagasse, BJ Ryder, TB AF Lagasse, Benjamin J. Ryder, T. Brandt TI SEX AND AGE-SPECIFIC VARIATION IN PROVISIONING BY A LONG DISTANCE NEOTROPICAL MIGRANT, THE WOOD THRUSH (HYLOCICHLA MUSTELINA) SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE age-assortative mating; age-specific variation; Hylociclzla mustelina; nestling provisioning ID MULTIPLE MALE FEEDERS; PARENTAL CARE; REPRODUCTIVE SUCCESS; JUVENILE SURVIVAL; TERRITORY QUALITY; MATE CHOICE; INVESTMENT; BIRDS; PERFORMANCE; WARBLERS AB Parental investment is a unique balance between optimizing reproductive success and survival, yet how individuals vary their effort with respect to age and the contributions of their partner remains poorly studied. Here, we examine the provisioning of nestlings by Wood Thrushes (Hylocichla mustelina) at 38 nests in southern Indiana during the breeding season of 2013 to address the influence of adult age and sex on reproductive investment. We used video cameras to quantify an adjusted provisioning rate (provisioning rate = adult visits/hr/nestling x mean prey size x mean number of prey/visit) by individuals in both age-assortative (same age) and disassortative (different age) pairs (n = 33 pairs), hereafter referred to as pair type. Disassortative pairs delivered less prey than expected given nestling age, and sexes differed in their respective provisioning effort. In contrast, age-assortative pairs consistently provisioned more, and provisioning effort was comparable between the sexes regardless of parental age. These findings are contrary to studies where older breeders had a greater foraging efficiency and provided young with more prey. Our results indicate that adult age is not an accurate predictor of provisioning in Wood Thrushes and highlight the previously overlooked importance of age-assortative mating on parental investment in this system. C1 [Lagasse, Benjamin J.] Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA. [Ryder, T. Brandt] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, POB 37012 MRC 5503, Washington, DC 20013 USA. [Lagasse, Benjamin J.] Univ Colorado, Dept Integrat Biol, Denver, CO 80217 USA. RP Ryder, TB (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, POB 37012 MRC 5503, Washington, DC 20013 USA. EM rydert@si.edu NR 59 TC 0 Z9 0 U1 1 U2 1 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 EI 1938-5447 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD DEC PY 2016 VL 128 IS 4 BP 821 EP 829 PG 9 WC Ornithology SC Zoology GA EJ5MR UT WOS:000393262800014 ER PT J AU Johnson, K Baysinger, D AF Johnson, Kirk Baysinger, Dave TI In his own words SO ACTA GEOLOGICA POLONICA LA English DT Editorial Material C1 [Johnson, Kirk] Smithsonian Natl Museum Nat Hist, Washington, DC 20560 USA. [Baysinger, Dave] Denver Museum Nat & Sci, Dept Paleontol, Denver, CO USA. RP Johnson, K (reprint author), Smithsonian Natl Museum Nat Hist, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU POLSKA AKAD NAUK, POLISH ACAD SCIENCES, UNIV WARSAW, GEOLOGY DEPT PI WARSZAWA PA PL DEFILAD 1, WARSZAWA, 00-901, POLAND SN 0001-5709 EI 2300-1887 J9 ACTA GEOL POL JI Acta Geol. Pol. PD DEC PY 2016 VL 66 IS 4 BP III EP XIII DI 10.1515/agp-2016-0030 PN 1 PG 11 WC Geology SC Geology GA EI8HK UT WOS:000392746600002 ER PT J AU Mecke, S Hartmann, L Mader, F Kieckbusch, M Kaiser, H AF Mecke, Sven Hartmann, Lukas Mader, Felix Kieckbusch, Max Kaiser, Hinrich TI Redescription of Cyrtodactylus fumosus (Muller, 1895) (Reptilia: Squamata: Gekkonidae), with a revised identification key to the bent-toed geckos of Sulawesi SO ACTA HERPETOLOGICA LA English DT Article DE Cyrtodactylus fumosus; C. marmoratus; Lacertilia; bent-toed geckos; reptiles; North Sulawesi; Indonesia; morphology ID INDONESIA; GRAY; MALAYSIA; ISLAND; JAVA AB The binominal Cyrtodactylus fumosus has frequently been used for populations of bent-toed geckos occurring on some Indonesian islands, including Java, Bali, Sulawesi, and Halmahera. Unfortunately, incorrect usage of this name for different geographic lineages has resulted in confusion about the true identity of C. fumosus. Examination of the type specimen and additional specimens from Rurukan and Mount Masarang, North Sulawesi Province, Indonesia, revealed that this population is distinct from other forms heretofore called 'fumosus' by a combination of unique morphological characters. In order to stabilize the taxonomy of C. fumosus sensu stricto, and to prevent further confusion, we provide a comprehensive redescription of this species, whose distribution we herein restrict to North Sulawesi. Cyrtodactylus fumosus is one of the most distinctive species among the six bent-toed geckos recorded from Sulawesi, and it differs from Sulawesi congeners by the presence of (1) precloacofemoral scales, including three pore-bearing scales on each thigh, separated from 10 or 11 pore-bearing scales in the precloacal region by 9-11 interscales in males, (2) a precloacal groove in adult males, (3) flat dorsal tubercles in 4-7 irregularly arranged longitudinal rows at midbody, and (4) a distinct lateral fold lacking tubercles. We also provide a revised identification key to the bent-toed gecko species of Sulawesi. C1 [Mecke, Sven; Hartmann, Lukas; Kieckbusch, Max] Philipps Univ Marburg, Dept Anim Evolut & Systemat & Zool Collect Marbur, Fac Biol, Karl von Frisch Str 8, D-35032 Marburg, Germany. [Hartmann, Lukas] Goethe Univ Frankfurt, Biol, Dept Ecol & Evolut, Max von Laue Str 13, D-60438 Frankfurt, Germany. [Mader, Felix] Janusstr 5, D-93051 Regensburg, Germany. [Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA. [Kaiser, Hinrich] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Mecke, S (reprint author), Philipps Univ Marburg, Dept Anim Evolut & Systemat & Zool Collect Marbur, Fac Biol, Karl von Frisch Str 8, D-35032 Marburg, Germany. EM meckes@staff.uni-marburg.de FU AMNH collection study grant FX The authors thank Denis Vallan and Urs Wuest (NMB), Patrick Campbell (BMNH), Esther Dondorp (RMNH), Raffael Ernst and Markus Auer (MTKD), Christopher J. Raxworthy, David A. Kizirian, David A. Dickey, and Lauren Vonnahme (AMNH), Joseph Martinez and Jose Rosado (MCZ), and Gunther Kohler and Linda Acker (SMF), for allowing examination of material in their care. We also thank Ka Schuster (Philipps-Universitat Marburg, Germany) for reading and commenting on a draft of this publication, and Olivier S.G. Pauwels (RBINS) and Lee L. Grismer (LSUHC) for their helpful reviews, which greatly improved this publication. This study was supported by an AMNH collection study grant to SM. NR 42 TC 0 Z9 0 U1 1 U2 1 PU FIRENZE UNIV PRESS PI FIRENZE PA JOURNALS DIVISION, BORGO ALBIZI, 28, FIRENZE, 50122, ITALY SN 1827-9635 EI 1827-9643 J9 ACTA HERPETOL JI Acta Herpetol. PD DEC PY 2016 VL 11 IS 2 BP 151 EP 160 DI 10.13128/Acta_Herpetol-17874 PG 10 WC Zoology SC Zoology GA EI6AX UT WOS:000392578500006 ER PT J AU Jaszczak, JA Rumsey, MS Bindi, L Hackney, SA Wise, MA Stanley, CJ Spratt, J AF Jaszczak, John A. Rumsey, Michael S. Bindi, Luca Hackney, Stephen A. Wise, Michael A. Stanley, Chris J. Spratt, John TI Merelaniite, Mo4Pb4VSbS15, a New Molybdenum-Essential Member of the Cylindrite Group, from the Merelani Tanzanite Deposit, Lelatema Mountains, Manyara Region, Tanzania SO MINERALS LA English DT Article DE merelaniite; cylindrite group; molybdenum; lead; Merelani tanzanite deposit; Tanzania ID CRYSTAL-STRUCTURE; IMA COMMISSION; FRANCKEITE; MINERALS AB Merelaniite is a new mineral from the tanzanite gem mines near Merelani, Lelatema Mountains, Simanjiro District, Manyara Region, Tanzania. It occurs sporadically as metallic dark gray cylindrical whiskers that are typically tens of micrometers in diameter and up to a millimeter long, although a few whiskers up to 12 mm long have been observed. The most commonly associated minerals include zoisite (variety tanzanite), prehnite, stilbite, chabazite, tremolite, diopside, quartz, calcite, graphite, alabandite, and wurtzite. In reflected polarized light, polished sections of merelaniite are gray to white in color, show strong bireflectance and strong anisotropism with pale blue and orange-brown rotation tints. Electron microprobe analysis (n = 13), based on 15 anions per formula unit, gives the formula Mo4.33Pb4.00As0.10V0.86Sb0.43Bi0.33Mn0.05W0.05Cu0.03(S14.70Se0.30)(Sigma 15), ideally Mo4Pb4VSbS15. An arsenic-rich variety has also been documented. X-ray diffraction, electron diffraction, and high-resolution transmission electron microscopy show that merelaniite is a member of the cylindrite group, with alternating centered pseudo-tetragonal (Q) and pseudo-hexagonal (H) layers with respective PbS and MoS2 structure types. The Q and H layers are both triclinic with space group C1 or C1. The unit cell parameters for the Q layer are: a = 5.929(8) angstrom; b = 5.961(5) angstrom; c = 12.03(1) angstrom; alpha = 91.33(9); beta = 90.88(5); gamma = 91.79(4); V = 425(2) angstrom(3); and Z = 4. For the H layer, a = 5.547(9) angstrom; b = 3.156(4) angstrom; c = 11.91(1) angstrom; alpha = 89.52(9); beta = 92.13(5); gamma = 90.18(4); V = 208(2) angstrom(3); and Z = 2. Among naturally occurring minerals of the cylindrite homologous series, merelaniite represents the first Mo-essential member and the first case of triangular-prismatic coordination in the H layers. The strongest X-ray powder diffraction lines [d in angstrom (I/I-0)] are 6.14 (30); 5.94 (60); 2.968 (25); 2.965 (100); 2.272 (40); 1.829 (30). The new mineral has been approved by the IMA CNMNC (2016-042) and is named after the locality of its discovery in honor of the local miners. C1 [Jaszczak, John A.] Michigan Technol Univ, Dept Phys, 1400 Townsend Dr, Houghton, MI 49931 USA. [Jaszczak, John A.] Michigan Technol Univ, AE Seaman Mineral Museum, 1400 Townsend Dr, Houghton, MI 49931 USA. [Rumsey, Michael S.; Stanley, Chris J.] Nat Hist Museum, Dept Earth Sci, Cromwell Rd, London SW7 5BD, England. [Bindi, Luca] Univ Florence, Dipartimento Sci Terra, Via La Pira 4, I-50121 Florence, Italy. [Hackney, Stephen A.] Michigan Technol Univ, Dept Mat Sci & Engn, 1400 Townsend Dr, Houghton, MI 49931 USA. [Wise, Michael A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Spratt, John] Nat Hist Museum, Dept Core Res Labs, Cromwell Rd, London SW7 5BD, England. RP Jaszczak, JA (reprint author), Michigan Technol Univ, Dept Phys, 1400 Townsend Dr, Houghton, MI 49931 USA.; Jaszczak, JA (reprint author), Michigan Technol Univ, AE Seaman Mineral Museum, 1400 Townsend Dr, Houghton, MI 49931 USA. EM jaszczak@mtu.edu; m.rumsey@nhm.ac.uk; luca.bindi@unifi.it; hackney@mtu.edu; wisem@si.edu; c.stanley@nhm.ac.uk; j.spratt@nhm.ac.uk OI Stanley, Christopher/0000-0002-6015-5210 NR 28 TC 0 Z9 0 U1 3 U2 3 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2075-163X J9 MINERALS-BASEL JI Minerals PD DEC PY 2016 VL 6 IS 4 AR 115 DI 10.3390/min6040115 PG 19 WC Mineralogy; Mining & Mineral Processing SC Mineralogy; Mining & Mineral Processing GA EI1BI UT WOS:000392209700018 ER PT J AU Muscarella, R Uriarte, M Erickson, DL Swenson, NG Kress, WJ Zimmerman, JK AF Muscarella, Robert Uriarte, Maria Erickson, David L. Swenson, Nathan G. Kress, W. John Zimmerman, Jess K. TI Variation of tropical forest assembly processes across regional environmental gradients SO PERSPECTIVES IN PLANT ECOLOGY EVOLUTION AND SYSTEMATICS LA English DT Article DE Abiotic filtering; Competition; Wood density; LMA; Maximum height; Functional diversity ID PHYLOGENETIC COMMUNITY STRUCTURE; PLANT FUNCTIONAL TRAITS; ECONOMICS SPECTRUM; WOOD DENSITY; RAIN-FOREST; PUERTO-RICO; PRECIPITATION GRADIENT; MEDITERRANEAN RANGELAND; SPECIES DISTRIBUTIONS; SUCCESSIONAL CHANGES AB Determining how the relative strength of community assembly processes varies along resource gradients is critical for understanding community responses to environmental change. A key challenge for addressing this issue at regional scales is that environmental gradients typically encompass multiple coupled resource gradients (e.g. water, light, soils), which can complicate hypotheses about the drivers of community variation. We used data on functional traits and phylogenetic relatedness to infer assembly processes of tree communities across regional environmental gradients in Puerto Rico. We censused trees in 24, 0.25-ha mature plots located along a precipitation gradient and on soils derived from two parent materials (limestone and volcanic). In each plot, we quantified abiotic conditions in terms of mean annual precipitation, canopy openness, and soil nutrients. We used three functional traits with relevance for drought tolerance and resource acquisition strategies (wood density [WD], leaf mass per area [LMA], and maximum height [H-max], and a molecular phylogeny, to characterize tree community composition in terms of (i) community-weighted mean trait values (i.e., plot average trait values, weighted by relative basal area), (ii) functional diversity, and (iii) phylogenetic diversity. Mean annual precipitation was negatively correlated with understory light availability (for plots on both soil types), and soil fertility (among plots on limestone soils). Soil fertility varied substantially between plots on each parent material, and was generally higher among plots on limestone-derived soils. Among the limestone soil plots, which occur on the drier half of the precipitation gradient, increasing mean annual precipitation was associated with lower community-weighted mean WD and LMA, and taller H-max. Additionally, functional diversity (of WD and H-max) and phylogenetic diversity increased with precipitation among limestone soil plots, suggesting an important role for abiotic filtering in driving functional and phylogenetic convergence in arid conditions. In contrast, we did not find significant relationships between environmental conditions and community-weighted mean traits or diversity metrics among plots on volcanic-derived soils, which occur along the wetter half of the precipitation gradient. Together, our results suggest that drought tolerance is the dominant assembly mechanism controlling tree composition in dry forests. In wetter forests, functional diversity appears to be maintained by a combination of hierarchical competition for light and niche partitioning. Overall, our results exhibit geographic variation in the mechanisms governing composition of tropical forests across regional environmental gradients, and highlight the importance of considering complex environmental gradients at large spatial scales. (C) 2016 Elsevier GmbH. All rights reserved. C1 [Muscarella, Robert; Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10017 USA. [Muscarella, Robert] Aarhus Univ, Ecoinformat & Biodivers, Aarhus, Denmark. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20523 USA. [Swenson, Nathan G.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Zimmerman, Jess K.] Univ Puerto Rico, Dept Environm Sci, San Juan, PR USA. RP Muscarella, R (reprint author), Aarhus Univ, Ecoinformat & Biodivers, Aarhus, Denmark. EM bob.muscarella@gmail.com FU Smithsonian Center for Tropical Forest Science grant; NSF [DEB 1050957, EF 1137239, DEB 1311367, DBI 1401312]; Earth Institute; Institute of Latin American studies at Columbia University FX We thank the Departmento de Recursos Naturales y Ambientales (DRNA) of Puerto Rico as well as individual forest officers for permission to conduct this research under DRNA permit #2011-IC-046. We also thank Alexis Massol-Gonzalez and Casa Pueblo for land access and accommodation. Marcos Rodriguez provided tireless assistance with all aspects of fieldwork and keen insight to the natural history of Puerto Rican trees. Benedict Bachelot collected canopy openness data. Fabiola Areces, Frank Axelrod, Papo Vives, and Pedro Acevedo assisted with species identification. Trait data collected by NGS was supported by a Smithsonian Center for Tropical Forest Science grant; Silvia Bibbo and Aaron Hogan helped collect additional functional trait data. We thank Robin Chazdon, Benedict Bachelot, Jesse Lasky and two anonymous reviewers for helpful comments on a previous version of this manuscript. This work was supported by NSF DEB 1050957 and EF 1137239 to MU, NSF DEB 1311367 to MU and RM, NSF DBI 1401312 to RM, and grants from the Earth Institute and the Institute of Latin American studies at Columbia University. The authors have no conflict of interest to declare. NR 108 TC 0 Z9 0 U1 22 U2 22 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1433-8319 J9 PERSPECT PLANT ECOL JI Perspect. Plant Ecol. Evol. Syst. PD DEC PY 2016 VL 23 BP 52 EP 62 DI 10.1016/j.ppees.2016.09.007 PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA EI5UV UT WOS:000392562200005 ER PT J AU Gonzalez-Terrazas, TP Viquez, LR Ibarra-Macias, A Ruiz, AT Torres-Knoop, L Jung, K Tschapka, M Medellin, RA AF Gonzalez-Terrazas, Tania P. Viquez, Luis R. Ibarra-Macias, Ana Ruiz, Adrian Tonatiuh Torres-Knoop, Leonora Jung, Kirsten Tschapka, Marco Medellin, Rodrigo A. TI New records and range extension of Promops centralis (Chiroptera: Molossidae) SO REVISTA MEXICANA DE BIODIVERSIDAD LA English DT Article DE Aerial insectivores; Bahia de Kino; Echolocation; Molossids; Northern Mexico ID MAMMALS; FAUNA; BATS AB We captured Promops centralis and recorded its echolocation calls in Bahia de Kino, Sonora, which represents the first record of this species for the state of Sonora, Mexico. Our new record extends the distribution of P. centralis at least 1,300 km northwest from the northernmost known locality, Cuautla, Jalisco. Until now, there was no evidence of the occurrence of P. centralis in the deserts of northern Mexico. These new records are ecologically significant as they show that this species also occurs in extreme dry areas such as the Sonoran Desert. Our findings suggest that P. centralis may be more widely distributed than previously thought. (C) 2016 Universidad Nacional Autonoma de Mexico, Instituto de Biologia. This is an open access article under the CC BY-NC-ND license. C1 [Gonzalez-Terrazas, Tania P.; Viquez, Luis R.; Jung, Kirsten; Tschapka, Marco] Inst Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Viquez, Luis R.; Ibarra-Macias, Ana; Torres-Knoop, Leonora; Medellin, Rodrigo A.] Univ Nacl Autonoma Mexico, Inst Ecol, Tercer Circuito S-N,Ciudad Univ, Mexico City 04318, DF, Mexico. [Ruiz, Adrian Tonatiuh] Univ Ulm, Inst Neural Informat Proc, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Panama. RP Gonzalez-Terrazas, TP (reprint author), Inst Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM tania.gonzalez@uni-ulm.de FU DFG-Conacyt Bilateral Cooperation program [190901, TS 81/8-1, TS 81/8-2] FX We want to think all the people who contributed to the field work. Scientific collecting permits were provided to R.A.M. by the Secretaria del Medio Ambiente y Recursos Naturales (FAUT-0001). This study was supported by a joint DFG-Conacyt Bilateral Cooperation program under the number 190901 [to R.A.M] and TS 81/8-1 and 8-2 [to M.T. and K.J.] NR 22 TC 0 Z9 0 U1 2 U2 2 PU INST BIOLOGIA, UNIV NACIONAL AUTONOMA MEXICO PI MEXICO PA APARTADO POSTAL 70-233, MEXICO, D F 00000, MEXICO SN 1870-3453 J9 REV MEX BIODIVERS JI Rev. Mex. Biodivers. PD DEC PY 2016 VL 87 IS 4 BP 1407 EP 1411 DI 10.1016/j.rmb.2016.10.008 PG 5 WC Biodiversity Conservation SC Biodiversity & Conservation GA EI0LR UT WOS:000392166500034 ER PT J AU Steiner, WE AF Steiner, Warren E., Jr. TI NEW ASSIGNMENTS AMONG THE GENERA HAPLANDRUS LECONTE, METACLISA JACQUELIN DU VAL AND THARSUS LECONTE WITH DESCRIPTIONS OF LARVAE AND PUPAE AND A NEW GENUS FOR NORTH AMERICA (COLEOPTERA: TENEBRIONIDAE) SO ANNALES ZOOLOGICI LA English DT Article; Proceedings Paper CT 4th International Tenebrionoidea Symposium (ITS) CY NOV 25-26, 2015 CL Inst Argentino Investigaciones Zonas Aridas, Mendoza, ARGENTINA SP CONICET, Centro Cientifico Tecnologico HO Inst Argentino Investigaciones Zonas Aridas DE Cnodalonini; darkling beetles; new combination; holarctic; larvae; pupae; saproxylic insects; synonymy; taxonomy; Tenebrionini ID DARKLING BEETLES COLEOPTERA; RECONSTITUTION; GLANDS; TRIBES AB The five species currently placed in the North American genus Haplandrus LeConte 1862 are examined, with new information on immature stages, distribution, and life history. The type-species, H. fulvipes (Herbst 1797) as a member of Stenochiinae/Cnodalonini is redescribed along with its larva and pupa; a closely related new species is proposed for specimens from peninsular Florida. Reassignments and new synonymies are proposed for the other species which belong in other genera and tribes of Tenebrioninae. Haplandrus ater (LeConte 1866) is transferred back to Metaclisa Jacquelin du Val 1861; H. collaris Casey 1924 and H. subangustus Casey 1924 are junior synonyms of that species. North American members of Metaclisa are reviewed, with a description of the larva and pupa of M. atra. Tharsus LeConte 1862 recognized as a new synonym of Metaclisa. With a discussion of morphology and placement of the genus, the new tribe Metaclisini is proposed. The new genus Bouchardandrus is proposed to include the boreal H. concolor LeConte 1866 which has characters that place it among genera of Tenebrionini. C1 [Steiner, Warren E., Jr.] Smithsonian Inst, Dept Entomol, NHB 187, Washington, DC 20560 USA. RP Steiner, WE (reprint author), Smithsonian Inst, Dept Entomol, NHB 187, Washington, DC 20560 USA. EM steinerw@si.edu NR 32 TC 1 Z9 1 U1 0 U2 0 PU MUSEUM & INST ZOOLOGY PAS-POLISH ACAD SCIENCES PI WARSAW PA WILCZA STREET 64, 00-679 WARSAW, POLAND SN 0003-4541 EI 1734-1833 J9 ANN ZOOL JI Ann. Zool. PD DEC PY 2016 VL 66 IS 4 BP 529 EP 550 DI 10.3161/00034541ANZ2016.66.4.005 PG 22 WC Entomology SC Entomology GA EH5MI UT WOS:000391816800005 ER PT J AU Collins, ES Gostel, MR Weeks, A AF Collins, Elizabeth S. Gostel, Morgan R. Weeks, Andrea TI AN EXPANDED NUCLEAR PHYLOGENOMIC PCR TOOLKIT FOR SAPINDALES SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE Anacardiaceae; Burseraceae; low-copy nuclear genes; microfluidic PCR; Rutaceae ID HISTORICAL BIOGEOGRAPHY; COMMIPHORA BURSERACEAE; EVOLUTION; PHYLOGENETICS; GENUS AB Premise of the study: We tested PCR amplification of 91 low-copy nuclear gene loci in taxa from Sapindales using primers developed for Bursera simaruba (Burseraceae). Methods and Results: Cross-amplification of these markers among 10 taxa tested was related to their phylogenetic distance from B. simaruba. On average, each Sapindalean taxon yielded product for 53 gene regions (range: 16-90). Arabidopsis thaliana (Brassicales), by contrast, yielded product for two. Single representatives of Anacardiaceae and Rutacaeae yielded 34 and 26 products, respectively. Twenty-six primer pairs worked for all Burseraceae species tested if highly divergent Aucoumea klaineana is excluded, and eight of these amplified product in every Sapindalean taxon. Conclusions: Our study demonstrates that customized primers for Bursera can amplify product in a range of Sapindalean taxa. This collection of primer pairs, therefore, is a valuable addition to the toolkit for nuclear phylogenomic analyses of Sapindales and warrants further investigation. C1 [Collins, Elizabeth S.; Weeks, Andrea] George Mason Univ, 4400 Univ Dr,MSN 3E1, Fairfax, VA 22030 USA. [Gostel, Morgan R.] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. RP Collins, ES (reprint author), George Mason Univ, 4400 Univ Dr,MSN 3E1, Fairfax, VA 22030 USA. EM ecolli11@masonlive.gmu.edu FU National Science Foundation [1403150]; Provost/COS/ESP Institutional Graduate Fellowship Research Award from George Mason University; George Mason University Libraries Open Access Publishing Fund FX The authors thank Cintia Silva-Luz for providing leaf material of Schinus and Beiselia. Research was supported in part by the National Science Foundation (grant no. 1403150 to M.R.G. and A.W.) and the Provost/COS/ESP Institutional Graduate Fellowship Research Award to E.S.C. from George Mason University. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. Publication of this article was funded in part by the George Mason University Libraries Open Access Publishing Fund. NR 15 TC 0 Z9 0 U1 2 U2 2 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD DEC PY 2016 VL 4 IS 12 AR 1600078 DI 10.3732/apps.1600078 PG 8 WC Plant Sciences SC Plant Sciences GA EH4DA UT WOS:000391720000002 ER PT J AU Gilbert, GS Ballesteros, JO Barrios-Rodriguez, CA Bonadies, EF Cedeno-Sanchez, ML Fossatti-Caballero, NJ Trejos-Rodriguez, MM Perez-Suniga, JM Holub-Young, KS Henn, LAW Thompson, JB Garcia-Lopez, CG Romo, AC Johnston, DC Barrick, PP Jordan, FA Hershcovich, S Russo, N Sanchez, JD Fabrega, JP Lumpkin, R McWilliams, HA Chester, KN Burgos, AC Wong, EB Diab, JH Renteria, SA Harrower, JT Hooton, DA Glenn, TC Faircloth, BC Hubbell, SP AF Gilbert, Gregory S. Ballesteros, Javier O. Barrios-Rodriguez, Cesar A. Bonadies, Ernesto F. Cedeno-Sanchez, Marjorie L. Fossatti-Caballero, Nohely J. Trejos-Rodriguez, Mariam M. Moises Perez-Suniga, Jose Holub-Young, Katharine S. Henn, Laura A. W. Thompson, Jennifer B. Garcia-Lopez, Cesar G. Romo, Amanda C. Johnston, Daniel C. Barrick, Pablo P. Jordan, Fulvia A. Hershcovich, Shiran Russo, Natalie David Sanchez, Juan Pablo Fabrega, Juan Lumpkin, Raleigh McWilliams, Hunter A. Chester, Kathleen N. Burgos, Alana C. Beatriz Wong, E. Diab, Jonathan H. Renteria, Sonia A. Harrower, Jennifer T. Hooton, Douglas A. Glenn, Travis C. Faircloth, Brant C. Hubbell, Stephen P. TI USE OF SONIC TOMOGRAPHY TO DETECT AND QUANTIFY WOOD DECAY IN LIVING TREES SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE acoustic tomography; Argus PiCUS 3 Sonic Tomograph; ImageJ; tropical trees ID STANDING TREES; FOREST; ROT AB Premise of the study: Field methodology and image analysis protocols using acoustic tomography were developed and evaluated as a tool to estimate the amount of internal decay and damage of living trees, with special attention to tropical rainforest trees with irregular trunk shapes. Methods and Results: Living trunks of a diversity of tree species in tropical rainforests in the Republic of Panama were scanned using an Argus Electronic PiCUS 3 Sonic Tomograph and evaluated for the amount and patterns of internal decay. A protocol using ImageJ analysis software was used to quantify the proportions of intact and compromised wood. The protocols provide replicable estimates of internal decay and cavities for trees of varying shapes, wood density, and bark thickness. Conclusions: Sonic tomography, coupled with image analysis, provides an efficient, noninvasive approach to evaluate decay patterns and structural integrity of even irregularly shaped living trees. C1 [Gilbert, Gregory S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Gilbert, Gregory S.] Univ Calif Santa Cruz, Dept Environm Studies, 1156 High St, Santa Cruz, CA 95064 USA. [Garcia-Lopez, Cesar G.; McWilliams, Hunter A.] Watsonville High Sch, 250 East Beach St, Watsonville, CA 95076 USA. [Bonadies, Ernesto F.; Johnston, Daniel C.] Inst Alberto Einstein, Apartado 6705, Panama, Panama. [Barrios-Rodriguez, Cesar A.; Henn, Laura A. W.; Jordan, Fulvia A.; Pablo Fabrega, Juan; McWilliams, Hunter A.] Acad Interamer Panam, Blvd Costa Este, Panama City, Panama. [Barrios-Rodriguez, Cesar A.; Thompson, Jennifer B.; Johnston, Daniel C.; Lumpkin, Raleigh] Acad Athens, 1281 Spartan Lane, Athens, GA 30606 USA. [Bonadies, Ernesto F.; Henn, Laura A. W.; Romo, Amanda C.] Lyons Community Sch, 223 Graham Ave, Brooklyn, NY 11206 USA. [Johnston, Daniel C.; Barrick, Pablo P.; David Sanchez, Juan] Ctr Educ Monse Francisco Beckmann, Panama City, Panama. [Barrios-Rodriguez, Cesar A.; Thompson, Jennifer B.; Barrick, Pablo P.; Hershcovich, Shiran; Burgos, Alana C.] Cabrillo Coll, Biol Dept, 6500 Soquel Dr, Aptos, CA 95003 USA. [Bonadies, Ernesto F.; Henn, Laura A. W.; Hershcovich, Shiran; Russo, Natalie] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Bonadies, Ernesto F.; Johnston, Daniel C.; Lumpkin, Raleigh] Dept Environm Hlth Sci, 150 Green St, Athens, GA 30602 USA. [Cedeno-Sanchez, Marjorie L.; Henn, Laura A. W.; Garcia-Lopez, Cesar G.; Johnston, Daniel C.; Russo, Natalie; Chester, Kathleen N.] Louisiana State Univ, Dept Biol Sci, 202 Life Sci Bldg, Baton Rouge, LA 70803 USA. [Gilbert, Gregory S.; Barrios-Rodriguez, Cesar A.; Moises Perez-Suniga, Jose; Thompson, Jennifer B.; Hershcovich, Shiran] Louisiana State Univ, Museum Nat Sci, 202 Life Sci Bldg, Baton Rouge, LA 70803 USA. RP Gilbert, GS (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama.; Gilbert, GS (reprint author), Univ Calif Santa Cruz, Dept Environm Studies, 1156 High St, Santa Cruz, CA 95064 USA.; Gilbert, GS (reprint author), Louisiana State Univ, Museum Nat Sci, 202 Life Sci Bldg, Baton Rouge, LA 70803 USA. EM ggilbert@ucsc.edu FU National Science Foundation [DEB-1136626, DEB-143741] FX This research was made possible by grants from the National Science Foundation (DEB-1136626 and DEB-143741), logistical support from the Smithsonian Tropical Research Institute, and permissions (SE/P-24-13, SE/APH-3-14, SE/P-17-14, SE/P-7-15) to conduct research in Panamanian forests from the Autoridad Nacional del Ambiente (ANAM), Republic of Panama. NR 25 TC 0 Z9 0 U1 5 U2 5 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD DEC PY 2016 VL 4 IS 12 AR 1600060 DI 10.3732/apps.1600060 PG 13 WC Plant Sciences SC Plant Sciences GA EH4DA UT WOS:000391720000001 ER PT J AU Zhou, JN Dudash, MR Fenster, CB Zimmer, EA AF Zhou, Juannan Dudash, Michele R. Fenster, Charles B. Zimmer, Elizabeth A. TI DEVELOPMENT OF HIGHLY VARIABLE MICROSATELLITE MARKERS FOR THE TETRAPLOID SILENE STELLATA (CARYOPHYLLACEAE) SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE Caryophyllaceae; microsatellites; plant-animal interaction; polyploidy; Silene stellata ID MODEL SYSTEM; EVOLUTION; POLLINATION; PLANT AB Premise of the study: We designed and tested microsatellite markers for the North American native species Silene stellata (Caryophyllaceae) to investigate its population genetic structure and identify selection on floral design through male reproductive success. Methods and Results: A total of 153 candidate microsatellite loci were isolated based on next-generation sequencing. We identified 18 polymorphic microsatellite loci in three populations of S. stellata, with di-or trinucleotide repeats. Genotyping results showed the number of alleles per locus ranged from six to 45 and expected heterozygosity ranged from 0.511 to 0.951. Five of these loci were successfully amplified in S. virginica and S. caroliniana and were also polymorphic. Conclusions: The microsatellite markers reported here provide a valuable tool for paternity analysis in S. stellata. They will also be useful for investigating the population genetic structures of S. stellata and related species. C1 [Zhou, Juannan] Univ Maryland, Behav Ecol Evolut & Systemat Grad Program, College Pk, MD 20742 USA. [Zhou, Juannan; Zimmer, Elizabeth A.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. [Dudash, Michele R.] South Dakota State Univ, Dept Nat Resource Management, Brookings, SD 57007 USA. [Fenster, Charles B.] South Dakota State Univ, Dept Biol & Microbiol, Brookings, SD 57007 USA. RP Zhou, JN (reprint author), Univ Maryland, Behav Ecol Evolut & Systemat Grad Program, College Pk, MD 20742 USA.; Zhou, JN (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. EM jnzhou@umd.edu NR 13 TC 0 Z9 0 U1 0 U2 0 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD DEC PY 2016 VL 4 IS 12 AR 1600117 DI 10.3732/apps.1600117 PG 4 WC Plant Sciences SC Plant Sciences GA EH4DA UT WOS:000391720000007 ER PT J AU Gautier, L Lachenaud, O van der Burgt, X Kenfack, D AF Gautier, Laurent Lachenaud, Olivier van der Burgt, Xander Kenfack, David TI Five new species of Englerophytum K. Krause (Sapotaceae) from central Africa SO CANDOLLEA LA English DT Article ID ERICALES AB Five new species of Englerophytum K. Krause (Sapotaceae) are described : Englerophytum paludosum L. Gaut., Burgt & O. Lachenaud, Englerophytum gigantifolium O. Lachenaud & L. Gaut., Englerophytum libenii O. Lachenaud & L. Gaut., Englerophytum sylverianum Kenfack & L. Gaut., and Englerophytum ferrugineum L. Gaut. & O. Lachenaud. All five species are illustrated with line drawings and three of them with field photos. Distribution maps are also provided, and a preliminary extinction risk assessment according to IUCN Categories and Criteria is carried out : Englerophytum paludosum is assessed as "Least Concern", Englerophytum sylverianum as "Vulnerable", Englerophytum libenii and Englerophytum ferrugineum as "Endangered", and Englerophytum gigantifolium as "Critically Endangered". C1 [Gautier, Laurent] Univ Geneva, Conservatoire & Jardin Bot Ville Geneve, CP 60, CH-1292 Chambesy, Switzerland. [Gautier, Laurent] Univ Geneva, Lab Systemat & Biodiversite, CP 60, CH-1292 Chambesy, Switzerland. [Lachenaud, Olivier] Domein Bouchout, Bot Garden Meise, B-1860 Meise, Belgium. [van der Burgt, Xander] Royal Bot Gardens, Herbarium, Richmond, Surrey, England. [Kenfack, David] NMNH, Ctr Trop Forest Sci, Forest Global Earth Observ, Smithsonian Trop Res Inst, POB 37012, Washington, DC 20013 USA. RP Gautier, L (reprint author), Univ Geneva, Conservatoire & Jardin Bot Ville Geneve, CP 60, CH-1292 Chambesy, Switzerland.; Gautier, L (reprint author), Univ Geneva, Lab Systemat & Biodiversite, CP 60, CH-1292 Chambesy, Switzerland. EM laurent.gautier@ville-ge.ch FU WWF-Gabon; Ministry of Water and Forests FX The authors would like to express their thanks to the curators and staff of the Herbaria BR, BRLU, COI, G, K, MO, P, WAG, Z for making accessible their collections through loans or digital images. We are also indebted to Barbara Mackinder and David Harris (E) who have made available unpublished results on phylogeny of Englerophytum and allied genera. Many thanks also to Antonio Fernandez, Gabriela Loza, Lucy Smith and Alice Tangerini for their nice drawings. Paul Maas kindly allowed us to publish his photograph of Englerophytum paludosum and Moses Sainge one of the photographs of E. sylverianum. The Center for Tropical Forest Science Forest Global Earth Observatory of the Smithsonian Tropical Research institute is thanked for their support of fieldwork that led to the discovery of E. sylverianum. OL wishes to thank the IPHAMETRA (Institut de Pharmacopee et de Medecine Traditionnelle, CENAREST) and its Director, Dr. Henri Paul Bourobou Bourobou, for supporting our research in Gabon. Fieldwork in Gabon was undertaken under the Memory of Understanding between the Centre National de la Recherche Scientifique et Technologique (CENAREST) and the Missouri Botanical Garden (MBG). He is also grateful to Eric Akouangou, Ehoarn Bidault, Archange Boupoya, Davy Ikabanga, Yves Issembe, John Kaparidi, Brandet Lissambou, Jean-Yves Serein and Tariq Stevart for their help during field work. Some of the collections that led to this paper were made during the inventory of the Bas-Ogooue Ramsar site, organised by the Missouri Botanical Garden with support from WWF-Gabon and the Ministry of Water and Forests. The type of E. gigantifolium was collected during the Environmental Impact Study of the Mabounie project in Gabon; the staff of the Maboumine company (Eramet) are acknowledged for their help and assistance in the field. Finally, Martin Callmander and an anonymous reviewer made helpful comments on the first version of this contribution. NR 16 TC 0 Z9 0 U1 0 U2 0 PU CONSERVATOIRE ET JARDIN BOTANIQUES VILLE GENEVE PI CHAMBESY PA CASE POSTALE 60, CH-1292 CHAMBESY, SWITZERLAND SN 0373-2967 J9 CANDOLLEA JI Candollea PD DEC PY 2016 VL 71 IS 2 BP 287 EP 305 DI 10.15553/c2016v712a14 PG 19 WC Plant Sciences SC Plant Sciences GA EH1VN UT WOS:000391555800014 ER PT J AU McCravy, KW Van Dyke, J Creedy, TJ Roubik, DW AF McCravy, Kenneth W. Van Dyke, Joseph Creedy, Thomas J. Roubik, David W. TI Orchid bees (Hymenoptera: Apidae: Euglossini) of Cusuco National Park, State of Cortes, Honduras SO FLORIDA ENTOMOLOGIST LA English DT Article DE Mesoamerican euglossines; Neotropical cloud forest; pollinator biodiversity; habitat fragmentation ID DIVERSITY; CHECKLIST; FLORIDA; PANAMA AB Orchid bees (Hymenoptera: Apidae: Euglossini) are abundant and important pollinators of Neotropical forests, but orchid bee diversity is still poorly known in much of Mesoamerica, particularly in cloud forests. This paper presents results of a 2012 to 2013 survey of orchid bee diversity in Cusuco National Park, a cloud forest environment in northwest Honduras. Orchid bees were collected using insect nets at bait stations with chemical attractants. Bait stations were located at 68 sample sites throughout the park. We collected 4,293 orchid bees representing 24 species and 4 genera. One species, Euglossa imperialis Cockerell, accounted for 67.6% of the total individuals collected. A substantial easterly range extension was established for Eufriesea pallida (Kimsey). Our study provides the first intensive inventory of cloud forest orchid bee diversity in the region. Furthermore, it provides baseline data for future studies of orchid bees in a key biodiversity area that is threatened by human population growth and associated land use changes. C1 [McCravy, Kenneth W.] Western Illinois Univ, Dept Biol Sci, 1 Univ Circle, Macomb, IL 61455 USA. [McCravy, Kenneth W.; Van Dyke, Joseph; Creedy, Thomas J.] Operat Wallacea, Hope House, Spilsby PE23 4EX, Lincs, England. [Van Dyke, Joseph] West Virginia Univ, Dept Biol, Morgantown, WV 26505 USA. [Creedy, Thomas J.] Univ Oxford, Museum Nat Hist, Hope Entomol Collect, Parks Rd, Oxford OX1 3PW, England. [Creedy, Thomas J.] Imperial Coll London, Dept Life Sci, Exhibit Rd, London SW7 2AZ, England. [Creedy, Thomas J.] Nat Hist Museum, Cromwell Rd, London SW7 5BD, England. [Roubik, David W.] Smithsonian Trop Res Inst, Balboa, Panama. RP McCravy, KW (reprint author), Western Illinois Univ, Dept Biol Sci, 1 Univ Circle, Macomb, IL 61455 USA.; McCravy, KW (reprint author), Operat Wallacea, Hope House, Spilsby PE23 4EX, Lincs, England. EM KW-McCravy@wiu.edu; JW-VanDyke2@wiu.edu; thomas@tjcreedy.co.uk; roubikd@si.edu FU Operation Wallacea; Western Illinois University Office of Sponsored Projects and Research Foundation FX We thank Brandon Taylor, Fabian Wagner, Harriet Downey, Katie Williams, and numerous Operation Wallacea volunteers, staff, and local guides for invaluable assistance with orchid bee collecting. We also thank Sarah Wilcer (Western Illinois University) for help with orchid bee pinning and labeling, and Shane Mason (Western Illinois University) for making and contributing the maps for Fig. 1. We thank Operation Wallacea for invaluable financial and logistical support, and the Western Illinois University Office of Sponsored Projects and Research Foundation for generous funding for this study. NR 24 TC 0 Z9 0 U1 10 U2 10 PU FLORIDA ENTOMOLOGICAL SOC PI LUTZ PA 16125 E LAKE BURRELL DR, LUTZ, FL 33548 USA SN 0015-4040 EI 1938-5102 J9 FLA ENTOMOL JI Fla. Entomol. PD DEC PY 2016 VL 99 IS 4 BP 765 EP 768 PG 4 WC Entomology SC Entomology GA EH1KO UT WOS:000391525700031 ER PT J AU Lee, JL Thompson, A Mulcahy, DG AF Lee, Justin L. Thompson, Adrian Mulcahy, Daniel G. TI Relationships between Numbers of Vertebrae, Scale Counts, and Body Size, with Implications for Taxonomy in Nightsnakes (Genus: Hypsiglena) SO JOURNAL OF HERPETOLOGY LA English DT Article ID GEOGRAPHIC-VARIATION; NIGHT SNAKE; EVOLUTION; TORQUATA; POPULATIONS; COLUBRIDAE; SELECTION AB The relationships between the number of trunk and caudal vertebrae, the number of ventral and subcaudal scales, and snout-vent length (SVL) and tail length were investigated in several species of Hypsiglena, including a few specimens from species contact zones. We confirm the presence of a 1: 1 relationship between trunk vertebrae and ventral scales within Hypsiglena (99 specimens total; 50 males; 49 females). We also found a positive relationship between the number of ventral scales and SVL in adult specimens. We did not find a 1: 1 relationship between caudal vertebrae and subcaudal scales, but there is a positive relationship between subcaudal scales and tail length. Because there is a positive relationship with the number of ventral scales and SVL, we infer-as general population trends-that snakes with more ventral scales have the capacity to grow to be larger than snakes with fewer ventral scales. Many other environmental factors influence body size, however, and this trend should be used only as a general comparison. Therefore, the number of ventral scales can be used as a proxy for general population trends in body size among species of Hypsiglena, as wide geographic-ranging species may be exposed to large-scale environmental gradients (e.g., lower temperatures at higher latitudes). Ventral and subcaudal scale counts may not be good diagnostic characters for assigning individual specimens to taxonomic groups or for diagnosing taxonomic groups, because species appear to show much overlapping variation. This variation may be good for examining different trends in body size between taxa across geographic landscapes. C1 [Lee, Justin L.; Mulcahy, Daniel G.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Thompson, Adrian] Howard Univ, Dept Biol, Washington, DC 20059 USA. RP Mulcahy, DG (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. EM MulcahyD@si.edu NR 39 TC 0 Z9 0 U1 1 U2 1 PU SOC STUDY AMPHIBIANS REPTILES PI ST LOUIS PA C/O ROBERT D ALDRIDGE, ST LOUIS UNIV, DEPT BIOLOGY, 3507 LACLEDE, ST LOUIS, MO 63103 USA SN 0022-1511 EI 1937-2418 J9 J HERPETOL JI J. Herpetol. PD DEC PY 2016 VL 50 IS 4 BP 616 EP 620 DI 10.1670/15-066 PG 5 WC Zoology SC Zoology GA EH5ND UT WOS:000391818900016 ER PT J AU Gallagher, AJ Brandl, SJ Stier, AC AF Gallagher, Austin J. Brandl, Simon J. Stier, Adrian C. TI Intraspecific variation in body size does not alter the effects of mesopredators on prey SO ROYAL SOCIETY OPEN SCIENCE LA English DT Article DE predator; risk; functional response; fish ID CORAL-REEF FISH; PREDATOR DENSITY; MODELS AB As humans continue to alter the species composition and size structure of marine food webs, it is critical to understand size-dependent effects of predators on prey. Yet, how shifts in predator body size mediate the effect of predators is understudied in tropical marine ecosystems, where anthropogenic harvest has indirectly increased the density and size of small-bodied predators. Here, we combine field surveys and a laboratory feeding experiment in coral reef fish communities to show that small and large predators of the same species can have similar effects. Specifically, surveys show that the presence of a small predator (Paracirrhites arcatus) was correlated with lower chances of prey fish presence, but these correlations were independent of predator size. Experimental trials corroborated the size-independent effect of the predator; attack rates were indistinguishable between small and large predators, suggesting relatively even effects of hawkfish in various size classes on the same type of prey. Our results indicate that the effects of small predators on coral reefs can be size-independent, suggesting that variation in predator size-structure alone may not always affect the functional role of these predators. C1 [Gallagher, Austin J.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. [Gallagher, Austin J.; Brandl, Simon J.] Beneath Waves Inc, Miami, FL 33133 USA. [Brandl, Simon J.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Stier, Adrian C.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. RP Gallagher, AJ (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA.; Gallagher, AJ (reprint author), Beneath Waves Inc, Miami, FL 33133 USA. EM agallagher@rsmas.miami.edu NR 30 TC 0 Z9 0 U1 1 U2 1 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 2054-5703 J9 ROY SOC OPEN SCI JI R. Soc. Open Sci. PD DEC PY 2016 VL 3 IS 12 AR 160414 DI 10.1098/rsos.160414 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EH4HH UT WOS:000391731800006 PM 28083093 ER PT J AU Birnstiel, T Fang, M Johansen, A AF Birnstiel, T. Fang, M. Johansen, A. TI Dust Evolution and the Formation of Planetesimals SO SPACE SCIENCE REVIEWS LA English DT Review DE Accretion disks; Planets and satellites: formation; Protoplanetary disks; Circumstellar matter ID YOUNG STELLAR OBJECTS; T-TAURI STARS; SPECTRAL ENERGY-DISTRIBUTIONS; SPITZER-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; TRANSITIONAL PROTOPLANETARY DISKS; HIGH-RESOLUTION SUBMILLIMETER; POLARIZED SCATTERED-LIGHT; HEAD-ON COLLISIONS; HERBIG AE/BE STARS AB The solid content of circumstellar disks is inherited from the interstellar medium: dust particles of at most a micrometer in size. Protoplanetary disks are the environment where these dust grains need to grow at least 13 orders of magnitude in size. Our understanding of this growth process is far from complete, with different physics seemingly posing obstacles to this growth at various stages. Yet, the ubiquity of planets in our galaxy suggests that planet formation is a robust mechanism. This chapter focuses on the earliest stages of planet formation, the growth of small dust grains towards the gravitationally bound "planetesimals", the building blocks of planets. We will introduce some of the key physics involved in the growth processes and discuss how they are expected to shape the global behavior of the solid content of disks. We will consider possible pathways towards the formation of larger bodies and conclude by reviewing some of the recent observational advances in the field. C1 [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Birnstiel, T.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Fang, M.] Purple Mt Observ, 2 West Beijing Rd, Nanjing 210008, Peoples R China. [Fang, M.] Key Lab Radio Astron, 2 West Beijing Rd, Nanjing 210008, Peoples R China. [Johansen, A.] Lund Univ, Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden. RP Birnstiel, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Birnstiel, T (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM tbirnstiel@cfa.harvard.edu; mfang@pmo.ac.cn; anders@astro.lu.se FU NASA Origins of Solar Systems grant [NNX12AJ04G]; DFG [KL 1469/13-1]; NSFC [11203081]; European Research Council [278675-PEBBLE2PLANET]; Knut and Alice Wallenberg Foundation; Swedish Research Council [2014-5775] FX We like to thank Liubin Pan, Christian Lenz, and the referees, Willy Benz and Alessandro Morbidelli for providing helpful comments that have significantly improved the manuscript. T.B. acknowledges support from the NASA Origins of Solar Systems grant NNX12AJ04G and from the DFG through grant KL 1469/13-1. M.F. acknowledges support by the NSFC through grant 11203081. A.J. is grateful for support from a Starting Grant from the European Research Council (278675-PEBBLE2PLANET) and the Knut and Alice Wallenberg Foundation and the Swedish Research Council (2014-5775). NR 239 TC 3 Z9 3 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2016 VL 205 IS 1-4 BP 41 EP 75 DI 10.1007/s11214-016-0256-1 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EH4VP UT WOS:000391769100003 ER PT J AU Baruteau, C Bai, XN Mordasini, C Molliere, P AF Baruteau, Clement Bai, Xuening Mordasini, Christoph Molliere, Paul TI Formation, Orbital and Internal Evolutions of Young Planetary Systems SO SPACE SCIENCE REVIEWS LA English DT Review DE Planets and satellites: formation; Planets and satellites: interiors; Protoplanetary disks; Planet-disk interactions ID EXTRASOLAR GIANT PLANETS; LOW-MASS PLANETS; IN-SITU FORMATION; STELLAR IRRADIATED DISCS; B-LIKE PLANETS; HD 100546 B; PROTOPLANETARY DISKS; BROWN DWARFS; SUPER-EARTHS; POPULATION SYNTHESIS AB The growing body of observational data on extrasolar planets and protoplanetary disks has stimulated intense research on planet formation and evolution in the past few years. The extremely diverse, sometimes unexpected physical and orbital characteristics of exoplanets lead to frequent updates on the mainstream scenarios for planet formation and evolution, but also to the exploration of alternative avenues. The aim of this review is to bring together classical pictures and new ideas on the formation, orbital and internal evolutions of planets, highlighting the key role of the protoplanetary disk in the various parts of the theory. We begin by briefly reviewing the conventional mechanism of core accretion by the growth of planetesimals, and discuss a relatively recent model of core growth through the accretion of pebbles. We review the basic physics of planet-disk interactions, recent progress in this area, and discuss their role in observed planetary systems. We address the most important effects of planets internal evolution, like cooling and contraction, the mass-luminosity relation, and the bulk composition expressed in the mass-radius and mass-mean density relations. C1 [Baruteau, Clement] Univ Toulouse, CNRS, Inst Rech Astrophys & Plan, Toulouse, France. [Bai, Xuening] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Mordasini, Christoph] Univ Bern, Phys Inst, Bern, Switzerland. [Molliere, Paul] Max Planck Inst Astron, Heidelberg, Germany. RP Baruteau, C (reprint author), Univ Toulouse, CNRS, Inst Rech Astrophys & Plan, Toulouse, France. EM clement.baruteau@irap.omp.eu FU Hubble Fellowship; ITC Fellowship; Swiss National Science Foundation [BSSGI0_155816 "PlanetsInTime"] FX We thank the organizers of the ISSI workshop "The Disk in Relation to the Formation of Planets and their Protoatmospheres", which was held in Beijing in August 2014. We thank D. Lin, N. Madhusudhan, Z. Sandor and S. Udry for stimulating discussions at the workshop. We thank Gabriel Marleau for interesting discussions and for providing Figure 7, and David Swoboda and Yann Alibert for providing the starting data for Figure 11. We also thank Aurelien Crida and Bertram Bitsch for detailed comments on an earlier draft of this paper, and the referee for a detailed and constructive report. XNB acknowledges support from Hubble and ITC Fellowships. CM acknowledges the support from the Swiss National Science Foundation under grant BSSGI0_155816 "PlanetsInTime". NR 293 TC 0 Z9 0 U1 3 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2016 VL 205 IS 1-4 BP 77 EP 124 DI 10.1007/s11214-016-0258-z PG 48 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EH4VP UT WOS:000391769100004 ER PT J AU Hirai, RY Schuettpelz, E Huiet, L Pryer, KM Smith, AR Prado, J AF Hirai, Regina Y. Schuettpelz, Eric Huiet, Layne Pryer, Kathleen M. Smith, Alan R. Prado, Jefferson TI Phylogeny and relationships of the neotropical Adiantum raddianum group (Pteridaceae) SO TAXON LA English DT Article DE chlN; cpDNA; ferns; maidenhair ID RBCL NUCLEOTIDE-SEQUENCES; VITTARIOID FERNS; EXTANT FERNS; CLASSIFICATION; AFFINITIES; EVOLUTION; INFERENCE; TAXONOMY; MRBAYES; GENES AB With more than 200 species, the maidenhair fern genus Adiantum is among the top ten most diverse fern genera. Adiantum is pantropical in distribution and, due to the presence of a unique synapomorphy (sporangia borne on indusia rather than laminae), perhaps the most easily recognized fern genus. Many of its members, including numerous cultivars derived from A. raddianum, are grown as ornamentals. Because of its size, a comprehensive taxonomic study of Adiantum is difficult and the genus is perhaps better approached through a series of narrower studies. Here, we focus specifically on A. raddianum and putative allies. We find a newly defined A. raddianum group to be strongly supported as monophyletic and segregated from other maidenhair ferns on the basis of genetic as well as morphological characteristics. Bayesian inference and maximum likelihood analyses of plastid atpA, chlL, chlN, rbcL, and rpoA sequences support the A. raddianum Glade as sister to A. poiretii and its allies. We identify round-reniform indusia to be a characteristic of the A. raddianum group (vs. lunate in the A. poiretii group). Additionally, we find species in the A. poiretii group to differ in having a unique 66 nucleotide deletion in our chlN gene alignment. The neotropical A. raddianum group comprises at least 17 species (14 studied here), some widely distributed; one was recently described (A. alan-smithii). C1 [Hirai, Regina Y.; Prado, Jefferson] Inst Bot, CP 68041, BR-04045972 Sao Paulo, SP, Brazil. [Schuettpelz, Eric] Smithsonian Inst, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. [Huiet, Layne; Pryer, Kathleen M.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Smith, Alan R.] Univ Calif Berkeley, Univ Herbarium, 1001 Valley Life Sci Bldg 2465, Berkeley, CA 94720 USA. RP Hirai, RY (reprint author), Inst Bot, CP 68041, BR-04045972 Sao Paulo, SP, Brazil. EM regina.hirai@gmail.com RI Hirai, Regina/K-3913-2013; Prado, Jefferson/C-4766-2012 OI Prado, Jefferson/0000-0003-4783-3125 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2011/07164-3]; National Science Foundation (NSF) [DEB-1405181, DEB-1145614] FX This study was supported by the Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP, Proc. n. 2011/07164-3, to R.Y.H. and J.P.) and the National Science Foundation (NSF awards DEB-1405181 to E.S. and DEB-1145614 to K.M.P. and L.H.). We thank The New York Botanical Garden and Dr. Robbin C. Moran for providing herbarium access and facilities for the first author; curators of herbaria for loans and/or permission to examine their collections (B, DUKE, K, MCNS, MO, NY, P, S, UC, US); and Michael Kessler, Robbin C. Moran, Michael Sundue, Pedro Fiaschi, and Pedro B. Schwartsburd for providing us with silica-dried material. We also thank two anonymous referees for their comments and suggestions to improve the manuscript. NR 53 TC 0 Z9 0 U1 4 U2 4 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD DEC PY 2016 VL 65 IS 6 BP 1225 EP 1235 DI 10.12705/656.1 PG 11 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA EG9BC UT WOS:000391351000001 ER PT J AU Peterson, PM Romaschenko, K Arrieta, YH AF Peterson, Paul M. Romaschenko, Konstantin Arrieta, Yolanda Herrera TI A molecular phylogeny and classification of the Cynodonteae (Poaceae: Chloridoideae) with four new genera: Orthacanthus, Triplasiella, Tripogonella, and Zaqiqah; three new subtribes: Dactylocteniinae, Orininae, and Zaqiqahinae; and a subgeneric classification of Distichlis SO TAXON LA English DT Article DE Dactylocteniinae; Distichlis sect. Bajaenses; Distichlis sect. Monanthochloe; Distichlis sect Spicatae; ITS; Orininae; Orthacanthus; plastid DNA sequences; systematics; Tridentopsis; Triplasiella; Tripogonella; Zaqiqah; Zaqiqahinae ID INDIA; GENUS; GRAMINEAE; TRIODIINAE; DISPERSAL; SEQUENCES; INFERENCE; GRASSES; MRBAYES; TREES AB Morphologically, the tribe Cynodonteae is a diverse group of grasses containing about 839 species in 96 genera and 18 subtribes, found primarily in Africa, Asia, Australia, and the Americas. Because the classification of these genera and species has been poorly understood, we conducted a phylogenetic analysis on 213 species (389 samples) in the Cynodonteae using sequence data from seven plastid regions (rps16-trnK spacer, rps16 intron, rpoC2, rp132-trnL spacer, ndhF, ndhA intron, ccsA) and the nuclear ribosomal internal transcribed spacer regions (ITS 1 & 2) to infer evolutionary relationships and refine the current classification. The phylogenetic tree from the combined plastid and nuclear region is well resolved depicting a strongly supported monophyletic Cynodonteae that includes 17 strongly supported clades corresponding to the subtribes Tripogoninae, Pappophorinae, Traginae, Muhlenbergiinae, Hilariinae, Scleropogoninae, Boutelouinae, Monanthochloinae, Dactylocteniinae, Eleusininae, Aeluropodinae, Triodiinae, Orcuttiinae, Zaqiqahinae, Farragininae, Perotidinae, and Gouiniinae, and two moderately supported clades corresponding to the Orininae and Hubbardochloinae. The plastid data places Odyssea paucinervis as sister to Neobouteloua in the Dactylocteniinae whereas the nuclear ITS data places it as sister to Aeluropus in the Aeluropodinae. Odyssea mucronata is strongly supported sister to the Cteniinae, Trichoneurinae, Farragininae, Perotidinae, Hubbardochloinae, and the Gouiniinae, and not closely related to Odyssea paucinervis. The nuclear data placed Acrachne racemosa as sister to Dactyloctenium in the Dactylocteniinae while the plastid data places it near the base of the Eleusininae. Our new classification recognizes three new subtribes (bringing the total to 21 subtribes): Dactylocteniinae that includes Acrachne, Brachychloa, Dactyloctenium, and Neobouteloua; Orininae with Cleistogenes and Orinus; and Zaqiqahinae with a single genus, Zaqiqah gen. nov.; Hubbardochloinae (resurrected here) with seven genera; and describes four new genera: Orthacanthus (Traginae) with a single species, Triplasiella (Gouiniinae) with a single species, Tripogonella (Tripogoninae) with three species, and Zaqiqah with a single species. We additionally provide a subgeneric classification of Distichlis recognizing three sections: D. sect. Monanthochloe, D. sect. Bajaenses, and D. sect. Spicatae, the latter two representing new sections. The following nine new combinations are made: Distichlis sect. Monanthochloe, Orthacanthus pedunculatus, Tridentopsis buckleyana, Tridentopsis mutica var. elongata, Triplasiella eragrotoides, Tripogonella loliiformis, Tripogonella minima, Tripogonella spicata, and Zaqiqah mucronata. We lectotypify the following five names: Festuca loliiformis, F. minima, F. mucronata, Triodia eragrostoides, and Uralepis elongata. C1 [Peterson, Paul M.; Romaschenko, Konstantin] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Romaschenko, Konstantin] Natl Acad Sci, MG Kholodny Inst Bot, UA-01601 Kiev, Ukraine. [Arrieta, Yolanda Herrera] Inst Politecn Nacl, CIIDIR Unidad Durango COFAA, Durango 34220, Mexico. RP Peterson, PM (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. EM peterson@si.edu FU National Geographic Society Committee for Research and Exploration [8848-10, 8087-06]; Smithsonian Institution's Restricted Endowments Fund; Scholarly Studies Program; Research Opportunities, Atherton Seidell Foundation; Biodiversity Surveys and Inventories Program; Small Grants Program; Laboratory of Analytical Biology; United States Department of Agriculture FX We thank the National Geographic Society Committee for Research and Exploration (Grant No. 8848-10, 8087-06) for field and laboratory support; the Smithsonian Institution's Restricted Endowments Fund, the Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation, Biodiversity Surveys and Inventories Program, Small Grants Program, the Laboratory of Analytical Biology; and the United States Department of Agriculture, all for financial support. We would also like to acknowledge Robert J. Soreng and Jeffery M. Saarela for accompanying the first author on numerous field expeditions; Robert J. Soreng for many extended discussions pertinent to the manuscript, especially regarding nomenclature; and Neil Snow and Jeffery M. Saarela for providing helpful comments on the manuscript; and Franz Stadler for critical review during production. NR 86 TC 0 Z9 0 U1 4 U2 4 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD DEC PY 2016 VL 65 IS 6 BP 1263 EP 1287 DI 10.12705/656.4 PG 25 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA EG9BC UT WOS:000391351000004 ER PT J AU Funk, VA Torland, NJ AF Funk, Vicki A. Torland, Nicholas J. TI Institutional Votes at the XIX International Botanical Congress, Shenzhen, 2017: Report of the Special Committee on Institutional Votes SO TAXON LA English DT Article DE Code; International Botanical Congress; Nomenclature; Nomenclature Section; institutional votes AB The Special Committee on Institutional Votes was established at the XVIII International Botanical Congress (IBC), in Melbourne in 2011, with the mandate to consider the procedure by which institutional votes are allocated and to report to the XIX IBC in Shenzheri in 2017. The Special Committee contacted institutions worldwide and urged them to update their entries in Index Herbariorum and to request institutional votes for the first time or an increase in allocated votes. The Committee sent its recommendations for changes to the list of institutional votes for the Melbourne IBC to the Bureau of Nomenclature, which, in collaboration with the Special Committee, revised the list to produce the new list for the Shenzhen IBC. This new list was sent to the General Committee for final approval, as required by the International Code of Nomenclature for algae, fungi, and plants. The General Committee approved the list, which is now presented in this report. C1 [Funk, Vicki A.] Smithsonian Inst, US Natl Herbarium, Dept Bot, NMNH, MRC 166,POB 37012, Washington, DC 20013 USA. [Torland, Nicholas J.] Free Univ Berlin, Bot Garten, Konigin Luise Str 6-8, D-14195 Berlin, Germany. [Torland, Nicholas J.] Free Univ Berlin, Bot Museum Berlin, Konigin Luise Str 6-8, D-14195 Berlin, Germany. RP Funk, VA (reprint author), Smithsonian Inst, US Natl Herbarium, Dept Bot, NMNH, MRC 166,POB 37012, Washington, DC 20013 USA.; Torland, NJ (reprint author), Free Univ Berlin, Bot Garten, Konigin Luise Str 6-8, D-14195 Berlin, Germany.; Torland, NJ (reprint author), Free Univ Berlin, Bot Museum Berlin, Konigin Luise Str 6-8, D-14195 Berlin, Germany. EM funkv@si.edu; ri.turland@bgbm.org NR 6 TC 1 Z9 1 U1 1 U2 1 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD DEC PY 2016 VL 65 IS 6 BP 1449 EP 1454 DI 10.12705/656.33 PG 6 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA EG9BC UT WOS:000391351000033 ER PT J AU Jesionek, MB Bahia, RG Hernandez-Kanttun, JJ Adey, WH Yoneshigue-Valentin, Y Longo, LL Amado-Filho, GM AF Jesionek, Michel B. Bahia, Ricardo G. Hernandez-Kanttun, Jazmin J. Adey, Walter H. Yoneshigue-Valentin, Yocie Longo, Leila L. Amado-Filho, Gilberto M. TI A taxonomic account of non-geniculate coralline algae (Corallinophycidae, Rhodophyta) from shallow reefs of the Abrolhos Bank, Brazil SO ALGAE LA English DT Article DE Atlantic; Corallinales; Hapalidiales; psbA; Sporolithales; taxonomy ID GENUS LITHOPHYLLUM LITHOPHYLLOIDEAE; PNEOPHYLLUM-CONICUM; SOUTHWESTERN ATLANTIC; SPP. CORALLINALES; RHODOLITH BEDS; INDIAN-OCEAN; SPOROLITHALES; REASSESSMENT; TITANODERMA; ARCHIPELAGO AB The Abrolhos Continental Shelf (ACS) encompasses the largest and richest coral reefs in the southern Atlantic Ocean. A taxonomic study of non-geniculate coralline algae (NGCA) from the region was undertaken using both morpho-anatomical and molecular data. Specimens of NGCA were collected in 2012 and 2014 from shallow reefs of the ACS. Phylogenetic analysis was performed using dataset of psbA DNA sequences from 16 specimens collected in the ACS and additional GenBank sequences of related NGCA species. Nine common tropical reef-building NGCA species were identified and described: Hydrolithon boergesenii, Lithophyllum kaiseri, Lithophyllum sp., Lithothamnion crispatum, Melyvonnea erubescens, Pneophyllum conicum, Porolithon onkodes, Sporolithon ptychoides, and Titanoderma prototypum. A key for species identification is also provided in this study. Our molecular phylogenetic analyses suggest that Lithophyllum sp. corresponds to a new species. Our study also confirms that Lithophyllum kaiseri is a new record in Brazil. The psbA sequences of Lithophyllum kaiseri and Melyvonnea erubescens matched with type specimens indirectly. The taxonomic identification of the remaining species was supported by morpho-anatomical evidences as DNA sequences of their types or topotypes remain unavailable. C1 [Jesionek, Michel B.; Bahia, Ricardo G.; Amado-Filho, Gilberto M.] Inst Pesquisas Jardim Bot Rio de Janeiro, Diretoria Pesquisa Cient, Rua Pacheco Leao 915, BR-22460030 Rio De Janeiro, RJ, Brazil. [Hernandez-Kanttun, Jazmin J.; Adey, Walter H.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. [Yoneshigue-Valentin, Yocie] Univ Fed Rio de Janeiro, Inst Biol, Dept Bot, Av Carlos Chagas Filho 373, BR-21941902 Rio De Janeiro, Brazil. [Longo, Leila L.] Univ Fed Espirito Santo, Dept Oceanog & Ecol, BR-29075910 Vitoria, ES, Brazil. RP Amado-Filho, GM (reprint author), Inst Pesquisas Jardim Bot Rio de Janeiro, Diretoria Pesquisa Cient, Rua Pacheco Leao 915, BR-22460030 Rio De Janeiro, RJ, Brazil. EM gilbertoamadofilho@gmail.com FU Brazilian Science Support Agency CNPq; Brazilian Science Support Agency FAPERJ; P&D program ANP/BRASOIL; Coordination for the Improvement of Higher Education Personnel (CAPES); CNPq [PDJ 400654/2014-8]; Smithsonian Institution FX Financial support was obtained from the Brazilian Science Support Agencies CNPq and FAPERJ and funds from P&D program ANP/BRASOIL. The first author acknowledges the Coordination for the Improvement of Higher Education Personnel (CAPES) for providing a master's scholarship. We also thank CNPq for providing a postdoctoral fellowship grant to RGB (process PDJ 400654/2014-8) and research fellowship to YYV and GMAF. J.J.H.-K. acknowledges the Smithsonian Institution for providing a postdoctoral fellowship. NR 62 TC 0 Z9 0 U1 2 U2 2 PU KOREAN SOC PHYCOLOGY PI SEOUL PA B1F, TRUST TOWER, 275-7 YANGJAE-DONG, SEOCHO-KU, SEOUL, 137-739, SOUTH KOREA SN 1226-2617 EI 2093-0860 J9 ALGAE-SEOUL JI Algae PD DEC PY 2016 VL 31 IS 4 BP 317 EP 340 DI 10.4490/algae.2016.31.11.16 PG 24 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA EG9YC UT WOS:000391416600003 ER PT J AU Ade, PAR Aghanim, N Aller, HD Aller, MF Arnaud, M Aumont, J Baccigalupi, C Banday, AJ Barreiro, RB Bartolo, N Battaner, E Benabed, K Benoit-Levy, A Bernard, JP Bersanelli, M Bielewicz, P Bonaldi, A Bonavera, L Bond, JR Borrill, J Bouchet, FR Burigana, C Calabrese, E Catalano, A Chiang, HC Christensen, PR Clements, DL Colomb, LPL Couchot, F Crill, BP Curto, A Cuttaia, F Danese, L Davies, RD Davis, RJ de Bernardis, P de Rosa, A de Zotti, G Delabrouille, J Dickinson, C Diego, JM Dole, H Donzelli, S Dore, O Ducout, A Dupac, X Efstathiou, G Elsner, F Eriksen, HK Finelli, F Forni, O Frailis, M Fraisse, AA Franceschi, E Galeotta, S Galli, S Ganga, K Giard, M Giraud-Heraud, Y Gjerlow, E Gonzalez-Nuevo, J Gorski, KM Gruppuso, A Gurwel, MA Hansen, FK Harrison, DL Henrot-Versille, S Hernandez-Monteagudo, C Hildebrandt, SR Hobson, M Hornstrup, A Hovatta, T Hovest, W Huffenberger, KM Hurier, G Jaffe, AH Jaffe, TR Jarvela, E Keihanen, E Keskitalo, R Kisner, TS Kneiss, R Knoche, J Kunz, M Kurki-Suonio, H Lahteenmaki, A Lamarre, JM Lasenby, A Lattanzi, M Lawrence, CR Leonardi, R Levrier, F Liguori, M Lilje, PB Linden-Vornle, M Lopez-Caniego, M Lubin, PM Macias-Perez, JF Maffei, B Maino, D Mandolesi, N Maris, M Martini, PG Martinez-Gonzalez, E Masi, S Matarrese, S Max-Moerbeck, W Meinhold, PR Melchiorri, A Mennella, A Migliaccio, M Millgaliev, M Miville-Deschenes, MA Moneti, A Montier, L Morgante, G Mortlock, D Munshi, D Murphy, JA Nati, F Natoli, P Nieppola, E Noviello, F Novikov, D Novikov, I Pagano, L Pajot, F Paoletti, D Partridge, B Pasian, F Pearson, TJ Perdereau, O Perotto, L Pettorino, V Piacentini, F Piat, M Pierpaoli, E Plaszczynski, S Pointecouteau, E Polenta, G Pratt, GW Ramakrishnan, V Rastorgueva-Foi, EA Readhead, ACS Reinecke, M Remazeilles, M Renault, C Renzi, A Richards, JL Ristorcelli, I Rocha, G Rossetti, M Roudier, G Rubino-Martin, JA Rusholme, B Sandri, M Savelainen, M Savini, G Scott, D Sotnikova, Y Stolyarov, V Sunyaev, R Sutton, D Suur-Uski, AS Sygnet, JF Tammi, J Tauber, JA Terenzi, L Toffolatti, L Tomasi, M Tornikoski, M Tristram, M Tucci, M Turler, M Valenziano, L Valiviita, J Valtaoja, E Van Tent, B Vielva, P Ville, F Wade, LA Wehrle, AE Wehus, IK Yvon, D Zacchei, A Zonca, A AF Ade, P. A. R. Aghanim, N. Aller, H. D. Aller, M. F. Arnaud, M. Aumont, J. Baccigalupi, C. Banday, A. J. Barreiro, R. B. Bartolo, N. Battaner, E. Benabed, K. Benoit-Levy, A. Bernard, J. -P. Bersanelli, M. Bielewicz, P. Bonaldi, A. Bonavera, L. Bond, J. R. Borrill, J. Bouchet, F. R. Burigana, C. Calabrese, E. Catalano, A. Chiang, H. C. Christensen, P. R. Clements, D. L. Colomb, L. P. L. Couchot, F. Crill, B. P. Curto, A. Cuttaia, F. Danese, L. Davies, R. D. Davis, R. J. de Bernardis, P. de Rosa, A. de Zotti, G. Delabrouille, J. Dickinson, C. Diego, J. M. Dole, H. Donzelli, S. Dore, O. Ducout, A. Dupac, X. Efstathiou, G. Elsner, F. Eriksen, H. K. Finelli, F. Forni, O. Frailis, M. Fraisse, A. A. Franceschi, E. Galeotta, S. Galli, S. Ganga, K. Giard, M. Giraud-Heraud, Y. Gjerlow, E. Gonzalez-Nuevo, J. Gorski, K. M. Gruppuso, A. Gurwel, M. A. Hansen, F. K. Harrison, D. L. Henrot-Versille, S. Hernandez-Monteagudo, C. Hildebrandt, S. R. Hobson, M. Hornstrup, A. Hovatta, T. Hovest, W. Huffenberger, K. M. Hurier, G. Jaffe, A. H. Jaffe, T. R. Jarvela, E. Keihanen, E. Keskitalo, R. Kisner, T. S. Kneiss, R. Knoche, J. Kunz, M. Kurki-Suonio, H. Lahteenmaki, A. Lamarre, J. -M. Lasenby, A. Lattanzi, M. Lawrence, C. R. Leonardi, R. Levrier, F. Liguori, M. Lilje, P. B. Linden-Vornle, M. Lopez-Caniego, M. Lubin, P. M. Macias-Perez, J. F. Maffei, B. Maino, D. Mandolesi, N. Maris, M. Martini, P. G. Martinez-Gonzalez, E. Masi, S. Matarrese, S. Max-Moerbeck, W. Meinhold, P. R. Melchiorri, A. Mennella, A. Migliaccio, M. Millgaliev, M. Miville-Deschenes, M. -A. Moneti, A. Montier, L. Morgante, G. Mortlock, D. Munshi, D. Murphy, J. A. Nati, F. Natoli, P. Nieppola, E. Noviello, F. Novikov, D. Novikov, I. Pagano, L. Pajot, F. Paoletti, D. Partridge, B. Pasian, F. Pearson, T. J. Perdereau, O. Perotto, L. Pettorino, V. Piacentini, F. Piat, M. Pierpaoli, E. Plaszczynski, S. Pointecouteau, E. Polenta, G. Pratt, G. W. Ramakrishnan, V. Rastorgueva-Foi, E. A. Readhead, A. C. S. Reinecke, M. Remazeilles, M. Renault, C. Renzi, A. Richards, J. L. Ristorcelli, I. Rocha, G. Rossetti, M. Roudier, G. Rubino-Martin, J. A. Rusholme, B. Sandri, M. Savelainen, M. Savini, G. Scott, D. Sotnikova, Y. Stolyarov, V. Sunyaev, R. Sutton, D. Suur-Uski, A. -S. Sygnet, J. -F. Tammi, J. Tauber, J. A. Terenzi, L. Toffolatti, L. Tomasi, M. Tornikoski, M. Tristram, M. Tucci, M. Turler, M. Valenziano, L. Valiviita, J. Valtaoja, E. Van Tent, B. Vielva, P. Ville, F. Wade, L. A. Wehrle, A. E. Wehus, I. K. Yvon, D. Zacchei, A. Zonca, A. CA Planck Collaboration TI Planck intermediate results XLV. Radio spectra of northern extragalactic radio sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: general; radio continuum: galaxies ID LONG-TERM VARIABILITY; BL LACERTAE OBJECTS; GAMMA-RAY OUTBURST; FLUX-DENSITY SCALE; QUASAR 3C 454.3; MULTIWAVELENGTH OBSERVATIONS; 2010 NOVEMBER; GASP-WEBT; BLAZAR; JET AB Continuum spectra covering centimetre to submillimetre wavelengths are presented for a northern sample of 104 extragalactic radio sources, mainly active galactic nuclei, based on four-epoch Planck data. The nine Planck frequencies, from 30 to 857 GHz, are complemented by a set of simultaneous ground-based radio observations between 1.1 and 37 GHz. The single-survey Planck data confirm that the flattest high-frequency radio spectral indices are close to zero, indicating that the original accelerated electron energy spectrum is much harder than commonly thought, with power-law index around 1.5 instead of the canonical 2.5. The radio spectra peak at high frequencies and exhibit a variety of shapes. For a small set of low-z sources, we find a spectral upturn at high frequencies, indicating the presence of intrinsic cold dust. Variability can generally be approximated by achromatic variations, while sources with clear signatures of evolving shocks appear to be limited to the strongest outbursts. C1 [Delabrouille, J.; Ganga, K.; Giraud-Heraud, Y.; Piat, M.; Remazeilles, M.; Roudier, G.] Univ Paris Diderot, APC, CNRS IN2P3, CEA lrfu,Observ Paris,Sorbonne Paris Cite, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France. [Jarvela, E.; Lahteenmaki, A.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Jarvela, E.; Lahteenmaki, A.] Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland. [Hovatta, T.; Nieppola, E.; Ramakrishnan, V.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, POB 13000, Aalto 00076, Finland. [Kunz, M.] African Inst Math Sci, 6-8 Melrose Rd, Cape Town, South Africa. [Natoli, P.; Polenta, G.] Agenzia Spaziale Italiana Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. [Curto, A.; Hobson, M.; Lasenby, A.; Stolyarov, V.] Univ Cambridge, Cavendish Lab, Astrophys Grp, J J Thomson Ave, Cambridge CB3 OHE, England. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, West Ville Campus,Private Bag X54001, ZA-4000 Durban, South Africa. [Kneiss, R.] ALMA Santiago Cent Offices, Atacama Large Millimeter Submillimeter Array, Alonso Cordova 3107, Santiago 7630355, Chile. [Bond, J. R.; Martini, P. G.; Miville-Deschenes, M. -A.] Univ Toronto, CITA, 60 St George St, Toronto, ON M5S 3H8, Canada. [Banday, A. J.; Bernard, J. -P.; Bielewicz, P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] CNRS, TRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Hovatta, T.; Max-Moerbeck, W.; Readhead, A. C. S.; Richards, J. L.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Crill, B. P.; Dore, O.; Hildebrandt, S. R.; Pearson, T. J.; Rocha, G.] CALTECH, Pasadena, CA 91125 USA. [Hernandez-Monteagudo, C.] CEFCA, Plaza San Juan 1,Planta 2, Teruel 44001, Spain. [Borrill, J.; Keskitalo, R.] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA. [Yvon, D.] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France. [Hornstrup, A.; Linden-Vornle, M.] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark. [Kunz, M.; Tucci, M.] Univ Geneva, Dept Phys Theor, 24 Quai E Ansermet, CH-12114 Geneva, Switzerland. [Rubino-Martin, J. A.] ULL, Dept Astrofis, San Cristobal la Laguna 38206, Spain. [Gonzalez-Nuevo, J.; Toffolatti, L.] Univ Oviedo, Dept Fis, Avda Calvo Sotelo S-N, Oviedo, Spain. [Scott, D.] Univ British Columbia, Dept Phys Astron, 6224 Agr Rd, Vancouver, BC, Canada. [Colomb, L. P. L.; Pierpaoli, E.] Univ Southern California, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA. [Benoit-Levy, A.; Elsner, F.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Huffenberger, K. M.] Florida State Univ, Dept Phys, Keen Phys Bldg,77 Chieftan Way, Tallahassee, FL USA. [Keihanen, E.; Kurki-Suonio, H.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, Helsinki 00560, Finland. [Chiang, H. C.; Fraisse, A. A.; Nati, F.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Richards, J. L.] Purdue Univ, Dept Phys, 525 Northwestern Ave, W Lafayette, IN 47907 USA. [Lubin, P. M.; Meinhold, P. R.; Zonca, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bartolo, N.; Liguori, M.; Matarrese, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, Via Marzolo 8, I-35131 Padua, Italy. [Burigana, C.; Lattanzi, M.; Mandolesi, N.; Natoli, P.] Univ Ferrara, Dipartimento Fis & Sci Terra, Via Saragat 1, I-44122 Ferrara, Italy. [de Bernardis, P.; Masi, S.; Melchiorri, A.; Pagano, L.; Piacentini, F.] Univ Roma La Sapienza, Dipartimento Fis, P Moro 2, I-00133 Rome, Italy. [Bersanelli, M.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] Univ Milan, Dipartimento Fis, Via Celoria 16, Milan, Italy. [Renzi, A.] Univ Roma Tor Vergata, Dipartimento Matemat, Via Ric Scientifica 1, I-00133 Rome, Italy. [Christensen, P. R.] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, Copenhagen, Denmark. [Kneiss, R.] ESO Vitacura, Alonso Cordova 3107, Santiago, Chile. [Dupac, X.; Leonardi, R.; Lopez-Caniego, M.] European Space Agcy, ESAC, Planck Sci Off, Camino Bajo Castillo S-N, Madrid 28691, Spain. [Tauber, J. A.] European Space Agcy, ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Terenzi, L.] Univ Campus, Facolta Ingn, Fac Ingn, Via Isimbardi 10, I-22060 Novedrate, Italy. [Nieppola, E.] Univ Turku, Finnish Ctr Astron ESO, FINCA, Vaisalantie 20, Piikkio 21500, Finland. [Matarrese, S.] Ist Nazl Fis Nucl, Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy. [Pettorino, V.] HGSFP, Philosophenweg 16, D-69120 Heidelberg, Germany. [Pettorino, V.] Heidelberg Univ, Dept Phys Theor, Philosophenweg 16, D-69120 Heidelberg, Germany. [Gurwel, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Partridge, B.] Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA. [Kurki-Suonio, H.; Lahteenmaki, A.; Savelainen, M.; Suur-Uski, A. -S.; Valiviita, J.] Univ Helsinki, Helsinki Inst Phys, Gustaf Hallstromin Katu 2, Helsinki 00560, Finland. [de Zotti, G.] INAF, Osservatorio Astronomico Padova, Vicolo dellOsservatorio 5, Padua, Italy. [Polenta, G.] Ist Nazl Fis Nucl, Osservatorio Astron Roma, Via Frascati 33, Monte Porzio Catone, Italy. [Frailis, M.; Galeotta, S.; Maris, M.; Pasian, F.; Zacchei, A.] INAF, Osservatorio Astron Trieste, Via G B Tiepolo 11, Trieste, Italy. [Burigana, C.; Cuttaia, F.; de Rosa, A.; Finelli, F.; Franceschi, E.; Gruppuso, A.; Mandolesi, N.; Morgante, G.; Natoli, P.; Paoletti, D.; Sandri, M.; Terenzi, L.; Toffolatti, L.; Valenziano, L.; Ville, F.] INAF, IASF Bologna, Via Gobetti 101, Bologna, Italy. [Bersanelli, M.; Donzelli, S.; Maino, D.; Mennella, A.; Rossetti, M.; Tomasi, M.] INAF, IASF Milano, Via Bassini 15, Milan, Italy. [Burigana, C.; Finelli, F.; Paoletti, D.] INFN, Sez Bologna, Via Irnerio 46, I-40126 Bologna, Italy. [Melchiorri, A.; Pagano, L.] Univ Roma Sapienza, INFN, Sez Roma 1, Piazzale Aldo Moro 2, I-00185 Rome, Italy. [Renzi, A.] Univ Roma Tor Vergata, INFN, Sez Roma 2, Via Ric Scientifica 1, I-00185 Rome, Italy. [Turler, M.] Univ Geneva, Dept Astron, ISDC, Ch dEcogia 16, CH-1290 Versoix, Switzerland. [Clements, D. L.; Ducout, A.; Jaffe, A. H.; Mortlock, D.] Imperial Coll London, Blackett Lab, Astrophys Grp, Prince Consort Rd, London SW7 2AZ, England. [Pearson, T. J.; Rusholme, B.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Dole, H.] Inst Univ France, 103 bd St Michel, F-75005 Paris, France. [Aghanim, N.; Aumont, J.; Dole, H.; Hurier, G.; Kunz, M.; Miville-Deschenes, M. -A.; Pajot, F.; Remazeilles, M.] Univ Paris Sud 11, Inst Astrophys Spatiale, CNRS UMR8617, Batiment 121, F-91405 Orsay, France. [Benabed, K.; Benoit-Levy, A.; Bouchet, F. R.; Ducout, A.; Elsner, F.; Moneti, A.; Sygnet, J. -F.] CNRS, Inst Astrophys Paris, UMR7095, 98bis Blv Arago, F-75014 Paris, France. [Efstathiou, G.; Harrison, D. L.; Migliaccio, M.; Sutton, D.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Eriksen, H. K.; Gjerlow, E.; Hansen, F. K.; Lilje, P. B.] Univ Oslo, Inst Theoret Astrophys, N-0371 Oslo, Norway. [Rubino-Martin, J. A.] Inst Astrofis Canarias, C Via Lactea S-N, San Cristobal la Laguna, Spain. [Barreiro, R. B.; Bonavera, L.; Curto, A.; Diego, J. M.; Gonzalez-Nuevo, J.; Lopez-Caniego, M.; Martinez-Gonzalez, E.; Toffolatti, L.; Vielva, P.] Univ Cantabria, CSIC, Inst Fis Cantabria, Avda Los Castros S-N, Santander 39005, Spain. [Bartolo, N.; Liguori, M.; Matarrese, S.] Ist Nazl Fis Nucl, Sez Padova, Via Mar zolo 8, I-35131 Padua, Italy. [Benoit-Levy, A.; Bonaldi, A.; Colomb, L. P. L.; Crill, B. P.; Dore, O.; Gorski, K. M.; Hildebrandt, S. R.; Lawrence, C. R.; Rocha, G.; Roudier, G.; Wade, L. A.; Wehus, I. K.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA USA. [Benoit-Levy, A.; Bonaldi, A.; Davies, R. D.; Davis, R. J.; Dickinson, C.; Maffei, B.; Noviello, F.; Remazeilles, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Galli, S.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Curto, A.; Harrison, D. L.; Lasenby, A.; Migliaccio, M.; Sutton, D.] Kavli Inst Cosmol Cambridge, Madingley Rd, Cambridge CB3 0HA, England. [Millgaliev, M.; Stolyarov, V.] Kazan Fed Univ, 18 Kremlyovskaya St, Kazan 420008, Russia. [Couchot, F.; Henrot-Versille, S.; Perdereau, O.; Plaszczynski, S.; Tristram, M.] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France. [Catalano, A.; Lamarre, J. -M.; Levrier, F.; Roudier, G.] CNRS, LERMA, Observ Paris, 61 Ave Observ, F-75000 Paris, France. [Arnaud, M.; Pratt, G. W.] Univ Paris Dide, CEA Saclay, CEA DSM CNRS, IRFU Serv Astrophys,Lab AIM, Bat 709, F-91191 Gif Sur Yvette, France. [Catalano, A.; Macias-Perez, J. F.; Perotto, L.; Renault, C.] Univ Grenoble Alpes, CNRS, IN2P3, Lab Phys Subatom & Cosmol, 53 Rue Martyrs, F-38026 Grenoble, France. [Van Tent, B.] Univ Paris Sud 11, Lab Phys Theor, Batiment 210, F-91405 Orsay, France. [Van Tent, B.] CNRS, Batiment 210, F-91405 Orsay, France. [Kisner, T. S.] Lawrence Berkeley Natl Lab, Berkeley, CA USA. [Novikov, D.; Novikov, I.] Russian Acad Sci, Lebedev Phys Inst, Astro Space Ctr, 84-32 Profsoyuznaya St,GSP 7, Moscow 117997, Russia. [Hernandez-Monteagudo, C.; Hovest, W.; Knoche, J.; Reinecke, M.; Sunyaev, R.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Max-Moerbeck, W.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA. [Murphy, J. A.] Natl Univ Ireland, Dept Expt Phys, Maynooth, Kildare, Ireland. [Bielewicz, P.] Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. [Christensen, P. R.; Novikov, I.] Niels Bohr Inst, Blegdamsvej 17, Copenhagen, Denmark. [Savini, G.] UCL, Optic Sci Lab, Gower St, London, England. [Baccigalupi, C.; Bielewicz, P.; Danese, L.; de Zotti, G.] SISSA, Astrophys Sect, Via Bonomea 265, I-34136 Trieste, Italy. [Rastorgueva-Foi, E. A.] Univ Tasmania, Sch Math & Phys, Private Bag 37, Hobart, Tas, Australia. [Ade, P. A. R.; Munshi, D.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Bouchet, F. R.] Sorbonne Univ UPMC, Inst Astrophys Paris, UMR7095, 98bis Blvd Arago, F-75014 Paris, France. [Sunyaev, R.] Russian Acad Sci, Space Res Inst IKI, Profsoyuznaya Str 84-32, Moscow 117997, Russia. [Wehrle, A. E.] Space Sci Inst, 4750 Walnut St,Suite 205, Suite, CO 205 USA. [Borrill, J.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Millgaliev, M.; Sotnikova, Y.; Stolyarov, V.] Russian Acad Sci, Special Astrophys Observ, Karachai 369167, Russia. [Calabrese, E.] Univ Oxford, Dept Astrophys, Keble Rd, Oxford OX1 3RH, England. [Valtaoja, E.] Turku Univ, Dept Phys & Astron, Tuorla Observ, Vaisalantie 20, Piikkio 21500, Finland. [Benabed, K.; Benoit-Levy, A.; Elsner, F.] UPMC, Univ Paris 06, UMR7095, 98bis Blvd Arago, F-75014 Paris, France. [Banday, A. J.; Benoit-Levy, A.; Bernard, J. -P.; Forni, O.; Giard, M.; Jaffe, T. R.; Montier, L.; Pointecouteau, E.; Ristorcelli, I.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Battaner, E.] Univ Granada, Fac Ciencias, Dept Fis Teorica & Cosmos, Granada 18071, Spain. [Battaner, E.] Univ Granada, Inst Carlos Fis Teor & Computac, Granada 18071, Spain. [Gorski, K. M.] Univ Warsaw Observ, Aleje Ujazdowskie 4, PL-00478 Warsaw, Poland. RP Lahteenmaki, A (reprint author), Dept Radio Sci & Engn, POB 13000, Aalto 00076, Finland.; Lahteenmaki, A (reprint author), Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA. EM anne.lahteenmaki@aalto.fi RI Lahteenmaki, Anne/L-5987-2013; Stolyarov, Vladislav/C-5656-2017; Ramakrishnan, Venkatessh/C-8628-2017; Barreiro, Rita Belen/N-5442-2014; bonavera, laura/E-9368-2017; Gonzalez-Nuevo, Joaquin/I-3562-2014; OI Toffolatti, Luigi/0000-0003-2645-7386; Lilje, Per/0000-0003-4324-7794; Savini, Giorgio/0000-0003-4449-9416; Pierpaoli, Elena/0000-0002-7957-8993; Stolyarov, Vladislav/0000-0001-8151-828X; Ramakrishnan, Venkatessh/0000-0002-9248-086X; Barreiro, Rita Belen/0000-0002-6139-4272; bonavera, laura/0000-0001-8039-3876; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Valiviita, Jussi/0000-0001-6225-3693; Kurki-Suonio, Hannu/0000-0002-4618-3063; Villa, Fabrizio/0000-0003-1798-861X; TERENZI, LUCA/0000-0001-9915-6379 FU ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); NASA (USA); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MINECO (Spain); JA (Spain); RES (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC (EU); PRACE (EU); Academy of Finland [212656, 210338, 121148]; Smithsonian Institution; Academia Sinica; NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911]; NSF; NASA; University of Michigan; Russian Government Programme of Competitive Growth of Kazan Federal University FX The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A description of the Planck Collaboration and a list of its members, indicating which technical or scientific activities they have been involved in, can be found at http://www.cosmos.esa.int/web/planck/planck-collaboration. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (Nos. 212656, 210338, 121148, and others). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The OVRO 40-m monitoring programme is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. UMRAO has been supported by a series of grants from the NSF and NASA, and by the University of Michigan. We also acknowledge support through the Russian Government Programme of Competitive Growth of Kazan Federal University. NR 60 TC 0 Z9 0 U1 2 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2016 VL 596 AR A106 DI 10.1051/0004-6361/201527780 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG1MX UT WOS:000390797900011 ER PT J AU Kospal, A Abraham, P Acosta-Pulido, JA Dunham, MM Garcia-Alvarez, D Hogerheijde, MR Kun, M Moor, A Farkas, A Hajdu, G Hodosan, G Kovacs, T Kriskovics, L Marton, G Molnar, L Pal, A Sarneczky, K Sodor, A Szakats, R Szalai, T Szegedi-Elek, E Szing, A Toth, I Vida, K Vinko, J AF Kospal, A. Abraham, P. Acosta-Pulido, J. A. Dunham, M. M. Garcia-Alvarez, D. Hogerheijde, M. R. Kun, M. Moor, A. Farkas, A. Hajdu, G. Hodosan, G. Kovacs, T. Kriskovics, L. Marton, G. Molnar, L. Pal, A. Sarneczky, K. Sodor, A. Szakats, R. Szalai, T. Szegedi-Elek, E. Szing, A. Toth, I. Vida, K. Vinko, J. TI Multiwavelength study of the low-luminosity outbursting young star HBC 722 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; circumstellar matter; infrared: stars; stars: individual: HBC 722 ID FU ORIONIS CANDIDATE; PROTOSTELLAR DISK MODELS; ENVIRONMENT; VARIABILITY; EVOLUTION; HERSCHEL AB Context. HBC 722 (V2493 Cyg) is a young eruptive star in outburst since 2010. Spectroscopic evidence suggests that the source is an FU Orionis-type object, with an atypically low outburst luminosity. Aims. Because it was well characterized in the pre-outburst phase, HBC 722 is one of the few FUors from which we can learn about the physical changes and processes associated with the eruption, including the role of the circumstellar environment. Methods. We monitored the source in the BVRIJHK(S) bands from the ground and at 3.6 and 4.5 mu m from space with the Spitzer Space Telescope. We analyzed the light curves and studied the evolving spectral energy distribution by fitting a series of steady accretion disk models at many epochs covering the outburst. We also analyzed the spectral properties of the source based on our new optical and infrared spectra, comparing our line inventory with those published in the literature for other epochs. We also mapped HBC 722 and its surroundings at millimeter wavelengths. Results. From the light-curve analysis we conclude that the first peak of the outburst in 2010 September was mainly due to an abrupt increase in the accretion rate in the innermost part of the system. This was followed after a few months by a long-term process, when the brightening of the source was mainly due to a gradual increase in the accretion rate and the emitting area. Our new observations show that the source is currently in a constant plateau phase. We found that the optical spectrum was similar in the first peak and following periods, but around the peak the continuum was bluer and the H alpha profile changed significantly between 2012 and 2013. The source was not detected in the millimeter continuum, but we discovered a flattened molecular gas structure with a diameter of 1700 au and mass of 0.3 M-circle dot centered on HBC 722. Conclusions. While the first brightness peak might be interpreted as a rapid fall of piled-up material from the inner disk onto the star, the later monotonic flux rise suggests the outward expansion of a hot component according to a previously described theory. Our study of HBC 722 demonstrates that accretion-related outbursts can occur in young stellar objects even with very low-mass disks in the late Class II phase. C1 [Kospal, A.; Abraham, P.; Kun, M.; Moor, A.; Farkas, A.; Kovacs, T.; Kriskovics, L.; Marton, G.; Molnar, L.; Pal, A.; Sarneczky, K.; Sodor, A.; Szakats, R.; Szegedi-Elek, E.; Toth, I.; Vida, K.; Vinko, J.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary. [Acosta-Pulido, J. A.; Garcia-Alvarez, D.] Inst Astrofis Canarias, Ave Via Lactea, Tenerife 38205, Spain. [Acosta-Pulido, J. A.; Garcia-Alvarez, D.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Dunham, M. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. [Garcia-Alvarez, D.] Grantecan SA, Ctr Astrofis La Palma, Brena Baja 38712, La Palma, Spain. [Hogerheijde, M. R.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Hajdu, G.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna, Santiago 4860, Chile. [Hajdu, G.] Inst Milenio Astrofis, Santiago, Chile. [Hodosan, G.] Univ St Andrews, Sch Phys & Astron, St Andrews, Fife, Scotland. [Pal, A.] Eotvos Lorand Univ, Dept Astron, Pazmany Peter Setany 1-A, H-1117 Budapest, Hungary. [Szakats, R.; Vinko, J.] Univ Szeged, Dept Opt & Quantum Elect, Dom Ter 9, H-6720 Szeged, Hungary. [Szing, A.] Univ Szeged, Baja Observ, KT 776, H-6500 Baja, Hungary. RP Kospal, A (reprint author), Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary. EM kospal@konkoly.hu FU Momentum grant of the MTA CSFK Lendulet Disk Research Group; Lendulet grant of the Hungarian Academy of Sciences [LP2012-31]; Hungarian Research Fund OTKA grant [K101393]; Bolyai Research Fellowship of the Hungarian Academy of Sciences; Ministry for the Economy, Development, and Tourism's Programa Iniciativa Milenio [IC 120009]; Proyecto Basal [PFB-06/2007]; CONICYT-PCHA/Doctorado Nacional grant [2014-63140099]; IRAM Plateau de Bure Interferometer [VA6C]; IRAM 30 m Telescope [260-11]; INSU/CNRS (France); MPG (Germany); IGN (Spain); European Community [RadioNet R113CT 2003 5058187] FX We thank the referee for the comments that greatly improved the paper and Z. Zhu for useful discussions on the accretion disk fitting. This work was supported by the Momentum grant of the MTA CSFK Lendulet Disk Research Group, the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences, and the Hungarian Research Fund OTKA grant K101393. A.M. acknowledges support from the Bolyai Research Fellowship of the Hungarian Academy of Sciences. G.H. acknowledges support by the Ministry for the Economy, Development, and Tourism's Programa Iniciativa Milenio through grant IC 120009; by Proyecto Basal PFB-06/2007; and by CONICYT-PCHA/Doctorado Nacional grant 2014-63140099. The William Herschel Telescope and its service program are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part on observations made with the Telescopio Carlos Sanchez operated on the island of Tenerife by the Instituto de Astrofisica de Canarias in the Observatorio del Teide. The authors wish to thank the telescope manager A. Oscoz, the support astronomers and telescope operators for their help during the observations, as well as the service mode observers. Based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. This work is partly based on observations carried out under project number VA6C with the IRAM Plateau de Bure Interferometer and under project number 260-11 with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). This work has benefited from research funding from the European Community's sixth Framework Programme under RadioNet R113CT 2003 5058187. NR 40 TC 1 Z9 1 U1 3 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2016 VL 596 AR A52 DI 10.1051/0004-6361/201528061 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG1MX UT WOS:000390797900024 ER PT J AU Lee, MY Madden, SC Lebouteiller, V Gusdorf, A Godard, B Wu, R Galametz, M Cormier, D Le Petit, F Roueff, E Bron, E Carlson, L Chevance, M Fukui, Y Galliano, F Hony, S Hughes, A Indebetouw, R Israel, FP Kawamura, A Le Bourlot, J Lesaffre, P Meixner, M Muller, E Nayak, O Onishi, T Roman-Duval, J Sewilo, M AF Lee, M. -Y. Madden, S. C. Lebouteiller, V. Gusdorf, A. Godard, B. Wu, R. Galametz, M. Cormier, D. Le Petit, F. Roueff, E. Bron, E. Carlson, L. Chevance, M. Fukui, Y. Galliano, F. Hony, S. Hughes, A. Indebetouw, R. Israel, F. P. Kawamura, A. Le Bourlot, J. Lesaffre, P. Meixner, M. Muller, E. Nayak, O. Onishi, T. Roman-Duval, J. Sewilo, M. TI Radiative and mechanical feedback into the molecular gas in the Large Magellanic Cloud I. N159W SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; Magellanic Clouds; galaxies: ISM; infrared: ISM ID FOURIER-TRANSFORM SPECTROMETER; HERSCHEL-SPIRE INSTRUMENT; LOW-VELOCITY SHOCKS; J CO OBSERVATIONS; STAR-FORMATION; PHOTODISSOCIATION REGIONS; INTERSTELLAR-MEDIUM; LINE EMISSION; MAGNETOHYDRODYNAMIC SHOCKS; PHOTOELECTRIC-EMISSION AB We present Herschel SPIRE Fourier Transform Spectrometer (FTS) observations of N159W, an active star-forming region in the Large Magellanic Cloud (LMC). In our observations, a number of far-infrared cooling lines, including carbon monoxide (CO) J = 4 -> 3 to J = 12 -> 11, [CI] 609 mu m and 370 mu m, and [NII] 205 mu m, are clearly detected. With an aim of investigating the physical conditions and excitation processes of molecular gas, we first construct CO spectral line energy distributions (SLEDs) on similar to 10 pc scales by combining the FTS CO transitions with ground-based low-J CO data and analyze the observed CO SLEDs using non-LTE (local thermodynamic equilibrium) radiative transfer models. We find that the CO-traced molecular gas in N159W is warm (kinetic temperature of 153-754 K) and moderately dense (H-2 number density of (1.1-4.5) x 103 cm 3). To assess the impact of the energetic processes in the interstellar medium on the physical conditions of the CO-emitting gas, we then compare the observed CO line intensities with the models of photodissociation regions (PDRs) and shocks. We first constrain the properties of PDRs by modeling Herschel observations of [OI] 145 mu m, [CII] 158 mu m, and [CI] 370 mu m fine-structure lines and find that the constrained PDR components emit very weak CO emission. X-rays and cosmic-rays are also found to provide a negligible contribution to the CO emission, essentially ruling out ionizing sources (ultraviolet photons, X-rays, and cosmic-rays) as the dominant heating source for CO in N159W. On the other hand, mechanical heating by low-velocity C-type shocks with similar to 10 km s(-1) appears sufficient enough to reproduce the observed warm CO. C1 [Lee, M. -Y.; Madden, S. C.; Lebouteiller, V.; Chevance, M.; Galliano, F.] CEA, IRFU, Serv Astrophys, Lab AIM, Bat 709, F-91191 Gif Sur Yvette, France. [Gusdorf, A.; Lesaffre, P.] PSL Res Univ, Ecole Normale Super, Observ Paris, LERMA,CNRS,UMR 8112, F-75014 Paris, France. [Gusdorf, A.; Le Bourlot, J.] UPMC Univ Paris 6, Sorbonne Univ, UMR 8112, LERMA, F-75005 Paris, France. [Godard, B.; Le Petit, F.; Roueff, E.; Bron, E.] PSL Res Univ, Observ Paris, LERMA, CNRS,UMR 8112, F-92190 Meudon, France. [Wu, R.] Univ Tokyo, JSPS, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Galametz, M.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Cormier, D.; Hony, S.] Heidelberg Univ, Zenturm Astron, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. [Bron, E.] CSIC, ICMM, Madrid 28049, Spain. [Carlson, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fukui, Y.] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Hughes, A.] CNRS, IRAP, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Indebetouw, R.] Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. [Indebetouw, R.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Israel, F. P.] Leiden Univ, Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands. [Kawamura, A.; Muller, E.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Meixner, M.; Roman-Duval, J.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Nayak, O.] Johns Hopkins Univ, Dept Phys & Astron, 366 Bloomberg Ctr,3400 N Charles St, Baltimore, MD 21218 USA. [Onishi, T.] Osaka Prefecture Univ, Grad Sch Sci, Dept Phys Sci, 1-1 Gakuen Cho, Sakai, Osaka 5998531, Japan. [Sewilo, M.] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA. RP Lee, MY (reprint author), CEA, IRFU, Serv Astrophys, Lab AIM, Bat 709, F-91191 Gif Sur Yvette, France. EM min-young.lee@cea.fr OI Lee, Min-Young/0000-0002-9888-0784 FU DIM ACAV of the Region Ile de France; SYMPATICO grant of the French Agence Nationale de la Recherche [ANR-11-BS56-0023]; CNRS PCMI program; DFG [HO 5475/2-1]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain); CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX We would like to thank the anonymous referee for the constructive comments that improved this work. We also thank Julia Kamenetzky, Edward Polehampton, Eric Pellegrini, and Naseem Rangwala for helpful discussions on FTS data reduction and science. M.-Y.L. acknowledges support from the DIM ACAV of the Region Ile de France, the SYMPATICO grant (ANR-11-BS56-0023) of the French Agence Nationale de la Recherche, and the CNRS PCMI program. S.H. acknowledges financial support from DFG programme HO 5475/2-1. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). NR 124 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2016 VL 596 AR A85 DI 10.1051/0004-6361/201628098 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG1MX UT WOS:000390797900025 ER PT J AU Roy, R Sollerman, J Silverman, JM Pastorello, A Fransson, C Drake, A Taddia, F Fremling, C Kankare, E Kumar, B Cappellaro, E Bose, S Benetti, S Filippenko, AV Valenti, S Nyholm, A Ergon, M Sutaria, F Kumar, B Pandey, SB Nicholl, M Garcia-Alvarez, D Tomasella, L Karamehmetoglu, E Migotto, K AF Roy, R. Sollerman, J. Silverman, J. M. Pastorello, A. Fransson, C. Drake, A. Taddia, F. Fremling, C. Kankare, E. Kumar, B. Cappellaro, E. Bose, S. Benetti, S. Filippenko, A. V. Valenti, S. Nyholm, A. Ergon, M. Sutaria, F. Kumar, B. Pandey, S. B. Nicholl, M. Garcia-Alvarez, D. Tomasella, L. Karamehmetoglu, E. Migotto, K. TI SN 2012aa: A transient between Type Ibc core-collapse and superluminous supernovae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE supernovae: general; supernovae: individual: SN 2012aa ID RICH CIRCUMSTELLAR MEDIUM; GAMMA-RAY BURST; EMISSION-LINE GALAXIES; DIGITAL SKY SURVEY; LIGHT CURVES; HOST GALAXIES; IC SUPERNOVAE; LUMINOUS SUPERNOVAE; IB/C SUPERNOVAE; SHOCK BREAKOUT AB Context. Research on supernovae (SNe) over the past decade has confirmed that there is a distinct class of events which are much more luminous (by similar to 2 mag) than canonical core-collapse SNe (CCSNe). These events with visual peak magnitudes less than or similar to-21 are called superluminous SNe (SLSNe). The mechanism that powers the light curves of SLSNe is still not well understood. The proposed scenarios are circumstellar interaction, the emergence of a magnetar after core collapse, or disruption of a massive star through pair production. Aims. There are a few intermediate events which have luminosities between these two classes. They are important for constraining the nature of the progenitors of these two different populations and their environments and powering mechanisms. Here we study one such object, SN 2012aa. Methods. We observed and analysed the evolution of the luminous Type Ic SN 2012aa. The event was discovered by the Lick Observatory Supernova Search in an anonymous galaxy (z approximate to 0.08). The optical photometric and spectroscopic follow-up observations were conducted over a time span of about 120 days. Results. With an absolute V-band peak of similar to-20 mag, the SN is an intermediate-luminosity transient between regular SNe Ibc and SLSNe. SN 2012aa also exhibits an unusual secondary bump after the maximum in its light curve. For SN 2012aa, we interpret this as a manifestation of SN-shock interaction with the circumstellar medium (CSM). If we assume a Ni-56-powered ejecta, the quasi-bolometric light curve requires roughly 1.3 M-circle dot of Ni-56 and an ejected mass of similar to 14 M-circle dot. This also implies a high kinetic energy of the explosion, similar to 5.4 x 10(51) erg. On the other hand, the unusually broad light curve along with the secondary peak indicate the possibility of interaction with CSM. The third alternative is the presence of a central engine releasing spin energy that eventually powers the light curve over a long time. The host of SN 2012aa is a star-forming Sa/Sb/Sbc galaxy. Conclusions. Although the spectral properties of SN 2012aa and its velocity evolution are comparable to those of normal SNe Ibc, its broad light curve along with a large peak luminosity distinguish it from canonical CCSNe, suggesting that the event is an intermediate-luminosity transient between CCSNe and SLSNe at least in terms of peak luminosity. In comparison to other SNe, we argue that SN 2012aa belongs to a subclass where CSM interaction plays a significant role in powering the SN, at least during the initial stages of evolution. C1 [Roy, R.; Sollerman, J.; Fransson, C.; Taddia, F.; Fremling, C.; Nyholm, A.; Ergon, M.; Karamehmetoglu, E.; Migotto, K.] Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, S-10691 Stockholm, Sweden. [Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Pastorello, A.; Cappellaro, E.; Benetti, S.; Tomasella, L.] INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Drake, A.] CALTECH, 1200 E Calif Blvd, Pasadena, CA 91225 USA. [Kankare, E.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Kumar, B.; Sutaria, F.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Bose, S.; Kumar, B.; Pandey, S. B.] Aryabhatta Res Inst Observat Sci ARIES, Manora Peak 263129, Nainital, India. [Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Valenti, S.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Nicholl, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Garcia-Alvarez, D.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Garcia-Alvarez, D.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Garcia-Alvarez, D.] Grantecan CALP, Brena Baja 38712, La Palma, Spain. RP Roy, R (reprint author), Stockholm Univ, Dept Astron, Oskar Klein Ctr, AlbaNova, S-10691 Stockholm, Sweden. EM rupak.roy@astro.su.se FU NTT Telescope at the La Silla and Paranal Observatories within European supernova in ESO-NTT large programme [184.D-1140]; W. M. Keck Foundation; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; PRIN-INAF under project "Transient Universe: unveiling new types of stellar explosions with PESSTO"; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916]; NASA FX We thank all of the observers at ST who provided their valuable time and support for observations of SN 2012aa. We are grateful to the staff of the CT, IGO, TNG, NTT, Lick, and Keck-I telescopes for their kind cooperation when conducting the observations. This work is partially based on observations made with the NOT, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias; on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias; and on observations made with NTT Telescope at the La Silla and Paranal Observatories within the European supernova collaboration involved in ESO-NTT large programme 184.D-1140 led by Stefano Benetti. Some of the data presented here were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank G. Leloudas for a valuable discussion of a draft of this paper. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. A.P., E.C., S.B., and L.T. are partially supported by the PRIN-INAF 2014 under the project "Transient Universe: unveiling new types of stellar explosions with PESSTO". A.V.F.'s research is supported by the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. Research at Lick Observatory is partially supported by a generous gift from Google. This work has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We also used NASA's Astrophysics Data System. NR 129 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2016 VL 596 AR A67 DI 10.1051/0004-6361/201527947 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG1MX UT WOS:000390797900018 ER PT J AU Salabert, D Garcia, RA Beck, PG Egeland, R Palle, PL Mathur, S Metcalfe, TS do Nascimento, JD Ceillier, T Andersen, MF Hage, AT AF Salabert, D. Garcia, R. A. Beck, P. G. Egeland, R. Palle, P. L. Mathur, S. Metcalfe, T. S. do Nascimento, J. -D., Jr. Ceillier, T. Andersen, M. F. Trivino Hage, A. TI Photospheric and chromospheric magnetic activity of seismic solar analogs Observational inputs on the solar-stellar connection from Kepler and Hermes SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: solar-type; stars: activity; stars: evolution; methods: data analysis; methods: observational ID MAIN-SEQUENCE STARS; SUN-LIKE STARS; CA-II H; ACTIVITY CYCLE PERIOD; EMISSION-LINE FLUXES; ROTATION PERIODS; PHOTOMETRIC VARIABILITY; ACTIVITY INDICATORS; FREQUENCY-SHIFTS; TIME VARIATIONS AB We identify a set of 18 solar analogs among the seismic sample of solar-like stars observed by the Kepler satellite rotating between 10 and 40 days. This set is constructed using the asteroseismic stellar properties derived using either the global oscillation properties or the individual acoustic frequencies. We measure the magnetic activity properties of these stars using observations collected by the photometric Kepler satellite and by the ground-based, high-resolution Hermes spectrograph mounted on the Mercator telescope. The photospheric (S-ph) and chromospheric (S index) magnetic activity levels of these seismic solar analogs are estimated and compared in relation to the solar activity. We show that the activity of the Sun is comparable to the activity of the seismic solar analogs, within the maximum-to-minimum temporal variations of the 11-yr solar activity cycle 23. In agreement with previous studies, the youngest stars and fastest rotators in our sample are actually the most active. The activity of stars older than the Sun seems to not evolve much with age. Furthermore, the comparison of the photospheric, S (ph), with the well-established chromospheric, S index, indicates that the S (ph) index can be used to provide a suitable magnetic activity proxy which can be easily estimated for a large number of stars from space photometric observations. C1 [Salabert, D.; Garcia, R. A.; Beck, P. G.; Ceillier, T.] Univ Paris 7 Diderot, IRFU SAp, Ctr Saclay, Lab AIM,CEA DRF CNRS, F-91191 Gif Sur Yvette, France. [Egeland, R.] Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. [Egeland, R.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Palle, P. L.; Trivino Hage, A.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Palle, P. L.; Trivino Hage, A.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Mathur, S.; Metcalfe, T. S.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Metcalfe, T. S.] Natl Solar Observ, 3665 Discovery Dr, Boulder, CO 80303 USA. [do Nascimento, J. -D., Jr.] Univ Fed Rio Grande do Norte, UFRN, Dept Fis, DFTE, CP1641, BR-59072970 Natal, RN, Brazil. [do Nascimento, J. -D., Jr.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Andersen, M. F.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. RP Salabert, D (reprint author), Univ Paris 7 Diderot, IRFU SAp, Ctr Saclay, Lab AIM,CEA DRF CNRS, F-91191 Gif Sur Yvette, France. EM david.salabert@cea.fr FU European Community's Seventh Framework Program [312844, 269194]; CNES GOLF grant; PLATO grant; ANR (Agence Nationale de la Recherche, France) program IDEE "Interaction Des Etoiles et des Exoplanetes" [ANR-12-BS05-0008]; Newkirk Fellowship at the High Altitude Observatory; NASA [NNX12AE17G, NNX15AF13G]; CNPq PDE Harvard grant [PQ 308830/2012-1 CNPQ] FX The authors wish to thank the entire Kepler team, without whom these results would not be possible. Funding for this Discovery mission is provided by NASA Science Mission Directorate. The ground-based observations are based on spectroscopy made with the Mercator Telescope, operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work utilizes data from the National Solar Observatory/Sacramento Peak Ca II K-line Monitoring Program, managed by the National Solar Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. The research leading to these results has received funding from the European Community's Seventh Framework Program ([FP7/2007-2013]) under grant agreement No. 312844 (SPACEINN) and under grant agreement No. 269194 (IRSES/ASK). D.S. and R.A.G. acknowledge the financial support from the CNES GOLF and PLATO grants. P.G.B. acknowledges the ANR (Agence Nationale de la Recherche, France) program IDEE (No ANR-12-BS05-0008) "Interaction Des Etoiles et des Exoplanetes". R.E. is supported by the Newkirk Fellowship at the High Altitude Observatory. S.M. acknowledges support from the NASA grants NNX12AE17G and NNX15AF13G. T.M. acknowledges support from the NASA grant NNX15AF13G. J.D.N. Jr. acknowledges support from CNPq PQ 308830/2012-1 CNPq PDE Harvard grant. D.S. acknowledges the Observatoire de la Cote d'Azur for support during his stays. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 86 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2016 VL 596 AR A31 DI 10.1051/0004-6361/201628583 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG1MX UT WOS:000390797900050 ER PT J AU Saulder, C Van Kampen, E Chilingarian, IV Mieske, S Zeilinger, WW AF Saulder, Christoph Van Kampen, Eelco Chilingarian, Igor V. Mieske, Steffen Zeilinger, Werner W. TI The matter distribution in the local Universe as derived from galaxy groups in SDSS DR12 and 2MRS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; galaxies: distances and redshifts; large-scale structure of Universe; galaxies: statistics ID DIGITAL-SKY-SURVEY; MORPHOLOGY-DENSITY RELATION; PROBE WMAP OBSERVATIONS; MASS RECONSTRUCTION PROJECT; STAR-FORMATION HISTORIES; LUMINOUS RED GALAXIES; 7TH DATA RELEASE; REDSHIFT SURVEY; STELLAR MASS; COSMOLOGICAL IMPLICATIONS AB Context. Friends-of-friends algorithms are a common tool to detect galaxy groups and clusters in large survey data. In order to be as precise as possible, they have to be carefully calibrated using mock catalogues. Aims. We create an accurate and robust description of the matter distribution in the local Universe using the most up-to-date available data. This will provide the input for a specific cosmological test planned as follow-up to this work, and will be useful for general extragalactic and cosmological research. Methods. We created a set of galaxy group catalogues based on the 2MRS and SDSS DR12 galaxy samples using a friends-of-friends based group finder algorithm. The algorithm was carefully calibrated and optimised on a new set of wide-angle mock catalogues from the Millennium simulation, in order to provide accurate total mass estimates of the galaxy groups taking into account the relevant observational biases in 2MRS and SDSS. Results. We provide four different catalogues: (i) a 2MRS based group catalogue; (ii) an SDSS DR12 based group catalogue reaching out to a redshift z = 0.11 with stellar mass estimates for 70% of the galaxies; (iii) a catalogue providing additional fundamental plane distances for all groups of the SDSS catalogue that host elliptical galaxies; (iv) a catalogue of the mass distribution in the local Universe based on a combination of our 2MRS and SDSS catalogues. Conclusions. While motivated by a specific cosmological test, three of the four catalogues that we produced are well suited to act as reference databases for a variety of extragalactic and cosmological science cases. Our catalogue of fundamental plane distances for SDSS groups provides further added value to this paper. C1 [Saulder, Christoph; Zeilinger, Werner W.] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. [Van Kampen, Eelco] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Chilingarian, Igor V.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St,MS09, Cambridge, MA 02138 USA. [Chilingarian, Igor V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, 13 Univ Ski Prospect, Moscow 119992, Russia. [Mieske, Steffen] European Southern Observ, Alonso Cordova 3107,Casilla 19001, Santiago, Chile. RP Saulder, C (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. EM christoph.saulder@equinoxomega.net FU ESO; Telescope Data Center, Smithsonian Astrophysical Observatory; Russian Foundation for Basic Research [15-52-15050, 15-32-21062]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; National Aeronautics and Space Administration; [MD-7355.2015.2] FX C.S. is grateful to Aaron Robotham for helpful advice and also acknowledges the support from an ESO studentship. I.C. is supported by the Telescope Data Center, Smithsonian Astrophysical Observatory. His activities related to catalogues and databases are supported by the grant MD-7355.2015.2 and Russian Foundation for Basic Research projects 15-52-15050 and 15-32-21062. IC also acknowledges the ESO Visiting Scientist programme. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSSIII is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 122 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2016 VL 596 AR A14 DI 10.1051/0004-6361/201526711 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG1MX UT WOS:000390797900003 ER PT J AU Bell, RC AF Bell, Rayna C. TI A New Species of Hyperolius (Amphibia: Hyperoliidae) from Principe Island, Democratic Republic of Sao Tome and Principe SO HERPETOLOGICA LA English DT Article DE Anura; Gulf of Guinea; Hyperolius drewesi sp nov.; Hyperolius molleri; Hyperolius thomensis ID OVERSEAS DISPERSAL; OCEANIC ISLANDS; REED FROGS; GUINEA; GULF AB I describe a new species of reed frog (Hyperolius: Hyperoliidae) from the island of Principe in the Gulf of Guinea archipelago. The new species is within the Hyperolius cinnamomeoventris species complex, which includes four described species: H. cinnamomeoventris, H. veithi, H. molleri, and H. thomensis. The new species is sexually monochromatic (males and females have green dorsal coloration) and is thus distinguished from H. cinnamomeoventris, which is sexually dichromatic, and from H. veithi, in which both males and females are tan with yellow dorsolateral lines. The new species is smaller in size than H. thomensis, and differs in coloration from H. molleri and H. thomensis by lacking a black contour along the edges of the green/yellow band of coloration that extends down the dorsal side of the thigh, by lacking red/orange coloration on the dorsal and ventral sides of the thigh, and in the mitochondrial 16s and cytochrome-b genes. Furthermore, previous work indicates that the new species is distinct from H. molleri and H. thomensis in analyses of genome-wide single-nucleotide polymorphisms. This new species is the third endemic amphibian described from this small oceanic island. The type material for the closely related H. molleri and H. thomensis was destroyed or lost; therefore, I designate neotype material for these two species to enable the description of the new species. C1 [Bell, Rayna C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Bell, Rayna C.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. RP Bell, RC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA.; Bell, RC (reprint author), Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. EM bellrc@si.edu FU University of California Chancellor's Postdoctoral Fellowship; California Academy of Sciences Gulf of Guinea Fund FX I thank the Ministry of Environment (Director General A. de Ceita Carvalho, V. Bonfim, and S. Sousa Pontes) for permission to collect and export specimens for study, STeP Up Sao Tome (E.N. Seligman, R. dos Santos, and Q. Quade Cabral) and HBD of Bom Bom Island Resort and the Omali Lodge for logistical support, and R.C. Drewes, A. Stanbridge, J.P. Pio, B. Simison, and V. Schnoll for assistance in the field. Fieldwork was conducted under Cornell University IACUC protocol 1999-0010. J. Vindum and L. Scheinberg (California Academy of Sciences) loaned specimens in their care. I thank R. Ayres for assistance with translating the abstract and K. Whitney for taking photographs of the type material. This work was supported by a University of California Chancellor's Postdoctoral Fellowship and the California Academy of Sciences Gulf of Guinea Fund. NR 17 TC 0 Z9 0 U1 1 U2 1 PU HERPETOLOGISTS LEAGUE PI EMPORIA PA EMPORIA STATE UNIV, DIVISION BIOLOGICAL SCIENCES, 1200 COMMERCIAL ST, EMPORIA, KS 66801-5087 USA SN 0018-0831 EI 1938-5099 J9 HERPETOLOGICA JI Herpetologica PD DEC PY 2016 VL 72 IS 4 BP 343 EP 351 PG 9 WC Zoology SC Zoology GA EG9FZ UT WOS:000391365600009 ER PT J AU Nandintsetseg, D Kaczensky, P Ganbaatar, O Leimgruber, P Mueller, T AF Nandintsetseg, Dejid Kaczensky, Petra Ganbaatar, Oyunsaikhan Leimgruber, Peter Mueller, Thomas TI Spatiotemporal habitat dynamics of ungulates in unpredictable environments: The khulan (Equus hemionus) in the Mongolian Gobi desert as a case study SO BIOLOGICAL CONSERVATION LA English DT Article DE Nomadic movement; Habitat dynamic; Water availability; Dryland; Khulan; Habitat connectivity ID MIGRATION; MOVEMENT; DISTRIBUTIONS; RANGELANDS; SERENGETI; GAZELLES; ECOLOGY; POPULATIONS; COMPETITION; LANDSCAPES AB In resource-poor environments many large herbivores do not perform seasonal migrations but show unpredictable, long-range movements within a given season. The few studies that have examined drivers for within season long-range movements suggest that these movements are a response to spatiotemporal dynamics of foraging resources. We tested this hypothesis and were especially interested in detecting dynamics of foraging habitat which may influence high mobility of khulan, Equus hemionus, during summers in the Dzungarian Gobi of Mongolia. We used six years of ground census data combined with remotely sensed imagery of vegetation productivity (NDVI) to build a dynamic habitat model. We subsequently predicted khulan habitat suitability for each of the seven 16-day NDVI intervals every summer between 2004 and 2009 and examined variability of the resulting 42 prediction maps to characterize spatiotemporal dynamics in khulan foraging habitat. Our analyses showed khulan summer foraging habitat was highly predictable with little spatiotemporal variability making it unlikely that broad scale variability of foraging habitats can explain the high mobility of khulan. The few and small areas that did show khulan habitat variability were related to locations around water sources. In addition, we found that khulan avoided habitats beyond 21 km from water sources. Together these findings suggest that water availability and switching among the sparsely located water bodies rather than broad scale dynamics of foraging habitats may be the key driver for the high mobility of khulan in the Dzungarian Gobi. Our findings highlight the importance of securing access to and connectivity among water bodies for wild ungulates and the need for further studies on possible drivers of nomadic movements in drylands. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Nandintsetseg, Dejid; Mueller, Thomas] Senckenberg Gesell Nat Forsch, Senckenberg Biodivers & Climate Res Ctr, Senckenberganlage 25, Frankfurt, Germany. [Nandintsetseg, Dejid; Mueller, Thomas] Goethe Univ Frankfurt, Dept Biol Sci, Max von Laue Str 9, D-60438 Frankfurt, Germany. [Kaczensky, Petra] Univ Vet Med, Res Inst Wildlife Ecol, Savoyenstr 1, Vienna, Austria. [Ganbaatar, Oyunsaikhan] Great Gobi B Strictly Protected Area Adm, Ulaanbaatar, Mongol Peo Rep. [Ganbaatar, Oyunsaikhan] Int Takhi Grp, Baigali Ordon, Ulaanbaatar, Mongol Peo Rep. [Leimgruber, Peter; Mueller, Thomas] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Nandintsetseg, D (reprint author), Senckenberg Gesell Nat Forsch, Senckenberg Biodivers & Climate Res Ctr, Senckenberganlage 25, Frankfurt, Germany. EM dnandintsetseg@gmail.com FU Austrian Science Foundation FWF project [P14992, P18624]; University of Veterinary Sciences in Vienna; Robert Bosch Foundation in Germany FX Logistical and financial support was funded by the Austrian Science Foundation FWF project P14992 and P18624, the University of Veterinary Sciences in Vienna, and the Robert Bosch Foundation in Germany. Our special thanks to the administration of the Great Gobi B Strictly Protected Area, and the rangers who helped with logistics and carried out the long-term wildlife monitoring under harsh climate conditions in the Dzungarian Gobi. Without their field work, this study would not have been completed. We are grateful to S.R.B. King for assistance in editing English of this manuscript. NR 54 TC 0 Z9 0 U1 6 U2 6 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD DEC PY 2016 VL 204 BP 313 EP 321 DI 10.1016/j.biocon.2016.10.021 PN B PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EG3TZ UT WOS:000390968900021 ER PT J AU Casadio, C Gomez, JL Jorstad, SG Marscher, AP Grandi, P Larionov, VM Lister, ML Smith, PS Gurwell, MA Lahteenmaki, A Agudo, I Molina, SN Bala, V Joshi, M Taylor, B Williamson, KE Kovalev, YY Savolainen, T Pushkarev, AB Arkharov, AA Blinov, DA Borman, GA Di Paola, A Grishina, TS Hagen-Thorn, VA Itoh, R Kopatskaya, EN Larionova, EG Larionova, LV Morozova, DA Rastorgueva-Foi, E Sergeev, SG Tornikoski, M Troitsky, IS Thum, C Wiesemeyer, H AF Casadio, Carolina Gomez, Jose L. Jorstad, Svetlana G. Marscher, Alan P. Grandi, Paola Larionov, Valeri M. Lister, Matthew L. Smith, Paul S. Gurwell, Mark A. Lahteenmaki, Anne Agudo, Ivan Molina, Sol N. Bala, Vishal Joshi, Manasvita Taylor, Brian Williamson, Karen E. Kovalev, Yuri Y. Savolainen, Tuomas Pushkarev, Alexander B. Arkharov, Arkady A. Blinov, Dmitry A. Borman, George A. Di Paola, Andrea Grishina, Tatiana S. Hagen-Thorn, Vladimir A. Itoh, Ryosuke Kopatskaya, Evgenia N. Larionova, Elena G. Larionova, Liudmila V. Morozova, Daria A. Rastorgueva-Foi, Elizaveta Sergeev, Sergey G. Tornikoski, Merja Troitsky, Ivan S. Thum, Clemens Wiesemeyer, Helmut TI The Connection between the Radio Jet and the gamma-ray Emission in the Radio Galaxy 3C 120 and the Blazar CTA 102 SO GALAXIES LA English DT Article DE galaxies: active; galaxies: radio continuum; galaxies: jets ID ACTIVE GALACTIC NUCLEI; OUTBURSTS; KINEMATICS; FLARE AB We present multi-wavelength studies of the radio galaxy 3C 120 and the blazar CTA 102 during unprecedented gamma-ray flares for both sources. In both studies the analysis of gamma-ray data has been compared with a series of 43 GHz VLBA images from the VLBA-BU-BLAZAR program, providing the necessary spatial resolution to probe the parsec scale jet evolution during the high energy events. To extend the radio dataset for 3C 120 we also used 15 GHz VLBA data from the MOJAVE sample. These two objects which represent very different classes of AGN, have similar properties during the gamma-ray events. The gamma-ray flares are associated with the passage of a new superluminal component through the mm VLBI core, but not all ejections of new components lead to gamma-ray events. In both sources gamma-ray events occurred only when the new components are moving in a direction closer to our line of sight. We locate the g-ray dissipation zone a short distance from the radio core but outside of the broad line region, suggesting synchrotron self-Compton scattering as the probable mechanism for the gamma-ray production. C1 [Casadio, Carolina; Kovalev, Yuri Y.; Savolainen, Tuomas; Pushkarev, Alexander B.; Wiesemeyer, Helmut] Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany. [Gomez, Jose L.; Agudo, Ivan; Molina, Sol N.] CSIC, Inst Astrofis Andalucia, Glorieta Astron,S-N, E-18008 Granada, Spain. [Jorstad, Svetlana G.; Marscher, Alan P.; Bala, Vishal; Joshi, Manasvita; Taylor, Brian; Williamson, Karen E.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.; Larionov, Valeri M.; Blinov, Dmitry A.; Grishina, Tatiana S.; Hagen-Thorn, Vladimir A.; Kopatskaya, Evgenia N.; Larionova, Elena G.; Larionova, Liudmila V.; Morozova, Daria A.; Troitsky, Ivan S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Grandi, Paola] Ist Nazl Astrofis IASFBO, I-40127 Bologna, Italy. [Larionov, Valeri M.; Lahteenmaki, Anne; Savolainen, Tuomas; Tornikoski, Merja] Aalto Univ, Metsahovi Radio Observ, FI-02540 Kylmala, Finland. [Lister, Matthew L.] Purdue Univ, Dept Phys, 610 Purdue Mall, W Lafayette, IN 47907 USA. [Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Gurwell, Mark A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lahteenmaki, Anne] Aalto Univ, Dept Radio Sci & Engn, FI-00076 Aalto, Finland. [Kovalev, Yuri Y.] Russian Acad Sci, Ctr Astro Space, Inst Phys, Moscow 117810, Russia. [Pushkarev, Alexander B.; Borman, George A.; Sergeev, Sergey G.] Crimean Astrophys Observ, Nauchny 98409, Crimea, Russia. [Pushkarev, Alexander B.; Arkharov, Arkady A.] Pulkovo Observ, St Petersburg 196140, Russia. [Blinov, Dmitry A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Greece. [Blinov, Dmitry A.] Univ Crete, Inst Plasma Phys, GR-71003 Iraklion, Greece. [Di Paola, Andrea] INAF, Osservatorio Astron Roma, I-00136 Rome, Italy. [Itoh, Ryosuke] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398511, Japan. [Rastorgueva-Foi, Elizaveta] Univ Tasmania, Sch Maths & Phys, Private Bag 37, Hobart, Tas 7001, Australia. [Thum, Clemens] Inst Radio Astron Milimetr, Granada 18012, Spain. RP Casadio, C (reprint author), Max Planck Inst Radioastron, Auf Hugel 69, D-53121 Bonn, Germany. EM casadio@mpifr-bonn.mpg.de; jlgomez@iaa.es; jorstad@bu.edu; marscher@bu.edu; paola.grandi@iasfbo.inaf.it; vlar2@yandex.ru; mlister@purdue.edu; psmith@as.arizona.edu; mgurwell@cfa.harvard.edu; anne.lahteenmaki@aalto.fi; iagudo@iaa.es; smolina@iaa.es; mjoshi@bu.edu; bwtaylor@bu.edu; kwilliam@bu.edu; yyk@asc.rssi.ru; tsavolainen@mpifr-bonn.mpg.de; apushkar@mpifr-bonn.mpg.de; arkadi@arharov.ru; dmitriy.blinov@gmail.com; borman.ga@gmail.com; andrea.dipaola@oa-roma.inaf.it; azt8@mail.ru; hth-home@yandex.ru; itoh@hep01.hepl.hiroshima-u.ac.jp; enik1346@rambler.ru; sung2v@mail.ru; lliudmila@yandex.ru; comitcont@gmail.com; gss2003@mail.ru; dernor@gmail.com; dernord3@gmail.com; troitsky@gmail.com; thum@iram.es; hwiese@mpifr-bonn.mpg.de RI Lahteenmaki, Anne/L-5987-2013; Morozova, Daria/H-1298-2013; Kovalev, Yuri/J-5671-2013 OI Morozova, Daria/0000-0002-9407-7804; Kovalev, Yuri/0000-0001-9303-3263 NR 16 TC 0 Z9 0 U1 5 U2 5 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2075-4434 J9 GALAXIES JI Galaxies PD DEC PY 2016 VL 4 IS 4 AR 34 DI 10.3390/galaxies4040034 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG4HH UT WOS:000391004000002 ER PT J AU Fish, VL Akiyama, K Bouman, KL Chael, AA Johnson, MD Doeleman, SS Blackburn, L Wardle, JFC Freeman, WT AF Fish, Vincent L. Akiyama, Kazunori Bouman, Katherine L. Chael, Andrew A. Johnson, Michael D. Doeleman, Sheperd S. Blackburn, Lindy Wardle, John F. C. Freeman, William T. CA Event Horizon Telescope TI Observing-and Imaging-Active Galactic Nuclei with the Event Horizon Telescope SO GALAXIES LA English DT Article DE galaxies: jets; galaxy: center; techniques: high angular resolution; techniques: image processing; techniques: interferometric ID SUPERMASSIVE BLACK-HOLE; SAGITTARIUS A-ASTERISK; NO-HAIR THEOREM; SCALE STRUCTURE; RADIO INTERFEROMETRY; ACCRETION FLOW; 3C 84; M87; BASE; VLBI AB Originally developed to image the shadow region of the central black hole in Sagittarius A* and in the nearby galaxy M87, the Event Horizon Telescope (EHT) provides deep, very high angular resolution data on other active galactic nucleus (AGN) sources too. The challenges of working with EHT data have spurred the development of new image reconstruction algorithms. This work briefly reviews the status of the EHT and its utility for observing AGN sources, with emphasis on novel imaging techniques that offer the promise of better reconstructions at 1.3 mm and other wavelengths. C1 [Fish, Vincent L.; Akiyama, Kazunori] MIT, Haystack Observ, Westford, MA 01886 USA. [Akiyama, Kazunori] Japan Soc Promot Sci, Chiyoda Ku, Tokyo 1020083, Japan. [Bouman, Katherine L.; Freeman, William T.] MIT, Comp Sci & Artificial Intelligence Lab, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Chael, Andrew A.; Johnson, Michael D.; Doeleman, Sheperd S.; Blackburn, Lindy] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wardle, John F. C.] Brandeis Univ, Dept Phys, Waltham, MA 02453 USA. [Freeman, William T.] Google Inc, 1600 Amphitheatre Pkwy, Mountain View, CA 94043 USA. RP Fish, VL (reprint author), MIT, Haystack Observ, Westford, MA 01886 USA. EM vfish@haystack.mit.edu; kazu@haystack.mit.edu; klbouman@mit.edu; achael@physics.harvard.edu; mjohnson@cfa.harvard.edu; sdoeleman@cfa.harvard.edu; lblackburn@cfa.harvard.edu; wardle@brandeis.edu; billf@mit.edu FU National Science Foundation; Gordon and Betty Moore Foundation FX This work is made possible by grants from the National Science Foundation and the Gordon and Betty Moore Foundation. NR 50 TC 0 Z9 0 U1 0 U2 0 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2075-4434 J9 GALAXIES JI Galaxies PD DEC PY 2016 VL 4 IS 4 AR 54 DI 10.3390/galaxies4040054 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG4HH UT WOS:000391004000022 ER PT J AU Michiyama, T Iono, D Nakanishi, K Ueda, J Saito, T Ando, M Kaneko, H Yamashita, T Matsuda, Y Hatsukade, B Kikuchi, K Komugi, S Muto, T AF Michiyama, Tomonari Iono, Daisuke Nakanishi, Kouichiro Ueda, Junko Saito, Toshiki Ando, Misaki Kaneko, Hiroyuki Yamashita, Takuji Matsuda, Yuichi Hatsukade, Bunyo Kikuchi, Kenichi Komugi, Shinya Muto, Takayuki TI Investigating the relation between CO (3-2) and far-infrared luminosities for nearby merging galaxies using ASTE SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: starburst ID STAR-FORMATION RATE; HIGH-REDSHIFT GALAXIES; HEINRICH-HERTZ-TELESCOPE; ACTIVE GALACTIC NUCLEI; DENSE MOLECULAR GAS; MERGER VV 114; ULTRALUMINOUS GALAXIES; FORMATION EFFICIENCY; CONVERSION FACTOR; FORMING GALAXIES AB We present the new single-dish CO (3-2) emission data obtained toward 19 early-stage and 7 late-stage nearby merging galaxies using the Atacama Submillimeter Telescope Experiment (ASTE). Combining with the single-dish and interferometric data of galaxies observed in previous studies, we investigate the relation between the CO (3-2) luminosity (LCO(3-2)') and the far-infrared luminosity (L-FIR) in a sample of 29 early-stage and 31 late-stage merging galaxies, and 28 nearby isolated spiral galaxies. We find that normal isolated spiral galaxies and merging galaxies have different slopes (alpha) in the log LCO(3-2)'-log L-FIR plane (alpha similar to 0.79 for spirals and similar to 1.12 for mergers). The large slope (alpha > 1) for merging galaxies can be interpreted as evidence for increasing star formation efficiency (SFE = L-FIR/LCO(3-2)') as a function of L-FIR. Comparing our results with sub-kpc-scale local star formation and global starburst activity in the high-z universe, we find deviations from the linear relationship in the log LCO(3-2)'-log L-FIR plane for the late-stage mergers and high-z star-forming galaxies. Finally, we find that the average SFE gradually increases from isolated galaxies to merging galaxies and to highz submillimeter galaxies/quasi-stellar objects. By comparing our findings with results from numerical simulations, we suggest that: (1) inefficient starbursts triggered by disk-wide dense clumps occur in the early stage of interaction, and (2) efficient starbursts triggered by central concentration of gas occur in the final stage. A systematic high spatial resolution survey of diffuse- and dense-gas tracers is the key to confirming this scenario. C1 [Michiyama, Tomonari; Iono, Daisuke; Nakanishi, Kouichiro; Ando, Misaki; Matsuda, Yuichi] SOKENDAI Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Michiyama, Tomonari; Iono, Daisuke; Nakanishi, Kouichiro; Saito, Toshiki; Ando, Misaki; Kaneko, Hiroyuki; Matsuda, Yuichi; Hatsukade, Bunyo; Kikuchi, Kenichi] Natl Astron Observ Japan, Natl Inst Nat Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Ueda, Junko] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Saito, Toshiki] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1330033, Japan. [Kaneko, Hiroyuki] Nobeyama Radio Observ, 462-2 Minamimaki, Minamimaki, Nagano 3841305, Japan. [Yamashita, Takuji] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. [Komugi, Shinya; Muto, Takayuki] Kogakuin Univ, Div Liberal Arts, Shinjuku Ku, 1-24-2 Nishi Shinjuku, Tokyo 1638677, Japan. RP Michiyama, T (reprint author), SOKENDAI Grad Univ Adv Studies, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.; Michiyama, T (reprint author), Natl Astron Observ Japan, Natl Inst Nat Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM t.michiyama@nao.ac.jp FU JSPS KAKENHI Grant [15H02074]; Japan Society for the Promotion of Science for Young Scientists; Center for the Promotion of Integrated Sciences (CPIS) of SOKENDAI; National Aeronautics and Space Administration FX We greatly appreciate the feedback offered by referee. D.I., K.K., S.K., and T.M. are supported by JSPS KAKENHI Grant Number 15H02074. T.S. is financially supported by a Research Fellowship from the Japan Society for the Promotion of Science for Young Scientists. This work was supported in part by the Center for the Promotion of Integrated Sciences (CPIS) of SOKENDAI.; The ASTE telescope is operated by the National Astronomical Observatory of Japan (NAOJ). This research is based on observations with AKARI, a JAXA project with the participation of ESA. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 70 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC PY 2016 VL 68 IS 6 AR 96 DI 10.1093/pasj/psw087 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG8GV UT WOS:000391295100008 ER PT J AU Comizzoli, P AF Comizzoli, Pierre TI Advanced biotechnologies for wildlife fertility preservation SO THAI JOURNAL OF VETERINARY MEDICINE LA English DT Review DE wildlife; reproduction; conservation biology; biotechnologies; fertility preservation; cryopreservation ID REPRODUCTIVE SCIENCE; SPERM CRYOPRESERVATION; CONSERVATION; REALITY AB Reproductive biotechnologies are critical tools for saving and maintaining endangered species. Some successes have been reported with the use and integration of artificial insemination (with fresh or frozen-thawed semen) in conservation programs. However, not a single species is currently managed through oocyte freezing or embryo-based technologies. This is primarily due to the lack of knowledge of species biology, as well as inadequate facilities, space, expertise, and funding needed for their successful application. More fundamental studies of animal reproductive biology as well as more fertility preservation options are needed with all parties involved (reproductive technologists, zoo biologists and conservationists) adopting parallel efforts to sustain wild populations and habitats. C1 [Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. RP Comizzoli, P (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. EM comizzolip@si.edu NR 16 TC 0 Z9 0 U1 12 U2 12 PU CHULALONGKORN UNIV PI BANGKOK PA FAC VETERINARY SCI, HENRI DUNANT RD, BANGKOK, 10330, THAILAND SN 0125-6491 J9 THAI J VET MED JI Thai J. Vet. Med. PD DEC PY 2016 VL 46 IS 4 BP 541 EP 545 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA EG2CY UT WOS:000390851600002 ER PT J AU Crawford, TM Chown, R Holder, GP Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crites, AT de Haan, T Dobbs, MA George, EM Halverson, NW Harrington, NL Holzapfel, WL Hou, Z Hrubes, JD Keisler, R Knox, L Lee, AT Leitch, EM Luong-Van, D Marrone, DP McMahon, JJ Meyer, SS Mocanu, LM Mohr, JJ Natoli, T Padin, S Pryke, C Reichardt, CL Ruhl, JE Sayre, JT Schaffer, KK Shirokoff, E Staniszewski, Z Stark, AA Story, KT Vanderlinde, K Vieira, JD Williamson, R AF Crawford, T. M. Chown, R. Holder, G. P. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H-M. Crites, A. T. de Haan, T. Dobbs, M. A. George, E. M. Halverson, N. W. Harrington, N. L. Holzapfel, W. L. Hou, Z. Hrubes, J. D. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Luong-Van, D. Marrone, D. P. McMahon, J. J. Meyer, S. S. Mocanu, L. M. Mohr, J. J. Natoli, T. Padin, S. Pryke, C. Reichardt, C. L. Ruhl, J. E. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Staniszewski, Z. Stark, A. A. Story, K. T. Vanderlinde, K. Vieira, J. D. Williamson, R. TI MAPS OF THE MAGELLANIC CLOUDS FROM COMBINED SOUTH POLE TELESCOPE AND PLANCK DATA SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE Magellanic Clouds; methods: data analysis ID SOURCE CATALOG; RESULTS. VI.; EMISSION; RADIO; SKY; HFI; SUBMILLIMETER; SPECTRUM; FIELD; DUST AB We present maps of the Large and Small Magellanic Clouds from combined South Pole Telescope (SPT) and Planck data. The Planck satellite observes in nine bands, while the SPT data used in this work were taken with the three-band SPT-SZ camera, The SPT-SZ bands correspond closely to three of the nine Planck bands, namely those centered at 1.4, 2.1, and 3.0 mm. The angular resolution of the Planck data ranges from 5 to 10 arcmin, while the SPT resolution ranges from 1.0 to 1.7 arcmin. The combined maps take advantage of the high resolution of the SPT data and the long-timescale stability of the space-based Planck observations to deliver robust brightness measurements on scales from the size of the maps down to similar to 1 arcmin. In each band, we first calibrate and color-correct the SPT data to match the Planck data, then we use noise estimates from each instrument and knowledge of each instrument's beam to make the inverse-variance-weighted combination of the two instruments' data as a function of angular scale. We create maps assuming a range of underlying emission spectra and at a range of final resolutions. We perform several consistency tests on the combined maps and estimate the expected noise in measurements of features in them. We compare maps from this work to those from the Herschel HERITAGE survey, finding general consistency between the data sets. All data products described in this paper are available for download from the NASA Legacy Archive for Microwave Background Data Analysis server. C1 [Crawford, T. M.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Hou, Z.; Keisler, R.; Leitch, E. M.; Meyer, S. S.; Mocanu, L. M.; Natoli, T.; Padin, S.; Schaffer, K. K.; Shirokoff, E.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Crawford, T. M.; Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Hou, Z.; Leitch, E. M.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Shirokoff, E.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Chown, R.; Holder, G. P.; de Haan, T.; Dobbs, M. A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, MS209,POB 500, Batavia, IL 60510 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H-M.] SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. [Crites, A. T.] CALTECH, Pasadena, CA 91125 USA. [de Haan, T.; George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [George, E. M.; Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Halverson, N. W.; Sayre, J. T.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.; Sayre, J. T.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Keisler, R.; Story, K. T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Ludwig Maximilians Univ Munchen, Fac Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Natoli, T.; Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Staniszewski, Z.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Story, K. T.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [Vieira, J. D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. RP Crawford, TM (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA.; Crawford, TM (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM tcrawfor@kicp.uchicago.edu OI Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; U.S. Department of Energy [DE-AC02-06CH11357] FX The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. Argonne National Laboratory work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. We thank M. Meixner and the HERITAGE team for making their data publicly available and K. Ganga for helpful discussion on Planck map properties. NR 28 TC 1 Z9 1 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD DEC PY 2016 VL 227 IS 2 AR 23 DI 10.3847/1538-4365/227/2/23 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EG1MF UT WOS:000390795900003 ER PT J AU Lee, MY Lee, SM Song, EG An, JH Voloshina, I Chong, JR Johnson, WE Min, MS Lee, H AF Lee, Mu-Yeong Lee, Seon-Mi Song, Eui-Geun An, Jung Hwa Voloshina, Inna Chong, Jong Royl Johnson, Warren E. Min, Mi-Sook Lee, Hang TI Phylogenetic relationships and genetic diversity of badgers from the Korean Peninsula: Implications for the taxonomic status of the Korean badger SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article DE Phylogenetic relationships; Korean badger; Taxonomic status; Mitochondrial DNA; Phylogeography ID MITOCHONDRIAL-DNA; SOUTH-KOREA; EAST-ASIA; POPULATION-STRUCTURE; PHYLOGEOGRAPHY; MUSTELIDAE; HISTORY; MELES; SEQUENCES; GENEALOGY AB Accurate taxonomic classification of wildlife species is crucial for guiding biological research and for developing effective management and conservation programs. The taxonomic status of Eurasian badgers from South Korea remains poorly resolved. Here we assessed the phylogenetic relationships and genetic variation of Eurasia badgers using partial mitochondrial fragments to elucidate the evolutionary history and taxonomic status of badgers from the Korean Peninsula. Forty-eight unique haplotypes from 125 individuals were observed. Phylogenetic reconstructions and reduced median networks indicate that Eurasian badgers consisted of four geographic clades (Japan, Eastern Eurasia, Western Eurasia, and Caucasus) with a relatively weak split observed within Eastern Eurasia. Estimated divergence time between the Japanese and Eastern Eurasian clades, including the Korean population, was 467,100 years (69,200-1,085,500 years). The results of this study support the hypothesis that the Japanese badger migrated from the Eurasian continent over the Korea-Japan land bridge and that the Korean Peninsula was an important refugia during the Pleistocene. Our study confirmed that the South Korean badger, Meles metes, belongs to the Eastern Eurasian clade. Based on these results and those of previous studies, we recommend that the scientific name of the Korean badger be changed from M. metes to Meles leucurus (Asian badger). (C) 2016 Elsevier Ltd. All rights reserved. C1 [Lee, Mu-Yeong; Lee, Seon-Mi; Song, Eui-Geun; Min, Mi-Sook; Lee, Hang] Seoul Natl Univ, Plus Program Creat Vet Sci Res BK21, Seoul 151742, South Korea. [Lee, Mu-Yeong; Lee, Seon-Mi; Song, Eui-Geun; Min, Mi-Sook; Lee, Hang] Seoul Natl Univ, Coll Vet Med, Conservat Genome Resource Bank Korean Wildlife CG, Seoul 151742, South Korea. [An, Jung Hwa] Natl Inst Biol Resources, Hwangyeong Ro 42, Inchon 404170, South Korea. [Voloshina, Inna] Lazovsky State Nat Reserve, 56 Centralnaya St Lazo, Primorsky Krai 692980, Russia. [Chong, Jong Royl] Korea Univ Japan, Fac Educ, 1-700 Ogawa Cho, Kodaira, Tokyo 187, Japan. [Johnson, Warren E.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Song, Eui-Geun] Natl Inst Ecol, Seocheon Gun 33657, Chungcheongnam, South Korea. RP Lee, H (reprint author), Seoul Natl Univ, Coll Vet Med, Sillim Dong San 56-1, Seoul 151742, South Korea. EM hanglee@snu.ac.kr FU National Research Foundation of Korea grant - the Korean Government [NRF-2011K1A5A2000058, 355-2011-1-C00055]; Unification Study Program from the Institute for Peace and Unification Studies through the Seoul National University [2011K1A5A2000058]; Research Institute for Veterinary Science, Seoul National University FX The authors gratefully acknowledge Donggul Wo at the National Institute of Ecology, South Korea for helpful comments on ecological aspects of the analyses and for providing many references of ecological studies. In addition, we would like to thank the numerous contributors who donated valuable samples to the CGRB to be used in this study. This study was supported in part by a gs1:National Research Foundation of Korea grant funded by the Korean Government (NRF-2011K1A5A2000058; 355-2011-1-C00055) and by the 2012 Unification Study Program from the Institute for Peace and Unification Studies through the Seoul National University (2011K1A5A2000058). This study was also partially supported by the Research Institute for Veterinary Science, Seoul National University. NR 51 TC 0 Z9 0 U1 3 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 EI 1873-2925 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD DEC PY 2016 VL 69 BP 18 EP 26 DI 10.1016/j.bse.2016.07.015 PG 9 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA EF7GE UT WOS:000390497300004 ER PT J AU Miller, JA DiMaria, RA Hurst, TP AF Miller, Jessica A. DiMaria, Ruth A. Hurst, Thomas P. TI Patterns of larval source distribution and mixing in early life stages of Pacific cod (Gadus macrocephalus) in the southeastern Bering Sea SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Otolith chemistry; Pacific cod; Alaska Peninsula; Bering Sea; Juvenile; Larval sources ID CORAL-REEF FISH; ROCKFISH SEBASTES-MELANOPS; OPEN-COAST FISH; OTOLITH CHEMISTRY; POPULATION-STRUCTURE; ELEMENTAL FINGERPRINTS; TRACE-ELEMENTS; NATURAL TAGS; GROWTH-RATE; TEMPERATURE AB Effective and sustainable management depends on knowledge of spawning locations and their relative contributions to marine fish populations. Pacific cod (Gadus macrocephalus) in the southeastern Bering Sea aggregate at discrete spawning locations but there is little information on patterns of larval dispersal and the relative contribution of specific spawning areas to nursery habitats. Age-0 Pacific cod from two cohorts (2006 and 2008) were examined to address the following questions: (1) does size, age, and otolith chemistry vary among known capture locations; (2) can variation in elemental composition of the otolith cores (early larval signatures) be used to infer the number of chemically distinct sources contributing to juvenile recruits in the Bering Sea; and (3) to what extent are juvenile collection locations represented by groups of fish with similar chemical histories throughout their early life history? Hierarchical cluster (HCA) and discriminant function analyses (DFA) were used to examine variation in otolith chemistry at discrete periods throughout the early life history. HCA identified five chemically distinct groups of larvae in the 2006 cohort and three groups in 2008; however, three sources accounted for 80-100% of the juveniles in each year. DFA of early larval signatures indicated that there were non-random spatial distributions of early larvae in both years, which may reflect interannual variation in regional oceanography. There was also a detectable and substantial level of coherence in chemical signatures within groups of fish throughout the early life history. The variation in elemental signatures throughout the early life history (hatch to capture) indicates that otolith chemical analysis could be an effective tool to further clarify larval sources and dispersal, identify juvenile nursery habitats, and estimate the contributions of juvenile nursery habitats to the adult population within the southeastern Bering Sea. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Miller, Jessica A.; DiMaria, Ruth A.] Oregon State Univ, Dept Fisheries & Wildlife, Coastal Oregon Marine Expt Stn, Hatfield Marine Sci Ctr, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. [Hurst, Thomas P.] NOAA, Fisheries Behav Ecol Program, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr,Natl Marine Fisheries Sc, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. [DiMaria, Ruth A.] Smithsonian Environm Res Ctr, Marine Invas Res Lab, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Miller, JA (reprint author), Oregon State Univ, Dept Fisheries & Wildlife, Coastal Oregon Marine Expt Stn, Hatfield Marine Sci Ctr, 2030 SE Marine Sci Dr, Newport, OR 97365 USA. EM jessica.miller@oregonstate.edu; DiMariaR@si.edu; thomas.hurst@noaa.gov FU North Pacific Research Board [R0816] FX We express sincere appreciation to the following people whose contributions made this research possible: the Ecosystems & Fisheries Oceanography Coordinated Investigations and the Bering-Aleutian Salmon International Survey programs for collections of larval and juvenile Pacific cod; A. Ungerer of the W.M. Keck Collaboratory for providing valuable assistance with ICPMS analyses; M. Spencer for assisting with ArcGIS mapping; C. Danley, A. Paul and W. Clerf for assistance with otolith preparation; and L Ciannelli, G. Boehlert, and two anonymous reviewers whose comments greatly improved the manuscript A portion of this work was completed in partial fulfillment of RAD.'s M.S. thesis at Oregon State University. This research was supported with funding from the North Pacific Research Board grant no. R0816. This contribution is North Pacific Research Board publication number 500. The findings and conclusions in this paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service. Reference to trade names does not imply endorsement by the National Marine Fisheries Service. NR 60 TC 2 Z9 2 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 EI 1879-0100 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD DEC PY 2016 VL 134 BP 270 EP 282 DI 10.1016/j.dsr2.2014.12.012 PG 13 WC Oceanography SC Oceanography GA EF7LG UT WOS:000390510500020 ER PT J AU Ergunay, K Litzba, N Brinkmann, A Gunay, F Kar, S Oter, K Orsten, S Sarikaya, Y Alten, B Nitsche, A Linton, YM AF Ergunay, Koray Litzba, Nadine Brinkmann, Annika Gunay, Filiz Kar, Sirri Oter, Kerem Orsten, Serra Sarikaya, Yasemen Alten, Bulent Nitsche, Andreas Linton, Yvonne-Marie TI Isolation and genomic characterization of Culex theileri flaviviruses in field-collected mosquitoes from Turkey SO INFECTION GENETICS AND EVOLUTION LA English DT Article DE Flavivirus; Mosquito; Culex; Turkey; Genome ID INSECT-SPECIFIC FLAVIVIRUSES; GENETIC-CHARACTERIZATION; TRANSMISSION; ALIGNMENT; RNA; SURVEILLANCE; EVOLUTION; DATABASE; VIRUSES AB Vector surveillance for the arthropod-borne infections has resulted in the isolation of a growing number of novel viruses, including several flavivirus strains that exclusively replicate in insects. This report describes the isolation and genomic characterization of four insect-specific flaviviruses frommosquitoes, previously collected from various locations in Turkey. C6/36 Aedes albopictus and Vero cell lines were inoculated with mosquito pools. On C6/36 cells, mild cytopathic effects, characterized as rounding and detachment, were observed in four pools that comprised female Culex theileri mosquitoes. Complete (3 isolates, 10,697 nucleotides) or near-complete (1 isolate, 10,452 nucleotides) genomic characterization was performed in these culture supernatants via next generation sequencing. All strains demonstrated high genetic similarities, with over 99% identity match on nucleotide and amino acid alignments, revealing them to be different isolates of the same virus. Sequence comparisons identified the closest relative to be the Culex theileri flavivirus (CTFV) strains, originally characterized in Portugal. Phylogenetic analyses demonstrated that the isolates remained distinct as a cluster but formed amonophyletic group with CTFV strains, and shared a common ancestor with Quang Binh or related Culex flaviviruses. The organization of the viral genome was consistent with the universal flavivirus structure and stem-loops; conserved motifs and imperfect tandem repeats were identified in the non-coding ends of the viral genomes. A potential ribosomal shifting site, resulting in the translation of an additional reading frame, was detected. The deduced viral polyprotein comprised 3357 amino acids and was highly-conserved. Amino acid variations, presumably associated with adaptive environmental pressures, were identified. These isolates comprise the first fully characterized insect-specific flaviviruses in Turkey. Their impact on West Nile virus circulation, which is also endemic in the study region, remains to be explored. (C) 2016 Elsevier B.V. All rights reserved. C1 [Ergunay, Koray; Orsten, Serra] Hacettepe Univ, Fac Med, Dept Med Microbiol, Virol Unit, Morphol Bldg 3rd Floor, TR-06100 Ankara, Turkey. [Ergunay, Koray; Litzba, Nadine; Brinkmann, Annika; Nitsche, Andreas] Robert Koch Inst, Ctr Biol Threats & Special Pathogens ZBS 1 1, Berlin, Germany. [Gunay, Filiz; Sarikaya, Yasemen; Alten, Bulent] Hacettepe Univ, Fac Sci, Dept Biol, Div Ecol, Ankara, Turkey. [Kar, Sirri] Namik Kemal Univ, Fac Arts & Sci, Dept Biol, Tekirdag, Turkey. [Oter, Kerem] Istanbul Univ, Fac Vet Med, Dept Parasitol, Istanbul, Turkey. [Linton, Yvonne-Marie] Smithsonian Inst, Museum Support Ctr MRC 534, Walter Reed Biosystemat Unit, Suitland, MD USA. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD USA. [Linton, Yvonne-Marie] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Ergunay, K (reprint author), Hacettepe Univ, Fac Med, Dept Med Microbiol, Virol Unit, Morphol Bldg 3rd Floor, TR-06100 Ankara, Turkey. EM ekoray@hacettepe.edu.tr FU Armed Forces Health Surveillance Center, Global Emerging Infections Surveillance and Response System (AFHSC-GEIS), United States [W81XWH-11-2-0174]; Georg Forster Research Fellowship (HERMES) for Experienced Researchers by Alexander von Humboldt Foundation; National Research Council (NRC) Research Associateship Award at the Walter Reed Army Institute of Research FX This study was partially supported by The Armed Forces Health Surveillance Center, Global Emerging Infections Surveillance and Response System (AFHSC-GEIS), United States (W81XWH-11-2-0174) (with Yvonne-Marie Linton as the principal investigator). KE is a recipient of the Georg Forster Research Fellowship (HERMES) for Experienced Researchers by the Alexander von Humboldt Foundation, 2015. This manuscript was prepared whilst YML held a National Research Council (NRC) Research Associateship Award at the Walter Reed Army Institute of Research. This research was performed in part under a Memorandum of Understanding between the Walter Reed Army Institute of Research and the Smithsonian Institution, with institutional support provided by both organizations. The funders had no role in study design, data collection and analysis, decision to publish or preparation of the manuscript. The material to be published reflects the views of the authors and should not be construed to represent those of the US Department of the Army or the US Department of Defense. NR 36 TC 1 Z9 1 U1 2 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1567-1348 EI 1567-7257 J9 INFECT GENET EVOL JI Infect. Genet. Evol. PD DEC PY 2016 VL 46 BP 138 EP 147 DI 10.1016/j.meegid.2016.11.008 PG 10 WC Infectious Diseases SC Infectious Diseases GA EF6QP UT WOS:000390456000021 PM 27840255 ER PT J AU Yu, SS Gordon, I Roy, PN AF Yu, Shanshan Gordon, Iouli Roy, Pierre-Nicholas TI Potentiology and spectroscopy in honor of Robert Le Roy: A preface to the special issue SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Biographical-Item C1 [Yu, Shanshan] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Gordon, Iouli] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, MS 50,60 Garden St, Cambridge, MA 02138 USA. [Roy, Pierre-Nicholas] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. RP Yu, SS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM shanshan.yu@jpl.nasa.gov; igordon@cfa.harvard.edu; pnroy@uwaterloo.ca RI Yu, Shanshan/D-8733-2016 NR 29 TC 0 Z9 0 U1 6 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD DEC PY 2016 VL 330 SI SI BP 1 EP 3 DI 10.1016/j.jms.2016.10.019 PG 3 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA EF9EX UT WOS:000390634600001 ER PT J AU Medvedev, ES Meshkov, VV Stolyarov, AV Ushakov, VG Gordon, IE AF Medvedev, Emile S. Meshkov, Vladimir V. Stolyarov, Andrey V. Ushakov, Vladimir G. Gordon, Iouli. E. TI Impact of the dipole-moment representation on the intensity of high overtones SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article DE NIDL; Spline; Numerov; sinc-DVR; sin-DVR ID DIATOMIC-MOLECULES; FOURIER COMPONENTS; MATRIX-ELEMENTS; GROUND-STATE; CO; SPECTRA; FIT AB Calculating intensities of ro-vibrational transitions is particularly challenging for transitions from a given vibrational state to all upper states up to the dissociation limit because their probabilities decrease exponentially with increasing An, the change in the vibrational quantum number. The experimental intensities available for low-An values are well reproduced by a variety of models but the models can greatly diverge in predicting the intensities of unobserved high-overtone transitions, the divergence rapidly increasing with the overtone number. In this paper, we investigate the impact of the dipole-moment function (DMF) representation on the high-overtone intensity simulation of the CO molecule. We tested various DMF forms including pointwise representation combined with cubic-spline interpolation, power and trigonometric expansions, and Fade approximants. Numerical calculations were performed with the highly accurate empirical potential-energy function (PEF) of Coxon and Hajigeorgiou (2004) using quadruple-precision arithmetic. Most calculated intensities fall off in the entire range of transitions according to the Normal Intensity Distribution Law (NIDL) (Medvedev, 2012). The slope of the NIDL trend line varies little between different analytical DMFs for a given PEF since the slope is basically associated with the PEF. Based on the NIDL, the limits within which the simulated intensities fall off up to the dissociation limit can be established. We claim that DMFs represented by analytical functions yield best results for all transitions. The pointwise functions (interpolated, in particular, by the conventional cubic splines) result in an unphysical flattening of the intensities at high-Delta n transitions, Delta n > 7 for CO. (C) 2016 Elsevier Inc. All rights reserved. C1 [Medvedev, Emile S.; Ushakov, Vladimir G.] Russian Acad Sci, Inst Problems Chem Phys, Prospect Akad Semenova 1, Chernogolovka 142432, Russia. [Meshkov, Vladimir V.; Stolyarov, Andrey V.] Lomonosov Moscow State Univ, Dept Chem, Leninskie Gory 1-3, Moscow 119991, Russia. [Gordon, Iouli. E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. RP Medvedev, ES (reprint author), Russian Acad Sci, Inst Problems Chem Phys, Prospect Akad Semenova 1, Chernogolovka 142432, Russia. EM esmedved@orc.ru RI Stolyarov, Andrey/H-7207-2012; OI Medvedev, Emile/0000-0002-4415-6926; Stolyarov, Andrey/0000-0001-7046-7202 FU Russian Foundation for Basic Research [15-03-03302a, 16-03-00526a]; NASA Planetary atmospheres grant [NNX13AI59G] FX It is our great pleasure to contribute to this special issue. Prof. Le Roy's influence on the field and underlying science is gratefully acknowledged. This work is financially supported by the Russian Foundation for Basic Research (grants 15-03-03302a and 16-03-00526a). IEG contribution is supported by the NASA Planetary atmospheres grant (No. NNX13AI59G). NR 41 TC 1 Z9 1 U1 3 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0022-2852 EI 1096-083X J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD DEC PY 2016 VL 330 SI SI BP 36 EP 42 DI 10.1016/j.jms.2016.06.013 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA EF9EX UT WOS:000390634600006 ER PT J AU Garriga, JA Ubelaker, DH Zapico, SC AF Garriga, Joe Adserias Ubelaker, Douglas H. Zapico, Sara C. TI Evaluation of macroscopic changes and the efficiency of DNA profiling from burnt teeth SO SCIENCE & JUSTICE LA English DT Article DE Forensic odontology; Burnt teeth; Macroscopic changes; DNA isolation; STR profiling; Housekeeping genes ID SEX DETERMINATION; DIAGNOSTIC-TOOL; BONE; IDENTIFICATION; FINGERPRINTS; REMAINS; REPEAT; PULP AB Identification of human remains subjected to incineration is extremely challenging. Our study evaluates the macroscopic changes and efficiency of DNA profiling in burnt teeth under controlled temperature and time conditions. 28 teeth were exposed to temperatures between 100 and 700 degrees C for a duration of 1-15 min. Two non burnt teeth were used as control. Macroscopic changes were evaluated and recorded. DNA was extracted using a silica-based methodology. Efficiency of DNA profiling was assessed through Quantitative PCR for STRs. Burnt teeth reached chalky white appearance at 400 degrees C 5 min and fractures were observed from 300 degrees C 10 min. Amplification of STRs was very low from 300 degrees C and 1 or 5 min. In contrast, the housekeeping gene, GAPDH, was amplified in all combinations of temperatures and times. Although it is possible to amplify the housekeeping gene at high temperature, DNA profiling is difficult to obtain, probably due to small size of these regions making them more prone to degradation. (C) 2016 The Chartered Society of Forensic Sciences. Published by Elsevier Ireland Ltd. All rights reserved. C1 [Garriga, Joe Adserias] Univ Girona, Emili Grahit 77, Girona, Cataluna, Spain. [Ubelaker, Douglas H.; Zapico, Sara C.] Smithsonian Inst, NMNH, Dept Anthropol, MRC 112,10th & Constitut Ave,NW,POB 37012, Washington, DC 20560 USA. RP Zapico, SC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, MRC 112,10th & Constitut Ave,NW,POB 37012, Washington, DC 20013 USA. EM saiczapico@gmail.com FU Smithsonian Institution FX Sara C. Zapico was supported by Peter Buck postdoctoral fellowship from Smithsonian Institution. The authors acknowledge Laboratories of Analytical Biology and Paleobiology Lab from Smithsonian Institution for providing the space and equipment to develop this work. Also, the authors thank Antonio Alvarez, from HURLE, S.L, for providing the equipment to burn the teeth. For her technical assistance, the authors acknowledge Rebecca Stone Gordon from American University. For editing the manuscript, the authors acknowledge Christian Thomas of the Smithsonian Institution. NR 25 TC 0 Z9 0 U1 4 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1355-0306 EI 1876-4452 J9 SCI JUSTICE JI Sci. Justice PD DEC PY 2016 VL 56 IS 6 BP 437 EP 442 DI 10.1016/j.scijus.2016.06.006 PG 6 WC Medicine, Legal; Pathology SC Legal Medicine; Pathology GA EG1WI UT WOS:000390823900005 PM 27914550 ER PT J AU Haussermann, V Forsterra, G Cairns, S AF Haussermann, Verena Forsterra, Gunter Cairns, Stephen TI New record of the primnoid gorgonian Primnoella delicatissima Kukenthal, 1909 for Chilean waters SO SPIXIANA LA English DT Editorial Material ID OCTOCORALLIA; ANTHOZOA C1 [Haussermann, Verena; Forsterra, Gunter] Pontificia Univ Catolica Valparaiso, Fac Recursos Nat, Escuela Ciencias Mar, Avda Brasil 2950, Valparaiso, Chile. [Cairns, Stephen] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst W329, POB 37012, Washington, DC 20560 USA. RP Haussermann, V (reprint author), Pontificia Univ Catolica Valparaiso, Fac Recursos Nat, Escuela Ciencias Mar, Avda Brasil 2950, Valparaiso, Chile. EM v.haussermann@gmail.com NR 9 TC 0 Z9 0 U1 0 U2 0 PU VERLAG DR FRIEDRICH PFEIL PI MUNICH PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY SN 0341-8391 J9 SPIXIANA JI Spixiana PD DEC PY 2016 VL 39 IS 2 BP 147 EP 148 PG 2 WC Biology; Zoology SC Life Sciences & Biomedicine - Other Topics; Zoology GA EG2AE UT WOS:000390834700002 ER PT J AU Neiss, M Sholts, SB Warmlander, SKTS AF Neiss, Michael Sholts, Sabrina B. Warmlander, Sebastian K. T. S. TI New applications of 3D modeling in artefact analysis: three case studies of Viking Age brooches SO ARCHAEOLOGICAL AND ANTHROPOLOGICAL SCIENCES LA English DT Article DE 3D laser scanner; Archaeometry; Artefact autopsy; Digital reconstruction; Scandinavian studies ID LASER-SCANNING TECHNOLOGY AB Three-dimensional (3D) laser scanning is a nondestructive and versatile technique that provides archaeologists with 3D models of archaeological and ethnographic objects. We have previously shown that 3D models facilitate shape analysis of archaeological bones and stone tools, due to the high measurement accuracy inherent in the latest generation of 3D laser scanners. Here, we explore the utility of 3D modeling as a tool for analyzing Viking Age metal artefacts with complex morphologies. Four highly ornate Viking Age brooches from Scandinavia and Russia were digitized with a portable laser scanner, and the resulting 3D models were used in three case studies of (a) artefact reconstruction, (b) tool mark analysis, and (c) motif documentation. The results revealed both strengths and limitations of the employed techniques. 3D modeling proved to be very well suited for artefact reconstruction and was helpful also in the stylistic and motif analysis. The tool mark analysis was only partially successful, due to the resolution limits of the laser scanner used. 3D-based motif analysis of a grandiose Scandinavian-style brooch from Yelets, Russia, identified an anthropomorphic figure with a bird-like body that previously has been overlooked. This figure may be a Rurikid coat of arms, possibly linking the object to a princely household and providing further evidence for a connection between Scandinavia and the Rurikids. As 3D technology keeps improving, we expect that additional applications for 3D modeling in archaeology will be developed, likely leading to many new findings when old objects are re-analyzed with modern techniques. However, our results indicate that 3D modeling cannot completely replace traditional artefact analysis-instead, we argue that the two approaches are best used in combination. C1 [Neiss, Michael] Uppsala Univ, Dept Archaeol & Ancient Hist, S-75105 Uppsala, Sweden. [Sholts, Sabrina B.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Warmlander, Sebastian K. T. S.] Stockholm Univ, Div Biophys, S-10691 Stockholm, Sweden. [Warmlander, Sebastian K. T. S.] Univ Calif Los Angeles, UCLA Getty Conservat Program, Cotsen Inst Archaeol, Los Angeles, CA USA. RP Warmlander, SKTS (reprint author), Stockholm Univ, Div Biophys, S-10691 Stockholm, Sweden. EM michaelneiss@hotmail.com; SholtsS@si.edu; seb@dbb.su.se FU Helge Ax:son Johnson Foundation; Swedish Institute, Svenska fornminnesforeningen; Royal Swedish Academy of Letters, History and Antiquities FX We thank Rafael Minasyan and Ekatarina Arnoldovna Shablavina at the Hermitage State Museum in St. Petersburg; Jytte Hostmark, Poul Otto Nielsen, Helga Schutze, Lars Jorgensen, and Peter Vang Petersen at the National Museum in Copenhagen; and Lotta Fernstal, Charlotte Hedenstierna Jonson, and Inga Ullen at the Swedish History Museum in Stockholm for their help in studying the original brooches. Natalia Eniosova at Moscow University and Vasily V. Novikov at the Gardarika Historical and Archaeological Centre generously provided information regarding the Gnezdovo hoard. Ole Thirup Kastholm at Roskilde Museum and Maria Panum Baastrup at the National Museum in Copenhagen equally generously provided information on the Vestervang brooch. Eva Hjarthner-Holdar and Yang Sook Koh at the National Heritage Board of Sweden kindly shared their metallurgical expertise with us. The project was financially supported by The Helge Ax:son Johnson Foundation, The Swedish Institute, Svenska fornminnesforeningen, and The Royal Swedish Academy of Letters, History and Antiquities. NR 41 TC 0 Z9 0 U1 9 U2 9 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1866-9557 EI 1866-9565 J9 ARCHAEOL ANTHROP SCI JI Archaeol. Anthropol. Sci. PD DEC PY 2016 VL 8 IS 4 SI SI BP 651 EP 662 DI 10.1007/s12520-014-0200-9 PG 12 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA EF0KX UT WOS:000390015400002 ER PT J AU Bannister, MT Alexandersen, M Benecchi, SD Chen, YT Delsanti, A Fraser, WC Gladman, BJ Granvik, M Grundy, WM Guilbert-Lepoutre, A Gwyn, SDJ Ip, WH Jakubik, M Jones, RL Kaib, N Kavelaars, JJ Lacerda, P Lawler, S Lehner, MJ Lin, HW Lykawka, PS Marsset, M Murray-Clay, R Noll, KS Parker, A Petit, JM Pike, RE Rousselot, P Schwamb, ME Shankman, C Veres, P Vernazza, P Volk, K Wang, SY Weryk, R AF Bannister, Michele T. Alexandersen, Mike Benecchi, Susan D. Chen, Ying-Tung Delsanti, Audrey Fraser, Wesley C. Gladman, Brett J. Granvik, Mikael Grundy, Will M. Guilbert-Lepoutre, Aurelie Gwyn, Stephen D. J. Ip, Wing-Huen Jakubik, Marian Jones, R. Lynne Kaib, Nathan Kavelaars, J. J. Lacerda, Pedro Lawler, Samantha Lehner, Matthew J. Lin, Hsing Wen Lykawka, Patryk Sofia Marsset, Michael Murray-Clay, Ruth Noll, Keith S. Parker, Alex Petit, Jean-Marc Pike, Rosemary E. Rousselot, Philippe Schwamb, Megan E. Shankman, Cory Veres, Peter Vernazza, Pierre Volk, Kathryn Wang, Shiang-Yu Weryk, Robert TI OSSOS. IV. DISCOVERY OF A DWARF PLANET CANDIDATE IN THE 9:2 RESONANCE WITH NEPTUNE SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper belt objects: individual (2015 RR245) ID KUIPER-BELT OBJECTS; OUTER SOLAR-SYSTEM; SCATTERED DISK; DYNAMICAL INSTABILITY; SIZE DISTRIBUTION; OORT CLOUD; SKY SURVEY; POPULATION; ORIGIN; RADIUS AB We report the discovery and orbit of a new dwarf planet candidate, 2015 RR245, by the Outer Solar System Origins Survey (OSSOS). The orbit of 2015 RR245 is eccentric (e = 0.586), with a semimajor axis near 82 au, yielding a perihelion distance of 34 au. 2015 RR245 has g - r = 0.59 +/- 0.11 and absolute magnitude H-r = 3.6 +/- 0.1; for an assumed albedo of p(V) = 12%, the object has a diameter of similar to 670. km. Based on astrometric measurements from OSSOS and Pan-STARRS1, we find that 2015 RR245 is securely trapped on ten-megayear timescales in the 9: 2 mean-motion resonance with Neptune. It is the first trans-Neptunian object (TNO) identified in this resonance. On hundred-megayear. timescales, particles in 2015 RR245-like orbits depart and sometimes return to the resonance, indicating that 2015 RR245 likely forms part of the long-lived metastable population of distant TNOs that drift between resonance sticking and actively scattering via gravitational encounters with Neptune. The discovery of a 9: 2 TNO stresses the role of resonances in the long-term evolution of objects in the scattering disk. and reinforces the view that distant resonances are heavily populated in the current solar system. This object further motivates detailed modeling of the transient sticking population. C1 [Bannister, Michele T.; Kavelaars, J. J.; Pike, Rosemary E.; Shankman, Cory] Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada. [Alexandersen, Mike; Chen, Ying-Tung; Lehner, Matthew J.; Pike, Rosemary E.; Wang, Shiang-Yu] Acad Sinica, Inst Astron & Astrophys, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan. [Alexandersen, Mike; Chen, Ying-Tung; Lehner, Matthew J.; Pike, Rosemary E.; Wang, Shiang-Yu] Natl Taiwan Univ, AS NTU 11F, 1 Roosevelt Rd,Sec 4, Taipei 10617, Taiwan. [Benecchi, Susan D.] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. [Delsanti, Audrey; Marsset, Michael; Vernazza, Pierre] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Bannister, Michele T.; Fraser, Wesley C.; Lacerda, Pedro] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Gladman, Brett J.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC, Canada. [Granvik, Mikael] Univ Helsinki, Dept Phys, POB 64, FIN-00014 Helsinki, Finland. [Grundy, Will M.] Lowell Observ, Flagstaff, AZ USA. [Guilbert-Lepoutre, Aurelie; Petit, Jean-Marc; Rousselot, Philippe] Univ Bourgogne Franche Comte, CNRS, Inst UTINAM,OSU Theta, UMR6213, F-25000 Besancon, France. [Bannister, Michele T.; Gwyn, Stephen D. J.; Kavelaars, J. J.; Lawler, Samantha] Natl Res Council Canada, NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. [Ip, Wing-Huen; Lin, Hsing Wen] Natl Cent Univ, Inst Astron, Taoyuan, Taiwan. [Ip, Wing-Huen] Macau Univ Sci & Technol, Space Sci Inst, Taipa, Macau, Peoples R China. [Jakubik, Marian] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Jones, R. Lynne] Univ Washington, Washington, DC USA. [Kaib, Nathan] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Lehner, Matthew J.] Univ Penn, Dept Phys & Astron, 209 S 33rd St, Philadelphia, PA 19104 USA. [Lehner, Matthew J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lykawka, Patryk Sofia] Kindai Univ, Sch Interdisciplinary Social & Human Sci, Astron Grp, Higashiosaka, Osaka, Japan. [Marsset, Michael] ESO, Alonso Cordova 3107,1900 Casilla Vitacura, Santiago, Chile. [Murray-Clay, Ruth] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Noll, Keith S.] NASA, Goddard Space Flight Ctr, Code 693, Greenbelt, MD 20771 USA. [Parker, Alex] Southwest Res Inst, Boulder, CO USA. [Schwamb, Megan E.] Northern Operat Ctr, Gemini Observ, 670 North Aohuku Pl, Hilo, HI 96720 USA. [Veres, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Volk, Kathryn] Univ Arizona, Lunar & Planetary Lab, Dept Planetary Sci, 1629 E Univ Blvd, Tucson, AZ 85721 USA. [Weryk, Robert] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. RP Bannister, MT (reprint author), Univ Victoria, Dept Phys & Astron, Elliott Bldg,3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada.; Bannister, MT (reprint author), Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland.; Bannister, MT (reprint author), Natl Res Council Canada, NRC Herzberg Astron & Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. EM michele.t.bannister@gmail.com OI Sofia Lykawka, Patryk/0000-0003-0926-2448 FU National Research Council of Canada; National Science and Engineering Research Council of Canada; Gemini Observatory; Slovak Grant Agency for Science [2/0031/14] FX This research was supported by funding from the National Research Council of Canada and the National Science and Engineering Research Council of Canada. The authors recognize and acknowledge the sacred nature of Maunakea. and appreciate the opportunity to observe from the mountain. This project could not have been a success without the dedicated staff of the Canada-France-Hawaii Telescope (CFHT) telescope. This work is based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA. CFHT is operated by the National Research Council of Canada, the Institute National des Sciences de l'universe of the Centre National de la Recherche Scientifique of France, and the University of Hawaii, with OSSOS receiving additional access due to contributions from the Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan. This work is based in part on data produced and hosted at the Canadian Astronomy Data Centre, with data processing and analysis performed using computing and storage capacity provided by the Canadian Advanced Network For Astronomy Research (CANFAR). MES was supported by the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., on behalf of the international Gemini partnership of Argentina, Brazil, Canada, Chile, and the United States of America. MJ acknowledges support from the Slovak Grant Agency for Science (grant no. 2/0031/14). NR 52 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 212 DI 10.3847/0004-6256/152/6/212 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF5AA UT WOS:000390341900004 ER PT J AU Hutchinson, TA Bolton, AS Dawson, KS Prieto, CA Bailey, S Bautista, JE Brownstein, JR Conroy, C Guy, J Myers, AD Newman, JA Prakash, A Carnero-Rosell, A Seo, HJ Tojeiro, R Vivek, M Ben Zhu, G AF Hutchinson, Timothy A. Bolton, Adam S. Dawson, Kyle S. Allende Prieto, Carlos Bailey, Stephen Bautista, Julian E. Brownstein, Joel R. Conroy, Charlie Guy, Julien Myers, Adam D. Newman, Jeffrey A. Prakash, Abhishek Carnero-Rosell, Aurelio Seo, Hee-Jong Tojeiro, Rita Vivek, M. Ben Zhu, Guangtun TI REDSHIFT MEASUREMENT AND SPECTRAL CLASSIFICATION FOR eBOSS GALAXIES WITH THE REDMONSTER SOFTWARE SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: data analysis; surveys; techniques: spectroscopic ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; INITIAL MASS FUNCTION; 1ST DATA RELEASE; SDSS-III; CHEMICAL-COMPOSITION; TARGET SELECTION; DATA REDUCTION; FINAL DATA; EVOLUTION AB We describe the redmon ster automated redshift measurement and spectral classification software designed for the extended Baryon Oscillation Spectroscopic Survey (eBOSS) of the Sloan Digital Sky Survey IV (SDSS-IV). We describe the algorithms, the template standard and requirements, and the newly developed galaxy templates to be used on eBOSS spectra. We present results from testing on early data from eBOSS, where we have found a 90.5% automated redshift and spectral classification success rate for the luminous red galaxy sample (redshifts 0.6 less than or similar to z less than or similar to 1.0). The redmon ster performance meets the eBOSS cosmology requirements for redshift classification and catastrophic failures and represents a significant improvement over the previous pipeline. We describe the empirical processes used to determine the optimum number of additive polynomial terms in our models and an acceptable Delta chi(2)(r) threshold for declaring statistical confidence. Statistical errors on redshift measurement due to photon shot noise are assessed, and we find typical values of a few tens of km s(-1). An investigation of redshift differences in repeat observations scaled by error estimates yields a distribution with a Gaussian mean and standard deviation of mu similar to 0.01 and sigma similar to 0.65, respectively, suggesting the reported statistical redshift uncertainties are over-estimated by similar to 54%. We assess the effects of object magnitude, signal-to-noise ratio, fiber number, and fiber head location on the pipeline's redshift success rate. Finally, we describe directions of ongoing development. C1 [Hutchinson, Timothy A.; Bolton, Adam S.; Dawson, Kyle S.; Bautista, Julian E.; Brownstein, Joel R.; Vivek, M.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Bolton, Adam S.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Allende Prieto, Carlos] Inst Astrofis Canarias, Via Lactea, E-38205 Tenerife, Spain. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Bailey, Stephen] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Guy, Julien] Univ Denis Diderot Paris 7, Univ Pierre & Marie Curie Paris 6, IN2P3, LPNHE,CNRS, 4 Pl Jussieu, F-75252 Paris, France. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Newman, Jeffrey A.; Prakash, Abhishek] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Newman, Jeffrey A.; Prakash, Abhishek] Univ Pittsburgh, PITT PACC, Pittsburgh, PA 15260 USA. [Carnero-Rosell, Aurelio] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero-Rosell, Aurelio] LIneA, Lab Interinst E Astron, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Seo, Hee-Jong] Ohio Univ, Dept Phys & Astron, 251B Clippinger Labs, Athens, OH 45701 USA. [Tojeiro, Rita] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Ben Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. RP Hutchinson, TA (reprint author), Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. EM t.hutchinson@utah.cdu FU Alfred P. Sloan Foundation; Center for High-Performance Computing at the University of Utah; Brazilian Participation Group; Carnegie Institution for Science; Carnegie Mellon University; Chilean Participation Group; Harvard-Smithsonian Center for Astrophysics; Instituto de AstrofIsica de Canarias; Johns Hopkins University; Kavli Institute for the Physics and Mathematics of the universe (IPMU)/University of Tokyo; Lawrence Berkeley National Laboratory; Leibniz Institut fur Astrophysik Potsdam (AIP); Max-Planck-Institut fur Astrophysik (MPA Garching); Max-Planck-Institut fur Extraterrestrische Physik (MPE); Max-Planck-Institut fur Astronomie (MPIA Heidelberg); National Astronomical Observatory of China; New Mexico State University; New York University; University of Notre Dame; Observatorio Nacional do Brasil; Ohio State University; Pennsylvania State University; Shanghai Astronomical Observatory; United Kingdom Participation Group; Universidad Nacional Autonoma de Mexico; University of Arizona; University of Colorado Boulder; University of Portsmouth; University of Utah; University of Washington; University of Wisconsin; Vanderbilt University; Yale University; U.S. Department of Energy, Office of Science, Office of High Energy Physics [DE-SC0010331, DE-SC0009959, DE-SC0007914] FX Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org.; SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de AstrofIsica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur Astrophysik (MPA Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE), Max-Planck-Institut fur Astronomie (MPIA Heidelberg), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatorio Nacional do Brasil, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autonoma de Mexico, University of Arizona, University of Colorado Boulder, University of Portsmouth, University of Utah, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.; The work of T.H., A.B., K.D., J.B., and M.V. was supported in part by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under Award Numbers DE-SC0010331 and DE-SC0009959, and that of J.N. and A.P. under Award Number DE-SC0007914. NR 51 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 205 DI 10.3847/0004-6256/152/6/205 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF5HK UT WOS:000390361100003 ER PT J AU Line, MR Stevenson, KB Bean, J Desert, JM Fortney, JJ Kreidberg, L Madhusudhan, N Showman, AP Diamond-Lowe, H AF Line, Michael R. Stevenson, Kevin B. Bean, Jacob Desert, Jean-Michel Fortney, Jonathan J. Kreidberg, Laura Madhusudhan, Nikku Showman, Adam P. Diamond-Lowe, Hannah TI NO THERMAL INVERSION AND A SOLAR WATER ABUNDANCE FOR THE HOT JUPITER HD 209458B FROM HST/WFC3 SPECTROSCOPY SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: statistical; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: gaseous planets; planets and satellites: individual (HD 209458b); techniques: spectroscopic ID HUBBLE-SPACE-TELESCOPE; NICMOS TRANSMISSION SPECTROSCOPY; SYSTEMATIC RETRIEVAL ANALYSIS; EXTRASOLAR GIANT PLANETS; FIELD CAMERA 3; SECONDARY ECLIPSE; EMISSION-SPECTRA; EXOPLANET ATMOSPHERE; MU-M; IRRADIATED ATMOSPHERES AB The nature of the thermal structure of hot Jupiter atmospheres is one of the key questions raised by the characterization of transiting exoplanets over the past decade. There have been claims that many hot Jupiters exhibit atmospheric thermal inversions. However, these claims have been based on broadband photometry rather than the unambiguous identification of emission features with spectroscopy, and the chemical species that could cause the thermal inversions by absorbing stellar irradiation at high altitudes have not been identified despite extensive theoretical and observational effort. Here we present high-precision Hubble Space Telescope WFC3 observations of the dayside thermal emission spectrum of the hot Jupiter HD 209458b, which was the first exoplanet suggested to have a thermal inversion. In contrast to previous results for this planet, our observations detect water in absorption at 6.2 sigma confidence. When combined with Spitzer photometry, the data are indicative of a monotonically decreasing temperature with pressure over the range of 1-0.001 bars at 7.7 sigma confidence. We test the robustness of our results by exploring a variety of model assumptions, including the temperature profile parameterization, presence of a cloud, and choice of Spitzer data reduction. We also introduce a new analysis method to determine the elemental abundances from the spectrally retrieved mixing ratios with thermochemical self-consistency and find plausible abundances consistent with solar metallicity (0.06-10 x solar) and carbon-to oxygen ratios less than unity. This work suggests that high-precision spectrophotometric results are required to robustly infer thermal structures and compositions of extrasolar planet atmospheres and to perform comparative exoplanetology. C1 [Line, Michael R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Line, Michael R.] Bay Area Environm Res Inst, 625 2nd St,Suite 209, Petaluma, CA 94952 USA. [Line, Michael R.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Stevenson, Kevin B.; Bean, Jacob; Kreidberg, Laura] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Desert, Jean-Michel] Univ Amsterdam, NL-1012 WX Amsterdam, Netherlands. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Showman, Adam P.] Univ Arizona, Dept Planetary Sci, 1629 E Univ Blvd, Tucson, AZ 85721 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. [Diamond-Lowe, Hannah] Harvard Smithsonian Ctr Astrophys, Dept Astron, 60 Garden St,MS-10, Cambridge, MA 02138 USA. RP Line, MR (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA.; Line, MR (reprint author), Bay Area Environm Res Inst, 625 2nd St,Suite 209, Petaluma, CA 94952 USA.; Line, MR (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. FU GO Treasury Program [13467]; NASA [NAS 5-26555]; David and Lucile Packard Foundation; NASA - Space Telescope Science Institute [51362]; NASA Exoplanet Science Institute Sagan Postdoctoral Fellowship FX These observations were made under the GO Treasury Program 13467 with the NASA/ESA Hubble Space Telescope at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under the contract NAS 5-26555. M.R.L. acknowledges support provided by NASA through Hubble Fellowship grant 51362 awarded by the Space Telescope Science Institute. K.B.S. acknowledges support from the NASA Exoplanet Science Institute Sagan Postdoctoral Fellowship. J.L.B. acknowledges support from the David and Lucile Packard Foundation. We also thank Dan Foreman-Mackey for making the corner.py plotting routine available to the public and Johannes Buchner for making pymultinest publicly available. We also thank Vivien Parmentier, Kevin Heng, Tom Evans, Drake Deming, Adam Burrows, and Heather Knutson for useful discussion and comments on the manuscript. We thank Drake Deming, Peter McCullough, Adam Burrows, Sara Seager, David Charbonneau, and Derek Homeier for being co-investigators on the HST observing proposal. Finally, we thank Roxana Lupu for support with the molecular absorption cross sections. NR 110 TC 3 Z9 3 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 203 DI 10.3847/0004-6256/152/6/203 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF5HK UT WOS:000390361100001 ER PT J AU Lopez-Morales, M Haywood, RD Coughlin, JL Zeng, L Buchhave, LA Giles, HAC Affer, L Bonomo, AS Charbonneau, D Cameron, AC Consentino, R Dressing, CD Dumusque, X Figueira, P Fiorenzano, AFM Harutyunyan, A Johnson, JA Latham, DW Lopez, ED Lovis, C Malavolta, L Mayor, M Micela, G Molinari, E Mortier, A Motalebi, F Nascimbeni, V Pepe, F Phillips, DF Piotto, G Pollacco, D Queloz, D Rice, K Sasselov, D Segransan, D Sozzetti, A Udry, S Vanderburg, A Watson, C AF Lopez-Morales, Mercedes Haywood, Raphaelle D. Coughlin, Jeffrey L. Zeng, Li Buchhave, Lars A. Giles, Helen A. C. Affer, Laura Bonomo, Aldo S. Charbonneau, David Cameron, Andrew Collier Consentino, Rosario Dressing, Courtney D. Dumusque, Xavier Figueira, Pedro Fiorenzano, Aldo F. M. Harutyunyan, Avet Johnson, John Asher Latham, David W. Lopez, Eric D. Lovis, Christophe Malavolta, Luca Mayor, Michel Micela, Giusi Molinari, Emilio Mortier, Annelies Motalebi, Fatemeh Nascimbeni, Valerio Pepe, Francesco Phillips, David F. Piotto, Giampaolo Pollacco, Don Queloz, Didier Rice, Ken Sasselov, Dimitar Segransan, Damien Sozzetti, Alessandro Udry, Stephane Vanderburg, Andrew Watson, Chris TI KEPLER-21b: A ROCKY PLANET AROUND A V=8.25 mag STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: formation; planets and satellites: individual (Kepler-21b); stars:individual (HD 179070); techniques: photometric; techniques: radial velocities; techniques: spectroscopic ID SOLAR-TYPE STARS; HARPS-N; GAPS PROGRAM; STELLAR ACTIVITY; EMISSION-SPECTRUM; TRANSITING PLANET; SUPER-EARTHS; RED GIANTS; MASS-LOSS; SYSTEM AB HD 179070, aka Kepler-21, is a V = 8.25 F6IV star and the brightest exoplanet host discovered by Kepler. An early detailed analysis by Howell et al. of the first 13 months (Q0-Q5) of Kepler light curves revealed transits of a planetary companion, Kepler-21b, with a radius of about 1.60 +/- 0.04 R(circle plus)and an orbital period of about 2.7857 days. However, they could not determine the mass of the planet from the initial radial velocity (RV) observations with Keck-HIRES, and were only able to impose a 2 sigma upper limit of 10 M-circle plus. Here, we present results from the analysis of 82 new RV observations of this system obtained with HARPS-N, together with the existing 14 HIRES data points. We detect the Doppler signal of Kepler-21b with a RV semiamplitude K = 2.00 +/- 0.65 m s(-1), which corresponds to a planetary mass of 5.1 +/- 1.7 M-circle plus. We also measure an improved radius for the planet of 1.639 +0.019/-0.015 R-circle plus, in agreement with the radius reported by Howell et al. We conclude that Kepler-21b, with a density of 6.4 +/- 2.1 g cm(-3), belongs to the population of small, less than or similar to 6 Me planets with iron and magnesium silicate interiors, which have lost the majority of their envelope volatiles via stellar winds or gravitational escape. The RV analysis presented in this paper serves as an example of the type of analysis that will be necessary to confirm the masses of TESS small planet candidates. C1 [Lopez-Morales, Mercedes; Haywood, Raphaelle D.; Charbonneau, David; Johnson, John Asher; Latham, David W.; Phillips, David F.; Sasselov, Dimitar; Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. [Coughlin, Jeffrey L.] SETI Inst, 189 Bernardo Ave Suite 200, Mountain View, CA 94043 USA. [Zeng, Li] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 01238 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-1350 Copenhagen, Denmark. [Giles, Helen A. C.; Dumusque, Xavier; Lovis, Christophe; Mayor, Michel; Motalebi, Fatemeh; Pepe, Francesco; Queloz, Didier; Segransan, Damien; Udry, Stephane] Univ Geneva, Astron Observ, Chemin Maillettes 51, CH-1290 Sauverny, Switzerland. [Affer, Laura; Micela, Giusi] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90124 Palermo, Italy. [Bonomo, Aldo S.; Sozzetti, Alessandro] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy. [Cameron, Andrew Collier; Mortier, Annelies] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Consentino, Rosario; Fiorenzano, Aldo F. M.; Harutyunyan, Avet; Molinari, Emilio] INAF Fdn Galileo Galilei, Rambla Jose Ana Fernandez Perez 7, E-38712 Brena Alta, Spain. [Dressing, Courtney D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Figueira, Pedro] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Oporto, Portugal. [Lopez, Eric D.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3JH, Midlothian, Scotland. [Malavolta, Luca; Nascimbeni, Valerio; Piotto, Giampaolo] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy. [Malavolta, Luca; Piotto, Giampaolo] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Molinari, Emilio] INAF IASF Milano, Via Bassini 15, I-20133 Milan, Italy. [Pollacco, Don] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England. [Queloz, Didier] Cavendish Lab, JJ Thomson Ave, Cambridge CB3 0HE, England. [Watson, Chris] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Lopez-Morales, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. EM mlopez-morales@cfa.harvard.cdu RI Figueira, Pedro/J-4916-2013; Rice, Ken/H-5084-2011 OI Figueira, Pedro/0000-0001-8504-283X; Rice, Ken/0000-0002-6379-9185 FU Prodex Program of the Swiss Space Office (SSO); Harvard University Origins of Life Initiative (HUOLI); Scottish Universities Physics Alliance (SUPA); University of Geneva; Smithsonian Astrophysical Observatory (SAO); Italian National Astrophysical Institute (INAF); University of St. Andrews; Queens University Belfast; University of Edinburgh; John Templeton Foundation; National Aeronautics and Space Administration [NNX15AC9OG]; European Union Seventh Framework Programme (FP7) [313014]; NASA through the Sagan Fellowship Program; Fundacao para a Ciencias e a Tecnologia (FCT) through Investigador FCT [IF/01037/2013]; POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade COMPETE"; Simons Foundation (SCOL) [337090]; NSF Graduate Research Fellowship [DGE 1144152]; Society in Science-Branco Weiss Fellowship; [IF/01037/2013CP1191/CT0001] FX We thank the anonymous referee for helpful comments to the manuscript. The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), the University of St. Andrews, Queens University Belfast, and the University of Edinburgh. This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based upon work supported by the National Aeronautics and Space Administration under grant No. NNX15AC9OG issued through the Exoplanets Research Program. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant Agreement No. 313014 (ETAEARTH). This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. P.F. acknowledges support by Fundacao para a Ciencias e a Tecnologia (FCT) through Investigador FCT contract of reference IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade COMPETE", and further support in the form of an exploratory project of reference IF/01037/2013CP1191/CT0001. L.Z. is supported by a grant from the Simons Foundation (SCOL, award #337090). A.V. is supported by the NSF Graduate Research Fellowship, Grant No. DGE 1144152. X.D. is grateful to the Society in Science-Branco Weiss Fellowship for its financial support. NR 73 TC 0 Z9 0 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 204 DI 10.3847/0004-6256/152/6/204 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF5HK UT WOS:000390361100002 ER PT J AU Matthews, LD Marengo, M Evans, NR AF Matthews, L. D. Marengo, M. Evans, N. R. TI A SEARCH FOR MASS LOSS ON THE CEPHEID INSTABILITY STRIP USING H I 21 cm LINE OBSERVATIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; radio lines: stars; stars: mass-loss; stars: variables: Cepheids ID GIANT BRANCH STARS; GALACTIC-CEPHEIDS; CLASSICAL CEPHEIDS; CIRCUMSTELLAR ENVELOPES; T-MONOCEROTIS; RS PUPPIS; EXTENDED ENVELOPES; DELTA CEPHEI; L-CARINAE; MIDINFRARED INTERFEROMETRY AB We present the results of a search for H I 21 cm line emission from the circumstellar environments of four Galactic Cepheids (RS Pup, X Cyg, zeta Gem, and T Mon) based on observations with the Karl G. Jansky Very Large Array. The observations were aimed at detecting gas associated with previous or ongoing mass loss. Near the long-period Cepheid T Mon, we report the detection of a partial shell-like structure whose properties appear consistent with originating from an earlier epoch of Cepheid mass loss. At the distance of T Mon, the nebula would have a mass (HI+He) of similar to 0.5M(circle dot), or similar to 6% of the stellar mass. Assuming that one-third of the nebular mass comprises swept up interstellar gas, we estimate an implied mass-loss rate of M similar to (0.6-2) x 10(-5) M-circle dot yr(-1). No clear signatures of circumstellar emission were found toward zeta Gem, RS Pup, or X Cyg, although in each case, line-of-sight confusion compromised portions of the spectral band. For the undetected stars, we derive model-dependent 3 sigma upper limits on the mass-loss rates, averaged over their lifetimes on the instability strip, of less than or similar to(0.3-6) x 10(-6) M-circle dot yr(-1) and estimate the total amount of mass lost to be less than a few percent of the stellar mass. C1 [Matthews, L. D.] MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Evans, N. R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-42, Cambridge, MA 02138 USA. RP Matthews, LD (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM lmatthew@haystack.mit.edu FU National Science Foundation [AST-1310930]; Chandra X-Ray Center NASA [NAS8-03060]; NRAO program [AM1087 (VLA/11B-035)] FX L.D.M. is supported by grant AST-1310930 from the National Science Foundation. Support to N.R.E. was provided from the Chandra X-Ray Center NASA contract NAS8-03060. The observations presented here were part of NRAO program AM1087 (VLA/11B-035). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 79 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 200 DI 10.3847/0004-6256/152/6/200 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF5HI UT WOS:000390360900003 ER PT J AU Cheung, E Stark, DV Huang, S Rubin, KHR Lin, LW Tremonti, C Zhang, K Yan, R Bizyaev, D Boquien, M Brownstein, JR Drory, N Gelfand, JD Knapen, JH Maiolino, R Malanushenko, O Masters, KL Merrifield, MR Pace, Z Pan, K Riffel, RA Roman-Lopes, A Rujopakarn, W Schneider, DP Stott, JP Thomas, D Weijmans, AM AF Cheung, Edmond Stark, David V. Huang, Song Rubin, Kate H. R. Lin, Lihwai Tremonti, Christy Zhang, Kai Yan, Renbin Bizyaev, Dmitry Boquien, Mederic Brownstein, Joel R. Drory, Niv Gelfand, Joseph D. Knapen, Johan H. Maiolino, Roberto Malanushenko, Olena Masters, Karen L. Merrifield, Michael R. Pace, Zach Pan, Kaike Riffel, Rogemar A. Roman-Lopes, Alexandre Rujopakarn, Wiphu Schneider, Donald P. Stott, John P. Thomas, Daniel Weijmans, Anne-Marie TI SDSS-IV MaNGA: A SERENDIPITOUS OBSERVATION OF A POTENTIAL GAS ACCRETION EVENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: formation; galaxies: starburst ID DIFFUSE IONIZED-GAS; DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; ULTRA DEEP FIELD; H-II REGIONS; REDSHIFT CIRCUMGALACTIC MEDIUM; STELLAR POPULATION SYNTHESIS; LOCAL TADPOLE GALAXIES; LAMBDA-CDM UNIVERSE; ON SPIRAL GALAXIES AB The nature of warm, ionized gas outside of galaxies may illuminate several key galaxy evolutionary processes. A serendipitous observation by the MaNGA survey has revealed a large, asymmetric H alpha complex with no optical counterpart that extends approximate to 8 '' (approximate to 6.3 kpc) beyond the effective radius of a dusty, starbursting galaxy. This H alpha extension is approximately three times the effective radius of the host galaxy and displays a tail-like morphology. We analyze its gas- phase metallicities, gaseous kinematics, and emission- line ratios and discuss whether this Ha extension could be diffuse ionized gas, a gas accretion event, or something else. We find that this warm, ionized gas structure is most consistent with gas accretion through recycled wind material, which could be an important process that regulates the low- mass end of the galaxy stellar mass function. C1 [Cheung, Edmond; Stark, David V.; Huang, Song] Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Rubin, Kate H. R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Tremonti, Christy] Univ Wisconsin, Dept Astron, 475 North Charter St, Madison, WI 53706 USA. [Zhang, Kai; Yan, Renbin] Univ Kentucky, Dept Phys & Astron, 505 Rose St, Lexington, KY 40506 USA. [Bizyaev, Dmitry] Apache Point Observ, POB 59, Sunspot, NM 88349 USA. [Bizyaev, Dmitry] New Mexico State Univ, POB 59, Sunspot, NM 88349 USA. [Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow, Russia. [Boquien, Mederic] Univ Antofagasta, Unidad Astron, Ave Angamos 601, Antofagasta 1270300, Chile. [Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA. [Drory, Niv] Univ Texas Austin, Dept Astron, McDonald Observ, 1 Univ Stn, Austin, TX 78712 USA. [Gelfand, Joseph D.] NYU Abu Dhabi, POB 129188, Abu Dhabi, U Arab Emirates. [Gelfand, Joseph D.] New York Univ, Ctr Cosmol & Particle Phys, Meyer Hall Phys,4 Washington Pl, New York, NY 10003 USA. [Knapen, Johan H.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Knapen, Johan H.] Univ Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Maiolino, Roberto] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England. [Maiolino, Roberto] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Masters, Karen L.] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England. [Merrifield, Michael R.] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. [Riffel, Rogemar A.] Univ Fed Santa Maria, Dept Fis, Ctr Ciencias Nat & Exatas, BR-97105900 Santa Maria, RS, Brazil. [Riffel, Rogemar A.] Lab Interinstituc Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Roman-Lopes, Alexandre] Univ La Serena, Fac Ciencias, Dept Fis & Astron, Cisternas 1200, La Serena, Chile. [Rujopakarn, Wiphu] Chulalongkorn Univ, Dept Phys, Fac Sci, 254 Phayathai Rd, Bangkok 10330, Thailand. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Stott, John P.] Univ Oxford, Sub Dept Astrophys, Dept Phys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Weijmans, Anne-Marie] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Cheung, E (reprint author), Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. EM ec2250@gmail.com OI Rujopakarn, Wiphu/0000-0002-0303-499X; Bizyaev, Dmitry/0000-0002-3601-133X; Yan, Renbin/0000-0003-1025-1711; Lin, Lihwai/0000-0001-7218-7407; Huang, Song/0000-0003-1385-7591 FU Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science; Center for High-Performance Computing at the University of Utah; Leverhulme Early Career Fellowship; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA2013-41243-P]; Spanish Ministry of Education, Culture and Sports [PR2015-00512]; [RSCF-14-22-00041] FX Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS Web site is www.sdss.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration, including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrofisica de Canarias, Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut fur Astrophysik Potsdam (AIP), Max-Planck-Institut fur Astronomie (MPIA Heidelberg), Max-Planck-Institut fur Astrophysik (MPA Garching), Max-Planck-Institut fur Extraterrestrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatario Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autonoma de Mexico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. D.B. is supported by grant RSCF-14-22-00041. A.W. acknowledges support from a Leverhulme Early Career Fellowship. J.H.K. acknowledges financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant number AYA2013-41243-P and thanks the Astrophysics Research Institute of Liverpool John Moores University for their hospitality, and the Spanish Ministry of Education, Culture and Sports for financial support of his visit there, through grant number PR2015-00512. NR 103 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 182 DI 10.3847/0004-637X/832/2/182 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100042 ER PT J AU Fernandez-Lopez, M Stephens, IW Girart, JM Looney, L Curiel, S Segura-Cox, D Eswaraiah, C Lai, SP AF Fernandez-Lopez, M. Stephens, I. W. Girart, J. M. Looney, L. Curiel, S. Segura-Cox, D. Eswaraiah, C. Lai, S. -P. TI 1.3 mm POLARIZED EMISSION IN THE CIRCUMSTELLAR DISK OF A MASSIVE PROTOSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Cepheus A HW2); ISM: magnetic fields; polarization; stars: formation; techniques: polarimetric ID CEPHEUS-A HW2; YOUNG STELLAR OBJECTS; THERMAL RADIO JET; MAGNETIC-FIELDS; HIGH-RESOLUTION; GRAIN ALIGNMENT; IRAS 4A; HL TAU; STAR; DUST AB We present the first resolved observations of the 1.3 mm polarized emission from the disk-like structure surrounding the high-mass protostar Cepheus A HW2. These CARMA data partially resolve the dust polarization, suggesting a uniform morphology of polarization vectors with an average position angle of 57 degrees +/- 6 degrees and an average polarization fraction of 2.0% +/- 0.4%. The distribution of the polarization vectors can be attributed to (1) the direct emission of magnetically aligned grains of dust by a uniform magnetic field, or (2) the pattern produced by the scattering of an inclined disk. We show that both models can explain the observations, and perhaps a combination of the two mechanisms produces the polarized emission. A third model including a toroidal magnetic field does not match the observations. Assuming scattering is the polarization mechanism, these observations suggest that during the first few 10(4) years of high-mass star formation, grain sizes can grow from 1 mu m to several 10s mu m. C1 [Fernandez-Lopez, M.] CCT La Plata, Inst Argentino Radioastron CONICET, RA-1894 Villa Elisa, Argentina. [Stephens, I. W.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Stephens, I. W.; Girart, J. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Stephens, I. W.] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA. [Girart, J. M.] CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Cerdanyola Del Valls, Catalonia, Spain. [Looney, L.; Segura-Cox, D.] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA. [Curiel, S.] Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF, Mexico. [Eswaraiah, C.; Lai, S. -P.] Natl Tsing Hua Univ, Inst Astron, 101,Sect 2,Kuang Fu Rd, Hsinchu 30013, Taiwan. [Eswaraiah, C.; Lai, S. -P.] Natl Tsing Hua Univ, Dept Phys, 101,Sect 2,Kuang Fu Rd, Hsinchu 30013, Taiwan. RP Fernandez-Lopez, M (reprint author), CCT La Plata, Inst Argentino Radioastron CONICET, RA-1894 Villa Elisa, Argentina. EM manferna@gmail.edu OI Stephens, Ian/0000-0003-3017-4418 FU Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; state of Illinois; state of California; state of Maryland; National Science Foundation; CARMA partner universities; MICINN [AYA2014-57369-C3-P]; MECD (Spain) [PRX15/00435]; SICGPS "Magnetic Fields and Massive Star Formation" (USA) grants; NSF [1139950]; DGAPA; UNAM; CONACyT, Mexico; Ministry of Science and Technology(MoST) of Taiwan [MoST 102-2119-M-007-004-MY3] FX We thank all members of the CARMA staff that made these observations possible. Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, the states of Illinois, California, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. JMG acknowledges support from MICINN AYA2014-57369-C3-P, the MECD PRX15/00435 (Spain), and SICGPS "Magnetic Fields and Massive Star Formation" (USA) grants. LL is supported in part by the NSF grant 1139950. SC acknowledges support from DGAPA, UNAM, and CONACyT, Mexico. EC and SPL are thankful for the support of the Ministry of Science and Technology(MoST) of Taiwan through Grant MoST 102-2119-M-007-004-MY3. NR 53 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 200 DI 10.3847/0004-637X/832/2/200 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100060 ER PT J AU Reid, MJ Dame, TM AF Reid, M. J. Dame, T. M. TI ON THE ROTATION SPEED OF THE MILKY WAY DETERMINED FROM H I EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: kinematics and dynamics; Galaxy: fundamental parameters; Galaxy: structure; ISM: atoms ID BLACK-HOLE; GALACTIC-CENTER; STELLAR ORBITS; GALAXY; KINEMATICS; DISTANCE; CURVE; MASS AB The circular rotation speed of the Milky Way at the solar radius, Theta(0), has been estimated to be 220 km s(-1) by fitting the maximum velocity of H I emission as a function of Galactic longitude. This result is in tension with a recent estimate of Theta(0) = 240 km s(-1), based on Very Long Baseline Interferometry (VLBI) parallaxes and proper motions from the BeSSeL and VERA surveys for large numbers of high-mass star-forming regions across the Milky Way. We find that the rotation curve best fitted to the VLBI data is slightly curved, and that this curvature results in a biased estimate of Theta(0) from the H I data when a flat rotation curve is assumed. This relieves the tension between the methods and favors Theta(0) = 240 km s(-1). C1 [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Reid, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 16 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 159 DI 10.3847/0004-637X/832/2/159 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100019 ER PT J AU Santos, FP Busquet, G Franco, GAP Girart, JM Zhang, QZ AF Santos, Fabio P. Busquet, Gemma Franco, Gabriel A. P. Girart, Josep Miquel Zhang, Qizhou TI MAGNETICALLY DOMINATED PARALLEL INTERSTELLAR FILAMENTS IN THE INFRARED DARK CLOUD G14.225-0.506 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; evolution; ISM: individual objects (SDC G14.225-0.506); ISM: magnetic fields; stars: formation; techniques: polarimetric ID MASSIVE STAR-FORMATION; H-II REGIONS; MOLECULAR CLOUD; WAVELENGTH DEPENDENCE; LINEAR-POLARIZATION; PHYSICAL CONDITIONS; PRESTELLAR CORES; STELLAR FEEDBACK; GRAIN ALIGNMENT; GALACTIC PLANE AB The infrared dark cloud G14.225-0.506 (IRDC G14.2) displays a remarkable complex of parallel dense molecular filaments projected on the plane of the sky. Previous studies of dust emission and molecular lines have speculated whether magnetic fields could have played an important role in the formation of such elongated structures, which are hosts to numerous young stellar sources. In this work we have conducted a vast polarimetric survey at optical and near-infrared wavelengths in order to study the morphology of magnetic field lines in IRDC G14.2 through the observation of background stars. The orientation of interstellar polarization, which traces magnetic field lines, is perpendicular to most of the filamentary features within the cloud. Additionally, the larger-scale molecular cloud as a whole exhibits an elongated shape also perpendicular to magnetic fields. Estimates of magnetic field strengths indicate values in the range 320-550 mu G, which allow sub-alfvenic conditions, but do not prevent the gravitational collapse of hub-filament structures, which in general are close to the critical state. These characteristics suggest that magnetic fields played the main role in regulating the collapse from large to small scales, leading to the formation of series of parallel elongated structures. The morphology is also consistent with numerical simulations that show how gravitational instabilities develop when subjected to strong magnetic fields. Finally, the results corroborate the hypothesis that strong support from internal magnetic fields might explain why the cloud seems to be contracting on a timescale 2-3 times longer than what is expected from a free-fall collapse. C1 [Santos, Fabio P.] Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. [Busquet, Gemma; Girart, Josep Miquel] CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Bellaterra, Catalunya, Spain. [Franco, Gabriel A. P.] Univ Fed Minas Gerais, ICEx, Dept Fis, Caixa Postal 702, BR-30123970 Belo Horizonte, MG, Brazil. [Girart, Josep Miquel; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Santos, FP (reprint author), Northwestern Univ, Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM fabiops@northwestern.edu; busquet@ice.cat; franco@fisica.ufmg.br; girart@ice.cat; qzhang@cfa.harvard.edu RI Franco, Gabriel/A-8009-2011; OI Franco, Gabriel/0000-0003-2020-2649; Zhang, Qizhou/0000-0003-2384-6589 FU CNPq; CAPES [2397/13-7]; FAPEMIG; Spanish Ministerio de Economia y Competitividad (MINECO) [FPDI-2013-18204]; Spanish MICINN [AYA2011-30228-C03]; MINECO [AYA2014-57369-C3]; National Aeronautics and Space Administration; National Science Foundation; NASA FX We are grateful to the anonymous referee for valuable suggestions and comments. We thank the staff of OPD/LNA (Brazil) for their hospitality and invaluable help during our observing runs. G.A.P.F. and F.P.S. acknowledge support from the Brazilian agencies CNPq, CAPES, and FAPEMIG. F.P.S. was supported by the CAPES grant 2397/13-7. G.B. acknowledges the support from the Spanish Ministerio de Economia y Competitividad (MINECO) under grant FPDI-2013-18204. G.B. and J.M.G. are supported by the Spanish MICINN grant AYA2011-30228-C03 and the MINECO grant AYA2014-57369-C3. This investigation made extensive use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We are grateful to Drs. A. M. Magalhaes and A. Pereyra for providing the polarimetric unit and the software used for data reductions. NR 110 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 186 DI 10.3847/0004-637X/832/2/186 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100046 ER PT J AU Shukla, A Mannheim, K Chitnis, VR Roy, J Acharya, BS Dorner, D Hughes, G Biland, A AF Shukla, A. Mannheim, K. Chitnis, V. R. Roy, J. Acharya, B. S. Dorner, D. Hughes, G. Biland, A. TI DETECTION OF VERY HARD gamma-RAY SPECTRUM FROM THE TEV BLAZAR MRK 501 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (Mrk 501); galaxies: jets ID LARGE-AREA TELESCOPE; BLACK-HOLE; PARTICLE-ACCELERATION; ENERGY; RADIATION; ABSORPTION; EMISSION; FLARES; SCALES; SWIFT AB The occasional hardening of the GeV-to-TeV spectrum observed from the blazar Mrk 501 has reopened the debate on the physical origin of radiation and particle acceleration processes in TeV blazars. We have used the similar to 7 years of Fermi-LAT data to search for the time intervals with unusually hard spectra from the nearby TeV blazar Mrk 501. We detected hard spectral components above 10 GeV with photon index <1.5 at a significance level of more than 5 sigma on 17 occasions, each with 30 day integration time. The photon index of the hardest component reached a value of 0.89 +/- 0.29. We interpret these hard spectra as signatures of intermittent injection of sharply peaked and localized particle distributions from the base of the jet. C1 [Shukla, A.; Chitnis, V. R.; Acharya, B. S.] Tata Inst Fundamental Res, Dept High Energy Phys, Bombay 400005, Maharashtra, India. [Shukla, A.; Hughes, G.] ETH, Inst Particle Phys, Otto Stern Weg 5, CH-8093 Zurich, Switzerland. [Shukla, A.; Mannheim, K.; Dorner, D.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Roy, J.] UM DAE, Ctr Excellence Basic Sci, Bombay 400098, Maharashtra, India. [Dorner, D.] Univ Erlangen Nurnberg, Erlangen, Germany. [Hughes, G.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. RP Shukla, A (reprint author), Tata Inst Fundamental Res, Dept High Energy Phys, Bombay 400005, Maharashtra, India.; Shukla, A (reprint author), ETH, Inst Particle Phys, Otto Stern Weg 5, CH-8093 Zurich, Switzerland.; Shukla, A (reprint author), Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. NR 36 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 177 DI 10.3847/0004-637X/832/2/177 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100037 ER PT J AU Vantyghem, AN McNamara, BR Russell, HR Hogan, MT Edge, AC Nulsen, PEJ Fabian, AC Combes, F Salome, P Baum, SA Donahue, M Main, RA Murray, NW O'Connell, RW O'Dea, CP Oonk, JBR Parrish, IJ Sanders, JS Tremblay, G Voit, GM AF Vantyghem, A. N. McNamara, B. R. Russell, H. R. Hogan, M. T. Edge, A. C. Nulsen, P. E. J. Fabian, A. C. Combes, F. Salome, P. Baum, S. A. Donahue, M. Main, R. A. Murray, N. W. O'Connell, R. W. O'Dea, C. P. Oonk, J. B. R. Parrish, I. J. Sanders, J. S. Tremblay, G. Voit, G. M. TI MOLECULAR GAS ALONG A BRIGHT H alpha FILAMENT IN 2A 0335+096 REVEALED BY ALMA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: individual (2A 0335+096); galaxies: ISM; galaxies: kinematics and dynamics ID COOLING FLOW CLUSTERS; EARLY-TYPE GALAXIES; GALACTIC NUCLEUS FEEDBACK; RAY-LUMINOUS CLUSTERS; DEEP CHANDRA OBSERVATION; SUPERMASSIVE BLACK-HOLE; FLUX-LIMITED SAMPLE; X-RAY; STAR-FORMATION; PERSEUS CLUSTER AB We present ALMA CO(1-0) and CO(3-2) observations of the brightest cluster galaxy (BCG) in the 2A 0335+096 galaxy cluster (z = 0.0346). The total molecular gas mass of 1.13 +/- 0.15 x 10(9) M-circle dot is divided into two components: a nuclear region and a 7 kpc long dusty filament. The central molecular gas component accounts for 3.2 +/- 0.4 x 10(8) M-circle dot of the total supply of cold gas. Instead of forming a rotationally supported ring or disk, it is composed of two distinct, blueshifted clumps south of the nucleus and a series of low-significance redshifted clumps extending toward a nearby companion galaxy. The velocity of the redshifted clouds increases with radius to a value consistent with the companion galaxy, suggesting that an interaction between these galaxies <20 Myr ago disrupted a pre-existing molecular gas reservoir within the BCG. Most of the molecular gas, 7.8 +/- 0.9 x 10(8) M-circle dot, is located in the filament. The CO emission is co-spatial with a 10(4) K emission-line nebula and soft X-rays from 0.5 keV gas, indicating that the molecular gas has cooled out of the intracluster medium over a period of 25-100 Myr. The filament trails an X-ray cavity, suggesting that the gas has cooled from low-entropy gas that has been lifted out of the cluster core and become thermally unstable. We are unable to distinguish between inflow and outflow along the filament with the present data. Cloud velocities along the filament are consistent with gravitational free-fall near the plane of the sky, although their increasing blueshifts with radius are consistent with outflow. C1 [Vantyghem, A. N.; McNamara, B. R.; Hogan, M. T.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.; Hogan, M. T.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [Russell, H. R.; Fabian, A. C.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Nulsen, P. E. J.] Univ Western Australia, ICRAR, 35 Stirling Hwy, Crawley, WA 6009, Australia. [Combes, F.; Salome, P.] UPMC, PSL Univ, CNRS, LERMA,Observ Paris, F-75014 Paris, France. [Combes, F.] Coll France, 11 Pl Marcelin Berthelot, F-75005 Paris, France. [Baum, S. A.; O'Dea, C. P.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, 567 Wilson Rd, E Lansing, MI 48824 USA. [Main, R. A.; Murray, N. W.; Parrish, I. J.] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada. [O'Connell, R. W.] Univ Virginia, Dept Astron, POB 400235, Charlottesville, VA 22904 USA. [Oonk, J. B. R.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Oonk, J. B. R.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Sanders, J. S.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Tremblay, G.] Yale Univ, Dept Phys, 217 Prospect St, New Haven, CT 06511 USA. [Tremblay, G.] Yale Univ, Yale Ctr Astron & Astrophys, 217 Prospect St, New Haven, CT 06511 USA. RP Vantyghem, AN (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. EM a2vantyg@uwaterloo.ca RI Combes, Francoise/F-6046-2011 OI Combes, Francoise/0000-0003-2658-7893 FU National Aeronautics and Space Administration through Chandra Award [G05-16134X]; National Aeronautics and Space Administration [NAS8-03060]; Natural Sciences and Engineering Research Council of Canada; Canadian Space Agency Space Science Enhancement Program; ERC Advanced Grant Feedback [340442] FX We thank the anonymous referee for helpful comments that improved this paper. Support for this work was provided in part by the National Aeronautics and Space Administration through Chandra Award Number G05-16134X issued by the Smithsonian Astrophysical Observatory for an on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. A.N.V. and B.R.M. acknowledge support from the Natural Sciences and Engineering Research Council of Canada. B.R.M. further acknowledges support from the Canadian Space Agency Space Science Enhancement Program. A.C.F. and H.R.R. acknowledge support from ERC Advanced Grant Feedback 340442. This paper makes use of the following ALMA data: ADS/JAO.ALMA 2012.1.00837.S. ALMA is a partnership of the ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration, 2013). This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 135 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 148 DI 10.3847/0004-637X/832/2/148 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100008 ER PT J AU Zahid, HJ Geller, MJ Fabricant, DG Hwang, HS AF Zahid, H. Jabran Geller, Margaret J. Fabricant, Daniel G. Hwang, Ho Seong TI THE SCALING OF STELLAR MASS AND CENTRAL STELLAR VELOCITY DISPERSION FOR QUIESCENT GALAXIES AT z < 0.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: structure ID DIGITAL SKY SURVEY; DARK-MATTER HALOS; STAR-FORMATION HISTORIES; HIGH-SPECTRAL-RESOLUTION; FIBER-FED SPECTROGRAPH; TO-LIGHT RATIOS; FUNDAMENTAL PLANE; ELLIPTIC GALAXIES; COSMIC TIME; POPULATION SYNTHESIS AB We examine the relation between stellar mass and central stellar velocity dispersion-the M*sigma relation-for massive quiescent galaxies at z < 0.7. We measure the local relation from the Sloan Digital Sky Survey and the intermediate redshift relation from the Smithsonian Hectospec Lensing Survey. Both samples are highly complete (>85%) and we consistently measure the stellar mass and velocity dispersion for the two samples. The M*sigma relation and its scatter are independent of redshift with sigma proportional to M*(0.3) for M* greater than or similar to 10(10.3) M-circle dot. The measured slope of the M*sigma relation is the same as the scaling between the total halo mass and the dark matter halo velocity dispersion obtained by N-body simulations. This consistency suggests that massive quiescent galaxies are virialized systems, where the central dark matter concentration is either a constant or negligible fraction of the stellar mass. The relation between the total galaxy mass (stellar + dark matter) and the central stellar velocity dispersion is consistent with the observed relation between the total mass of a galaxy cluster and the velocity dispersion of the cluster members. This result suggests that the central stellar velocity dispersion is directly proportional to the velocity dispersion of the dark matter halo. Thus, the central stellar velocity dispersion is a fundamental, directly observable property of galaxies, which may robustly connect galaxies to dark matter halos in N-body simulations. To interpret the results further in the context of Lambda CDM, it would be useful to analyze the relationship between the velocity dispersion of stellar particles and the velocity dispersion characterizing their dark matter halos in high-resolution cosmological hydrodynamic simulations. C1 [Zahid, H. Jabran; Geller, Margaret J.; Fabricant, Daniel G.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Hwang, Ho Seong] Korea Inst Adv Study, Sch Phys, 85 Hoegiro, Seoul 02455, South Korea. RP Zahid, HJ (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM zahid@cfa.harvard.edu FU Clay Postdoctoral Fellowship; Smithsonian Institution; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX H.J.Z. gratefully acknowledges the generous support of the Clay Postdoctoral Fellowship. M.J.G. and D.G.F. are supported by the Smithsonian Institution. We thank Scott Tremaine for carefully reading the manuscript and providing many useful comments. This work benefited from discussions with Ken Rines, Antonaldo Diaferio, Neta Bahcall, Mark Vogelsberger, and Paul Torrey. Masato Onodera kindly pointed out a mistake in Equation (5). This research has made use of NASA's Astrophysics Data System Bibliographic Services. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 89 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 203 DI 10.3847/0004-637X/832/2/203 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100063 ER PT J AU Zhang, YC Arce, HG Mardones, D Cabrit, S Dunham, MM Garay, G Noriega-Crespo, A Offner, SSR Raga, AC Corder, SA AF Zhang, Yichen Arce, Hector G. Mardones, Diego Cabrit, Sylvie Dunham, Michael M. Garay, Guido Noriega-Crespo, Alberto Offner, Stella S. R. Raga, Alejandro C. Corder, Stuartt A. TI ALMA CYCLE 1 OBSERVATIONS OF THE HH46/47 MOLECULAR OUTFLOW: STRUCTURE, ENTRAINMENT, AND CORE IMPACT SO ASTROPHYSICAL JOURNAL LA English DT Article DE Herbig-Haro objects; ISM: clouds; ISM: individual objects (HH 46, HH 47); jets and outflows; stars: formation ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; HUBBLE-SPACE-TELESCOPE; STAR CLUSTER FORMATION; HYDRODYNAMIC SIMULATIONS; PROTOSTELLAR SYSTEM; JET-DRIVEN; HH 46/47; CIRCUMSTELLAR ENVIRONMENT; INTERSTELLAR-MEDIUM AB We present Atacama Large Millimeter/sub-millimeter Array Cycle 1 observations of the HH 46/47 molecular outflow using combined 12 m array and Atacama Compact Array observations. The improved angular resolution and sensitivity of our multi-line maps reveal structures that help us study the entrainment process in much more detail and allow us to obtain more precise estimates of outflow properties than in previous observations. We use (CO)-C-13 (1-0) and (CO)-O-18 (1-0) emission to correct for the (CO)-C-12 (1-0) optical depth to accurately estimate the outflow mass, momentum, and kinetic energy. This correction increases the estimates of the mass, momentum, and kinetic energy by factors of about 9, 5, and 2, respectively, with respect to estimates assuming optically thin emission. The new (CO)-C-13 and (CO)-O-18 data also allow us to trace denser and slower outflow material than that traced by the (CO)-C-12 maps, and they reveal an outflow cavity wall at very low velocities (as low as 0.2 km s(-1) with respect to the core's central velocity). Adding the slower material traced only by (CO)-C-13 and (CO)-O-18, there is another factor of three increase in the mass estimate and 50% increase in the momentum estimate. The estimated outflow properties indicate that the outflow is capable of dispersing the parent core within the typical lifetime of the embedded phase of a low-mass protostar and that it is responsible for a core-to-star efficiency of 1/4 to 1/3. We find that the outflow cavity wall is composed of multiple shells associated with a series of jet bow-shock events. Within about 3000 au of the protostar the (CO)-C-13 and (CO)-O-18 emission trace a circumstellar envelope with both rotation and infall motions, which we compare with a simple analytic model. The CS (2-1) emission reveals tentative evidence of a slowly moving rotating outflow, which we suggest is entrained not only poloidally but also toroidally by a disk wind that is launched from relatively large radii from the source. C1 [Zhang, Yichen; Mardones, Diego; Garay, Guido] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. [Zhang, Yichen; Arce, Hector G.] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. [Cabrit, Sylvie] UCP, UPMC, ENS, LERMA,Observ Paris,UMR CNRS 8112, 61 Av Observ, F-75014 Paris, France. [Cabrit, Sylvie] IPAG, UMR 5274, F-38041 Grenoble, France. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Noriega-Crespo, Alberto] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Offner, Stella S. R.] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. [Raga, Alejandro C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Ap 70-543, Mexico City 04510, DF, Mexico. [Corder, Stuartt A.] Joint ALMA Observ, Av Alonso Cordova 3107, Santiago, Chile. RP Zhang, YC (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile.; Zhang, YC (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM yczhang.astro@gmail.com OI Zhang, Yichen/0000-0001-7511-0034; Mardones, Diego/0000-0002-5065-9175; Arce, Hector/0000-0001-5653-7817 FU CONICYT Project [PFB-06]; NSF [AST-1510021] FX We thank the anonymous referee for helpful discussions. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2012.1.00382.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. YZ, DM and GG acknowledge support from the CONICYT Project PFB-06. SSRO acknowledges support from NSF grant AST-1510021. NR 70 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 158 DI 10.3847/0004-637X/832/2/158 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7DK UT WOS:000390490100018 ER PT J AU Kjer, K Borowiec, ML Frandsen, PB Ware, J Wiegmann, BM AF Kjer, Karl Borowiec, Marek L. Frandsen, Paul B. Ware, Jessica Wiegmann, Brian M. TI Advances using molecular data in insect systematics SO CURRENT OPINION IN INSECT SCIENCE LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; SPECIES-TREE; COMPARATIVE PHYLOGEOGRAPHY; ULTRACONSERVED ELEMENTS; BIODIVERSITY ASSESSMENT; PHYLOGENOMICS RESOLVES; HOLOMETABOLOUS INSECTS; RAPID DIVERSIFICATION; EVOLUTIONARY HISTORY; PARTITIONING SCHEMES AB The size of molecular datasets has been growing exponentially since the mid 1980s, and new technologies have now dramatically increased the slope of this increase. New datasets include genomes, transcriptomes, and hybrid capture data, producing hundreds or thousands of loci. With these datasets, we are approaching a consensus on the higher level insect phylogeny. Huge datasets can produce new challenges in interpreting branch support, and new opportunities in developing better models and more sophisticated partitioning schemes. Dating analyses are improving as we recognize the importance of careful fossil calibration selection. With thousands of genes now available, coalescent methods have come of age. Barcode libraries continue to expand, and new methods are being developed for incorporating them into phylogenies with tens of thousands of individuals. C1 [Kjer, Karl; Ware, Jessica] Rutgers State Univ, Dept Biol Sci, 415 Boyden Hall, Newark, NJ 07012 USA. [Borowiec, Marek L.] Univ Rochester, 226 Hutchison Hall, Rochester, NY 14627 USA. [Frandsen, Paul B.] Smithsonian Inst, Off Res Informat Serv, Off Chief Informat Officer, Washington, DC 20024 USA. [Wiegmann, Brian M.] North Carolina State Univ, Dept Entomol & Plant Pathol, Raleigh, NC 27695 USA. RP Wiegmann, BM (reprint author), North Carolina State Univ, Dept Entomol & Plant Pathol, Raleigh, NC 27695 USA. EM bwiegman@ncsu.edu FU US National Science Foundation [DEB-1328784, DEB-1542395]; Schlinger foundation FX MB would like to thank Bonnie Blaimer and Michael Branstetter for providing data set size information. JW thanks Philip Barden, Manpreet Kohli and Jessica Thomas for thoughtful discussions on the topic of divergence time estimation. This contribution was partially supported by grants from the US National Science Foundation, DEB-1328784 and DEB-1542395 to BMW and the Schlinger foundation to KMK. NR 101 TC 0 Z9 0 U1 8 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2214-5745 EI 2214-5753 J9 CURR OPIN INSECT SCI JI Curr. Opin. Insect Sci. PD DEC PY 2016 VL 18 BP 40 EP 47 DI 10.1016/j.cois.2016.09.006 PG 8 WC Biology; Ecology; Entomology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Entomology GA EE8ZH UT WOS:000389914800007 PM 27939709 ER PT J AU Liang, MX Liu, XB Gilbert, GS Zheng, Y Luo, S Huang, FM Yu, SX AF Liang, Minxia Liu, Xubing Gilbert, Gregory S. Zheng, Yi Luo, Shan Huang, Fengmin Yu, Shixiao TI Adult trees cause density-dependent mortality in conspecific seedlings by regulating the frequency of pathogenic soil fungi SO ECOLOGY LETTERS LA English DT Article DE Host density; Janzen-Connell effect; seedling survival; soil-borne plant pathogens; subtropical forest ID BORNEAN RAIN-FOREST; TROPICAL FOREST; SPECIES-DIVERSITY; NEGATIVE FEEDBACK; PLANT DIVERSITY; TEMPERATE TREE; HOST-RANGE; SURVIVAL; COMMUNITY; MAINTENANCE AB Negative density-dependent seedling mortality has been widely detected in tropical, subtropical and temperate forests, with soil pathogens as a major driver. Here we investigated how host density affects the composition of soil pathogen communities and consequently influences the strength of plant-soil feedbacks. In field censuses of six 1-ha permanent plots, we found that survival was much lower for newly germinated seedlings that were surrounded by more conspecific adults. The relative abundance of pathogenic fungi in soil increased with increasing conspecific tree density for five of nine tree species; more soil pathogens accumulated around roots where adult tree density was higher, and this greater pathogen frequency was associated with lower seedling survival. Our findings show how tree density influences populations of soil pathogens, which creates plant-soil feedbacks that contribute to community-level and population-level compensatory trends in seedling survival. C1 [Liang, Minxia; Liu, Xubing; Zheng, Yi; Luo, Shan; Huang, Fengmin; Yu, Shixiao] Sun Yat Sen Univ, State Key Lab Biocontrol, Sch Life Sci, Dept Ecol, Guangzhou 510275, Guangdong, Peoples R China. [Gilbert, Gregory S.] Univ Calif Santa Cruz, Dept Environm Studies, 1156 High St, Santa Cruz, CA 95064 USA. [Gilbert, Gregory S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Liu, XB; Yu, SX (reprint author), Sun Yat Sen Univ, State Key Lab Biocontrol, Sch Life Sci, Dept Ecol, Guangzhou 510275, Guangdong, Peoples R China. EM liuxubing@mail.sysu.edu.cn; lssysx@mail.sysu.edu.cn FU National Natural Science Foundation of China [31500334, 31400363, 31230013]; China Postdoctoral Science Foundation [2015M572401]; Science Foundation of the State Key Laboratory of Biocontrol [SKLBC10B02]; Zhang-Hongda Science Foundation in Sun Yat-sen University FX We are grateful to Weinan Ye, Zhiming Zhang and Qinghua Kang for their assistance in the field. We thank three anonymous reviewers and the editor for their insightful comments that further improved our manuscript. This research was funded by the National Natural Science Foundation of China (grant 31500334,31400363 & 31230013), China Postdoctoral Science Foundation (grant 2015M572401), the Science Foundation of the State Key Laboratory of Biocontrol (grant SKLBC10B02) and the Zhang-Hongda Science Foundation in Sun Yat-sen University. NR 50 TC 0 Z9 0 U1 22 U2 22 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X EI 1461-0248 J9 ECOL LETT JI Ecol. Lett. PD DEC PY 2016 VL 19 IS 12 BP 1448 EP 1456 DI 10.1111/ele.12694 PG 9 WC Ecology SC Environmental Sciences & Ecology GA EF0OK UT WOS:000390025100007 PM 27790825 ER PT J AU Bujan, J Wright, SJ Kaspari, M AF Bujan, Jelena Wright, S. Joseph Kaspari, Michael TI Biogeochemical drivers of Neotropical ant activity and diversity SO ECOSPHERE LA English DT Article DE Azteca; fertilization; Formicidae; Gigante; nutrient limitation; Panama; phosphorus; tropics ID BOTTOM-UP FORCES; RAIN-FOREST; PHOSPHORUS LIMITATION; NUTRIENT LIMITATION; TROPICAL FOREST; TRADE-OFF; EXPLOITATION ECOSYSTEMS; BEHAVIORAL DOMINANCE; PRIMARY PRODUCTIVITY; COMMUNITY STRUCTURE AB Human activities are rapidly changing biogeochemistry across the globe, yet little is known about biogeochemical impacts on higher-level consumers. In a Panamanian rainforest, we measured the effects of chronic nitrogen, phosphorus, and potassium fertilization on ants: hyper-abundant terrestrial arthropods and ecosystem engineers. We tested two compatible hypotheses: the nutrient limitation hypothesis-where adding a limiting nutrient increases ant activity and abundance; and the community homogenization hypothesis-where adding a limiting nutrient decreases ant diversity. Lowland tropical rainforests are expected to be phosphorus-limited, so we predicted higher ant activity but lower diversity on phosphorus plots. In each fertilization plot, we baited trees and lianas to attract both canopy and ground nesting ants. After controlling for temperature, which accounted for roughly 20% of the variation in ant foraging activity, ant activity remained higher on phosphorus addition plots than on any other fertilization treatment. Genus level diversity was 16% lower on plots receiving phosphorus than the control, consistent with the paradox of enrichment frequently observed in plant communities. This pattern, however, did not hold for species level diversity. The community-level response was largely driven by the most abundant genus, Azteca, which increased foraging activity and abundance across phosphorus plots. The high activity and low diversity of ants on experimental phosphorus plots point to the potentially strong influence of biogeochemistry on these ubiquitous insects with potential ramifications for the forest food web. This is, to our knowledge, the first study relating biogeochemistry of macronutrients to foraging activity, diversity, and abundance of consumers, implicating strong bottom-up structuring of the ant community in one of the world's most diverse ecosystems. C1 [Bujan, Jelena; Kaspari, Michael] Univ Oklahoma, Grad Program Ecol & Evolutionary Biol, Dept Biol, Norman, OK 73019 USA. [Wright, S. Joseph; Kaspari, Michael] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. RP Bujan, J (reprint author), Univ Oklahoma, Grad Program Ecol & Evolutionary Biol, Dept Biol, Norman, OK 73019 USA. EM jelena.bujan@ou.edu FU National Science Foundation Macrosystem Grant; Biology Department (OU); College of Arts and Sciences (OU); Graduate Student Senate (OU) FX Field assistance with intense baiting was carried out with the help of David Fowler. Comments of Ana Jesovnik, David Donoso, Natalie Clay, and Jackson Helms greatly improved the early versions of the manuscript. Oris Acevedo and Belkys Jimenez of Smithsonian Topical Research Institute provided logistical support in Panama. This study was funded by the Biology Department (OU), the College of Arts and Sciences (OU), Graduate Student Senate (OU), and National Science Foundation Macrosystem Grant to MK. The experiments in this study comply with current laws of the Republic of Panama. NR 82 TC 0 Z9 0 U1 10 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD DEC PY 2016 VL 7 IS 12 AR e01597 DI 10.1002/ecs2.1597 PG 11 WC Ecology SC Environmental Sciences & Ecology GA EF2EE UT WOS:000390136700007 ER PT J AU Gonzalez-Akre, E Meakem, V Eng, CY Tepley, AJ Bourg, NA McShea, W Davies, SJ Anderson-Teixeira, K AF Gonzalez-Akre, Erika Meakem, Victoria Eng, Cheng-Yin Tepley, Alan J. Bourg, Norman A. McShea, William Davies, Stuart J. Anderson-Teixeira, Kristina TI Patterns of tree mortality in a temperate deciduous forest derived from a large forest dynamics plot SO ECOSPHERE LA English DT Article DE annual mortality census; Center for Tropical Forest Science-Forest Global Earth Observatory; large forest dynamics plot; temperate broadleaf deciduous forest; tree mortality ID CLIMATE-CHANGE; LONG-TERM; UNITED-STATES; TROPICAL FORESTS; GLOBAL CHANGE; GAP MODELS; DROUGHT; GROWTH; RATES; SIZE AB Tree mortality is one of the most influential drivers of forest dynamics, and characterizing patterns of tree mortality is critical to understanding forest dynamics and ecosystem function in the present era of global change. Here, we use a unique data set of mortality in a temperate deciduous forest to characterize rates and drivers of mortality. At the 25.6-ha Center for Tropical Forest Science-Forest Global Earth Observatory forest dynamics plot at the Smithsonian Conservation Biology Institute (Virginia, USA), we conducted two full tree censuses in 2008 and 2013 and then tracked mortality over the next 2 years (2014 and 2015). Overall, the mortality rate, m, of stems >= 10 cm diameter was 1.3-2.1%/yr. Biomass mortality, M, was 1.9-3.4 Mg.ha(-1).yr(-1) at the stand level (0.6-1.1%/yr of biomass), less than biomass gains from growth and recruitment, resulting in net live biomass accumulation. Small stems died at the highest rate; however, contributions to M increased toward larger size classes. Most species had m <2%/yr and M < 0.25 Mg.ha(-1).yr(-1) (<3%/yr of biomass), whereas two to four species had anomalously high mortality rates during each census period, accounting for 15-24% of m (n = 2, Cercis canadensis, Ulmus species) and 39-75% of M(n = 4 Quercus species). Stems that died, whether or not in association with mechanical damage, tended to grow more slowly in preceding years than surviving stems and, for certain shade-intolerant species, tended to be in neighborhoods with higher basal area. These findings show how relatively fine-scale mortality processes contribute to stand-level compositional change and carbon cycling. The mortality patterns reported here will provide a valuable basis for understanding future disturbance events within eastern deciduous forests and for comparing across forest types. C1 [Gonzalez-Akre, Erika; Meakem, Victoria; Eng, Cheng-Yin; Tepley, Alan J.; McShea, William; Anderson-Teixeira, Kristina] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Bourg, Norman A.] US Geol Survey, Natl Res Program, Eastern Branch, Reston, VA 20192 USA. [Davies, Stuart J.; Anderson-Teixeira, Kristina] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Panama City 9100, Panama. [Davies, Stuart J.] Smithsonian Natl Museum Nat Hist, Washington, DC 20013 USA. RP Anderson-Teixeira, K (reprint author), Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA.; Anderson-Teixeira, K (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Panama City 9100, Panama. EM teixeirak@si.edu; teixeirak@si.edu OI Tepley, Alan/0000-0002-5701-9613 FU Next Generation Ecosystem Experiment (NGEE) Tropics project; Mary Jean Hale Fund; Smithsonian Institution Center for Tropical Forest Science-Forest Global Earth Observatory (CTFS-ForestGEO); Smithsonian Competitive Grants Program in Science FX We thank Valentine Hermann, Maria Wang, Gabriela Reyes, Haley Overstreet, Maryam Sedaghatpour, and Romaric Moncrieffe for assisting with mortality censuses and Helene Muller-Landau for the use of her R scripts. Funds for the full tree censuses were provided by the Smithsonian Institution Center for Tropical Forest Science-Forest Global Earth Observatory (CTFS-ForestGEO). Annual mortality censuses and the analyses presented here were funded by a Smithsonian Competitive Grants Program in Science award to KAT. CYE received support from the Mary Jean Hale Fund. SJD received support from the Next Generation Ecosystem Experiment (NGEE) Tropics project. NR 82 TC 0 Z9 0 U1 14 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD DEC PY 2016 VL 7 IS 12 AR e01595 DI 10.1002/ecs2.1595 PG 17 WC Ecology SC Environmental Sciences & Ecology GA EF2EE UT WOS:000390136700012 ER PT J AU Lin, DM Anderson-Teixeira, KJ Lai, JS Mi, XC Ren, HB Ma, KP AF Lin, Dunmei Anderson-Teixeira, Kristina J. Lai, Jiangshan Mi, Xiangcheng Ren, Haibao Ma, Keping TI Traits of dominant tree species predict local scale variation in forest aboveground and topsoil carbon stocks SO PLANT AND SOIL LA English DT Article DE Carbon stocks; Biodiversity and ecosystem functioning; Functional trait; Functional diversity; Mass ratio hypothesis; Niche complementarity ID PLANT FUNCTIONAL DIVERSITY; BROAD-LEAVED FOREST; SOIL CARBON; ECONOMICS SPECTRUM; ECOSYSTEM SERVICES; TROPICAL FORESTS; PHYLOGENETIC DIVERSITY; BIODIVERSITY; STORAGE; PRODUCTIVITY AB Forests play a vital role in regulation of the global carbon cycle. Mechanistically understanding how their ecosystem functioning relates to biodiversity is necessary for predicting the consequences of biodiversity loss and for setting conservation priorities. Here, we test whether carbon stocks in a subtropical evergreen broad-leaved forest in China are more strongly influenced by plant functional diversity (FD), as would be predicted by the 'niche complementarity hypothesis', or by community-weighted mean (CWM) functional trait values, as would be predicted by the 'mass ratio hypothesis'. Using data from a 24-ha plot subdivided into 400 m(2) quadrats, we determined relationships of aboveground carbon (AGC) and topsoil (1-10 cm) organic carbon (SOC) to topographic variables, stem density, CWM and FD of six functional traits hypothesized to influence carbon stocks. After accounting for topographic variables and tree stem density, boosted regression tree models revealed that CWMs were the dominant driving factors for both AGC and SOC, whereas FD had negligible effects. AGC and SOC were influenced by different functional traits, with AGC responding most strongly to CWM values for wood density and maximum tree height, and SOC responding most strongly to elevation, indicating that these carbon stocks are shaped by different underlying mechanisms. Our results support the mass ratio hypothesis but not the niche complementarity hypothesis. Our study implies that, when it comes to maximizing forest carbon storage, conservation priorities should focus on protection of species with traits associated to high carbon stocks. C1 [Lin, Dunmei] Chongqing Univ, Key Lab Gorges Reservoir Reg Ecoenvironm 3, Minist Educ, Chongqing 400045, Peoples R China. [Lin, Dunmei; Lai, Jiangshan; Mi, Xiangcheng; Ren, Haibao; Ma, Keping] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Lin, Dunmei] Chongqing Univ, Natl Ctr Int Res Low Carbon & Green Buildings, Chongqing 400045, Peoples R China. [Anderson-Teixeira, Kristina J.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA USA. [Anderson-Teixeira, Kristina J.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci Forest Global Earth Observ, Panama City, Panama. RP Ma, KP (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China.; Lin, DM (reprint author), Chongqing Univ, Natl Ctr Int Res Low Carbon & Green Buildings, Chongqing 400045, Peoples R China. EM lindunmei@cqu.edu.cn; kpma@ibcas.ac.cn FU National Natural Science Foundation of China [31270496]; Fundamental Research Funds for the Central Universities [106112015CDJXY210012]; 111 Project [B13041] FX This work was financially supported by the National Natural Science Foundation of China (NO.31270496), the Fundamental Research Funds for the Central Universities (106112015CDJXY210012) and the 111 Project (B13041). NR 63 TC 0 Z9 0 U1 15 U2 15 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0032-079X EI 1573-5036 J9 PLANT SOIL JI Plant Soil PD DEC PY 2016 VL 409 IS 1-2 BP 435 EP 446 DI 10.1007/s11104-016-2976-0 PG 12 WC Agronomy; Plant Sciences; Soil Science SC Agriculture; Plant Sciences GA EF0RZ UT WOS:000390034900030 ER PT J AU Lund, MN Chaplin, WJ Casagrande, L Aguirre, VS Basu, S Bieryla, A Christensen-Dalsgaard, J Latham, DW White, TR Davies, GR Huber, D Buchhave, LA Handberg, R AF Lund, Mikkel N. Chaplin, William J. Casagrande, Luca Aguirre, Victor Silva Basu, Sarbani Bieryla, Allyson Christensen-Dalsgaard, Jorgen Latham, David W. White, Timothy R. Davies, Guy R. Huber, Daniel Buchhave, Lars A. Handberg, Rasmus TI Asteroseismic Properties of Solar-type Stars Observed with the NASA K2 Mission: Results from Campaigns 1-3 and Prospects for Future Observations SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE asteroseismology; methods: data analysis; stars: distances; stars: fundamental parameters; stars: oscillations; stars: solar-type ID GENEVA-COPENHAGEN SURVEY; STELLAR EVOLUTION CODE; SURFACE BRIGHTNESS RELATIONS; MASS-LUMINOSITY-RELATION; SPIN-ORBIT MISALIGNMENT; MAIN-SEQUENCE STARS; FUNDAMENTAL PROPERTIES; GALACTIC ARCHAEOLOGY; KEPLER MISSION; OB ASSOCIATION AB We present an asteroseismic analysis of 33 solar-type stars observed in short cadence (SC) during Campaigns (C) 1-3 of the NASA K2 mission. We were able to extract both average seismic parameters and individual mode frequencies for stars with dominant frequencies up to similar to 3300 mu Hz, and we find that data for some targets are good enough to allow for a measurement of the rotational splitting. Modeling of the extracted parameters is performed by using grid-based methods using average parameters and individual frequencies together with spectroscopic parameters. For the target selection in C3, stars were chosen as in C1 and C2 to cover a wide range in parameter space to better understand the performance and noise characteristics. For C3 we still detected oscillations in 73% of the observed stars that we proposed. Future K2 campaigns hold great promise for the study of nearby clusters and the chemical evolution and age-metallicity relation of nearby field stars in the solar neighborhood. We expect oscillations to be detected in similar to 388 SC targets if the K2 mission continues until C18, which will greatly complement the similar to 500 detections of solar-like oscillations made for SC targets during the nominal Kepler mission. For similar to 30-40 of these, including several members of the Hyades open cluster, we furthermore expect that inference from interferometry should be possible. C1 [Lund, Mikkel N.; Chaplin, William J.; Davies, Guy R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Lund, Mikkel N.; Chaplin, William J.; Aguirre, Victor Silva; Christensen-Dalsgaard, Jorgen; White, Timothy R.; Davies, Guy R.; Huber, Daniel; Handberg, Rasmus] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Casagrande, Luca] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Basu, Sarbani] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. [Bieryla, Allyson; Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Huber, Daniel] Univ Sydney, SIfA, Sch Phys, Sydney, NSW 2006, Australia. [Huber, Daniel] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. RP Lund, MN (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England.; Lund, MN (reprint author), Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. EM lundm@bison.ph.bham.ac.uk OI Lund, Mikkel Norup/0000-0001-9214-5642 FU NASA's Science Mission Directorate; Danish Council for Independent Research | Natural Science grant [DFF-4181-00415]; European Community [312844]; Danish National Research Foundation [DNRF106]; ASTERISK project - European Research Council [267864]; UK Science and Technology Facilities Council (STFC); VILLUM FONDEN research grant [10118]; NASA [NNX13AE70G]; NSF [AST-1514676]; Kepler mission [NNX13AB58A]; Smithsonian Astrophysical Observatory; Australian Research Council [DE140101364]; NASA through Kepler Participating Scientist Program [NNX14AB92G]; National Aeronautics and Space Administration; National Science Foundation FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors acknowledge the dedicated team behind the Kepler and K2 missions, without whom this work would not have been possible. M.N.L. acknowledges the support of The Danish Council for Independent Research | Natural Science (grant DFF-4181-00415). M.N.L. was partly supported by the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 312844 (SpaceInn), which is gratefully acknowledged. Funding for the Stellar Astrophysics Centre (SAC) is provided by The Danish National Research Foundation (grant DNRF106). The research was supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No. 267864). W.J.C. and G.R.D. acknowledge the support of the UK Science and Technology Facilities Council (STFC). V.S.A. and T.R.W. acknowledge support from VILLUM FONDEN (research grant 10118). S.B. acknowledges partial support of NASA grant NNX13AE70G and NSF grant AST-1514676. D.W.L. acknowledges partial support from the Kepler mission via Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. D.H. acknowledges support by the Australian Research Council's Discovery Projects funding scheme (project number DE140101364) and support by the NASA grant NNX14AB92G issued through the Kepler Participating Scientist Program. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration 2013). This research has made use of the SIMBAD database and VizieR access tool, operated at CDS, Strasbourg, France. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 124 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2016 VL 128 IS 970 AR 124204 DI 10.1088/1538-3873/128/970/124204 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF4XX UT WOS:000390336400006 ER PT J AU Fox, NJ Velli, MC Bale, SD Decker, R Driesman, A Howard, RA Kasper, JC Kinnison, J Kusterer, M Lario, D Lockwood, MK McComas, DJ Raouafi, NE Szabo, A AF Fox, N. J. Velli, M. C. Bale, S. D. Decker, R. Driesman, A. Howard, R. A. Kasper, J. C. Kinnison, J. Kusterer, M. Lario, D. Lockwood, M. K. McComas, D. J. Raouafi, N. E. Szabo, A. TI The Solar Probe Plus Mission: Humanity's First Visit to Our Star SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar Probe Plus; SPP; Corona; Heliophysics; NASA mission; Solar wind ID REDUCED MAGNETOHYDRODYNAMIC TURBULENCE; KELVIN-HELMHOLTZ INSTABILITIES; PROTON TEMPERATURE ANISOTROPY; HIGH HELIOGRAPHIC LATITUDES; FIELD POLARITY INVERSIONS; HELIOS PLASMA-EXPERIMENT; MAGNETIC-FIELD; CORONAL HOLES; ENERGETIC PARTICLES; ALFVEN WAVES AB Solar Probe Plus (SPP) will be the first spacecraft to fly into the low solar corona. SPP's main science goal is to determine the structure and dynamics of the Sun's coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what processes accelerate energetic particles. Understanding these fundamental phenomena has been a top-priority science goal for over five decades, dating back to the 1958 Simpson Committee Report. The scale and concept of such a mission has been revised at intervals since that time, yet the core has always been a close encounter with the Sun. The mission design and the technology and engineering developments enable SPP to meet its science objectives to: (1) Trace the flow of energy that heats and accelerates the solar corona and solar wind; (2) Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind; and (3) Explore mechanisms that accelerate and transport energetic particles. The SPP mission was confirmed in March 2014 and is under development as a part of NASA's Living with a Star (LWS) Program. SPP is scheduled for launch in mid-2018, and will perform 24 orbits over a 7-year nominal mission duration. Seven Venus gravity assists gradually reduce SPP's perihelion from 35 solar radii () for the first orbit to for the final three orbits. In this paper we present the science, mission concept and the baseline vehicle for SPP, and examine how the mission will address the key science questions. C1 [Fox, N. J.; Decker, R.; Driesman, A.; Kinnison, J.; Kusterer, M.; Lario, D.; Lockwood, M. K.; Raouafi, N. E.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Velli, M. C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Bale, S. D.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Howard, R. A.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Kasper, J. C.] Univ Michigan, Ann Arbor, MI 48109 USA. [Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [McComas, D. J.] Southwest Res Inst, San Antonio, TX 78228 USA. [McComas, D. J.] Univ Texas San Antonio, San Antonio, TX 78249 USA. [Szabo, A.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Fox, NJ (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. EM Nicola.Fox@jhuapl.edu RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 FU NASA [NNN06AA01C, NNN10AA08T] FX The Solar Probe Plus mission is the result of tireless efforts by countless scientists from all over the world who first imagined this project in the 1950s and never ceased in their efforts over the following decades to ensure that the mission will finally become a reality. We are deeply indebted to all of them for their outstanding work and remarkable determination and vision. We acknowledge the continuous support of NASA to the project. Solar Probe Plus is part of NASA's Living With a Star program. We, the authors, acknowledge the support from NASA under contract NNN06AA01C (Task NNN10AA08T). We would like also to acknowledge the leadership and friendship of the late Andrew Dantzler (the first Solar Probe Plus Project Manager). We are very grateful to the anonymous referees for the constructive criticism that helped improve the quality of the manuscript. NR 126 TC 8 Z9 8 U1 5 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2016 VL 204 IS 1-4 BP 7 EP 48 DI 10.1007/s11214-015-0211-6 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF0XX UT WOS:000390050700002 ER PT J AU Kasper, JC Abiad, R Austin, G Balat-Pichelin, M Bale, SD Belcher, JW Berg, P Bergner, H Berthomier, M Bookbinder, J Brodu, E Caldwell, D Case, AW Chandran, BDG Cheimets, P Cirtain, JW Cranmer, SR Curtis, DW Daigneau, P Dalton, G Dasgupta, B DeTomaso, D Diaz-Aguado, M Djordjevic, B Donaskowski, B Effinger, M Florinski, V Fox, N Freeman, M Gallagher, D Gary, SP Gauron, T Gates, R Goldstein, M Golub, L Gordon, DA Gurnee, R Guth, G Halekas, J Hatch, K Heerikuisen, J Ho, G Hu, Q Johnson, G Jordan, SP Korreck, KE Larson, D Lazarus, AJ Li, G Livi, R Ludlam, M Maksimovic, M McFadden, JP Marchant, W Maruca, BA McComas, DJ Messina, L Mercer, T Park, S Peddie, AM Pogorelov, N Reinhart, MJ Richardson, JD Robinson, M Rosen, I Skoug, RM Slagle, A Steinberg, JT Stevens, ML Szabo, A Taylor, ER Tiu, C Turin, P Velli, M Webb, G Whittlesey, P Wright, K Wu, ST Zank, G AF Kasper, Justin C. Abiad, Robert Austin, Gerry Balat-Pichelin, Marianne Bale, Stuart D. Belcher, John W. Berg, Peter Bergner, Henry Berthomier, Matthieu Bookbinder, Jay Brodu, Etienne Caldwell, David Case, Anthony W. Chandran, Benjamin D. G. Cheimets, Peter Cirtain, Jonathan W. Cranmer, Steven R. Curtis, David W. Daigneau, Peter Dalton, Greg Dasgupta, Brahmananda DeTomaso, David Diaz-Aguado, Millan Djordjevic, Blagoje Donaskowski, Bill Effinger, Michael Florinski, Vladimir Fox, Nichola Freeman, Mark Gallagher, Dennis Gary, S. Peter Gauron, Tom Gates, Richard Goldstein, Melvin Golub, Leon Gordon, Dorothy A. Gurnee, Reid Guth, Giora Halekas, Jasper Hatch, Ken Heerikuisen, Jacob Ho, George Hu, Qiang Johnson, Greg Jordan, Steven P. Korreck, Kelly E. Larson, Davin Lazarus, Alan J. Li, Gang Livi, Roberto Ludlam, Michael Maksimovic, Milan McFadden, James P. Marchant, William Maruca, Bennet A. McComas, David J. Messina, Luciana Mercer, Tony Park, Sang Peddie, Andrew M. Pogorelov, Nikolai Reinhart, Matthew J. Richardson, John D. Robinson, Miles Rosen, Irene Skoug, Ruth M. Slagle, Amanda Steinberg, John T. Stevens, Michael L. Szabo, Adam Taylor, Ellen R. Tiu, Chris Turin, Paul Velli, Marco Webb, Gary Whittlesey, Phyllis Wright, Ken Wu, S. T. Zank, Gary TI Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar probe plus; SWEAP; Solar wind plasma; Corona; Heating; Acceleration ID ION-CYCLOTRON WAVES; KINETIC SHELL-MODEL; MAGNETIC-FIELD; MAGNETOHYDRODYNAMIC TURBULENCE; PARTICLE-ACCELERATION; ALFVEN WAVES; COSMIC-RAYS; FLUCTUATIONS; DISSIPATION; TEMPERATURE AB The Solar Wind Electrons Alphas and Protons (SWEAP) Investigation on Solar Probe Plus is a four sensor instrument suite that provides complete measurements of the electrons and ionized helium and hydrogen that constitute the bulk of solar wind and coronal plasma. SWEAP consists of the Solar Probe Cup (SPC) and the Solar Probe Analyzers (SPAN). SPC is a Faraday Cup that looks directly at the Sun and measures ion and electron fluxes and flow angles as a function of energy. SPAN consists of an ion and electron electrostatic analyzer (ESA) on the ram side of SPP (SPAN-A) and an electron ESA on the anti-ram side (SPAN-B). The SPAN-A ion ESA has a time of flight section that enables it to sort particles by their mass/charge ratio, permitting differentiation of ion species. SPAN-A and -B are rotated relative to one another so their broad fields of view combine like the seams on a baseball to view the entire sky except for the region obscured by the heat shield and covered by SPC. Observations by SPC and SPAN produce the combined field of view and measurement capabilities required to fulfill the science objectives of SWEAP and Solar Probe Plus. SWEAP measurements, in concert with magnetic and electric fields, energetic particles, and white light contextual imaging will enable discovery and understanding of solar wind acceleration and formation, coronal and solar wind heating, and particle acceleration in the inner heliosphere of the solar system. SPC and SPAN are managed by the SWEAP Electronics Module (SWEM), which distributes power, formats onboard data products, and serves as a single electrical interface to the spacecraft. SWEAP data products include ion and electron velocity distribution functions with high energy and angular resolution. Full resolution data are stored within the SWEM, enabling high resolution observations of structures such as shocks, reconnection events, and other transient structures to be selected for download after the fact. This paper describes the implementation of the SWEAP Investigation, the driving requirements for the suite, expected performance of the instruments, and planned data products, as of mission preliminary design review. C1 [Kasper, Justin C.] Univ Michigan, Ann Arbor, MI 48109 USA. [Kasper, Justin C.; Austin, Gerry; Bergner, Henry; Bookbinder, Jay; Caldwell, David; Case, Anthony W.; Cheimets, Peter; Daigneau, Peter; Freeman, Mark; Gauron, Tom; Gates, Richard; Golub, Leon; Guth, Giora; Jordan, Steven P.; Korreck, Kelly E.; Park, Sang; Stevens, Michael L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Abiad, Robert; Bale, Stuart D.; Berg, Peter; Curtis, David W.; Dalton, Greg; Diaz-Aguado, Millan; Djordjevic, Blagoje; Donaskowski, Bill; Gordon, Dorothy A.; Hatch, Ken; Johnson, Greg; Larson, Davin; Livi, Roberto; Ludlam, Michael; McFadden, James P.; Marchant, William; Maruca, Bennet A.; Messina, Luciana; Mercer, Tony; Robinson, Miles; Rosen, Irene; Slagle, Amanda; Taylor, Ellen R.; Tiu, Chris; Turin, Paul] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Balat-Pichelin, Marianne; Brodu, Etienne] PROMES CNRS, Lab Proc Mat & Energie Solaire, 7 Rue 4 Solaire, F-66120 Font Romeu, France. [Belcher, John W.; Lazarus, Alan J.; Richardson, John D.] MIT, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Berthomier, Matthieu] Ecole Polytech, Lab Phys Plasmas, Palaiseau, France. [Chandran, Benjamin D. G.] Univ New Hampshire, Durham, NH 03824 USA. [Cirtain, Jonathan W.; Effinger, Michael; Gallagher, Dennis] Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Cirtain, Jonathan W.; Effinger, Michael; Gallagher, Dennis] Univ Colorado, Boulder, CO 80309 USA. [Dasgupta, Brahmananda; Florinski, Vladimir; Heerikuisen, Jacob; Hu, Qiang; Li, Gang; Pogorelov, Nikolai; Webb, Gary; Whittlesey, Phyllis; Wright, Ken; Wu, S. T.; Zank, Gary] Univ Alabama Huntsville, Huntsville, AL 35805 USA. [DeTomaso, David; Fox, Nichola; Gurnee, Reid; Ho, George; Reinhart, Matthew J.] Appl Phys Lab, Laurel, MD 20723 USA. [Gary, S. Peter; Skoug, Ruth M.; Steinberg, John T.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Goldstein, Melvin; Peddie, Andrew M.; Szabo, Adam] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Halekas, Jasper] Univ Iowa, Iowa City, IA 52242 USA. [Maksimovic, Milan] LESIA, Observ Paris, CNRS, UMR 8109, F-92195 Meudon, France. [McComas, David J.] Southwest Res Inst, San Antonio, TX 78228 USA. [McComas, David J.] Univ Texas San Antonio, San Antonio, TX 78249 USA. [Velli, Marco] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP Kasper, JC (reprint author), Univ Michigan, Ann Arbor, MI 48109 USA.; Kasper, JC (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM jckasper@umich.edu RI Bale, Stuart/E-7533-2011; OI Bale, Stuart/0000-0002-1989-3596; Halekas, Jasper/0000-0001-5258-6128 FU NASA [NNN06AA01C, NNN10AA08T]; CNES; NASA; rest of the SPP team FX We acknowledge support from NASA under contract NNN06AA01C (Task NNN10AA08T). We are grateful for the creativity and dedication of the many people at SWEAP institutions who make this investigation possible. We also acknowledge early support for technology development by the Smithsonian Institution, NASA Marshall Space Flight Center and the CNRS PROMES research group in Odeillo-Font Romeu, France. We thank Jean-Yves Prado and CNES for providing financial support for our activities in France. We also thank NASA and the rest of the SPP team for their support on this project. J.C. Kasper personally thanks John Alexander Simpson and Alan Jay Lazarus for their contributions to Solar Probe and for exposing a student to this exciting mission of discovery. NR 103 TC 5 Z9 5 U1 2 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2016 VL 204 IS 1-4 BP 131 EP 186 DI 10.1007/s11214-015-0206-3 PG 56 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF0XX UT WOS:000390050700005 ER PT J AU McComas, DJ Alexander, N Angold, N Bale, S Beebe, C Birdwell, B Boyle, M Burgum, JM Burnham, JA Christian, ER Cook, WR Cooper, SA Cummings, AC Davis, AJ Desai, MI Dickinson, J Dirks, G Do, DH Fox, N Giacalone, J Gold, RE Gurnee, RS Hayes, JR Hill, ME Kasper, JC Kecman, B Klemic, J Krimigis, SM Labrador, AW Layman, RS Leske, RA Livi, S Matthaeus, WH McNutt, RL Mewaldt, RA Mitchell, DG Nelson, KS Parker, C Rankin, JS Roelof, EC Schwadron, NA Seifert, H Shuman, S Stokes, MR Stone, EC Vandegriff, JD Velli, M von Rosenvinge, TT Weidner, SE Wiedenbeck, ME Wilson, P AF McComas, D. J. Alexander, N. Angold, N. Bale, S. Beebe, C. Birdwell, B. Boyle, M. Burgum, J. M. Burnham, J. A. Christian, E. R. Cook, W. R. Cooper, S. A. Cummings, A. C. Davis, A. J. Desai, M. I. Dickinson, J. Dirks, G. Do, D. H. Fox, N. Giacalone, J. Gold, R. E. Gurnee, R. S. Hayes, J. R. Hill, M. E. Kasper, J. C. Kecman, B. Klemic, J. Krimigis, S. M. Labrador, A. W. Layman, R. S. Leske, R. A. Livi, S. Matthaeus, W. H. McNutt, R. L., Jr. Mewaldt, R. A. Mitchell, D. G. Nelson, K. S. Parker, C. Rankin, J. S. Roelof, E. C. Schwadron, N. A. Seifert, H. Shuman, S. Stokes, M. R. Stone, E. C. Vandegriff, J. D. Velli, M. von Rosenvinge, T. T. Weidner, S. E. Wiedenbeck, M. E. Wilson, P. TI Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation SO SPACE SCIENCE REVIEWS LA English DT Review DE Solar Probe Plus; ISIS; Solar energetic particles; SEPs; CMEs; Corona; Particle acceleration ID HELIOSPHERIC MAGNETIC-FIELD; CORONAL MASS EJECTIONS; HE-3-RICH SOLAR-FLARES; INTERPLANETARY SHOCKS; SPECTRAL PROPERTIES; CHARGED-PARTICLES; HEAVY-IONS; 1 AU; MAGNETOHYDRODYNAMIC TURBULENCE; ULTRAHEAVY IONS AB The Integrated Science Investigation of the Sun (ISIS) is a complete science investigation on the Solar Probe Plus (SPP) mission, which flies to within nine solar radii of the Sun's surface. ISIS comprises a two-instrument suite to measure energetic particles over a very broad energy range, as well as coordinated management, science operations, data processing, and scientific analysis. Together, ISIS observations allow us to explore the mechanisms of energetic particles dynamics, including their: (1) Origins-defining the seed populations and physical conditions necessary for energetic particle acceleration; (2) Acceleration-determining the roles of shocks, reconnection, waves, and turbulence in accelerating energetic particles; and (3) Transport-revealing how energetic particles propagate from the corona out into the heliosphere. The two ISIS Energetic Particle Instruments measure lower (EPI-Lo) and higher (EPI-Hi) energy particles. EPI-Lo measures ions and ion composition from similar to 20 keV/nucleon-15 MeV total energy and electrons from similar to 25-1000 keV. EPI-Hi measures ions from similar to 1-200 MeV/nucleon and electrons from similar to 0.5-6 MeV. EPI-Lo comprises 80 tiny apertures with fields-of-view (FOVs) that sample over nearly a complete hemisphere, while EPI-Hi combines three telescopes that together provide five large-FOV apertures. ISIS observes continuously inside of 0.25 AU with a high data collection rate and burst data (EPI-Lo) coordinated with the rest of the SPP payload; outside of 0.25 AU, ISIS runs in low-rate science mode whenever feasible to capture as complete a record as possible of the solar energetic particle environment and provide calibration and continuity for measurements closer in to the Sun. The ISIS Science Operations Center plans and executes commanding, receives and analyzes all ISIS data, and coordinates science observations and analyses with the rest of the SPP science investigations. Together, ISIS' unique observations on SPP will enable the discovery, untangling, and understanding of the important physical processes that govern energetic particles in the innermost regions of our heliosphere, for the first time. This paper summarizes the ISIS investigation at the time of the SPP mission Preliminary Design Review in January 2014. C1 [McComas, D. J.; Alexander, N.; Angold, N.; Beebe, C.; Birdwell, B.; Desai, M. I.; Dickinson, J.; Dirks, G.; Livi, S.; Weidner, S. E.; Wilson, P.] Southwest Res Inst, San Antonio, TX 78228 USA. [McComas, D. J.; Desai, M. I.; Livi, S.] Univ Texas San Antonio, San Antonio, TX 78249 USA. [Bale, S.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Boyle, M.; Burgum, J. M.; Cooper, S. A.; Do, D. H.; Fox, N.; Gold, R. E.; Gurnee, R. S.; Hayes, J. R.; Hill, M. E.; Krimigis, S. M.; Layman, R. S.; McNutt, R. L., Jr.; Mitchell, D. G.; Nelson, K. S.; Parker, C.; Roelof, E. C.; Seifert, H.; Stokes, M. R.; Vandegriff, J. D.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Burnham, J. A.; Cook, W. R.; Cummings, A. C.; Davis, A. J.; Kecman, B.; Klemic, J.; Labrador, A. W.; Leske, R. A.; Mewaldt, R. A.; Rankin, J. S.; Stone, E. C.] CALTECH, Pasadena, CA 91125 USA. [Christian, E. R.; Shuman, S.; von Rosenvinge, T. T.] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Giacalone, J.] Univ Arizona, Tucson, AZ 85721 USA. [Kasper, J. C.] Univ Michigan, Ann Arbor, MI 48109 USA. [Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Matthaeus, W. H.] Univ Delaware, Newark, DE 19716 USA. [Schwadron, N. A.] Univ New Hampshire, Durham, NH 03824 USA. [Velli, M.; Wiedenbeck, M. E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP McComas, DJ (reprint author), Southwest Res Inst, San Antonio, TX 78228 USA. EM dmccomas@swri.edu RI Bale, Stuart/E-7533-2011 OI Bale, Stuart/0000-0002-1989-3596 FU NASA FX We are deeply indebted to all of the outstanding men and women who have made the Solar Probe Plus Mission and ISIS investigation a reality. These include members of the Solar Probe/Solar Probe Plus Science and Technology Definition Team (STDT), NASA headquarters personnel who have supported and continue to support the mission, project team members at APL and GSFC, instrument team members at a variety of universities and other institutions across the country and around the world, and other members of the community who support this critical mission through their advisory work for the NRC and informally through many other means. We also thank Wendy Mills for the great job she did in assembling and editing this paper for the ISIS Team. NR 87 TC 4 Z9 4 U1 2 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD DEC PY 2016 VL 204 IS 1-4 BP 187 EP 256 DI 10.1007/s11214-014-0059-1 PG 70 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF0XX UT WOS:000390050700006 ER PT J AU Kim, HC Kwon, YS Kim, MR Park, CU Yun, SM Lee, WJ Chong, ST Klein, TA Robbins, RG AF Kim, Heung-Chul Kwon, Young-Soo Kim, Mi-Ran Park, Chang-Uk Yun, Seok-Min Lee, Won-Ja Chong, Sung-Tae Klein, Terry A. Robbins, Richard G. TI Ticks collected from Chilbal Island, Jeollanam Province, Republic of Korea, during 2014-2015 SO SYSTEMATIC AND APPLIED ACAROLOGY LA English DT Article DE Ornithodoros sawaii; Ixodes signatus; Haemaphysalis flava; Synthliboramphus antiquus; Hydrobates monorhis; Korea ID HYDROBATES MONORHIS; CAPENSIS NEUMANN; ARGASIDAE; JAPAN; ACARI; SEABIRDS; IXODIDAE; VIRUS; BIRDS AB The 65th Medical Brigade and Public Health Command District-Korea, in collaboration with the Migratory Birds Center, National Park Research Institute, conducted a migratory bird tick-borne disease surveillance program on Chilbal Island, a small, remote, uninhabited island in southwestern Jeollanam Province, Republic of Korea (ROK), during 2014-2015. Ticks were collected by dragging vegetation and from nest soil and litter of the Ancient Murrelet, Synthliboramphus antiquus, and Swinhoe's Storm Petrel, Hydrobates monorhis, using Tullgren funnels. A total of 115 ticks belonging to three genera and three species were collected. Ornithodoros sawaii (98.3%, 113 ticks) was the most frequently collected tick species, followed by Ixodes signatus (0.9%, 1 nymph) collected from nest soil and litter, and Haemaphysalis flava (0.9%, 1 male) collected by tick drag. C1 [Kim, Heung-Chul] 65th Med Brigade, Multifunct Med Battal 168, Med Detachment 5, Unit 15247, APO, AP 96205 USA. [Kwon, Young-Soo; Kim, Mi-Ran; Park, Chang-Uk; Chong, Sung-Tae] Korea Natl Pk Serv, Korea Natl Pk Res Inst, Migratory Bird Res Ctr, Shinan Gun 58863, Jeonnam Provinc, South Korea. [Yun, Seok-Min; Lee, Won-Ja] Korea Ctr Dis Control & Prevent, Natl Inst Hlth, Ctr Immunol & Pathol, Div Arboviruses, Cheongju 28159, Chungbuk Provin, South Korea. [Klein, Terry A.] MEDDAC K 65th Med Brigade, Unit 15281, APO, AP 96205 USA. [Robbins, Richard G.] MSC, Smithsonian Inst, Walter Reed Biosystemat Unit, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. RP Robbins, RG (reprint author), MSC, Smithsonian Inst, Walter Reed Biosystemat Unit, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM RobbinsRG@si.edu OI Yun, Seok-Min/0000-0003-2087-3661 FU National Institute of Health [2014-ND53001-00]; Korea Centers for Disease Control and Prevention, Cheongju, Chungcheongbuk Province, Republic of Korea; Public Health Command District-Korea; 65th Medical Brigade, Seoul, Korea; Armed Forces Health Surveillance Branch-Global Emerging Infections Surveillance and Response System (AFHSC-GEIS), Silver Spring, MD, USA FX We thank the staff of the Migratory Birds Center, National Park Research Institute, Korea National Park Service, on Heuksan Island, Jeollanam Province, Republic of Korea, for collecting nest soil and litter during seabird conservation and breeding surveys. Tick surveillance was supported by the National Institute of Health (2014-ND53001-00), Korea Centers for Disease Control and Prevention, Cheongju, Chungcheongbuk Province, Republic of Korea; the Public Health Command District-Korea; the 65th Medical Brigade, Seoul, Korea; and the Armed Forces Health Surveillance Branch-Global Emerging Infections Surveillance and Response System (AFHSC-GEIS), Silver Spring, MD, USA. NR 34 TC 0 Z9 0 U1 1 U2 1 PU SYSTEMATIC & APPLIED ACAROLOGY SOC LONDON, NATURAL HISTORY MUSEUM PI LONDON PA DEPT ENTOMOLOGY, LONDON, SW7 5BD, ENGLAND SN 1362-1971 J9 SYST APPL ACAROL-UK JI Syst. Appl. Acarol. PD DEC PY 2016 VL 21 IS 12 BP 1641 EP 1650 DI 10.11158/saa.21.12.5 PG 10 WC Entomology SC Entomology GA EF4YE UT WOS:000390337100005 ER PT J AU Peters, VE Carlo, TA Mello, MAR Rice, RA Tallamy, DW Caudill, SA Fleming, TH AF Peters, Valerie E. Carlo, Tomas A. Mello, Marco A. R. Rice, Robert A. Tallamy, Doug W. Caudill, S. Amanda Fleming, Theodore H. TI Using Plant-Animal Interactions to Inform Tree Selection in Tree-Based Agroecosystems for Enhanced Biodiversity SO BIOSCIENCE LA English DT Article DE connectors; hubs; network theory; phenophase length; restoration ID BRAZILIAN ATLANTIC FOREST; SEED DISPERSAL; COFFEE PLANTATIONS; PEST-CONTROL; BIRD; BATS; DIVERSITY; POLLINATION; MANAGEMENT; ABUNDANCE AB The Neotropical region harbors the world's most diverse terrestrial plant communities. A key component of this diversity is a range of plant-animal interactions involving frugivory, nectarivory, and insectivory. Millions of Neotropical hectares subjected to human land-use systems contain trees that are either planted by land managers or retained from the pre-existing forests. Biodiversity-conservation approaches in these systems are often ineffective because of the unfounded assumption that all plants provide equal benefits for consumers. We propose criteria for tree-species selection based on plant-animal interaction research that could guide decisionmakers. We show that tree-species identity is key for enhancing biodiversity and recommend that selection be guided by the structure of plant-animal interaction networks. We also recommend that selection practices consider the timing of resource production, because the year-round availability of food resources in the Neotropics plays an important role in the adaptive radiation of nectar-and fruit-eating vertebrates. C1 [Peters, Valerie E.] Eastern Kentucky Univ, Dept Biol Sci, Richmond, KY 40475 USA. [Carlo, Tomas A.] Penn State Univ, Dept Biol, University Pk, PA 16802 USA. [Mello, Marco A. R.] Univ Fed Minas Gerais, Dept Gen Biol, Belo Horizonte, MG, Brazil. [Rice, Robert A.; Caudill, S. Amanda] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. [Tallamy, Doug W.] Univ Delaware Newark, Dept Entomol & Wildlife Ecol, Delaware, OH USA. [Fleming, Theodore H.] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. RP Peters, VE (reprint author), Eastern Kentucky Univ, Dept Biol Sci, Richmond, KY 40475 USA. EM valerie.peters@eku.edu; tac17@psu.edu; marmello@gmail.com; ricer@si.edu; dtallamy@udel.edu; CaudillS@si.edu; tedfleming@dakotacom.net NR 77 TC 0 Z9 0 U1 19 U2 19 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD DEC PY 2016 VL 66 IS 12 BP 1046 EP 1056 DI 10.1093/biosci/biw140 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA EE5IZ UT WOS:000389641500007 ER PT J AU Caughlin, TT Graves, SJ Asner, GP van Breugel, M Hall, JS Martin, RE Ashton, MS Bohlman, SA AF Caughlin, T. Trevor Graves, Sarah J. Asner, Gregory P. van Breugel, Michiel Hall, Jefferson S. Martin, Roberta E. Ashton, Mark S. Bohlman, Stephanie A. TI A hyperspectral image can predict tropical tree growth rates in single-species stands SO ECOLOGICAL APPLICATIONS LA English DT Article DE canopy biology; field planting trials; forest dynamics; hyperspectral; light detection and ranging; Panama; plantation; precision forestry; reforestation; remote sensing; tree demography; tropical forest ID PLANTATION FORESTS; SPECTRAL INDEXES; CANOPY; TRAITS; LEAF; SPECTROSCOPY; REGRESSION; FIELD; TEMPERATE; STRESS AB Remote sensing is increasingly needed to meet the critical demand for estimates of forest structure and composition at landscape to continental scales. Hyperspectral images can detect tree canopy properties, including species identity, leaf chemistry and disease. Tree growth rates are related to these measurable canopy properties but whether growth can be directly predicted from hyperspectral data remains unknown. We used a single hyperspectral image and light detection and ranging-derived elevation to predict growth rates for 20 tropical tree species planted in experimental plots. We asked whether a consistent relationship between spectral data and growth rates exists across all species and which spectral regions, associated with different canopy chemical and structural properties, are important for predicting growth rates. We found that a linear combination of narrowband indices and elevation is correlated with standardized growth rates across all 20 tree species (R-2 = 53.70%). Although wavelengths from the entire visible-to-shortwave infrared spectrum were involved in our analysis, results point to relatively greater importance of visible and near-infrared regions for relating canopy reflectance to tree growth data. Overall, we demonstrate the potential for hyperspectral data to quantify tree demography over a much larger area than possible with field-based methods in forest inventory plots. C1 [Caughlin, T. Trevor; Graves, Sarah J.; Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32601 USA. [Asner, Gregory P.; Martin, Roberta E.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [van Breugel, Michiel] Yale NUS Coll, Singapore, Singapore. [van Breugel, Michiel; Hall, Jefferson S.; Bohlman, Stephanie A.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Ashton, Mark S.] Yale Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Caughlin, TT (reprint author), Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32601 USA. EM trevor.caughlin@gmail.com FU Frank Levinson Family Foundation; School of Forestry and Environmental Studies, Yale University; NSF [1415297]; Grantham Foundation for the Protection of the Environment; Avatar Alliance Foundation; Margaret A. Cargill Foundation; David and Lucile Packard Foundation; Gordon and Betty Moore Foundation; W. M. Keck Foundation; John D. and Catherine T. MacArthur Foundation; Andrew Mellon Foundation FX We thank the Carnegie Airborne Observatory and PRORENA staff for data collection and processing support. Funding for PRORENA is from the Frank Levinson Family Foundation and the School of Forestry and Environmental Studies, Yale University. T. T. Caughlin was supported by NSF grant #1415297. Airborne data collection, processing and analysis was funded by the Grantham Foundation for the Protection of the Environment and William R. Hearst III. The Carnegie Airborne Observatory has been made possible by grants and donations to G.P. Asner from the Avatar Alliance Foundation, Margaret A. Cargill Foundation, David and Lucile Packard Foundation, Gordon and Betty Moore Foundation, Grantham Foundation for the Protection of the Environment, W. M. Keck Foundation, John D. and Catherine T. MacArthur Foundation, Andrew Mellon Foundation, Mary Anne Nyburg Baker and G. Leonard Baker Jr, and William R. Hearst III. NR 36 TC 0 Z9 0 U1 14 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD DEC PY 2016 VL 26 IS 8 BP 2367 EP 2373 PG 7 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA EE1BU UT WOS:000389316400001 PM 27907255 ER PT J AU Rodriguez-Ronderos, ME Bohrer, G Sanchez-Azofeifa, A Powers, JS Schnitzer, SA AF Rodriguez-Ronderos, M. Elizabeth Bohrer, Gil Sanchez-Azofeifa, Arturo Powers, Jennifer S. Schnitzer, Stefan A. TI Contribution of lianas to plant area index and canopy structure in a Panamanian forest SO ECOLOGY LA English DT Article DE canopy structure; competition; ground-based LiDAR; LAI-2000; leaf area index (LAI); lianas; light attenuation; Panama; plant area index (PAI); secondary tropical forest; trees; wood area index (WAI) ID REDUCE CARBON ACCUMULATION; TROPICAL RAIN-FOREST; UNCERTAINTY PRINCIPLE; LOWLAND FOREST; COSTA-RICA; DRY FOREST; TREE; DIVERSITY; ABUNDANCE; GROWTH AB Lianas are an important component of tropical forests, where they reduce tree growth, fecundity, and survival. Competition for light from lianas may be intense; however, the amount of light that lianas intercept is poorly understood. We used a large-scale liana-removal experiment to quantify light interception by lianas in a Panamanian secondary forest. We measured the change in plant area index (PAI) and forest structure before and after cutting lianas (for 4 yr) in eight 80mx80m plots and eight control plots (16 plots total). We used ground-based LiDAR to measure the 3-dimensional canopy structure before cutting lianas, and then annually for 2 yr afterwards. Six weeks after cutting lianas, mean plot PAI was 20% higher in control vs. liana removal plots. One yr after cutting lianas, mean plot PAI was similar to 17% higher in control plots. The differences between treatments diminished significantly 2 yr after liana cutting and, after 4 yr, trees had fully compensated for liana removal. Ground-based LiDAR revealed that lianas attenuated light in the upper- and middle-forest canopy layers, and not only in the upper canopy as was previously suspected. Thus, lianas compete with trees by intercepting light in the upper- and mid-canopy of this forest. C1 [Rodriguez-Ronderos, M. Elizabeth; Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, Milwaukee, WI 53203 USA. [Rodriguez-Ronderos, M. Elizabeth] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA. [Rodriguez-Ronderos, M. Elizabeth; Powers, Jennifer S.; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. [Bohrer, Gil; Sanchez-Azofeifa, Arturo] Ohio State Univ, Dept Civil Environm & Geodet Engn, Columbus, OH 43210 USA. [Sanchez-Azofeifa, Arturo] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Sanchez-Azofeifa, Arturo] Univ Alberta, CEOS, Edmonton, AB T6G 2E3, Canada. [Powers, Jennifer S.] Univ Minnesota, Dept Ecol, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Ecol & Behav, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Schnitzer, SA (reprint author), Marquette Univ, Dept Biol Sci, Milwaukee, WI 53203 USA.; Schnitzer, SA (reprint author), Smithsonian Trop Res Inst, Apartado 2072, Balboa, Panama. EM S1@marquette.edu FU U.S. NSF [DEB-0845071, DEB-1019436, DEB-1558093, DEB-1019441]; U.S. DOE Ameriflux Management Project Flux Core Site [7096915] FX We thank S. Perez, O. Valdes, A. Valdes, S. Valdes, B. Bernal, L. Martinez-Izquierdo, M. Garcia-Leon, J. La-Che, K. Maurer, T. Morin, A. Fotis, W. Kenny and A. Matheny for assistance in the field. We are grateful to R. Burnham, K. Barry, and an anonymous reviewer for comments on the manuscript. Financial support was provided by U.S. NSF DEB-0845071, DEB-1019436, and DEB-1558093 (to SAS), DEB-1019441 (to JSP), and the U.S. DOE Ameriflux Management Project Flux Core Site Agreement No. 7096915 (to GB). NR 47 TC 0 Z9 0 U1 14 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD DEC PY 2016 VL 97 IS 12 BP 3271 EP 3277 DI 10.1002/ecy.1597 PG 7 WC Ecology SC Environmental Sciences & Ecology GA EE2WC UT WOS:000389444800003 PM 27912027 ER PT J AU Wasson, K Hughes, BB Berriman, JS Chang, AL Deck, AK Dinnel, PA Endris, C Espinoza, M Dudas, S Ferner, MC Grosholz, ED Kimbro, D Ruesink, JL Trimble, AC Schaaf, DV Zabin, CJ Zacherl, DC AF Wasson, Kerstin Hughes, Brent B. Berriman, John S. Chang, Andrew L. Deck, Anna K. Dinnel, Paul A. Endris, Charlie Espinoza, Michael Dudas, Sarah Ferner, Matthew C. Grosholz, Edwin D. Kimbro, David Ruesink, Jennifer L. Trimble, Alan C. Schaaf, Dick Vander Zabin, Chela J. Zacherl, Danielle C. TI Coast-wide recruitment dynamics of Olympia oysters reveal limited synchrony and multiple predictors of failure SO ECOLOGY LA English DT Article DE biogeography; bivalves; conservation; population cycles; population ecology; regional studies; restoration ID OSTREA-LURIDA CARPENTER; SUPPLY-SIDE ECOLOGY; MARINE POPULATIONS; SOUTHERN CALIFORNIA; INVERTEBRATE LARVAE; LOCAL RECRUITMENT; PATTERNS; CONNECTIVITY; HISTORY; BAY AB Recruitment of new propagules into a population can be a critical determinant of adult density. We examined recruitment dynamics in the Olympia oyster (Ostrea lurida), a species occurring almost entirely in estuaries. We investigated spatial scales of interannual synchrony across 37 sites in eight estuaries along 2,500km of Pacific North American coastline, predicting that high vs. low recruitment years would coincide among neighboring estuaries due to shared exposure to regional oceanographic factors. Such synchrony in recruitment has been found for many marine species and some migratory estuarine species, but has never been examined across estuaries in a species that can complete its entire life cycle within the same estuary. To inform ongoing restoration efforts for Olympia oysters, which have declined in abundance in many estuaries, we also investigated predictors of recruitment failure. We found striking contrasts in absolute recruitment rate and frequency of recruitment failure among sites, estuaries, and years. Although we found a positive relationship between upwelling and recruitment, there was little evidence of synchrony in recruitment among estuaries along the coast, and only limited synchrony of sites within estuaries, suggesting recruitment rates are affected more strongly by local dynamics within estuaries than by regional oceanographic factors operating at scales encompassing multiple estuaries. This highlights the importance of local wetland and watershed management for the demography of oysters, and perhaps other species that can complete their entire life cycle within estuaries. Estuaries with more homogeneous environmental conditions had greater synchrony among sites, and this led to the potential for estuary-wide failure when all sites had no recruitment in the same year. Environmental heterogeneity within estuaries may thus buffer against estuary-wide recruitment failure, analogous to the portfolio effect for diversity. Recruitment failure was correlated with lower summer water temperature, higher winter salinity, and shorter residence time: all indicators of stronger marine influence on estuaries. Recruitment failure was also more common in estuaries with limited networks of nearby adult oysters. Large existing oyster networks are thus of high conservation value, while estuaries that lack them would benefit from restoration efforts to increase the extent and connectivity of sites supporting oysters. C1 [Wasson, Kerstin; Endris, Charlie] Elkhorn Slough Natl Estuarine Res Reserve, 1700 Elkhorn Rd, Santa Cruz, CA 95064 USA. [Wasson, Kerstin; Hughes, Brent B.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, 100 Shaffer Rd, Santa Cruz, CA 95060 USA. [Hughes, Brent B.] Duke Univ, Div Marine Sci & Conservat, Nicholas Sch Environm, Beaufort, NC 28516 USA. [Berriman, John S.] Chapman Univ, Schmid Coll Sci & Technol, Dept Biol Sci, Orange, CA 92866 USA. [Berriman, John S.; Espinoza, Michael; Zacherl, Danielle C.] Calif State Univ Fullerton, Dept Biol Sci MH 282, POB 6850, Fullerton, CA 92834 USA. [Chang, Andrew L.; Zabin, Chela J.] Smithsonian Environm Res Ctr, 3152 Paradise Dr, Tiburon, CA 94920 USA. [Chang, Andrew L.; Deck, Anna K.; Ferner, Matthew C.] San Francisco Bay Natl Estuarine Res Reserve, 3152 Paradise Dr, Tiburon, CA 94920 USA. [Chang, Andrew L.; Deck, Anna K.; Grosholz, Edwin D.; Zabin, Chela J.] Univ Calif Davis, Dept Environm Sci & Policy, One Shields Ave, Davis, CA 95616 USA. [Dinnel, Paul A.] Skagit Cty Marine Resources Comm, 1800 Continental Pl, Washington, DC 98273 USA. [Dudas, Sarah] Vancouver Isl Univ, 900 Fifth St, Nanaimo, BC V9R 5S5, Canada. [Kimbro, David] Northeastern Univ, Dept Marine & Environm Sci, Ctr Marine Sci, Nahant, MA 01908 USA. [Ruesink, Jennifer L.; Trimble, Alan C.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Schaaf, Dick Vander] Nature Conservancy, 821 SE 14th Ave, Portland, OR 97214 USA. RP Wasson, K (reprint author), Elkhorn Slough Natl Estuarine Res Reserve, 1700 Elkhorn Rd, Santa Cruz, CA 95064 USA.; Wasson, K (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, 100 Shaffer Rd, Santa Cruz, CA 95060 USA. EM Kerstin.Wasson@gmail.com RI Chang, Andrew/J-8058-2016 OI Chang, Andrew/0000-0002-7870-285X FU David H. Smith Research Conservation Fellowship; NOAA Coastal Zone Management Administration Award; Environmental Protection Agency's Puget Sound Partnership; Taylor Shellfish Company; Puget Sound Restoration Fund; Andrew W. Mellon Foundation; Washington Sea [R/LME-3]; California Sea Grant; UC EIPD Program; Ocean Sciences Trust; Point Reyes National Seashore; UC Marine Council Fellowship; Bodega Marine Laboratory; NSF-UMEB [0102614, 0602922]; CSU Fullerton Faculty-Undergraduate Student Support Initiative; CSU Fullerton General Faculty Research Award FX We are indebted to P. Raimondi for extensive support of the statistical analyses, from conceptualization to implementation. Two reviewers and the editor provided helpful suggestions that improved the analyses and writing. We are grateful to a large number of students and community volunteers who helped collect the data across all our sites, especially S. Attoe, A. Baukus, C. Coleman-Hulbert, A. Hettinger, S. Murphy, B. Steves, and several Zacherl lab students. The National Estuarine Research Reserve System Science Collaborative and NOAA's Office of Coastal Management supported data collection and analysis at Elkhorn Slough and San Francisco Bay. The following grants or organizations supported work by particular authors: David H. Smith Research Conservation Fellowship (B. B. Hughes); NOAA Coastal Zone Management Administration Award, Environmental Protection Agency's Puget Sound Partnership, Taylor Shellfish Company, and Puget Sound Restoration Fund (P. A. Dinnel); Andrew W. Mellon Foundation and Washington Sea Grant R/LME-3 (J. L. Ruesink and A. C. Trimble); California Sea Grant (E. D. Grosholz and C. J. Zabin); UC EIPD Program (E. D. Grosholz); Ocean Sciences Trust (E. D. Grosholz and C. J. Zabin), Point Reyes National Seashore (D. L. Kimbro and E. D. Grosholz); UC Marine Council Fellowship (D. L. Kimbro), Bodega Marine Laboratory (D. L. Kimbro); NSF-UMEB grants #0102614 and #0602922 (to students L. Sam, E. Casillas, S. Pfremmer, and A. Cisneros), CSU Fullerton Faculty-Undergraduate Student Support Initiative (D. C. Zacherl), CSU Fullerton General Faculty Research Award (D. C. Zacherl). NR 67 TC 0 Z9 0 U1 7 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD DEC PY 2016 VL 97 IS 12 BP 3503 EP 3516 DI 10.1002/ecy.1602 PG 14 WC Ecology SC Environmental Sciences & Ecology GA EE2WC UT WOS:000389444800027 PM 27912012 ER PT J AU Lu, M Caplan, JS Bakker, JD Langley, JA Mozdzer, TJ Drake, BG Megonigal, JP AF Lu, Meng Caplan, Joshua S. Bakker, Jonathan D. Langley, J. Adam Mozdzer, Thomas J. Drake, Bert G. Megonigal, J. Patrick TI Allometry data and equations for coastal marsh plants SO ECOLOGY LA English DT Article; Data Paper DE allometric equations; biomass estimation; coastal wetlands; elevated CO2; nitrogen pollution; plant allometry AB Coastal marshes are highly valued for ecosystem services such as protecting inland habitats from storms, sequestering carbon, removing nutrients and other pollutants from surface water, and providing habitat for fish, shellfish, and birds. Because plants largely determine the structure and function of coastal marshes, quantifying plant biomass is essential for evaluating these ecosystem services, understanding the biogeochemical processes that regulate ecosystem function, and forecasting tidal wetland responses to accelerated sea level rise. Allometry is a convenient and efficient technique for nondestructive estimation of plant biomass, and it is commonly used in studies of carbon and nitrogen cycles, energy flows, and marsh surface elevation change. We present plant allometry data and models developed for three long-term experiments at the Smithsonian Global Change Research Wetland, a brackish marsh in the Rhode River subestuary of the Chesapeake Bay. The dataset contains 9,771 measurements of stem height, dry mass, and (in 9638 cases) stem width across 11 plant species. The vast majority of observations are for Schoenoplectus americanus (8430) and Phragmites australis (311), with fewer observations for other common species: Amaranthus cannabinus, Atriplex patula, Iva frutescens, Kosteletzkya virginica, Polygonum hydropiper, Solidago sempervirens, Spartina alterniflora, Spartina cynosuroides, and Typha angustifolia. Allometric relationships take the form of linear regressions of biomass (transformed using the Box-Cox procedure) on either stem height and width, or on stem height alone. Allometric relationships for Schoenoplectus americanus were not meaningfully altered by elevated CO2, N enrichment, the community context, interannual variation in climate, or year, showing that a single equation can be used across a broad range of conditions for this species. Archived files include: (1) raw data used to derive allometric equations for each species, (2) reports and evaluations of the allometric equations we derived from the data, and (3) R code with which our derivations can be replicated. Methodological details of our experiments, data collection efforts, and statistical modeling are described in the metadata. The allometric equations can be used for biomass estimation in empirical and modeling studies of North American coastal wetlands, and the data can be used in ecological studies of terrestrial plant allometry. C1 [Lu, Meng; Caplan, Joshua S.; Langley, J. Adam; Mozdzer, Thomas J.; Drake, Bert G.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. [Caplan, Joshua S.; Mozdzer, Thomas J.] Bryn Mawr Coll, Dept Biol, 101 N Merion Ave, Bryn Mawr, PA 19010 USA. [Bakker, Jonathan D.] Univ Washington, Sch Environm & Forest Sci, Box 354115, Seattle, WA 98195 USA. [Langley, J. Adam] Villanova Univ, Dept Biol, 800 Lancaster Ave, Villanova, PA 19085 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM megonigalp@si.edu NR 0 TC 0 Z9 0 U1 22 U2 22 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD DEC PY 2016 VL 97 IS 12 BP 3554 EP 3554 DI 10.1002/ecy.1600 PG 1 WC Ecology SC Environmental Sciences & Ecology GA EE2WC UT WOS:000389444800032 PM 27911995 ER PT J AU Melo, BF Vari, RP Oliveira, C AF Melo, Bruno F. Vari, Richard P. Oliveira, Claudio TI Curimatopsis maculosa, a new species from the Rio Tapajos, Amazon basin, Brazil (Teleostei: Curimatidae) SO ICHTHYOLOGICAL EXPLORATION OF FRESHWATERS LA English DT Article ID CHARACIFORMES CURIMATIDAE; FISHES AB Curimatopsis maculosa, new species, is described from the middle portion of the Rio Tapajos, a southern tributary of the Rio Amazonas. It differs from all congeners by the presence of a pointed small, rotund spot of dark pigmentation overlying the posterior most midlateral scales and the base of the middle caudal-fin rays together with morphometric and meristic features. It shares two synapomorphies with C. macrolepis and C. microlepis, related to the postorbital portion of head and an upturned mouth, and is hypothesized to be most closely related to those species. C1 [Melo, Bruno F.; Oliveira, Claudio] Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Distr Rubiao Jr S-N, BR-18618970 Botucatu, SP, Brazil. [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MCR 159,Box, Washington, DC 20013 USA. RP Melo, BF (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Distr Rubiao Jr S-N, BR-18618970 Botucatu, SP, Brazil. EM melo@ibb.unesp.br RI Gesseff, Ednilson/A-3019-2017 FU FAPESP [2011/08374-1, 2013/16436-2]; CNPq [140193/2015-4]; National Science Foundation [DEB-1257898] FX We thank Francisco Langeani (DZSJRP), Alessi Datovo and Michel D. Gianeti (MZUSP), and Lucia R. Py-Daniel and Renildo R. Oliveira (INPA) for curatorial assistance and the loan of specimens. Thanks to Ricardo C. Benine and Valter M. A. Santos for their assistance in obtaining part of the type series and to Ricardo Britzke who provided the habitat photograph and information. Research was supported by grants from FAPESP 2011/08374-1, 2013/16436-2 and CNPq 140193/2015-4 (BFM and CO) and the National Science Foundation DEB-1257898 (RPV). NR 19 TC 0 Z9 0 U1 7 U2 7 PU VERLAG DR FRIEDRICH PFEIL PI MUNICH PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY SN 0936-9902 J9 ICHTHYOL EXPLOR FRES JI Ichthyol. Explor. Freshw. PD DEC PY 2016 VL 27 IS 4 BP 303 EP 308 PG 6 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA EE4HR UT WOS:000389563400003 ER PT J AU Tanpradit, N Chatdarong, K Comizzoli, P AF Tanpradit, Nae Chatdarong, Kaywalee Comizzoli, Pierre TI Carbonyl cyanide 4-(trifluoromethoxy)phenylhydrazone (FCCP) pre-exposure ensures follicle integrity during in vitro culture of ovarian tissue but not during cryopreservation in the domestic cat model SO JOURNAL OF ASSISTED REPRODUCTION AND GENETICS LA English DT Article DE Carbonyl cyanide 4-(trifluoromethoxy)phenylhydrazone (FCCP); Domestic cat; Ovarian tissue; In vitro culture; Mitochondrialmembrane potential; Follicular viability ID STROMAL CELL-PROLIFERATION; OXYGEN SPECIES PRODUCTION; PRIMORDIAL FOLLICLES; DEVELOPMENTAL COMPETENCE; MITOCHONDRIAL UNCOUPLER; FERTILITY PRESERVATION; PREANTRAL FOLLICLES; PLASMA-MEMBRANE; TRANSPLANTATION; VITRIFICATION AB Temporary and reversible downregulation of metabolism may improve the survival of tissues exposed to non-physiological conditions during transport, in vitro culture, and cryopreservation. The objectives of the study were to (1) optimize the concentration and duration of carbonyl cyanide 4-(trifluoromethoxy)phenylhydrazone (FCCP-a mitochondrial uncoupling agent) exposures for biopsies of domestic cat ovarian tissue and (2) examine the effects of FCCP pre-exposures on follicle integrity after tissue culture and/or cryopreservation. Biopsies of cat ovarian tissue were first treated with various concentrations of FCCP (0, 10, 40, or 200 nM) for 10 or 120 min to determine the most suitable pre-exposure conditions. Based on these results, tissues were pre-exposed to 200 nM FCCP for 120 min for the subsequent studies on culture and cryopreservation. In all experiments and for each treatment group, tissue activity and integrity were measured by mitochondrial membrane potential (relative optical density of rhodamine 123 fluorescence), follicular viability (calcein assay), follicular morphology (histology), granulosa cell proliferation (Ki-67 immunostaining), and follicular density. Ovarian tissues incubated with 200 nM FCCP for 120 min led to the lowest mitochondrial activity (1.17 +/- 0.09; P < 0.05) compared to control group (0 nM; 1.30 +/- 0.12) while maintaining a constant percentage of viable follicles (75.3 +/- 7.8 %) similar to the control group (71.8 +/- 11.7 %; P > 0.05). After 2 days of in vitro culture, percentage of viable follicles (78.8 +/- 8.9 %) in similar pre-exposure conditions was higher (P < 0.05) than in the absence of FCCP (61.2 +/- 12.0 %) with percentages of morphologically normal follicles (57.6 +/- 17.3 %) not different from the fresh tissue (70.2 +/- 7.1 %; P > 0.05). Interestingly, percentages of cellular proliferation and follicular density were unaltered by the FCCP exposures. Based on the indicators mentioned above, the FCCP-treated tissue fragments did not have a better follicle integrity after freezing and thawing. Pre-exposure to 200 nM FCCP during 120 min protects and enhances the follicle integrity in cat ovarian tissue during short-term in vitro culture. However, FCCP does not appear to exert a beneficial or detrimental effect during ovarian tissue cryopreservation. C1 [Tanpradit, Nae; Chatdarong, Kaywalee] Chulalongkorn Univ, Dept Obstet Gynaecol & Reprod, Fac Vet Sci, Bangkok 10330, Thailand. [Comizzoli, Pierre] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Comizzoli, P (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. EM comizzolip@si.edu FU Royal Golden Jubilee Ph.D. Program [PHD/0199/2552]; Chulalongkorn University Fund (Ratchadaphiseksomphot Endowment Fund); Research Unit of Obstetrics and Reproduction in Animals, Chulalongkorn University FX Financial support for this work was provided by the Royal Golden Jubilee Ph.D. Program (PHD/0199/2552), the 90th Anniversary of Chulalongkorn University Fund (Ratchadaphiseksomphot Endowment Fund), and Research Unit of Obstetrics and Reproduction in Animals, Chulalongkorn University. NR 53 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1058-0468 EI 1573-7330 J9 J ASSIST REPROD GEN JI J. Assist. Reprod. Genet. PD DEC PY 2016 VL 33 IS 12 BP 1621 EP 1631 DI 10.1007/s10815-016-0810-5 PG 11 WC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology SC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology GA EF0OJ UT WOS:000390025000011 PM 27639998 ER PT J AU Martinez-Polanco, MF AF Fernanda Martinez-Polanco, Maria TI THE GUINEA PIG (CAVIA SP.), A KEY FOOD RESOURCE IN AGUAZUQUE, AN ARCHEOLOGICAL SITE OF THE SAVANNAH IN BOGOTA, COLOMBIA SO LATIN AMERICAN ANTIQUITY LA Spanish DT Article ID HUMAN CONSUMPTION; DIET; MANAGEMENT; DIVERSITY; FORAGERS; BASIN; PERU C1 [Fernanda Martinez-Polanco, Maria] Smithsonian Trop Res Inst, Lab Arqueol, Edificio 352, Ciudad De Panama, Panama. RP Martinez-Polanco, MF (reprint author), Smithsonian Trop Res Inst, Lab Arqueol, Edificio 352, Ciudad De Panama, Panama. EM mfmartinezp@gmail.com NR 62 TC 0 Z9 0 U1 0 U2 0 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD DEC PY 2016 VL 27 IS 4 BP 512 EP 526 DI 10.7183/1045-6635.27.4.512 PG 15 WC Archaeology SC Archaeology GA EE5YB UT WOS:000389684400005 ER PT J AU Hong, T AF Hong, Terry TI A Separation SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD DEC PY 2016 VL 141 IS 20 BP 85 EP 85 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA EE2FA UT WOS:000389397900089 ER PT J AU Werding, B Christensen, B Hiller, A AF Werding, Bernd Christensen, Bent Hiller, Alexandra TI Three way symbiosis between a goby, a shrimp, and a crab SO MARINE BIODIVERSITY LA English DT Article DE Goby-shrimp association; Gobiidae; Alpheidae; Porcellanidae; Symbiosis; Indo-West Pacific ID DECAPODA; CRUSTACEA; ANOMURA; PORCELLANIDAE; PACIFIC; PETROLISTHES; GOBIIDAE; ECOLOGY; GENUS AB A unique case of triple symbiosis between a goby, a pistol shrimp, and a porcellanid crab sharing the same burrow close to reef patches in Lembeh Strait, Indonesia, is described from direct observations for the first time. The burrow, typically occupied by shrimps and gobies, is shared with the porcellanid Enosteoides lobatus. In the goby-shrimp association, the fish inhabits the burrow, which is constructed and kept clean by the shrimp, and the fish warns the shrimp of potential dangers approaching their refuge. The porcellanid lives in the burrow and also benefits from living in a habitat where it could not survive without the two sentinel species. Because the limiting resource for the suspension-feeding porcellanid is protected space, this liaison is an adaptation by E. lobatus to a symbiotic life in a habitat that protects it from predation, and is optimal for filter feeding. C1 [Werding, Bernd] Justus Liebig Univ Giessen, Inst Allgemenie & Spezielle Zool, Heinrich Buff Ring 26-32, D-35392 Giessen, Germany. [Christensen, Bent] Umea Univ, Dept Ecol & Environm Sci, SE-90187 Umea, Sweden. [Hiller, Alexandra] Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. RP Hiller, A (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM hillera@si.edu FU Smithsonian grant FX NAD-Lembeh, Indonesia, graciously provided to B.C extensive logistic help. H.A. Lessios (STRI) critically read an earlier draft of this mansucript. I. Karplus (Agricultural Research Organization - ARO, Volcani Center, Israel) reviewed this manuscript and kindly helped with identification of fish species. A. Anker (Universidade Federal do Ceara, Brazil) helped identifying the alpheid species. L. Corbari (Museum National d'Histoire Naturelle, Paris, France) provided us with porcellanid material. We thank the editor and reviewers for their contributions to improve this manuscript. This study was supported by a Smithsonian grant to A.H. NR 35 TC 0 Z9 0 U1 16 U2 16 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1867-1616 EI 1867-1624 J9 MAR BIODIVERS JI Mar. Biodivers. PD DEC PY 2016 VL 46 IS 4 BP 897 EP 900 DI 10.1007/s12526-016-0453-x PG 4 WC Biodiversity Conservation; Marine & Freshwater Biology SC Biodiversity & Conservation; Marine & Freshwater Biology GA EF0FW UT WOS:000390002100017 ER PT J AU Wolfe, BT Sperry, JS Kursar, TA AF Wolfe, Brett T. Sperry, John S. Kursar, Thomas A. TI Does leaf shedding protect stems from cavitation during seasonal droughts? A test of the hydraulic fuse hypothesis SO NEW PHYTOLOGIST LA English DT Article DE drought deciduousness; hydraulic limitation; hydraulic segmentation hypothesis; leaf abscission; leaf phenology; seasonally dry tropical forest; xylem cavitation ID TROPICAL DRY FOREST; XYLEM VULNERABILITY; WATER-STRESS; COSTA-RICA; DECIDUOUS FOREST; CANOPY TREES; WOODY-PLANTS; PHENOLOGY; EMBOLISM; CONDUCTIVITY AB During droughts, leaves are predicted to act as 'hydraulic fuses' by shedding when plants reach critically low water potential (Toant), thereby slowing water loss, stabilizing T plan I and protecting against cavitation-induced loss of stem hydraulic conductivity (K-s). We tested these predictions among trees in seasonally dry tropical forests, where leaf shedding is common, yet variable, among species. We tracked leaf phenology, Toara and K-s in saplings of six tree species distributed across two forests. Species differed in their timing and extent of leaf shedding, yet converged in shedding leaves as they approached the Toa,,t value associated with a 50% loss of K-s and at which their model-estimated maximum sustainable transpiration rate approached zero. However, after shedding all leaves, the Toat value of one species, Genipa americana, continued to decline, indicating that water loss continued after leaf shedding. K-s was highly variable among saplings within species and seasons, suggesting a minimal influence of seasonal drought on K-s. Hydraulic limits appear to drive diverse patterns of leaf shedding among tropical trees, supporting the hydraulic fuse hypothesis. However, leaf shedding is not universally effective at stabilizing Toant, suggesting that the main function of drought deciduousness may vary among species. C1 [Wolfe, Brett T.; Sperry, John S.; Kursar, Thomas A.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Wolfe, Brett T.; Kursar, Thomas A.] Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Anton, Panama. RP Wolfe, BT (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA.; Wolfe, BT (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Anton, Panama. EM btwolfe@gmail.com FU Smithsonian Tropical Research Institute; NSF [DEB-0444590]; University of Utah (UU); UU Global Change and Sustain ability Center grant; National Science Foundation (NSF) GK-12 Program fellowship fiom the UU's Think Globally Teach Locally Program FX B.T.W. was supported by a short-term fellowship from the Smithsonian Tropical Research Institute, a University of Utah (UU) Graduate Research Fellowship, a UU Global Change and Sustain ability Center grant and a National Science Foundation (NSF) GK-12 Program fellowship fiom the UU's Think Globally Teach Locally Program. Funding was provided by NSF grant DEB-0444590 to T.A.K. We thank Joe Wright for advice and support, Sarah Bruemmer for laboratory assistance, and Parque Natural Metropolitano and Eugene Eisenimum Reserve for study site access. NR 60 TC 1 Z9 1 U1 18 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD DEC PY 2016 VL 212 IS 4 BP 1007 EP 1018 DI 10.1111/nph.14087 PG 12 WC Plant Sciences SC Plant Sciences GA ED9KQ UT WOS:000389189100001 PM 27373446 ER PT J AU Ellis, KS Jehl, JR Knight, RN Marvel, KS Larsen, RT AF Ellis, Kristen S. Jehl, Joseph R., Jr. Knight, Robert N. Marvel, Keeli S. Larsen, Randy T. TI Spring Downings Clarify the Migration Biology of Eared Grebes (Podiceps nigricollis) SO WATERBIRDS LA English DT Article DE downing; Eared Grebe; Great Salt Lake; migration; mortality; Podiceps nigricollis ID MASS-MORTALITY EVENTS; POPULATION; UTAH AB Eared Grebes (Podiceps nigricollis) staging at the Great Salt Lake, Utah, USA, sometimes experience weather-induced downings where many individuals are killed. Downings of Eared Grebes moving south during the fall have been reported for decades; however, spring downings are rare and underrepresented in the literature. On 15 April 2013, 13,500 Eared Grebes flying northward encountered inclement weather, were attracted to lights on Dugway Proving Ground, and downed. This spring downing was documented, and population characteristics were compared with those observed in previous downings. An estimated 38% were killed outright. Rescue efforts promoted the survival of 88% of those not killed on impact. Grebes that were 9-10 months old were, on average, 10% lighter than adults in the same flight, perhaps indicating slow growth or age differences in foraging efficiency. Adults dominated all downings, supporting previous information that adults and young migrate on different schedules. The sex ratio in the North American population appears to be 1:1. Downings occur when Eared Grebes encounter inclement weather and are attracted to lights. Knowledge of the route, migration period, and flight speed of Eared Grebes allows predictions about when and where downings are likely to occur. Reducing the number and intensity of lights on snowy nights in high risk areas may decrease mortality. C1 [Ellis, Kristen S.] Brigham Young Univ, Plant & Wildlife Sci Dept, 4112 Life Sci Bldg, Provo, UT 84602 USA. [Jehl, Joseph R., Jr.] US Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20560 USA. [Knight, Robert N.; Marvel, Keeli S.] US Army Dugway Proving Ground, Environm Programs, Dugway, UT 84022 USA. [Larsen, Randy T.] Brigham Young Univ, Plant & Wildlife Sci Dept, 5046 Life Sci Bldg, Provo, UT 84602 USA. [Larsen, Randy T.] Brigham Young Univ, Monte L Bean Life Sci Museum, 5046 Life Sci Bldg, Provo, UT 84602 USA. RP Ellis, KS (reprint author), Brigham Young Univ, Plant & Wildlife Sci Dept, 4112 Life Sci Bldg, Provo, UT 84602 USA. EM kristensue.ellis@gmail.com NR 31 TC 0 Z9 0 U1 0 U2 0 PU WATERBIRD SOC PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 1524-4695 EI 1938-5390 J9 WATERBIRDS JI Waterbirds PD DEC PY 2016 VL 39 IS 4 BP 338 EP 345 PG 8 WC Ornithology SC Zoology GA EE9SH UT WOS:000389966000002 ER PT J AU Hartman, JD Bakos, GA Bhatti, W Penev, K Bieryla, A Latham, DW Kovacs, G Torres, G Csubry, Z de Val-Borro, M Buchhave, L Kovacs, T Quinn, S Howard, AW Isaacson, H Fulton, BJ Everett, ME Esquerdo, G Beky, B Szklenar, T Falco, E Santerne, A Boisse, I Hebrard, G Burrows, A Lazar, J Papp, I Sari, P AF Hartman, J. D. Bakos, G. A. Bhatti, W. Penev, K. Bieryla, A. Latham, D. W. Kovacs, G. Torres, G. Csubry, Z. de Val-Borro, M. Buchhave, L. Kovacs, T. Quinn, S. Howard, A. W. Isaacson, H. Fulton, B. J. Everett, M. E. Esquerdo, G. Beky, B. Szklenar, T. Falco, E. Santerne, A. Boisse, I. Hebrard, G. Burrows, A. Lazar, J. Papp, I. Sari, P. TI HAT-P-65b AND HAT-P-66b: TWO TRANSITING INFLATED HOT JUPITERS AND OBSERVATIONAL EVIDENCE FOR THE REINFLATION OF CLOSE-IN GIANT PLANETS SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: individual (HAT-P-65, GSC 1111-00383, HAT-P-66, GSC 3814-00307) techniques: photometric; techniques: spectroscopic ID SOLAR-TYPE STAR; METAL-POOR STAR; BRIGHT F-STAR; RISE LIGHT CURVES; SUN-LIKE STAR; K-DWARF STAR; LOW-DENSITY; EXTRASOLAR PLANET; ECCENTRIC ORBIT; KEPLER FIELD AB We present the discovery of the transiting exoplanets HAT-P-65b and HAT-P-66b, with orbital periods of 2.6055 and 2.9721 days, masses of 0.527 +/- 0.083 M-J and 0.783 +/- 0.057 M-J, and inflated radii of 1.89 +/- 0.13 R-J and 1.59(-0.10)(+0.16) R-J, respectively. They orbit moderately bright (V = 13.145 +/- 0.029 and V = 12.993 +/- 0.052) stars of mass 1.212 +/- 0.050 M-circle dot and 1.255(-0.054)(-0.107) M-circle dot. The stars are at the main-sequence turnoff. While it is well known that the radii of close-in giant planets are correlated with their equilibrium temperatures, whether or not the radii of planets increase in time as their hosts evolve and become more luminous is an open question. Looking at the broader sample of well-characterized close-in transiting giant planets, we find that there is a statistically significant correlation between planetary radii and the fractional ages of their host stars, with a false-alarm probability of only 0.0041%. We find that the correlation between the radii of planets and the fractional ages of their hosts is fully explained by the known correlation between planetary radii and their present-day equilibrium temperatures; however, if the zero-age main-sequence equilibrium temperature is used in place of the present-day equilibrium temperature, then a correlation with age must also be included to explain the planetary radii. This suggests that, after contracting during the pre-main-sequence, close-in giant planets are reinflated over time due to the increasing level of irradiation received from their host stars. Prior theoretical work indicates that such a dynamic response to irradiation requires a significant fraction of the incident energy to be deposited deep within the planetary interiors. C1 [Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Penev, K.; Csubry, Z.; de Val-Borro, M.; Burrows, A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bieryla, A.; Latham, D. W.; Torres, G.; Esquerdo, G.; Falco, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kovacs, G.; Kovacs, T.] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary. [Buchhave, L.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Quinn, S.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Howard, A. W.; Fulton, B. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Isaacson, H.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Everett, M. E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Szklenar, T.] Hungarian Astron Assoc, Budapest, Hungary. [Boisse, I.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Santerne, A.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, PT-4150762 Oporto, Portugal. [Hebrard, G.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, 98bis Blvd Arago, F-75014 Paris, France. [Beky, B.] Google, Googleplex, 1600 Amphitheatre Pkwy, Mountain View, CA 94043 USA. RP Hartman, JD (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. EM jhartman@astro.princeton.edu OI Bakos, Gaspar/0000-0001-7204-6727; Hartman, Joel/0000-0001-8732-6166; Latham, David/0000-0001-9911-7388 FU NASA [NNG04GN74G, NNX13AJ15G, NNX09AB29G, NNX14AE87G, NNX13AQ62G]; NSF [AST-1108686]; Kepler Mission under NASA [NCC2-1390]; European Union [627202]; Fundacao para a Ciencia e a Tecnologia (FCT, Portugal) [UID/FIS/04434/2013]; FEDER [POCI-01-0145-FEDER-007672] FX HATNet operations have been funded by NASA grants NNG04GN74G and NNX13AJ15G. Follow-up of HATNet targets has been partially supported through NSF grant AST-1108686. G.A.B., Z.C., and K.P. acknowledge partial support from NASA grant NNX09AB29G. J.H. acknowledges support from NASA grant NNX14AE87G. K.P. acknowledges support from NASA grant NNX13AQ62G. We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (DWL, PI). A.S. is supported by the European Union under a Marie Curie Intra-European Fellowship for Career Development with reference FP7-PEOPLE-2013-IEF, number 627202. Part of this work was supported by Fundacao para a Ciencia e a Tecnologia (FCT, Portugal, ref. UID/FIS/04434/2013) through national funds and by FEDER through COMPETE2020 (ref. POCI-01-0145-FEDER-007672). Data presented in this paper are based on observations obtained at the HAT station at the Submillimeter Array of SAO and the HAT station at the Fred Lawrence Whipple Observatory of SAO. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and the National Optical Astronomy Observatory. This work was supported by a NASA WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. We gratefully acknowledge R. W. Noyes for his many contributions to the HATNet transit survey, and we also gratefully acknowledge contributions from J. Johnson and from G. Marcy to the collection and reduction of the Keck/HIRES observations presented here. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 231 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 182 DI 10.3847/0004-6256/152/6/182 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EE1FT UT WOS:000389327100011 ER PT J AU Stassun, KG Torres, G AF Stassun, Keivan G. Torres, Guillermo TI ECLIPSING BINARY STARS AS BENCHMARKS FOR TRIGONOMETRIC PARALLAXES IN THE GAIA ERA SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; catalogs; methods: observational; parallaxes; stars: distances ID STELLAR EVOLUTION MODELS; LINED SPECTROSCOPIC BINARIES; AUTOMATED SURVEY CATALOG; ABSOLUTE PROPERTIES; MAIN-SEQUENCE; OPEN CLUSTERS; PHYSICAL PARAMETERS; MAGELLANIC-CLOUD; PHOTOMETRIC ANALYSIS; HIPPARCOS DISTANCES AB We present fits to the broadband photometric spectral energy distributions (SEDs) of 158 eclipsing binaries (EBs) in the Tycho-2 catalog. These EBs were selected because they have highly precise stellar radii, effective temperatures, and in many cases metallicities previously determined in the literature, and thus have bolometric luminosities that are typically good to less than or similar to 10%. In most cases the available broadband photometry spans a wavelength range 0.4-10 mu m, and in many cases spans 0.15-22 mu m. The resulting SED fits, which have only extinction as a free parameter, provide a virtually model-independent measure of the bolometric flux at Earth. The SED fits are satisfactory for 156 of the EBs, for which we achieve typical precisions in the bolometric flux of approximate to 3%. Combined with the accurately known bolometric luminosity, the result for each EB is a predicted parallax that is typically precise to less than or similar to 5%. These predicted parallaxes-with typical uncertainties of 200 mu as-are 4-5 times more precise than those determined by Hipparcos for 99 of the EBs in our sample, with which we find excellent agreement. There is no evidence among this sample for significant systematics in the Hipparcos parallaxes of the sort that notoriously afflicted the Pleiades measurement. The EBs are distributed over the entire sky, span more than 10 mag in brightness, reach distances of more than 5 kpc, and in many cases our predicted parallaxes should also be more precise than those expected from the Gaia first data release. The EBs studied here can thus serve as empirical, independent benchmarks for these upcoming fundamental parallax measurements. C1 [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr Ln, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, 1000 17th Ave N, Nashville, TN 37208 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Stassun, KG (reprint author), Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr Ln, Nashville, TN 37235 USA.; Stassun, KG (reprint author), Fisk Univ, Dept Phys, 1000 17th Ave N, Nashville, TN 37208 USA. EM keivan.stassun@vanderbilt.edu OI Stassun, Keivan/0000-0002-3481-9052 FU NSF [AST-1358862, AST-1509375] FX KGS acknowledges partial support from NSF PAARE grant AST-1358862. GT acknowledges partial support from NSF grant AST-1509375. This work made extensive use of the Filtergraph data visualization system (Burger et al. 2013) at.filtergraph.vanderbilt.edu. NR 105 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 180 DI 10.3847/0004-6256/152/6/180 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EE1FT UT WOS:000389327100009 ER PT J AU Trilling, DE Mommert, M Hora, J Chesley, S Emery, J Fazio, G Harris, A Mueller, M Smith, H AF Trilling, David E. Mommert, Michael Hora, Joseph Chesley, Steve Emery, Joshua Fazio, Giovanni Harris, Alan Mueller, Michael Smith, Howard TI NEOSURVEY 1: INITIAL RESULTS FROM THE WARM SPITZER EXPLORATION SCIENCE SURVEY OF NEAR-EARTH OBJECT PROPERTIES SO ASTRONOMICAL JOURNAL LA English DT Article DE catalogs; infrared: planetary systems; minor planets, asteroids: general; surveys ID NEOWISE REACTIVATION MISSION; KUIPER-BELT OBJECTS; PHYSICAL-CHARACTERIZATION; ABSOLUTE MAGNITUDES; ASTEROID POPULATION; SPACE-TELESCOPE; THERMAL-MODEL; ALBEDO; CHELYABINSK; PERFORMANCE AB Near-Earth objects (NEOs) are small solar system bodies whose orbits bring them close to the Earth's orbit. We are carrying out a Warm Spitzer Cycle. 11 Exploration Science program entitled NEOSurvey-a fast and efficient flux-limited survey of 597. known NEOs in which we derive a diameter and albedo for each target. The vast majority of our targets are too faint to be observed by NEOWISE, though a small sample has been or will be observed by both observatories, which allows for a cross-check of our mutual results. Our primary goal is to create a large and uniform catalog of NEO properties. We present here the first results from this new program: fluxes and derived diameters and albedos for 80 NEOs, together with a description of the overall program and approach, including several updates to our thermal model. The largest source of error in our diameter and albedo solutions, which derive from our single-band thermal emission measurements, is uncertainty in eta, the beaming parameter used in our thermal modeling; for albedos, improvements in solar system absolute magnitudes would also help significantly. All data and derived diameters and albedos from this entire program are being posted on a publicly accessible Web page at nearearthobjects. nau. edu C1 [Trilling, David E.; Mommert, Michael] No Arizona Univ, Dept Phys & Astron, POB 6010, Flagstaff, AZ 86011 USA. [Hora, Joseph; Fazio, Giovanni; Smith, Howard] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-65, Cambridge, MA 02138 USA. [Chesley, Steve] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Emery, Joshua] Univ Tennessee, Dept Earth & Planetary Sci, 306 EPS Bldg,1412 Circle Dr, Knoxville, TN 37996 USA. [Harris, Alan] German Aerosp Ctr DLR, Inst Planetary Res, Rutherfordstr 2, D-12489 Berlin, Germany. [Mueller, Michael] SRON Netherlands Inst Space Res, SRON, POB 800, NL-9700 AV Groningen, Netherlands. [Mueller, Michael] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. RP Trilling, DE (reprint author), South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa.; Trilling, DE (reprint author), Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa. OI Chesley, Steven/0000-0003-3240-6497 FU Arizona's Technology and Research Initiative Fund; NASA FX We acknowledge the thorough and prompt hard work of the staff at the Spitzer Science Center, without whom the execution of this program would not be possible. We also appreciate the support that NASA's Planetary Science Division and Solar System Observations program provide for the Spitzer mission and its NEO observations. We thank two anonymous referees for their detailed comments that improved this paper. We also thank Scott Gaudi for useful advice. Some of the computational analyses were run on Northern Arizona University's monsoon computing cluster, funded by Arizona's Technology and Research Initiative Fund. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by JPL/Caltech under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We make use of data from the AstDys database, as well as extensive use of the JPL/Horizons system. NR 51 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 172 DI 10.3847/0004-6256/152/6/172 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EE1FT UT WOS:000389327100001 ER PT J AU Cleeves, LI Oberg, KI Wilner, DJ Huang, J Loomis, RA Andrews, SM Czekala, I AF Cleeves, L. Ilsedore Oberg, Karin I. Wilner, David J. Huang, Jane Loomis, Ryan A. Andrews, Sean M. Czekala, Ian TI THE COUPLED PHYSICAL STRUCTURE OF GAS AND DUST IN THE IM Lup PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; astrochemistry; circumstellar matter; stars: individual (IM Lup); stars: pre-main sequence; techniques: imaging spectroscopy ID T-TAURI STARS; RADIATIVE-TRANSFER; FAR-ULTRAVIOLET; X-RAY; PROTOSTELLAR DISKS; H-2 FLUORESCENCE; PLANETARY SYSTEM; SURFACE-DENSITY; CARBON-MONOXIDE; OB ASSOCIATION AB The spatial distribution of gas and solids in protoplanetary disks determines the composition and formation efficiency of planetary systems. A number of disks show starkly different distributions for the gas and small grains compared to millimeter-centimeter-sized dust. We present new Atacama Large Millimeter/Submillimeter Array observations of the dust continuum, CO, (CO)-C-13, and (CO)-O-18 in the IM Lup protoplanetary disk, one of the first systems where this dust-gas dichotomy was clearly seen. The (CO)-C-12 is detected out to a radius of 970 au, while the millimeter continuum emission is truncated at just 313 au. Based upon these data, we have built a comprehensive physical and chemical model for the disk structure, which takes into account the complex, coupled nature of the gas and dust and the interplay between the local and external environment. We constrain the distributions of gas and dust, the gas temperatures, the CO abundances, the CO optical depths, and the incident external radiation field. We find that the reduction/removal of dust from the outer disk exposes this region to higher stellar and external radiation and decreases the rate of freeze-out, allowing CO to remain in the gas out to large radial distances. We estimate a gas-phase CO abundance of 5% of the interstellar medium value and a low external radiation field (G(0) less than or similar to 4). The latter is consistent with that expected from the local stellar population. We additionally find tentative evidence for ring-like continuum substructure, suggestions of isotope-selective photodissociation, and a diffuse gas halo. C1 [Cleeves, L. Ilsedore; Oberg, Karin I.; Wilner, David J.; Huang, Jane; Loomis, Ryan A.; Andrews, Sean M.; Czekala, Ian] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Cleeves, LI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ilse.cleeves@cfa.harvard.edu OI Cleeves, L. Ilsedore/0000-0003-2076-8001; Czekala, Ian/0000-0002-1483-8811; Wilner, David/0000-0003-1526-7587 FU NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51356.001-A]; NASA [NAS 5-26555]; Packard Fellowship for Science and Engineering from the David and Lucile Packard Foundation; National Science Foundation [DGE-1144152]; Smithsonian Institution FX The authors thank Michiel Hogerheijde, James Owen, and Richard Teague for useful discussions, along with the anonymous referee. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.00694 and ADS/JAO. ALMA#2013.1.00226.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We acknowledge the use of public data from the Swift data archive. LIC acknowledges the support of NASA through Hubble Fellowship grant HST-HF2-51356.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. KIO also acknowledges funding through a Packard Fellowship for Science and Engineering from the David and Lucile Packard Foundation. JH and RAL acknowledge support by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144152. IC gratefully acknowledges funding support from the Smithsonian Institution. NR 117 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 110 DI 10.3847/0004-637X/832/2/110 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EE0DJ UT WOS:000389243600001 ER PT J AU Furst, F Tomsick, JA Yamaoka, K Dauser, T Miller, JM Clavel, M Corbel, S Fabian, A Garcia, J Harrison, FA Loh, A Kaaret, P Kalemci, E Migliari, S Miller-Jones, JCA Pottschmidt, K Rahoui, F Rodriguez, J Stern, D Stuhlinger, M Walton, DJ Wilms, J AF Furst, F. Tomsick, J. A. Yamaoka, K. Dauser, T. Miller, J. M. Clavel, M. Corbel, S. Fabian, A. Garcia, J. Harrison, F. A. Loh, A. Kaaret, P. Kalemci, E. Migliari, S. Miller-Jones, J. C. A. Pottschmidt, K. Rahoui, F. Rodriguez, J. Stern, D. Stuhlinger, M. Walton, D. J. Wilms, J. TI GRS 1739-278 OBSERVED AT VERY LOW LUMINOSITY WITH XMM-NEWTON AND NuSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion; accretion disks; stars: black holes; X-rays: binaries; X-rays: individual (GRS 1739-278) ID X-RAY BINARIES; ADVECTION-DOMINATED ACCRETION; LOW-HARD STATE; NEAR-INFRARED OBSERVATIONS; PHOTON IMAGING CAMERA; BLACK-HOLE TRANSIENTS; GX 339-4; LOW/HARD STATE; XTE J1550-564; MULTIWAVELENGTH EVOLUTION AB We present a detailed spectral analysis of XMM-Newton and NuSTAR observations of the accreting transient black hole GRS 1739-278 during a very faint low hard state at similar to 0.02% of the Eddington luminosity (for a distance of 8.5 kpc and a mass of 10 M-circle dot). The broadband X-ray spectrum between 0.5 and 60 keV can be well-described by a power-law continuum with an exponential cutoff. The continuum is unusually hard for such a low luminosity, with a photon index of Gamma = 1.39 +/- 0.04. We find evidence for an additional reflection component from an optically thick accretion disk at the 98% likelihood level. The reflection fraction is low, with R-refl = 0.043(-0.023)(+0.033). In combination with measurements of the spin and inclination parameters made with NuSTAR during a brighter hard state by Miller et al., we seek to constrain the accretion disk geometry. Depending on the assumed emissivity profile of the accretion disk, we find a truncation radius of 15-35 R-g (5-12 R-ISCO) at the 90% confidence limit. These values depend strongly on the assumptions and we discuss possible systematic uncertainties. C1 [Furst, F.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Tomsick, J. A.; Clavel, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Yamaoka, K.] Nagoya Univ, Solar Terr Environm Lab, Chikuka Ku, Furo Cho, Nagoya, Aichi 4648601, Japan. [Yamaoka, K.] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Chikuka ku, Furo Cho, Nagoya, Aichi 4648602, Japan. [Dauser, T.] Dr Karl Remeis Sternwarte & ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Corbel, S.; Loh, A.] Univ Paris Diderot, CEA DSM IRFU SAp, Lab AIM, CEA IRFU CNRS INSU, F-91191 Gif Sur Yvette, France. [Corbel, S.] Univ Orleans, PSL Res Univ, CNRS, Stn Radioastron Nancay,Observ Paris, F-18330 Nancay, France. [Fabian, A.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kalemci, E.] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Migliari, S.; Stuhlinger, M.] ESAC, E-28692 Madrid, Spain. [Migliari, S.] Univ Barcelona, Dept Quantum Phys & Astrophys, E-08028 Barcelona, Spain. [Migliari, S.] Univ Barcelona, Inst Cosmos Sci, E-08028 Barcelona, Spain. [Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. [Pottschmidt, K.] UMBC, CRESST, Dept Phys, Baltimore, MD 21250 USA. [Pottschmidt, K.] UMBC, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pottschmidt, K.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rahoui, F.] European Southern Observ, D-85748 Garching, Germany. [Rahoui, F.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Furst, F (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Clavel, Maica/0000-0003-0724-2742; Garcia, Javier/0000-0003-3828-2448; Miller-Jones, James/0000-0003-3124-2814; Walton, Dominic/0000-0001-5819-3552 FU ESA Member States; NASA [NNX16AH17G, NNG08FD60C]; NASA under Swift Guest Observer grants [NNX15AB81G, NNX15AR52G]; TUBITAK [115F488]; French Research National Agency: CHAOS project [ANR-12-BS05-0009]; UnivEarthS Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; Australian Research Council [FT140101082]; National Aeronautics and Space Administration FX We thank the referee for their helpful comments. We thank the schedulers and SOC of XMM-Newton and NuSTAR for making these observations possible. Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This work is based upon work supported by NASA under award No. NNX16AH17G. J.A.T. acknowledges partial support from NASA under Swift Guest Observer grants NNX15AB81G and NNX15AR52G. E.K.. acknowledges support of TUBITAK Project No 115F488. S.C. and A.L. acknowledge funding support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 and the UnivEarthS Labex program of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). J.C.A. M.-J. is the recipient of an Australian Research Council Future Fellowship (FT140101082). This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). We would like to thank John E. Davis for the slxfig module, which was used to produce all figures in this work. This research has made use of MAXI data provided by RIKEN, JAXA and the MAXI team. The Swift/BAT transient monitor results were provided by the Swift/BAT team. This research has made use of a collection of ISIS functions (ISISscripts) provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). NR 73 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 115 DI 10.3847/0004-637X/832/2/115 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EE0DJ UT WOS:000389243600006 ER PT J AU Ma, JZ Gonzalez, AH Vieira, JD Aravena, M Ashby, MLN Bethermin, M Bothwell, MS Brandt, WN de Breuck, C Carlstrom, JE Chapman, SC Gullberg, B Hezaveh, Y Litke, K Malkan, M Marrone, P McDonald, M Murphy, EJ Spilker, JS Sreevani, J Stark, AA Strandet, M Wang, SX AF Ma, Jingzhe Gonzalez, Anthony H. Vieira, J. D. Aravena, M. Ashby, M. L. N. Bethermin, M. Bothwell, M. S. Brandt, W. N. de Breuck, C. Carlstrom, J. E. Chapman, S. C. Gullberg, B. Hezaveh, Y. Litke, K. Malkan, M. Marrone, P. McDonald, M. Murphy, E. J. Spilker, J. S. Sreevani, J. Stark, A. A. Strandet, M. Wang, S. X. TI SPT0346-52: NEGLIGIBLE AGN ACTIVITY IN A COMPACT, HYPER-STARBURST GALAXY AT z=5.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift ID STAR-FORMING GALAXIES; DEEP FIELD-SOUTH; X-RAY-PROPERTIES; C II EMISSION; LUMINOUS INFRARED GALAXIES; GRAVITATIONAL LENS MODELS; 158 MU-M; SUBMILLIMETER GALAXIES; GALACTIC NUCLEI; MOLECULAR GAS AB We present Chandra ACIS-S and Australia Telescope Compact Array (ATCA) radio continuum observations of the strongly lensed dusty, star-forming galaxy SPT-S J034640-5204.9 (hereafter SPT0346-52) at z = 5.656. This galaxy has also been observed with ALMA, HST, Spitzer, Herschel, Atacama Pathfinder EXperiment, and the Very Large Telescope. Previous observations indicate that if the infrared (IR) emission is driven by star formation, then the inferred lensing-corrected star formation rate (SFR) (similar to 4500 M-circle dot yr(-1)) and SFR surface density Sigma(SFR) (similar to 2000 M-circle dot yr(-1) kpc(-2)) are both exceptionally high. It remained unclear from the previous data, however, whether a central active galactic nucleus (AGN) contributes appreciably to the IR luminosity. The Chandra upper limit shows that SPT0346-52 is consistent with being star formation dominated in the X-ray, and any AGN contribution to the IR emission is negligible. The ATCA radio continuum upper limits are also consistent with the FIR-to-radio correlation for star-forming galaxies with no indication of an additional AGN contribution. The observed prodigious intrinsic IR luminosity of (3.6 +/- 0.3) x 10(13) L-circle dot originates almost solely from vigorous star formation activity. With an intrinsic source size of 0.61 +/- 0.03 kpc, SPT0346-52 is confirmed to have one of the highest Sigma(SFR) of any known galaxy. This high Sigma(SFR), which approaches the Eddington limit for a radiation pressure supported starburst, may be explained by a combination of very high star formation efficiency and gas fraction. C1 [Ma, Jingzhe; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Vieira, J. D.] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, 1002 West Green St, Urbana, IL 61801 USA. [Aravena, M.] Univ Diego Port, Fac Ingn, Nucl Astron, Av Ejercito 441, Santiago, Chile. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bethermin, M.; de Breuck, C.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Bothwell, M. S.] Univ Cambridge, Cavendish Lab, JJ Thompson Ave, Cambridge CB3 0HA, England. [Brandt, W. N.] Penn State Univ, Inst Gravitat, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.; Wang, S. X.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Carlstrom, J. E.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Chapman, S. C.] Univ Chicago, Kavli Inst Cosmol Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA. [Hezaveh, Y.] Dalhousie Univ, Halifax, NS, Canada. [Litke, K.; Marrone, P.; Spilker, J. S.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Malkan, M.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [McDonald, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Murphy, E. J.] MIT, Kavli Inst Astrophys & Space Res, 37-582C, Cambridge, MA 02139 USA. [Strandet, M.] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Strandet, M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. RP Ma, JZ (reprint author), Univ Florida, Dept Astron, Gainesville, FL 32611 USA. EM jingzhema@ufl.edu OI Stark, Antony/0000-0002-2718-9996 FU Australian Government; Chandra grant [GO5-16116A]; U.S. National Science Foundation [AST-1312950]; FONDECYT [1140099]; Hubble Fellowship - Space Telescope Science Institute [51358.001-A] FX We thank the anonymous referee for insightful and constructive comments, which. have significantly improved the paper. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory and the Australia Telescope Compact Array. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa. The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO. The associated HST, Spitzer, and ALMA data are from PID12659, PID10094, and PID2011.0.00958.S, respectively. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00958.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ.; We acknowledge support from the Chandra grant GO5-16116A and the U.S. National Science Foundation under grant No. AST-1312950. M.A. acknowledges partial support from FONDECYT through grant 1140099. Y.H. acknowledges support from Hubble Fellowship grant 51358.001-A awarded by the Space Telescope Science Institute. This research has made use of NASA's Astrophysics Data System. NR 77 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 114 DI 10.3847/0004-637X/832/2/114 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EE0DJ UT WOS:000389243600005 ER PT J AU Zhang, B He, K Wan, T Chen, P Sun, GZ Liu, SY Nguyen, S Lin, LK Jiang, XL AF Zhang, Bin He, Kai Wan, Tao Chen, Peng Sun, Guozheng Liu, Shaoying Truong Son Nguyen Lin, Liangkong Jiang, Xuelong TI Multi-locus phylogeny using topotype specimens sheds light on the systematics of Niviventer (Rodentia, Muridae) in China SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Cryptic species; Species delimitation; Niviventer; Phylogenetics; Taxonomy; Topotype ID SPECIES DELIMITATION; SUBSTITUTION MODELS; COMPLEX; GENUS; DIVERSITY; EVOLUTION; INFERENCE; GENETICS; TALPIDAE; MAMMALIA AB Background: Niviventer is a genus of white-bellied rats that are among the most common rodents in the Indo-Sundaic region. The taxonomy of the genus has undergone extensive revisions and remains controversial. The current phylogeny is unresolved and was developed primarily on the basis of mitochondrial genes. Identification is extremely difficult, and a large number of GenBank sequences seem to be problematic. We extensively sampled specimens of Niviventer in China and neighboring northern Vietnam, including topotypes of the most reported species (n = 6), subspecies (n = 8), and synonyms (n = 4). We estimated phylogenetic relationships on the basis of one mitochondrial and three nuclear genes, using concatenation and coalescent-based approaches. We also employed molecular species delimitation approaches to test the existence of cryptic and putative new species. Results: Our phylogeny was finely resolved, especially for the N. confucianus-like species. Our data provided the first support for N. brahma and N. eha as sister species, an assignment that is congruent with their morphological similarities. Species delimitation analyses provided new insight into species diversity and systematics. Three geographic populations of N. confucianus and one of N. fulvescens were supported as genetically distinct in our species delimitation analyses, while three recognized species (N. coninga, N. huang, and N. lotipes) were not strongly supported as distinct. Conclusions: Our results suggested that several genetically distinct species may be contained within the species currently known as N. confucianus and N. fulvescens. In addition, the results of Bayesian Phylogenetics and Phylogeography (BPP) for N. coninga, N. huang, and N. lotipes indicated that either inter-specific gene flow had occurred or imperfect taxonomy was present. Morphological examinations and morphometric analyses are warranted to examine the molecular results. C1 [Zhang, Bin; He, Kai; Wan, Tao; Jiang, Xuelong] Chinese Acad Sci, Kunming Inst Zool, State Key Lab Genet Resources & Evolut, Kunming, Yunnan, Peoples R China. [Zhang, Bin] Univ Chinese Acad Sci, Kunming Coll Life Sci, Kunming, Yunnan, Peoples R China. [He, Kai] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Chen, Peng] Chengdu Res Base Giant Panda Breeding, Sichuan Key Lab Conservat Biol Endangered Wildlif, Chengdu, Sichuan, Peoples R China. [Sun, Guozheng] China Forest Explorat & Design Inst Kunming, Kunming, Yunnan, Peoples R China. [Liu, Shaoying] Sichuan Acad Forestry, Chengdu, Sichuan, Peoples R China. [Truong Son Nguyen] Vietnam Acad Sci & Technol, Inst Ecol & Biol Resources, Dept Vertebrate Zool, Hanoi, Vietnam. [Lin, Liangkong] Tunghai Univ, Dept Life Sci, Lab Wildlife Ecol, Taichung, Taiwan. [He, Kai] Kyoto Univ, Kyoto Univ Museum, Kyoto 6068501, Japan. RP He, K; Jiang, XL (reprint author), Chinese Acad Sci, Kunming Inst Zool, State Key Lab Genet Resources & Evolut, Kunming, Yunnan, Peoples R China.; He, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.; He, K (reprint author), Kyoto Univ, Kyoto Univ Museum, Kyoto 6068501, Japan. EM hekai@mail.kiz.ac.cn; jiangxl@mail.kiz.ac.cn FU National Natural Science Foundation of China [31272276]; Fund of State Key Laboratory of Genetic Resources and Evolution, Kunming Institute of Zoology, Chinese Academy of Sciences [GREKF13-07] FX This research was funded by the National Natural Science Foundation of China (No. 31272276) and the Fund of State Key Laboratory of Genetic Resources and Evolution, Kunming Institute of Zoology, Chinese Academy of Sciences (GREKF13-07). NR 55 TC 0 Z9 0 U1 9 U2 9 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD DEC 1 PY 2016 VL 16 AR 261 DI 10.1186/s12862-016-0832-8 PG 12 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA EE2MM UT WOS:000389418500004 PM 27905886 ER PT J AU Baeza, JA Gueron, R Simpson, L Ambrosio, LJ AF Baeza, J. Antonio Gueron, Rodrigo Simpson, Lunden Ambrosio, Louis J. TI Population distribution, host-switching, and chemical sensing in the symbiotic shrimp Lysmata pederseni: implications for its mating system in a changing reef seascape SO CORAL REEFS LA English DT Article DE Shifting baselines; Reef escape; Mating system; Monogamy; Shrimp ID SIMULTANEOUS HERMAPHRODITIC SHRIMP; PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; SEX ALLOCATION; MARINE SHRIMP; WURDEMANNI CARIDEA; LIFE-HISTORY; CORAL-REEFS; CRABS; DECAPODA; HIPPOLYTIDAE AB Lysmata pederseni, a protandric simultaneously hermaphroditic shrimp that inhabits the tube sponge Callyspongia vaginalis, is monogamous in the central and southeastern Caribbean Sea. We tested the null hypothesis of monogamy in a northern Caribbean population. In the Florida Keys, shrimps did not inhabit host individuals in pairs with a frequency greater than expected by chance alone. Hermaphrodites inhabited sponges solitarily and often brooded embryos. Hermaphrodites do not store sperm and need to be inseminated shortly after molting to fertilize a new batch of eggs. Thus, males and/or other hermaphrodites are likely switching among host individuals in search of sexual partners. Field experiments demonstrated low shrimp host fidelity. Host residence time was similar to 2 times shorter for males than for hermaphrodites. We inferred a polygynandrous mating system in L. pederseni from the Florida Keys, with male-role and young hermaphrodites often moving among sponges in search of older, more sedentary, female-role hermaphrodites. We expected shrimps to use water-borne chemical cues originating from conspecifics or sponges to locate sexual partners. Experiments demonstrated that shrimps were attracted to water-borne cues originating from sponges but not conspecifics. We have described the mating system of a reef-associated shrimp in a fast-pace shifting seascape increasingly dominated by sponges and vanishing stony corals. In the central and southeastern Caribbean Sea, with greater coral cover and lower sponge abundance than in the Florida Keys, the same species is monogamous. Whether or not similar shifts in the social organization of other coral reef-dwelling marine organisms are occurring due to contemporary changes in seascapes is a relevant topic that deserves further attention. C1 [Baeza, J. Antonio; Simpson, Lunden; Ambrosio, Louis J.] Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA. [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. [Baeza, J. Antonio] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. [Gueron, Rodrigo] Inst Fed Educ Ciencia & Tecnol Espirito Santo, Campus Alegre, Espirito Santo, Brazil. RP Baeza, JA (reprint author), Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA.; Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.; Baeza, JA (reprint author), Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. EM jbaezam@clemson.edu NR 49 TC 0 Z9 0 U1 5 U2 5 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2016 VL 35 IS 4 BP 1213 EP 1224 DI 10.1007/s00338-016-1467-3 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA ED1FZ UT WOS:000388591500009 ER PT J AU Glynn, PW Grassian, B Kleemann, KH Mate, JL AF Glynn, Peter W. Grassian, Benjamin Kleemann, Karl H. Mate, Juan L. TI The true identity of Siderastrea glynni Budd & Guzman, 1994, a highly endangered eastern Pacific scleractinian coral SO CORAL REEFS LA English DT Article DE Siderastreidae; Synonymy; Panama; Accidental introduction; Morphometrics ID PANAMA; ANTHOZOA; PATTERNS; CNIDARIA; REGION; REEFS AB Siderastrea glynni Budd & Guzman, 1994 was erroneously erected from live colonies of S. siderea (Ellis & Solander, 1768) unintentionally transferred from the Caribbean to the Pacific side of the Isthmus of Panama. These corals had been used in experiments conducted in the early 1980s by KH Kleemann at Uraba Island, Taboga Islands, Gulf of Panama, at the same site of the subsequent S. glynni discovery. Here, we offer evidence that live fragments deposited at Uraba Island in 1982 are the same found by Guzman in 1992, and were inadvertently introduced from colonies of Caribbean S. siderea that were presumed to be dead. This morphological study builds on and supports recent genetic analyses of the S. glynni holobiont. In light of these findings, S. glynni should be regarded as a subjective junior synonym of S. siderea. C1 [Glynn, Peter W.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. [Grassian, Benjamin] Univ Rhode Isl, Grad Sch Oceanog, 215 S Ferry Rd, Narragansett, RI 02882 USA. [Kleemann, Karl H.] Univ Vienna, Dept Paleontol, Geozentrum, UZA 2,Althanstr 14, A-1090 Vienna, Austria. [Mate, Juan L.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. RP Glynn, PW (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM pglynn@rsmas.miami.edu FU Smithsonian Tropical Research Institute; NSF [OCE-9314798] FX Thanks are due to Ann F. Budd, Stephen D. Cairns, and Nancy Voss for helping with various aspects of this study. Insights on coral calcification by Derek P. Manzello were helpful, and we also thank Milton Solano and Michael P. Fuller who kindly assisted with the production of figures. Field support was provided by the Smithsonian Tropical Research Institute and NSF grant OCE-9314798. NR 26 TC 0 Z9 0 U1 1 U2 1 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD DEC PY 2016 VL 35 IS 4 BP 1399 EP 1404 DI 10.1007/s00338-016-1470-8 PG 6 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA ED1FZ UT WOS:000388591500027 ER PT J AU Wojtusik, J Pennington, P Songsasen, N Padilla, LR Citino, SB Pukazhenthi, BS AF Wojtusik, Jessye Pennington, Parker Songsasen, Nucharin Padilla, Luis R. Citino, Scott B. Pukazhenthi, Budhan S. TI Pretreatment of Addra gazelle (Nanger dama ruficollis) spermatozoa with cholesterol-loaded cyclodextrins improves cryosurvival SO CRYOBIOLOGY LA English DT Article DE Cryopreservation; Cholesterol; Antelope; Acrosome reaction; Endangered species ID OSMOTIC TOLERANCE LIMITS; METHYL-BETA-CYCLODEXTRIN; GENETIC RESOURCE BANKS; BOAR SPERMATOZOA; PLASMA-MEMBRANE; COLD-SHOCK; BULL SPERM; ARTIFICIAL-INSEMINATION; SEMEN CRYOPRESERVATION; FLUCTUATING ASYMMETRY AB Preserving genetic diversity of the critically endangered Addra gazelle (Nanger dama ruficollis) could be enhanced through the use of frozen-thawed sperm and artificial insemination. Our aim was to characterize Addra ejaculate traits and to assess the effects of cholesterol-loaded cyclodextrin (CLC) on sperm cryosurvival. Fresh ejaculates were treated with CLC (0, 0.5, 1.5, 3.0, and 6.0 mg/ml) prior to cryopreservation. All males produced spermic ejaculates with >75% sperm motility. The mean +/- SEM seminal volume, sperm concentration, percent motility, forward progression, and percent morphologically normal spermatozoa were 3.2 +/- 0.3 ml, 1.2 03 x 10(9), 75.82 +/- 2.7%, 3.2 +/- 0.3 (0-5 scale; 5 = most progressive), and 57.12 +/- 3.8%, respectively. More than 92% contained an intact acrosome. There was no effect of time or in vitro incubation on progression or acrosomal integrity on thawed samples (P > 0.05). Spermatozoa pre-treated with 0.5 mg/ml CLC retained higher (P < 0.05) motility post-thaw than aliquots treated with 0, 3.0, or 6.0 mg/ml of CLC. Spermatozoa pre-treated with 0.5, 1.5, or 3.0 mg/ml CLC exhibited greater viability than counterparts (P < 0.05). Sperm kinetics including beat cross frequency (BCE), average path velocity (VAP), curvilinear velocity (VCL), and straight line velocity (VSL) did not differ among samples (P > 0.05). Linearity (LIN) and straightness (STR) were different among samples after thawing. Results demonstrate treatment with CLC (0.5 mg/ml) protects Addra spermatozoa from cryo-damage. Reported advances will facilitate establishment of a frozen repository and support the genetic management of this critically endangered north African desert antelope. Published by Elsevier Inc. C1 [Wojtusik, Jessye; Pennington, Parker; Songsasen, Nucharin; Padilla, Luis R.; Pukazhenthi, Budhan S.] Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. [Wojtusik, Jessye; Pennington, Parker] George Mason Univ, Dept Environm Sci & Policy, 4400 Univ Dr, Fairfax, VA 22030 USA. [Citino, Scott B.] White Oak Conservat, 581705 Gilman Dr, Yulee, FL 32097 USA. [Wojtusik, Jessye] Cincinnati Zoo & Bot Garden, Ctr Conservat & Res Endangered Wildlife CREW, 3400 Vine St, Cincinnati, OH 45220 USA. [Pennington, Parker] San Diego Zoo Global, Inst Conservat Res, 15600 San Pasqual Valley Rd, Escondido, CA 92027 USA. [Padilla, Luis R.] St Louis Zoo, 1 Govt Dr, St Louis, MO 63110 USA. RP Pukazhenthi, BS (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. EM pukazhenthib@si.edu FU George Mason University; Sichel Endowment Fund FX We would like to thank the George Mason University for providing financial support to Jessye Wojtusik and the Sichel Endowment Fund for research support. NR 69 TC 0 Z9 0 U1 4 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 EI 1090-2392 J9 CRYOBIOLOGY JI Cryobiology PD DEC PY 2016 VL 73 IS 3 BP 388 EP 395 DI 10.1016/j.cryobiol.2016.08.012 PG 8 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA ED7BL UT WOS:000389010600013 PM 27621115 ER PT J AU Tepley, AJ Veblen, TT Perry, GLW Stewart, GH Naficy, CE AF Tepley, Alan J. Veblen, Thomas T. Perry, George L. W. Stewart, Glenn H. Naficy, Cameron E. TI Positive Feedbacks to Fire-Driven Deforestation Following Human Colonization of the South Island of New Zealand SO ECOSYSTEMS LA English DT Article DE Alternative stable states; fire; hysteresis; Kunzea; Leptospermum; Nothofagus; microclimate; reburn; tipping point ID SAVANNA-FOREST TRANSITION; BEECH NOTHOFAGUS FORESTS; NORTHERN NEW-ZEALAND; LANDSCAPE TRANSFORMATION; REGIME SHIFTS; VEGETATION; PATAGONIA; REGENERATION; DISPERSAL; ECOLOGY AB Altered fire regimes in the face of climatic and land-use change could potentially transform large areas from forest to shorter-statured or open-canopy vegetation. There is growing concern that once initiated, these nonforested landscapes could be perpetuated almost indefinitely through a suite of positive feedbacks with fire. The rapid deforestation of much of New Zealand following human settlement (ca. 750 years ago) provides a rare opportunity to evaluate the feedback mechanisms that facilitated such extensive transformation and thereby help us to identify factors that confer vulnerability or resilience to similar changes in other regions. Here we evaluate the structure of living and dead vegetation (fuel loading) and microclimate (fuel moisture) in beech (Nothofagaceae) forests and adjacent stands that burned within the last 60-140 years and are dominated by mAnuka (Leptospermum scoparium) or kAnuka (Kunzea spp.). We show that the burning of beech forests initiates a positive feedback cycle whereby the loss of microclimatic amelioration under the dense forest canopy and the abundant fine fuels that dry readily beneath the sparse mAnuka/kAnuka canopy enables perpetuation of these stands by facilitating repeated burning. Beech regeneration was limited to a narrow zone along the margin of unburned stands. The high flammability of vegetation that develops after fire and the long time to forest recovery were the primary factors that facilitated extensive deforestation with the introduction of human-ignited fire. Evaluating these two characteristics may be key to determining which regions may be near a tipping point where relatively small land-use- or climatically driven changes to fire regimes could bring about extensive deforestation. C1 [Tepley, Alan J.; Veblen, Thomas T.; Naficy, Cameron E.] Univ Colorado, Dept Geog, Boulder, CO 80309 USA. [Perry, George L. W.] Univ Auckland, Sch Environm, Private Bag 92019, Auckland, New Zealand. [Stewart, Glenn H.] Fac Environm Soc & Design, Dept Environm Management, POB 85085, Christchurch 7647, New Zealand. [Tepley, Alan J.] Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. RP Tepley, AJ (reprint author), Univ Colorado, Dept Geog, Boulder, CO 80309 USA.; Tepley, AJ (reprint author), Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM TepleyA@si.edu OI Tepley, Alan/0000-0002-5701-9613 FU National Science Foundation Partnerships for International Research and Education (PIRE) grant [OISE-0966472] FX We would like to thank Javier Fernandez for assistance in the field and Janet Wilmshurst, Matt McGlone, Jenny Hurst, and Landcare Research for aiding in selecting sample sites and logistical support. We are grateful to Robert Holdaway for providing crown allometry models. Kristina Anderson-Teixeira and two anonymous reviewers provided valuable feedback on earlier versions of this manuscript. This work was supported by a National Science Foundation Partnerships for International Research and Education (PIRE) grant (OISE-0966472). NR 73 TC 0 Z9 0 U1 21 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 EI 1435-0629 J9 ECOSYSTEMS JI Ecosystems PD DEC PY 2016 VL 19 IS 8 BP 1325 EP 1344 DI 10.1007/s10021-016-0008-9 PG 20 WC Ecology SC Environmental Sciences & Ecology GA ED5YC UT WOS:000388928800001 ER PT J AU Helbig, M Wischnewski, K Kljun, N Chasmer, LE Quinton, WL Detto, M Sonnentag, O AF Helbig, Manuel Wischnewski, Karoline Kljun, Natascha Chasmer, Laura E. Quinton, William L. Detto, Matteo Sonnentag, Oliver TI Regional atmospheric cooling and wetting effect of permafrost thaw-induced boreal forest loss SO GLOBAL CHANGE BIOLOGY LA English DT Article DE boreal forest; climate change; eddy covariance; energy flux; evapotranspiration; land cover change; permafrost; wetland ID ENERGY-BALANCE CLOSURE; EDDY-COVARIANCE METHOD; BLACK SPRUCE FOREST; SURFACE HEAT-FLUX; BOUNDARY-LAYER; CLIMATE-CHANGE; WATER-VAPOR; DISCONTINUOUS PERMAFROST; NORTHWEST-TERRITORIES; STOMATAL CONDUCTANCE AB In the sporadic permafrost zone of North America, thaw-induced boreal forest loss is leading to permafrost-free wetland expansion. These land cover changes alter landscape-scale surface properties with potentially large, however, still unknown impacts on regional climates. In this study, we combine nested eddy covariance flux tower measurements with satellite remote sensing to characterize the impacts of boreal forest loss on albedo, eco-physiological and aerodynamic surface properties, and turbulent energy fluxes of a lowland boreal forest region in the Northwest Territories, Canada. Planetary boundary layer modelling is used to estimate the potential forest loss impact on regional air temperature and atmospheric moisture. We show that thaw-induced conversion of forests to wetlands increases albedo: and bulk surface conductance for water vapour and decreases aerodynamic surface temperature. At the same time, heat transfer efficiency is reduced. These shifts in land surface properties increase latent at the expense of sensible heat fluxes, thus, drastically reducing Bowen ratios. Due to the lower albedo of forests and their masking effect of highly reflective snow, available energy is lower in wetlands, especially in late winter. Modelling results demonstrate that a conversion of a present-day boreal forest-wetland to a hypothetical homogeneous wetland landscape could induce a near-surface cooling effect on regional air temperatures of up to 3-4 degrees C in late winter and 1-2 degrees C in summer. An atmospheric wetting effect in summer is indicated by a maximum increase in water vapour mixing ratios of 2mmolmol(-1). At the same time, maximum boundary layer heights are reduced by about a third of the original height. In fall, simulated air temperature and atmospheric moisture between the two scenarios do not differ. Therefore, permafrost thaw-induced boreal forest loss may modify regional precipitation patterns and slow down regional warming trends. C1 [Helbig, Manuel; Wischnewski, Karoline; Sonnentag, Oliver] Univ Montreal, Dept Geog, 520 Chemin Cote St Catherine, Montreal, PQ H2V 2B8, Canada. [Helbig, Manuel; Wischnewski, Karoline; Sonnentag, Oliver] Univ Montreal, Ctr Etud Nord, 520 Chemin Cote St Catherine, Montreal, PQ H2V 2B8, Canada. [Kljun, Natascha] Swansea Univ, Dept Geog, Singleton Pk, Swansea SA2 8PP, W Glam, Wales. [Chasmer, Laura E.] Univ Lethbridge, Dept Geog, 4401 Univ Dr, Lethbridge, AB T1K 3M4, Canada. [Quinton, William L.] Wilfrid Laurier Univ, Cold Reg Res Ctr, 75 Univ Ave W, Waterloo, ON N2L 3C5, Canada. [Detto, Matteo] Smithsonian Trop Res Inst, Luis Clement Ave,Bldg 401 Tupper, Balboa Ancon, Panama. RP Helbig, M (reprint author), Univ Montreal, Dept Geog, 520 Chemin Cote St Catherine, Montreal, PQ H2V 2B8, Canada.; Helbig, M (reprint author), Univ Montreal, Ctr Etud Nord, 520 Chemin Cote St Catherine, Montreal, PQ H2V 2B8, Canada. EM manuel.helbig@umontreal.ca RI Kljun, Natascha/B-8467-2008 OI Kljun, Natascha/0000-0001-9650-2184 FU Fonds de recherche du Quebec - Nature et technologies (FRQNT); German Academic Exchange Service (DAAD); Canada Research Chairs; Canada Foundation for Innovation Leaders Opportunity Fund; Natural Sciences and Engineering Research Council Discovery Grant; Forest Global Earth Observatory (Forest-GEO); Liidlii Kue First Nation; Jean-Marie River First Nation FX The authors are grateful to C. Pappas for discussions improving the manuscript. We thank Dr. C. Hopkinson for providing LiDAR data and E. Houghton for supplying snow density measurements. M. Helbig was funded through graduate student scholarships provided by the Fonds de recherche du Quebec - Nature et technologies (FRQNT) and the German Academic Exchange Service (DAAD). Funding for this research was awarded to O. Sonnentag by the Canada Research Chairs, Canada Foundation for Innovation Leaders Opportunity Fund and Natural Sciences and Engineering Research Council Discovery Grant programs. M. Detto was supported by The Forest Global Earth Observatory (Forest-GEO). We are grateful for the support of the Liidlii Kue First Nation and Jean-Marie River First Nation for their support of the Scotty Creek Research Station. NR 118 TC 0 Z9 0 U1 23 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD DEC PY 2016 VL 22 IS 12 BP 4048 EP 4066 DI 10.1111/gcb.13348 PG 19 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EC0TJ UT WOS:000387813300019 PM 27153776 ER PT J AU McCulloh, KA Petitmermet, J Stefanski, A Rice, KE Rich, RL Montgomery, RA Reich, PB AF McCulloh, Katherine A. Petitmermet, Joshua Stefanski, Artur Rice, Karen E. Rich, Roy L. Montgomery, Rebecca A. Reich, Peter B. TI Is it getting hot in here? Adjustment of hydraulic parameters in six boreal and temperate tree species after 5years of warming SO GLOBAL CHANGE BIOLOGY LA English DT Article DE Boreal Forest Warming at an Ecotone in Danger; boreal-temperate ecotone; conduit diameter; elevated temperature; hydraulic conductivity; saplings ID PINUS-TAEDA SEEDLINGS; WATER TRANSPORT; PONDEROSA PINE; WOOD DENSITY; SCOTS PINE; CONTRASTING CLIMATES; GROWTH TEMPERATURE; GAS-EXCHANGE; ELEVATED CO2; XYLEM AB Global temperatures (T) are rising, and for many plant species, their physiological response to this change has not been well characterized. In particular, how hydraulic parameters may change has only been examined experimentally for a few species. To address this, we measured characteristics of the hydraulic architecture of six species growing in ambient T and ambient +3.4 degrees C T plots in two experimentally warmed forest sites in Minnesota. These sites are at the temperate-boreal ecotone, and we measured three species from each forest type. We hypothesized that relative to boreal species, temperate species near their northern range border would increase xylem conduit diameters when grown under elevated T. We also predicted a continuum of responses among wood types, with conduit diameter increases correlating with increases in the complexity of wood structure. Finally, we predicted that increases in conduit diameter and specific hydraulic conductivity would positively affect photosynthetic rates and growth. Our results generally supported our hypotheses, and conduit diameter increased under elevated T across all species, although this pattern was driven predominantly by three species. Two of these species were temperate angiosperms, but one was a boreal conifer, contrary to predictions. We observed positive relationships between the change in specific hydraulic conductivity and both photosynthetic rate (P=0.080) and growth (P=0.012). Our results indicate that species differ in their ability to adjust hydraulically to increases in T. Specifically, species with more complex xylem anatomy, particularly those individuals growing near the cooler edge of their range, appeared to be better able to increase conduit diameters and specific hydraulic conductivity, which permitted increases in photosynthesis and growth. Our data support results that indicate individual's ability to physiologically adjust is related to their location within their species range, and highlight that some wood types may adjust more easily than others. C1 [McCulloh, Katherine A.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Petitmermet, Joshua] Oregon State Univ, Dept Forest Engn Resources & Management, Corvallis, OR 97331 USA. [Stefanski, Artur; Rice, Karen E.; Rich, Roy L.; Montgomery, Rebecca A.; Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Rich, Roy L.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Reich, Peter B.] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2753, Australia. RP McCulloh, KA (reprint author), Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. EM kmcculloh@wisc.edu FU U.S. Department of Energy Program on Ecological Research 385 Grant [DE-FG02-07ER64456]; Wilderness Research Foundation; University of Wisconsin-Madison Graduate School and College of Letters and Science FX The authors are grateful to William Arrett, Colin Sayre, Beth Rutila, and Chelsey Baranczyk for assistance with collection in the field and sample measurement, and to Cindy Buschena for organizational assistance. The authors are also appreciative of Cecile Ane and Bret Larget for statistical advice. The comments of two anonymous reviewers greatly improved the manuscript. Funding provided by: U.S. Department of Energy Program on Ecological Research 385 Grant No. DE-FG02-07ER64456, Wilderness Research Foundation, and the University of Wisconsin-Madison Graduate School and College of Letters and Science. NR 53 TC 0 Z9 0 U1 32 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD DEC PY 2016 VL 22 IS 12 BP 4124 EP 4133 DI 10.1111/gcb.13323 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EC0TJ UT WOS:000387813300024 PM 27122300 ER PT J AU Heimann, A Yonts, JA Wise, MA AF Heimann, Adriana Yonts, Jason A. Wise, Michael A. TI Melt evolution in felsic dikes inferred from the composition of gahnite in two new occurrences, Pala Chief and Elizabeth R composite dikes, California SO MINERALOGY AND PETROLOGY LA English DT Article DE Gahnite; Aplite; California; Elizabeth R; Pala Chief; Zoning; Evolution; Pala District ID SAN-DIEGO COUNTY; BORBOREMA PEGMATITE PROVINCE; ELEMENT GRANITIC PEGMATITES; PENINSULAR RANGES BATHOLITH; CHEMICAL-COMPOSITION; NORTHEASTERN BRAZIL; INTERNAL EVOLUTION; BAJA-CALIFORNIA; ZINCIAN SPINEL; GROUP MINERALS AB We report the occurrence and composition of gahnite ([Zn,Fe,Mg,Mn]Al2O4) in aplites of the Pala Chief and Elizabeth R layered pegmatite-aplite dikes, Pala District, California, and the significance for felsic melt evolution. The aplite is characterized by alternating bands of white, fine-grained plagioclase + quartz + muscovite +/- black tourmaline and thin laminations defined by concentrations of reddish-brown garnet ("line rock"). Accessory gahnite occurs as extremely fine-grained (50-250 mu m) green to bluish-green crystals. Gahnite compositions in both occurrences are similar and defined by end-member ranges Ghn(83.5-90.9)Hc(8.7-15)Spl(0-1.4). Zinc contents in gahnite are high (36.7-39.5 wt.% ZnO for Pala Chief, 37.2-40.2 wt.% ZnO for Elizabeth R), the MgO and MnO contents are negligible (< 0.7 wt.%), and Fe is the main substitution present (< 6.9 wt.% FeO). Gahnite is chemically zoned and characterized by higher Zn (< 2 wt.% ZnO) and lower Fe, Mg, and Mn contents in rims compared to cores, which shows the substitution mechanism, and reflects fast growth during melt evolution via fractional crystallization followed by fast cooling. Compositional variations are greater within individual crystals than among crystals and between laminations, which indicate a homogeneous melt at the aplite scale. Compared with the composition of gahnite from pegmatites worldwide, the studied gahnite reflects a moderate degree of melt evolution. This study confirms the incompatible character of Zn in evolving pegmatite-aplite melts and shows the usefulness of gahnite as a petrogenetic indicator. Because gahnite is a resistant mineral, surficial findings of gahnite with very low Mg contents and Zn contents similar or higher than those measured here may indicate a source of granitic pegmatite-aplite. C1 [Heimann, Adriana; Yonts, Jason A.] East Carolina Univ, Dept Geol Sci, 101 Graham Bldg, Greenville, NC 27858 USA. [Wise, Michael A.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Heimann, A (reprint author), East Carolina Univ, Dept Geol Sci, 101 Graham Bldg, Greenville, NC 27858 USA. EM heimanna@ecu.edu FU Harriot College of Arts and Sciences; Division of Research and Graduate Studies at East Carolina University; U.S. Geological Survey Mineral Resources External Research Program [G10AP00051]; Society of Economic Geologists McKinstry Research Grant; Sigma Xi, The Scientific Research Society FX Funding for this project was provided by the Harriot College of Arts and Sciences and the Division of Research and Graduate Studies at East Carolina University and by a U.S. Geological Survey Mineral Resources External Research Program grant (# G10AP00051; to AH), for which we are grateful. Additional funding was graciously provided by a Society of Economic Geologists McKinstry Research Grant and a Sigma Xi, The Scientific Research Society, grant-in-aid of research (to JY). This work would not have been possible without the generosity of David London, who provided the samples for study as well as helpful discussions and comments from an early version of the manuscript. We thank Nick Foster for help with EMP analysis at FSU and Tom Fink for help with SEM analysis at ECU. Josh Bitner is thanked for cutting the samples. Associate Editor Leonid Danyushevsky handled the manuscript and provided suggestions while David Lentz and Aleksandr Stepanov provided constructive reviews, all of which helped improve the original manuscript and are greatly appreciated. NR 73 TC 0 Z9 0 U1 2 U2 2 PU SPRINGER WIEN PI WIEN PA SACHSENPLATZ 4-6, PO BOX 89, A-1201 WIEN, AUSTRIA SN 0930-0708 EI 1438-1168 J9 MINER PETROL JI Mineral. Petrol. PD DEC PY 2016 VL 110 IS 6 BP 731 EP 746 DI 10.1007/s00710-016-0446-2 PG 16 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA ED4QE UT WOS:000388834300003 ER PT J AU Jasso-Martinez, JM Castaneda-Sortibran, AN Pozo, C Garcia-Sandoval, R Prado, BR Luis-Martinez, A Llorente-Bousquets, J Rodriguez-Arnaiz, R AF Jasso-Martinez, J. M. Castaneda-Sortibran, A. N. Pozo, C. Garcia-Sandoval, R. Prado, B. R. Luis-Martinez, A. Llorente-Bousquets, J. Rodriguez-Arnaiz, R. TI The Enantia jethys Complex(1): Insights from COI Confirm the Species Complex and Reveal a New Potential Cryptic Species SO SOUTHWESTERN ENTOMOLOGIST LA English DT Article ID DNA BARCODES; SEQUENCE ALIGNMENT; DIVERGENCE TIMES; MOLECULAR-DATA; LEPIDOPTERA; SUBSTITUTIONS AB DNA barcoding regions have been used for identifying organisms and delimiting species. Our research focused on butterflies belonging to the Enantia jethys species complex (Lepidoptera: Pieridae) in Mexico, specifically to resolve the taxonomic problem of the number of species in the group. We used the standard segment of approximately 650 base pairs of the mitochondrial cytochrome oxidase subunit I (COI) gene. Our study is the first to use DNA sequences to examine phylogenetic relationships of this complex species. Three phylogenetic inference methods used were parsimony, maximum likelihood, and Bayesian inference. Two-species delimitation methods also were used: generalized mixed Yule-coalescent and Poisson tree process (bPTP). We used all the analyses to obtain 155 COI sequences and a persistent clade with four monophyletic groups: three corresponding to Enantia albania (Bates), Enantia jethys (Boisduval), and Enantia mazai Llorente, and a fourth corresponding to a new potential cryptic species, which must be described. C1 [Jasso-Martinez, J. M.; Castaneda-Sortibran, A. N.; Garcia-Sandoval, R.; Luis-Martinez, A.; Llorente-Bousquets, J.; Rodriguez-Arnaiz, R.] Univ Nacl Autonoma Mexico, Fac Ciencias, Ave Univ 3000, Ciudad De Mexico 04510, DF, Mexico. [Pozo, C.; Prado, B. R.] El Colegio Frontera Sur, Unidad Chetumal, Ave Centenario,Km 5-5 S-N, Chetmal 77014, Quintana Roo, Mexico. [Llorente-Bousquets, J.] Smithsonian Inst, POB 37012, Washington, DC 20013 USA. RP Rodriguez-Arnaiz, R (reprint author), Univ Nacl Autonoma Mexico, Fac Ciencias, Ave Univ 3000, Ciudad De Mexico 04510, DF, Mexico. FU [DGAPA - PAPIIT202415] FX Daniel Pinero and Alejandro Zaldivar provided valuable suggestions and commentaries on an early version of the manuscript. Arturo Arellano provided assistance in the field. Thanks to Holger Weissenberger for helping produce Fig. 2 and to Arely Martinez for processing samples in the laboratory. Part of the project was funded from DGAPA - PAPIIT202415. This work represents a contribution of the "Red Tematica Codigo de Barras de la Vida. MEXBOL-CONACyT". NR 50 TC 0 Z9 0 U1 1 U2 1 PU SOUTHWESTERN ENTOMOLOGICAL SOC PI DALLAS PA 17360 COIT RD, DALLAS, TX 75252-6599 USA SN 0147-1724 EI 2162-2647 J9 SOUTHWEST ENTOMOL JI Southw. Entomol. PD DEC PY 2016 VL 41 IS 4 BP 1005 EP 1019 PG 15 WC Entomology SC Entomology GA ED3FB UT WOS:000388733700011 ER PT J AU Nieves-Uribe, S Castro-Gerardino, J Flores-Gallardo, A Llorente-Bousquets, J AF Nieves-Uribe, Sandra Castro-Gerardino, Jimena Flores-Gallardo, Adrian Llorente-Bousquets, Jorge TI Chorionic Study of Three Species of Colias Fabricius, 1807 and Zerene cesonia cesonia (Stoll, 1790) SO SOUTHWESTERN ENTOMOLOGIST LA Spanish DT Article ID LEPIDOPTERA PIERIDAE; BUTTERFLIES LEPIDOPTERA; STRUCTURAL ULTRAVIOLET; EXTERNAL MORPHOLOGY; MITOCHONDRIAL-DNA; EVOLUTION; GENERA; SYSTEMATICS; COLIADINAE; PHYLOGENY AB We studied and illustrated the chorionic structure of four species of the subfamily Coliadinae: Colias (C. dimera, C. erate, y C. eurytheme) and Zerene (Z. c. cesonia). Previous descriptions of C. dimera, C. eurytheme, and Z. c. cesonia were reviewed and compared with new materials from Mexico and Colombia. Also, the chorion of C. erate was described for first time and the micro-grid of three in four species, previously thought absent in both genera because of its lack in C. dimera. Using a scanning electron microscope (SEM), photographs were taken of four chorionic regions (micropylar, perimicropylar or apical, equator, and base), which are described, illustrated, and compared on a tab. SEM images allowed analysis and resolved that C. dimera presents characters from less derived genera within Coliadinae, while C. eurytheme expresses characters found in derived genera. However, reticular characters on basal area, number of axes and their double thickness compared to the ribs placed C. dimera as a derived species within the group. Both conditions expose C. dimera as a species with a mosaic of ancestral and derived chorionic characters. C1 [Nieves-Uribe, Sandra; Castro-Gerardino, Jimena; Flores-Gallardo, Adrian; Llorente-Bousquets, Jorge] Smithsonian Inst, POB 37012, Washington, DC 20013 USA. RP Llorente-Bousquets, J (reprint author), Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM s.nieves.uribe@outlook.com; dijica@prodigy.net.mx; emileusher@hotmail.com; enantia@prodigy.net.mx NR 63 TC 0 Z9 0 U1 1 U2 1 PU SOUTHWESTERN ENTOMOLOGICAL SOC PI DALLAS PA 17360 COIT RD, DALLAS, TX 75252-6599 USA SN 0147-1724 EI 2162-2647 J9 SOUTHWEST ENTOMOL JI Southw. Entomol. PD DEC PY 2016 VL 41 IS 4 BP 1121 EP 1141 PG 21 WC Entomology SC Entomology GA ED3FB UT WOS:000388733700020 ER PT J AU Llorente-Bousquets, J Castro-Gerardino, DJ Le Crom, JF AF Llorente-Bousquets, Jorge Jimena Castro-Gerardino, Diana Francois Le Crom, Jean TI Study of the Genus Moschoneura Butler, 1870 and a New Subspecies of Moschoneura ela (Lepidoptera: Pieridae, Dismorphiinae) SO SOUTHWESTERN ENTOMOLOGIST LA Spanish DT Article AB A historical review of the genus Moschoneura Butler is described, highlighting some taxonomic problems prevailing for this genus. The diagnosis was based on morphological aspects of habitus, antennal club, male genitalia, and distributional aspects (ecological and geographical). When examining M. pinthous, M. ithomia, and M. ela species, the habitat preference of the latter is distinguished. The sulci and male genitalia of two species of the genus (M. pinthous monica and M. ela winhardi ssp. nov.) are illustrated. The distribution of the type localities of the taxa Moschoneura in the Andean region is plotted. While describing M. ela winhardi ssp. nov., a comparison was made with M. e. xanthella, and data of their habitat and habits are synthesized. C1 [Llorente-Bousquets, Jorge; Jimena Castro-Gerardino, Diana] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Evolut Biol, Museo Zool Entomol, Mexico City, DF, Mexico. [Francois Le Crom, Jean] Calle 45 9-42 Of 202 Ed Carlec, Bogota, Colombia. [Llorente-Bousquets, Jorge; Jimena Castro-Gerardino, Diana] Smithsonian Inst, POB 3702, Washington, DC 20013 USA. RP Llorente-Bousquets, J (reprint author), Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Evolut Biol, Museo Zool Entomol, Mexico City, DF, Mexico.; Llorente-Bousquets, J (reprint author), Smithsonian Inst, POB 3702, Washington, DC 20013 USA. EM enantia@prodigy.net.mx; jflecrom@cable.ne.co NR 27 TC 0 Z9 0 U1 0 U2 0 PU SOUTHWESTERN ENTOMOLOGICAL SOC PI DALLAS PA 17360 COIT RD, DALLAS, TX 75252-6599 USA SN 0147-1724 EI 2162-2647 J9 SOUTHWEST ENTOMOL JI Southw. Entomol. PD DEC PY 2016 VL 41 IS 4 BP 1143 EP 1159 PG 17 WC Entomology SC Entomology GA ED3FB UT WOS:000388733700021 ER PT J AU Detto, M Muller-Landau, HC AF Detto, Matteo Muller-Landau, Helene C. TI Stabilization of species coexistence in spatial models through the aggregation-segregation effect generated by local dispersal and nonspecific local interactions SO THEORETICAL POPULATION BIOLOGY LA English DT Article DE Spatially explicit model; Nonspecific local interactions; Dispersal limitation; Time to extinction; Species diversity; Relative species abundance ID MOMENT EQUATIONS; COMPETITIVE COEXISTENCE; COMMUNITY MODELS; NATURAL ENEMIES; POPULATION; CONSEQUENCES; DIVERSITY; ECOLOGY; PLANTS; BIODIVERSITY AB Spatial interactions are widely acknowledged to play a significant role in sustaining diversity in ecological communities. However, theoretical work on this topic has focused on how spatial processes affect coexistence of species that differ in their strategies, with less attention to how spatial processes matter when competitors are equivalent. Furthermore, though it is recognized that models with local dispersal and local competition may sustain higher diversities of equivalent competitors than models in which these are not both localized, there is debate as to whether this reflects merely equalizing effects or whether there is also a stabilizing component. In this study, we explore how dispersal limitation and nonspecific local competition influence the outcome of species coexistence in communities driven by stochastic drift. We demonstrate that space alone acts as a stabilizing factor in a continuous space model with local dispersal and competition, as individuals of rare species on average experience lower total neighborhood densities, causing per capita reproductive rates to decrease systematically with increasing abundance. These effects prolong time to extinction in a closed system and enhance species diversity in an open system with constant immigration. Fundamentally, these stabilizing effects are obtained when dispersal limitation interacts with local competition to generate fluctuations in population growth rates. Thus this effect can be considered a fluctuating mechanism similar to spatial or temporal storage effects, but generated purely endogenously without requiring any exogenous environmental variability or species dissimilarities. (C) 2016 Elsevier Inc. All rights reserved. C1 [Detto, Matteo; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Panama City, Panama. RP Detto, M (reprint author), DPO AA, Unit 9100, Miami, FL 34002 USA. EM dettom@si.edu FU Smithsonian Institution Global Earth Observatory (SIGEO) FX We thank Peter Chesson and several anonymous reviewers for helpful comments on an earlier version of this manuscript. This work was supported by Smithsonian Institution Global Earth Observatory (SIGEO). NR 46 TC 0 Z9 0 U1 3 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0040-5809 EI 1096-0325 J9 THEOR POPUL BIOL JI Theor. Popul. Biol. PD DEC PY 2016 VL 112 BP 97 EP 108 DI 10.1016/j.tpb.2016.08.008 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA ED9EQ UT WOS:000389173400010 PM 27609405 ER PT J AU Greggor, AL Berger-Tal, O Blumstein, DT Angeloni, L Bessa-Gomes, C Blackwell, BF St Clair, CC Crooks, K de Silva, S Fernandez-Juricic, E Goldenberg, SZ Mesnick, SL Owen, M Price, CJ Saltz, D Schell, CJ Suarez, AV Swaisgood, RR Winchell, CS Sutherland, WJ AF Greggor, Alison L. Berger-Tal, Oded Blumstein, Daniel T. Angeloni, Lisa Bessa-Gomes, Carmen Blackwell, Bradley F. St Clair, Colleen Cassady Crooks, Kevin de Silva, Shermin Fernandez-Juricic, Esteban Goldenberg, Shifra Z. Mesnick, Sarah L. Owen, Megan Price, Catherine J. Saltz, David Schell, Christopher J. Suarez, Andrew V. Swaisgood, Ronald R. Winchell, Clark S. Sutherland, William J. TI Research Priorities from Animal Behaviour for Maximising Conservation Progress SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID POPULATION VIABILITY; ECOLOGICAL TRAPS; CLIMATE-CHANGE; ET-AL; WILDLIFE; BIOLOGY; DETERRENTS; FRAMEWORK; SCIENCE; AREAS AB Poor communication between academic researchers and wildlife managers limits conservation progress and innovation. As a result, input from overlapping fields, such as animal behaviour, is underused in conservation management despite its demonstrated utility as a conservation tool and countless papers advocating its use. Communication and collaboration across these two disciplines are unlikely to improve without clearly identified management needs and demonstrable impacts of behavioural-based conservation management. To facilitate this process, a team of wildlife managers and animal behaviour researchers conducted a research prioritisation exercise, identifying 50 key questions that have great potential to resolve critical conservation and management problems. The resulting agenda highlights the diversity and extent of advances that both fields could achieve through collaboration. C1 [Greggor, Alison L.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. [Berger-Tal, Oded; Saltz, David] Ben Gurion Univ Negev, Mitrani Dept Desert Ecol, Midreshet Ben Gurion, Israel. [Blumstein, Daniel T.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. [Angeloni, Lisa; Schell, Christopher J.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Bessa-Gomes, Carmen] Univ Paris Saclay, Ecol Systemat Evolut, Univ Paris Sud, CNRS,AgroParisTech, Orsay, France. [Blackwell, Bradley F.; Schell, Christopher J.] Wildlife Serv, USDA, Natl Wildlife Res Ctr, Ft Collins, CO USA. [St Clair, Colleen Cassady] Univ Alberta, Biol Sci, Edmonton, AB, Canada. [Crooks, Kevin] Colorado State Univ, Dept Fish Wildlife & Conservat Biol, Ft Collins, CO 80523 USA. [de Silva, Shermin] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [de Silva, Shermin] Trunk & Leaves Inc, Newtonville, MA USA. [Fernandez-Juricic, Esteban] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Goldenberg, Shifra Z.] Save Elephants, Nairobi, Kenya. [Mesnick, Sarah L.] Natl Marine Fisheries Serv, Southwest Fisheries Sci Ctr, Natl Ocean & Atmospher Adm, Washington, DC USA. [Owen, Megan; Swaisgood, Ronald R.] San Diego Zoo Global, Inst Conservat Res, Escondido, CA USA. [Price, Catherine J.] Univ Sydney, Sch Life & Environm Sci, Sydney, NSW, Australia. [Suarez, Andrew V.] Univ Illinois, Dept Anim Biol, Champaign, IL 61820 USA. [Suarez, Andrew V.] Univ Illinois, Dept Entomol, Champaign, IL 61820 USA. [Winchell, Clark S.] US Fish & Wildlife Serv, Conservat Partnerships Program, Carlsbad, CA USA. [Sutherland, William J.] Univ Cambridge, Conservat Sci Grp, Dept Zool, Cambridge, England. RP Greggor, AL (reprint author), Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. EM Alison.L.Greggor@dartmouth.edu OI Schell, Christopher/0000-0002-2073-9852; Greggor, Alison/0000-0003-0998-618X NR 84 TC 1 Z9 1 U1 26 U2 26 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD DEC PY 2016 VL 31 IS 12 BP 953 EP 964 DI 10.1016/j.tree.2016.09.001 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA EE2DU UT WOS:000389394700014 PM 27692480 ER PT J AU Remo, JL Lawrence, RJ Jacobsen, SB Furnish, MD AF Remo, J. L. Lawrence, R. J. Jacobsen, S. B. Furnish, M. D. TI High energy density soft X-ray momentum coupling to comet analogs for NEO mitigation SO ACTA ASTRONAUTICA LA English DT Article ID DEFLECTION AB We applied MBBAY high fluence pulsed radiation intensity driven momentum transfer analysis to calculate Xray momentum coupling coefficients C-M=(Pa s)/(J/m(2)) for two simplified comet analog materials: i) water ice, and ii) 70% water ice and 30% distributed olivine grains. The momentum coupling coefficients (C-M) (max) of 50x10(-5) s/m, are about an order of magnitude greater than experimentally determined and computed MBBAY values for meteoritic materials that are analogs for asteroids. From the values for comet analog materials we infer applied energies (via momentum transfer) required to deflect an Earth crossing comet from impacting Earth by a sufficient amount (-1 cm/s) to avert collision-a year in advance. Comet model calculations indicate for C-M=5x10(-4) s/m the deflection of a 2 km comet with a density 600 kg/m(3) by 1 cm/s requires an applied energy on the target surface of 5x10(13) J, the equivalent of 12 kT of TNT. Depending on the geometrical configuration of the interaction the explosive yield required could be an order of magnitude higher. C1 [Remo, J. L.] Harvard Univ, Dept Astron, 20 Oxford St, Cambridge, MA 02138 USA. [Remo, J. L.; Jacobsen, S. B.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Remo, J. L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lawrence, R. J.; Furnish, M. D.] Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. RP Furnish, MD (reprint author), Sandia Natl Labs, POB 5800, Albuquerque, NM 87185 USA. EM jremo@cfa.harvard.edu; mdfurni@sandia.gov FU Department of Energy National Nuclear Security Administration [DE-FG52-09NA29457, DE-NA0001804, DE-NA0002937]; Harvard University; U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000] FX A portion of this research was conducted under the Sandia Z Fundamental Science Program and supported by the Department of Energy National Nuclear Security Administration under Award Numbers DE-FG52-09NA29457, DE-NA0001804 and DE-NA0002937 to S. B. Jacobsen (PI) with Harvard University. This research is the authors' views and not those of the DOE. Sandia National Laboratories is a multi-mission laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. NR 17 TC 0 Z9 0 U1 5 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 EI 1879-2030 J9 ACTA ASTRONAUT JI Acta Astronaut. PD DEC PY 2016 VL 129 BP 384 EP 388 DI 10.1016/j.actaastro.2016.09.026 PG 5 WC Engineering, Aerospace SC Engineering GA ED7YF UT WOS:000389087900043 ER PT J AU Buchhave, LA Dressing, CD Dumusque, X Rice, K Vanderburg, A Mortier, A Lopez-Morales, M Lopez, E Lundkvist, MS Kjeldsen, H Affer, L Bonomo, AS Charbonneau, D Cameron, AC Cosentino, R Figueira, P Fiorenzano, AFM Harutyunyan, A Haywood, RD Johnson, JA Latham, DW Lovis, C Malavolta, L Mayor, M Micela, G Molinari, E Motalebi, F Nascimbeni, V Pepe, F Phillips, DF Piotto, G Pollacco, D Queloz, D Sasselov, D Segransan, D Sozzetti, A Udry, S Watson, C AF Buchhave, Lars A. Dressing, Courtney D. Dumusque, Xavier Rice, Ken Vanderburg, Andrew Mortier, Annelies Lopez-Morales, Mercedes Lopez, Eric Lundkvist, Mia S. Kjeldsen, Hans Affer, Laura Bonomo, Aldo S. Charbonneau, David Cameron, Andrew Collier Cosentino, Rosario Figueira, Pedro Fiorenzano, Aldo F. M. Harutyunyan, Avet Haywood, Raphaelle D. Johnson, John Asher Latham, David W. Lovis, Christophe Malavolta, Luca Mayor, Michel Micela, Giusi Molinari, Emilio Motalebi, Fatemeh Nascimbeni, Valerio Pepe, Francesco Phillips, David F. Piotto, Giampaolo Pollacco, Don Queloz, Didier Sasselov, Dimitar Segransan, Damien Sozzetti, Alessandro Udry, Stephane Watson, Chris TI A 1.9 EARTH RADIUS ROCKY PLANET AND THE DISCOVERY OF A NON-TRANSITING PLANET IN THE KEPLER-20 SYSTEM SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: composition; stars: individual; techniques: radial velocities ID SUPER-EARTHS; MASS PLANET; SOLAR-TYPE; HARPS-N; STELLAR; STARS; ASTEROSEISMOLOGY; PARAMETERS; EXOPLANETS; CANDIDATES AB Kepler-20 is a solar-type star (V = 12.5) hosting a compact system of five transiting planets, all packed within the orbital distance of Mercury in our own solar system. A transition from rocky to gaseous planets with a planetary transition radius of similar to 1.6 R-circle plus has recently been proposed by several articles in the literature. Kepler-20b (R-p similar to 1.9 R-circle plus) has a size beyond this transition radius; however, previous mass measurements were not sufficiently precise to allow definite conclusions to be drawn regarding its composition. We present new mass measurements of three of the planets in the Kepler-20 system that are facilitated by 104 radial velocity measurements from the HARPS-N spectrograph and 30 archival Keck/HIRES observations, as well as an updated photometric analysis of the Kepler data and an asteroseismic analysis of the host star (M-star = 0.948 +/- 0.051M and R-star =. 0.964 +/- 0.018 R). Kepler-20b is a 1.868(-0.034)(+0.066) R-circle plus planetiat 3.7 day period with a mass of 9.70(-1.44)(+1.41) M-circle plus, resulting in a mean density of 8.2(-1.3)(+1.5) g cm(-3), indicating a rocky composition with an iron-tosilicate ratio consistent with that of the Earth. This makes Kepler-20b the most massive planet with a rocky composition found to date. Furthermore, we report the discovery of an additional non-transiting planet with a minimum mass of 19.96(-3.61)(+3.08) M-circle plus and an orbital period of similar to 34 days in the gap between Kepler-20f (P similar to 11 days) and Kepler-20d (P similar to 78 days). C1 [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Dressing, Courtney D.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Dumusque, Xavier; Lovis, Christophe; Mayor, Michel; Motalebi, Fatemeh; Pepe, Francesco; Queloz, Didier; Segransan, Damien; Udry, Stephane] Univ Geneva, Observ Astron, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. [Rice, Ken; Lopez, Eric] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Vanderburg, Andrew; Lopez-Morales, Mercedes; Charbonneau, David; Haywood, Raphaelle D.; Johnson, John Asher; Latham, David W.; Phillips, David F.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Mortier, Annelies; Cameron, Andrew Collier] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Lundkvist, Mia S.; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Lundkvist, Mia S.] Heidelberg Univ, Zentrum Astron, Landessternwarte, Knigstuhl 12, D-69117 Heidelberg, Germany. [Affer, Laura; Micela, Giusi] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90124 Palermo, Italy. [Bonomo, Aldo S.; Sozzetti, Alessandro] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy. [Cosentino, Rosario; Fiorenzano, Aldo F. M.; Harutyunyan, Avet; Molinari, Emilio] INAF Fdn Galileo Galilei, Rambla Jose Ana Fernandez Perez 7, E-38712 Brena Baja, Spain. [Figueira, Pedro] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, PT-4150762 Oporto, Portugal. [Malavolta, Luca; Nascimbeni, Valerio; Piotto, Giampaolo] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy. [Malavolta, Luca; Piotto, Giampaolo] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Molinari, Emilio] INAF IASF Milano, Via Bassini 15, I-20133 Milan, Italy. [Pollacco, Don] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England. [Queloz, Didier] Cavendish Lab, JJ Thomson Ave, Cambridge CB3 0HE, England. [Watson, Chris] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Buchhave, LA (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark.; Buchhave, LA (reprint author), Univ Copenhagen, Niels Bohr Inst, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. EM buchhave@nbi.ku.dk RI Rice, Ken/H-5084-2011; Figueira, Pedro/J-4916-2013; OI Rice, Ken/0000-0002-6379-9185; Figueira, Pedro/0000-0001-8504-283X; Lundkvist, Mia Sloth/0000-0002-8661-2571; Buchhave, Lars A./0000-0003-1605-5666; Vanderburg, Andrew/0000-0001-7246-5438 FU Prodex Program of the Swiss Space Office (SSO); Harvard-University Origin of Life Initiative (HUOLI); Scottish Universities Physics Alliance (SUPA); University of Geneva; Smithsonian Astrophysical Observatory (SAO); Italian National Astrophysical Institute (INAF); University of St. Andrews; Queen's University Belfast; University of Edinburgh; European Union Seventh Framework Programme (FP7) [313014]; NASA through the Sagan Fellowship Program; NSF Graduate Research Fellowship [DGE 1144152]; John Templeton Foundation; NASA [NNX15AC90G]; Danish National Research Foundation [DNRF106]; ASTERISK project - European Research Council [267864]; Danish Council for Independent Research's Sapere Aude program [DFF-5051-00130]; Fundacao para a Ciencia e a Tecnologia (FCT) through Investigador FCT [IF/01037/2013]; FEDER; Society in Science-Branco Weiss Fellowship; [IF/01037/2013CP1191/CT0001] FX The HARPS-N project was funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard-University Origin of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), University of St. Andrews, Queen's University Belfast, and University of Edinburgh. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/20072013) under Grant Agreement No. 313014 (ETAEARTH).; This work was performed in part under contract with the California Institute of Technology/Jet Propulsion Laboratory, which is funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute.; A.V. is supported by the NSF Graduate Research Fellowship, Grant No. DGE 1144152.; This publication was made possible by a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. This material is based upon work supported by NASA under grant No. NNX15AC90G issued through the Exoplanets Research Program.; Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement no.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no.: 267864). M.S.L. is supported by The Danish Council for Independent Research's Sapere Aude program (grant agreement no.: DFF-5051-00130).; P.F. acknowledges support by Fundacao para a Ciencia e a Tecnologia (FCT) through Investigador FCT contract of reference IF/01037/2013 and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade-COMPETE," and further support in the form of an exploratory project of reference IF/01037/2013CP1191/CT0001.; The research leading to these results also received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH).; X.D. is grateful to the Society in Science-Branco Weiss Fellowship for its financial support. NR 61 TC 1 Z9 1 U1 6 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 160 DI 10.3847/0004-6256/152/6/160 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED1TB UT WOS:000388626700001 ER PT J AU de Val-Borro, M Bakos, GA Brahm, R Hartman, JD Espinoza, N Penev, K Ciceri, S Jordan, A Bhatti, W Csubry, Z Bayliss, D Bento, J Zhou, G Rabus, M Mancini, L Henning, T Schmidt, B Tan, TG Tinney, CG Wright, DJ Kedziora-Chudczer, L Bailey, J Suc, V Durkan, S Lazar, J Papp, I Sari, P AF de Val-Borro, M. Bakos, G. A. Brahm, R. Hartman, J. D. Espinoza, N. Penev, K. Ciceri, S. Jordan, A. Bhatti, W. Csubry, Z. Bayliss, D. Bento, J. Zhou, G. Rabus, M. Mancini, L. Henning, T. Schmidt, B. Tan, T. G. Tinney, C. G. Wright, D. J. Kedziora-Chudczer, L. Bailey, J. Suc, V. Durkan, S. Lazar, J. Papp, I. Sari, P. TI HATS-31B THROUGH HATS-35B: FIVE TRANSITING HOT JUPITERS DISCOVERED BY THE HATSOUTH SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual; techniques: photometric; techniques: spectroscopic ID PLANET-DETECTION; KEPLER FIELD; STAR; STELLAR; TELESCOPE; MISSION; MASS; ISOCHRONES; ALGORITHM; NETWORK AB We report the discovery of five new transiting hot-Jupiter planets discovered by the HATSouth survey, HATS-31b through HATS-35b. These planets orbit moderately bright stars with V magnitudes within the range of 11.9-14.4 mag while the planets span a range of masses of. 0.88-1.22 M-J. and have somewhat inflated radii between 1.23 and 1.64 R-J. These planets can be classified as typical hot Jupiters, with HATS-31b and HATS-35b being moderately inflated gas giant planets with radii of 1.64 +/- 0.22 R-J and 1.464(-0.044)(+0.069) R-J, respectively, that can be used to constrain inflation mechanisms. All five systems present a higher Bayesian evidence for a fixed-circular-orbit model than for an eccentric orbit. The orbital periods range from 1.8209993 +/- 0.0000016 day for HATS-35b) to 3.377960 +/- 0.000012 day for HATS-31b. Additionally, HATS-35b orbits a relatively young F star with an age of 2.13 +/- 0.51 Gyr. We discuss the analysis to derive the properties of these systems and compare them in the context of the sample of well-characterized transiting hot Jupiters known to date. C1 [de Val-Borro, M.; Bakos, G. A.; Hartman, J. D.; Penev, K.; Bhatti, W.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Brahm, R.; Espinoza, N.; Jordan, A.; Rabus, M.; Suc, V.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile. [Brahm, R.; Espinoza, N.; Jordan, A.] Millennium Inst Astrophys, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile. [Ciceri, S.; Rabus, M.; Mancini, L.; Henning, T.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Ciceri, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Bayliss, D.] Univ Geneva, Observ Astron, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. [Bento, J.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Zhou, G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Tinney, C. G.; Wright, D. J.; Kedziora-Chudczer, L.; Bailey, J.] Univ New South Wales, Sch Phys, Exoplanetary Sci, Sydney, NSW 2052, Australia. [Tinney, C. G.; Wright, D. J.; Kedziora-Chudczer, L.; Bailey, J.] Univ New South Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Durkan, S.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, H-1451 Budapest, Hungary. RP de Val-Borro, M (reprint author), Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. OI Bakos, Gaspar/0000-0001-7204-6727; Espinoza Perez, Nestor/0000-0001-9513-1449; Tan, Thiam-Guan/0000-0001-5603-6895; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI [NSF/AST-0723074]; NASA [NNX09AB29G, NNX12AH91H]; FONDECYT [1130857]; Millenium Science Initiative, Chilean Ministry of Economy [IC120009]; CONICYT-PCHA/Doctorado Nacional; Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; BASAL CATA [PFB-06]; FONDECYT postdoctoral fellowship [3120097]; ARC Laureate Fellowship [FL0992131]; Robert Martin Ayers Sciences Fund; SIMBAD database; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074. Operations have been supported by NASA grants NNX09AB29G and NNX12AH91H. and follow-up observations receive partial support from grant NSF/AST-1108686. A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. are supported by CONICYT-PCHA/Doctorado Nacional. R.B. and N.E. acknowledge additional support from project IC120009 "Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. M.R. acknowledges support from FONDECYT postdoctoral fellowship 3120097. This work is based on observations made with ESO Telescopes at the La Silla Observatory. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. Operations at the MPG. 2.2 m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. We thank the MPG. 2.2 m Telescope support crew for their technical assistance during observations. We are grateful to P. Sackett for her help in the early phase of the HATSouth project. G.B. wishes to thank the warm hospitality of Adele and Joachim Cranz at the farm Isabis, supporting the operations and service missions of HATSouth. Observing times. were obtained through proposals CN2013A-171, CN2013B-55, CN2014A-104, CN2014B-57, CN2015A-51, and ESO 096.C-0544. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. NR 38 TC 0 Z9 0 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 161 DI 10.3847/0004-6256/152/6/161 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED1TB UT WOS:000388626700002 ER PT J AU Grunblatt, SK Huber, D Gaidos, EJ Lopez, ED Fulton, BJ Vanderburg, A Barclay, T Fortney, JJ Howard, AW Isaacson, HT Mann, AW Petigura, E Aguirre, VS Sinukoff, EJ AF Grunblatt, Samuel K. Huber, Daniel Gaidos, Eric J. Lopez, Eric D. Fulton, Benjamin J. Vanderburg, Andrew Barclay, Thomas Fortney, Jonathan J. Howard, Andrew W. Isaacson, Howard T. Mann, Andrew W. Petigura, Erik Aguirre, Victor Silva Sinukoff, Evan J. TI K2-97b: A (RE-?)INFLATED PLANET ORBITING A RED GIANT STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE asteroseismology; planets and satellites: detection; planets and satellites: gaseous planets; planets and satellites: physical evolution; planet-star interactions ID SOLAR-LIKE OSCILLATIONS; TRANSITING EXTRASOLAR PLANETS; HOT JUPITERS; LIGHT CURVES; M-DWARF; FUNDAMENTAL PROPERTIES; STELLAR EVOLUTION; ERROR-CORRECTION; BROWN DWARFS; HOST STARS AB Strongly irradiated giant planets are observed to have radii larger than thermal evolution models predict. Although these inflated planets have been known for over 15 years, it is unclear whether their inflation is caused by the. deposition of energy from the host star. or the. inhibited cooling of the planet. These processes can be distinguished if the planet becomes highly irradiated only when the host star evolves onto the red giant branch. We report the discovery of K2-97b, a 1.31 +/- 0.11 R-J, 1.10 +/- 0.11 M-J planet orbiting a 4.20 +/- 0.14 R-circle dot, 1.16 +/- 0.12 M-circle dot red giant star with an orbital period of 8.4 days. We precisely constrained stellar and planetary parameters by combining asteroseismology, spectroscopy, and granulation noise modeling along with transit and radial velocity measurements. The uncertainty in planet radius is dominated by systematic differences in transit depth, which we measure to be up to 30% between different light-curve reduction methods. Our calculations indicate the incident flux on this planet was 170(-60)(+140) times the incident flux on Earth, while the star was on the main sequence. Previous studies suggest that this incident flux is insufficient to delay planetary cooling enough to explain the present planet radius. This system thus provides the first evidence that planets may be inflated directly by incident stellar radiation rather than by delayed loss of heat from formation. Further studies of planets around red giant branch stars will confirm or contradict this hypothesis. and may reveal a new class of re-inflated planets. C1 [Grunblatt, Samuel K.; Fulton, Benjamin J.; Howard, Andrew W.; Sinukoff, Evan J.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Huber, Daniel] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia. [Huber, Daniel] SETI Inst, 189 Bernardo Ave, Mountain View, CA 94043 USA. [Huber, Daniel; Aguirre, Victor Silva] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Gaidos, Eric J.] Univ Hawaii Manoa, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Gaidos, Eric J.] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [Lopez, Eric D.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Blackford Hill, Edinburgh, Midlothian, Scotland. [Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Howard, Andrew W.; Petigura, Erik] CALTECH, Pasadena, CA 91125 USA. [Isaacson, Howard T.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Mann, Andrew W.] Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. RP Grunblatt, SK (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM skg@ifa.hawaii.edu OI Isaacson, Howard/0000-0002-0531-1073; Vanderburg, Andrew/0000-0001-7246-5438; Fulton, Benjamin/0000-0003-3504-5316 FU NASA [NNX11AC33G, NNX16AH45G, NAS5-26555, NNX09AF08G]; Australian Research Council [DE140101364]; National Aeronautics and Space Administration [NNX14AB92G]; University of Hawaii; University of California; California Institute of Technology; European Union [313014]; National Science Foundation [2014184874] FX The authors would like to thank Jeffrey C. Smith, Suzanne Aigrain, and Travis Berger for helpful discussions. This research was supported by NASA Origins of Solar Systems grant NNX11AC33G to E.G. and by the NASA K2 Guest Observer Award NNX16AH45G to D.H.. D.H. acknowledges support by the Australian Research Council's Discovery Projects funding scheme (project number DE140101364) and support by the National Aeronautics and Space Administration under Grant NNX14AB92G issued through the Kepler Participating Scientist Program. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at Exoplanets. org. This work was based on observations at the W. M. Keck Observatory granted by the University of Hawaii, the University of California, and the California Institute of Technology. We thank the observers who contributed to the measurements reported here and acknowledge the efforts of the Keck Observatory staff. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. SNIFS on the UH 2.2 m telescope is part of the Nearby Supernova Factory project, a scientific collaboration among the Centre de Recherche Astronomique de Lyon, Institut de Physique Nuclaire de Lyon, Laboratoire de Physique Nuclaire et des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and the Centre de Physique des Particules de Marseille. Based on data from the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. Some/all of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of the SIMBAD and VIZIER Astronomical Databases, operated at CDS, Strasbourg, France (http://cdsweb.u-strasbg.fr/), and of NASAs Astrophysics Data System, of the Jean-Marie Mariotti Center Search service (http://www.jmmc.fr/searchcal), co-developed by FIZEAU and LAOG/IPAG. E.D.L. received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). B.J.F. notes that this material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 2014184874. Any opinion, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. NR 108 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 185 DI 10.3847/0004-6256/152/6/185 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED7OS UT WOS:000389057100003 ER PT J AU Piskorz, D Benneke, B Crockett, NR Lockwood, AC Blake, GA Barman, TS Bender, CF Bryan, ML Carr, JS Fischer, DA Howard, AW Isaacson, H Johnson, JA AF Piskorz, Danielle Benneke, Bjorn Crockett, Nathan R. Lockwood, Alexandra C. Blake, Geoffrey A. Barman, Travis S. Bender, Chad F. Bryan, Marta L. Carr, John S. Fischer, Debra A. Howard, Andrew W. Isaacson, Howard Johnson, John A. TI EVIDENCE FOR THE DIRECT DETECTION OF THE THERMAL SPECTRUM OF THE NON-TRANSITING HOT GAS GIANT HD 88133 b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; techniques: spectroscopic ID TAU BOOTIS B; ORBITAL MOTION; LINE-PROFILES; F-STAR; EXOPLANET; MASS; ATMOSPHERES; WATER; SPECTROMETER; SPECTROSCOPY AB We target the thermal emission spectrum of the non-transiting gas giant HD 88133 b with high-resolution near-infrared spectroscopy, by treating the planet and its host star as a spectroscopic binary. For sufficiently deep summed flux observations of the star and planet across multiple epochs, it is possible to resolve the signal of the hot gas giant's atmosphere compared to the brighter stellar spectrum, at a level consistent with the aggregate shot noise of the full data set. To do this, we first perform a principal component analysis to remove the contribution of the Earth's atmosphere to the observed spectra. Then, we use a cross-correlation analysis to tease out the spectra of the host star and HD 88133 b to determine its orbit and identify key sources of atmospheric opacity. In total, six epochs of Keck NIRSPEC L-band observations and three epochs of Keck NIRSPEC K-band observations of the HD 88133 system were obtained. Based on an analysis of the maximum likelihood curves calculated from the multi-epoch cross-correlation of the full data set with two atmospheric models, we report the direct detection of the emission spectrum of the non-transiting exoplanet HD 88133 b and measure a radial projection of the Keplerian orbital velocity of 40 +/- 15 km s(-1), a true mass of 1.02(-0.28)(+0.61) M-J, a nearly face-on orbital inclination of 15(-5)(+60), and an atmosphere opacity structure at high dispersion dominated by water vapor. This, combined with 11 years of radial velocity measurements of the system, provides the most up-to-date ephemeris for HD 88133. C1 [Piskorz, Danielle; Benneke, Bjorn; Crockett, Nathan R.; Lockwood, Alexandra C.; Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lockwood, Alexandra C.] King Abdullah Univ Sci & Technol, Thuwal, Saudi Arabia. [Barman, Travis S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Bender, Chad F.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Bender, Chad F.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bryan, Marta L.; Howard, Andrew W.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Carr, John S.] Naval Res Lab, Washington, DC 20375 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, 260 Whitney Ave, New Haven, CT 06520 USA. [Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Johnson, John A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson, John A.] Inst Theory & Computat, Cambridge, MA 02138 USA. RP Piskorz, D (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. OI Fischer, Debra/0000-0003-2221-0861 FU W.M. Keck Foundation; NSF Astronomy Astrophysics; NASA Exoplanets Research Programs [AST-1109857, NNX16AI14G]; Pennsylvania State Unviersity; Eberly College of Science; Pennsylvania Space Grant Consortium; 6.1 base funding FX The authors would like to thank Heather Knutson for helpful discussions throughout the preparation of this manuscript. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work was partially supported by funding from the NSF Astronomy & Astrophysics and NASA Exoplanets Research Programs (grants AST-1109857 and NNX16AI14G, G.A. Blake P.I.), and the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State Unviersity, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Basic research in infrared astrophysics at the Naval Research Laboratory is supported by 6.1 base funding. Finally, we thank an anonymous reviewer for helpful insights which improved the content of this paper. NR 49 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 131 DI 10.3847/0004-637X/832/2/131 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED7MM UT WOS:000389049800002 ER PT J AU Stello, D Vanderburg, A Casagrande, L Gilliland, R Aguirre, VS Sandquist, E Leiner, E Mathieu, R Soderblom, DR AF Stello, Dennis Vanderburg, Andrew Casagrande, Luca Gilliland, Ron Aguirre, Victor Silva Sandquist, Eric Leiner, Emily Mathieu, Robert Soderblom, David R. TI THE K2 M67 STUDY: REVISITING OLD FRIENDS WITH K2 REVEALS OSCILLATING RED GIANTS IN THE OPEN CLUSTER M67 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (M67); stars: fundamental parameters; stars: interiors; stars: oscillations (including pulsations); techniques: photometric ID SOLAR-LIKE OSCILLATIONS; NGC 6819; GALACTIC ARCHAEOLOGY; ECLIPSING BINARY; KEPLER MISSION; BOLOMETRIC CORRECTIONS; POPULATION SYNTHESIS; SCALING RELATION; CCD PHOTOMETRY; STARS AB Observations of stellar clusters have had a tremendous impact in forming our understanding of stellar evolution. The open cluster M67 has a particularly important role as a calibration benchmark for stellar evolution theory due to its near-solar composition and age. As a result, it has been observed extensively, including attempts to detect solar-like oscillations in its main sequence and red giant stars. However, any asteroseismic inference has so far remained elusive due to the difficulty in measuring these extremely low-amplitude oscillations. Here we report the first unambiguous detection of solar-like oscillations in the red giants of M67. We use data from the Kepler ecliptic mission, K2, to measure the global asteroseismic properties. We find a model-independent seismic-informed distance of 816 +/- 11 pc, or (m - M)(0) = 9.57 +/- 0.03 mag, an average red giant mass of 1.36 +/- 0.01 M-circle dot, in agreement with the dynamical mass from an eclipsing binary near the cluster turn-off, and ages of individual stars compatible with isochrone fitting. We see no evidence of strong mass loss on the red giant branch. We also determine seismic log g of all the cluster giants with a typical precision of similar to 0.01 dex. Our results generally show good agreement with independent methods and support the use of seismic scaling relations to determine global properties of red giant stars with near-solar metallicity. We further illustrate that the data are of such high quality that future work on individual mode frequencies should be possible, which would extend the scope of seismic analysis of this cluster. C1 [Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Stello, Dennis] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia. [Stello, Dennis; Aguirre, Victor Silva] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Casagrande, Luca] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Gilliland, Ron] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Sandquist, Eric] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Leiner, Emily; Mathieu, Robert] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Soderblom, David R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Stello, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia.; Stello, D (reprint author), Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia.; Stello, D (reprint author), Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. OI Stello, Dennis/0000-0002-4879-3519; Vanderburg, Andrew/0000-0001-7246-5438; Soderblom, David/0000-0002-0322-8161 FU Danish National Research Foundation [DNRF106]; ASTERISK project - European Research Council [267864]; Australian Research Council; NSF [DGE 1144152]; VILLUM FONDEN [10118] FX We acknowledge Susan Agrain, Tim Bedding, Karsten Brogaard, Hans Kjeldsen, Daniel Huber, Marc Pionsonneault, and Jie Yu for fruitful discussions and helpful comments. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). The research was supported by the ASTERISK project (ASTER-oseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement No. 267864). D.S. acknowledges support from the Australian Research Council. A.V. is supported by the NSF Graduate Research Fellowship, Grant No. DGE 1144152. V.S.A. acknowledges support from VILLUM FONDEN (research grant 10118). NR 56 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2016 VL 832 IS 2 AR 133 DI 10.3847/0004-637X/832/2/133 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED7MM UT WOS:000389049800004 ER PT J AU Racicot, RA Gearty, W Kohno, N Flynn, JJ AF Racicot, Rachel A. Gearty, William Kohno, Naoki Flynn, John J. TI Comparative anatomy of the bony labyrinth of extant and extinct porpoises (Cetacea: Phocoenidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE auditory acuity; Cetacea; CT scan; inner ear ID HIGH-FREQUENCY CLICKS; INNER-EAR; TOOTHED WHALES; COCHLEAR STRUCTURE; BASILAR-MEMBRANE; UPPER MIOCENE; SKULL SHAPE; HEARING; ODONTOCETI; EVOLUTION AB The inner ear anatomy of cetaceans, now more readily accessible by means of nondestructive high-resolution X-ray computed tomographic (CT) scanning, provides a window into their acoustic abilities and ecological preferences. Inner ear labyrinths also may be a source for additional morphological characters for phylogenetic analyses. In this study, we explore digital endocasts of the inner ear labyrinths of representative species of extinct and extant porpoises (Mammalia: Cetacea: Phocoenidae), a clade of some of the smallest odontocete cetaceans, which produce some of the highest-frequency clicks for biosonar and communication. Metrics used to infer hearing ranges based on cochlear morphology indicate that all taxa considered could hear high-frequency sounds, thus the group had already acquired high-frequency hearing capabilities by the Miocene (9-11Mya) at the latest. Vestibular morphology indicates that extant species with pelagic preferences have similarly low semicircular canal deviations from 90 degrees, values indicating more sensitivity to head rotations. Species with near-shore preferences have higher canal deviation values, indicating less sensitivity to head rotations. Extending these analyses to the extinct species, we demonstrate a good match between those predicted to have coastal (such as Semirostrum cerutti) preferences and high canal deviation values. We establish new body length relationships based on correlations with inner ear labyrinth volume, which can be further explored among other aquatic mammals to infer body size of specimens consisting of fragmentary material. C1 [Racicot, Rachel A.] Nat Hist Museum Los Angeles Cty, Dinosaur Inst, Los Angeles, CA USA. [Racicot, Rachel A.] Smithsonian Inst, POB 37012,MRC 121, Washington, DC 20013 USA. [Gearty, William] Stanford Univ, Dept Geol Sci, Stanford, CA 94305 USA. [Kohno, Naoki] Natl Museum Nat & Sci, Dept Geol & Paleontol, Div Biot Evolut, Tokyo, Japan. [Kohno, Naoki] Univ Tsukuba, Grad Sch Life & Environm Sci, Tsukuba, Ibaraki, Japan. [Flynn, John J.] Amer Museum Nat Hist, Dept Vertebrate Paleontol, Div Paleontol, New York, NY 10024 USA. [Flynn, John J.] Amer Museum Nat Hist, Richard Gilder Grad Sch, New York, NY 10024 USA. RP Racicot, RA (reprint author), Nat Hist Museum Los Angeles Cty, Dinosaur Inst, Los Angeles, CA USA.; Racicot, RA (reprint author), Smithsonian Inst, POB 37012,MRC 121, Washington, DC 20013 USA. EM rracicot@nhm.org FU Yale Institute for Biospheric Studies Dissertation Enhancement Grant; AMNH Lerner-Gray Fund for Marine Research; NSF-East Asia Pacific Summer Institute; NSF [DEB 1331980, PLR 134175] FX Scans were funded in part by a Yale Institute for Biospheric Studies Dissertation Enhancement Grant, AMNH Lerner-Gray Fund for Marine Research, and NSF-East Asia Pacific Summer Institute grant to RAR, who is presently funded by NSF (grants DEB 1331980 and PLR 134175). We thank museums and staff for access to specimens and loaning specimens for CT scanning: T. Demere and K. Randall (SDNHM); K. Helgen and C. Potter (NMNH); C. Conroy (MVZ, Berkeley); M. Flannery (CAS); P. Holroyd (UCMP); N.R.P. Gooddall (AMMA); R. Pittman and W. Perrin (Southwest Fisheries Science Center); E. Westwig and N. Duncan (AMNH); T. K. Yamada, Y. Tajima, N. Kurihara (NMNS); Y. Hikida (NMV); S. Yamashita (NFM); H. Furusawa (SMAC); Y. Okazaki and H. Ohashi (KMNH); and H. Sawamura (AMP). The authors thank M. Colbert and J. Maisano at the University of Texas High-Resolution X-Ray CT facility, J. Thostensen and M. Hill of the AMNH MIF, and C. Sakata of the National Museum of Nature and Science, Tokyo, for CT scanning specimens for this study. We gratefully acknowledge the helpful comments of the reviewers (Drs. Maeva Orliac, Eric Ekdale, and Robert W. Boessenecker), which significantly improved the final version of this manuscript. NR 68 TC 0 Z9 0 U1 3 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4066 EI 1095-8312 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD DEC PY 2016 VL 119 IS 4 BP 831 EP 846 DI 10.1111/bij.12857 PG 16 WC Evolutionary Biology SC Evolutionary Biology GA ED0AO UT WOS:000388505600006 ER PT J AU Yang, YS Richards-Zawacki, CL Devar, A Dugas, MB AF Yang, Yusan Richards-Zawacki, Corinne L. Devar, Anisha Dugas, Matthew B. TI Poison frog color morphs express assortative mate preferences in allopatry but not sympatry SO EVOLUTION LA English DT Article DE Behavioral isolation; contact zone; female preference; polymorphism; speciation ID DEL-TORO-ARCHIPELAGO; SEXUAL SELECTION; DENDROBATES-PUMILIO; REPRODUCTIVE ISOLATION; HYBRID ZONE; DART FROG; POPULATION DIVERGENCE; OOPHAGA-PUMILIO; NO EVIDENCE; SPECIATION AB The concurrent divergence of mating traits and preferences is necessary for the evolution of reproductive isolation via sexual selection, and such coevolution has been demonstrated in diverse lineages. However, the extent to which assortative mate preferences are sufficient to drive reproductive isolation in nature is less clear. Natural contact zones between lineages divergent in traits and preferences provide exceptional opportunities for testing the predicted evolutionary consequences of such divergence. The strawberry poison frog (Oophaga pumilio) displays extreme color polymorphism in and around the young Bocas del Toro archipelago. In a transition zone between red and blue allopatric lineages, we asked whether female preferences diverged along with coloration, and whether any divergent preferences persist in a zone of sympatry. When choosing among red, blue and phenotypically intermediate males, females from monomorphic red and monomorphic blue populations both expressed assortative preferences. However, red, blue, and intermediate females from the contact zone all preferred red males, suggesting that divergent preferences may be insufficient to effect behavioral isolation. Our results highlight the complexity of behavioral isolation, and the need for studies that can reveal the circumstances under which divergent preferences do and do not contribute to speciation. C1 [Yang, Yusan; Richards-Zawacki, Corinne L.; Devar, Anisha] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Yang, Yusan; Richards-Zawacki, Corinne L.] Univ Pittsburgh, Dept Biol Sci, Pittsburgh, PA 15260 USA. [Yang, Yusan] Univ Pittsburgh, Dept Biol Sci, 2429 Fifth Ave, Pittsburgh, PA 15260 USA. [Richards-Zawacki, Corinne L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Dugas, Matthew B.] Case Western Reserve Univ, Dept Biol, Cleveland, OH 44106 USA. RP Yang, YS (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA.; Yang, YS (reprint author), Univ Pittsburgh, Dept Biol Sci, Pittsburgh, PA 15260 USA. EM yusan.yang8@gmail.com FU National Science Foundation [1146370] FX We thank Deyvis Gonzalez, Ricardo Cossio, Justin Yeager, and numerous undergraduates for captive frog care and Caitlin Wamelink for compiling data for these analyses. Simone Blomenkamp and Heike Prohl generously shared unpublished analyses. Nathan Brouwer and Ling-Wan Chen provided suggestions and programming help on statistical analysis. Janette Boughman and two anonymous reviewers provided comments that greatly improved the quality of this manuscript. The Smithsonian Tropical Research Institute provided logistical support, and we particularly thank Gabriel Jacome and Plinio Gondola of the Bocas del Toro Research Station. This study was supported by a grant from the National Science Foundation (Award. No. 1146370). The Panamanian National Authority for the Environment (ANAM) provided research, collection, and export permission. This work complied with IACUC protocols (Tulane University Nos. 0382 and 0382R and STRI No. 2007-17-12-15-07 and 2012-0519-2015). NR 75 TC 1 Z9 1 U1 18 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD DEC PY 2016 VL 70 IS 12 BP 2778 EP 2788 DI 10.1111/evo.13079 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA ED1SD UT WOS:000388624300010 PM 27704539 ER PT J AU Peron, G Gaillard, JM Barbraud, C Bonenfant, C Charmantier, A Choquet, R Coulson, T Grosbois, V Loison, A Marzolin, G Owen-Smith, N Pardo, D Plard, F Pradel, R Toigo, C Gimenez, O AF Peron, Guillaume Gaillard, Jean-Michel Barbraud, Christophe Bonenfant, Christophe Charmantier, Anne Choquet, Remi Coulson, Tim Grosbois, Vladimir Loison, Anne Marzolin, Gilbert Owen-Smith, Norman Pardo, Deborah Plard, Floriane Pradel, Roger Toigo, Carole Gimenez, Olivier TI Evidence of reduced individual heterogeneity in adult survival of long-lived species SO EVOLUTION LA English DT Article DE Capture-recapture; comparative analyses; individual differences; life-history evolution; mixture models; random-effect models; vertebrates ID CAPTURE-RECAPTURE MODELS; LIFE-HISTORY TRAITS; JOLLY-SEBER MODEL; GENERATION TIME; MARKED ANIMALS; POPULATIONS; SENESCENCE; AGE; MORTALITY; EVOLUTION AB The canalization hypothesis postulates that the rate at which trait variation generates variation in the average individual fitness in a population determines how buffered traits are against environmental and genetic factors. The ranking of a species on the slow-fast continuum - the covariation among life-history traits describing species-specific life cycles along a gradient going from a long life, slow maturity, and low annual reproductive output, to a short life, fast maturity, and high annual reproductive output - strongly correlates with the relative fitness impact of a given amount of variation in adult survival. Under the canalization hypothesis, long-lived species are thus expected to display less individual heterogeneity in survival at the onset of adulthood, when reproductive values peak, than short-lived species. We tested this life-history prediction by analysing long-term time series of individual-based data in nine species of birds and mammals using capture-recapture models. We found that individual heterogeneity in survival was higher in species with short-generation time (< 3 years) than in species with long generation time (> 4 years). Our findings provide the first piece of empirical evidence for the canalization hypothesis at the individual level from the wild. C1 [Peron, Guillaume] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Peron, Guillaume; Gaillard, Jean-Michel; Bonenfant, Christophe; Plard, Floriane] UCB Lyon 1, UMR 5558, CNRS, LBBE Biometrie & Biol Evolut, F-69622 Villeurbanne, France. [Barbraud, Christophe] Univ La Rochelle, CNRS, Ctr Etud Biol Chize, UMR 7372, F-79360 Villiers En Bois, France. [Charmantier, Anne; Choquet, Remi; Marzolin, Gilbert; Pardo, Deborah; Pradel, Roger; Gimenez, Olivier] Univ Paul Valery Montpellier, EPHE, Univ Montpellier, CEFE,UMR 5175,CNRS, 1919 Route Mende, F-34293 Montpellier 5, France. [Coulson, Tim] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Grosbois, Vladimir] UR AGIRs Anim & Gest Integree Risques, TA C 22-E Campus Int Baillarguet, F-34398 Montpellier 5, France. [Loison, Anne] Univ Savoie Mt Blanc, Lab Ecol Alpine, F-73376 Le Bourget Du Lac, France. [Loison, Anne] CNRS, Lab Ecol Alpine, F-38000 Grenoble, France. [Owen-Smith, Norman] Univ Witwatersrand, Sch Anim Plant & Environm Sci, Ctr African Ecol, ZA-2050 Johannesburg, South Africa. [Plard, Floriane] Swiss Ornithol Inst, CH-6204 Sempach, Switzerland. [Toigo, Carole] ONCFS Unite Faune Montagne, 5 Allee Bethleem, F-38610 Zi De Mayencin, Gieres, France. RP Peron, G (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA.; Peron, G (reprint author), UCB Lyon 1, UMR 5558, CNRS, LBBE Biometrie & Biol Evolut, F-69622 Villeurbanne, France. EM peron_guillaume@yahoo.fr RI Choquet, Remi/F-6462-2011 FU IPEV program [109]; Office National de la Chasse et de la Faune Sauvage; BioAdapt grant [ANR-12-ADAP-0006-02-PEPS]; ANR grant [08-JCJC-0028-01] FX We thank everyone involved in fieldwork and data management for the long-term monitoring of marked individuals. Critical support for the longterm studies was provided by IPEV program no109, Zone Atelier Antarctique, and TAAF; Office National de la Chasse et de la Faune Sauvage; BioAdapt grant ANR-12-ADAP-0006-02-PEPS to A.C.; ANR grant 08-JCJC-0028-01 to O.G. This is a contribution of the GDR 3645 "Statistical Ecology." We are most grateful to Stephen Dobson for insightful comments on an earlier draft of this article. NR 33 TC 0 Z9 0 U1 15 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0014-3820 EI 1558-5646 J9 EVOLUTION JI Evolution PD DEC PY 2016 VL 70 IS 12 BP 2909 EP 2914 DI 10.1111/evo.13098 PG 6 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA ED1SD UT WOS:000388624300020 PM 27813056 ER PT J AU Zattara, EE Bely, AE AF Zattara, Eduardo E. Bely, Alexandra E. TI Phylogenetic distribution of regeneration and asexual reproduction in Annelida: regeneration is ancestral and fission evolves in regenerative clades SO INVERTEBRATE BIOLOGY LA English DT Article DE Annelida; regeneration; asexual reproduction; fission; phylogenetic methods; evolution; post-embryonic development; ancestral state reconstruction ID PLANARIAN DUGESIA-JAPONICA; NEMATOSTELLA-VECTENSIS; MOLECULAR PHYLOGENY; ANIMAL REGENERATION; EVOLUTIONARY LOSS; CHARACTER STATES; GENE-EXPRESSION; SEQUENCE DATA; POLYCHAETA; CLITELLATA AB Regeneration, the ability to replace lost body structures, and agametic asexual reproduction, such as fission and budding, are post-embryonic developmental capabilities widely distributed yet highly variable across animals. Regeneration capabilities vary dramatically both within and across phyla, but the evolution of regeneration ability has rarely been reconstructed in an explicitly phylogenetic context. Agametic reproduction appears strongly associated with high regenerative abilities, and there are also extensive developmental similarities between these two processes, suggesting that the two are evolutionarily related. However, the directionality leading to this relationship remains unclear: while it has been proposed that regeneration precedes asexual reproduction, the reverse hypothesis has also been put forward. Here, we use phylogenetically explicit methods to reconstruct broad patterns of regeneration evolution and formally test these hypotheses about the evolution of fission in the phylum Annelida (segmented worms). We compiled from the literature a large dataset of information on anterior regeneration, posterior regeneration, and fission abilities for 401 species and mapped this information onto a phylogenetic tree based on recent molecular studies. We used Markovian maximum likelihood and Bayesian MCMC methods to evaluate different models for the evolution of regeneration and fission and to estimate the likelihood of each of these traits being present at each node of the tree. Our results strongly support anterior and posterior regeneration ability being present at the basal node of the annelid tree and being lost 18 and 5 times, respectively, but never regained. By contrast, the ability to fission is reconstructed as being absent at the basal node and being gained at least 19 times, with several possible losses. Models assuming independent evolution of regeneration and fission yield significantly lower likelihoods. Our findings suggest that anterior and posterior regeneration are ancestral for Annelida and are consistent with the hypothesis that regenerative ability is required to evolve fission. C1 [Zattara, Eduardo E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Zattara, Eduardo E.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. [Zattara, Eduardo E.; Bely, Alexandra E.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Zattara, EE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA.; Zattara, EE (reprint author), Indiana Univ, Dept Biol, Bloomington, IN 47405 USA.; Zattara, EE (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM ezattara@gmail.com OI Zattara, Eduardo/0000-0002-9947-9036 NR 80 TC 0 Z9 0 U1 18 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1077-8306 EI 1744-7410 J9 INVERTEBR BIOL JI Invertebr. Biol. PD DEC PY 2016 VL 135 IS 4 BP 400 EP 414 DI 10.1111/ivb.12151 PG 15 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA ED1RM UT WOS:000388622600009 ER PT J AU Hoyos-Santillan, J Lomax, BH Large, D Turner, BL Boom, A Lopez, OR Sjogersten, S AF Hoyos-Santillan, Jorge Lomax, Barry H. Large, David Turner, Benjamin L. Boom, Arnoud Lopez, Omar R. Sjoegersten, Sofie TI Quality not quantity: Organic matter composition controls of CO2 and CH4 fluxes in neotropical peat profiles SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Neotropical peatland; Pyrolysis; Greenhouse gases; Methane; Carbon dioxide; Palm and mixed forest swamp ID TROPICAL PEATLANDS; CARBON LOSS; BOTANICAL COMPOSITION; OMBROTROPHIC PEAT; PLANT CUTICLES; PYROLYSIS; METHANE; DECOMPOSITION; VEGETATION; LITTER AB Tropical peatlands represent an important source of carbon dioxide (CO2) and methane (CH4) to the atmosphere. However, we do not know where in the peat profile these gases are produced and how controlling factors, such as substrate quality, which can vary substantially with peat age, and anoxic-oxic conditions, interact to determine production rates. To address this knowledge gap, this study investigated if substrate limitation of CO2 and CH4 production differs under anoxic-oxic peat conditions using entire peat profiles, from tropical peatlands in Panama. We determined the variation in peat organic chemistry through stratigraphic profiles using tetramethylammonium-pyrolysis-gas chromatography mass spectrometry (TMAH-Py-GC/IVIS). To explore how variation in peat organic chemistry through the depth profile impacted on CO2 and CH4 production rates under anoxic-oxic conditions we carried out a series of incubation experiments. The TMAH-Py-GC/MS analysis showed high concentrations of long chain fatty acids (>C-20) in surface peat, and variation in the distribution of the lignin monomers through the peat profile. Both anoxic CH4 and CO2 production was greatest from the surface of the peat profile with surface peat accounting for 92 1.7 and 54 2.9% of the cumulative CH4 and CO2 production, respectively. The high CO2 and CH4 production rate under anoxic conditions, in surface peat, was strongly related to greater concentrations of lignin, but also long chain fatty acids and polysaccharides, in this section of the peat profile. As expected, CH4 production decreased, and became decoupled from peat organic chemistry, following peat aeration. In contrast, aeration dramatically increased CO2 emissions throughout the entire peat profile. This demonstrates that the recalcitrance of buried peat does not protect C stocks in tropical peatlands, if their water tables are lowered in response to drainage or prolonged drought. In conclusion, our work highlight that information on both labile substrate availability and water table fluctuation are needed to predict CO2 and CH4 fluxes from tropical peatlands. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Hoyos-Santillan, Jorge; Lomax, Barry H.; Sjoegersten, Sofie] Univ Nottingham, Sch Biosci, Sci Sutton Bonington Campus, Loughborough LE12 5RD, Leics, England. [Large, David] Univ Nottingham, Dept Chem & Environm Engn, Nottingham NG7 2RD, England. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Boom, Arnoud] Univ Leicester, Dept Geog, Leicester LE1 7RH, Leics, England. [Lopez, Omar R.] Inst Invest Cient & Serv Alta Tecnol INDICASAT, Ctr Biodiversidad & Descubrimiento Drogas, Clayton, Panama. RP Hoyos-Santillan, J (reprint author), Univ Nottingham, Sch Biosci, Sci Sutton Bonington Campus, Loughborough LE12 5RD, Leics, England. EM jhoyosantillan@hotmail.com RI Turner, Benjamin/E-5940-2011; Lomax, Barry/B-1136-2010 OI Turner, Benjamin/0000-0002-6585-0722; Lomax, Barry/0000-0003-0475-7839 FU National Council on Science and Technology (CONACyT) [211962] FX Jorge Hoyos would like to thank The National Council on Science and Technology (CONACyT) for his PhD scholarship (211962). The authors would like to thank the Light Hawk program for its support in the aerial surveys. We thank Erick Brown for his invaluable help as field assistant. Thanks to Gabriel Jacome, Plinio Gondola, Tania Romero, Luis A. Ramos, Vanessa Pardo, Dianne del la Cruz, and Dayana Agudo from the STRI for their logistical support and laboratory assistance. NR 63 TC 0 Z9 0 U1 29 U2 29 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD DEC PY 2016 VL 103 BP 86 EP 96 DI 10.1016/j.soilbio.2016.08.017 PG 11 WC Soil Science SC Agriculture GA ED3VA UT WOS:000388775400009 ER PT J AU Benedetti-Rossi, G Sicardy, B Buie, MW Ortiz, JL Vieira-Martins, R Keller, JM Braga-Ribas, F Camargo, JIB Assafin, M Morales, N Duffard, R Dias-Oliveira, A Santos-Sanz, P Desmars, J Gomes, AR Leiva, R Bardecker, J Bean, JK Olsen, AM Ruby, DW Sumner, R Thirouin, A Gomez-Munoz, MA Gutierrez, L Wasserman, L Charbonneau, D Irwin, J Levine, S Skiff, B AF Benedetti-Rossi, G. Sicardy, B. Buie, M. W. Ortiz, J. L. Vieira-Martins, R. Keller, J. M. Braga-Ribas, F. Camargo, J. I. B. Assafin, M. Morales, N. Duffard, R. Dias-Oliveira, A. Santos-Sanz, P. Desmars, J. Gomes-Junior, A. R. Leiva, R. Bardecker, J. Bean, J. K., Jr. Olsen, A. M. Ruby, D. W. Sumner, R. Thirouin, A. Gomez-Munoz, M. A. Gutierrez, L. Wasserman, L. Charbonneau, D. Irwin, J. Levine, S. Skiff, B. TI RESULTS FROM THE 2014 NOVEMBER 15TH MULTI-CHORD STELLAR OCCULTATION BY THE TNO (229762) 2007 UK126 SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper belt objects: individual (229762, 2007 UK126); occultations; planets and satellites: fundamental parameters ID OBJECTS; SYSTEM; ALBEDO; RADIUS; PLANET; PLUTO AB We present results derived from the first multi-chord stellar occultation by the trans-Neptunian object (229762) 2007 UK126, observed on 2014 November 15. The event was observed by the Research and Education Collaborative Occultation Network project and International Occultation Timing Association collaborators throughout the United States. Use of two different data analysis methods obtain a satisfactory fit to seven chords, yielding an elliptical fit to the chords with an equatorial radius of = R 338(-10)(+15) km and equivalent radius of = Req 319(-7)(+14) km. A circular fit also gives a radius of = R 324(-23)(+30) km. Assuming that the object is a Maclaurin spheroid with indeterminate aspect angle, and using two published absolute magnitudes for the body, we derive possible ranges for geometric albedo between p(V) = 0.159(-0.013) (+ 0.007) and p(R) = 0.189(-0.015)(+0.009), and for the body oblateness between is an element of= 0.105 (-0.040) (+0.050) and is an element of= 0.118 (-0.048) (+0.055). For a nominal rotational period of 11.05 hr, an upper limit for density of rho = 1740 kg m(-3) is estimated for the body. C1 [Benedetti-Rossi, G.; Vieira-Martins, R.; Camargo, J. I. B.; Dias-Oliveira, A.] ON MCT&I, Rio De Janeiro, Brazil. [Sicardy, B.] Univ Paris Diderot, Univ Pierre & Marie Curie, CNRS UMR 8109, LESIA,Observ Paris, Meudon, France. [Buie, M. W.] Southwest Res Inst, Boulder, CO USA. [Ortiz, J. L.; Morales, N.; Duffard, R.; Santos-Sanz, P.] IAA CSIC, Apt 3004, E-18080 Granada, Spain. [Vieira-Martins, R.; Assafin, M.] OV UFRJ, Rio De Janeiro, Brazil. [Keller, J. M.] Calif Polytech State Univ San Luis Obispo, San Luis Obispo, CA 93407 USA. [Braga-Ribas, F.] Univ Tecnol Fed Parana, UTFPR DAFIS, Curitiba, PR, Brazil. [Camargo, J. I. B.] Lab Interinst & Astron LIneA, Rio De Janeiro, Brazil. [Desmars, J.] Univ Lille 1, Sorbonne Univ, PSL Res Univ, Observ Paris,IMCCE,CNRS,UPMC, F-75014 Paris, France. [Leiva, R.] Pontificia Univ Catlica Chile, Inst Astrofs, Fac Fsica, Santiago 7820436, Chile. [Bardecker, J.; Olsen, A. M.] IOTA, Iota, LA USA. [Bardecker, J.; Bean, J. K., Jr.; Ruby, D. W.; Sumner, R.] RECON, Reno, NV USA. [Ruby, D. W.] Univ Nevada, Reno, NV 89557 USA. [Thirouin, A.; Wasserman, L.; Levine, S.; Skiff, B.] Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. [Gomez-Munoz, M. A.; Gutierrez, L.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City, DF, Mexico. [Charbonneau, D.; Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Benedetti-Rossi, G (reprint author), ON MCT&I, Rio De Janeiro, Brazil. EM gustavorossi@on.br FU National Science Foundation; David and Lucile Packard Foundation Fellowship for Science and Engineering; John Templeton Foundation; NSF [AST-1212159, AST-1413287, AST-1413072]; RECON; European Research Council under the European Community's H (ERC) [669416]; Spanish grant [AYA-2014-56637-C2-1-P]; Proyecto de Excelencia de la Junta de Andaluca [2012-FQM1776]; CAPES [BEX 9110/12-7, E-26/200.464/2015]; CAPES/Brazil; FAPERJ [E-01/2015/209545, E-26/111.488/2013]; CNPq [308489/2013-6, 473002/2013-2, 308721/2011-0]; CONACYT [167236]; European Unions Horizon Research and Innovation Programme [687378]; DCT; National Science Foundation [AST-1005313]; [CNPq-306885/2013]; [CAPES/Cofecub-2506/2015]; [FAPERJ/PAPDRJ-45/2013]; [FAPERJ/CNE/05-2015] FX The RECON project would not be possible without all of the support from our community teams (teachers, students, and community members) and was funded by NSF grants AST-1212159, AST-1413287, and AST-1413072. Special thanks to Dean and Starizona for their support of RECON above and beyond the usual bounds of a commercial relationship.; Part of the research leading to these results has received funding from the European Research Council under the European Community's H2020 (2014-2020/ERC Grant Agreement n 669416 "LUCKY STAR").; Funding from Spanish grant AYA-2014-56637-C2-1-P is acknowledged, as is the Proyecto de Excelencia de la Junta de Andaluca, J. A. 2012-FQM1776. R.D. acknowledges the support of MINECO for his Ramon y Cajal Contract. FEDER funds are also acknowledged.; A.D.O. is thankful for the support of the CAPES (BEX 9110/12-7) FAPERJ/PAPDRJ (E-26/200.464/2015) grants.; G.B.R. is thankful for the support of CAPES/Brazil and FAPERJ (Grant E-01/2015/209545).; J.I.B.C. acknowledges CNPq for a PQ2 fellowship (process number 308489/2013-6).; L.G. thanks the support from CONACYT through grant 167236.; M.A. thanks the CNPq (Grants 473002/2013-2 and 308721/2011-0) and FAPERJ (Grant E-26/111.488/2013).; P.S.-S. acknowledges that part of the research leading to these results has received funding from the European Unions Horizon 2020 Research and Innovation Programme, under Grant Agreement no 687378.; R.V.M. acknowledges the following grants: CNPq-306885/2013, CAPES/Cofecub-2506/2015, FAPERJ/PAPDRJ-45/2013, FAPERJ/CNE/05-2015.; This research was partially based on data obtained at the Lowell Observatory's Discovery Channel Telescope (DCT). Lowell operates the DCT in partnership with Boston University, Northern Arizona University, the University of Maryland, and the University of Toledo. Partial support of the DCT was provided by Discovery Communications. LMI was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). A.T., S.L., and B.S. acknowledge Lowell Observatory funding.; The MEarth project acknowledges funding from the National Science Foundation, the David and Lucile Packard Foundation Fellowship for Science and Engineering, and the John Templeton Foundation. The opinions expressed here are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. NR 38 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD DEC PY 2016 VL 152 IS 6 AR 156 DI 10.3847/0004-6256/152/6/156 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC6PJ UT WOS:000388258100002 ER PT J AU Ballantine, DL Ruiz, H Lozada-Troche, C Norris, JN AF Ballantine, David L. Ruiz, Hector Lozada-Troche, Chad Norris, James N. TI The genus Ramicrusta (Peyssonneliales, Rhodophyta) in the Caribbean Sea, including Ramicrusta bonairensis sp nov and Ramicrusta monensis sp nov. SO BOTANICA MARINA LA English DT Article DE Caribbean; Peyssonneliaceae; Ramicrusta bonairensis; Ramicrusta monensis; Ramicrusta textilis ID RIBOSOMAL-RNA GENE; KILLING RED ALGA; PUERTO-RICO; METAPEYSSONNELIA-CORALLEPIDA; RHODYMENIALES RHODOPHYTA; RDNA SEQUENCES; GIGARTINALES; DNA; REPRESENTATIVES; MORPHOLOGY AB Two new species of Ramicrusta (Peyssonneliaceae, Rhodophyta), Ramicrusta bonairensis from Bonaire, The Netherlands Antilles and Puerto Rico and Ramicrusta monensis from Puerto Rico are described on the basis of both morphological and genetic criteria. Both grow closely appressed to their substrata, a characteristic that differs from their Caribbean congener, Ramicrusta textilis, which forms flared or broadly fluted, expanded erect tissue, and is not closely appressed throughout. The new species also share with each other, the character, seen in microscopic sections, of appearing layered due to an abrupt decrease in cell size that occurs in the perithallus. Ramicrusta bonairensis is thicker than R. monensis, forming crusts up to 840 mu m thick and carposporangia that measure up to 80 mu m in length. Ramicrusta monensis is less thick, 585-650 mu m, and produces smaller carposporangia, 40-50 mu m in length. Overgrowing thalli in R. monensis are commonly observed, frequently resulting in gaps visible in transverse microscopic sections. Irregular perithallial growth may also result in hollow regions. Male gametophytes are reported for the first time in R. textilis and in R. monensis. Mixed reproductive phases in individual thalli, with both male gametophytic structures and tetrasporangial nemathecia, are also observed in R. monensis. C1 [Ballantine, David L.; Ruiz, Hector; Lozada-Troche, Chad] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA. [Ballantine, David L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB166, Washington, DC 20560 USA. [Ruiz, Hector] POB 1126, Hormigueros, PR 00660 USA. [Lozada-Troche, Chad] Univ Puerto Rico, Dept Biol, POB 372230,Cayey Campus, Cayey, PR 00737 USA. [Norris, James N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB166, Washington, DC 20560 USA. RP Ballantine, DL (reprint author), Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA.; Ballantine, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB166, Washington, DC 20560 USA. EM ballantined@si.edu FU NSF grant SI-DSG [642079]; NOAA Caribbean Coral Reef Institute (CCRI), University of Puerto Rico FX We thank Ms. Caren E. Eckrich, CIEE (Council of International Education Exchange) Research Station, Bonaire, Caribbean Leeward Islands, The Netherlands, who alerted us to the Curacao Ramicrusta and provided specimens for molecular and morphological analyses. Dr. Godfried van Moorsel (Ecosub, The Netherlands) provided the in situ photographs of Ramicrusta bonairensis. This contribution was supported in part by the NOAA Caribbean Coral Reef Institute (CCRI), University of Puerto Rico. JN also thank for the partial support from NSF grant SI-DSG#642079. NR 43 TC 0 Z9 0 U1 2 U2 2 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0006-8055 EI 1437-4323 J9 BOT MAR JI Bot. Marina PD DEC PY 2016 VL 59 IS 6 BP 417 EP 431 DI 10.1515/bot-2016-0086 PG 15 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA ED1DO UT WOS:000388584400003 ER PT J AU Hambleton, K Kurtz, DW Prsa, A Quinn, SN Fuller, J Murphy, SJ Thompson, SE Latham, DW Shporer, A AF Hambleton, K. Kurtz, D. W. Prsa, A. Quinn, S. N. Fuller, J. Murphy, S. J. Thompson, S. E. Latham, D. W. Shporer, A. TI KIC 3749404: a heartbeat star with rapid apsidal advance indicative of a tertiary component SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: eclipsing; stars: individual: KIC 3749404; stars: oscillations ID ECCENTRIC BINARY-SYSTEMS; LIGHT CURVES; ECLIPSING BINARIES; STELLAR STRUCTURE; CLOSE BINARIES; MOTION TEST; ORBITAL SOLUTIONS; DYNAMIC TIDES; DELTA-SCUTI; SPACED DATA AB Heartbeat stars are eccentric (e > 0.2) ellipsoidal variables whose light curves resemble a cardiogram. We present the observations and corresponding model of KIC 3749404, a highly eccentric (e = 0.66), short period (P = 20.3 d) heartbeat star with tidally induced pulsations. A binary star model was created using PHOEBE, which we modified to include tidally induced pulsations and Doppler boosting. The morphology of the photometric periastron variation (heartbeat) depends strongly on the eccentricity, inclination and argument of periastron. We show that the inclusion of tidally induced pulsations in the model significantly changes the parameter values, specifically the inclination and those parameters dependent on it. Furthermore, we determine the rate of apsidal advance by modelling the periastron variation at the beginning and end of the 4-yr Kepler data set and dividing by the elapsed time. We compare the model with the theoretical expectations for classical and general relativistic apsidal motion and find the observed rate to be two orders of magnitude greater than the theoretical rate. We find that the observed rate cannot be explained by tidally induced pulsations alone and consequently hypothesize the presence of a third body in the system. C1 [Hambleton, K.] Villanova Univ, Dept Astron & Astrophys, 800 East Lancaster Ave, Villanova, PA 19085 USA. [Hambleton, K.; Kurtz, D. W.; Prsa, A.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Quinn, S. N.] Georgia State Univ, Dept Phys & Astron, 25 Pk Pl Suite 605, Atlanta, GA 30302 USA. [Fuller, J.] Walter Burke Inst Theoret Phys, TAPIR, Mailcode 350-17, Pasadena, CA USA. [Murphy, S. J.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Thompson, S. E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Thompson, S. E.] SETI Inst, 189 Bernardo Ave Suite 100, Mountain View, CA 94043 USA. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Shporer, A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Hambleton, K (reprint author), Villanova Univ, Dept Astron & Astrophys, 800 East Lancaster Ave, Villanova, PA 19085 USA.; Hambleton, K (reprint author), Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. EM kelly.hambleton@villanova.edu FU NASA's Science Mission Directorate; NSF [1517460]; STFC (Science and Technology Funding Council); NASA [11-KEPLER11-0056, 14-K2GO1_2-0057]; RAS; Kepler mission under NASA [NNX11AB99A]; NASA through the Sagan Fellowship Program FX The authors express their sincere thanks to NASA and the Kepler team for allowing them to work with and analyse the Kepler data making this work possible. The Kepler mission is funded by NASA's Science Mission Directorate. KH and AP acknowledge support from the NSF grant #1517460. This work was also supported by the STFC (Science and Technology Funding Council). The authors would like to thank Ed Guinan for the enlightening discussion on apsidal motion. KH, ST and JF acknowledge support through NASA K2 GO grant (11-KEPLER11-0056). We would like to thank the RAS for providing grants which enabled KH's attendance to conferences and thus enabled the development of collaborations and the successful completion of this work. AP acknowledges support through NASA K2 GO grant (NASA 14-K2GO1_2-0057). For the spectroscopic observations and results from TRES, DWL and SNQ acknowledge partial support from the Kepler mission under NASA Cooperative Agreement NNX11AB99A to the Smithsonian Astrophysical Observatory. This work was performed in part under contract with the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. NR 83 TC 3 Z9 3 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2016 VL 463 IS 2 BP 1199 EP 1212 DI 10.1093/mnras/stw1970 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC4RY UT WOS:000388122400007 ER PT J AU Schirmer, M Malhotra, S Levenson, NA Fu, H Davies, RL Keel, WC Torrey, P Bennert, VN Pancoast, A Turner, JEH AF Schirmer, Mischa Malhotra, Sangeeta Levenson, Nancy A. Fu, Hai Davies, Rebecca L. Keel, William C. Torrey, Paul Bennert, Vardha N. Pancoast, Anna Turner, James E. H. TI About AGN ionization echoes, thermal echoes and ionization deficits in low-redshift Ly alpha blobs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; galaxies: active; galaxies: evolution; ultraviolet: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; BLACK-HOLE ACCRETION; NARROW-LINE REGION; GREEN PEA GALAXIES; STELLAR POPULATION SYNTHESIS; FAR-ULTRAVIOLET OBSERVATIONS; SEYFERT 2 GALAXIES; BROAD-BAND SURVEY AB We report the discovery of 14 Ly alpha blobs (LABs) at z similar to 0.3, existing at least 4-7 billion years later in the Universe than all other LABs known. Their optical diameters are 20-70 kpc, and GALEX data imply Ly alpha luminosities of (0.4-6.3) x 10(43) erg s(-1). Contrary to high-z LABs, they live in low-density areas. They are ionized by AGN, suggesting that cold accretion streams as a power source must deplete between z = 2 and 0.3. We also show that transient AGN naturally explain the ionization deficits observed in many LABs. Their Ly alpha and X-ray fluxes decorrelate below less than or similar to 10(6) years because of the delayed escape of resonantly scattering Ly alpha photons. High Ly alpha luminosities do not require currently powerful AGN, independent of obscuration. Chandra X-ray data reveal intrinsically weak AGN, confirming the luminous optical nebulae as impressive ionization echoes. For the first time, we also report mid-infrared thermal echoes from the dusty tori. We conclude that the AGN have faded by three to four orders of magnitude within the last 10(4-5) years, leaving fossil UV, optical and thermal radiation behind. The host galaxies belong to the group of previously discovered Green Bean galaxies (GBs). Gemini optical imaging reveals smooth spheres, mergers, spectacular outflows and ionization cones. Because of their proximity and high flux densities, GBs are perfect targets to study AGN feedback, mode switching and the Ly alpha escape. The fully calibrated, co-added optical FITS images are publicly available. C1 [Schirmer, Mischa; Levenson, Nancy A.; Turner, James E. H.] Gemini Observ, Casilla 603, La Serena, Chile. [Malhotra, Sangeeta] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52245 USA. [Davies, Rebecca L.] Australian Natl Univ, Res Sch Astron & Astrophys, Cotter Rd, Weston, ACT 2611, Australia. [Keel, William C.] Univ Alabama, Dept Phys & Astron, Box 870324, Tuscaloosa, AL 35487 USA. [Torrey, Paul; Pancoast, Anna] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Bennert, Vardha N.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 93407 USA. RP Schirmer, M (reprint author), Gemini Observ, Casilla 603, La Serena, Chile. EM mschirme@gemini.edu FU National Aeronautics and Space Administration through Chandra Award [G04-15110X]; National Aeronautics Space Administration [NAS8-03060]; National Science Foundation (NSF) Research at Undergraduate Institutions (RUI) [AST-1312296]; NASA FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G04-15110X (PI: M. Schirmer) issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. VNB gratefully acknowledges assistance from a National Science Foundation (NSF) Research at Undergraduate Institutions (RUI) grant AST-1312296. Note that findings and conclusions do not necessarily represent views of the NSF.; The scientific results reported in this paper are based in part on observations made by the Chandra X-ray Observatory, and on data obtained from the Chandra Data Archive. The authors also made use of the software provided by the Chandra X-ray Center (CXC) in the application packages CIAO.; Based on observations made with the NASA Galaxy Evolution Explorer. GALEX is a NASA Small Explorer launched in 2003 April. The authors gratefully acknowledge NASA's support for the construction, operation and science analysis for the GALEX mission, developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Education. Based on data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 172 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2016 VL 463 IS 2 BP 1554 EP 1586 DI 10.1093/mnras/stw1819 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC4RY UT WOS:000388122400034 ER PT J AU Bernard, EJ Ferguson, AMN Schlafly, EF Martin, NF Rix, HW Bell, EF Finkbeiner, DP Goldman, B Martinez-Delgado, D Sesar, B Wyse, RFG Burgett, WS Chambers, KC Draper, PW Hodapp, KW Kaiser, N Kudritzki, RP Magnier, EA Metcalfe, N Wainscoat, RJ Waters, C AF Bernard, Edouard J. Ferguson, Annette M. N. Schlafly, Edward F. Martin, Nicolas F. Rix, Hans-Walter Bell, Eric F. Finkbeiner, Douglas P. Goldman, Bertrand Martinez-Delgado, David Sesar, Branimir Wyse, Rosemary F. G. Burgett, William S. Chambers, Kenneth C. Draper, Peter W. Hodapp, Klaus W. Kaiser, Nicholas Kudritzki, Rolf-Peter Magnier, Eugene A. Metcalfe, Nigel Wainscoat, Richard J. Waters, Christopher TI A synoptic map of halo substructures from the Pan-STARRS1 3 pi survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; Hertzsprung-Russell and colour-magnitude diagrams; Galaxy: halo-Galaxy: structure ID DIGITAL SKY SURVEY; MILKY-WAY HALO; TRIANGULUM-ANDROMEDA REGION; GLOBULAR-CLUSTER PALOMAR-5; SURVEY COMMISSIONING DATA; DWARF SPHEROIDAL GALAXY; STELLAR TIDAL STREAMS; SATELLITE SEGUE 1; DARK-MATTER HALO; DEBRIS STREAM AB We present a panoramic map of the entire MilkyWay halo north of delta similar to -30 degrees (similar to 30 000 deg(2)), constructed by applying the matched-filter technique to the Pan-STARRS1 3 pi Survey data set. Using single-epoch photometry reaching to g similar to 22, we are sensitive to stellar substructures with heliocentric distances between 3.5 and similar to 35 kpc. We recover almost all previously reported streams in this volume and demonstrate that several of these are significantly more extended than earlier data sets have indicated. In addition, we also report five new candidate stellar streams. One of these features appears significantly broader and more luminous than the others and is likely the remnant of a dwarf galaxy. The other four streams are consistent with a globular cluster origin, and three of these are rather short in projection (less than or similar to 10 degrees), suggesting that streams like Ophiuchus may not be that rare. Finally, a significant number of more marginal substructures are also revealed by our analysis; many of these features can also be discerned in matched-filter maps produced by other authors from SDSS data, and hence they are very likely to be genuine. However, the extant 3 pi data is currently too shallow to determine their properties or produce convincing colour-magnitude diagrams. The global view of the Milky Way provided by Pan-STARRS1 provides further evidence for the important role of both globular cluster disruption and dwarf galaxy accretion in building the Milky Way's stellar halo. C1 [Bernard, Edouard J.] Univ Cote dAzur, CNRS, OCA, Lagrange, France. [Bernard, Edouard J.; Ferguson, Annette M. N.; Wyse, Rosemary F. G.] Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Schlafly, Edward F.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Martin, Nicolas F.] Univ Strasbourg, CNRS, UMR 7550, Observ Astron Strasbourg, 11 Rue Univ, F-67000 Strasbourg, France. [Martin, Nicolas F.; Rix, Hans-Walter; Goldman, Bertrand; Sesar, Branimir] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Bell, Eric F.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. [Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Martinez-Delgado, David] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Wyse, Rosemary F. G.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. [Burgett, William S.] GMTO Corp, 465 N Halstead St,Suite 250, Pasadena, CA 91107 USA. [Chambers, Kenneth C.; Hodapp, Klaus W.; Kaiser, Nicholas; Kudritzki, Rolf-Peter; Magnier, Eugene A.; Wainscoat, Richard J.; Waters, Christopher] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Draper, Peter W.; Metcalfe, Nigel] Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. RP Bernard, EJ (reprint author), Univ Cote dAzur, CNRS, OCA, Lagrange, France.; Bernard, EJ (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM ebernard@oca.eu FU STFC; CNES; DFG [SFB 881]; Leverhulme Trust; National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877] FX The authors are grateful to Ana Bonaca for granting permission to use part of her maps in this publication, and to Jorge Penarrubia and the anonymous referee for useful comments. EJB acknowledges support from a consolidated grant from STFC and from the CNES postdoctoral fellowship program. HWR acknowledges support from the DFG grant SFB 881 (A3). RFGW acknowledges support through a Visiting Professorship from the Leverhulme Trust, held at the University of Edinburgh. This research work has made use of the Python packages Numpy4 (Walt, Colbert & Varoquaux 2011), Astropy5 (Astropy Collaboration et al. 2013), Matplotlib6 (Hunter 2007), and Pandas7 (McKinney 2010); the IAC-STAR Synthetic CMD computation code, which is supported and maintained by the computer division of the Instituto de Astrofisica de Canarias; and the NASA/IPAC Extragalactic Database which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; The PS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, and the University of Maryland. NR 86 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2016 VL 463 IS 2 BP 1759 EP 1768 DI 10.1093/mnras/stw2134 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC4RY UT WOS:000388122400049 ER PT J AU Burningham, B Hardcastle, M Nichols, JD Casewell, SL Littlefair, SP Stark, C Burleigh, MR Metchev, S Tannock, ME van Weeren, RJ Williams, WL Wynn, GA AF Burningham, Ben Hardcastle, M. Nichols, J. D. Casewell, S. L. Littlefair, S. P. Stark, C. Burleigh, M. R. Metchev, S. Tannock, M. E. van Weeren, R. J. Williams, W. L. Wynn, G. A. TI A LOFAR mini-survey for low-frequency radio emission from the nearest brown dwarfs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; brown dwarfs; stars: low-mass ID IONOSPHERE COUPLING CURRENTS; JUPITERS MIDDLE MAGNETOSPHERE; ELECTRON-CYCLOTRON MASER; MAIN AURORAL OVAL; H-ALPHA EMISSION; ULTRACOOL DWARFS; T-DWARFS; PEDERSEN CONDUCTIVITY; PROPER MOTIONS; GIANT PLANETS AB We have conducted a mini-survey for low-frequency radio emission from some of the closest brown dwarfs to the Sun with rapid rotation rates: SIMP J013656.5+093347, WISEPC J150649.97+702736.0 and WISEPA J174124.26+255319.5. We have placed robust 3 sigma upper limits on the flux density in the 111-169 MHz frequency range for these targets: WISE 1506: < 0.72 mJy; WISE 1741: < 0.87 mJy; SIMP 0136: < 0.66 mJy. At 8 h of integration per target to achieve these limits, we find that systematic and detailed study of this class of object at LOFAR frequencies will require a substantial dedication of resources. C1 [Burningham, Ben] NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA. [Burningham, Ben; Hardcastle, M.; Williams, W. L.] Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Nichols, J. D.; Casewell, S. L.; Burleigh, M. R.; Wynn, G. A.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Littlefair, S. P.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Stark, C.] Abertay Univ, Div Comp & Math, Kydd Bldg, Dundee DD1 1HG, Scotland. [Metchev, S.; Tannock, M. E.] Univ Western Ontario, Dept Phys & Astron, Ctr Planetary Sci & Explorat, London, ON N6A 3K7, Canada. [Metchev, S.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Burningham, B (reprint author), NASA, Ames Res Ctr, Mail Stop 245-3, Moffett Field, CA 94035 USA.; Burningham, B (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM b.burningham@herts.ac.uk RI Stark, Craig /A-7667-2016; Nichols, Jonathan/F-5764-2010; OI Nichols, Jonathan/0000-0002-8004-6409; Hardcastle, Martin/0000-0003-4223-1117 FU European Commission in the form of a Marie Curie International Outgoing Fellowship [PIOF-GA-2013- 629435]; UK's Science and Technology Facilities Council [ST/M001008/1, ST/M001350/1]; College of Science and Engineering at the University of Leicester FX BB acknowledges financial support from the European Commission in the form of a Marie Curie International Outgoing Fellowship (PIOF-GA-2013- 629435). MJH and WLW acknowledge support from the UK's Science and Technology Facilities Council [grant number ST/M001008/1]. SLC is supported by the College of Science and Engineering at the University of Leicester. SPL acknowledges support from the UK's Science and Technology Facilities Council [grant number ST/M001350/1]. NR 60 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2016 VL 463 IS 2 BP 2202 EP 2209 DI 10.1093/mnras/stw2065 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC4RY UT WOS:000388122400083 ER PT J AU Scaringi, S Manara, CF Barenfeld, SA Groot, PJ Isella, A Kenworthy, MA Knigge, C Maccarone, TJ Ricci, L Ansdell, M AF Scaringi, S. Manara, C. F. Barenfeld, S. A. Groot, P. J. Isella, A. Kenworthy, M. A. Knigge, C. Maccarone, T. J. Ricci, L. Ansdell, M. TI The peculiar dipping events in the disc-bearing young-stellar object EPIC 204278916 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE comets: general; planets and satellites: dynamical evolution and stability; stars: early-type; stars: individual: (EPIC 204278916); stars: peculiar ID SCORPIUS OB ASSOCIATION; MAIN-SEQUENCE STARS; LOW-MASS STARS; T-TAURI STARS; NGC 2264; AA TAURI; ACCRETION; VARIABILITY; POPULATION; EVOLUTION AB EPIC 204278916 has been serendipitously discovered from its K2 light curve that displays irregular dimmings of up to 65 per cent for approximate to 25 consecutive days out of 78.8 d of observations. For the remaining duration of the observations, the variability is highly periodic and attributed to stellar rotation. The star is a young, low-mass (M-type) pre-main-sequence star with clear evidence of a resolved tilted disc from Atacama Large Millimeter/submillimeter Array (ALMA) observations. We examine the K2 light curve in detail and hypothesize that the irregular dimmings are caused by either a warped inner disc edge or transiting cometary-like objects in either circular or eccentric orbits. The explanations discussed here are particularly relevant for other recently discovered young objects with similar absorption dips. C1 [Scaringi, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Manara, C. F.] European Space Res & Technol Ctr ESA ESTEC, Directorate Sci, Sci Support Off, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Barenfeld, S. A.] CALTECH, Dept Astron, MC 249-17, Pasadena, CA 91125 USA. [Groot, P. J.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Isella, A.] Rice Univ, Dept Phys & Astron, 6100 Main St, Houston, TX 77005 USA. [Kenworthy, M. A.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Knigge, C.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Maccarone, T. J.] Texas Tech Univ, Dept Phys & Astron, Lubbock, TX 79409 USA. [Ricci, L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ansdell, M.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. RP Scaringi, S (reprint author), Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. EM simo@mpe.mpg.de OI Groot, Paul/0000-0002-4488-726X FU Alexander von Humboldt Foundation; ESA; NASA Science Mission Directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; National Science Foundation [DGE-1144469] FX We gratefully thank the anonymous referee for providing useful and insightful comments which have improved this manuscript. SS acknowledges funding from the Alexander von Humboldt Foundation. CFM acknowledges ESA research fellowship funding. This research has made use of NASA's Astrophysics Data System Bibliographic Services. Additionally, this work acknowledges the use of the astronomy and astrophysics package for MATLAB (Ofek 2014). This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission Directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper additionally makes use of the following ALMA data: ADS/JAO. ALMA#2013.1.00395. S. ALMA is a partnership of European Southern Observatory (ESO, representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. NR 37 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2016 VL 463 IS 2 BP 2265 EP 2272 DI 10.1093/mnras/stw2155 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC4RY UT WOS:000388122400087 ER PT J AU De Leon, LF Lopez, OR AF Fernando De Leon, Luis Lopez, Omar R. TI Biodiversity beyond trees: Panama's Canal provides limited conservation lessons for Nicaragua SO BIODIVERSITY AND CONSERVATION LA English DT Editorial Material DE Biodiversity; Conservation; Environmental benefits; Nicaragua Canal; Panama Canal AB Megaprojects pose a major global environmental challenge. For instance, the forthcoming construction of the Nicaraguan Canal has generated controversy regarding its social and environmental consequences. To some, it will represent an unparalleled environmental catastrophe; to others, it will lead to net environmental and social benefits. In both cases, the Panama Canal emerges as an analogy to inform the environmental and social fate of Nicaragua. In our view, this comparison is incomplete and does not accurately represent the social and environmental realities of the two countries, and therefore, it might be of limited use for predicting the future of Nicaragua. Our analysis-based on evidence from the literature-revealed three emerging themes. First, our current understanding of the long-term environmental consequences of the two Canals in Central America is rather limited, even after 100 years of experience in Panama. Second, the historical, environmental and political differences between the two countries make the Panama Canal a poor predictor for the environmental and social fate of Nicaragua. Finally, previous assessments of the consequences of both megaprojects might be biased by a focus on forest conservation alone. This suggests that the apparent environmental and social benefits provided by such megaprojects might be more marginal than expected. This calls for a deeper analysis of costs and benefits of the construction and management of the two Canals in the Central American region, and their impacts on the natural world. These uncertainties might be a common consequence of many large-scale megaprojects around the world. C1 [Fernando De Leon, Luis; Lopez, Omar R.] Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Ctr Biodiversidad & Descubrimiento Drogas, POB 0843-01103, Panama City, Panama. [Fernando De Leon, Luis] Univ Massachusetts, Dept Biol, 100 Morrissey Blvd, Boston, MA 02125 USA. [Lopez, Omar R.] Smithsonian Trop Res Inst, POB 0843-03092, Panama City, Panama. RP De Leon, LF (reprint author), Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Ctr Biodiversidad & Descubrimiento Drogas, POB 0843-01103, Panama City, Panama.; De Leon, LF (reprint author), Univ Massachusetts, Dept Biol, 100 Morrissey Blvd, Boston, MA 02125 USA. EM luis.deleonreyna@gmail.com NR 13 TC 0 Z9 0 U1 9 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 EI 1572-9710 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD DEC PY 2016 VL 25 IS 13 BP 2821 EP 2825 DI 10.1007/s10531-016-1197-4 PG 5 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EB6FC UT WOS:000387475900015 ER PT J AU Arendt, D Musser, JM Baker, CVH Bergman, A Cepko, C Erwin, DH Pavlicev, M Schlosser, G Widder, S Laubichler, MD Wagner, GP AF Arendt, Detlev Musser, Jacob M. Baker, Clare V. H. Bergman, Aviv Cepko, Connie Erwin, Douglas H. Pavlicev, Mihaela Schlosser, Gerhard Widder, Stefanie Laubichler, Manfred D. Wagner, Gunter P. TI The origin and evolution of cell types SO NATURE REVIEWS GENETICS LA English DT Review ID REGULATES DENDRITIC SPINE; GENE-EXPRESSION; TRANSCRIPTION FACTORS; CONE PHOTORECEPTORS; HUMAN ENDOMETRIUM; NERVOUS-SYSTEM; N-CADHERIN; C-ELEGANS; PROTEIN COMPLEXES; STROMAL CELLS AB Cell types are the basic building blocks of multicellular organisms and are extensively diversified in animals. Despite recent advances in characterizing cell types, classification schemes remain ambiguous. We propose an evolutionary definition of a cell type that allows cell types to be delineated and compared within and between species. Key to cell type identity are evolutionary changes in the 'core regulatory complex' (CoRC) of transcription factors, that make emergent sister cell types distinct, enable their independent evolution and regulate cell type-specific traits termed apomeres. We discuss the distinction between developmental and evolutionary lineages, and present a roadmap for future research. C1 [Arendt, Detlev; Musser, Jacob M.] European Mol Biol Lab, Dev Biol Unit, Meyerhofstr 1, D-69012 Heidelberg, Germany. [Arendt, Detlev] Heidelberg Univ, Ctr Organismal Studies, Neuenheimer Feld 230, D-69120 Heidelberg, Germany. [Baker, Clare V. H.] Univ Cambridge, Dept Physiol Dev & Neurosci, Anat Bldg,Downing St, Cambridge CB2 3DY, England. [Bergman, Aviv] Albert Einstein Coll Med, Dominick P Purpura Dept Neurosci, Dept Syst & Computat Biol, 1301 Morris Pk Ave, Bronx, NY 10461 USA. [Bergman, Aviv] Albert Einstein Coll Med, Dept Pathol, 1301 Morris Pk Ave, Bronx, NY 10461 USA. [Bergman, Aviv; Erwin, Douglas H.; Laubichler, Manfred D.] Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. [Cepko, Connie] Harvard Med Sch, Howard Hughes Med Inst, Dept Genet, Boston, MA 02115 USA. [Cepko, Connie] Harvard Med Sch, Howard Hughes Med Inst, Dept Ophthalmol, Boston, MA 02115 USA. [Erwin, Douglas H.] Smithsonian Inst, Dept Paleobiol, MRC 121, POB 37012, Washington, DC 20013 USA. [Pavlicev, Mihaela] Cincinnati Childrens Hosp Med Ctr, Perinatal Inst, Cincinnati, OH 45229 USA. [Schlosser, Gerhard] Sch Nat Sci, Biomed Sci Bldg,Newcastle Rd, Galway, Ireland. [Schlosser, Gerhard] Regenerat Med Inst REMEDI, Biomed Sci Bldg,Newcastle Rd, Galway, Ireland. [Widder, Stefanie] Univ Vienna, Dept Microbial Ecol & Ecosyst Sci, CUBE, Althanstr 14, A-1090 Vienna, Austria. [Laubichler, Manfred D.] Arizona State Univ, Sch Life Sci, POB 4501, Tempe, AZ 85287 USA. [Laubichler, Manfred D.] Marine Biol Lab, 7 MBL St, Woods Hole, MA 02543 USA. [Wagner, Gunter P.] Yale Univ, Yale Syst Biol Inst, New Haven, CT 06511 USA. [Wagner, Gunter P.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06511 USA. [Wagner, Gunter P.] Yale Univ, Sch Med, Dept Obstet Gynecol & Reprod Sci, 333 Cedar St, New Haven, CT 06510 USA. [Wagner, Gunter P.] Wayne State Univ, Dept Obstet & Gynecol, Detroit, MI 48201 USA. RP Arendt, D (reprint author), European Mol Biol Lab, Dev Biol Unit, Meyerhofstr 1, D-69012 Heidelberg, Germany.; Arendt, D (reprint author), Heidelberg Univ, Ctr Organismal Studies, Neuenheimer Feld 230, D-69120 Heidelberg, Germany.; Laubichler, MD (reprint author), Santa Fe Inst, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA.; Laubichler, MD (reprint author), Arizona State Univ, Sch Life Sci, POB 4501, Tempe, AZ 85287 USA.; Laubichler, MD (reprint author), Marine Biol Lab, 7 MBL St, Woods Hole, MA 02543 USA.; Wagner, GP (reprint author), Yale Univ, Yale Syst Biol Inst, New Haven, CT 06511 USA.; Wagner, GP (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06511 USA.; Wagner, GP (reprint author), Yale Univ, Sch Med, Dept Obstet Gynecol & Reprod Sci, 333 Cedar St, New Haven, CT 06510 USA.; Wagner, GP (reprint author), Wayne State Univ, Dept Obstet & Gynecol, Detroit, MI 48201 USA. EM arendt@embl.de; manfred.laubichler@asu.edu; gunter.wagner@yale.edu RI Widder, Stefanie/B-9584-2014 FU Arizona State University (ASU)-SFI Center for Biosocial Complex Systems; European Research Council [294810 Brain Evo-Devo]; John Templeton Foundation [54860] FX This paper resulted from discussions of a working group at the Santa Fe Institute (SFI), New Mexico, USA, sponsored by the Arizona State University (ASU)-SFI Center for Biosocial Complex Systems. The authors are grateful for their support. Research on neuron type evolution in the Arendt laboratory is financially supported by a European Research Council Advanced grant (294810 Brain Evo-Devo). Research on cell type origination in the Wagner laboratory is financially supported by a grant from the John Templeton Foundation (grant no. 54860). The opinions expressed in this article are not those of the John Templeton Foundation. NR 170 TC 1 Z9 1 U1 27 U2 27 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1471-0056 EI 1471-0064 J9 NAT REV GENET JI Nat. Rev. Genet. PD DEC PY 2016 VL 17 IS 12 BP 744 EP 757 DI 10.1038/nrg.2016.127 PG 14 WC Genetics & Heredity SC Genetics & Heredity GA EC0KP UT WOS:000387789800009 PM 27818507 ER PT J AU Holmes, R Hayes, J Matthaei, C Closs, G Williams, M Goodwin, E AF Holmes, R. Hayes, J. Matthaei, C. Closs, G. Williams, M. Goodwin, E. TI Riparian management affects instream habitat condition in a dairy stream catchment SO NEW ZEALAND JOURNAL OF MARINE AND FRESHWATER RESEARCH LA English DT Article DE Dairy; GIS; fine sediment; fish habitat; riparian management; stock exclusion ID NEW-ZEALAND; WATER-QUALITY; LAND-USE; BROWN TROUT; AGRICULTURAL STREAMS; FISH COMMUNITIES; LOWLAND STREAM; FINE SEDIMENT; EELS ANGUILLA; SALMO-TRUTTA AB Using a space-for-time substitution design, we investigated the response of structural instream habitat and fish populations to different riparian management practices throughout a Dairy Best Practice Catchment. We found a significant negative correlation between the upstream area of stock exclusion fencing and deposited instream fine sediment cover. Furthermore, we determined that this relationship emerges when 300m lengths of upstream riparian area were included in the analysis, indicating the scale at which stock exclusion fencing results in a positive instream habitat response. Specifically, for this historically degraded spring-fed stream, our findings indicate that riparian segments with 5 m wide stock exclusion fences (both banks) are required to achieve instream fine sediment cover below 20% in downstream reaches. Fish were sparse and evenly spread throughout the catchment. Fish distributions were not correlated with reach-scale riparian or instream habitat variables, possibly because the available habitat quality gradient was too narrow. C1 [Holmes, R.; Hayes, J.; Goodwin, E.] Cawthron Inst, Nelson, New Zealand. [Matthaei, C.; Closs, G.] Univ Otago, Dept Zool, Dunedin, New Zealand. [Williams, M.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RP Holmes, R (reprint author), Cawthron Inst, Nelson, New Zealand. EM robin.holmes@cawthron.org.nz FU New Zealand Ministry for Business, Innovation and Employment (MBIE) [C01X1002]; DairyNZ; Cawthron Institute: Internal Investment Fund FX This research was funded by the New Zealand Ministry for Business, Innovation and Employment (MBIE) (Grant number: Maintenance and Rehabilitation of Aquatic Ecosystems Programme C01X1002), DairyNZ and the Cawthron Institute: Internal Investment Fund. NR 71 TC 0 Z9 0 U1 2 U2 2 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0028-8330 EI 1175-8805 J9 NEW ZEAL J MAR FRESH JI N. Z. J. Mar. Freshw. Res. PD DEC PY 2016 VL 50 IS 4 BP 581 EP 599 DI 10.1080/00288330.2016.1184169 PG 19 WC Fisheries; Marine & Freshwater Biology; Oceanography SC Fisheries; Marine & Freshwater Biology; Oceanography GA EA7TO UT WOS:000386835400007 ER PT J AU Duncan, FE Zelinski, M Gunn, AH Pahnke, JE O'Neill, CL Songsasen, N Woodruff, RI Woodruff, TK AF Duncan, Francesca E. Zelinski, Mary Gunn, Alexander H. Pahnke, Jennifer E. O'Neill, Conor L. Songsasen, Nucharin Woodruff, Ryan I. Woodruff, Teresa K. TI Ovarian tissue transport to expand access to fertility preservation: from animals to clinical practice SO REPRODUCTION LA English DT Review ID IN-VITRO MATURATION; FEMALE CANCER SURVIVORS; DOMESTIC CAT OOCYTES; PRIMORDIAL FOLLICLES; DEVELOPMENTAL COMPETENCE; LIVE BIRTH; CRYOPRESERVATION; TRANSPLANTATION; TEMPERATURE; CORTEX AB Primordial follicles dictate a female's reproductive life span and therefore are central to fertility preservation for both endangered species and individuals with fertility-threatening conditions. Ovarian tissue containing primordial follicles can be cryopreserved and later thawed and transplanted back into individuals to restore both endocrine function and fertility. Importantly, increasing numbers of human live births have been reported following ovarian tissue cryopreservation and transplantation. A current limitation of this technology is patient access to sites that are approved or equipped to process and cryopreserve ovarian tissue - especially in larger countries or low resource settings. Here, we review empirical evidence from both animal models and human studies that suggest that ovarian tissue can be transported at cold temperatures for several hours while still maintaining the integrity and reproductive potential of the primordial follicles within the tissue. In fact, several human live births have been reported in European countries using tissue that was transported at cold temperatures for up to 20 h before cryopreservation and transplantation. Ovarian tissue transport, if implemented widely in clinical practice, could therefore expand both patient and provider access to emerging fertility preservation options. C1 [Duncan, Francesca E.; Gunn, Alexander H.; Pahnke, Jennifer E.; O'Neill, Conor L.; Woodruff, Ryan I.; Woodruff, Teresa K.] Northwestern Univ, Feinberg Sch Med, Dept Obstet & Gynecol, Chicago, IL 60611 USA. [Zelinski, Mary] Oregon Natl Primate Res Ctr, Beaverton, OR USA. [Songsasen, Nucharin] Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Woodruff, TK (reprint author), Northwestern Univ, Feinberg Sch Med, Dept Obstet & Gynecol, Chicago, IL 60611 USA. EM tkw@northwestern.edu FU Thomas J Watkins Endowment (TKW, Northwestern University, Chicago, IL, USA); Center for Reproductive Health After Disease from the National Institutes of Health National Center for Translational Research in Reproduction and Infertility (NCTRI) [P50HD076188] FX This work was funded through the Thomas J Watkins Endowment (TKW, Northwestern University, Chicago, IL, USA) and by the Center for Reproductive Health After Disease (P50HD076188) from the National Institutes of Health National Center for Translational Research in Reproduction and Infertility (NCTRI). NR 77 TC 0 Z9 0 U1 2 U2 2 PU BIOSCIENTIFICA LTD PI BRISTOL PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT, ENGLAND SN 1470-1626 J9 REPRODUCTION JI Reproduction PD DEC PY 2016 VL 152 IS 6 BP R201 EP R210 DI 10.1530/REP-15-0598 PG 10 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA EC0ES UT WOS:000387771600002 PM 27492079 ER PT J AU Griffiths, SM Fox, G Briggs, PJ Donaldson, IJ Hood, S Richardson, P Leaver, GW Truelove, NK Preziosi, RF AF Griffiths, Sarah M. Fox, Graeme Briggs, Peter J. Donaldson, Ian J. Hood, Simon Richardson, Pen Leaver, George W. Truelove, Nathan K. Preziosi, Richard F. TI A Galaxy-based bioinformatics pipeline for optimised, streamlined microsatellite development from Illumina next-generation sequencing data SO CONSERVATION GENETICS RESOURCES LA English DT Article DE Microsatellite isolation; Pal_finder; PANDAseq; Trimmomatic; Pal_filter; Seq-SSR; SSRs; Galaxy; Next-generation sequencing; Illumina ID MARKERS AB Microsatellites are useful tools for ecologists and conservationist biologists, but are taxa-specific and traditionally expensive and time-consuming to develop. New methods using next-generation sequencing (NGS) have reduced these problems, but the plethora of software available for processing NGS data may cause confusion and difficulty for researchers new to the field of bioinformatics. We developed a bioinformatics pipeline for microsatellite development from Illumina paired-end sequences, which is packaged in the open-source bioinformatics tool Galaxy. This optimises and streamlines the design of a microsatellite panel and provides a user-friendly graphical user interface. The pipeline utilises existing programs along with our own novel program and wrappers to: quality-filter and trim reads (Trimmomatic); generate sequence quality reports (FastQC); identify potentially-amplifiable microsatellite loci (Pal_finder); design primers (Primer3); assemble pairs of reads to enhance marker amplification success rates (PANDAseq); and filter optimal loci (Pal_filter). The complete pipeline is freely available for use via a pre-configured Galaxy instance, accessible at https://palfinder.ls.manchester.ac.uk. C1 [Griffiths, Sarah M.; Fox, Graeme; Preziosi, Richard F.] Univ Manchester, Fac Life Sci, Manchester M13 9PT, Lancs, England. [Briggs, Peter J.; Donaldson, Ian J.] Univ Manchester, Bioinformat Core Facil, Fac Life Sci, Manchester M13 9PT, Lancs, England. [Hood, Simon; Richardson, Pen; Leaver, George W.] Univ Manchester, Res Infrastruct Team, Res Comp, Manchester M13 9PL, Lancs, England. [Truelove, Nathan K.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Griffiths, SM (reprint author), Univ Manchester, Fac Life Sci, Manchester M13 9PT, Lancs, England. EM griffiths.sarahm@gmail.com OI Griffiths, Sarah/0000-0003-4743-049X FU Faculty of Life Sciences, University of Manchester; Natural Environment Research Council (NERC) FX This work was funded by the Faculty of Life Sciences, University of Manchester, and a studentship awarded to SMG from the Natural Environment Research Council (NERC). We are grateful to the Genomic Technologies Core Facility and the DNA Sequencing Facility at the University of Manchester for their services and advice in this project. Thanks to Ezemvelo KwaZulu Natal Wildlife and C. Weldon for the use of the A. hymenopus tissue sample (permit OP526/2014). Thanks also to J-D Hibbitt and Sea Life for providing the R. undulata sample, and M. Butler IV and D. Behringer for samples used in the initial development of this tool. NR 22 TC 0 Z9 0 U1 4 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1877-7252 EI 1877-7260 J9 CONSERV GENET RESOUR JI Conserv. Genet. Resour. PD DEC PY 2016 VL 8 IS 4 BP 481 EP 486 DI 10.1007/s12686-016-0570-7 PG 6 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA EB6HN UT WOS:000387482700027 ER PT J AU Lloyd, MW Widmeyer, PA Neel, MC AF Lloyd, Michael W. Widmeyer, Paul A. Neel, Maile C. TI Temporal variability in potential connectivity of Vallisneria americana in the Chesapeake Bay SO LANDSCAPE ECOLOGY LA English DT Article DE Graph theory; Submersed aquatic vegetation; Fragmentation ID SUBMERSED AQUATIC VEGETATION; LONG-DISTANCE DISPERSAL; LANDSCAPE CONNECTIVITY; WATER-QUALITY; HABITAT LOSS; WILD CELERY; VASCULAR PLANTS; FRAGMENTED LANDSCAPES; POPULATION-DYNAMICS; DEPTH DISTRIBUTION AB Submersed aquatic vegetation (SAV) performs water quality enhancing functions that are critical to the overall health of estuaries such as the Chesapeake Bay. However, eutrophication and sedimentation have decimated the Bay's SAV population to a fraction of its historical coverage. Understanding the spatial distribution of and connectedness among patches is important for assessing the dynamics and health of the remaining SAV population. We seek to explore the distribution of SAV patches and patterns of potential connectivity in the Chesapeake Bay through time. We assess critical distances, from complete patch isolation to connection of all patches, in a merged composite coverage map that represents the sum of all probable Vallisneria americana containing patches between 1984 and 2010 and in coverage maps for individual years within that timeframe for which complete survey data are available. We have three key findings: First, the amount of SAV coverage in any given year is much smaller than the total recently occupied acreage. Second, the vast majority of patches of SAV that are within the tolerances of V. americana are ephemeral, being observed in only 1 or 2 years out of 26 years. Third, this high patch turnover results in highly variable connectivity from year to year, dependent on dispersal distance and patch arrangement. Most of the connectivity thresholds are beyond reasonable dispersal distances for V. americana. If the high turnover in habitat occupancy is due to marginal water quality, relatively small improvements could greatly increase V. americana growth and persistence. C1 [Lloyd, Michael W.; Widmeyer, Paul A.; Neel, Maile C.] Univ Maryland, Dept Plant Sci & Landscape Architecture, 2102 Plant Sci Bldg, College Pk, MD 20742 USA. [Lloyd, Michael W.] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Widmeyer, Paul A.; Neel, Maile C.] Univ Maryland, Dept Entomol, 2102 Plant Sci Bldg, College Pk, MD 20742 USA. RP Lloyd, MW (reprint author), Univ Maryland, Dept Plant Sci & Landscape Architecture, 2102 Plant Sci Bldg, College Pk, MD 20742 USA.; Lloyd, MW (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. EM lloydm@si.edu RI Lloyd, Michael/C-8430-2017 OI Lloyd, Michael/0000-0003-1021-8129 NR 87 TC 0 Z9 0 U1 14 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 EI 1572-9761 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD DEC PY 2016 VL 31 IS 10 BP 2307 EP 2321 DI 10.1007/s10980-016-0401-y PG 15 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA EB4GS UT WOS:000387329100008 ER PT J AU Collins, LS Geary, DH Grossman, EL AF Collins, Laurel S. Geary, Dana H. Grossman, Ethan L. TI Variability of foraminiferal stable isotope ratios in Caribbean shallow waters of Panama: A modern framework for Neogene studies SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Foraminifera; Panama; Neritic; Paleoceanography; Analysis of Variance ID BOCAS-DEL-TORO; SEA BENTHIC FORAMINIFERA; SPINOSE PLANKTONIC FORAMINIFER; SAN-FRANCISCO BAY; ORBULINA-UNIVERSA; CIBICIDOIDES-WUELLERSTORFI; UVIGERINA-PEREGRINA; CONTINENTAL-MARGIN; LABORATORY CULTURE; AMERICAN SEAWAY AB Oxygen and carbon isotope analyses of the foraminifera Orbulina universa (planktic), Uvigerina peregrina (benthic) and Cibicides pachyderma (benthic) in 45 bottom samples from the archipelago of Bocas del Toro, Caribbean Panama, are used to address the reliability of stable isotope values in distinguishing differences among neritic surface water and middle neritic to upper bathyal depths. The significance of variation in isotope values within stations, between stations within depth-defined groups, and between depths was determined with Analysis of Variance. Isotope values differ significantly among stations with few exceptions; thus, within-station error is minimal. delta O-18 values of O. universa across the open shelf are the same. Oxygen isotope ratios of U. peregrina discriminate outer shelf to upper slope depths well. delta O-18 values of C. pachyderma from the inner middle shelf, outer middle shelf, and inner outer shelf are significantly different, and mean values from 33 m to 240 m are strongly correlated with water depth. Cibicides pachyderma from two stations shows strong delta O-18 evidence of downslope transport of 80 and 160 m, corroborated by foraminiferal assemblages. delta C-13 can only differentiate middle shelf and outermost outer shelf to upper slope depths. Oxygen isotope values of O. universa and U. peregrina generally agree with predicted temperatures, and those of C. pachyderma are consistently low. Comparisons of delta O-18 values of benthic and planktic foraminifera, and neritic and deep-sea planktic foraminifera, enable qualitative and even quantitative estimates of paleodepth and paleosalinity, enabling their use in Neogene studies of sedimentary rocks within the region. (C) 2016 Elsevier B.V. All rights reserved. C1 [Collins, Laurel S.] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. [Collins, Laurel S.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Collins, Laurel S.] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama. [Geary, Dana H.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Grossman, Ethan L.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA. RP Collins, LS (reprint author), Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA.; Collins, LS (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA.; Collins, LS (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama. EM collinsl@fiu.edu FU STRI; National Science Foundation [EAR-9304654, EAR-1325683] FX We are grateful to the Smithsonian Tropical Research Institute (STRI), Panama, for shiptime on the R/V Benjamin and Captain David West's positioning skills. We thank K. C Lohmann's Stable Isotope Laboratory, University of Michigan, for the analyses. Shen Mei, Brian Bodenbender, Diane Ritchey and Erin Wilson prepared foraminiferal samples. Lora Wingate ran isotopic analyses, and Bonnie Miljour prepared the map. Comments by William Anderson, Enriqueta Barrera, Martin Buzas, Lee-Ann Hayek, G. P. Lohmann, Christina Ravelo and Divya Saxena greatly improved the paper's quality. This research was supported by a STRI postdoctoral fellowship to Collins and National Science Foundation grants EAR-9304654 and EAR-1325683. NR 75 TC 0 Z9 0 U1 12 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC 1 PY 2016 VL 463 BP 1 EP 10 DI 10.1016/j.palaeo.2016.09.004 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA EB6WJ UT WOS:000387526000001 ER PT J AU Liutkus-Pierce, CM Zimmer, BW Carmichael, SK McIntosh, W Deino, A Hewitt, SM McGinnis, KJ Hartney, T Brett, J Mana, S Deocampo, D Richmond, BG Hatala, K Harcourt-Smith, W Pobiner, B Metallo, A Rossi, V AF Liutkus-Pierce, C. M. Zimmer, B. W. Carmichael, S. K. McIntosh, W. Deino, A. Hewitt, S. M. McGinnis, K. J. Hartney, T. Brett, J. Mana, S. Deocampo, D. Richmond, B. G. Hatala, K. Harcourt-Smith, W. Pobiner, B. Metallo, A. Rossi, V. TI Radioisotopic age, formation, and preservation of Late Pleistocene human footprints at Engare Sero, Tanzania SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Engare Sero; Hominin; Footprints; Lake Natron; Pleistocene ID OLDOINYO-LENGAI; LAETOLI FOOTPRINTS; NORTHERN TANZANIA; RIFT-VALLEY; KENYA; ETHIOPIA; HOMINID; BIOMECHANICS; MORPHOLOGY; SUBSTRATE AB We report on the radioisotopic age, formation, and preservation of a late Pleistocene human footprint site in northern Tanzania on the southern shore of Lake Natron near the village of Engare Sero. Over 400 human footprints, as well as tracks of zebra and bovid, are preserved in a series of volcaniclastic deposits. Based on field mapping along with geochemical and grain-size analyses, we propose that these deposits originated as proximal volcanic material from the nearby active volcano, Oldoinyo L'engai, and were then fluvially transported to the footprint site. Stable isotope results (delta O-18 and delta C-13) suggest that the footprints were originally emplaced on a mudflat saturated by a freshwater spring and were later inundated by the rising alkaline waters of Lake Natron. We employed the Ar-40/Ar-39 and C-14 dating methods to investigate the age of the site and determined that the footprint level is older than 5760 +/- 30 yrs. BP and younger than 19.1 +/- 3.1 ka. These radioisotopic ages are supported by stratigraphic correlations with previously documented debris avalanche deposits and the stable isotope signatures associated with the most recent highstand of Lake Natron, further constraining the age to latest Pleistocene. Since modern humans (Homo sapiens) were present in Africa ca. 200 ka, Engare Sero represents the most abundant and best-preserved footprint site of anatomically modern Homo sapiens currently known in Africa. Fossil footprints are a snapshot in time, recording behavior at a specific moment in history; but the actual duration of time captured by the snapshot is often not well defined. Through analog experiments, we constrain the depositional window in which the prints were made, buried, and ultimately preserved to within a few hours to days or months. (C) 2016 Elsevier B.V. All rights reserved. C1 [Liutkus-Pierce, C. M.; Zimmer, B. W.; Carmichael, S. K.; Hewitt, S. M.; McGinnis, K. J.; Hartney, T.] Appalachian State Univ, Dept Geol, POB 32067, Boone, NC 28608 USA. [McIntosh, W.] New Mexico Inst Min & Technol, Geochronol Res Lab, Socorro, NM 87801 USA. [Deino, A.] Berkeley Geochronol Ctr, Berkeley, CA 94709 USA. [Brett, J.] Penn Inst Conservat Educ, Elysburg, PA 17824 USA. [Mana, S.] Salem State Univ, Dept Geol Sci, Salem, MA 01970 USA. [Deocampo, D.] Georgia State Univ, Dept Geosci, Atlanta, GA 30303 USA. [Richmond, B. G.] Amer Museum Nat Hist, Dept Anthropol, New York, NY 10024 USA. [Hatala, K.] Max Planck Inst Evolutionary Anthropol, D-04103 Leipzig, Germany. [Harcourt-Smith, W.] CUNY, Dept Anthropol, New York, NY 10016 USA. [Pobiner, B.] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Metallo, A.; Rossi, V.] Smithsonian Inst, Digitizat Program Off, Washington, DC 20560 USA. RP Liutkus-Pierce, CM (reprint author), Appalachian State Univ, Dept Geol, POB 32067, Boone, NC 28608 USA. EM liuticuscm@appstate.edu FU National Geographic Society's Committee for Research and Exploration [8748-10]; National Science Foundation (NSF) [BCS-1128170]; Leakey Foundation [71483-0001]; Appalachian State University (University Research Council); Appalachian State University (Office of International Education and Development); Appalachian State University (Office of Student Research); George Washington University; Evolving Earth Foundation; Smithsonian Institution's Human Origins Program; Pennsylvania Institute for Conservation Education; NSF [EAR-1322017] FX The research presented here was funded by the National Geographic Society's Committee for Research and Exploration (8748-10), the National Science Foundation (NSF BCS-1128170), the Leakey Foundation (71483-0001), Appalachian State University (the University Research Council, the Office of International Education and Development, and the Office of Student Research), the George Washington University, the Evolving Earth Foundation, the Smithsonian Institution's Human Origins Program, and the Pennsylvania Institute for Conservation Education. We sincerely thank the Tanzanian Commission on Science and Technology, the Department of Antiquities and their representatives (Donatius Kamamba, Felix Ndunguru, Godfrey Olle Moita, Christowaja Ntandu, and Neema Mbwana), and the Ministry of Natural Resources and Tourism (Permanent Secretary Dr. Ladislaus Komba) for their continued assistance and permission to conduct research at Engare Sero since 2009 (COSTECH permit #2011-89-ER-2009-75). Kongo Sakkae, of the Engare Sero Village, is credited with discovering this site prior to 2006, while Julian von Mutius and Gerald Gwau were instrumental in bringing this site to the attention of the scientific community. Tim Leach and the staff of the Lake Natron Tented Camp are warmly thanked for their commitment to this project as well as their accommodation, as are Ndashy Munuo and the residents of the Engare Sero Village. Good Earth Tours and Global Rescue provided field support. NSF Grant EAR-1322017 supported dating efforts at the BGC. The authors would also like to thank the following individuals for their assistance: Dr. Jorg Keller, Dr. James D. Wright, Dr. Craig Feibel, Dr. Henning Scholz, Dr. Bert Van Bocxlaer, Dr. Kate Scharer, Dr. Scott Marshall, Steven Davis, Katie Wolf, Dr. Nelia Dunbar, Dr. Richard Abbott, Anthony Love, Dr. Johnny Waters, Barbara Waters, Carol Liutkus, and Dr. Michael Manyak. This paper has been significantly improved through the efforts of two anonymous reviewers. NR 65 TC 1 Z9 1 U1 4 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD DEC 1 PY 2016 VL 463 BP 68 EP 82 DI 10.1016/j.palaeo.2016.09.019 PG 15 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA EB6WJ UT WOS:000387526000006 ER PT J AU Cornelius, ML Dieckhoff, C Hoelmer, KA Olsen, RT Weber, DC Herlihy, MV Talamas, EJ Vinyard, BT Greenstone, MH AF Cornelius, Mary L. Dieckhoff, Christine Hoelmer, Kim A. Olsen, Richard T. Weber, Donald C. Herlihy, Megan V. Talamas, Elijah J. Vinyard, Bryan T. Greenstone, Matthew H. TI Biological control of sentinel egg masses of the exotic invasive stink bug Halyomorpha halys (Stal) in Mid-Atlantic USA ornamental landscapes SO BIOLOGICAL CONTROL LA English DT Article DE Natural enemies; Urban landscape; Egg parasitoid; Biological invasion ID TRISSOLCUS BASALIS INSECTA; MICHIGAN NATIVE PLANTS; HEMIPTERA-PENTATOMIDAE; HETEROPTERA-PENTATOMIDAE; HYMENOPTERA SCELIONIDAE; NATURAL ENEMIES; NORTH-AMERICA; PATCH DEFENSE; ABUNDANCE; PARASITOIDS AB Biological invasions have far reaching effects on native plant and arthropod communities. This study evaluated the effect of natural enemies on eggs of the exotic invasive brown marmorated stink bug Halyomorpha halys (Stal) in experimental plots comprising species pairs of 16 ornamental trees and shrub genera from either Eurasia or North America and in wooded areas adjacent to the plots. Sentinel egg masses were placed on leaves of Acer, Cercis, Hydrangea, and Prunus in the plots and in seven genera of trees and shrubs in adjacent woods. Overall, rates of parasitism and predation in experimental plots were low, accounting for only 3.8% and 4.4% of egg mortality, respectively. There were no significant differences in parasitism and predation rates between native or exotic plots or between plants of different genera. In 2015, predation was significantly higher in the experimental plots than in the wooded sites, but parasitism was significantly higher in the wooded sites. In the experimental plots, seven native and one exotic parasitoid species attacked sentinel egg masses. Six native parasitoid species attacked sentinel egg masses in the wooded sites. Parasitoids in the genus Trissolcus were more likely to attack egg masses in exotic plots than in native plots. There is no evidence that native natural enemies attacking eggs of the exotic BMSB were more prevalent in landscapes with native ornamental trees and shrubs than those with exotic trees and shrubs. Published by Elsevier Inc. C1 [Cornelius, Mary L.; Weber, Donald C.; Herlihy, Megan V.; Greenstone, Matthew H.] USDA ARS, Invas Insect Biocontrol & Behav Lab, Beltsville Agr Res Ctr, 10300 Baltimore Ave, Beltsville, MD 20705 USA. [Dieckhoff, Christine; Hoelmer, Kim A.] USDA ARS, Beneficial Insects Intro Res Lab, 501 South Chapel St, Newark, DE 19713 USA. [Olsen, Richard T.] USDA ARS, US USNA, 3501 New York Ave NE, Washington, DC 20002 USA. [Talamas, Elijah J.] USDA ARS, Systemat Entomol Lab, Natl Museum Nat Hist, Smithsonian Inst, 10th & Constitut Ave NW,MRC 168, Washington, DC 20560 USA. [Vinyard, Bryan T.] USDA ARS, Stat Grp, Northeast Area Off, 10300 Baltimore Ave, Beltsville, MD 20705 USA. RP Cornelius, ML (reprint author), USDA ARS, Invas Insect Biocontrol & Behav Lab, Beltsville Agr Res Ctr, 10300 Baltimore Ave, Beltsville, MD 20705 USA. EM mary.cornelius@ars.usda.gov FU U.S. Department of Agriculture - National Institute of Food and Agriculture - Specialty Crop Research Initiative (USDA-NIFA-SCRI) [2011-51181-30937] FX We are indebted to Colien Hefferan and Margaret Pooler for institutional support; Scott Aker and Christopher Carley for advice on horticultural protocols; Anthony Vlhakis, Tanya Zastrow; Emily Hren, Jing Hu, and Michael Fizdale for assistance with plot maintenance; Ruby Rivera-Cruz and Rosario Vidales for field assistance during the 2014 season; and The University of Puerto Rico, Florida International University, and Friends of Agricultural Research Beltsville, for enabling the participation of Mss Rivera-Cruz and Vidales. We also thank Charley Williams for designing plots that closely simulate urban landscapes, David Kidwell-Slak for additional assistance in the field, and Jason Mottern, USDA ARS BARC Systematic Entomology Laboratory, for identification of Ooencyrtus. This work was partially supported by the U.S. Department of Agriculture - National Institute of Food and Agriculture - Specialty Crop Research Initiative (USDA-NIFA-SCRI) #2011-51181-30937. NR 48 TC 3 Z9 3 U1 30 U2 30 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1049-9644 EI 1090-2112 J9 BIOL CONTROL JI Biol. Control PD DEC PY 2016 VL 103 BP 11 EP 20 DI 10.1016/j.biocontrol.2016.07.011 PG 10 WC Biotechnology & Applied Microbiology; Entomology SC Biotechnology & Applied Microbiology; Entomology GA EA2ZZ UT WOS:000386468300002 ER PT J AU Tanaka, Y Fordyce, RE AF Tanaka, Y. Fordyce, R. E. TI Papahu-like fossil dolphin from Kaikoura, New Zealand, helps to fill the Early Miocene gap in the history of Odontoceti SO NEW ZEALAND JOURNAL OF GEOLOGY AND GEOPHYSICS LA English DT Article DE Cetacea; systematics; phylogeny; fossil; Miocene; Pacific; New Zealand ID PHYLOGENETIC-RELATIONSHIPS; INTEGRATED STRATIGRAPHY; MIDDLE MIOCENE; WHALE CETACEA; MAMMALIA; DELPHINOIDEA; JAPAN; PHOCOENIDAE; BELGIUM; SKULL AB An early Miocene dolphin (ZMT73: partial skull and ear bones) from Kaikoura, New Zealand, is the sister taxon to the previously named Early Miocene Papahu taitapu. The new specimen, although insufficient to justify a new species name, includes an informative squamosal and periotic that help move the Papahu clade from the stem Odontoceti to either the Platanistoidea, or to become the sister taxon to the Ziphiidae+Eurhinodelphinidae+Delphinida. The fossils usefully add to the taxonomic and structural diversity of Cetacea during the important but poorly known Early Miocene. C1 [Tanaka, Y.; Fordyce, R. E.] Univ Otago, Dept Geol, Dunedin, New Zealand. [Tanaka, Y.] Numata Fossil Museum, Numata, Hokkaido, Japan. [Tanaka, Y.] Hokkaido Univ Museum, Div Acad Resources & Specimens, Sapporo, Hokkaido, Japan. [Fordyce, R. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Fordyce, R. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Tanaka, Y (reprint author), Univ Otago, Dept Geol, Dunedin, New Zealand.; Tanaka, Y (reprint author), Numata Fossil Museum, Numata, Hokkaido, Japan.; Tanaka, Y (reprint author), Hokkaido Univ Museum, Div Acad Resources & Specimens, Sapporo, Hokkaido, Japan. EM yoshihiro.tanaka@otago.ac.nz FU New Zealand University Grants Committee PhD Scholarship FX RE Fordyce's initial studies of ZMT 73 in the later 1970s were supported by a New Zealand University Grants Committee PhD Scholarship. NR 56 TC 0 Z9 0 U1 5 U2 5 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0028-8306 EI 1175-8791 J9 NEW ZEAL J GEOL GEOP JI N. Z. J. Geol. Geophys. PD DEC PY 2016 VL 59 IS 4 BP 551 EP 567 DI 10.1080/00288306.2016.1211540 PG 17 WC Geology; Geosciences, Multidisciplinary SC Geology GA EB0LW UT WOS:000387036300006 ER PT J AU Tipkantha, W Thuwanut, P Morrell, J Comizzoli, P Chatdarong, K AF Tipkantha, W. Thuwanut, P. Morrell, J. Comizzoli, P. Chatdarong, K. TI Influence of living status (single vs. paired) and centrifugation with colloids on the sperm morphology and functionality in the clouded leopard (Neofelis nebulosa) SO THERIOGENOLOGY LA English DT Article DE Clouded leopard; Teratospermia; Sperm selection; Single-layer centrifugation ID TERATOSPERMIC DOMESTIC CATS; CHEETAH ACINONYX-JUBATUS; FREE HAMSTER OVA; STALLION SPERMATOZOA; LAYER CENTRIFUGATION; ACROSOME REACTION; DENSITY GRADIENT; SILICA COLLOIDS; FELIS-CATUS; SWIM-UP AB The objectives of the present study were to evaluate sperm characteristic of captive clouded leopards in Thailand and examine the structural and functional properties of sperm after selection with the single-layer centrifugation (SLC) method. Twenty-two ejaculates from 11 captive clouded leopards (four housed with access to a female in estrus, and seven housed singly) were collected and assessed for semen traits during 2013 to 2015. Twelve fresh ejaculates were chosen from seven males, and each was divided between two sperm preparation methods; (1) simple washing and (2) SLC. Cryopreservation was performed after semen preparation. Sperm qualities after selections including motility, progressive motility, sperm motility index, viability, acrosome integrity, DNA integrity, and morphology were evaluated in fresh, chilled, and frozen thawed samples. In addition, sperm functionality after cryopreservation was tested by heterologous IVF using domestic cat oocytes. Sperm motility in the ejaculates was 52.5% to 91.3% (76.8 +/- 2.0%, mean standard error). A high proportion of morphologically abnormal sperm (63.9 +/- 2.0%) was observed, with the major abnormality being tightly coiled tail (13.5 +/- 0.5%). An interesting observation was that males housed together with a female had a significantly higher proportion of sperm with intact acrosome (47.9 +/- 3.4% and 38.4 +/- 2.8%) and lower proportion of sperm with bent midpiece and droplet (7.1 +/- 0.6% and 102 +/- 0.5%) than the males living singly. The sperm motility index, intact acrosome, and sperm with normal tail in the fresh and chilled semen samples were improved by the SLC. In the postthawed semen, the SLC selected higher numbers of viable sperm (34.1 +/- 2.2% and 27.9 +/- 1.8%), sperm with intact acrosome (31.2 +/- 2.1% and 243 +/- 22%), and sperm with normal tail (342 +/- 2.7% and 24.3 +/- 2.7%) than simple washing. Also, the proportion of sperm with tightly coiled tail was lower in the SLC-processed than the simple washed samples (8.1 +/- 3.1% and 135 +/- 3.4%). The SLC-processed group had significantly higher penetration rate in heterologous IVF (29.4 +/- 3.0%) than the simple washing group (15.8 +/- 3.2%). In conclusion, ejaculates of clouded leopards living in Thailand demonstrated teratospermic characteristic similar to the previous reports from other continents. Single -layer centrifugation is a promising tool to select morphologically normal sperm of teratospermic donors. The successes of assisted reproductive technology could be enhanced by the improved quality of postthaw sperm in this species. (C) 2016 Elsevier Inc. All rights reserved. C1 [Tipkantha, W.; Thuwanut, P.; Chatdarong, K.] Chulalongkorn Univ, Dept Obstet Gynaecol & Reprod, Fac Vet Sci, Bangkok, Thailand. [Tipkantha, W.] Zool Pk Org, Bur Conservat & Res, Bangkok, Thailand. [Morrell, J.] Swedish Univ Agr Sci SLU, Dept Clin Sci, Uppsala, Sweden. [Comizzoli, P.] Natl Zoo, Smithsonian Conservat Biol Inst, Washington, DC USA. RP Chatdarong, K (reprint author), Chulalongkorn Univ, Dept Obstet Gynaecol & Reprod, Fac Vet Sci, Bangkok, Thailand. EM kaywalee.c@chula.ac.th OI Chatdarong, Kaywalee/0000-0002-9470-8426 FU Royal Golden Jubilee PhD Program [PHD/0100/2555]; Veterinary Research Fund [RG8/2556]; 90th Anniversary of Chulalongkorn University Fund (Ratchadaphiseksomphot Endowment Fund) FX The Royal Golden Jubilee PhD Program (grant number PHD/0100/2555) supported the PhD stipendium of W. Tipkantha. The research project was granted by Veterinary Research Fund (RG8/2556), the 90th Anniversary of Chulalongkorn University Fund (Ratchadaphiseksomphot Endowment Fund), and Research Unit of Obstetrics and Reproduction in Animals, Department of Obstetrics, Gynecology and Reproduction, Faculty of Veterinary Science, Chulalongkorn University and The Zoological Park Organization. The authors thank the Clouded Leopard Corsortium of Thailand staffs, Khao Kheow Open Zoo and Dusit Zoo staffs, Bureau of Conservation and Research staffs for their great supports on animal handling. NR 44 TC 0 Z9 0 U1 5 U2 5 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X EI 1879-3231 J9 THERIOGENOLOGY JI Theriogenology PD DEC PY 2016 VL 86 IS 9 BP 2202 EP 2209 DI 10.1016/j.theriogenology.2016.07.020 PG 8 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA EA3XC UT WOS:000386541600013 PM 27568458 ER PT J AU Deutsch, JI AF Deutsch, James I. TI Sabato Rodia's Towers in Watts: Art, Migrations, Development SO WESTERN FOLKLORE LA English DT Book Review C1 [Deutsch, James I.] Smithsonian Inst, Washington, DC 20560 USA. RP Deutsch, JI (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU CALIFORNIA FOLKLORE SOC PI POMONA PA WESTERN FOLKLORE DEPT OF ENGL/FOREIGN LANGUAGES 3801 W.TEMPLE AVENUE, POMONA, CA 91768-4010 USA SN 0043-373X J9 WESTERN FOLKLORE JI West. Folk. PD WIN PY 2016 VL 75 IS 1 BP 109 EP 111 PG 3 WC Folklore SC Arts & Humanities - Other Topics GA DZ8FB UT WOS:000386105200005 ER PT J AU Johnson, CB Schall, M Tennison, ME Garcia, ME Shea-Shumsky, NB Raghanti, MA Lewandowski, AH Bertelsen, MF Waller, LC Walsh, T Roberts, JF Hof, PR Sherwood, CC Manger, PR Jacobs, B AF Johnson, Cameron B. Schall, Matthew Tennison, Mackenzie E. Garcia, Madeleine E. Shea-Shumsky, Noah B. Raghanti, Mary Ann Lewandowski, Albert H. Bertelsen, Mads F. Waller, Leona C. Walsh, Timothy Roberts, John F. Hof, Patrick R. Sherwood, Chet C. Manger, Paul R. Jacobs, Bob TI Neocortical Neuronal Morphology in the Siberian Tiger (Panthera tigris altaica) and the Clouded Leopard (Neofelis nebulosa) SO JOURNAL OF COMPARATIVE NEUROLOGY LA English DT Article DE dendrite; morphometry; Golgi method; brain evolution; neocortex ID CAT VISUAL-CORTEX; PRIMARY AUDITORY-CORTEX; INVERTED PYRAMIDAL NEURONS; PRIMARY MOTOR CORTEX; CEREBRAL-CORTEX; PREFRONTAL CORTEX; PROJECTION NEURONS; POSTCRUCIATE GYRUS; HUMAN-BRAIN; BETZ CELLS AB Despite extensive investigations of the neocortex in the domestic cat, little is known about neuronal morphology in larger felids. To this end, the present study characterized and quantified the somatodendritic morphology of neocortical neurons in prefrontal, motor, and visual cortices of the Siberian tiger (Panthera tigris altaica) and clouded leopard (Neofelis nebulosa). After neurons were stained with a modified Golgi technique (N = 194), dendritic branching and spine distributions were analyzed using computer-assisted morphometry. Qualitatively, aspiny and spiny neurons in both species appeared morphologically similar to those observed in the domestic cat. Although the morphology of spiny neurons was diverse, with the presence of extraverted, inverted, horizontal, and multiapical pyramidal neurons, the most common variant was the typical pyramidal neuron. Gigantopyramidal neurons in the motor cortex were extremely large, confirming the observation of Brodmann ([1909] Vergleichende Lokalisationlehre der Grosshirnrinde in ihren Prinzipien dargestellt auf Grund des Zellenbaues. Leipzig, Germany: J.A. Barth), who found large somata for these neurons in carnivores in general, and felids in particular. Quantitatively, a MARSplines analysis of dendritic measures differentiated typical pyramidal neurons between the Siberian tiger and the clouded leopard with 93% accuracy. In general, the dendrites of typical pyramidal neurons were more complex in the tiger than in the leopards. Moreover, dendritic measures in tiger pyramidal neurons were disproportionally large relative to body/brain size insofar as they were nearly as extensive as those observed in much larger mammals (e.g., African elephant). Comparison of neuronal morphology in a more diverse collection of larger felids may elucidate the comparative context for the relatively large size of the pyramidal neurons observed in the present study. (C) 2016 Wiley Periodicals, Inc. C1 [Johnson, Cameron B.; Schall, Matthew; Tennison, Mackenzie E.; Garcia, Madeleine E.; Shea-Shumsky, Noah B.; Waller, Leona C.; Jacobs, Bob] Colorado Coll, Neurosci Program, Lab Quantitat Neuromorphol, 14 E Cache La Poudre, Colorado Springs, CO 80903 USA. [Raghanti, Mary Ann] Kent State Univ, Dept Anthropol, Kent, OH 44242 USA. [Raghanti, Mary Ann] Kent State Univ, Sch Biomed Sci, Kent, OH 44242 USA. [Lewandowski, Albert H.] Cleveland Metropk Zoo, Cleveland, OH 44109 USA. [Bertelsen, Mads F.] Copenhagen Zoo, Ctr Zoo & Wild Anim Hlth, DK-2000 Frederiksberg, Denmark. [Walsh, Timothy] Smithsonian Natl Zool Pk, Washington, DC 20008 USA. [Roberts, John F.] Alabama Dept Agr & Ind, Thompson Bishop Sparks State Diagnost Lab, Auburn, AL 36849 USA. [Hof, Patrick R.] Icahn Sch Med Mt Sinai, Fishberg Dept Neurosci, New York, NY 10029 USA. [Hof, Patrick R.] Icahn Sch Med Mt Sinai, Friedman Brain Inst, New York, NY 10029 USA. [Sherwood, Chet C.] George Washington Univ, Dept Anthropol, Washington, DC 20052 USA. [Manger, Paul R.] Univ Witwatersrand, Fac Hlth Sci, Sch Anat Sci, ZA-2000 Johannesburg, South Africa. RP Jacobs, B (reprint author), Colorado Coll, Neurosci Program, Lab Quantitat Neuromorphol, 14 E Cache La Poudre, Colorado Springs, CO 80903 USA. EM BJacobs@ColoradoCollege.edu OI Bertelsen, Mads/0000-0001-9201-7499 FU James S. McDonnell Foundation [22002078, 220020293]; South African National Research Foundation FX Grant sponsor: The James S. McDonnell Foundation; Grant numbers: 22002078 (to P.R.H. and C.C.S.) and 220020293 (to C.C.S.); Grant sponsor: South African National Research Foundation (to P.R.M.). NR 141 TC 0 Z9 0 U1 9 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-9967 EI 1096-9861 J9 J COMP NEUROL JI J. Comp. Neurol. PD DEC 1 PY 2016 VL 524 IS 17 BP 3641 EP 3665 DI 10.1002/cne.24022 PG 25 WC Neurosciences; Zoology SC Neurosciences & Neurology; Zoology GA DZ4BU UT WOS:000385803400009 PM 27098982 ER PT J AU Zhao, L Li, X Zhang, N Zhang, SD Yi, TS Ma, H Guo, ZH Li, DZ AF Zhao, Lei Li, Xia Zhang, Ning Zhang, Shu-Dong Yi, Ting-Shuang Ma, Hong Guo, Zhen-Hua Li, De-Zhu TI Phylogenomic analyses of large-scale nuclear genes provide new insights into the evolutionary relationships within the rosids SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Coalescence; Rosids phylogenomics; Nuclear genes; Gene tree; Species tree ID SPECIES-TREE ESTIMATION; MULTISPECIES COALESCENT MODEL; ANGIOSPERM PHYLOGENY; MISSING DATA; MAXIMUM-LIKELIHOOD; DATA SETS; LAND PLANTS; EARLY DIVERSIFICATION; NUCLEOTIDE-SEQUENCES; ANCIENT DIVERGENCES AB The Rosids is one of the largest groups of flowering plants, with 140 families and 70,000 species. Previous phylogenetic studies of the rosids have primarily utilized organelle genes that likely differ in evolutionary histories from nuclear genes. To better understand the evolutionary history of rosids, it is necessary to investigate their phylogenetic relationships using nuclear genes. Here, we employed large-scale phylogenomic datasets composed of nuclear genes, including 891 clusters of putative orthologous genes. Combined with comprehensive taxon sampling covering 63 species representing 14 out of the 17 orders, we reconstructed the rosids phylogeny with coalescence and concatenation methods, yielding similar tree topologies from all datasets. However, these topologies did not agree on the placement of Zygophyllales. Through comprehensive analyses, we found that missing data and gene tree heterogeneity were potential factors that may mislead concatenation methods, in particular, large amounts of missing data under high gene tree heterogeneity. Our results provided new insights into the deep phylogenetic relationships of the rosids, and demonstrated that coalescence methods may effectively resolve the phylogenetic relationships of the rosids with missing data under high gene tree heterogeneity. (C) 2016 Elsevier Inc. All rights reserved. C1 [Zhao, Lei; Li, Xia; Zhang, Shu-Dong; Yi, Ting-Shuang; Guo, Zhen-Hua; Li, De-Zhu] Chinese Acad Sci, Kunming Inst Bot, Plant Germplasm & Genom Ctr, Germplasm Bank Wild Species, Kunming 650201, Yunnan, Peoples R China. [Zhao, Lei] Univ Chinese Acad Sci, Kunming Coll Life Sci, Kunming 650201, Yunnan, Peoples R China. [Zhang, Ning] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. [Ma, Hong] Fudan Univ, Minist Educ, Key Lab Biodivers Sci & Ecol Engn,Sch Life Sci, Inst Plant Biol,Inst Biodivers Sci,Ctr Evolutiona, Shanghai 200032, Peoples R China. RP Guo, ZH; Li, DZ (reprint author), Chinese Acad Sci, Kunming Inst Bot, 132 Lanhei Rd, Kunming 650201, Yunnan, Peoples R China. EM guozhenhua@mail.kib.ac.cn; dzl@mail.kib.ac.cn FU National Key Basic Research Program [2014CB954100]; Kunming Institute of Botany, Chinese Academy of Sciences [2014KIB02] FX We thank Peng-Fei Ma, Yu-Xiao Zhang, Jun He, Guo-Qian Yang, and Hui-Fu Zhuang of Kunming Institute of Botany, Chinese Academy of Sciences for help and computational supports. We are grateful to Bo-Jian Zhong of Nanjing Normal University for his suggestions. This study is funded by the National Key Basic Research Program (No. 2014CB954100) and Kunming Institute of Botany, Chinese Academy of Sciences (No. 2014KIB02). NR 133 TC 0 Z9 0 U1 43 U2 43 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD DEC PY 2016 VL 105 BP 166 EP 176 DI 10.1016/j.ympev.2016.06.007 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA DY3BB UT WOS:000384964700014 PM 27369455 ER PT J AU Grant, JA Parker, TJ Crumpler, LS Wilson, SA Golombek, MP Mittlefehldt, DW AF Grant, J. A. Parker, T. J. Crumpler, L. S. Wilson, S. A. Golombek, M. P. Mittlefehldt, D. W. TI The degradational history of Endeavour crater, Mars SO ICARUS LA English DT Article DE Mars; Mars, surface; Cratering; Impact processes; Geological processes ID MARTIAN IMPACT CRATERS; PLANUM LANDING SITE; MERIDIANI-PLANUM; SEDIMENTARY-ROCKS; BURNS FORMATION; OPPORTUNITY; GRADATION; EROSION; ORIGIN; EJECTA AB Endeavour crater (2.28 degrees S, 354.77 degrees E) is a Noachian-aged 22 km-diameter impact structure of complex morphology in southern Meridiani Planum. The degradation state of the crater has been studied using orbital data from the Mars Reconnaissance Orbiter and in situ data from the Opportunity rover. Multiple exposed crater rim segments range in elevation from similar to 10 m to over 100 m above the level of the embaying Burns Formation. The crater is 200-500 m deep and the interior wall exposes over similar to 300 m of relief around the southern half of the crater. Slopes of 6-16% flank the exterior of the largest western rim segment. On the west side of the crater, both pre-impact rocks (Matijevic Formation) and Endeavour impact ejecta (Shoemaker Formation) are present at Cape York, but only the Shoemaker Formation (up to similar to 140 m section) outcrops at Cape Tribulation. Study of similar sized pristine craters Bopolu and Tooting (with complex morphology) and use of metrics for describing the morphometry of martian craters suggest the original rim of Endeavour averaged 410 m in elevation, but relief varied about +/- 200 m around the circumference. A 250-275 m section of ejecta (+/- 50-60 m) would have comprised a significant fraction of the rim height. The original crater was likely 1.5-2.2 km deep and may have had a central peak (no obvious evidence is present) between 200 and 500 m high. Comparison between the predicted original and current form of Endeavour suggests 100-200 m of rim degradation ranging from nearly complete ejecta removal in some locations to preservation of a thick ejecta section in others. Differences in rim relief are at least partially due to degradation and not just original rim relief and (or) due to offsets along rim faults. Most degradation occurred prior to deposition of the Burns Formation which is similar to 200 m thick outside the crater, but likely thicker inside the crater. Aeolian stripping of the Burns Formation continues today via prevailing winds and lesser mass wasting is important on steeper walls. However, analogy with degraded Noachian craters south of Meridiani suggests fluvial processes were most important in early degradation and is consistent with the nearly complete removal of ejecta from some rim segments, gaps in the rim, formation of Marathon Valley, and interpretation of a pediment flanking the western rim. Slope processes likely accompanied incision that may have accounted for tens of metres rim lowering near Marathon Valley to more than 100 m at Cape York. Published by Elsevier Inc. C1 [Grant, J. A.; Wilson, S. A.] Smithsonian Inst, NASM CEPS, 6th Independence Ave SW, Washington, DC 20560 USA. [Parker, T. J.; Golombek, M. P.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Crumpler, L. S.] New Mexico Museum Nat Hist & Sci, 1801 Mt Rd NW, Albuquerque, NM 87104 USA. [Mittlefehldt, D. W.] NASA, Astromat Res Off, Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. RP Grant, JA (reprint author), Smithsonian Inst, NASM CEPS, 6th Independence Ave SW, Washington, DC 20560 USA. EM grantj@si.edu FU NASA under JPL [1243174, 1272218] FX The authors would like to thank Nadine Barlow and an anonymous reviewer for their constructive comments that improved this manuscript. This research in this paper was supported by NASA under JPL Subcontracts 1243174 (MER) and 1272218 (HiRISE, Univ. of Arizona) to Grant and some of the research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 56 TC 1 Z9 1 U1 12 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC PY 2016 VL 280 BP 22 EP 36 DI 10.1016/j.icarus.2015.08.019 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8HR UT WOS:000384629200003 ER PT J AU Guo, LC Shih, CK Li, LF Ren, D AF Guo, Lichao Shih, Chungkun Li, Longfeng Ren, Dong TI New pelecinid wasps (Hymenoptera: Pelecinidae) from Upper Cretaceous Myanmar amber SO CRETACEOUS RESEARCH LA English DT Article DE Apocrita; New genus; New species; Mesozoic; Brachypelecinus ID NORTHERN MYANMAR; YIXIAN FORMATION; GENUS; PROCTOTRUPOIDEA; EVANIOIDEA; INSECTA; CHINA AB A new genus with a new species, Brachypelecinus euthyntus gen. et sp. nov., and two new species, Abropelecinus tytthus sp. nov. and Zoropelecinus periosus sp. nov., are described and figured from three exquisitely preserved pelecinid wasps in the Upper Cretaceous Myanmar (Burma) amber. These taxa, owing to their well-preserved characters in amber, provide a better understanding of morphological changes and relationships among the constituent groups, while further highlighting the diversity of Pelecinidae in the Mesozoic. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Guo, Lichao; Shih, Chungkun; Li, Longfeng; Ren, Dong] Capital Normal Univ, Coll Life Sci, 105 Xisanhuanbeilu, Beijing 100048, Peoples R China. [Shih, Chungkun] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, 105 Xisanhuanbeilu, Beijing 100048, Peoples R China. EM rendong@mail.cnu.edu.cn FU National Basic Research Program of China (973 Program) [2012CB821906]; National Nature Science Foundational of China [31230065, 41272006]; Program for Changjiang Scholars and Innovative Research Team in University [IRT13081] FX We sincerely appreciate critical review and comments from the editor and reviewers in improving our manuscript. We thank Dr. Taiping Gao and Drs. Mei Wang (College of Life Sciences, Capital Normal University) for their kind help. This research was supported by grants from the National Basic Research Program of China (973 Program) (Grant 2012CB821906), the National Nature Science Foundational of China (No. 31230065, 41272006), Program for Changjiang Scholars and Innovative Research Team in University (IRT13081). NR 19 TC 1 Z9 1 U1 9 U2 10 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD DEC 1 PY 2016 VL 67 BP 84 EP 90 DI 10.1016/j.cretres.2016.07.003 PG 7 WC Geology; Paleontology SC Geology; Paleontology GA DU6UV UT WOS:000382351000008 ER PT J AU Ulak, JT AF Ulak, James T. TI The Life and Afterlives of Hanabusa Itcho, Artist-Rebel of Edo. SO JOURNAL OF JAPANESE STUDIES LA English DT Book Review C1 [Ulak, James T.] Smithsonian Inst, Freer Gallery Art, Japanese Art, Washington, DC 20560 USA. [Ulak, James T.] Smithsonian Inst, Arthur M Sackler Gallery, Japanese Art, Washington, DC 20560 USA. RP Ulak, JT (reprint author), Smithsonian Inst, Freer Gallery Art, Japanese Art, Washington, DC 20560 USA.; Ulak, JT (reprint author), Smithsonian Inst, Arthur M Sackler Gallery, Japanese Art, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU SOC JAPANESE STUD PI SEATTLE PA UNIV WASHINGTON THOMSON HALL DR-05, SEATTLE, WA 98195 USA SN 0095-6848 J9 J JPN STUD JI J. Jpn. Stud. PD WIN PY 2016 VL 42 IS 1 BP 147 EP 152 PG 6 WC Area Studies; Asian Studies SC Area Studies; Asian Studies GA DD8YW UT WOS:000370213800011 ER PT J AU Lacki, M Baranov, MA Pichler, H Zoller, P AF Lacki, M. Baranov, M. A. Pichler, H. Zoller, P. TI Nanoscale "Dark State" Optical Potentials for Cold Atoms SO PHYSICAL REVIEW LETTERS LA English DT Article ID QUANTUM GASES; GAUGE POTENTIALS; POLAR-MOLECULES; ULTRACOLD GASES; EDGE STATES; FERMI GAS; LATTICES; COLLOQUIUM; CREATION; MATTER AB We discuss the generation of subwavelength optical barriers on the scale of tens of nanometers, as conservative optical potentials for cold atoms. These arise from nonadiabatic corrections to Born-Oppenheimer potentials from dressed "dark states" in atomic. configurations. We illustrate the concepts with a double layer potential for atoms obtained from inserting an optical subwavelength barrier into a well generated by an off-resonant optical lattice, and discuss bound states of pairs of atoms interacting via magnetic dipolar interactions. The subwavelength optical barriers represent an optical "Kronig-Penney" potential. We present a detailed study of the band structure in optical Kronig-Penney potentials, including decoherence from spontaneous emission and atom loss to open "bright" channels. C1 [Lacki, M.; Baranov, M. A.; Pichler, H.; Zoller, P.] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. [Lacki, M.; Baranov, M. A.; Pichler, H.; Zoller, P.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Pichler, H.] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Pichler, H.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. RP Lacki, M (reprint author), Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria.; Lacki, M (reprint author), Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. RI Pichler, Hannes/M-5150-2015; Zoller, Peter/O-1639-2014; OI Pichler, Hannes/0000-0003-2144-536X; Zoller, Peter/0000-0003-4014-1505; Lacki, Mateusz/0000-0002-4027-1919 FU ERC Synergy Grant UQUAM; Austrian Science Fund through SFB FOQUS (FWF Project) [F4016-N23]; EU FET Proactive Initiative SIQS; NSF; Smithsonian Astrophysical Observatory FX We thank J. Budich, L. Chomaz, J. Dalibard, M. Dalmonte, F. Ferlaino, R. Grimm, T. Pfau, and T. Porto for helpful comments. Work at Innsbruck is supported by the ERC Synergy Grant UQUAM, the Austrian Science Fund through SFB FOQUS (FWF Project No. F4016-N23), and EU FET Proactive Initiative SIQS. H. P. was supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory. NR 67 TC 0 Z9 0 U1 7 U2 7 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD NOV 30 PY 2016 VL 117 IS 23 AR 233001 DI 10.1103/PhysRevLett.117.233001 PG 6 WC Physics, Multidisciplinary SC Physics GA EG9PN UT WOS:000391391400009 PM 27982643 ER PT J AU Sharma, D Holmes, I Vergara-Asenjo, G Miller, WN Cunampio, M Cunampio, RB Cunampio, MB Potvin, C AF Sharma, Divya Holmes, Ignacia Vergara-Asenjo, Gerardo Miller, William N. Cunampio, Mitzy Cunampio, Raquel B. Cunampio, Mara B. Potvin, Catherine TI A comparison of influences on the landscape of two social-ecological systems SO LAND USE POLICY LA English DT Article DE Eastern Panama; Governance; History; Indigenous; Land cover; Ostrom's social-ecological systems framework ID LAND-COVER CHANGE; TROPICAL DEFORESTATION; ECUADORIAN AMAZON; BIOSPHERE RESERVE; BRAZILIAN AMAZON; FOREST COVER; DYNAMICS; PANAMA; FRAMEWORK; REGION AB Case studies of social-ecological landscapes that consider local, spatially explicit land cover changes are necessary for the development of generalised knowledge on deforestation. This study focussed on two indigenous territories of eastern Panama that share the same settlement history, size and location but are perceived by local dwellers to differ in terms of land cover. By considering the territories social-ecological systems made up of Resource Systems, Resource Units, Actors and Governance Structures, following Ostrom's framework for analysing the sustainability of social-ecological systems (McGinnis and Ostrom, 2014), we sought to determine which social-ecological factors could have led to divergent land cover outcomes to address local leaders' concerns and inform future land management strategies. We conducted quantitative, spatial analysis using ArcGIS and multivariate statistics from numerical ecology on land cover data from participatory maps, and household level socio-economic data from semi-structured interviews and surveys. Results illustrate that the Resource System's topography and Actors' socioeconomics, namely number of people at home and household land ownership, are constraining variables on land cover and help explain divergent forest cover. To reconstruct the influence of history and Governance Structure on the landscapes, we conducted qualitative data collection, namely participatory pebble scoring of historical land cover, interviews with key informants, an archival search, and creation of a participatory historical timeline. Historical governmental timber extraction in the region pre-settlement, guided by topography constraints, may have led to degraded Resource Units (forests) susceptible to clearing. The Governance Structure's self-organizing, monitoring and networking activities with outside institutions in scientific projects, enabled by Actors' leadership and social capital, likely encouraged forest conservation in the forest-rich territory. Future land management could therefore benefit from establishment of a local non-governmental organisation to coordinate a communal vision of management and harness external conservation resources. Our findings suggest that inputting both qualitative and quantitative data obtained by participatory methods into Ostrom's framework can help diagnose territories with divergent landscapes, and thereby inform both forest conservation science and local land management. (C) 2016 The Author(s). Published by Elsevier Ltd. C1 [Sharma, Divya; Holmes, Ignacia; Vergara-Asenjo, Gerardo; Potvin, Catherine] McGill Univ, Dept Biol, 1205 Dr Penfield Ave, Montreal, PQ H3A 1B1, Canada. [Vergara-Asenjo, Gerardo] Forest Res Inst, Fundo Teja Norte S-N, Valdivia, Chile. [Miller, William N.] McGill Univ, Sch Environm, 3534 Univ St, Montreal, PQ H3A 2A7, Canada. [Cunampio, Mitzy; Cunampio, Raquel B.; Cunampio, Mara B.] Community Piriati Embera, Panama City, Panama. [Potvin, Catherine] Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. RP Sharma, D (reprint author), McGill Univ, Dept Biol, 1205 Dr Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM divya.sharma2@mail.mcgill.ca NR 60 TC 0 Z9 0 U1 93 U2 93 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0264-8377 EI 1873-5754 J9 LAND USE POLICY JI Land Use Pol. PD NOV 30 PY 2016 VL 57 BP 499 EP 513 DI 10.1016/j.landusepol.2016.06.018 PG 15 WC Environmental Studies SC Environmental Sciences & Ecology GA DU6RB UT WOS:000382341200045 ER PT J AU Watters, TR Montesi, LGJ Oberst, J Preusker, F AF Watters, Thomas R. Montesi, Laurent G. J. Oberst, Juergen Preusker, Frank TI Fault-bound valley associated with the Rembrandt basin on Mercury SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CALORIS BASIN; LOBATE SCARPS; MESSENGER; LITHOSPHERE; HEMISPHERE; TOPOGRAPHY; EVOLUTION; PLAINS; RIDGES; IMPACT AB The Rembrandt basin is crosscut by the largest fault scarp on Mercury, Enterprise Rupes, and a second scarp complex, Belgica Rupes, extends to the basin's rim. Topographic data derived from MESSENGER orbital stereo images show that these tectonic landforms bound a broad, relatively flat-floored valley with a mean width of similar to 400 km. Crosscutting relations suggest that the accumulation of structural relief likely postdates the formation and volcanic infilling of the Rembrandt basin. The valley floor, bound by fault scarps of opposite vergence, is significantly offset below the elevation of the back-scarp terrains. Along with an offset section of Rembrandt's rim, the elevation differences are evidence that the valley floor was lowered as a result of the formation of bounding fault scarps. The localization of the widely spaced thrust faults of Enterprise and Belgica Rupis and the offset of the valley floor may be the result of long-wavelength buckling of Mercury's lithosphere. C1 [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Montesi, Laurent G. J.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Oberst, Juergen; Preusker, Frank] German Aerosp Ctr, Inst Planetary Res, Berlin, Germany. [Oberst, Juergen] Moscow State Univ Geodesy & Cartog MIIGAiK, Extraterr Lab, Moscow, Russia. RP Watters, TR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu OI Montesi, Laurent/0000-0002-3519-1412 FU Russian Science Foundation [14-22-00197]; NASA [NNX07AR60G] FX We thank the anonymous reviewers for their helpful comments and suggestions that greatly improved the manuscript. We also thank S.C. Solomon and S.A. Hauck, II for their helpful suggestions on an early manuscript. J. Oberst gratefully acknowledges being hosted by MIIGAiK and supported by the Russian Science Foundation under project 14-22-00197. We are grateful to the MESSENGER engineers and technical support personnel at the Johns Hopkins University Applied Physics Laboratory. This work is also supported by NASA grant NNX07AR60G. Data used to produce the results of this paper can be obtained upon request from the first author. MESSENGER images are available from the Planetary Data System Cartography and Imaging Sciences Node (http://pds-imaging.jpl.nasa.gov/schedules/mess_release.html). NR 43 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD NOV 28 PY 2016 VL 43 IS 22 BP 11536 EP 11544 DI 10.1002/2016GL070205 PG 9 WC Geosciences, Multidisciplinary SC Geology GA EJ4SV UT WOS:000393208100007 ER PT J AU Ames, CL Ryan, JF Bely, AE Cartwright, P Collins, AG AF Ames, Cheryl Lewis Ryan, Joseph F. Bely, Alexandra E. Cartwright, Paulyn Collins, Allen G. TI A new transcriptome and transcriptome profiling of adult and larval tissue in the box jellyfish Alatina alata: an emerging model for studying venom, vision and sex (vol 17, 650, 2016) SO BMC GENOMICS LA English DT Correction C1 [Ames, Cheryl Lewis; Collins, Allen G.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Ames, Cheryl Lewis] Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. [Ryan, Joseph F.] Univ Florida, Whitney Lab Marine Biosci, St Augustine, FL 32080 USA. [Ryan, Joseph F.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Bely, Alexandra E.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Cartwright, Paulyn] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, NOAA Fisheries, Natl Systemat Lab, Washington, DC 20560 USA. [Ames, Cheryl Lewis] Smithsonian Inst, Natl Museum Nat Hist, 10th & Constitut Ave NW, Washington, DC 20560 USA. RP Ames, CL (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA.; Ames, CL (reprint author), Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. EM amesc@si.edu NR 2 TC 0 Z9 0 U1 6 U2 6 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2164 J9 BMC GENOMICS JI BMC Genomics PD NOV 28 PY 2016 VL 17 AR 980 DI 10.1186/s12864-016-3305-y PG 2 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA ED3UI UT WOS:000388773600003 ER PT J AU Silva, GSC Melo, BF Oliveira, C Benine, RC AF Silva, Gabriel S. C. Melo, Bruno F. Oliveira, Claudio Benine, Ricardo C. TI Revision of the South American genus Tetragonopterus Cuvier, 1816 (Teleostei: Characidae) with description of four new species SO ZOOTAXA LA English DT Article DE Amazon basin; Characiformes; DNA barcode; Moenkhausia; Neotropical region ID CHARACIFORMES CHARACIDAE; BRAZIL; PHYLOGENY; FISHES; TAXA AB The systematics of the characid genus Tetragonopterus is reviewed based on morphological and molecular data of specimens from its entire geographical range encompassing all major South American river drainages from Orinoco basin southward to the La Plata basin. Eight previously described species (T. anostomus, T. araguaiensis, T. argenteus, T. carvalhoi, T. chalceus, T. denticulatus, T. georgiae n. comb., and T. rarus) are recognized as valid, four of which are redescribed (T. argenteus, T. chalceus, T. georgiae, and T. rarus), and four new species from the Brazilian Shield in the Amazon and Sao Francisco river basins are herein described. We also provide evidence for the reallocation of Moenkhausia georgiae into Tetragonopterus and recognize T. akamai as junior synonym of T. anostomus. DNA barcodes of Tetragonopterus revealed genetic support for each recognized species and provided valuable population-level information within T. argenteus, T. chalceus, T. georgiae, and T. rarus. C1 [Silva, Gabriel S. C.; Melo, Bruno F.; Oliveira, Claudio] Univ Estadual Paulista, Inst Biociencias, Dept Morfol, R Prof Dr Antonio CW Zanin S-N, BR-18618689 Botucatu, SP, Brazil. [Melo, Bruno F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Benine, Ricardo C.] Univ Estadual Paulista, Inst Biociencias, Dept Zool, R Prof Dr Antonio CW Zanin S-N, BR-18618689 Botucatu, SP, Brazil. RP Benine, RC (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Zool, R Prof Dr Antonio CW Zanin S-N, BR-18618689 Botucatu, SP, Brazil. EM gabriel_biota@yahoo.com.br; melo@ibb.unesp.br; claudio@ibb.unesp.br; rbenine@ibb.unesp.br RI Gesseff, Ednilson/A-3019-2017; Melo, Bruno F./G-1644-2012 OI Melo, Bruno F./0000-0002-0499-567X FU FAPESP [2012/01622-2, 2011/08374-1, 2010/17009-2, 2014/26508-3, 2006/00545-3]; CNPq [PDJ 40258/2014-7]; FAPESP Thematic Project "Phylogenetic relationships in the Characidae (Ostariophysi: Characiformes)" (FAPESP) [04/09219-6]; FAPESP Thematic Project "South American Characiformes Inventory" (FAPESP) [11/50282-7] FX We thank Raphael Covain (MHNG) for providing important sequences of Tetragonopterus species from the Guianas. We also thank many colleagues for loan of specimens and curatorial assistance: Flavio A. Bockmann and Ricardo M. C. Castro (LIRP), Mario C. C. de Pinna, Alessio Datovo, Osvaldo T. Oyakawa, Michel D. Gianeti and Fernando Dagosta (MZUSP), Carla S. Pavanelli (NUP), Paulo H. F. Lucinda (UNT), Richard P. Vari (USNM), Brian L. Sidlauskas and Benjamin W. Frable (OS), John G. Lundberg, Mark Sabaj Perez and Kyle R. Luckenbill (ANSP), Raphael Covain and Sonia Fisch-Muller (MHNG). We also thank Fernando Dagosta, Jose L. O. Birindelli, Kyle R. Luckenbill, Martin I. Taylor, Raphael Covain and Tiago P. Carvalho for providing photographs of specimens. We also thank Flavio A. Bockmann, Ricardo M. C. Castro and Hertz Santos (LIRP) for assistance with x-ray diffraction images (FAPESP proc. 09/54931-0). Thanks to Flavio C. T. Lima and Oscar A. Shibatta who reviewed early versions of this manuscript as members of the Master dissertation committee. This paper was developed as a Master's dissertation in Biological Sciences with emphasis in Zoology by the first author. Authors received support from FAPESP proc. 2012/01622-2 (GSCS), CNPq PDJ 40258/2014-7 and FAPESP proc. 2011/08374-1 (BFM), FAPESP proc. 2010/17009-2 and FAPESP proc. 2014/26508-3 (CO) and FAPESP proc. 2006/00545-3 (RCB). This study was part of the FAPESP Thematic Project "Phylogenetic relationships in the Characidae (Ostariophysi: Characiformes)" (FAPESP proc. 04/09219-6) and benefits from the FAPESP Thematic Project " South American Characiformes Inventory" (FAPESP proc. 11/50282-7). NR 59 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 28 PY 2016 VL 4200 IS 1 BP 1 EP 46 DI 10.11646/zootaxa.4200.1.1 PG 46 WC Zoology SC Zoology GA EC9MF UT WOS:000388468000001 ER PT J AU Kear, BP Aplin, KP Westerman, M AF Kear, Benjamin P. Aplin, Ken P. Westerman, Michael TI Bandicoot fossils and DNA elucidate lineage antiquity amongst xeric-adapted Australasian marsupials SO SCIENTIFIC REPORTS LA English DT Article ID 5 NUCLEAR GENES; MISSING DATA; NORTHWESTERN QUEENSLAND; PHYLOGENETIC-RELATIONSHIPS; OLIGOMIOCENE DEPOSITS; DIDELPHID MARSUPIALS; YARALA-BURCHFIELDI; LOCAL FAUNA; PERAMELEMORPHIA; MIOCENE AB Bandicoots (Peramelemorphia) are a unique order of Australasian marsupials whose sparse fossil record has been used as prima facie evidence for climate change coincident faunal turnover. In particular, the hypothesized replacement of ancient rainforest-dwelling extinct lineages by antecedents of xeric-tolerant extant taxa during the late Miocene (-10 Ma) has been advocated as a broader pattern evident amongst other marsupial clades. Problematically, however, this is in persistent conflict with DNA phylogenies. We therefore determine the pattern and timing of bandicoot evolution using the first combined morphological + DNA sequence dataset of Peramelemorphia. In addition, we document a remarkably archaic new fossil peramelemorphian taxon that inhabited a latest Quaternary mosaic savannah-riparian forest ecosystem on the Aru Islands of Eastern Indonesia. Our phylogenetic analyses reveal that unsuspected dental homoplasy and the detrimental effects of missing data collectively obscure stem bandicoot relationships. Nevertheless, recalibrated molecular clocks and multiple ancestral area optimizations unanimously infer an early diversification of modern xeric-adapted forms. These probably originated during the late Palaeogene (30-40 Ma) alongside progenitors of other desert marsupials, and thus occupied seasonally dry heterogenous habitats long before the onset of late Neogene aridity. C1 [Kear, Benjamin P.] Uppsala Univ, Museum Evolut, Norbyvagen 16, SE-75236 Uppsala, Sweden. [Kear, Benjamin P.] Uppsala Univ, Dept Earth Sci, Villavagen 16, SE-75236 Uppsala, Sweden. [Aplin, Ken P.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. [Westerman, Michael] La Trobe Univ, Dept Ecol Environm & Evolut, Melbourne, Vic 3086, Australia. RP Kear, BP (reprint author), Uppsala Univ, Museum Evolut, Norbyvagen 16, SE-75236 Uppsala, Sweden.; Kear, BP (reprint author), Uppsala Univ, Dept Earth Sci, Villavagen 16, SE-75236 Uppsala, Sweden. EM benjamin.kear@em.uu.se FU Swedish Research Council; Uppsala University; La Trobe University FX The authors thank Sandy Ingleby and Yong Yi Zhen (Australian Museum), Gavin Dally (Museum & Art Gallery of the Northern Territory), Wayne Longmore, Rory O'Brien and David Pickering (Museum Victoria), Robert Meredith and Mark Springer (University of California), Kenny Travouillon (Western Australian Museum), Michael Archer (University of New South Wales), and David Stemmer (South Australian Museum) for access to specimens, sequence data, and information. The Swedish Research Council, Uppsala University, and La Trobe University provided financial support. NR 80 TC 0 Z9 0 U1 1 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD NOV 24 PY 2016 VL 6 AR 37537 DI 10.1038/srep37537 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA ED6LJ UT WOS:000388966800001 PM 27881865 ER PT J AU Caudill, SA Rice, RA AF Caudill, S. Amanda Rice, Robert A. TI Do Bird Friendly (R) Coffee Criteria Benefit Mammals? Assessment of Mammal Diversity in Chiapas, Mexico SO PLOS ONE LA English DT Article ID BIODIVERSITY CONSERVATION; SOUTHERN MEXICO; WESTERN-GHATS; FOREST; AGROECOSYSTEMS; LANDSCAPES; FRAGMENTATION; CERTIFICATION; AGROFORESTRY; PLANTATIONS AB Biodiversity-friendly coffee certifications offer a viable way to protect wildlife habitat while providing a financial incentive to farmers. Most studies related to these certifications focus on avian habitat requirements and it is not known whether these standards also apply to other wildlife, such as mammals, that inhabit the coffee landscapes. We assessed the non-volant mammalian fauna and their associated habitat requirements in 23 sites representing forest, Bird Friendly (R) shade, conventional shade, and sun coffee habitats. We used Sherman trap-grids to measure small mammal abundance and richness, while camera traps were set for medium-sized and large mammals. We detected 17 species of mammals, representing 11 families. This preliminary study indicates that coffee farms in this region provide an important refuge for mammalian wildlife. Mammal species density ranked significantly higher in Bird Friendly (R) coffee sites than other coffee habitats, although there was no significant difference for species richness (using Chao2 estimator) among the habitat types. No significant difference was found in small mammal abundance among the habitat types. We found a higher species density of medium and large mammals in sites with larger, more mature shade trees associated with, but not required by Bird Friendly (R) certification standards. However, lower strata vegetation (5 cm to 1 m tall), the only vegetation parameter found to increase abundance and density for small mammals, is not specified in the Bird Friendly (R) standards. Our findings suggest that although the standards devised for avian habitat do benefit mammals, further study is needed on the requirements specific for mammals that could be included to enhance the coffee habitat for mammals that inhabit these coffee landscapes. C1 [Caudill, S. Amanda; Rice, Robert A.] Natl Zool Pk, Smithsonian Conservat Biol Inst, MRC 5503, Washington, DC 20013 USA. RP Caudill, SA (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, MRC 5503, Washington, DC 20013 USA. EM caudills@si.edu FU Smithsonian Migratory Bird Center FX SAC received financial support from the Smithsonian Migratory Bird Center.We would like to thank Finca Argovia and Dra. Consuelo Lorenzo Monterrubio for their supportand assistance with logistics for the study, as well as Bruno Giesemann E., Rainer E.Boehme Trueb, Eduardo Bracamontes for their participation in the study and for allowing usaccess to their farms. This study would not have been possible without the hard work of those who assisted with the field work: Megan Banner, Stephen Brennen, Caitlin Campbell, Tim Lima, Adaberto, and Daniel Dixon. We would like to thank Mirian Tsuchiya for the genetics lab work. We would also like to thank the valuable input of the anonymous reviewers whose comments and recommendations improved the manuscript. SAC received financial support from the Smithsonian Migratory Bird Center. NR 41 TC 0 Z9 0 U1 8 U2 8 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD NOV 23 PY 2016 VL 11 IS 11 AR e0165662 DI 10.1371/journal.pone.0165662 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA ED5KB UT WOS:000388889500013 PM 27880773 ER PT J AU O'Mara, MT Bauer, K Blank, D Baldwin, JW Dechmann, DKN AF O'Mara, M. Teague Bauer, Karla Blank, Dominik Baldwin, Justin W. Dechmann, Dina K. N. TI Common Noctule Bats Are Sexually Dimorphic in Migratory Behaviour and Body Size but Not Wing Shape SO PLOS ONE LA English DT Article ID NYCTALUS-NOCTULA; ELECTRICAL-CONDUCTIVITY; VESPERTILIONID BATS; POINTED WINGS; HABITAT USE; MORPHOLOGY; GROWTH; CONSERVATION; CHIROPTERA; ADAPTATION AB Within the large order of bats, sexual size dimorphism measured by forearm length and body mass is often female-biased. Several studies have explained this through the effects on load carrying during pregnancy, intrasexual competition, as well as the fecundity and thermoregulation advantages of increased female body size. We hypothesized that wing shape should differ along with size and be under variable selection pressure in a species where there are large differences in flight behaviour. We tested whether load carrying, sex differential migration, or reproductive advantages of large females affect size and wing shape dimorphism in the common noctule (Nyctalus noctula), in which females are typically larger than males and only females migrate long distances each year. We tested for univariate and multivariate size and shape dimorphism using data sets derived from wing photos and biometric data collected during pre-migratory spring captures in Switzerland. Females had forearms that are on average 1% longer than males and are 1% heavier than males after emerging from hibernation, but we found no sex differences in other size, shape, or other functional characters in any wing parameters during this pre-migratory period. Female-biased size dimorphism without wing shape differences indicates that reproductive advantages of big mothers are most likely responsible for sexual dimorphism in this species, not load compensation or shape differences favouring aerodynamic efficiency during pregnancy or migration. Despite large behavioural and ecological sex differences, morphology associated with a specialized feeding niche may limit potential dimorphism in narrow-winged bats such as common noctules and the dramatic differences in migratory behaviour may then be accomplished through plasticity in wing kinematics. C1 [O'Mara, M. Teague; Bauer, Karla; Blank, Dominik; Baldwin, Justin W.; Dechmann, Dina K. N.] Max Planck Inst Ornithol, Dept Migrat & Immuno Ecol, Radolfzell am Bodensee, Germany. [O'Mara, M. Teague; Bauer, Karla; Blank, Dominik; Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, Constance, Germany. [O'Mara, M. Teague; Dechmann, Dina K. N.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP O'Mara, MT (reprint author), Max Planck Inst Ornithol, Dept Migrat & Immuno Ecol, Radolfzell am Bodensee, Germany.; O'Mara, MT (reprint author), Univ Konstanz, Dept Biol, Constance, Germany.; O'Mara, MT (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama. EM tomara@orn.mpg.de OI O'Mara, M. Teague/0000-0002-6951-1648 FU Max Planck Poland Biodiversity Initiative; Max Planck Institute for Ornithology FX This work was funded by the Max Planck Poland Biodiversity Initiative and the Max Planck Institute for Ornithology. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 48 TC 0 Z9 0 U1 8 U2 8 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD NOV 23 PY 2016 VL 11 IS 11 AR e0167027 DI 10.1371/journal.pone.0167027 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA ED5KB UT WOS:000388889500056 PM 27880791 ER PT J AU Ceriaco, LMP Gutierrez, EE Dubois, A AF Ceriaco, Luis M. P. Gutierrez, Eliecer E. Dubois, Alain TI Photography-based taxonomy is inadequate, unnecessary, and potentially harmful for biological sciences SO ZOOTAXA LA English DT Article C1 [Ceriaco, Luis M. P.] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Ceriaco, Luis M. P.] Museu Nacl Hist Nat & Ciencia, Lisbon, Portugal. [Gutierrez, Eliecer E.] Univ Brasilia, Dept Zool, Inst Ciencias Biol, BR-70910900 Brasilia, DF, Brazil. [Gutierrez, Eliecer E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Dubois, Alain] Sorbonne Univ, Museum Natl Hist Nat, ISYEB, Paris, France. RP Ceriaco, LMP (reprint author), Villanova Univ, Dept Biol, Villanova, PA 19085 USA.; Ceriaco, LMP (reprint author), Museu Nacl Hist Nat & Ciencia, Lisbon, Portugal. EM luisceriaco@gmail.com RI Faundez, Eduardo/C-9604-2017; Oliveira, Sarah/D-6711-2013; Goncalves, Pablo/F-7589-2013; Gesseff, Ednilson/A-3019-2017; Hirschmann, Alice/D-9119-2016; Cozzuol, Mario/H-8302-2012; Vieira, Leandro/B-7712-2011; Fernandes, Daniel/D-7168-2013; Rodrigues, Miguel/F-8174-2012; Justine, Jean-Lou/B-1298-2010; Moreira, Felipe/E-5768-2011 OI Bornschein, Marcos Ricardo/0000-0002-6486-7055; Rojas-Runjaic, Fernando J. M./0000-0001-5409-4231; TSCHOPP, Emanuel/0000-0002-5245-6910; Miller, Matthew/0000-0002-2939-0239; Quintela Alonso, Pablo/0000-0003-2346-6367; Semedo, Thiago/0000-0003-4379-5993; Reis, Roberto/0000-0003-3746-6894; Langeani, Francisco/0000-0001-7376-4798; La Terza, Antonietta/0000-0002-1244-1503; Perez-Gonzalez, Abel/0000-0002-4245-3302; Cianferoni, Fabio/0000-0003-3170-0774; Faundez, Eduardo/0000-0003-2596-2292; Goncalves, Pablo/0000-0002-4923-2334; Hirschmann, Alice/0000-0001-7012-6416; Cozzuol, Mario/0000-0003-3645-0401; Fernandes, Daniel/0000-0001-6155-6246; Justine, Jean-Lou/0000-0002-7155-4540; NR 12 TC 5 Z9 6 U1 14 U2 14 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 23 PY 2016 VL 4196 IS 3 BP 435 EP 445 DI 10.11646/zootaxa.4196.3.9 PG 11 WC Zoology SC Zoology GA EC5HW UT WOS:000388165400009 ER PT J AU Amorisco, NC Gomez, FA Vegetti, S White, SDM AF Amorisco, Nicola C. Gomez, Facundo A. Vegetti, Simona White, Simon D. M. TI Gaps in globular cluster streams: giant molecular clouds can cause them too SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: haloes; galaxies: kinematics and dynamics; galaxies: structure; cosmology: theory; dark matter ID DARK-MATTER HALO; COLD STELLAR STREAM; MILKY-WAY; TIDAL STREAMS; PALOMAR 5; MISSING SATELLITES; CLUMPY STREAMS; STAR-FORMATION; SUBSTRUCTURE; SUBHALOES AB As a result of their internal dynamical coherence, thin stellar streams formed by disrupting globular clusters (GCs) can act as detectors of dark matter (DM) substructure in the Galactic halo. Perturbations induced by close flybys amplify into detectable density gaps, providing a probe both of the abundance and of the masses of DM subhaloes. Here, we use N-body simulations to show that the Galactic population of giant molecular clouds (GMCs) can also produce gaps (and clumps) in GC streams, and so may confuse the detection of DM subhaloes. We explore the cases of streams analogous to the observed Palomar 5 and GD1 systems, quantifying the expected incidence of structure caused by GMC perturbations. Deep observations should detect such disturbances regardless of the substructure content of the Milky Way's halo. Detailed modelling will be needed to demonstrate that any detected gaps or clumps were produced by DM subhaloes rather than by molecular clouds. C1 [Amorisco, Nicola C.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. [Amorisco, Nicola C.; Gomez, Facundo A.; Vegetti, Simona; White, Simon D. M.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. RP Amorisco, NC (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA.; Amorisco, NC (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM nicola.amorisco@cfa.harvard.edu NR 51 TC 0 Z9 0 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2016 VL 463 IS 1 BP L17 EP L21 DI 10.1093/mnrasl/slw148 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ8XX UT WOS:000386157100004 ER PT J AU Bagge, LE Osborn, KJ Johnsen, S AF Bagge, Laura E. Osborn, Karen J. Johnsen, Sonke TI Nanostructures and Monolayers of Spheres Reduce Surface Reflections in Hyperiid Amphipods SO CURRENT BIOLOGY LA English DT Article ID OPTICAL-PROPERTIES; TRANSPARENCY; CEPHALOPODS; ARRAY; DEEP; EYES AB Transparent zooplankton and nekton are often nearly invisible when viewed under ambient light in the pelagic zone [1-3]. However, in this environment, where the light field is directional (and thus likely to cause reflections), and under the bioluminescent searchlights of potential predators, animals may be revealed by reflections from their body surface [4-7]. We investigated the cuticle surfaces of seven species of hyperiids (Crustacea; Amphipoda) using scanning electron microscopy and found two undocumented features that may reduce reflectance. We found that the legs of Cystisoma spp. (n = 5) are covered with an ordered array of nanoprotuberances 200 20 nm SD in height that function optically as a gradient refractive index material [6, 8, 9]. Additionally, we observed that Cystisoma and six other species of hyperiids are covered with a monolayer of homogenous spheres (diameters ranging from 52 7 nm SD on Cystisoma spp. to 320 15 nm SD on Phronima spp.). Optical modeling using effective medium theory and transfer matrix methods demonstrated that both the nanoprotuberances and the monolayers reduce reflectance by as much as 100 fold, depending on the wavelength and angle of the incident light and the thickness of the gradient layer. Even though we only consider surface reflectance and not internal light scattering, our study demonstrates that these nanoprotuberances and spheres can improve crypsis in a featureless habitat where the smallest reflection can render an animal vulnerable to visual predation. C1 [Bagge, Laura E.; Johnsen, Sonke] Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA. [Osborn, Karen J.] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Bagge, LE (reprint author), Duke Univ, Dept Biol, Box 90338, Durham, NC 27708 USA. EM laura.elizabeth.bagge@gmail.com OI Osborn, Karen/0000-0002-4226-9257 FU National Science Foundation [OCE-0852138]; Office of Naval Research [N00014-09-1-1053]; Sigma Xi; Rathbun Crustacean Research Endowment at Smithsonian NMNH FX We thank three anonymous reviewers; Eleanor Caves; Kate Thomas; Benjamin (Jay) Wheeler; and Drs. Jamie Baldwin Fergus, Dan Speiser, Robert Fitak, Lorian Schweikert, and Nicholas Brandley for comments on earlier versions of this manuscript. We thank Richard Dillaman and Mark Gay (UNC Wilmington), Michelle Gignac (Duke's Shared Materials Instrumentation Facility), and Scott Whittacker (Smithsonian) for assistance with electron microscopy. We also thank the affiliates of the RV Endeavour, RV Kilo Moana, RV Western Flyer, and RV Sunburst for facilitating specimen collection. Funding was provided by grants from the National Science Foundation (OCE-0852138) and Office of Naval Research (N00014-09-1-1053) to S.J. and Sigma Xi Grant-in-Aid of Research and Rathbun Crustacean Research Endowment at Smithsonian NMNH to L.E.B. NR 25 TC 1 Z9 1 U1 2 U2 2 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD NOV 21 PY 2016 VL 26 IS 22 BP 3071 EP 3076 DI 10.1016/j.cub.2016.09.033 PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA ED0QB UT WOS:000388545900027 PM 28094029 ER PT J AU Lawrence, A Bruce, AG MacLeod, C Gezari, S Elvis, M Ward, M Smartt, SJ Smith, KW Wright, D Fraser, M Marshall, P Kaiser, N Burgett, W Magnier, E Tonry, J Chambers, K Wainscoat, R Waters, C Price, P Metcalfe, N Valenti, S Kotak, R Mead, A Inserra, C Chen, TW Soderberg, A AF Lawrence, A. Bruce, A. G. MacLeod, C. Gezari, S. Elvis, M. Ward, M. Smartt, S. J. Smith, K. W. Wright, D. Fraser, M. Marshall, P. Kaiser, N. Burgett, W. Magnier, E. Tonry, J. Chambers, K. Wainscoat, R. Waters, C. Price, P. Metcalfe, N. Valenti, S. Kotak, R. Mead, A. Inserra, C. Chen, T. W. Soderberg, A. TI Slow-blue nuclear hypervariables in PanSTARRS-1 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; gravitational lensing: micro; galaxies: active; galaxies: nuclei; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; TIDAL DISRUPTION EVENTS; QUASAR ACCRETION DISKS; BROAD-LINE REGIONS; X-RAY OUTBURST; LIGHT CURVES; ENERGY-DISTRIBUTIONS; LUMINOSITY FUNCTION AB We discuss 76 large amplitude transients (Delta m > 1.5) occurring in the nuclei of galaxies, nearly all with no previously known active galactic nucleus (AGN). They have been discovered as part of the Pan-STARRS1 (PS1) 3 pi survey, by comparison with Sloan Digital Sky Survey (SDSS) photometry a decade earlier, and then monitored with the Liverpool Telescope, and studied spectroscopically with the William Herschel Telescope (WHT). Based on colours, light-curve shape, and spectra, these transients fall into four groups. A few are misclassified stars or objects of unknown type. Some are red/fast transients and are known or likely nuclear supernovae. A few are either radio sources or erratic variables and so likely blazars. However the majority (66 per cent) are blue and evolve slowly, on a time-scale of years. Spectroscopy shows them to be AGN at z 0.3 - 1.4, which must have brightened since the SDSS photometry by around an order of magnitude. It is likely that these objects were in fact AGN a decade ago, but too weak to be recognized by SDSS; they could then be classed as 'hypervariable' AGN. By searching the SDSS Stripe 82 quasar database, we find 15 similar objects. We discuss several possible explanations for these slow-blue hypervariables - (i) unusually luminous tidal disruption events; (ii) extinction events; (iii) changes in accretion state; and (iv) large amplitude microlensing by stars in foreground galaxies. A mixture of explanations (iii) and (iv) seems most likely. Both hold promise of considerable new insight into the AGN phenomenon. C1 [Lawrence, A.; Bruce, A. G.; MacLeod, C.; Mead, A.] Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Gezari, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Elvis, M.; Soderberg, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ward, M.; Metcalfe, N.] Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. [Smartt, S. J.; Smith, K. W.; Wright, D.; Fraser, M.; Valenti, S.; Kotak, R.; Inserra, C.; Chen, T. W.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Fraser, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 OHA, England. [Marshall, P.] SLAC Natl Accelerator Lab, KIPAC, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. [Kaiser, N.; Burgett, W.; Magnier, E.; Tonry, J.; Chambers, K.; Wainscoat, R.; Waters, C.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Price, P.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Lawrence, A (reprint author), Univ Edinburgh, Royal Observ, SUPA, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM al@roe.ac.uk FU National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877]; University of Maryland FX The Pan-STARRS1 (PS1) Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, and the University of Maryland. NR 108 TC 0 Z9 0 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2016 VL 463 IS 1 BP 296 EP 331 DI 10.1093/mnras/stw1963 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA2YZ UT WOS:000386464900023 ER PT J AU Li, GJ Adams, FC AF Li, Gongjie Adams, Fred C. TI Cross-sections for planetary systems interacting with passing stars and binaries (vol 448, pg 344, 2015) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Correction DE planets and satellites: dynamical evolution and stability; planetary systems C1 [Li, Gongjie] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Adams, Fred C.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM gli@cfa.harvard.edu NR 3 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2016 VL 463 IS 1 BP 393 EP 393 DI 10.1093/mnras/stw2014 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA2YZ UT WOS:000386464900029 ER PT J AU Mocz, P Pakmor, R Springel, V Vogelsberger, M Marinacci, F Hernquist, L AF Mocz, Philip Pakmor, Ruediger Springel, Volker Vogelsberger, Mark Marinacci, Federico Hernquist, Lars TI A moving mesh unstaggered constrained transport scheme for magnetohydrodynamics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE magnetic fields; MHD; methods: numerical; Galaxy: formation; cosmology: theory ID COSMOLOGICAL MAGNETIC-FIELDS; SMALL-SCALE DYNAMO; HYDRODYNAMIC SIMULATION; GALAXY FORMATION; PARTICLE METHODS; STAR-FORMATION; TURBULENCE; CODE; REFINEMENT; ACCRETION AB We present a constrained transport (CT) algorithm for solving the 3D ideal magnetohydrodynamic (MHD) equations on a moving mesh, which maintains the divergence-free condition on the magnetic field to machine-precision. Our CT scheme uses an unstructured representation of the magnetic vector potential, making the numerical method simple and computationally efficient. The scheme is implemented in the moving mesh code arepo. We demonstrate the performance of the approach with simulations of driven MHD turbulence, a magnetized disc galaxy, and a cosmological volume with primordial magnetic field. We compare the outcomes of these experiments to those obtained with a previously implemented Powell divergence-cleaning scheme. While CT and the Powell technique yield similar results in idealized test problems, some differences are seen in situations more representative of astrophysical flows. In the turbulence simulations, the Powell cleaning scheme artificially grows the mean magnetic field, while CT maintains this conserved quantity of ideal MHD. In the disc simulation, CT gives slower magnetic field growth rate and saturates to equipartition between the turbulent kinetic energy and magnetic energy, whereas Powell cleaning produces a dynamically dominant magnetic field. Such difference has been observed in adaptive-mesh refinement codes with CT and smoothed-particle hydrodynamics codes with divergence-cleaning. In the cosmological simulation, both approaches give similar magnetic amplification, but Powell exhibits more cell-level noise. CT methods in general are more accurate than divergence-cleaning techniques, and, when coupled to a moving mesh can exploit the advantages of automatic spatial/temporal adaptivity and reduced advection errors, allowing for improved astrophysical MHD simulations. C1 [Mocz, Philip; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pakmor, Ruediger; Springel, Volker] Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, Astron Recheninst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Vogelsberger, Mark; Marinacci, Federico] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Mocz, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmocz@cfa.harvard.edu FU National Science Foundation Graduate Research Fellowship [DGE-1144152]; NASA Earth and Space Science Fellowship; NASA [NNX12AC67G]; NSF [AST-1312095]; European Research Council under ERC-StG grant [EXAGAL-308037]; FAS Division of Science, Research Computing Group at Harvard University FX This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant no. DGE-1144152. PM is supported in part by the NASA Earth and Space Science Fellowship. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. RP and VS acknowledge support through the European Research Council under ERC-StG grant EXAGAL-308037, and thank the Klaus Tschira Foundation. VS also acknowledges subproject EXAMAG of the Priority Programme 1648 'Software for Exascale Computing' of the German Science Foundation. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. NR 56 TC 2 Z9 3 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2016 VL 463 IS 1 BP 477 EP 488 DI 10.1093/mnras/stw2004 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA2YZ UT WOS:000386464900037 ER PT J AU Zou, S Maughan, BJ Giles, PA Vikhlinin, A Pacaud, F Burenin, R Hornstrup, A AF Zou, S. Maughan, B. J. Giles, P. A. Vikhlinin, A. Pacaud, F. Burenin, R. Hornstrup, A. TI The X-ray luminosity-temperature relation of a complete sample of low-mass galaxy clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: observational; methods: statistical; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: groups: general; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; SCALING RELATIONS; PARAMETER CONSTRAINTS; COOLING FLOWS; AGN FEEDBACK; T RELATION; CHANDRA; EVOLUTION; II.; COSMOLOGY AB We present Chandra observations of 23 galaxy groups and low-mass galaxy clusters at 0.03 < z < 0.15 with a median temperature of similar to 2keV. The sample is a statistically complete flux-limited subset of the 400 deg(2) survey. We investigated the scaling relation between X-ray luminosity (L) and temperature (T), taking selection biases fully into account. The logarithmic slope of the bolometric L-T relation was found to be 3.29 +/- 0.33, consistent with values typically found for samples of more massive clusters. In combination with other recent studies of the L-T relation, we show that there is no evidence for the slope, normalization, or scatter of the L-T relation of galaxy groups being different than that of massive clusters. The exception to this is that in the special case of the most relaxed systems, the slope of the core-excised L-T relation appears to steepen from the self-similar value found for massive clusters to a steeper slope for the lower mass sample studied here. Thanks to our rigorous treatment of selection biases, these measurements provide a robust reference against which to compare predictions of models of the impact of feedback on the X-ray properties of galaxy groups. C1 [Zou, S.; Maughan, B. J.; Giles, P. A.] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Zou, S.] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, 98bis Blvd Arago, F-75014 Paris, France. [Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02140 USA. [Vikhlinin, A.; Burenin, R.] Russian Acad Sci, Space Res Inst, Profsoyuznaya Ul 84-32, Moscow 117997, Russia. [Pacaud, F.] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. [Burenin, R.] Moscow Inst Phys & Technol, Inst Sky Per 9, Dolgoprudnyi 141700, Russia. [Hornstrup, A.] Tech Univ Denmark, Natl Space Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. RP Zou, S (reprint author), Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England.; Zou, S (reprint author), Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, 98bis Blvd Arago, F-75014 Paris, France. EM sz13769@my.bristol.ac.uk FU STFC [ST/J001414/1, ST/M000907/1]; RNF grant [14-22-00271] FX BJM and PAG acknowledge support from STFC grants ST/J001414/1 and ST/M000907/1.; RB was supported by RNF grant 14-22-00271. NR 51 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2016 VL 463 IS 1 BP 820 EP 831 DI 10.1093/mnras/stw1992 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA2YZ UT WOS:000386464900067 ER PT J AU Churazov, E Arevalo, P Forman, W Jones, C Schekochihin, A Vikhlinin, A Zhuravleva, I AF Churazov, E. Arevalo, P. Forman, W. Jones, C. Schekochihin, A. Vikhlinin, A. Zhuravleva, I. TI Arithmetic with X-ray images of galaxy clusters: effective equation of state for small-scale perturbations in the ICM SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: intracluster medium; galaxies: clusters: individual: Perseus; X-rays: galaxies: clusters ID PERSEUS CLUSTER; SURFACE BRIGHTNESS; INTRACLUSTER MEDIUM; GASEOUS ATMOSPHERE; VIRGO CLUSTER; XMM-NEWTON; HOT GAS; CHANDRA; TEMPERATURE; FLUCTUATIONS AB We discuss a novel technique of manipulating X-ray images of galaxy clusters to reveal the nature of small-scale density/temperature perturbations in the intracluster medium (ICM). As we show, this technique can be used to differentiate between sound waves and isobaric perturbations in Chandra images of the Perseus and M87/Virgo clusters. The comparison of the manipulated images with the radio data and with the results of detailed spectral analysis shows that this approach successfully classifies the types of perturbations and helps to reveal their nature. For the central regions (5-100 kpc) of the M87 and Perseus clusters, this analysis suggests that observed images are dominated by isobaric perturbations, followed by perturbations caused by bubbles of relativistic plasma and weak shocks. Such a hierarchy is best explained in a 'slow' active galactic nuclei feedback scenario, when much of the mechanical energy output of a central black hole is captured by the bubble enthalpy that is gradually released during buoyant rise of the bubbles. The 'image arithmetic' works best for prominent structure and for data sets with excellent statistics, visualizing the perturbations with a given effective equation of state. The same approach can be extended to faint perturbations via cross-spectrum analysis of surface brightness fluctuations in X-ray images in different energy bands. C1 [Churazov, E.] Max Planck Inst Astrophys MPA, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Churazov, E.] Space Res Inst IKI, Profsoyuznaya 84-32, Moscow 117997, Russia. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Gran Bretana N 1111, Valparaiso, Chile. [Forman, W.; Jones, C.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Schekochihin, A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, 1 Keble Rd, Oxford OX1 3NP, England. [Schekochihin, A.] Univ Oxford Merton Coll, Merton St, Oxford OX1 4JD, England. [Zhuravleva, I.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. [Zhuravleva, I.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. RP Churazov, E (reprint author), Max Planck Inst Astrophys MPA, Karl Schwarzschild Str 1, D-85741 Garching, Germany.; Churazov, E (reprint author), Space Res Inst IKI, Profsoyuznaya 84-32, Moscow 117997, Russia. EM churazov@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 FU Russian Scientific Foundation [14-22-00271]; NASA [NAS8-03060]; Smithsonian Institution; Fondecyt [1140304] FX EC acknowledges support by grant No. 14-22-00271 from the Russian Scientific Foundation. WF and CJ acknowledge support from NASA contract NAS8-03060 and the Smithsonian Institution. PA acknowledges support from Fondecyt grant 1140304. NR 33 TC 0 Z9 0 U1 4 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 21 PY 2016 VL 463 IS 1 BP 1057 EP 1067 DI 10.1093/mnras/stw2044 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA2YZ UT WOS:000386464900082 ER PT J AU de Haan, T Benson, BA Bleem, LE Allen, SW Applegate, DE Ashby, MLN Bautz, M Bayliss, M Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Chiu, I Cho, HM Clocchiatti, A Crawford, TM Crites, AT Desai, S Dietrich, JP Dobbs, MA Doucouliagos, AN Foley, RJ Forman, WR Garmire, GP George, EM Gladders, MD Gonzalez, AH Gupta, N Halverson, NW Hlavacek-Larrondo, J Hoekstra, H Holder, GP Holzapfel, WL Hou, Z Hrubes, JD Huang, N Jones, C Keisler, R Knox, L Lee, AT Leitch, EM von der Linden, A Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Meyer, SS Mocanu, LM Mohr, JJ Murray, SS Padin, S Pryke, C Rapetti, D Reichardt, CL Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Schrabback, T Shirokoff, E Song, J Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, KT Stubbs, CW Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zenteno, A AF de Haan, T. Benson, B. A. Bleem, L. E. Allen, S. W. Applegate, D. E. Ashby, M. L. N. Bautz, M. Bayliss, M. Bocquet, S. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chiu, I. Cho, H-M. Clocchiatti, A. Crawford, T. M. Crites, A. T. Desai, S. Dietrich, J. P. Dobbs, M. A. Doucouliagos, A. N. Foley, R. J. Forman, W. R. Garmire, G. P. George, E. M. Gladders, M. D. Gonzalez, A. H. Gupta, N. Halverson, N. W. Hlavacek-Larrondo, J. Hoekstra, H. Holder, G. P. Holzapfel, W. L. Hou, Z. Hrubes, J. D. Huang, N. Jones, C. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. von der Linden, A. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Meyer, S. S. Mocanu, L. M. Mohr, J. J. Murray, S. S. Padin, S. Pryke, C. Rapetti, D. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Schrabback, T. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. T. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zenteno, A. TI COSMOLOGICAL CONSTRAINTS FROM GALAXY CLUSTERS IN THE 2500 SQUARE-DEGREE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general ID SOUTH-POLE TELESCOPE; WEAK-LENSING MASSES; BACKGROUND POWER SPECTRUM; X-RAY-PROPERTIES; SUNYAEV-ZELDOVICH; SCALING RELATIONS; OBSERVED GROWTH; DARK ENERGY; VELOCITY DISPERSIONS; SPACE-TELESCOPE AB We present cosmological parameter constraints obtained from galaxy clusters identified by their SunyaevZel'dovich effect signature in the 2500 square-degree South Pole Telescope Sunyaev Zel'dovich (SPT-SZ) survey. We consider the 377 cluster candidates identified at z > 0.25 with a detection significance greater than five, corresponding to the 95% purity threshold for the survey. We compute constraints on cosmological models using the measured cluster abundance as a function of mass and redshift. We include additional constraints from multi-wavelength observations, including Chandra X-ray data for 82 clusters and a weak lensing-based prior on the normalization of the mass-observable scaling relations. Assuming a spatially flat Lambda CDM cosmology, we combine the cluster data with a prior on H-0 and find sigma(8)= 0.784. +/- 0.039 and Omega(m) = 0.289. +/- 0.042, with the parameter combination sigma(8) (Omega(m)/0.27)(0.3) = 0.797 +/- 0.031. These results are in good agreement with constraints from the cosmic microwave background (CMB) from SPT, WMAP, and Planck, as well as with constraints from other cluster data sets. We also consider several extensions to Lambda CDM, including models in which the equation of state of dark energy w, the species-summed neutrino mass, and/or the effective number of relativistic species (N-eff) are free parameters. When combined with constraints from the Planck CMB, H-0, baryon acoustic oscillation, and SNe, adding the SPT cluster data improves the w constraint by 14%, to w = -1.023 +/- 0.042. C1 [de Haan, T.; George, E. M.; Holzapfel, W. L.; Huang, N.; Lee, A. T.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Shirokoff, E.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mocanu, L. M.; Schaffer, K. K.; Shirokoff, E.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Bleem, L. E.; Carlstrom, J. E.; Hou, Z.; Keisler, R.; Meyer, S. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Bocquet, S.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Allen, S. W.; Keisler, R.; von der Linden, A.; Mantz, A.; Story, K. T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. [Allen, S. W.; Hlavacek-Larrondo, J.; Keisler, R.; von der Linden, A.; Mantz, A.; Story, K. T.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. [Applegate, D. E.; Schrabback, T.] Argelander Inst Astron, Auf Hugel 71, D-53121 Bonn, Germany. [Ashby, M. L. N.; Bayliss, M.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Bayliss, M.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Gupta, N.; Mohr, J. J.; Rapetti, D.; Saro, A.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Gupta, N.; Mohr, J. J.; Rapetti, D.; Saro, A.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, 5110 Rockhill Rd, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H-M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica, Dept Astron & Astrofis, Santiago, Region Metropol, Chile. [Crites, A. T.; Padin, S.; Williamson, R.] CALTECH, Pasadena, CA 91125 USA. [Doucouliagos, A. N.; Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Garmire, G. P.] Huntingdon Inst X Ray Astron LLC, Huntingdon, PA 16652 USA. [George, E. M.; Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.; Sayre, J. T.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.; Sayre, J. T.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hlavacek-Larrondo, J.] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada. [Hlavacek-Larrondo, J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [von der Linden, A.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [von der Linden, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Marrone, D. P.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Inst Chicago, Sch Art, Liberal Arts Dept, Chicago, IL 60603 USA. [Song, J.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [Zenteno, A.] Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. RP de Haan, T (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. OI Bocquet, Sebastian/0000-0002-4900-805X; Hoekstra, Henk/0000-0002-0641-3231; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF [PHY-1125897]; US Department of Energy [DE-AC02-76SF00515, DE-AC02-06CH11357]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Miller Research Fellowship; Natural Science and Engineering Research Council of Canada Postgraduate Scholarship-Doctoral award; Fermi Research Alliance, LLC [De-AC02-07CH11359]; United States Department of Energy; German Federal Ministry of Economics and Technology (BMWi) [50 OR 1210, 50 OR 1407]; Alfred P. Sloan Foundation; University of Melbourne; Australian Research Council [DP150103208]; NSERC; FRQNT; DFG Cluster of Excellence "Origin and Structure of the universe"; Transregio program TR33 "The Dark universe"; Danish National Research Foundation; NSF [ANT-1009649] FX The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation grant GBMF 947. This work used resources of McGill University's High Performance Computing centre, a part of Compute Canada. This work was supported in part by the Kavli Institute for Cosmological Physics at the University of Chicago through grant NSF PHY-1125897 and an endowment from the Kavli Foundation and its founder Fred Kavli. This work was supported in part by the US Department of Energy under contract number DE-AC02-76SF00515. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. TdH is supported by a Miller Research Fellowship, as well as receiving support from a Natural Science and Engineering Research Council of Canada Postgraduate Scholarship-Doctoral award. BB is supported by the Fermi Research Alliance, LLC under Contract No. De-AC02-07CH11359 with the United States Department of Energy. Argonne National Laboratorys work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. DA and TS acknowledge support from the German Federal Ministry of Economics and Technology (BMWi) provided through DLR under projects 50 OR 1210 and 50 OR 1407. RJF gratefully acknowledges support from the Alfred P. Sloan Foundation. CR acknowledges support from the University of Melbourne and from the Australian Research Council's Discovery Projects scheme (DP150103208). JHL is supported by NSERC through the discovery grant and Canada Research Chair programs, as well as FRQNT. The Munich group acknowledges the support of the DFG Cluster of Excellence "Origin and Structure of the universe" and the Transregio program TR33 "The Dark universe." The Dark Cosmology Centre is funded by the Danish National Research Foundation. Optical and infrared followup of SPT Clusters at the Harvard-Smithsonian Center for Astrophysics was supported by NSF grant ANT-1009649. NR 102 TC 3 Z9 3 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2016 VL 832 IS 1 AR 95 DI 10.3847/0004-637X/832/1/95 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED3IW UT WOS:000388743800025 ER PT J AU Kreidberg, L Loeb, A AF Kreidberg, Laura Loeb, Abraham TI PROSPECTS FOR CHARACTERIZING THE ATMOSPHERE OF PROXIMA CENTAURI b SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (Proxima Centauri b) ID THERMAL PHASE CURVES; EARTH-LIKE PLANETS; TIDALLY LOCKED EXOPLANETS; TERRESTRIAL PLANETS; M-DWARFS; HABITABLE PLANETS; M STARS; CIRCULATION; SPECTROSCOPY; ROTATION AB The newly detected Earth-mass planet in the habitable zone of Proxima Centauri could potentially host life-if it has an atmosphere that supports surface liquid water. We show that thermal phase curve observations with the James Webb Space Telescope (JWST) from 5-12 mu m can be used to test for the existence of such an atmosphere. We predict the thermal variation for a bare rock versus a planet with 35% heat redistribution to the nightside and show that a JWST phase curve measurement can distinguish between these cases at 4 sigma confidence, assuming photon-limited precision. We also consider the case of an Earth-like atmosphere, and find that the 9.8 mu m ozone band could be detected with longer integration times (a few months). We conclude that JWST observations have the potential to put the first constraints on the possibility of life around the the solar system's nearest star. C1 [Kreidberg, Laura] Harvard Univ, 78 Mt Auburn St, Cambridge, MA 02138 USA. [Kreidberg, Laura; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Kreidberg, L (reprint author), Harvard Univ, 78 Mt Auburn St, Cambridge, MA 02138 USA. EM laura.kreidberg@cfa.harvard.edu NR 52 TC 2 Z9 2 U1 9 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2016 VL 832 IS 1 AR L12 DI 10.3847/2041-8205/832/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED1VC UT WOS:000388632000005 ER PT J AU Leiner, E Mathieu, RD Stello, D Vanderburg, A Sandquist, E AF Leiner, Emily Mathieu, Robert D. Stello, Dennis Vanderburg, Andrew Sandquist, Eric TI THE K2 M67 STUDY: AN EVOLVED BLUE STRAGGLER IN M67 FROM K2 MISSION ASTEROSEISMOLOGY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE asteroseismology; binaries: spectroscopic; blue stragglers; open clusters and associations: individual (M67); stars: evolution ID OPEN CLUSTER M67; MASS-TRANSFER; WHITE-DWARF; RED GIANTS; NGC 6791; STELLAR COLLISIONS; GLOBULAR-CLUSTERS; MAIN-SEQUENCE; BINARIES; PHOTOMETRY AB Yellow straggler stars (YSSs) fall above the subgiant branch in optical color-magnitude diagrams (CMDs), between the blue stragglers and the red giants. YSSs may represent a population of evolved blue stragglers, but none have the direct and precise mass and radius measurements needed to determine their evolutionary states and formation histories. Here we report the first asteroseismic mass and radius measurements of such a star, the yellow straggler S1237 in the open cluster M67. We apply asteroseismic scaling relations to a frequency analysis of the Kepler K2 light curve and find a mass of 2.9 +/- 0.2 M-circle dot and a radius of 9.2 +/- 0.2 R-circle dot This is more than twice the mass of the main-sequence turnoff in M67, suggesting that S1237 is indeed an evolved blue straggler. S1237 is the primary in a spectroscopic binary. We update the binary orbital solution and use spectral energy distribution fitting to constrain the CMD location of the secondary star. We find that the secondary is likely an upper main-sequence star near the turnoff, but a slightly hotter blue straggler companion is also possible. We then compare the asteroseismic mass of the primary to its mass from CMD fitting, finding that the photometry implies a mass and radius more than 2 sigma below the asteroseismic measurement. Finally, we consider formation mechanisms for this star and suggest that S1237 may have formed from dynamical encounters resulting in stellar collisions or a binary merger. C1 [Leiner, Emily; Mathieu, Robert D.] Univ Wisconsin, Dept Astron, 475 North Charter St, Madison, WI 53706 USA. [Stello, Dennis] Univ Sydney, Sydney Inst Astron SIfA, Sch Phys, Sydney, NSW 2006, Australia. [Stello, Dennis] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Stello, Dennis] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia. [Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sandquist, Eric] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Leiner, E (reprint author), Univ Wisconsin, Dept Astron, 475 North Charter St, Madison, WI 53706 USA. EM leiner@astro.wisc.edu OI Stello, Dennis/0000-0002-4879-3519; Vanderburg, Andrew/0000-0001-7246-5438 FU NASA Science Mission directorate; NASA [NNX15AW69G]; Wisconsin Space Grant Consortium; NSF [DGE 1144152] FX This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate.; E.L. and R.M. are supported by NASA Grant NNX15AW69G. E.L. is also funded by the Wisconsin Space Grant Consortium. A.V. is supported by the NSF Graduate Research Fellowship, grant No. DGE 1144152. NR 43 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 20 PY 2016 VL 832 IS 1 AR L13 DI 10.3847/2041-8205/832/1/L13 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED1VC UT WOS:000388632000006 ER PT J AU Tahani, K Plume, R Bergin, EA Tolls, V Phillips, TG Caux, E Cabrit, S Goicoechea, JR Goldsmith, PF Johnstone, D Lis, DC Pagani, L Menten, KM Muller, HSP Ossenkopf-Okada, V Pearson, JC van der Tak, FFS AF Tahani, K. Plume, R. Bergin, E. A. Tolls, V. Phillips, T. G. Caux, E. Cabrit, S. Goicoechea, J. R. Goldsmith, P. F. Johnstone, D. Lis, D. C. Pagani, L. Menten, K. M. Mueller, H. S. P. Ossenkopf-Okada, V. Pearson, J. C. van der Tak, F. F. S. TI ANALYSIS OF THE HERSCHEL/HEXOS SPECTRAL SURVEY TOWARD ORION SOUTH: A MASSIVE PROTOSTELLAR ENVELOPE WITH STRONG EXTERNAL IRRADIATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (Orion South); ISM: kinematics and dynamics; ISM: lines and bands; ISM: molecules ID MOLECULAR LINE SURVEY; EXTRAORDINARY SOURCES ANALYSIS; LIMITED MILLIMETER SURVEY; STAR-FORMING REGIONS; CLOUD CORES; MU-M; SUBMILLIMETER ARRAY; OBSERVATIONAL DATA; INTERSTELLAR JETS; ODIN SATELLITE AB We present results from a comprehensive submillimeter spectral survey toward the source Orion South, based on data obtained with the Heterodyne Instrument for the Far-Infrared instrument on board the Herschel Space Observatory, covering the frequency range of 480 to 1900 GHz. We detect 685 spectral lines with signal-to-noise ratios (S/Ns) > 3 sigma, originating from 52 different molecular and atomic species. We model each of the detected species assuming conditions of Local Thermodynamic Equilibrium. This analysis provides an estimate of the physical conditions of Orion South (column density, temperature, source size, and VLSR). We find evidence for three different cloud components: a cool (T-ex similar to 20-40 K), spatially extended (> 60 ''), and quiescent (Delta V-FWHM similar to 4 km s(-1)) component; a warmer (T-ex similar to 80-100 K), less spatially extended (similar to 30 ''), and dynamic (Delta V-FWHM similar to 8 km s(-1)) component, which is likely affected by embedded outflows; and a kinematically distinct region (T-ex > 100 K; V-LSR similar to 8 km s(-1)), dominated by emission from species that trace ultraviolet irradiation, likely at the surface of the cloud. We find little evidence for the existence of a chemically distinct "hot-core" component, likely due to the small filling factor of the hot core or hot cores within the Herschel beam. We find that the chemical composition of the gas in the cooler, quiescent component of Orion South more closely resembles that of the quiescent ridge in Orion-KL. The gas in the warmer, dynamic component, however, more closely resembles that of the Compact Ridge and Plateau regions of Orion-KL, suggesting that higher temperatures and shocks also have an influence on the overall chemistry of Orion South. C1 [Tahani, K.; Plume, R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Bergin, E. A.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. [Tolls, V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Phillips, T. G.; Lis, D. C.] CALTECH, Cahill Ctr Astron & Astrophys 301 17, Pasadena, CA 91125 USA. [Caux, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse, France. [Caux, E.] IRAP, CNRS, 9 Av Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Cabrit, S.; Lis, D. C.; Pagani, L.] UPMC Univ Paris 06, Sorbonne Univ, PSL Res Univ, LERMA,Observ Paris,CNRS, F-75014 Paris, France. [Goicoechea, J. R.] CSIC, Inst Ciencia Mat Madrid, Sor Juana Ines de la Cruz 3, E-28049 Madrid, Spain. [Goldsmith, P. F.; Pearson, J. C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Johnstone, D.] Natl Res Council Canada, Herzberg Inst Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. [Menten, K. M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Mueller, H. S. P.] Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. [van der Tak, F. F. S.] SRON Netherlands Inst Space Res, POB 800, NL-9700 AV Groningen, Netherlands. [van der Tak, F. F. S.] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands. RP Tahani, K (reprint author), Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. EM ktahani@ucalgary.ca FU Deutsche Forschungsgemeinschaft (DFG) [SFB 956]; ERC; Spanish MINECO [ERC-2013-Syg-610256, AYA2012-32032]; National Sciences and Engineering Research Council of Canada (NSERC); NASA FX HIFI was designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of the SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri- INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronmico Nacional (IGN), Centro de Astrobiologa (CSIC-INTA). Sweden: Chalmers University of Technology-MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University-Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. We also need to acknowledge the support by the Deutsche Forschungsgemeinschaft (DFG) via the collaborative research grant SFB 956, project C1 & C3, as well as the ERC and the Spanish MINECO for funding support under grants ERC-2013-Syg-610256 and AYA2012-32032. Support for this work was provided, in part, by a National Sciences and Engineering Research Council of Canada (NSERC) grant to R. Plume and K. Tahani and by NASA through an award issued by JPL/Caltech. This work was carried out in part at the Jet Propulsion Laboratory, which is operated for NASA by the California Institute of Technology. NR 94 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2016 VL 832 IS 1 AR 12 DI 10.3847/0004-637X/832/1/12 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC5US UT WOS:000388203200001 ER PT J AU Crepp, JR Gonzales, EJ Bechter, EB Montet, BT Johnson, JA Piskorz, D Howard, AW Isaacson, H AF Crepp, Justin R. Gonzales, Erica J. Bechter, Eric B. Montet, Benjamin T. Johnson, John Asher Piskorz, Danielle Howard, Andrew W. Isaacson, Howard TI THE TRENDS HIGH-CONTRAST IMAGING SURVEY. VI. DISCOVERY OF A MASS, AGE, AND METALLICITY BENCHMARK BROWN DWARF SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; stars: individual (HD 4747); techniques: high angular resolution; techniques: radial velocities ID GEMINI PLANET IMAGER; SOLAR-TYPE STARS; GIANT PLANETS; T-DWARFS; HD 19467; COMPANION; I.; SEARCH; MULTIPLICITY; EXOPLANET AB The mass and age of substellar objects are degenerate parameters leaving the evolutionary state of brown dwarfs ambiguous without additional information. Theoretical models are normally used to help distinguish between old, massive brown dwarfs and young, low-mass brown dwarfs but these models have yet to be properly calibrated. We have carried out an infrared high-contrast imaging program with the goal of detecting substellar objects as companions to nearby stars to help break degeneracies in inferred physical properties such as mass, age, and composition. Rather than using imaging observations alone, our targets are pre-selected based on the existence of dynamical accelerations informed from years of stellar radial velocity (RV) measurements. In this paper, we present the discovery of a rare benchmark brown dwarf orbiting the nearby (d = 18.69 +/- 0.19 pc), solar-type (G9V) star HD. 4747 ([Fe/H] = -0.22 +/- 0.04) with a projected separation of only rho = 11.3 +/- 0.2 au (theta = 0.'' 6). Precise Doppler measurements taken over 18 years reveal the companion's orbit and allow us to place strong constraints on its mass using dynamics (msini=55.3. 1.9M(Jup)). Relative photometry (Delta K-s = 9.05 +/- 0.14, M-Ks= 13.00 +/- 0.14, K-s - L' = 1.34 +/- 0.46) indicates that HD. 4747. B is most likely a late-type L-dwarf and, if near the L/T transition, an intriguing source for studying cloud physics, variability, and polarization. We estimate a model-dependent mass of m = 72(-13)(+3) M-Jup for an age of 3.3(-1.9)(+2.3) Gyr based on gyrochronology. Combining astrometric measurements with RV data, we calculate the companion dynamical mass (m = 60.2 +/- 3.3M(Jup)) and orbit (e = 0.740 +/- 0.002) directly. As a new mass, age, and metallicity benchmark, HD 4747 B will serve as a laboratory for precision astrophysics to test theoretical models that describe the emergent radiation of brown dwarfs. C1 [Crepp, Justin R.; Gonzales, Erica J.; Bechter, Eric B.] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. [Montet, Benjamin T.; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Montet, Benjamin T.; Piskorz, Danielle] CALTECH, Div Geol & Planetary Sci, 1200 E Calif Blvd, Pasadena, CA 91125 USA. [Howard, Andrew W.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Crepp, JR (reprint author), Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA. EM jcrepp@nd.edu OI Montet, Benjamin/0000-0001-7516-8308; Isaacson, Howard/0000-0002-0531-1073 FU National Science Foundation Graduate Research Fellowship [DGE-1144469]; NASA Origins [NNX13AB03G]; PI Crepp's NASA Early Career Fellowship; W. M. Keck Foundation; NASA Keck PI Data Award FX We thank the many California Planet Search observers for help over the years securing precise RV measurements that ultimately led to the direct imaging discovery of HD 4747 B. Chris Matthews estimated the L' apparent magnitude of HD 4747. A by fitting an SED to its flux measured at visible and near-infrared wavelengths. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144469. The TRENDS high-contrast imaging program is supported in part by NASA Origins grant NNX13AB03G and PI Crepp's NASA Early Career Fellowship. We are also grateful for the vision and support of the Potenziani family. NR 45 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2016 VL 831 IS 2 AR 136 DI 10.3847/0004-637X/831/2/136 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC0LM UT WOS:000387792500022 ER PT J AU Kozarev, KA Schwadron, NA AF Kozarev, Kamen A. Schwadron, Nathan A. TI A DATA-DRIVEN ANALYTIC MODEL FOR PROTON ACCELERATION BY LARGE-SCALE SOLAR CORONAL SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; shock waves; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: particle emission ID PARTICLE-ACCELERATION; COMPRESSION REGIONS; CHARGED-PARTICLES; WAVE; SDO/AIA; SIMULATIONS; PROPAGATION; FRONTS; EVENT; EUV AB We have recently studied the development of an eruptive filament-driven, large-scale off-limb coronal bright front (OCBF) in the low solar corona, using remote observations from the Solar Dynamics Observatory's Advanced Imaging Assembly EUV telescopes. In that study, we obtained high-temporal resolution estimates of the OCBF parameters regulating the efficiency of charged particle acceleration within the theoretical framework of diffusive shock acceleration (DSA). These parameters include the time-dependent front size, speed, and strength, as well as the upstream coronal magnetic field orientations with respect to the front's surface normal direction. Here we present an analytical particle acceleration model, specifically developed to incorporate the coronal shock/ compressive front properties described above, derived from remote observations. We verify the model's performance through a grid of idealized case runs using input parameters typical for large-scale coronal shocks, and demonstrate that the results approach the expected DSA steady-state behavior. We then apply the model to the event of 2011 May 11 using the OCBF time-dependent parameters derived by Kozarev et al. We find that the compressive front likely produced energetic particles as low as 1.3 solar radii in the corona. Comparing the modeled and observed fluences near Earth, we also find that the bulk of the acceleration during this event must have occurred above 1.5 solar radii. With this study we have taken a first step in using direct observations of shocks and compressions in the innermost corona to predict the onsets and intensities of solar energetic particle events. C1 [Kozarev, Kamen A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Schwadron, Nathan A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. RP Kozarev, KA (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI Kozarev, Kamen/0000-0002-6591-4482 FU CASHeW (NASA GI) project [NNX15AN41G S01]; C-SWEPA (NASA) project [NNX13AI75G]; Sun-2-Ice (NSF) project [AGS1135432]; DREAM2 (NASA) [NNX14AG13A] FX The authors thank the referee for the insightful comments that improved the manuscript. K.A.K. was supported by the CASHeW (NASA GI grant number NNX15AN41G S01) project. N.A.S. was supported by C-SWEPA (NASA grant number NNX13AI75G), Sun-2-Ice (NSF grant number AGS1135432) projects, and DREAM2 (NASA grant NNX14AG13A). The authors thank Maher Al Dayeh for providing the SOHO/ERNE data. NR 40 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 20 PY 2016 VL 831 IS 2 AR 120 DI 10.3847/0004-637X/831/2/120 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC0LM UT WOS:000387792500006 ER PT J AU Jacob, DJ Turner, AJ Maasakkers, JD Sheng, JX Sun, K Liu, X Chance, K Aben, I McKeever, J Frankenberg, C AF Jacob, Daniel J. Turner, Alexander J. Maasakkers, Joannes D. Sheng, Jianxiong Sun, Kang Liu, Xiong Chance, Kelly Aben, Ilse McKeever, Jason Frankenberg, Christian TI Satellite observations of atmospheric methane and their value for quantifying methane emissions SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID HIGH-SPATIAL-RESOLUTION; NATURAL-GAS PRODUCTION; BARNETT SHALE REGION; GEOS-CHEM; TROPOSPHERIC METHANE; CH4 EMISSIONS; TRACE GASES; TANSO-FTS; ANTHROPOGENIC EMISSIONS; SENTINEL-5 PRECURSOR AB Methane is a greenhouse gas emitted by a range of natural and anthropogenic sources. Atmospheric methane has been measured continuously from space since 2003, and new instruments are planned for launch in the near future that will greatly expand the capabilities of space-based observations. We review the value of current, future, and proposed satellite observations to better quantify and understand methane emissions through inverse analyses, from the global scale down to the scale of point sources and in combination with suborbital (surface and aircraft) data. Current global observations from Greenhouse Gases Observing Satellite (GOSAT) are of high quality but have sparse spatial coverage. They can quantify methane emissions on a regional scale (100-1000 km) through multiyear averaging. The Tropospheric Monitoring Instrument (TROPOMI), to be launched in 2017, is expected to quantify daily emissions on the regional scale and will also effectively detect large point sources. A different observing strategy by GHGSat (launched in June 2016) is to target limited viewing domains with very fine pixel resolution in order to detect a wide range of methane point sources. Geostationary observation of methane, still in the proposal stage, will have the unique capability of mapping source regions with high resolution, detecting transient "super-emitter" point sources and resolving diurnal variation of emissions from sources such as wetlands and manure. Exploiting these rapidly expanding satellite measurement capabilities to quantify methane emissions requires a parallel effort to construct high-quality spatially and sectorally resolved emission inventories. Partnership between top-down inverse analyses of atmospheric data and bottom-up construction of emission inventories is crucial to better understanding methane emission processes and subsequently informing climate policy. C1 [Jacob, Daniel J.; Turner, Alexander J.; Maasakkers, Joannes D.; Sheng, Jianxiong] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Sun, Kang; Liu, Xiong; Chance, Kelly] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Aben, Ilse] SRON Netherlands Inst Space Res, NL-3584 Utrecht, Netherlands. [McKeever, Jason] GHGSat Inc, Montreal, PQ H2W 1Y5, Canada. [Frankenberg, Christian] CALTECH, Pasadena, CA 91125 USA. RP Jacob, DJ (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM djacob@fas.harvard.edu RI Liu, Xiong/P-7186-2014; Chem, GEOS/C-5595-2014; Frankenberg, Christian/A-2944-2013 OI Liu, Xiong/0000-0003-2939-574X; Frankenberg, Christian/0000-0002-0546-5857 FU NASA Carbon Monitoring System; NASA GEO-CAPE Atmospheric Sciences Working Group; ExxonMobil Upstream Research Company; US DOE Advanced Research Projects Agency - Energy; Smithsonian Astrophysical Observatory FX This work was funded by the NASA Carbon Monitoring System, by the NASA GEO-CAPE Atmospheric Sciences Working Group, by the ExxonMobil Upstream Research Company, and by the US DOE Advanced Research Projects Agency - Energy. Kelly Chance acknowledges funding from the Smithsonian Astrophysical Observatory. We thank Helen Worden for pointing out an error in the original submitted paper. NR 134 TC 1 Z9 1 U1 31 U2 31 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD NOV 18 PY 2016 VL 16 IS 22 BP 14371 EP 14396 DI 10.5194/acp-16-14371-2016 PG 26 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EC2UQ UT WOS:000387980100003 ER PT J AU Pichler, H Zhu, GY Seif, A Zoller, P Hafezi, M AF Pichler, Hannes Zhu, Guanyu Seif, Alireza Zoller, Peter Hafezi, Mohammad TI Measurement Protocol for the Entanglement Spectrum of Cold Atoms SO PHYSICAL REVIEW X LA English DT Article ID ONE-DIMENSIONAL SYSTEMS; MANY-BODY SYSTEM; QUANTUM ENTANGLEMENT; OPTICAL LATTICES; ENTROPY; TRANSITION; STATES; PHASE; MODEL; CHAIN AB Entanglement, and, in particular, the entanglement spectrum, plays a major role in characterizing many-body quantum systems. While there has been a surge of theoretical works on the subject, no experimental measurement has been performed to date because of the lack of an implementable measurement scheme. Here, we propose a measurement protocol to access the entanglement spectrum of many-body states in experiments with cold atoms in optical lattices. Our scheme effectively performs a Ramsey spectroscopy of the entanglement Hamiltonian and is based on the ability to produce several copies of the state under investigation, together with the possibility to perform a global swap gate between two copies conditioned on the state of an auxiliary qubit. We show how the required conditional swap gate can be implemented with cold atoms, either by using Rydberg interactions or coupling the atoms to a cavity mode. We illustrate these ideas on a simple (extended) Bose-Hubbard model where such a measurement protocol reveals topological features of the Haldane phase. C1 [Pichler, Hannes] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Pichler, Hannes] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Pichler, Hannes; Zoller, Peter] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. [Zhu, Guanyu; Seif, Alireza; Hafezi, Mohammad] Univ Maryland, NIST, Joint Quantum Inst, College Pk, MD 20742 USA. [Zoller, Peter] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Hafezi, Mohammad] Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Hafezi, Mohammad] Univ Maryland, Dept Elect & Comp Engn, College Pk, MD 20742 USA. [Hafezi, Mohammad] Univ Maryland, Inst Res Elect & Appl Phys, College Pk, MD 20742 USA. RP Pichler, H (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA.; Pichler, H (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA.; Pichler, H (reprint author), Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. EM hannes.pichler@cfa.harvard.edu; gzhu123@umd.edu RI Zoller, Peter/O-1639-2014; Pichler, Hannes/M-5150-2015 OI Zoller, Peter/0000-0003-4014-1505; Pichler, Hannes/0000-0003-2144-536X FU NSF [PHY11-25915]; Smithsonian Astrophysical Observatory; ERC; Austrian Science Fund through SFB FOQUS; EU; ONR-YIP at the Joint Quantum Institute; ARO-MURI at the Joint Quantum Institute; AFOSR at the Joint Quantum Institute; NSF-PFC at the Joint Quantum Institute; Sloan Foundation FX We thank L. Bonnes, E. Kapit, A. M. Lauchli, M. Ozols, A. Sterdyniak, A. Turner, and F. Verstraete for useful discussions. H. P. was supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory. The work at Innsbruck is supported by the ERC Synergy Grant UQUAM, the Austrian Science Fund through SFB FOQUS, and the EU FET Proactive Initiative SIQS and RYQS. The work at the University of Maryland was supported by ONR-YIP, ARO-MURI, AFOSR, NSF-PFC at the Joint Quantum Institute, and the Sloan Foundation. Kavli Institute for Theoretical Physics is supported by NSF PHY11-25915. NR 72 TC 3 Z9 3 U1 6 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2160-3308 J9 PHYS REV X JI Phys. Rev. X PD NOV 17 PY 2016 VL 6 IS 4 AR 041033 DI 10.1103/PhysRevX.6.041033 PG 12 WC Physics, Multidisciplinary SC Physics GA EC6XM UT WOS:000388280000002 ER PT J AU Tanner, EVJ Sheldrake, MWA Turner, BL AF Tanner, Edmund Vincent John Sheldrake, Merlin W. A. Turner, Benjamin L. TI Changes in soil carbon and nutrients following 6 years of litter removal and addition in a tropical semi-evergreen rain forest SO BIOGEOSCIENCES LA English DT Article ID ATMOSPHERIC CO2 ENRICHMENT; ORGANIC-MATTER; PINE FOREST; CLIMATE; SEQUESTRATION; MANIPULATION; DYNAMICS; CONSTRAINTS; RESPONSES; TURNOVER AB Increasing atmospheric CO2 and temperature may increase forest productivity, including litterfall, but the consequences for soil organic matter remain poorly understood. To address this, we measured soil carbon and nutrient concentrations at nine depths to 2 m after 6 years of continuous litter removal and litter addition in a semi-evergreen rain forest in Panama. Soils in litter addition plots, compared to litter removal plots, had higher pH and contained greater concentrations of KCl-extractable nitrate (both to 30 cm); Mehlich-III extractable phosphorus and total carbon (both to 20 cm); total nitrogen (to 15 cm); Mehlich-III calcium (to 10 cm); and Mehlich-III magnesium and lower bulk density (both to 5 cm). In contrast, litter manipulation did not affect ammonium, manganese, potassium or zinc, and soils deeper than 30 cm did not differ for any nutrient. Comparison with previous analyses in the experiment indicates that the effect of litter manipulation on nutrient concentrations and the depth to which the effects are significant are increasing with time. To allow for changes in bulk density in calculation of changes in carbon stocks, we standardized total carbon and nitrogen on the basis of a constant mineral mass. For 200 kg m(-2) of mineral soil (approximately the upper 20 cm of the profile) about 0.5 kg C m(-2) was "missing" from the litter removal plots, with a similar amount accumulated in the litter addition plots. There was an additional 0.4 kg C m(-2) extra in the litter standing crop of the litter addition plots compared to the control. This increase in carbon in surface soil and the litter standing crop can be interpreted as a potential partial mitigation of the effects of increasing CO2 concentrations in the atmosphere. C1 [Tanner, Edmund Vincent John; Sheldrake, Merlin W. A.] Univ Cambridge, Dept Plant Sci, Downing St, Cambridge CB2 3EA, England. [Tanner, Edmund Vincent John; Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. RP Tanner, EVJ (reprint author), Univ Cambridge, Dept Plant Sci, Downing St, Cambridge CB2 3EA, England.; Tanner, EVJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM evt1@cam.ac.uk RI Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Mellon Foundation; Gates Cambridge Trust; University of Cambridge Domestic Research Studentship Scheme; Wolfson College Alice Evans Fund; Drummond Fund of Gonville; Caius College; Cambridge University FX We thank J. Bee, L. Hayes, S. Queenborough, R. Upson and M. Vorontsova for surveying the plots, J. Bee for setting up the experiment in 2000 and 2001; E. Sayer for running the experiment from 2001-2009; A. Vincent for helping to maintain the experiment from 2003-2005. T. Jucker did the statistics to compare the effect of treatment on soil C relative to mineral matter. Funding for the project was originally from the Mellon Foundation (1999-2002); ongoing costs were paid for by the Gates Cambridge Trust (E. Sayer); The University of Cambridge Domestic Research Studentship Scheme and the Wolfson College Alice Evans Fund (A. Vincent); and The Drummond Fund of Gonville and Caius College and Cambridge University (E. Tanner). The whole of the experiment depended on the continuous raking of litter, which was done by Jesus Valdez and Francisco Valdez. We thank D. Agudo and T. Romero for doing the laboratory work and J. Rodriguez for collecting the samples in the forest. S. J. Wright has been a frequent source of help for many aspects of the experiment. NR 35 TC 0 Z9 0 U1 31 U2 31 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 EI 1726-4189 J9 BIOGEOSCIENCES JI Biogeosciences PD NOV 17 PY 2016 VL 13 IS 22 BP 6183 EP 6190 DI 10.5194/bg-13-6183-2016 PG 8 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA EC1KX UT WOS:000387864700001 ER PT J AU Kennedy, EV Tonk, L Foster, NL Chollett, I Ortiz, JC Dove, S Hoegh-Guldberg, O Mumby, PJ Stevens, JR AF Kennedy, Emma V. Tonk, Linda Foster, Nicola L. Chollett, Iliana Ortiz, Juan-Carlos Dove, Sophie Hoegh-Guldberg, Ove Mumby, Peter J. Stevens, Jamie R. TI Symbiodinium biogeography tracks environmental patterns rather than host genetics in a key Caribbean reef-builder, Orbicella annularis SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE symbiont diversity; Zooxanthellae; environmental drivers; coral bleaching; denaturing gel gradient electrophoresis; Internal Transcribed Spacer 2 ID MONTASTRAEA-ANNULARIS; GENUS SYMBIODINIUM; CORAL ENDOSYMBIONTS; SPECIES COMPLEX; INDO-PACIFIC; DIVERSITY; POPULATIONS; ECOLOGY; SPECIFICITY; COMMUNITIES AB The physiological performance of a reef-building coral is a combined outcome of both the coral host and its algal endosymbionts, Symbiodinium. While Orbicella annularis-a dominant reef-building coral in the Wider Caribbean-is known to be a flexible host in terms of the diversity of Symbiodinium types it can associate with, it is uncertain how this diversity varies across the Caribbean, and whether spatial variability in the symbiont community is related to either O. annularis genotype or environment. Here, we target the Symbiodinium-ITS2 gene to characterize and map dominant Symbiodinium hosted by O. annularis at an unprecedented spatial scale. We reveal northwest-southeast partitioning across the Caribbean, both in terms of the dominant symbiont taxa hosted and in assemblage diversity. Multivariate regression analyses incorporating a suite of environmental and genetic factors reveal that observed spatial patterns are predominantly explained by chronic thermal stress (summer temperatures) and are unrelated to host genotype. Furthermore, we were able to associate the presence of specific Symbiodinium types with local environmental drivers (for example, Symbiodinium C7 with areas experiencing cooler summers, B1j with nutrient loading and B17 with turbidity), associations that have not previously been described. C1 [Kennedy, Emma V.; Foster, Nicola L.; Mumby, Peter J.; Stevens, Jamie R.] Univ Exeter, Coll Life & Environm Sci, Stocker Rd, Exeter EX4 4QD, Devon, England. [Kennedy, Emma V.] Griffith Univ, Australian Rivers Inst, Nathan, Qld 4111, Australia. [Tonk, Linda; Dove, Sophie; Hoegh-Guldberg, Ove] Univ Queensland, Sch Biol Sci, Coral Reef Ecosyst Lab, St Lucia, Qld 4072, Australia. [Foster, Nicola L.] Univ Plymouth, Sch Marine Sci & Engn, Plymouth PL4 8AA, Devon, England. [Chollett, Iliana] Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Ortiz, Juan-Carlos; Mumby, Peter J.] Univ Queensland, Sch Biol Sci, Marine Spatial Ecol Lab, St Lucia, Qld 4072, Australia. RP Kennedy, EV (reprint author), Univ Exeter, Coll Life & Environm Sci, Stocker Rd, Exeter EX4 4QD, Devon, England.; Kennedy, EV (reprint author), Griffith Univ, Australian Rivers Inst, Nathan, Qld 4111, Australia. EM emma.kennedy@griffith.edu.au RI Kennedy, Emma/M-3193-2014; OI Kennedy, Emma/0000-0003-1821-9740; Stevens, Jamie/0000-0002-1317-6721 FU NERC [NE/E010393/1]; European Union [244161]; University of Exeter FX This project was funded primarily by an NERC grant, no. NE/E010393/1 (J.R.S. and P.J.M.), European Union FP7 project Future of Reefs in a Changing Environment (FORCE) under grant agreement no. 244161 (P.J.M. and J.R.S.) and a University of Exeter studentship (E.V.K.). NR 44 TC 0 Z9 0 U1 8 U2 8 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD NOV 16 PY 2016 VL 283 IS 1842 AR 20161938 DI 10.1098/rspb.2016.1938 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA ED2ZL UT WOS:000388718700012 ER PT J AU Kao, DM Lai, AG Stamataki, E Rosic, S Konstantinides, N Jarvis, E Di Donfrancesco, A Pouchkina-Stancheva, N Semon, M Grillo, M Bruce, H Kumar, S Siwanowicz, I Le, A Lemire, A Eisen, MB Extavour, C Browne, WE Wolff, C Averof, M Patel, NH Sarkies, P Pavlopoulos, A Aboobaker, A AF Kao, Damian Lai, Alvina G. Stamataki, Evangelia Rosic, Silvana Konstantinides, Nikolaos Jarvis, Erin Di Donfrancesco, Alessia Pouchkina-Stancheva, Natalia Semon, Marie Grillo, Marco Bruce, Heather Kumar, Suyash Siwanowicz, Igor Le, Andy Lemire, Andrew Eisen, Michael B. Extavour, Cassandra Browne, William E. Wolff, Carsten Averof, Michalis Patel, Nipam H. Sarkies, Peter Pavlopoulos, Anastasios Aboobaker, Aziz TI The genome of the crustacean Parhyale hawaiensis, a model for animal development, regeneration, immunity and lignocellulose digestion SO ELIFE LA English DT Article ID DNA METHYLATION PATTERNS; HOX GENE-EXPRESSION; SYNDROME-VIRUS WSSV; AMPHIPOD CRUSTACEAN; PANCRUSTACEAN PHYLOGENY; DROSOPHILA-MELANOGASTER; HOMEOBOX GENES; DAPHNIA-PULEX; SEQUENCE DATA; CELL LINEAGE AB The amphipod crustacean Parhyale hawaiensis is a blossoming model system for studies of developmental mechanisms and more recently regeneration. We have sequenced the genome allowing annotation of all key signaling pathways, transcription factors, and non-coding RNAs that will enhance ongoing functional studies. Parhyale is a member of the Malacostraca clade, which includes crustacean food crop species. We analysed the immunity related genes of Parhyale as an important comparative system for these species, where immunity related aquaculture problems have increased as farming has intensified. We also find that Parhyale and other species within Multicrustacea contain the enzyme sets necessary to perform lignocellulose digestion ('wood eating'), suggesting this ability may predate the diversification of this lineage. Our data provide an essential resource for further development of Parhyale as an experimental model. The first malacostracan genome will underpin ongoing comparative work in food crop species and research investigating lignocellulose as an energy source. C1 [Kao, Damian; Lai, Alvina G.; Di Donfrancesco, Alessia; Pouchkina-Stancheva, Natalia; Aboobaker, Aziz] Univ Oxford, Dept Zool, Oxford, England. [Stamataki, Evangelia; Kumar, Suyash; Siwanowicz, Igor; Le, Andy; Lemire, Andrew; Pavlopoulos, Anastasios] Howard Hughes Med Inst, Janelia Farm Res Campus, Ashburn, VA 20147 USA. [Rosic, Silvana; Sarkies, Peter] Imperial Coll London, MRC Clin Sci Ctr, London, England. [Rosic, Silvana; Sarkies, Peter] Imperial Coll London, Clin Sci, London, England. [Konstantinides, Nikolaos; Semon, Marie; Grillo, Marco; Averof, Michalis] CNRS, Genom Fonct Lyon 5Inst, Lyon, France. [Konstantinides, Nikolaos; Semon, Marie; Grillo, Marco; Averof, Michalis] Ecole Normale Super Lyon, Lyon, France. [Jarvis, Erin; Bruce, Heather; Patel, Nipam H.] Univ Calif Berkeley, Dept Mol & Cell Biol, Berkeley, CA 94720 USA. [Eisen, Michael B.] Univ Calif Berkeley, Howard Hughes Med Inst, Mol & Cell Biol, Berkeley, CA 94720 USA. [Extavour, Cassandra] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Browne, William E.] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC USA. [Wolff, Carsten] Humboldt Univ, Inst Biol, Vergleichende Zool, Berlin, Germany. RP Aboobaker, A (reprint author), Univ Oxford, Dept Zool, Oxford, England.; Pavlopoulos, A (reprint author), Howard Hughes Med Inst, Janelia Farm Res Campus, Ashburn, VA 20147 USA. EM pavlopoulosa@janelia.hhmi.org; aziz.aboobaker@zoo.ox.ac.uk FU Biotechnology and Biological Sciences Research Council [BB/K007564/1]; Medical Research Council [MR/M000133/1, MRC MC-A652-5PZ80]; Human Frontier Science Program; University of Oxford; Howard Hughes Medical Institute; Agence Nationale de la Recherche [ANR-12-CHEX-0001-01]; National Science Foundation [IOS-1257379]; Imperial College London; John Fell Fund, University of Oxford FX Biotechnology and Biological Sciences Research Council BB/K007564/1 Damian Kao Alvina G Lai Alessia Di Donfrancesco Natalia Pouchkina-Stancheva Aziz Aboobaker; Medical Research Council MR/M000133/1 Damian Kao Alvina G Lai Alessia Di Donfrancesco Natalia Pouchkina-Stancheva Aziz Aboobaker; Human Frontier Science Program Alvina G Lai; University of Oxford Elizabeth Hannah Jenkinson Fund Alvina G Lai Aziz Aboobaker; Howard Hughes Medical Institute Evangelia Stamataki Suyash Kumar Igor Siwanowicz Andy Le Andrew Lemire Michael B Eisen; Medical Research Council MRC MC-A652-5PZ80 Silvana Rosic Peter Sarkies; Agence Nationale de la Recherche ANR-12-CHEX-0001-01 Nikolaos Konstantinides Marie Semon Marco Grillo Michalis Averof; National Science Foundation IOS-1257379 Erin Jarvis Heather Bruce Nipam H Patel; Imperial College London Peter Sarkies; John Fell Fund, University of Oxford Aziz Aboobaker; The funders had no role in study design, data collection and interpretation, or the decision to submit the work for publication. NR 179 TC 1 Z9 1 U1 14 U2 14 PU ELIFE SCIENCES PUBLICATIONS LTD PI CAMBRIDGE PA SHERATON HOUSE, CASTLE PARK, CAMBRIDGE, CB3 0AX, ENGLAND SN 2050-084X J9 ELIFE JI eLife PD NOV 16 PY 2016 VL 5 AR e20062 DI 10.7554/eLife.20062 PG 45 WC Biology SC Life Sciences & Biomedicine - Other Topics GA ED2LX UT WOS:000388677900001 ER PT J AU Hong, T AF Hong, Terry TI The Boy Who Escaped Paradise SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 15 PY 2016 VL 141 IS 19 BP 79 EP 79 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA EC8ZZ UT WOS:000388432900095 ER PT J AU Hong, T AF Hong, Terry TI The Refugees SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 15 PY 2016 VL 141 IS 19 BP 82 EP 83 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA EC8ZZ UT WOS:000388432900114 ER PT J AU Croft, B Wentworth, GR Martin, RV Leaitch, WR Murphy, JG Murphy, BN Kodros, JK Abbatt, JPD Pierce, JR AF Croft, B. Wentworth, G. R. Martin, R. V. Leaitch, W. R. Murphy, J. G. Murphy, B. N. Kodros, J. K. Abbatt, J. P. D. Pierce, J. R. TI Contribution of Arctic seabird-colony ammonia to atmospheric particles and cloud-albedo radiative effect SO NATURE COMMUNICATIONS LA English DT Article ID SULFURIC-ACID; OXIDATION-PRODUCTS; WET DEPOSITION; BLACK CARBON; AEROSOL; EMISSIONS; NUCLEATION; MODEL; SUMMER; TRANSPORT AB The Arctic region is vulnerable to climate change and able to affect global climate. The summertime Arctic atmosphere is pristine and strongly influenced by natural regional emissions, which have poorly understood climate impacts related to atmospheric particles and clouds. Here we show that ammonia from seabird-colony guano is a key factor contributing to bursts of newly formed particles, which are observed every summer in the near-surface atmosphere at Alert, Nunavut, Canada. Our chemical-transport model simulations indicate that the pan-Arctic seabird-influenced particles can grow by sulfuric acid and organic vapour condensation to diameters sufficiently large to promote pan-Arctic cloud-droplet formation in the clean Arctic summertime. We calculate that the resultant cooling tendencies could be large (about -0.5Wm(-2) pan-Arctic-mean cooling), exceeding -1Wm(-2) near the largest seabird colonies due to the effects of seabird-influenced particles on cloud albedo. These coupled ecological-chemical processes may be susceptible to Arctic warming and industrialization. C1 [Croft, B.; Martin, R. V.; Pierce, J. R.] Dalhousie Univ, Dept Phys & Atmospher Sci, 6310 Coburg Rd, Halifax, NS B3H 4R2, Canada. [Wentworth, G. R.; Murphy, J. G.; Abbatt, J. P. D.] Univ Toronto, Dept Chem, 80 St George St, Toronto, ON M5S 3H6, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Leaitch, W. R.] Environm & Climate Change Canada, Div Climate Res, 4905 Dufferin St, Toronto, ON M3H 5T4, Canada. [Murphy, B. N.] Stockholm Univ, Dept Environm Sci & Analyt Chem ACES, Svante Arrhenius Vag 8, SE-11418 Stockholm, Sweden. [Murphy, B. N.] Stockholm Univ, Bolin Ctr Climate Res, Svante Arrhenius Vag 8, SE-11418 Stockholm, Sweden. [Kodros, J. K.; Pierce, J. R.] Colorado State Univ, Dept Atmospher Sci, 3915W Laporte, Ft Collins, CO 80523 USA. [Murphy, B. N.] US EPA, Computat Exposure Div, 200 Pk Dr, Res Triangle Pk, NC 27709 USA. [Wentworth, G. R.] Alberta Environm & Pk, Environm Monitoring & Sci Div, 9888 Jasper Ave NW, Edmonton, AB T5J 5C6, Canada. RP Croft, B (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, 6310 Coburg Rd, Halifax, NS B3H 4R2, Canada.; Wentworth, GR (reprint author), Univ Toronto, Dept Chem, 80 St George St, Toronto, ON M5S 3H6, Canada.; Wentworth, GR (reprint author), Alberta Environm & Pk, Environm Monitoring & Sci Div, 9888 Jasper Ave NW, Edmonton, AB T5J 5C6, Canada. EM betty.croft@dal.ca; greg.wentworth@gov.ab.ca RI Murphy, Jennifer/C-2367-2011; Pierce, Jeffrey/E-4681-2013 OI Pierce, Jeffrey/0000-0002-4241-838X FU Climate Change and Atmospheric Research programme at NSERC; Environment and Climate Change (ECCC) aerosol programme at Alert FX NETCARE is supported by the Climate Change and Atmospheric Research programme at NSERC. We thank O. Kupiainen-Maatta, T. Olenius, J. Julin, H. Vehkamaki and I. Riipinen for their support of this project through constructive discussions, suggestions and provision of the Atmospheric Cluster Dynamics Code (ACDC). We thank Sangeeta Sharma, Desiree Toom, Alina Chivulescu, Dan Veber, the Observatory operators at Alert, Andrew Platt and Carrie Taylor for their support of the Environment and Climate Change (ECCC) aerosol programme at Alert. We thank Kevin Rawlings (www.krawlings.com) for the provision of his photographic image of two Arctic terns on tundra. Our sincere thanks are also extended to Kathy Kuletz of the U.S. Fish and Wildlife Service for her helpful discussions regarding Arctic seabirds. We are grateful for the hard work and dedication of the CCGS Amundsen crew. We also thank Maurice Levasseur, Emma Mungall, Alex Lee, Vickie Irish, Heather Stark and Jeremy Wentzell for help with the Amundsen measurements, for example, during mobilization, demobilization and calibration of the AIM-IC. NR 80 TC 0 Z9 0 U1 18 U2 18 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD NOV 15 PY 2016 VL 7 AR 13444 DI 10.1038/ncomms13444 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EC2RV UT WOS:000387972500001 PM 27845764 ER PT J AU Quinones-Lebron, SG Kralj-Fiser, S Gregoric, M Lokovsek, T Candek, K Haddad, CR Kuntner, M AF Quinones-Lebron, Shakira G. Kralj-Fiser, Simona Gregoric, Matjaz Lokovsek, Tjasa Candek, Klemen Haddad, Charles R. Kuntner, Matjaz TI Potential costs of heterospecific sexual interactions in golden orbweb spiders (Nephila spp.) SO SCIENTIFIC REPORTS LA English DT Article ID REPRODUCTIVE INTERFERENCE; SPERM COMPETITION; FEMALE; SIZE; CONSEQUENCES; CANNIBALISM; INVESTMENT; GIGANTISM; EVOLUTION; BEHAVIOR AB Though not uncommon in other animals, heterospecific mating is rarely reported in arachnids. We investigated sexual interactions among four closely related and syntopical African golden orbweb spiders, Nephila inaurata, N. fenestrata, N. komaci, and N. senegalensis. In two South African localities, female webs were often inhabited by heterospecific males that sometimes outnumbered conspecifics. Species association of males with females was random in nature. In subsequent laboratory choice experiments, N. inaurata males chose heterospecific females in 30% of trials. We also observed natural mating interactions between N. inaurata males and N. komaci females, and between N. komaci males and N. inaurata females in laboratory experiments. While heterospecific mating in the laboratory never produced offspring, conspecific mating did. We discuss potential ecological and evolutionary consequences of heterospecific mating interactions in Nephila that may be particularly costly to the rarer species. C1 [Quinones-Lebron, Shakira G.; Kralj-Fiser, Simona; Gregoric, Matjaz; Lokovsek, Tjasa; Candek, Klemen; Kuntner, Matjaz] Biol Inst ZRC SAZU, Evolutionary Zool Lab, Ljubljana, Slovenia. [Haddad, Charles R.] Univ Free State, Dept Zool & Entomol, Bloemfontein, South Africa. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Kuntner, Matjaz] Hubei Univ, CBEE, Coll Life Sci, Wuhan, Peoples R China. RP Kuntner, M (reprint author), Biol Inst ZRC SAZU, Evolutionary Zool Lab, Ljubljana, Slovenia.; Kuntner, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA.; Kuntner, M (reprint author), Hubei Univ, CBEE, Coll Life Sci, Wuhan, Peoples R China. EM kuntner@gmail.com FU Slovenian Research Agency [J1-6729, P1-10236]; National Research Foundation of South Africa [95569] FX Fieldwork was in agreement with iSimangaliso Wetland Park and Ezemvelo KZN Wildlife, permit num. OP 552/2015. We thank Nerosha Govender, Xander Combrink, and Scotty R. Kyle for their help. Slovenian Research Agency granted J1-6729 and P1-10236 to MK, National Research Foundation of South Africa granted #95569 to CH. NR 26 TC 0 Z9 0 U1 10 U2 10 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD NOV 15 PY 2016 VL 6 AR 36908 DI 10.1038/srep36908 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB8MR UT WOS:000387645700002 PM 27845369 ER PT J AU Xia, YQ Weller, DE Williams, MN Jordan, TE Yan, XY AF Xia, Yongqiu Weller, Donald E. Williams, Meghan N. Jordan, Thomas E. Yan, Xiaoyuan TI Using Bayesian hierarchical models to better understand nitrate sources and sinks in agricultural watersheds SO WATER RESEARCH LA English DT Article DE Bayesian hierarchical models; Export coefficient model; Nutrient sources and sinks; Uncertainty; Temporal and spatial variation ID LAND-USE CHANGE; CHESAPEAKE BAY; EXPORT COEFFICIENTS; RIPARIAN BUFFERS; NUTRIENT DISCHARGES; AQUATIC ECOSYSTEMS; NITROGEN EXPORT; DENITRIFICATION; COVER; PHOSPHORUS AB Export coefficient models (ECMs) are often used to predict nutrient sources and sinks in watersheds because ECMs can flexibly incorporate processes and have minimal data requirements. However, ECM5 do not quantify uncertainties in model structure, parameters, or predictions; nor do they account for spatial and temporal variability in land characteristics, weather, and management practices. We applied Bayesian hierarchical methods to address these problems in ECMs used to predict nitrate concentration in streams. We compared four model formulations, a basic ECM and three models with additional terms to represent competing hypotheses about the sources of error in ECM5 and about spatial and temporal variability of coefficients: an ADditive Error Model (ADEM), a SpatioTemporal Parameter. Model (STPM), and a Dynamic Parameter Model (DPM). The DPM incorporates a first-order random walk to represent spatial correlation among parameters and a dynamic linear model to accommodate temporal correlation. We tested the modeling approach in a proof of concept using watershed characteristics and nitrate export measurements from watersheds in the Coastal Plain physiographic province of the Chesapeake Bay drainage. Among the four models, the DPM was the best it had the lowest mean error, explained the most variability (R-2 = 0.99), had the narrowest prediction intervals, and provided the most effective tradeoff between fit complexity (its deviance information criterion, DIC, was 45.6 units lower than any other model, indicating overwhelming support for the DPM). The superiority of the DPM supports its underlying hypothesis that the main source of error in ECMs is their failure to account for parameter variability rather than structural error. Analysis of the fitted DPM coefficients, for cropland export and instream retention revealed some of the factors controlling nitrate concentration: cropland nitrate exports were positively related to stream flow and watershed average slope, while instream nitrate retention was positively correlated with nitrate concentration. By quantifying spatial and temporal variability in sources and sinks, the DPM provides new information to better target management actions to the most effective times and places. Given the wide use of ECMs as research and management tools, our approach can be broadly applied in other watersheds and to other materials. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Xia, Yongqiu; Yan, Xiaoyuan] Chinese Acad Sci, Inst Soil Sci, Key Lab Soil & Sustainable Agr, Nanjing 210008, Jiangsu, Peoples R China. [Xia, Yongqiu; Weller, Donald E.; Williams, Meghan N.; Jordan, Thomas E.] Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Xia, YQ (reprint author), Chinese Acad Sci, Inst Soil Sci, Key Lab Soil & Sustainable Agr, Nanjing 210008, Jiangsu, Peoples R China. EM yqxia@issas.ac.cn RI XIA, Yongqiu/D-6236-2017; OI Xia, Yongqiu/0000-0001-6856-5671; Weller, Donald/0000-0002-7629-5437; Williams, Meghan/0000-0003-1224-753X FU Charles County, Maryland, USA; U. S. National Science Foundation [DEB-93-17968]; National Natural Science Foundation of China [41471238]; State Key Laboratory of Soil and Sustainable Agriculture, Institute of Soil Science [Y212000013]; China Scholarship Council [201404910320] FX The measurements of watershed discharges were supported by a contract from Charles County, Maryland, USA and by a grant from the U. S. National Science Foundation (DEB-93-17968). The model comparison was financially supported by the National Natural Science Foundation of China through Grant (41471238), and Young Talents in State Key Laboratory of Soil and Sustainable Agriculture, Institute of Soil Science (No. Y212000013). We thank the China Scholarship Council (No. 201404910320) for supporting study abroad. NR 62 TC 0 Z9 0 U1 39 U2 39 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0043-1354 J9 WATER RES JI Water Res. PD NOV 15 PY 2016 VL 105 BP 527 EP 539 DI 10.1016/j.watres.2016.09.033 PG 13 WC Engineering, Environmental; Environmental Sciences; Water Resources SC Engineering; Environmental Sciences & Ecology; Water Resources GA DZ5KW UT WOS:000385902000054 PM 27676387 ER PT J AU Newell, AN Dowdell, DA Santamore, DH AF Newell, Arthur N. Dowdell, Dontray A. Santamore, D. H. TI Surface effects on nitrogen vacancy centers neutralization in diamond SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID AMBIENT CONDITIONS; IB DIAMOND; SPIN; MAGNETOMETRY; SPECTROSCOPY; IRRADIATION; STATE AB The performance of nitrogen vacancy (NV-) based magnetic sensors strongly depends on the stability of nitrogen vacancy centers near the diamond surface. The sensitivity of magnetic field detection is diminished as the NV- turns into the neutralized charge state NV0. We investigate the neutralization of NV- and calculate the ratio of NV0 to total NV (NV- + NV0) caused by a hydrogen terminated diamond with a surface water layer. We find that NV- neutralization exhibits two distinct regions: near the surface, where the NV- is completely neutralized, and in the bulk, where the neutralization ratio is inversely proportional to depth following the electrostatic force law. In addition, small changes in concentration can lead to large differences in neutralization behavior. This phenomenon allows one to carefully control the concentration to decrease the NV- neutralization. The presence of nitrogen dopant greatly reduces NV- neutralization as the nitrogen ionizes in preference to NV- neutralization at the same depth. The water layer pH also affects neutralization. If the pH is very low due to cleaning agent residue, then we see a change in the band bending and the reduction of the two-dimensional hole gas region. Finally, we find that dissolved carbon dioxide resulting from direct contact with the atmosphere at room temperature hardly affects the NV- neutralization. Published by AIP Publishing. C1 [Newell, Arthur N.; Dowdell, Dontray A.; Santamore, D. H.] Delaware State Univ, Dept Phys & Engn Phys, Dover, DE 19901 USA. [Newell, Arthur N.; Dowdell, Dontray A.; Santamore, D. H.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Santamore, DH (reprint author), Delaware State Univ, Dept Phys & Engn Phys, Dover, DE 19901 USA.; Santamore, DH (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. EM dsantamore@desu.edu FU NSF [DMR-1505641] FX This work was supported by NSF DMR-1505641. We are grateful to ITAMP at Harvard-Smithsonian Center for Astrophysics for hosting us during the summer, where the majority of this work has been carried out. We thank Hossein Sadeghpour, Mikhail Lukin and his group, and Ron Walsworth and his group for useful discussions and valuable input. NR 46 TC 0 Z9 0 U1 8 U2 8 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-8979 EI 1089-7550 J9 J APPL PHYS JI J. Appl. Phys. PD NOV 14 PY 2016 VL 120 IS 18 AR 185104 DI 10.1063/1.4967735 PG 7 WC Physics, Applied SC Physics GA ED3FK UT WOS:000388734700022 ER PT J AU Schroder, C Bland, PA Golombek, MP Ashley, JW Warner, NH Grant, JA AF Schroder, Christian Bland, Phil A. Golombek, Matthew P. Ashley, James W. Warner, Nicholas H. Grant, John A. TI Amazonian chemical weathering rate derived from stony meteorite finds at Meridiani Planum on Mars SO NATURE COMMUNICATIONS LA English DT Article ID MOSSBAUER-SPECTROSCOPY; CLIMATE-CHANGE; EROSION RATES; CRATER; DESERT AB Spacecraft exploring Mars such as the Mars Exploration Rovers Spirit and Opportunity, as well as the Mars Science Laboratory or Curiosity rover, have accumulated evidence for wet and habitable conditions on early Mars more than 3 billion years ago. Current conditions, by contrast, are cold, extremely arid and seemingly inhospitable. To evaluate exactly how dry today's environment is, it is important to understand the ongoing current weathering processes. Here we present chemical weathering rates determined for Mars. We use the oxidation of iron in stony meteorites investigated by the Mars Exploration Rover Opportunity at Meridiani Planum. Their maximum exposure age is constrained by the formation of Victoria crater and their minimum age by erosion of the meteorites. The chemical weathering rates thus derived are similar to 1 to 4 orders of magnitude slower than that of similar meteorites found in Antarctica where the slowest rates are observed on Earth. C1 [Schroder, Christian] Univ Stirling, Fac Nat Sci, Biol & Environm Sci, Stirling FK9 4LA, Scotland. [Bland, Phil A.] Curtin Univ, Dept Appl Geol, Perth, WA 6845, Australia. [Golombek, Matthew P.; Ashley, James W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Warner, Nicholas H.] SUNY Coll Geneseo, Dept Geol Sci, Geneseo, NY 14454 USA. [Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DE 20560 USA. RP Schroder, C (reprint author), Univ Stirling, Fac Nat Sci, Biol & Environm Sci, Stirling FK9 4LA, Scotland. EM christian.schroeder@stir.ac.uk RI Schroder, Christian/B-3870-2009 OI Schroder, Christian/0000-0002-7935-6039 FU University of Stirling; NASA FX C.S. acknowledges an Impact Fellowship awarded by the University of Stirling. Part of the work described herein was done by the Mars Exploration Rover Project, Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The authors thank James F. Bell III for providing the seam-corrected mosaic shown in Fig. 2. NR 40 TC 0 Z9 0 U1 14 U2 14 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD NOV 11 PY 2016 VL 7 AR 13459 DI 10.1038/ncomms13459 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB6DE UT WOS:000387470500001 PM 27834377 ER PT J AU Smartt, SJ Chambers, KC Smith, KW Huber, ME Young, DR Cappellaro, E Wright, DE Coughlin, M Schultz, ASB Denneau, L Flewelling, H Heinze, A Magnier, EA Primak, N Rest, A Sherstyuk, A Stalder, B Stubbs, CW Tonry, J Waters, C Willman, M Anderson, JP Baltay, C Botticella, MT Campbell, H Dennefeld, M Chen, TW Della Valle, M Elias-Rosa, N Fraser, M Inserra, C Kankare, E Kotak, R Kupfer, T Harmanen, J Galbany, L Gal-Yam, A Le Guillou, L Lyman, JD Maguire, K Mitra, A Nicholl, M Olivares, F Rabinowitz, D Razza, A Sollerman, J Smith, M Terreran, G Valenti, S Gibson, B Goggia, T AF Smartt, S. J. Chambers, K. C. Smith, K. W. Huber, M. E. Young, D. R. Cappellaro, E. Wright, D. E. Coughlin, M. Schultz, A. S. B. Denneau, L. Flewelling, H. Heinze, A. Magnier, E. A. Primak, N. Rest, A. Sherstyuk, A. Stalder, B. Stubbs, C. W. Tonry, J. Waters, C. Willman, M. Anderson, J. P. Baltay, C. Botticella, M. T. Campbell, H. Dennefeld, M. Chen, T. -W. Della Valle, M. Elias-Rosa, N. Fraser, M. Inserra, C. Kankare, E. Kotak, R. Kupfer, T. Harmanen, J. Galbany, L. Gal-Yam, A. Le Guillou, L. Lyman, J. D. Maguire, K. Mitra, A. Nicholl, M. Olivares E, F. Rabinowitz, D. Razza, A. Sollerman, J. Smith, M. Terreran, G. Valenti, S. Gibson, B. Goggia, T. TI Pan-STARRS and PESSTO search for an optical counterpart to the LIGO gravitational-wave source GW150914 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves; stars: black holes; gamma-ray burst: general; stars: neutron; supernovae: general ID DIGITAL SKY SURVEY; COMPACT OBJECT MERGERS; GAMMA-RAY BURSTS; INTEGRAL-FIELD SPECTROGRAPH; CORE-COLLAPSE SUPERNOVA; ENERGY CAMERA SEARCH; IA SUPERNOVAE; SUPERLUMINOUS SUPERNOVAE; II SUPERNOVAE; ELECTROMAGNETIC COUNTERPARTS AB We searched for an optical counterpart to the first gravitational-wave source discovered by LIGO (GW150914), using a combination of the Pan-STARRS1 wide-field telescope and the Public ESO Spectroscopic Survey of Transient Objects (PESSTO) spectroscopic follow-up programme. As the final LIGO sky maps changed during analysis, the total probability of the source being spatially coincident with our fields was finally only 4.2 per cent. Therefore, we discuss our results primarily as a demonstration of the survey capability of Pan-STARRS and spectroscopic capability of PESSTO. We mapped out 442 deg(2) of the northern sky region of the initial map. We discovered 56 astrophysical transients over a period of 41 d from the discovery of the source. Of these, 19 were spectroscopically classified and a further 13 have host galaxy redshifts. All transients appear to be fairly normal supernovae (SNe) and AGN variability and none is obviously linked with GW150914. We illustrate the sensitivity of our survey by defining parametrized light curves with time-scales of 4, 20 and 40 d and use the sensitivity of the Pan-STARRS1 images to set limits on the luminosities of possible sources. The Pan-STARRS1 images reach limiting magnitudes of iP1 = 19.2, 20.0 and 20.8, respectively, for the three time-scales. For long time-scale parametrized light curves (with full width half-maximum similar or equal to 40 d), we set upper limits of M-i <= -17.2(+1.4)(-0.9) if the distance to GW150914 is D-L = 400 +/- 200 Mpc. The number of Type Ia SN we find in the survey is similar to that expected from the cosmic SN rate, indicating a reasonably complete efficiency in recovering SN like transients out to D-L = 400 +/- 200 Mpc. C1 [Smartt, S. J.; Smith, K. W.; Young, D. R.; Wright, D. E.; Inserra, C.; Kankare, E.; Kotak, R.; Maguire, K.; Terreran, G.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Chambers, K. C.; Huber, M. E.; Schultz, A. S. B.; Denneau, L.; Flewelling, H.; Heinze, A.; Magnier, E. A.; Primak, N.; Sherstyuk, A.; Stalder, B.; Tonry, J.; Waters, C.; Willman, M.; Gibson, B.; Goggia, T.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Cappellaro, E.; Elias-Rosa, N.; Terreran, G.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Coughlin, M.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rest, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Anderson, J. P.] European Southern Observ, Alonso Cordova 3107, Santiago, Chile. [Baltay, C.; Rabinowitz, D.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Botticella, M. T.; Della Valle, M.] INAF, Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy. [Campbell, H.; Fraser, M.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Dennefeld, M.] CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France. [Dennefeld, M.] Univ Paris 06, 98 Bis Blvd Arago, F-75014 Paris, France. [Chen, T. -W.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Kupfer, T.] CALTECH, MC 290-17, Pasadena, CA 91125 USA. [Kupfer, T.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Harmanen, J.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaialantie 20, FI-21500 Piikkio, Finland. [Galbany, L.; Olivares E, F.; Razza, A.] Millennium Inst Astrophys, Casilla 36-D, Santiago, Chile. [Galbany, L.; Razza, A.] Univ Chile, Dept Astron, Camino Observ 1515, Santiago, Chile. [Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Le Guillou, L.; Mitra, A.] Univ Paris 06, LPNHE, UMR 7585, Sorbonne Univ, F-75005 Paris, France. [Le Guillou, L.; Mitra, A.] CNRS, UMR 7585, Lab Phys Nucl & Hautes Energies, 4 Pl Jussieu, F-75005 Paris, France. [Lyman, J. D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Nicholl, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Olivares E, F.] Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile. [Sollerman, J.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Sollerman, J.] Stockholm Univ, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden. [Smith, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Valenti, S.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Valenti, S.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Smartt, SJ (reprint author), Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. EM s.smartt@qub.ac.uk RI Galbany, Lluis/A-8963-2017; Elias-Rosa, Nancy/D-3759-2014; OI Galbany, Lluis/0000-0002-1296-6887; Elias-Rosa, Nancy/0000-0002-1381-9125; Kotak, Rubina/0000-0001-5455-3653 FU University of Hawaii; NASA's Planetary Defense Office [NNX14AM74G]; Queen's University Belfast; NASA [NNX08AR22G]; National Science Foundation [AST-1238877]; European Organization for Astronomical Research in the Southern hemisphere, Chile as part of PESSTO ESO programmes [188.D-3003, 191.D-0935]; European Research Council under the European Union [291222]; STFC [ST/I001123/1, ST/L000709/1]; European Union FP7 programme through ERC [320360]; STFC through an Ernest Rutherford Fellowship; FONDECYT [3140326] FX Pan-STARRS is supported by the University of Hawaii and the NASA's Planetary Defense Office under Grant no. NNX14AM74G. The Pan-STARRS-LIGO effort is in collaboration with the LIGO Consortium and supported by Queen's University Belfast. The Pan-STARRS1 Sky Surveys have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, and the NASA under Grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant no. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. This work is based (in part) on observations collected at the European Organization for Astronomical Research in the Southern hemisphere, Chile as part of PESSTO ESO programmes 188.D-3003, 191.D-0935. Some of the data presented herein were obtained at the Palomar Observatory, California Institute of Technology. SJS acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no. [291222] and STFC grants ST/I001123/1 and ST/L000709/1. MF is supported by the European Union FP7 programme through ERC grant number 320360. KM acknowledges support from the STFC through an Ernest Rutherford Fellowship FOE acknowledges support from FONDECYT through postdoctoral grant 3140326. NR 137 TC 5 Z9 5 U1 5 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 11 PY 2016 VL 462 IS 4 BP 4094 EP 4116 DI 10.1093/mnras/stw1893 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY6LH UT WOS:000385231600047 ER PT J AU Ilee, JD Cyganowski, CJ Nazari, P Hunter, TR Brogan, CL Forgan, DH Zhang, Q AF Ilee, J. D. Cyganowski, C. J. Nazari, P. Hunter, T. R. Brogan, C. L. Forgan, D. H. Zhang, Q. TI G11.92-0.61 MM1: a Keplerian disc around a massive young proto-O star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: G11.92-0.61; stars: massive; stars: pre-main-sequence; stars: protostars; radio continuum: stars; submillimetre: stars ID EXTENDED GREEN OBJECTS; HYPERCOMPACT HII-REGIONS; NEAR-INFRARED H-2; H-II REGIONS; STELLAR OBJECTS; FORMING REGIONS; ACCRETION DISKS; CONTINUUM SURVEY; MOLECULAR CORES; GLIMPSE SURVEY AB The formation process of massive stars is not well understood, and advancement in our understanding benefits from high-resolution observations and modelling of the gas and dust surrounding individual high-mass (proto) stars. Here, we report subarcsecond (less than or similar to 1550 au) resolution observations of the young massive star G11.92-0.61 MM1 with the Submillimeter Array (SMA) and Very Large Array (VLA). Our 1.3 mm SMA observations reveal consistent velocity gradients in compact molecular line emission from species such as CH3CN, CH3OH, OCS, HNCO, H2CO, DCN and CH3CH2CN, oriented perpendicular to the previously reported bipolar molecular outflow from MM1. Modelling of the compact gas kinematics suggests a structure undergoing rotation around the peak of the dust continuum emission. The rotational profile can be well fitted by a model of a Keplerian disc, including infall, surrounding an enclosed mass of similar to 30-60M(circle dot), of which 2-3M(circle dot) is attributed to the disc. From modelling the CH3CN emission, we determine that two temperature components, of similar to 150 K and 230 K, are required to adequately reproduce the spectra. Our 0.9 and 3.0 cm VLA continuum data exhibit an excess above the level expected from dust emission; the full centimetre-submillimetre wavelength spectral energy distribution of MM1 is well reproduced by a model including dust emission, an unresolved hypercompact H II region, and a compact ionized jet. In combination, our results suggest that MM1 is an example of a massive proto-O star forming via disc accretion, in a similar way to that of lower mass stars. C1 [Ilee, J. D.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Cyganowski, C. J.; Nazari, P.; Forgan, D. H.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Scotland. [Hunter, T. R.; Brogan, C. L.] NRAO, 520 Edgemont Rd, Charlottesville, VA 22903 USA. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ilee, JD (reprint author), Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM jdilee@ast.cam.ac.uk OI Zhang, Qizhou/0000-0003-2384-6589 FU DISCSIM project [341137]; European Research Council [2013-ADG, ERC-2011-ADG]; STFC [ST/M001296/1]; Undergraduate Research Bursary from the Royal Astronomical Society; ECOGAL project [291227]; Smithsonian Institution; Academia Sinica FX JDI gratefully acknowledges support from the DISCSIM project, grant agreement 341137, funded by the European Research Council under ERC-2013-ADG. CJC acknowledges support from STFC grant ST/M001296/1. PN, CJC and JDI gratefully acknowledge support in the form of an Undergraduate Research Bursary from the Royal Astronomical Society. DF acknowledges support from the ECOGAL project, grant agreement 291227, funded by the European Research Council under ERC-2011-ADG. This research has made use of NASA's Astrophysics Data System Bibliographic Services; Astropy, a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013); APLPY, an open-source plotting package for PYTHON hosted at http://aplpy.github.com, and the CASSIS software and VADMC data bases (http://www.vamdc.eu/). CASSIS has been developed by IRAP-UPS/CNRS (http://cassis.irap.omp.eu). The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under agreement by the Associated Universities, Inc. NR 80 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 11 PY 2016 VL 462 IS 4 BP 4386 EP 4401 DI 10.1093/mnras/stw1912 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY6LH UT WOS:000385231600066 ER PT J AU See, V Jardine, M Vidotto, AA Donati, JF Saikia, SB Bouvier, J Fares, R Folsom, CP Gregory, SG Hussain, G Jeffers, SV Marsden, SC Morin, J Moutou, C do Nascimento, JD Petit, P Waite, IA AF See, V. Jardine, M. Vidotto, A. A. Donati, J. -F. Saikia, S. Boro Bouvier, J. Fares, R. Folsom, C. P. Gregory, S. G. Hussain, G. Jeffers, S. V. Marsden, S. C. Morin, J. Moutou, C. do Nascimento, J. D., Jr. Petit, P. Waite, I. A. TI The connection between stellar activity cycles and magnetic field topology SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: polarimetric; stars: activity; stars: evolution; stars: magnetic field; stars: rotation ID SUN-LIKE STARS; MAIN-SEQUENCE STARS; PLANET-HOSTING STAR; SOLAR-TYPE STARS; ACTIVITY-ROTATION RELATIONSHIP; TAU-BOOTIS; LARGE-SCALE; CHROMOSPHERIC VARIATIONS; EPSILON ERIDANI; TIME EVOLUTION AB Zeeman-Doppler imaging (ZDI) has successfully mapped the large-scale magnetic fields of stars over a large range of spectral types, rotation periods and ages. When observed over multiple epochs, some stars show polarity reversals in their global magnetic fields. On the Sun, polarity reversals are a feature of its activity cycle. In this paper, we examine the magnetic properties of stars with existing chromospherically determined cycle periods. Previous authors have suggested that cycle periods lie on multiple branches, either in the cycle period-Rossby number plane or the cycle period-rotation period plane. We find some evidence that stars along the active branch show significant average toroidal fields that exhibit large temporal variations while stars exclusively on the inactive branch remain dominantly poloidal throughout their entire cycle. This lends credence to the idea that different shear layers are in operation along each branch. There is also evidence that the short magnetic polarity switches observed on some stars are characteristic of the inactive branch while the longer chromospherically determined periods are characteristic of the active branch. This may explain the discrepancy between the magnetic and chromospheric cycle periods found on some stars. These results represent a first attempt at linking global magnetic field properties obtained from ZDI and activity cycles. C1 [See, V.; Jardine, M.; Gregory, S. G.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Vidotto, A. A.] Univ Geneva, Observ Geneve, Chemin Maillettes 51, CH-1290 Sauverny, Switzerland. [Vidotto, A. A.] Univ Dublin, Sch Phys, Trinity Coll Dublin, Dublin 2, Ireland. [Donati, J. -F.; Petit, P.] Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, F-31400 Toulouse, France. [Donati, J. -F.; Petit, P.] CNRS, Inst Rech Astrophys & Planetol, 14 Ave Edouard Belin, F-31400 Toulouse, France. [Saikia, S. Boro; Jeffers, S. V.] Univ Gottingen, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany. [Bouvier, J.; Folsom, C. P.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Bouvier, J.; Folsom, C. P.] CNRS, IPAG, F-38000 Grenoble, France. [Fares, R.] INAF Osservatorio Astrofis Catania, Via Santa Sofia 78, I-95123 Catania, Italy. [Hussain, G.] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Marsden, S. C.; Waite, I. A.] Univ Southern Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Morin, J.] Univ Montpellier, CNRS, LUPM, Pl E Bataillon, F-34095 Montpellier, France. [Moutou, C.] CNRS, Canada France Hawaii Telescope Corp, 65-238 Mamalahoa Hwy, Kamuela, HI 96743 USA. [Moutou, C.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [do Nascimento, J. D., Jr.] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil. [do Nascimento, J. D., Jr.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP See, V (reprint author), Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. EM wcvs@st-andrews.ac.uk OI Petit, Pascal/0000-0001-7624-9222; Boro Saikia, Sudeshna/0000-0002-3673-3746; Gregory, Scott/0000-0003-3674-5568; Vidotto, Aline/0000-0001-5371-2675 FU Science and Technology Facilities Council (STFC); Swiss National Science Foundation; Deutsche Forchungsgemeinschaft (DFG) under grant SFB; STFC [ST/J003255/1]; grant ANR [Blanc SIMI5-6 020 01] FX The authors would like to thank Steven Saar for refereeing their manuscript and providing constructive criticism that helped improve this work. VS acknowledges the support of a Science and Technology Facilities Council (STFC) studentship. AAV acknowledges support from the Swiss National Science Foundation through an Ambizione Fellowship. SBS and SVJ acknowledge research funding by the Deutsche Forchungsgemeinschaft (DFG) under grant SFB, project A16. SGG acknowledges support from the STFC via an Ernest Rutherford Fellowship [ST/J003255/1]. This study was supported by the grant ANR 2011 Blanc SIMI5-6 020 01 'Toupies: towards understanding the spin evolution of stars' (http://ipag.osug.fr/Anr_Toupies/). This work is based on observations obtained with ESPaDOnS at the CFHT and with NARVAL at the TBL. CFHT/ESPaDOnS are operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique (INSU/CNRS) of France and the University of Hawaii, while TBL/NARVAL are operated by INSU/CNRS. NR 64 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 11 PY 2016 VL 462 IS 4 BP 4442 EP 4450 DI 10.1093/mnras/stw2010 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY6LH UT WOS:000385231600071 ER PT J AU Huertas-Company, M Bernardi, M Perez-Gonzalez, PG Ashby, MLN Barro, G Conselice, C Daddi, E Dekel, A Dimauro, P Faber, SM Grogin, NA Kartaltepe, JS Kocevski, DD Koekemoer, AM Koo, DC Mei, S Shankar, F AF Huertas-Company, M. Bernardi, M. Perez-Gonzalez, P. G. Ashby, M. L. N. Barro, G. Conselice, C. Daddi, E. Dekel, A. Dimauro, P. Faber, S. M. Grogin, N. A. Kartaltepe, J. S. Kocevski, D. D. Koekemoer, A. M. Koo, D. C. Mei, S. Shankar, F. TI Mass assembly and morphological transformations since z similar to 3 from CANDELS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: high-redshift; galaxies: structure ID EXTRAGALACTIC LEGACY SURVEY; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION HISTORY; EARLY-TYPE GALAXIES; STELLAR MASS; QUIESCENT GALAXIES; PHOTOMETRIC CATALOGS; FORMING GALAXIES; HIGH-REDSHIFT; COSMIC TIME AB We quantify the evolution of the stellar mass functions (SMFs) of star-forming and quiescent galaxies as a function of morphology from z similar to 3 to the present. Our sample consists of similar to 50 000 galaxies in the CANDELS fields (similar to 880 arcmin(2)), which we divide into four main morphological types, i. e. pure bulge-dominated systems, pure spiral disc-dominated, intermediate two-component bulge+ disc systems and irregular disturbed galaxies. At z similar to 2, 80 per cent of the stellarmass density of star-forming galaxies is in irregular systems. However, by z similar to 0.5, irregular objects only dominate at stellar masses below 10(9) M-circle dot. A majority of the star-forming irregulars present at z similar to 2 undergo a gradual transformation from disturbed to normal spiral disc morphologies by z similar to 1 without significant interruption to their star formation. Rejuvenation after a quenching event does not seem to be common except perhaps for the most massive objects, because the fraction of bulge-dominated star-forming galaxies with M*/M-circle dot > 10(10.7) reaches 40 per cent at z < 1. Quenching implies the presence of a bulge: the abundance of massive red discs is negligible at all redshifts over 2 dex in stellar mass. However, the dominant quenching mechanism evolves. At z > 2, the SMF of quiescent galaxies aboveM* is dominated by compact spheroids. Quenching at this early epoch destroys the disc and produces a compact remnant unless the star-forming progenitors at even higher redshifts are significantly more dense. At 1 < z< 2, the majority of newly quenched galaxies are discs with a significant central bulge. This suggests that mass quenching at this epoch starts from the inner parts and preserves the disc. At z < 1, the high-mass end of the passive SMF is globally in place and the evolution mostly happens at stellar masses below 10(10) M-circle dot. These low-mass galaxies are compact, bulge-dominated systems, which were environmentally quenched: destruction of the disc through ram-pressure stripping is the likely process. C1 [Huertas-Company, M.; Dimauro, P.; Mei, S.] Univ Paris Sorbonne Cite, Univ Paris Diderot, PSL Res Univ, GEPI,Observ Paris,CNRS, 61 Ave Observ, F-75014 Paris, France. [Huertas-Company, M.; Bernardi, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Perez-Gonzalez, P. G.] Univ Complutense Madrid, Dept Astrofs, Fac CC Fs, E-28040 Madrid, Spain. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Barro, G.] Univ Calif Berkeley, Dept Astrophys, Berkeley, CA 94720 USA. [Conselice, C.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Daddi, E.] Univ Paris Diderot, Lab AIM, CEA DSM CNRS, Irfu Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Dekel, A.] Hebrew Univ Jerusalem, Racah Inst Phys, Ctr Astrophys & Planetary Sci, IL-91904 Jerusalem, Israel. [Faber, S. M.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Grogin, N. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kartaltepe, J. S.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Koekemoer, A. M.] Colby Coll, Dept Phys & Astron, Waterville, ME 04961 USA. [Mei, S.] CALTECH, Pasadena, CA 91125 USA. [Shankar, F.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. RP Huertas-Company, M (reprint author), Univ Paris Sorbonne Cite, Univ Paris Diderot, PSL Res Univ, GEPI,Observ Paris,CNRS, 61 Ave Observ, F-75014 Paris, France.; Huertas-Company, M (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM marc.huertas@obspm.fr RI Daddi, Emanuele/D-1649-2012; OI Daddi, Emanuele/0000-0002-3331-9590; Koekemoer, Anton/0000-0002-6610-2048 NR 76 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 11 PY 2016 VL 462 IS 4 BP 4495 EP 4516 DI 10.1093/mnras/stw1866 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY6LH UT WOS:000385231600076 ER PT J AU Aliu, E Archambault, S Archer, A Benbow, W Bird, R Biteau, J Buchovecky, M Buckley, JH Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Eisch, JD Falcone, A Feng, Q Finley, JP Fleischhack, H Flinders, A Fortin, P Fortson, L Furniss, A Gillanders, GH Griffin, S Grube, J Gyuk, G Hutten, M Hakansson, N Holder, J Humensky, TB Johnson, CA Kaaret, P Kar, P Kelley-Hoskins, N Kertzman, M Kieda, D Krause, M Lang, MJ Loo, A Maier, G McArthur, S McCann, A Meagher, K Moriarty, P Mukherjee, R Nguyen, T Nieto, D De Bhroithe, AO Ong, RA Otte, AN Pandel, D Park, N Pelassa, V Petrashyk, A Pohl, M Popkow, A Pueschel, E Quinn, J Ragan, K Reynolds, PT Richards, GT Roache, E Rulten, C Santander, M Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weiner, OM Weinstein, A Wilhelm, A Williams, DA Zitzer, B Chernyakova, M Roberts, MSE AF Aliu, E. Archambault, S. Archer, A. Benbow, W. Bird, R. Biteau, J. Buchovecky, M. Buckley, J. H. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Eisch, J. D. Falcone, A. Feng, Q. Finley, J. P. Fleischhack, H. Flinders, A. Fortin, P. Fortson, L. Furniss, A. Gillanders, G. H. Griffin, S. Grube, J. Gyuk, G. Huetten, M. Hakansson, N. Holder, J. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kelley-Hoskins, N. Kertzman, M. Kieda, D. Krause, M. Lang, M. J. Loo, A. Maier, G. McArthur, S. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nguyen, T. Nieto, D. De Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Pandel, D. Park, N. Pelassa, V. Petrashyk, A. Pohl, M. Popkow, A. Pueschel, E. Quinn, J. Ragan, K. Reynolds, P. T. Richards, G. T. Roache, E. Rulten, C. Santander, M. Sembroski, G. H. Shahinyan, K. Smith, A. W. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Vincent, S. Wakely, S. P. Weiner, O. M. Weinstein, A. Wilhelm, A. Williams, D. A. Zitzer, B. Chernyakova, M. Roberts, M. S. E. TI A SEARCH FOR VERY HIGH ENERGY GAMMA RAYS FROM THE MISSING LINK BINARY PULSAR J1023+0038 WITH VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; gamma rays: general; pulsars: general; pulsars: individual (PSR J1023+0038) ID MILLISECOND PULSAR; PSR J1023+0038; 1ST J102347.6+003841; NUSTAR OBSERVATIONS; STATE CHANGE; EMISSION; TRANSITION; TELESCOPE; PERIASTRON; DISCOVERY AB The binary millisecond radio pulsar PSR J1023+0038 exhibits many characteristics similar to the gamma-ray binary system PSR B1259-63/LS 2883, making it an ideal candidate for the study of high-energy nonthermal emission. It has been the subject of multiwavelength campaigns following the disappearance of the pulsed radio emission in 2013 June, which revealed the appearance of an accretion disk around the neutron star. We present the results of very high energy (VHE) gamma-ray observations carried out by the Very Energetic Radiation Imaging Telescope Array System before and after this change of state. Searches for steady and pulsed emission of both data sets yield no significant gamma-ray signal above 100 GeV, and upper limits are given for both a steady and pulsed gamma-ray flux. These upper limits are used to constrain the magnetic field strength in the shock region of the PSR J1023+0038 system. Assuming that VHE gamma rays are produced via an inverse Compton mechanism in the shock region, we constrain the shock magnetic field to be greater than similar to 2 G before the disappearance of the radio pulsar and greater than similar to 10 G afterward. C1 [Aliu, E.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; McCann, A.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Buchovecky, M.; Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Byrum, K.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Cardenzana, J. V.; Dickinson, H. J.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Hakansson, N.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Fleischhack, H.; Huetten, M.; Kelley-Hoskins, N.; Krause, M.; Maier, G.; Telezhinsky, I.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany. [Ciupik, L.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Flinders, A.; Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Fortson, L.; Rulten, C.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA. [Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.; Loo, A.; Weiner, O. M.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Meagher, K.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Park, N.; Staszak, D.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Phys Sci, Cork, Ireland. [Smith, A. W.] Univ Maryland, Coll Park NASA GSFC, College Pk, MD 20742 USA. [Chernyakova, M.] Dublin City Univ, Sch Phys Sci, Dublin 9, Ireland. [Chernyakova, M.] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland. [Roberts, M. S. E.] New York Univ Abu Dhabi, POB 129188 Saadiyat Isl, Abu Dhabi, U Arab Emirates. [Roberts, M. S. E.] Eureka Sci, 2452 Delmer St,Suite 100, Oakland, CA 94602 USA. RP Aliu, E (reprint author), Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM ester.aliu.fuste@gmail.com; gtrichards@gatech.edu; masha.chernyakova@dcu.ie; malloryr@gmail.com OI Krause, Maria/0000-0001-7595-0914; Roberts, Mallory/0000-0002-9396-9720; Pandel, Dirk/0000-0003-2085-5586; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; Smithsonian Institution; NSERC in Canada; Spanish Ministerio de Economia y Competitividad (MINECO) [AYA2013-47447-C3-1-P]; U.S. National Science Foundation FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, and by NSERC in Canada. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. E.A. acknowledges support by the Spanish Ministerio de Economia y Competitividad (MINECO) under grants AYA2013-47447-C3-1-P. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. NR 56 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2016 VL 831 IS 2 AR 193 DI 10.3847/0004-637X/831/2/193 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC6DU UT WOS:000388227500004 ER PT J AU McClure, MK Bergin, EA Cleeves, LI van Dishoeck, EF Blake, GA Ii, NJE Green, JD Henning, T Oberg, KI Pontoppidan, KM Salyk, C AF McClure, M. K. Bergin, E. A. Cleeves, L. I. van Dishoeck, E. F. Blake, G. A. Ii, N. J. Evans Green, J. D. Henning, Th. Oeberg, K. I. Pontoppidan, K. M. Salyk, C. TI MASS MEASUREMENTS IN PROTOPLANETARY DISKS FROM HYDROGEN DEUTERIDE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; protoplanetary disks; radiative transfer ID T-TAURI STARS; YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DUST DISKS; FORMING REGION; CHAMELEON-I; MOLECULAR CLOUD; PRETRANSITIONAL DISKS; TEMPERATURE STRUCTURE; TRANSITIONAL DISKS; SUBMILLIMETER VIEW AB The total gas mass of a protoplanetary disk is a fundamental, but poorly determined, quantity. A new technique has been demonstrated to assess directly the bulk molecular gas reservoir of molecular hydrogen using the HD J = 1-0 line at 112 mu m. In this work we present a Herschel Space Observatory(10) survey of six additional T Tauri disks in the HD line. Line emission is detected at >3 sigma significance in two cases: DM Tau and GM Aur. For the other four disks, we establish upper limits to the line flux. Using detailed disk structure and ray-tracing models, we calculate the temperature structure and dust mass from modeling the observed spectral energy distributions, and we include the effect of UV gas heating to determine the amount of gas required to fit the HD line. The ranges of gas masses are 1.0-4.7 x 10(-2) for DM Tau and 2.5-20.4 x 10(-2) for GM Aur. These values are larger than those found using CO for GM Aur, while the CO-derived gas mass for DM Tau is consistent with the lower end of our mass range. This suggests a CO chemical depletion from the gas phase of up to a factor of five for DM Tau and up to two orders of magnitude for GM Aur. We discuss how future analysis can narrow the mass ranges further. C1 [McClure, M. K.] Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Bergin, E. A.; Cleeves, L. I.] Univ Michigan, Dept Astron, 500 Church St,830 Dennison Bldg, Ann Arbor, MI 48109 USA. [Cleeves, L. I.; Oeberg, K. I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Blake, G. A.] CALTECH, Mail Stop 150-21, Pasadena, CA 91125 USA. [Ii, N. J. Evans; Green, J. D.] Univ Texas Austin, Dept Astron, RLM 15-312A, Austin, TX 78712 USA. [Green, J. D.; Pontoppidan, K. M.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Henning, Th.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Salyk, C.] Vassar Coll, Dept Phys & Astron, Vassar Coll Box 745, Poughkeepsie, NY 12604 USA. RP McClure, MK (reprint author), Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM mmcclure@eso.org; ebergin@umich.edu; ilse.cleeves@cfa.harvard.edu; ewine@strw.leidenuniv.nl; gab@gps.caltech.edu; nje@astro.as.utexas.edu; jgreen@stsci.edu; henning@mpia.de; koberg@cfa.harvard.edu; pontoppi@stsci.edu; cosalyk@vassar.edu OI Green, Joel/0000-0003-1665-5709; Evans , Neal/0000-0001-5175-1777; Cleeves, L. Ilsedore/0000-0003-2076-8001 FU NASA FX This work is based on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. We thank Davide Fedele for useful discussions regarding the data reduction and line flux determinations. We would also like to thank the anonymous referee for constructive suggestions. NR 85 TC 3 Z9 3 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 10 PY 2016 VL 831 IS 2 AR 167 DI 10.3847/0004-637X/831/2/167 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC1PI UT WOS:000387878200018 ER PT J AU Oberg, KI Bergin, EA AF Oberg, Karin I. Bergin, Edwin A. TI EXCESS C/O AND C/H IN OUTER PROTOPLANETARY DISK GAS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; molecular processes; planet-disk interactions; planets and satellites: atmospheres; planets and satellites: formation; protoplanetary disks ID PLANET FORMATION; GIANT PLANETS; SOLAR-SYSTEM; GRAIN-GROWTH; FRAGMENTATION; ATMOSPHERES; COAGULATION; CARBON; STARS; WATER AB The compositions of nascent planets depend on the compositions of their birth disks. In particular, the elemental compositions of gas giant gaseous envelopes depend on the elemental compositions of the disk gas from which the envelopes are accreted. Previous models have demonstrated that sequential freeze-out of O- and C-bearing volatiles in disks will result in supersolar C/O ratios and subsolar C/H ratios in the gas between water and CO snowlines. However, this result does not take into account the expected grain growth and radial drift of pebbles in disks, and the accompanying redistribution of volatiles from the outer to the inner disk. Using a toy model we demonstrate that when drift is considered, CO is enhanced between the water and CO snowline, resulting in both supersolar C/O and C/H ratios in the disk gas in the gas giant formation zone. This result appears to be robust for the disk model as long as there is substantial pebble drift across the CO snowline, and the efficiency of CO vapor diffusion is limited. Gas giants that accrete their gaseous envelopes exterior to the water snowline and do not experience substantial core-envelope mixing may thus feature both superstellar C/O and C/H ratios in their atmospheres. Pebble drift will also affect the nitrogen and noble gas abundances in the planet-forming zones, which may explain some of Jupiter's peculiar abundance patterns. C1 [Oberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, 311 West Hall,1085 S Univ Ave, Ann Arbor, MI 48109 USA. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Packard Fellowship for Science and Engineering from the David and Lucile Packard Foundation; National Science Foundation [AST-1514670, AST-1344133]; NASA XRP program [NNX16AB48G] FX The authors are grateful to Ellen Price for computational advice, and for helpful comments from the anonymous referee. K.I.O. acknowledges funding through a Packard Fellowship for Science and Engineering from the David and Lucile Packard Foundation. E.A.B. acknowledges support from the National Science Foundation under grants AST-1514670 and AST-1344133 (INSPIRE), and NASA XRP program NNX16AB48G. NR 23 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 10 PY 2016 VL 831 IS 2 AR L19 DI 10.3847/2041-8205/831/2/L19 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC1YI UT WOS:000387904900003 ER PT J AU Krell, FT Klimes, P Rocha, LA Fikacek, M Miller, SE AF Krell, Frank T. Klimes, Petr Rocha, Luiz A. Fikacek, Martin Miller, Scott E. TI Preserve specimens for reproducibility SO NATURE LA English DT Letter C1 [Krell, Frank T.] Denver Museum Nat & Sci, Denver, CO 80205 USA. [Klimes, Petr] Biol Ctr CAS, Inst Entomol, Ceske Budejovice, Czech Republic. [Rocha, Luiz A.] Calif Acad Sci, San Francisco, CA 94118 USA. [Fikacek, Martin] Natl Museum, Prague, Czech Republic. [Fikacek, Martin] Charles Univ Prague, CR-11636 Prague 1, Czech Republic. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Krell, FT (reprint author), Denver Museum Nat & Sci, Denver, CO 80205 USA. EM frank.krell@dmns.org RI Klimes, Petr/G-6823-2014 NR 0 TC 3 Z9 4 U1 7 U2 7 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD NOV 10 PY 2016 VL 539 IS 7628 BP 168 EP 168 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB4CZ UT WOS:000387318500016 PM 27830800 ER PT J AU Miyashita, LK Richardson, JP Duffy, JE AF Miyashita, Leonardo K. Richardson, J. Paul Duffy, J. Emmett TI Effects of predator richness and habitat heterogeneity on prey suppression in an estuarine food chain SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Biodiversity; Ecosystem functioning; Habitat structure; Predator richness; Trophic cascade; Food webs; Complementarity; Omnivory ID CRABS CALLINECTES-SAPIDUS; SHRIMP PALAEMONETES-PUGIO; DAMPENS TROPHIC CASCADES; JUVENILE BLUE-CRAB; CHESAPEAKE BAY; INTRAGUILD PREDATION; CRANGON-SEPTEMSPINOSA; ECOSYSTEM PROPERTIES; FUNCTIONAL-ROLE; MARINE MYSIDS AB Predator influence on the structure of prey communities can be mediated by habitat heterogeneity, the effects of which may cascade to the base of the food webs, altering producer biomass and species composition. We carried out a mesocosm experiment manipulating the identity and richness of predators and habitat heterogeneity to test their influence on resource use effectiveness, competition among predators, and trophic cascades in a model estuarine system with 3 trophic levels (microalgae, mysids, and the predators blue crab Callinectes sapidus, sand shrimp Crangon septemspinosa, and grass shrimp Palaemonetes pugio). We hypothesized that increasing predator species richness would increase mysid suppression because of complementarity among predators, that complementarity would be better expressed in more heterogeneous habitats, and that higher mysid suppression would increase algae biomass through cascading effects. Assemblages with multiple predators were more effective at suppressing prey than the average single predator, but not in comparison to the most effective predator (i.e. no transgressive overyielding). Predator diversity effects increased with habitat heterogeneity, possibly because it allowed interspecific complementarity among predators to be expressed. Moreover, habitat heterogeneity dampened intraspecific predation and/or negative behavioral interactions between predators. A trophic cascade was not observed because of the low mysid grazing impact on microalgae, probably related to the omnivorous feeding of mysids. Our findings indicate that the loss of both biodiversity and habitat heterogeneity should alter the energy flux in marine food webs; therefore, both must be considered for the proper management of natural ecosystems. C1 [Miyashita, Leonardo K.; Richardson, J. Paul; Duffy, J. Emmett] Coll William & Mary, Virginia Inst Marine Sci, Dept Biol Sci, Gloucester Point, VA 23062 USA. [Miyashita, Leonardo K.] Univ Sao Paulo, Oceanog Inst, Dept Biol Oceanog, BR-05508120 Sao Paulo, SP, Brazil. [Duffy, J. Emmett] Smithsonian Inst, Tennenbaum Marine Observ Network, Washington, DC 20013 USA. RP Miyashita, LK (reprint author), Coll William & Mary, Virginia Inst Marine Sci, Dept Biol Sci, Gloucester Point, VA 23062 USA.; Miyashita, LK (reprint author), Univ Sao Paulo, Oceanog Inst, Dept Biol Oceanog, BR-05508120 Sao Paulo, SP, Brazil. EM lkenjim@gmail.com FU National Council for Scientific and Technological Development (CNPq) [142203/2010-6, 142050/2012-1, 245466/2012-6] FX We thank S. Chak, J. Lefcheck, K. Gadeken, D. Hall, and S. Ziegler for their help with the mesocosm experiment, and D. Calliari for comments and text editing on an earlier version of this manuscript. L.K.M. was supported by the National Council for Scientific and Technological Development (CNPq, grants 142203/2010-6, 142050/2012-1 and 245466/2012-6). NR 58 TC 0 Z9 0 U1 14 U2 14 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD NOV 9 PY 2016 VL 559 BP 13 EP 20 DI 10.3354/meps11893 PG 8 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA EC6CW UT WOS:000388225000002 ER PT J AU Lubcker, N Condit, R Beltran, RS de Bruyn, PJN Bester, MN AF Luebcker, Nico Condit, Richard Beltran, Roxanne S. de Bruyn, P. J. Nico Bester, Marthan N. TI Vibrissal growth parameters of southern elephant seals Mirounga leonina: obtaining fine-scale, time-based stable isotope data SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Biomonitoring; Marine mammals; Moult; Pinnipeds; Shedding; Whiskers ID MARION ISLAND; FORAGING STRATEGIES; TROPHIC ECOLOGY; PHOCA-VITULINA; DIET; CARBON; PATTERNS; WHISKERS AB Stable isotopes provide a powerful, indirect approach to assess the trophic ecology of individuals on a spatial and temporally integrated basis (especially when combined with telemetry). However, using stable isotopes requires accurate, species-specific quantification of the period of biomolecule deposition in the sampled tissue. Sequentially sampled vibrissae (whiskers) provide a chronology of biogeochemical data, although knowledge of vibrissal growth is required for temporal interpretations. We sampled vibrissae from southern elephant seals Mirounga leonina (hereafter SES) at Marion Island, southern Indian Ocean, to address the following aims: (1) define the prevalence and timing of their vibrissal replacement, (2) determine the vibrissal regrowth rate and temporal resolution of isotopic data captured along the length of sequentially sampled vibrissae, and (3) explore assumptions regarding their vibrissal growth. Contrary to the previously described asynchronous vibrissal shedding pattern of SES, 71.1% of individuals displayed vibrissal shedding during the annual pelage moult. Furthermore, vibrissal growth ceased once the asymptotic length was reached, and the vibrissae were retained before being replaced. Vibrissae with known growth histories were resampled at multiple known intervals to control for unknown growth starting dates. Vibrissae followed a von Bertalanffy growth function as the growth rate decreased near the asymptotic length. The resolution of the isotopic data obtainable per 2 mm section ranged from 3.5 d at the vibrissal tip to >40 d at the base. Using these defined growth rates and shedding patterns, researchers can prudently apply timestamps to stable isotope values along vibrissae. C1 [Luebcker, Nico; de Bruyn, P. J. Nico; Bester, Marthan N.] Univ Pretoria, Mammal Res Inst, Dept Zool & Entomol, Private Bag X20, ZA-0028 Pretoria, South Africa. [Condit, Richard] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Beltran, Roxanne S.] Univ Alaska Anchorage, Dept Biol Sci, Anchorage, AK 99508 USA. [Beltran, Roxanne S.] Univ Alaska, Dept Biol & Wildlife, Fairbanks, AK 99775 USA. RP Lubcker, N (reprint author), Univ Pretoria, Mammal Res Inst, Dept Zool & Entomol, Private Bag X20, ZA-0028 Pretoria, South Africa. EM nlubcker@zoology.up.ac.za FU South African Department of Science and Technology; National Research Foundation (NRF), within the South African National Antarctic Programme (SANAP) FX Field personnel followed the guidelines for handling and treatment of marine mammals in field research supported by the Society for Marine Mammalogy (Gales et al. 2009). The tagging and handling of seals at Marion Island are carried out under the provisions of the South African Sea Birds and Seals Protection Act, 1973 (Act 46, 1973), the Marine Living Resources Act, 1998 (Act 18 of 1998) and the Prince Edward Islands Management Plan. The project has ethics clearance from the Animal Use and Care Committee (AUCC) of the Faculty of Veterinary Science, University of Pretoria, under AUCC 040827-022, AUCC 040827-023, AUCC 040827-024 and EC030602-016 and is carried out under permit from the Director-General: Department of Environmental Affairs, South Africa. Funding was provided by the South African Department of Science and Technology, through the National Research Foundation (NRF), within the South African National Antarctic Programme (SANAP). The Department of Environmental Affairs (DEA) provided logistical support at Marion Island. The opinions and conclusions drawn and discussed are attributed to the authors and not necessarily to the NRF. We thank the various dedicated collaborators, as well as field and laboratory assistants, in particular, Wiam Haddad, Mia Wege, Hennie Louw, Christiaan Brink, Frikkie van der Vyver, Dr Grant Hall, Nicolas Prinsloo, Andre van Tonder, Tanita Cronje, Inger Fabris-Rotelli and Christine Kraam winkel. NR 42 TC 0 Z9 0 U1 7 U2 7 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD NOV 9 PY 2016 VL 559 BP 243 EP 255 DI 10.3354/meps11899 PG 13 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA EC6CW UT WOS:000388225000019 ER PT J AU Labandeira, CC Kustatscher, E Wappler, T AF Labandeira, Conrad C. Kustatscher, Evelyn Wappler, Torsten TI Floral Assemblages and Patterns of Insect Herbivory during the Permian to Triassic of Northeastern Italy SO PLOS ONE LA English DT Article ID NORTH-CENTRAL TEXAS; PRA-DELLA-VACCA; FOREST-NATIONAL-PARK; PLANT-ARTHROPOD INTERACTIONS; NEW-SOUTH-WALES; COAL MEASURES; COMPONENT COMMUNITY; MASS EXTINCTION; EUROPEAN RUSSIA; SEED-FERNS AB To discern the effect of the end-Permian (P-Tr) ecological crisis on land, interactions between plants and their insect herbivores were examined for four time intervals containing ten major floras from the Dolomites of northeastern Italy during a Permian-Triassic interval. These floras are: (i) the Kungurian Tregiovo Flora; (ii) the Wuchiapingian Bletterbach Flora; (iii) three Anisian floras; and (iv) five Ladinian floras. Derived plant-insect interactional data is based on 4242 plant specimens (1995 Permian, 2247 Triassic) allocated to 86 fossil taxa (32 Permian, 56 Triassic), representing lycophytes, sphenophytes, pteridophytes, pterido-sperms, ginkgophytes, cycadophytes and coniferophytes from 37 million-year interval (23 m. yr. Permian, 14 m. yr. Triassic). Major Kungurian herbivorized plants were unaffiliated taxa and pteridosperms; later during the Wuchiapingian cycadophytes were predominantly consumed. For the Anisian, pteridosperms and cycadophytes were preferentially consumed, and subordinately pteridophytes, lycophytes and conifers. Ladinian herbivores overwhelming targeted pteridosperms and subordinately cycadophytes and conifers. Throughout the interval the percentage of insect-damaged leaves in bulk floras, as a proportion of total leaves examined, varied from 3.6% for the Kungurian (N = 464 leaves), 1.95% for the Wuchiapingian (N = 1531), 11.65% for the pooled Anisian (N = 1324), to 10.72% for the pooled Ladinian (N = 923), documenting an overall herbivory rise. The percentage of generalized consumption, equivalent to external foliage feeding, consistently exceeded the level of specialized consumption from internal feeding. Generalized damage ranged from 73.6% (Kungurian) of all feeding damage, to 79% (Wuchiapingian), 65.5% (pooled Anisian) and 73.2% (pooled Ladinian). Generalized-to-specialized ratios show minimal change through the interval, although herbivore component community structure (herbivore species feeding on a single plant-host species) increasingly was partitioned from Wuchiapingian to Ladinian. The Paleozoic plant with the richest herbivore component community, the coniferophyte Pseudovoltzia liebeana, harbored four damage types (DTs), whereas its Triassic parallel, the pteridosperm Scytophyllum bergeri housed 11 DTs, almost four times that of P. liebeana. Although generalized DTs of P. liebeana were similar to S. bergeri, there was expansion of Triassic specialized feeding types, including leaf mining. Permian-Triassic generalized herbivory remained relatively constant, but specialized herbivores more finely partitioned plant- host tissues via new feeding modes, especially in the Anisian. Insect-damaged leaf percentages for Dolomites Kungurian and Wuchiapingian floras were similar to those of lower Permian, north-central Texas, but only one-third that of southeastern Brazil. Global herbivore patterns for Early Triassic plant-insect interactions remain unknown. C1 [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Kustatscher, Evelyn] Museum Nat South Tyrol, Bindergasse 1, I-39100 Bozen Bolzano, Italy. [Kustatscher, Evelyn] Ludwig Maximilians Univ & Bayer Staatssammlung Pa, Dept Geo & Umweltwissensch, Palaontol & Geobiol, Richard Wagner Str 10, D-80333 Munich, Germany. [Wappler, Torsten] Univ Bonn, Steinmann Inst, Nussallee 8, D-53115 Bonn, Germany. RP Wappler, T (reprint author), Univ Bonn, Steinmann Inst, Nussallee 8, D-53115 Bonn, Germany. EM twappler@uni-bonn.de OI Wappler, Torsten/0000-0003-1592-0988 FU Deutsche Forschungsgemeinschaft (DFG) [WA 1496/8-1]; Promotion of Educational Policies, University; Research Department of the Autonomous Province of Bolzano-South Tyrol; Euregio Tirol-SiAtirol-Trentino Science Fund FX This research was possible thanks to grants of the Deutsche Forschungsgemeinschaft (DFG, Heisenberg grant WA 1496/8-1) to TW. The study of the material has been partly carried out within the project "The Permian-Triassic ecological crisis in the Dolomites: extinction and recovery dynamics in Terrestrial Ecosystems" financed by the Promotion of Educational Policies, University and Research Department of the Autonomous Province of Bolzano-South Tyrol and by the "The end-Permian mass extinction in the Southern and Eastern Alps: extinction rates vs taphonomic biases in different depositional environments" financed by the Euregio Tirol-SiAtirol-Trentino Science Fund. NR 181 TC 0 Z9 0 U1 5 U2 5 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD NOV 9 PY 2016 VL 11 IS 11 AR e0165205 DI 10.1371/journal.pone.0165205 PG 49 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB9OG UT WOS:000387724300031 PM 27829032 ER PT J AU Kuntner, M Cheng, RC Kralj-Fiser, S Liao, CP Schneider, JM Elgar, MA AF Kuntner, Matjaz Cheng, Ren-Chung Kralj-Fiser, Simona Liao, Chen-Pan Schneider, Jutta M. Elgar, Mark A. TI The evolution of genital complexity and mating rates in sexually size dimorphic spiders SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Sexual selection; Sexual size dimorphism; Sexual conflict; Female gigantism; Sexually antagonistic coevolution; Nephila ID ORB-WEB SPIDER; NEPHILA PLUMIPES ARANEOIDEA; MALE-MALE COMPETITION; SPERM COMPETITION; WEAVING SPIDER; ANTAGONISTIC COEVOLUTION; PHYLOGENETIC ANALYSIS; MALE ADAPTATION; MATE CHOICE; WATER STRIDERS AB Background: Genital diversity may arise through sexual conflict over polyandry, where male genital features function to manipulate female mating frequency against her interest. Correlated genital evolution across animal groups is consistent with this view, but a link between genital complexity and mating rates remains to be established. In sexually size dimorphic spiders, golden orbweaving spiders (Nephilidae) males mutilate their genitals to form genital plugs, but these plugs do not always prevent female polyandry. In a comparative framework, we test whether male and female genital complexity coevolve, and how these morphologies, as well as sexual cannibalism, relate to the evolution of mating systems. Results: Using a combination of comparative tests, we show that male genital complexity negatively correlates with female mating rates, and that levels of sexual cannibalism negatively correlate with male mating rates. We also confirm a positive correlation between male and female genital complexity. The macroevolutionary trajectory is consistent with a repeated evolution from polyandry to monandry coinciding with the evolution towards more complex male genitals. Conclusions: These results are consistent with the predictions from sexual conflict theory, although sexual conflict may not be the only mechanism responsible for the evolution of genital complexity and mating systems. Nevertheless, our comparative evidence suggests that in golden orbweavers, male genital complexity limits female mating rates, and sexual cannibalism by females coincides with monogyny. C1 [Kuntner, Matjaz; Cheng, Ren-Chung; Kralj-Fiser, Simona] Slovenian Acad Sci & Arts, Inst Biol Res, Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. [Liao, Chen-Pan] Tunghai Univ, Dept Life Sci, Taichung, Taiwan. [Schneider, Jutta M.] Univ Hamburg, Inst Zool, Biozentrum Grindel, Hamburg, Germany. [Elgar, Mark A.] Univ Melbourne, Sch Biosci, Melbourne, Vic 3010, Australia. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol Res, Ljubljana, Slovenia.; Kuntner, M (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. EM kuntner@gmail.com RI Schneider, Jutta /G-3727-2010; OI Kuntner, Matjaz/0000-0002-0057-2178 FU Slovenian Research Agency [P1-10236, J1-6729]; Australian Research Council FX MK, RCC and SKF were supported by the Slovenian Research Agency (grants P1-10236 and J1-6729 to MK); and MAE was supported by the Australian Research Council. NR 93 TC 0 Z9 0 U1 12 U2 12 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD NOV 9 PY 2016 VL 16 AR 242 DI 10.1186/s12862-016-0821-y PG 9 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA EB9PJ UT WOS:000387727200001 PM 27829358 ER PT J AU Zliobaite, I Rinne, J Toth, AB Mechenich, M Liu, LP Behrensmeyer, AK Fortelius, M AF Zliobaite, Indre Rinne, Janne Toth, Aniko B. Mechenich, Michael Liu, Liping Behrensmeyer, Anna K. Fortelius, Mikael TI Herbivore teeth predict climatic limits in Kenyan ecosystems SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE herbivorous mammals; dental traits; ecometrics; Kenya; paleoecology ID MAMMALS AB A major focus in evolutionary biology is to understand how the evolution of organisms relates to changes in their physical environment. In the terrestrial realm, the interrelationships among climate, vegetation, and herbivores lie at the heart of this question. Here we introduce and test a scoring scheme for functional traits present on the worn surfaces of large mammalian herbivore teeth to capture their relationship to environmental conditions. We modeled local precipitation, temperature, primary productivity, and vegetation index as functions of dental traits of large mammal species in 13 national parks in Kenya over the past 60 y. We found that these dental traits can accurately estimate local climate and environment, even at small spatial scales within areas of relatively uniform climate ( within two ecoregions), and that they predict limiting conditions better than average conditions. These findings demonstrate that the evolution of key functional properties of organisms may be more reflective of demands during recurring adverse episodes than under average conditions or during isolated severe events. C1 [Zliobaite, Indre; Rinne, Janne; Mechenich, Michael; Fortelius, Mikael] Univ Helsinki, Dept Geosci & Geog, FI-00014 Helsinki, Finland. [Zliobaite, Indre] Aalto Univ, Helsinki Inst Informat Technol, FI-00076 Aalto, Finland. [Rinne, Janne] Lund Univ, Dept Phys Geog & Ecosyst Sci, S-22362 Lund, Sweden. [Toth, Aniko B.; Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Evolut Terr Ecosyst Program, Washington, DC 20013 USA. [Toth, Aniko B.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Liu, Liping] Swedish Museum Nat Hist, Dept Paleobiol, SE-11418 Stockholm, Sweden. [Fortelius, Mikael] Univ Oslo, Dept Biosci, Ctr Ecol & Evolutionary Synth, NO-0316 Oslo, Norway. [Fortelius, Mikael] Museum Nat Hist, D-10115 Berlin, Germany. RP Zliobaite, I (reprint author), Univ Helsinki, Dept Geosci & Geog, FI-00014 Helsinki, Finland.; Zliobaite, I (reprint author), Aalto Univ, Helsinki Inst Informat Technol, FI-00076 Aalto, Finland. EM indre.zliobaite@helsinki.fi RI Rinne, Janne/A-6302-2008; OI Rinne, Janne/0000-0003-1168-7138; Fortelius, Mikael/0000-0002-4851-783X; Zliobaite, Indre/0000-0003-2427-5407 FU Academy of Finland (Expected Climate Change and Options for European Silviculture project); Evolution of Terrestrial Ecosystems Program; Natural History Research Experiences program at the National Museum of Natural History, Smithsonian Institution; Alexander von Humboldt Foundation FX Aleksis Karme and Juha Saarinen helped develop the FCT scheme, and Nikos Solounias helped to form the new Greek terms. A.B.T. and A.K.B. thank S. Kate Lyons and members of the National Museum of Natural History Ecological Reading Group for help with data compilation for the Kenyan national parks and reserves. The research leading to these results was funded in part by the Academy of Finland (Expected Climate Change and Options for European Silviculture project). Funding for data compilation by A.B.T., as published previously (12), was provided by the Evolution of Terrestrial Ecosystems Program and the Natural History Research Experiences program at the National Museum of Natural History, Smithsonian Institution. M.F. was the recipient of a research award from the Alexander von Humboldt Foundation. This is Evolution of Terrestrial Ecosystems Program (ETE) publication 344. It is also and equally a contribution from the Valio Armas Korvenkontio Unit of Dental Anatomy in Relation to Evolutionary Theory. NR 22 TC 1 Z9 1 U1 4 U2 4 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD NOV 8 PY 2016 VL 113 IS 45 BP 12751 EP 12756 DI 10.1073/pnas.1609409113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EC4CL UT WOS:000388073300064 ER PT J AU Childress, MJ Tucker, BE Yuan, F Scalzo, R Ruiter, A Seitenzahl, I Zhang, B Schmidt, B Anguiano, B Aniyan, S Bayliss, DDR Bento, J Bessell, M Bian, F Davies, R Dopita, M Fogarty, L Fraser-McKelvie, A Freeman, K Kuruwita, R Medling, AM Murphy, SJ Murphy, SJ Owers, M Panther, F Sweet, SM Thomas, AD Zhou, G AF Childress, Michael J. Tucker, Brad E. Yuan, Fang Scalzo, Richard Ruiter, Ashley Seitenzahl, Ivo Zhang, Bonnie Schmidt, Brian Anguiano, Borja Aniyan, Suryashree Bayliss, Daniel D. R. Bento, Joao Bessell, Michael Bian, Fuyan Davies, Rebecca Dopita, Michael Fogarty, Lisa Fraser-McKelvie, Amelia Freeman, Ken Kuruwita, Rajika Medling, Anne M. Murphy, Simon J. Murphy, Simon J. Owers, Matthew Panther, Fiona Sweet, Sarah M. Thomas, Adam D. Zhou, George TI The ANU WiFeS SuperNovA Programme (AWSNAP) SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE supernovae: general; supernovae: individual: (SN 2012dn) ID FIELD SPECTROGRAPH WIFES; MASS-METALLICITY RELATION; CORE-COLLAPSE SUPERNOVAE; HIGH-VELOCITY FEATURES; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; IA SUPERNOVAE; OPTICAL-SPECTRA; WHITE-DWARF; SN 2011FE AB This paper presents the first major data release and survey description for the ANUWiFeS SuperNovA Programme. ANU WiFeS SuperNovA Programme is an ongoing supernova spectroscopy campaign utilising the Wide Field Spectrograph on the Australian National University 2.3-m telescope. The first and primary data release of this programme (AWSNAP-DR1) releases 357 spectra of 175 unique objects collected over 82 equivalent full nights of observing from 2012 July to 2015 August. These spectra have been made publicly available via the WISEREP supernova spectroscopy repository. We analyse the ANUWiFeS SuperNovA Programme sample of Type Ia supernova spectra, including measurements of narrow sodium absorption features afforded by the high spectral resolution of the Wide Field Spectrograph instrument. In some cases, we were able to use the integral-field nature of the Wide Field Spectrograph instrument to measure the rotation velocity of the SN host galaxy near the SN location in order to obtain precision sodium absorption velocities. We also present an extensive time series of SN 2012dn, including a near-nebular spectrum which both confirms its 'super-Chandrasekhar' status and enables measurement of the sub-solar host metallicity at the SN site. C1 [Childress, Michael J.; Tucker, Brad E.; Yuan, Fang; Scalzo, Richard; Ruiter, Ashley; Seitenzahl, Ivo; Zhang, Bonnie; Schmidt, Brian; Aniyan, Suryashree; Bayliss, Daniel D. R.; Bento, Joao; Bessell, Michael; Bian, Fuyan; Davies, Rebecca; Dopita, Michael; Freeman, Ken; Kuruwita, Rajika; Medling, Anne M.; Murphy, Simon J.; Panther, Fiona; Sweet, Sarah M.; Thomas, Adam D.; Zhou, George] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Childress, Michael J.; Tucker, Brad E.; Yuan, Fang; Ruiter, Ashley; Seitenzahl, Ivo; Panther, Fiona] ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT, Australia. [Childress, Michael J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Anguiano, Borja; Owers, Matthew] Macquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia. [Bayliss, Daniel D. R.] Univ Geneva, Observ Astron, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. [Fogarty, Lisa; Murphy, Simon J.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Fraser-McKelvie, Amelia] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia. [Fraser-McKelvie, Amelia] Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia. [Murphy, Simon J.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Owers, Matthew] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. [Zhou, George] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Childress, MJ (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia.; Childress, MJ (reprint author), ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT, Australia.; Childress, MJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM m.j.childress@soton.ac.uk OI Schmidt, Brian/0000-0001-6589-1287; Scalzo, Richard/0000-0003-3740-1214 FU Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Australian Research Council Laureate Grant [FL0992131] FX This research was conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. IRS was supported by Australian Research Council Laureate Grant FL0992131. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System (ADS). NR 120 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD NOV 8 PY 2016 VL 33 AR e055 DI 10.1017/pasa.2016.47 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC5OY UT WOS:000388186700001 ER PT J AU Seersholm, FV Pedersen, MW Soe, MJ Shokry, H Mak, SST Ruter, A Raghavan, M Fitzhugh, W Kjaer, KH Willerslev, E Meldgaard, M Kapel, CMO Hansen, AJ AF Seersholm, Frederik Valeur Pedersen, Mikkel Winther Soe, Martin Jensen Shokry, Hussein Mak, Sarah Siu Tze Ruter, Anthony Raghavan, Maanasa Fitzhugh, William Kjaer, Kurt H. Willerslev, Eske Meldgaard, Morten Kapel, Christian M. O. Hansen, Anders Johannes TI DNA evidence of bowhead whale exploitation by Greenlandic Paleo-Inuit 4,000 years ago SO NATURE COMMUNICATIONS LA English DT Article ID ANCIENT DNA; NORSE GREENLAND; GENOME SEQUENCE; WEST GREENLAND; THULE CULTURE; ICE-AGE; MACROFOSSILS; SETTLEMENT; SEDIMENTS; INSIGHTS AB The demographic history of Greenland is characterized by recurrent migrations and extinctions since the first humans arrived 4,500 years ago. Our current understanding of these extinct cultures relies primarily on preserved fossils found in their archaeological deposits, which hold valuable information on past subsistence practices. However, some exploited taxa, though economically important, comprise only a small fraction of these sub-fossil assemblages. Here we reconstruct a comprehensive record of past subsistence economies in Greenland by sequencing ancient DNA from four well-described midden deposits. Our results confirm that the species found in the fossil record, like harp seal and ringed seal, were a vital part of Inuit subsistence, but also add a new dimension with evidence that caribou, walrus and whale species played a more prominent role for the survival of Paleo-Inuit cultures than previously reported. Most notably, we report evidence of bowhead whale exploitation by the Saqqaq culture 4,000 years ago. C1 [Seersholm, Frederik Valeur; Pedersen, Mikkel Winther; Soe, Martin Jensen; Shokry, Hussein; Mak, Sarah Siu Tze; Ruter, Anthony; Raghavan, Maanasa; Kjaer, Kurt H.; Willerslev, Eske; Meldgaard, Morten; Hansen, Anders Johannes] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, DK-1350 Copenhagen, Denmark. [Seersholm, Frederik Valeur] Curtin Univ, Dept Environm & Agr, Trace & Environm DNA TrEnD Lab, Perth, WA 6102, Australia. [Soe, Martin Jensen; Kapel, Christian M. O.] Univ Copenhagen, Dept Plant & Environm Sci, DK-1871 Frederiksberg, Denmark. [Raghavan, Maanasa; Willerslev, Eske] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Fitzhugh, William] Smithsonian Inst, Washington, DC 20013 USA. [Meldgaard, Morten] Univ Greenland, Manutooq 1, Nuussuaq 3905, Greenland. RP Seersholm, FV; Pedersen, MW (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, DK-1350 Copenhagen, Denmark.; Seersholm, FV (reprint author), Curtin Univ, Dept Environm & Agr, Trace & Environm DNA TrEnD Lab, Perth, WA 6102, Australia. EM frederikseersholm@gmail.com; mwpedersen@snm.ku.dk RI Kapel, Christian/G-9168-2014; OI Kapel, Christian/0000-0002-9539-457X; Soe, Martin/0000-0002-0386-6294; Pedersen, Mikkel Winther/0000-0002-7291-8887; Mak, Sarah S.T./0000-0003-1119-0519 FU Danish Advanced Technology Foundation; University of Copenhagen Initiative 'The Genomic History of Denmark'; Villum Foundation FX We thank Bjarne Gronnow for his advice and expertise concerning Saqqaq culture archaeology. Furthermore we thank Anders Anker Bjork for providing the map of Greenland presented in Fig. 1. This work was supported by the Danish Advanced Technology Foundation, the University of Copenhagen 2016 Initiative 'The Genomic History of Denmark' and the Villum Foundation through the pilot project 'Alle Tiders Mennesker'. Special thanks to the Greenland National Museum & Archive in Nuuk, Christian Koch Madsen and Ann Eileen Lennert. NR 59 TC 0 Z9 0 U1 19 U2 19 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD NOV 8 PY 2016 VL 7 AR 13389 DI 10.1038/ncomms13389 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB3JE UT WOS:000387259600001 PM 27824339 ER PT J AU Smith-Vaniz, WF Johnson, GD AF Smith-Vaniz, William F. Johnson, G. David TI Hidden diversity in deep-water bandfishes: review of Owstonia with descriptions of twenty-one new species (Teleostei: Cepolidae: Owstoniinae) SO ZOOTAXA LA English DT Article DE Pisces; Cepolidae; Owstonia; bandfishes; taxonomy; Indo-West Pacific ID PERCIFORMES CEPOLIDAE; FISHES; PISCES AB The bandfish family Cepolidae, comprising the subfamilies Owstoniinae and Cepolinae, is characterized, and defining characters of the three groups are identified and discussed. Characters of larvae of both subfamilies are described and illustrated. Six nominal genera of owstoniines had been proposed by various authors, but we recognize only Owstonia Tanaka. Utility of selected identification characters of the genus are discussed. Differences in lateral-line patterns have been the primary character used by some recent authors for recognition of two owstoniine genera, with Sphenanthias Weber possessing the plesiomorphic lateral-line condition. Several other patterns also occur in these fishes bringing into question the phylogenetic significance of lateral line plasticity. Sexual dimorphism in pelvic fin lengths is also present in several species. Identification keys, descriptions, synonymies, distribution maps and photographs or illustrations are provided for all Owstonia species for which adults are available. Although only 15 valid species were previously known, a remarkable hidden diversity of these fishes was discovered in major museum collections with the following 21 species here described as new: O. ainonaka (eastern Australia), O. contodon (Philippines), O. crassa (New Caledonia and Solomon Islands), O. dispar (Solomon Islands), O. elongata (New Caledonia and Vanuatu), O. fallax (eastern Australia and New Caledonia), O. geminata (Vanuatu and Philippines), O. hastata (eastern Australia), O. hawaiiensis (Hawaiian Islands); O. ignota (Mariana Islands), O. lepiota (Tanzania), O. melanoptera (Philippines), O. merensis (eastern Australia, Torres Strait), O. mundyi (Kiribati, Christmas Island), O. nalani (eastern Australia and New Caledonia), O. nudibucca (eastern Indian Ocean, Mentawai Islands and off Myanmar), O. psilos (Western Australia), O. raredonae (Mozambique), O. rhamma (Vanuatu), O. scottensis (Western Australia, Scott Reefs) and O. similis (Madagascar). Several specimens based on small juveniles, which we describe as Owstonia sp., appear to be additional new species but are not formally described as such. C1 [Smith-Vaniz, William F.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. RP Smith-Vaniz, WF (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM smithvaniz@gmail.com; johnson@si.edu NR 81 TC 0 Z9 0 U1 3 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD NOV 8 PY 2016 VL 4187 IS 1 BP 1 EP 103 DI 10.11646/zootaxa.4187.1.1 PG 103 WC Zoology SC Zoology GA EB0GE UT WOS:000387020900001 ER PT J AU Collins-Fekete, CA Brousmiche, S Portillo, SKN Beaulieu, L Seco, J AF Collins-Fekete, Charles-Antoine Brousmiche, Sebastien Portillo, Stephen K. N. Beaulieu, Luc Seco, Joao TI A maximum likelihood method for high resolution proton radiography/proton CT SO PHYSICS IN MEDICINE AND BIOLOGY LA English DT Article DE proton imaging; proton radiography; multiple Coulomb scattering; proton computed tomography ID COMPUTED-TOMOGRAPHY; STOPPING POWER; MONTE-CARLO; RANGE CALCULATIONS; PATH FORMALISM; LIKELY PATH; X-RAY; THERAPY; CALIBRATION; SCATTERING AB Multiple Coulomb scattering (MCS) is the largest contributor to blurring in proton imaging. In this work, we developed a maximum likelihood least squares estimator that improves proton radiography's spatial resolution. The water equivalent thickness (WET) through projections defined from the source to the detector pixels were estimated such that they maximizes the likelihood of the energy loss of every proton crossing the volume. The length spent in each projection was calculated through the optimized cubic spline path estimate. The proton radiographies were produced using Geant4 simulations. Three phantoms were studied here: a slanted cube in a tank of water to measure 2D spatial resolution, a voxelized head phantom for clinical performance evaluation as well as a parametric Catphan phantom (CTP528) for 3D spatial resolution. Two proton beam configurations were used: a parallel and a conical beam. Proton beams of 200 and 330 MeV were simulated to acquire the radiography. Spatial resolution is increased from 2.44 lp cm(-1) to 4.53 lp cm(-1) in the 200 MeV beam and from 3.49 lp cm(-1) to 5.76 lp cm(-1) in the 330 MeV beam. Beam configurations do not affect the reconstructed spatial resolution as investigated between a radiography acquired with the parallel (3.49 lp cm(-1) to 5.76 lp cm(-1)) or conical beam (from 3.49 lp cm(-1) to 5.56 lp cm(-1)). The improved images were then used as input in a photon tomography algorithm. The proton CT reconstruction of the Catphan phantom shows high spatial resolution (from 2.79 to 5.55 lp cm(-1) for the parallel beam and from 3.03 to 5.15 lp cm(-1) for the conical beam) and the reconstruction of the head phantom, although qualitative, shows high contrast in the gradient region. The proposed formulation of the optimization demonstrates serious potential to increase the spatial resolution (up by 65%) in proton radiography and greatly accelerate proton computed tomography reconstruction. C1 [Collins-Fekete, Charles-Antoine; Beaulieu, Luc] Univ Laval, Dept Phys Genie Phys & Opt, Quebec City, PQ, Canada. [Collins-Fekete, Charles-Antoine; Beaulieu, Luc] Univ Laval, Ctr Rech Canc, Quebec City, PQ, Canada. [Collins-Fekete, Charles-Antoine; Beaulieu, Luc] CHU Quebec, Dept Radiooncol, Quebec City, PQ, Canada. [Collins-Fekete, Charles-Antoine; Beaulieu, Luc] CHU Quebec, CRCHU Quebec, Quebec City, PQ, Canada. [Collins-Fekete, Charles-Antoine; Seco, Joao] Massachusetts Gen Hosp, Francis H Burr Proton Therapy Ctr, Dept Radiat Oncol, Boston, MA 02114 USA. [Brousmiche, Sebastien] IBA, Louvain La Neuve, Belgium. [Portillo, Stephen K. N.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Seco, Joao] Deutsch Krebsforschungszentrum Heidelberg, Baden Baden, DE, Germany. [Seco, Joao] Heidelberg Univ, Dept Phys & Astron Heidelberg, Baden Baden, DE, Germany. RP Collins-Fekete, CA (reprint author), Univ Laval, Dept Phys Genie Phys & Opt, Quebec City, PQ, Canada.; Collins-Fekete, CA (reprint author), Univ Laval, Ctr Rech Canc, Quebec City, PQ, Canada.; Collins-Fekete, CA (reprint author), CHU Quebec, Dept Radiooncol, Quebec City, PQ, Canada.; Collins-Fekete, CA (reprint author), CHU Quebec, CRCHU Quebec, Quebec City, PQ, Canada.; Collins-Fekete, CA (reprint author), Massachusetts Gen Hosp, Francis H Burr Proton Therapy Ctr, Dept Radiat Oncol, Boston, MA 02114 USA. EM charles-antoine.collins-fekete.1@ulaval.ca OI Portillo, Stephen/0000-0001-8132-8056 FU Fonds de Recherche du Quebec-Nature et technologies; CREATE Medical Physics Research Training Network grant of the Natural Sciences and Engineering Research Council [432290]; Canada Foundation for Innovation (CFI); NanoQuebec; RMGA; Fonds de Recherche du Quebec-Nature et Technologies (FRQ-NT) FX The authors would like to acknowledge Zachary Slepian for helpful discussions and help in text revision. Charles-Antoine Collins-Fekete is supported by a scholarship from Fonds de Recherche du Quebec-Nature et technologies. CACF acknowledges partial support by the CREATE Medical Physics Research Training Network grant of the Natural Sciences and Engineering Research Council (Grant number: 432290). Computations were made on the supercomputer Colosse from Universite Laval, managed by Calcul Quebec and Compute Canada. The operation of this supercomputer is funded by the Canada Foundation for Innovation (CFI), NanoQuebec, RMGA and the Fonds de Recherche du Quebec-Nature et Technologies (FRQ-NT). NR 33 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0031-9155 EI 1361-6560 J9 PHYS MED BIOL JI Phys. Med. Biol. PD NOV 3 PY 2016 VL 61 IS 23 BP 8232 EP 8248 DI 10.1088/0031-9155/61/23/8232 PG 17 WC Engineering, Biomedical; Radiology, Nuclear Medicine & Medical Imaging SC Engineering; Radiology, Nuclear Medicine & Medical Imaging GA EC1QS UT WOS:000387882600001 PM 27811399 ER PT J AU Wang, JJ Yang, YP Sun, H Wen, J Deng, T Nie, ZL Meng, Y AF Wang, Jia-Jian Yang, Yong-Ping Sun, Hang Wen, Jun Deng, Tao Nie, Ze-Long Meng, Ying TI The Biogeographic South-North Divide of Polygonatum (Asparagaceae Tribe Polygonateae) within Eastern Asia and Its Recent Dispersals in the Northern Hemisphere SO PLOS ONE LA English DT Article ID HISTORICAL BIOGEOGRAPHY; MOLECULAR PHYLOGENETICS; DNA-SEQUENCES; EVOLUTION; TERTIARY; AMERICA; DIVERSIFICATION; DISJUNCT; ANGIOSPERMS; CHINA AB Eastern Asia (EA) is a key region for the diversification of flowering plants in the Northern Hemisphere, but few studies have focused on the biogeographic history within EA in the context of the other northern continents. Polygonatum is an important medicinal genus widely distributed in the Northern Hemisphere with its highest species richness in EA, and it represents an excellent model for studying the evolution of biogeographic patterns in this region. Divergence time estimation was used to examine the biogeographic history of Polygonatum based on nuclear ITS and four plastid sequences (rbcL, matK, psbA-trnH and trnC-petN) from 30 Polygonatum species and 35 outgroup taxa. The ancestral area of Polygonatum and subsequent dispersal routes were inferred using Bayes-Lagrange. Polygonatum was estimated to have originated in southern EA during the middle Miocene (14.34-13.57 Ma) with subsequent south-to-north expansion in the late Miocene. Multiple intercontinental dispersal events were inferred between EA and Europe or North America, and all of them have occurred recently in the late Miocene to Pliocene. The separation of Polygonatum into the south and north lineages and their subsequent diversifications in the late Miocene supports the existence of a biogeographic divide between the northern and southern parts of EA that also coincides with the retreat and redevelopment of the arid zone in EA in the Neogene. Our results demonstrate the complexity of biogeographic history of Polygonatum in the Northern Hemisphere including early vicariance followed by frequent and recent dispersals in the Neogene. C1 [Wang, Jia-Jian; Nie, Ze-Long; Meng, Ying] Jishou Univ, Coll Biol & Environm Sci, Key Lab Plant Resources Conservat & Utilizat, Jishou 416000, Hunan, Peoples R China. [Yang, Yong-Ping; Sun, Hang; Deng, Tao] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog E Asia, Kunming 650201, Yunnan, Peoples R China. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. RP Nie, ZL; Meng, Y (reprint author), Jishou Univ, Coll Biol & Environm Sci, Key Lab Plant Resources Conservat & Utilizat, Jishou 416000, Hunan, Peoples R China. EM zelongnie@163.com; mengyingnie@163.com FU Natural Sciences Foundation of China [NSFC31270273, 31570211, 31590823]; Laboratory of Analytical Biology of the National Museum of Natural History; Smithsonian Institution; Small Grants Program of the National Museum of Natural History FX This study was supported by grants from Natural Sciences Foundation of China (NSFC31270273, 31570211, 31590823). This work was also partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, Smithsonian Institution, as well as the Small Grants Program of the National Museum of Natural History, the Smithsonian Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 0 Z9 0 U1 24 U2 24 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD NOV 3 PY 2016 VL 11 IS 11 AR e0166134 DI 10.1371/journal.pone.0166134 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EA8SX UT WOS:000386910000104 ER PT J AU MacIsaac, HJ De Roy, EM Leung, B Grgicak-Mannion, A Ruiz, GM AF MacIsaac, Hugh J. De Roy, Emma M. Leung, Brian Grgicak-Mannion, Alice Ruiz, Gregory M. TI Possible Ballast Water Transfer of Lionfish to the Eastern Pacific Ocean SO PLOS ONE LA English DT Article ID PTEROIS-VOLITANS LINNAEUS; GULF-OF-MEXICO; RECENT INVASION; ATLANTIC COAST; UNITED-STATES; SCORPAENIDAE; TOLERANCE; AMERICA; SHIPS; NORTH AB The Indo-Pacific Red Lionfish was first reported off the Florida coast in 1985, following which it has spread across much of the SE USA, Gulf of Mexico, and Caribbean Sea. Lion fish negatively impact fish and invertebrate assemblages and abundances, thus further spread is cause for concern. To date, the fish has not been reported on the Pacific coast of North or Central America. Here we examine the possibility of ballast water transfer of lion fish from colonized areas in the Atlantic Ocean to USA ports on the Pacific coast. Over an eight-year period, we documented 27 commercial vessel-trips in which ballast water was loaded in colonized sites and later discharged untreated into Pacific coast ports in the USA. California had the highest number of discharges including San Francisco Bay and Los Angeles-Long Beach. A species distribution model suggests that the probability of lionfish establishment is low for the western USA, Colombia and Panama, low to medium for Costa Rica, Nicaragua, El Salvador and Guatemala, medium to high for mainland Ecuador, and very high for western Mexico, Peru and the Galapagos Islands. Given the species' intolerance of freshwater conditions, we propose that ballast water exchange be conducted in Gatun Lake, Panama for western-bound vessels carrying 'risky' ballast water to prevent invasion of the eastern Pacific Ocean. C1 [MacIsaac, Hugh J.; De Roy, Emma M.; Grgicak-Mannion, Alice] Univ Windsor, Great Lakes Inst Environm Res, Windsor, ON, Canada. [Leung, Brian] McGill Univ, Dept Biol, Montreal, PQ, Canada. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RP MacIsaac, HJ (reprint author), Univ Windsor, Great Lakes Inst Environm Res, Windsor, ON, Canada. EM hughm@uwindsor.ca OI Ruiz, Gregory/0000-0003-2499-441X FU Smithsonian Institution; NSERC Discovery grants; Canada Research Chair FX Financial support was provided by the Smithsonian Institution to GMR, NSERC Discovery grants to BL and HJM, and a Canada Research Chair to HJM.; We are grateful to two reviewers who helped improve the manuscript. Financial support was provided by the Smithsonian Institution to GMR, NSERC Discovery grants to BL and HJM, and a Canada Research Chair to HJM. We are grateful to the National Ballast Information Clearinghouse for database records, Dr. Pam Schofield of the United States Geological Survey for lionfish reports, Dr. Matthias Herb org for initial data compilation and GIS support and Dr. Nick Mandrak for information regarding lionfish biology. NR 46 TC 0 Z9 0 U1 16 U2 16 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD NOV 2 PY 2016 VL 11 IS 11 AR e0165584 DI 10.1371/journal.pone.0165584 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EA6DJ UT WOS:000386715500038 PM 27806076 ER PT J AU Gingerich, O AF Gingerich, Owen TI The Almagest: Introduction to the Mathematics of the Heavens SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ogingerich@cfa.harvard.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD NOV PY 2016 VL 47 BP 448 EP 449 DI 10.1177/0021828616668752 PN 4 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA EI6OQ UT WOS:000392615600022 ER PT J AU Nami, HG de la Pena, P Vasquez, CA Feathers, J Wurz, S AF Nami, Hugo G. de la Pena, Paloma Vasquez, Carlos A. Feathers, James Wurz, Sarah TI Palaeomagnetic results and new dates of sedimentary deposits from Klasies River Cave 1, South Africa SO SOUTH AFRICAN JOURNAL OF SCIENCE LA English DT Article DE Klasies River main site; palaeomagnetism; palaeosecular variation; Late Pleistocene; Holocene ID MIDDLE STONE-AGE; LASCHAMP GEOMAGNETIC EXCURSION; MAGNETIC-FIELD; SECULAR VARIATION; BRUNHES CHRON; ARGENTINA; SITE; SUSCEPTIBILITY; STRATIGRAPHY; REVERSALS AB Palaeomagnetic data from Klasies River main site Cave 1 (Eastern Cape Province, South Africa) are reported. Natural remanent magnetisation directions obtained from 77 oriented samples were determined by progressive alternating field demagnetisation methodology. Three palaeomagnetic samplings from the Witness Baulk from the Middle Stone Age (MSA) Late Pleistocene White Sand member and the Holocene Later Stone Age (LSA) middens in Cave 1 were dated and analysed to obtain the palaeomagnetic directions recorded in the sediments. Here we provide new optically stimulated luminescence (OSL) dates for the White Sand Member, and new accelerator mass spectrometry (AMS) radiocarbon dates for the LSA midden of areas not previously dated. The palaeomagnetic analysis took into account rock magnetism and directional analysis. The former reveals that the main magnetic carrier was magnetite; the latter shows that characteristic remanent magnetisation of normal and anomalous directions were observed in the lower portion of the White Sand Member and LSA midden. Normal directions correspond to the palaeosecular variation record for South Africa during the Late Pleistocene. On the other hand, the anomalous directions recorded in the LSA midden might represent the likely Sterno-Etrussia geomagnetic field excursion which occurred during the Late Holocene and is observed in other places on the planet. Finally, the directional data obtained are a potential tool for discussing the age of deposits corresponding to those periods. Significance: New dates confirm and extend previous age determinations for the LSA and White Sand Member from Klasies River C1 [Nami, Hugo G.; Vasquez, Carlos A.] Univ Buenos Aires, Dept Geol Sci, Daniel A Valencio Palaeomagnetism Lab, CONICET IGEBA, Buenos Aires, DF, Argentina. [Nami, Hugo G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [de la Pena, Paloma; Wurz, Sarah] Univ Witwatersrand, Evolutionary Studies Inst, Sch Geosci, Johannesburg, South Africa. [de la Pena, Paloma; Wurz, Sarah] Univ Witwatersrand, Sch Geog Archaeol & Environm Sci, Johannesburg, South Africa. [Vasquez, Carlos A.] Univ Buenos Aires, Ciclo Basico Comun, Buenos Aires, DF, Argentina. [Feathers, James] Univ Washington, Luminescence Lab, Seattle, WA 98195 USA. RP de la Pena, P (reprint author), Univ Witwatersrand, Evolutionary Studies Inst, Sch Geosci, Johannesburg, South Africa.; de la Pena, P (reprint author), Univ Witwatersrand, Sch Geog Archaeol & Environm Sci, Johannesburg, South Africa. EM paloma.delapenya@gmail.com FU DST/NRF Centre of Excellence in Palaeosciences; Palaeontological Scientific Trust; National Research Foundation (South Africa) FX DST/NRF Centre of Excellence in Palaeosciences; Palaeontological Scientific Trust; National Research Foundation (South Africa) NR 62 TC 0 Z9 0 U1 2 U2 2 PU ACAD SCIENCE SOUTH AFRICA A S S AF PI LYNWOOD RIDGE PA PO BOX 72135, LYNWOOD RIDGE 0040, SOUTH AFRICA SN 0038-2353 EI 1996-7489 J9 S AFR J SCI JI S. Afr. J. Sci. PD NOV-DEC PY 2016 VL 112 IS 11-12 AR 2016-0051 DI 10.17159/sajs.2016/20160051 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EI5FE UT WOS:000392518700009 ER PT J AU Brandl, SJ Emslie, MJ Ceccarelli, DM AF Brandl, Simon J. Emslie, Michael J. Ceccarelli, Daniela M. TI Habitat degradation increases functional originality in highly diverse coral reef fish assemblages SO ECOSPHERE LA English DT Article DE biodiversity; climatic disturbance; coral cover; coral reef fish; Cyclone Ita; functional redundancy; functional richness; functional traits; habitat loss; niche partitioning; response diversity; tropical storm ID ECOSYSTEM FUNCTION; BIODIVERSITY LOSS; SPECIES RICHNESS; TROPICAL FOREST; LAND-USE; REDUNDANCY; COMMUNITIES; DISTURBANCE; VULNERABILITY; PRODUCTIVITY AB As anthropogenic and natural disturbances intensify, there is mounting concern about the loss of functionally important or unique species. Functional redundancy, or the presence of several different species occupying similar functional niches, can provide insurance against diversity loss, but evidence for this effect is rare. Likewise, the ways in which functional redundancy patterns respond to disturbances are poorly known, impeding a thorough understanding of community-level dynamics post disturbance. Here, we use an extensive reduction of hard coral cover following a tropical cyclone to explore the response of a highly diverse reef fish assemblage to habitat degradation. We demonstrate that despite clear trait value-specific susceptibility of fishes to the disturbance, five of six functional indices (including functional richness and evenness) showed no relationship with habitat degradation. In contrast, functional originality, which quantifies the average functional uniqueness of species within an assemblage, increased post disturbance, exhibiting a negative, albeit weak, relationship with decreasing coral cover. The increase in functional originality is simultaneously driven by the loss of functionally similar species in susceptible groups (predominantly small planktivorous and omnivorous species that associate with live coral habitat) and the addition of functionally unique species in groups that benefit from the disturbance (large, non-territorial species feeding on algal turfs, detritus, and invertebrates). Our findings suggest that coral reefs with high coral cover can foster fish assemblages with low functional originality (i.e., high functional redundancy), therefore preventing detectible changes in some of the most commonly applied functional indices post disturbance. However, we caution that the limited resolution of trait-based approaches may mask the loss of functionally unique species and that, with an increase in functional originality, post disturbance assemblages may be less suited to adequately maintain certain ecosystem functions in the face of future disturbances. Thus, there is an urgent need for further exploration of the dynamics between disturbances, functional redundancy, and ecosystem functioning. C1 [Brandl, Simon J.; Ceccarelli, Daniela M.] James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia. [Brandl, Simon J.] James Cook Univ, Coll Sci & Engn, Marine Biol & Aquaculture, Townsville, Qld 4811, Australia. [Brandl, Simon J.] Smithsonian Environm Res Ctr, Tennenbaum Marine Observ Network, Edgewater, MD 21037 USA. [Emslie, Michael J.] Australian Inst Marine Sci, PMB 3 Townsville Mail Ctr, Townsville, Qld 4810, Australia. RP Brandl, SJ (reprint author), James Cook Univ, ARC Ctr Excellence Coral Reef Studies, Townsville, Qld 4811, Australia.; Brandl, SJ (reprint author), James Cook Univ, Coll Sci & Engn, Marine Biol & Aquaculture, Townsville, Qld 4811, Australia.; Brandl, SJ (reprint author), Smithsonian Environm Res Ctr, Tennenbaum Marine Observ Network, Edgewater, MD 21037 USA. EM brandls@si.edu FU John and Laurine Proud Family Estate Trust; Lizard Island Reef Research Foundation; Australian Museum's Lizard Island Research Station; Australian Museum; Isobel Bennett Marine Biology Fellowship FX We thank the John and Laurine Proud Family Estate Trust and the Lizard Island Reef Research Foundation and the Australian Museum's Lizard Island Research Station for support. This study was funded by the Australian Museum and an Isobel Bennett Marine Biology 2015 Fellowship (DMC). We thank Z Richards and T Lewis for field assistance and JEK Byrnes, M Carr, JM Casey, MJ Kramer, BS Cheng, TL Barnum, and four anonymous reviewers for helpful comments on the manuscript. SJB, MJE, and DMC designed the study; DMC and MJE collected the data; SJB performed the analyses; and SJB, MJE, and DMC wrote the manuscript. NR 83 TC 0 Z9 0 U1 14 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD NOV PY 2016 VL 7 IS 11 AR e01557 DI 10.1002/ecs2.1557 PG 19 WC Ecology SC Environmental Sciences & Ecology GA EI1AP UT WOS:000392207600003 ER PT J AU Elvis, M Milligan, T Krolikowski, A AF Elvis, Martin Milligan, Tony Krolikowski, Alanna TI The peaks of eternal light: A near-term property issue on the moon SO SPACE POLICY LA English DT Article DE Moon; Resources; Legal; Policy; Ethics ID ASTEROIDS; RIGHTS; SPACE AB The Outer Space Treaty makes it clear that the Moon is the 'province of all mankind', with the latter ordinarily understood to exclude state or private appropriation of any portion of its surface. However, there are indeterminacies in the Treaty and in space law generally over the issue of appropriation. These indeterminacies might permit a close approximation to a property claim or some manner of 'quasi-property'. The recently revealed highly inhomogeneous distribution of lunar resources changes the context of these issues. We illustrate this altered situation by considering the Peaks of Eternal Light. They occupy about one square kilometer of the lunar surface. We consider a thought experiment in which a Solar telescope is placed on one of the Peaks of Eternal Light at the lunar South pole for scientific research. Its operation would require non-disturbance, and hence that the Peak remain unvisited by others, effectively establishing a claim of protective exclusion and de facto appropriation. Such a telescope would be relatively easy to emplace with today's technology and so poses a near-term property issue on the Moon. While effective appropriation of a Peak might proceed without raising some of the familiar problems associated with commercial development (especially lunar mining), the possibility of such appropriation nonetheless raises some significant issues concerning justice and the safeguarding of scientific practice oh the lunar surface. We consider this issue from scientific, technical, ethical and policy viewpoints. Published by Elsevier Ltd. C1 [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Milligan, Tony] Kings Coll London, Dept Theol & Religious Studies, Virginia Wolf Bldg,22 Kingsway, London WC2B 6NR, England. [Krolikowski, Alanna] Georg August Univ Gottingen, Heinrich Duker Weg 14, D-37073 Gottingen, Germany. RP Elvis, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM melvis@cfa.harvard.edu; alanna.krolikowski@gmail.com OI Elvis, Martin/0000-0001-5060-1398 FU NSF [1066293]; Social Sciences and Humanities Research Council of Canada FX We thank Bob Bussey for permission to reproduce the figures. ME thanks the Aspen Center for Physics, funded by NSF grant #1066293, for their hospitality while this paper was completed. AK gratefully acknowledges a Postdoctoral Fellowship from the Social Sciences and Humanities Research Council of Canada. NR 33 TC 0 Z9 0 U1 1 U2 1 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0265-9646 EI 1879-338X J9 SPACE POLICY JI Space Policy PD NOV PY 2016 VL 38 BP 30 EP 38 DI 10.1016/j.spacepol.2016.05.011 PG 9 WC International Relations; Social Sciences, Interdisciplinary SC International Relations; Social Sciences - Other Topics GA EH6QJ UT WOS:000391898700005 ER PT J AU Paudel, S Brown, JL Thapaliya, S Dhakal, IP Mikota, SK Gairhe, KP Shimozuru, M Tsubota, T AF Paudel, Sarad Brown, Janine L. Thapaliya, Sharada Dhakal, Ishwari P. Mikota, Susan K. Gairhe, Kamal P. Shimozuru, Michito Tsubota, Toshio TI Comparison of cortisol and thyroid hormones between tuberculosis-suspect and healthy elephants of Nepal SO JOURNAL OF VETERINARY MEDICAL SCIENCE LA English DT Article DE Asian elephant; cortisol; thyroxine; triiodothyronine; tuberculosis ID CAPTIVE ASIAN ELEPHANTS; MYCOBACTERIUM-TUBERCULOSIS; COMPARATIVE ENDOCRINOLOGY; AFRICAN ELEPHANTS; INFECTION; DIAGNOSIS; MAXIMUS AB We compared cortisol and thyroid hormone (T3 and T4) concentrations between tuberculosis (TB)-suspected (n=10) and healthy (n=10) elephants of Nepal. Whole blood was collected from captive elephants throughout Nepal, and TB testing was performed using the ElephantTB STAT-PAK (R) and DPP VetTB (R) serological assays that detect antibodies against Mycobacterium tuberculosis and M bovis in elephant serum. Cortisol, T3 and T4 were quantified by competitive enzyme immunoassays, and the results showed no significant differences in hormone concentrations between TB-suspect and healthy elephants. These preliminary data suggest neither adrenal nor thyroid function is altered by TB disease status. However, more elephants, including those positively diagnosed for TB by trunk wash cultures, need to be evaluated over time to confirm results. C1 [Paudel, Sarad; Shimozuru, Michito; Tsubota, Toshio] Hokkaido Univ, Grad Sch Vet Med, Lab Wildlife Biol & Med, Kita Ku, Kita 18,Nishi 9, Sapporo, Hokkaido 0600818, Japan. [Brown, Janine L.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Thapaliya, Sharada; Dhakal, Ishwari P.] Agr & Forestry Univ, Rampur, Chitwan, Nepal. [Mikota, Susan K.] Elephant Care Int, 166 Limo View Lane, Hohenwald, TN 38462 USA. [Gairhe, Kamal P.] Dept Natl Pk & Wildlife Conservat, Kathmandu, Nepal. RP Tsubota, T (reprint author), Hokkaido Univ, Grad Sch Vet Med, Lab Wildlife Biol & Med, Kita 18 Nishi 9, Sapporo, Hokkaido 0600818, Japan. EM tsubota@vetmed.hokudai.ac.jp FU Richard Hughes Scholarship, Chester Zoo, U. K.; National Trust for Nature Conservation (NTNC); Nepal Department of National Parks and Wildlife Conservation (DNPWC); Ministry for Forests and Soil Conservation; Government of Nepal; Asian Rhino and Elephant Action Strategy (AREAS), WWF-Nepal FX We acknowledge National Trust for Nature Conservation (NTNC), the Nepal Department of National Parks and Wildlife Conservation (DNPWC), the Ministry for Forests and Soil Conservation, and the Government of Nepal for their kind support and co-operation for this project. We are thankful to Chitra Bahadur Khadka, Purushottam Pandey and Kiran Rijal for helping with sample collection from elephants. We thank Christy Williams, Asian Rhino and Elephant Action Strategy (AREAS), WWF-Nepal for providing funding support in part. Additional funding support was provided by the Richard Hughes Scholarship, Chester Zoo, U. K. NR 22 TC 0 Z9 0 U1 0 U2 0 PU JAPAN SOC VET SCI PI TOKYO PA UNIV TOKYO, 1-1-1 YAYOI, BUNKYO-KU, TOKYO, 103, JAPAN SN 0916-7250 EI 1347-7439 J9 J VET MED SCI JI J. Vet. Med. Sci. PD NOV PY 2016 VL 78 IS 11 BP 1713 EP 1716 DI 10.1292/jvms.16-0212 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA EF9DN UT WOS:000390631000013 PM 27452878 ER PT J AU Schneider, H Schuettpelz, E AF Schneider, Harald Schuettpelz, Eric TI Systematics and evolution of lycophytes and ferns SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Editorial Material ID CLIMATE-CHANGE; DIVERSITY; GENETICS C1 [Schneider, Harald] Sun Yat Sen Univ, Sch Life Sci, Inst Ecol & Evolut, Guangzhou, Guangdong, Peoples R China. [Schneider, Harald] Nat Hist Museum, Dept Life Sci, London, England. [Schuettpelz, Eric] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Schneider, H (reprint author), Sun Yat Sen Univ, Sch Life Sci, Inst Ecol & Evolut, Guangzhou, Guangdong, Peoples R China.; Schneider, H (reprint author), Nat Hist Museum, Dept Life Sci, London, England. NR 20 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD NOV PY 2016 VL 54 IS 6 SI SI BP 561 EP 562 DI 10.1111/jse.12231 PG 2 WC Plant Sciences SC Plant Sciences GA EF4TB UT WOS:000390323800001 ER PT J AU Schuettpelz, E Schneider, H Smith, AR Hovenkamp, P Prado, J Rouhan, G Salino, A Sundue, M Almeida, TE Parris, B Sessa, EB Field, AR de Gasper, AL Rothfels, CJ Windham, MD Lehnert, M Dauphin, B Ebihara, A Lehtonen, S Schwartsburd, PB Metzgar, J Zhang, LB Kuo, LY Brownsey, PJ Kato, M Arana, MD Assis, FC Barker, MS Barrington, DS Chang, HM Chang, YH Chao, YS Chen, CW Chen, DK Chiou, WL Dittrich, VAD Duan, YF Dubuisson, JY Farrar, DR Fawcett, S Galan, JMGY Goes-Neto, LAD Grant, JR Grusz, AL Haufler, C Hauk, W He, H Hennequin, S Hirai, RY Huiet, L Kessler, M Korall, P Labiak, PH Larsson, A Leon, B Li, CX Li, FW Link-Perez, M Liu, HM Lu, NT Meza-Torres, EI Miao, XY Moran, R Mynssen, CM Nagalingum, N Ollgaard, B Paul, AM Pereira, JBD Perrie, LR Ponce, M Ranker, TA Schulz, C Shinohara, W Shmakov, A Sigel, EM de Souza, FS Sylvestre, LD Testo, W Triana-Moreno, LA Tsutsumi, C Tuomisto, H Valdespino, IA Vasco, A Viveros, RS Weakley, A Wei, R Weststrand, S Wolf, PG Yatskievych, G Xu, XG Yan, YH Zhang, L Zhang, XC Zhou, XM AF Schuettpelz, Eric Schneider, Harald Smith, Alan R. Hovenkamp, Peter Prado, Jefferson Rouhan, Germinal Salino, Alexandre Sundue, Michael Almeida, Thais Elias Parris, Barbara Sessa, Emily B. Field, Ashley R. de Gasper, Andre Luis Rothfels, Carl J. Windham, Michael D. Lehnert, Marcus Dauphin, Benjamin Ebihara, Atsushi Lehtonen, Samuli Schwartsburd, Pedro Bond Metzgar, Jordan Zhang, Li-Bing Kuo, Li-Yaung Brownsey, Patrick J. Kato, Masahiro Arana, Marcelo Daniel Assis, Francine C. Barker, Michael S. Barrington, David S. Chang, Ho-Ming Chang, Yi-Han Chao, Yi-Shan Chen, Cheng-Wei Chen, De-Kui Chiou, Wen-Liang Dittrich, Vinicius Antonio de Oliveira Duan, Yi-Fan Dubuisson, Jean-Yves Farrar, Donald R. Fawcett, Susan Gabriel y Galan, Jose Maria Goes-Neto, Luiz Armando de Araujo Grant, Jason R. Grusz, Amanda L. Haufler, Christopher Hauk, Warren He, Hai Hennequin, Sabine Hirai, Regina Yoshie Huiet, Layne Kessler, Michael Korall, Petra Labiak, Paulo H. Larsson, Anders Leon, Blanca Li, Chun-Xiang Li, Fay-Wei Link-Perez, Melanie Liu, Hong-Mei Ngan Thi Lu Meza-Torres, Esteban I. Miao, Xin-Yuan Moran, Robbin Mynssen, Claudine Massi Nagalingum, Nathalie Ollgaard, Benjamin Paul, Alison M. Pereira, Jovani B. de S. Perrie, Leon R. Ponce, Monica Ranker, Tom A. Schulz, Christian Shinohara, Wataru Shmakov, Alexander Sigel, Erin M. de Souza, Filipe Soares Sylvestre, Lana da Silva Testo, Weston Triana-Moreno, Luz Amparo Tsutsumi, Chie Tuomisto, Hanna Valdespino, Ivan A. Vasco, Alejandra Viveros, Raquel Stauffer Weakley, Alan Wei, Ran Weststrand, Stina Wolf, Paul G. Yatskievych, George Xu, Xiao-Gang Yan, Yue-Hong Zhang, Liang Zhang, Xian-Chun Zhou, Xin-Mao CA Pteridophyte Phylogeny Grp TI A community-derived classification for extant lycophytes and ferns SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE classification; ferns; lycophytes; monophyly; phylogeny; pteridophytes ID EUPOLYPOD II FERNS; DNA-SEQUENCE DATA; MOLECULAR PHYLOGENETIC-RELATIONSHIPS; SUBG. NOTHOPERANEMA DRYOPTERIDACEAE; GENUS TRICHOMANES HYMENOPHYLLACEAE; GRAMMITID FERNS; TAXONOMIC REVISION; RBCL SEQUENCES; GENERIC CLASSIFICATION; HISTORICAL BIOGEOGRAPHY AB Phylogeny has long informed pteridophyte classification. As our ability to infer evolutionary trees has improved, classifications aimed at recognizing natural groups have become increasingly predictive and stable. Here, we provide a modern, comprehensive classification for lycophytes and ferns, down to the genus level, utilizing a community-based approach. We use monophyly as the primary criterion for the recognition of taxa, but also aim to preserve existing taxa and circumscriptions that are both widely accepted and consistent with our understanding of pteridophyte phylogeny. In total, this classification treats an estimated 11 916 species in 337 genera, 51 families, 14 orders, and two classes. This classification is not intended as the final word on lycophyte and fern taxonomy, but rather a summary statement of current hypotheses, derived from the best available data and shaped by those most familiar with the plants in question. We hope that it will serve as a resource for those wanting references to the recent literature on pteridophyte phylogeny and classification, a framework for guiding future investigations, and a stimulus to further discourse. C1 [Schuettpelz, Eric; Sigel, Erin M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Schneider, Harald] Sun Yat Sen Univ, Sch Life Sci, Inst Ecol & Evolut, Guangzhou, Guangdong, Peoples R China. [Schneider, Harald; Paul, Alison M.] Nat Hist Museum, Dept Life Sci, London, England. [Smith, Alan R.; Rothfels, Carl J.] Univ Calif Berkeley, Univ Herbarium, Berkeley, CA 94720 USA. [Hovenkamp, Peter] Naturalis Biodivers Ctr, Res & Educ, Leiden, Netherlands. [Prado, Jefferson; Hirai, Regina Yoshie] Herbario SP, Inst Bot, Sao Paulo, Brazil. [Rouhan, Germinal] Sorbonne Univ, Museum Natl Hist Nat, Herbier Natl, Inst Systemat,Evolut,Biodivers, Paris, France. [Salino, Alexandre; Assis, Francine C.; Goes-Neto, Luiz Armando de Araujo; de Souza, Filipe Soares; Viveros, Raquel Stauffer] Univ Fed Minas Gerais, Dept Bot, Belo Horizonte, MG, Brazil. [Sundue, Michael; Barrington, David S.; Fawcett, Susan; Testo, Weston] Univ Vermont, Dept Plant Biol, Pringle Herbarium, Burlington, VT 05405 USA. [Almeida, Thais Elias] Univ Fed Oeste Para, Herbario HSTM, Santarem, Para, Brazil. [Parris, Barbara] Fern Res Fdn, Kerikeri, New Zealand. [Sessa, Emily B.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Field, Ashley R.] James Cook Univ, Dept Sci & Innovat, Queensland Herbarium, Townsville, Qld, Australia. [Field, Ashley R.] James Cook Univ, Australian Trop Herbarium, Townsville, Qld, Australia. [de Gasper, Andre Luis] Univ Reg Blumenau, Dept Ciencias Nat, Blumenau, SC, Brazil. [Rothfels, Carl J.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Windham, Michael D.; Huiet, Layne; Li, Fay-Wei] Duke Univ, Dept Biol, Durham, NC 27706 USA. [Lehnert, Marcus] Rhein Friedrich Wilhelms Univ Bonn, Nees Inst Biodivers Pflanzen, Bonn, Germany. [Dauphin, Benjamin; Grant, Jason R.] Univ Neuchatel, Inst Biol, Lab Bot Evolut, Neuchatel, Switzerland. [Ebihara, Atsushi; Kato, Masahiro; Tsutsumi, Chie] Natl Museum Nat & Sci, Dept Bot, Tokyo, Japan. [Lehtonen, Samuli; Tuomisto, Hanna] Univ Turku, Dept Biol, Turku, Finland. [Schwartsburd, Pedro Bond] Univ Fed Vicosa, Dept Biol Vegetal, Vicosa, MG, Brazil. [Metzgar, Jordan] Univ Alaska Fairbanks, Museum North, Fairbanks, AK USA. [Zhang, Li-Bing; Zhou, Xin-Mao] Missouri Bot Garden, Pob 299, St Louis, MO 63166 USA. [Kuo, Li-Yaung] Natl Taiwan Univ, Inst Ecol & Evolutionary Biol, Taipei, Taiwan. [Brownsey, Patrick J.; Perrie, Leon R.] Museum New Zealand Te Papa Tongarewa, Collect Res & Learning, Wellington, New Zealand. [Arana, Marcelo Daniel] Univ Nacl Rio Cuarto, Dept Ciencias Nat, Rio Cuarto, Argentina. [Barker, Michael S.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Chang, Ho-Ming] Taiwan Endem Species Res Inst, Div Bot, Nantou, Taiwan. [Chang, Yi-Han] Taiwan Forestry Res Inst, Hengchun Res Ctr, Taipei, Taiwan. [Chao, Yi-Shan] Kaohsiung Med Univ, Dept Biomed Sci & Environm Biol, Kaohsiung, Taiwan. [Chen, Cheng-Wei] Taiwan Forestry Res Inst, Div Bot Garden, Taipei, Taiwan. [Chen, De-Kui; He, Hai] Chongqing Normal Univ, Coll Life Sci, Chongqing, Peoples R China. [Chiou, Wen-Liang] Taiwan Forestry Res Inst, Herbarium, Taipei, Taiwan. [Dittrich, Vinicius Antonio de Oliveira] Univ Fed Juiz de Fora, Dept Bot, Juiz De Fora, MG, Brazil. [Duan, Yi-Fan; Xu, Xiao-Gang] Nanjing Forestry Univ, Coll Biol & Environm, Dept Bot, Nanjing, Jiangsu, Peoples R China. [Dubuisson, Jean-Yves; Hennequin, Sabine] Univ Paris 06, Sorbonne Univ, Inst Systemat, Evolut,Biodivers, Paris, France. [Farrar, Donald R.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA USA. [Gabriel y Galan, Jose Maria] Univ Complutense Madrid, Dept Biol Vegetal 1, Madrid, Spain. [Grusz, Amanda L.] Univ Minnesota Duluth, Dept Biol, Duluth, MN USA. [Haufler, Christopher] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Hauk, Warren] Denison Univ, Dept Biol, Granville, OH 43023 USA. [Kessler, Michael] Univ Zurich, Dept Systemat & Evolutionary Bot, Zurich, Switzerland. [Korall, Petra; Larsson, Anders; Weststrand, Stina] Uppsala Univ, Evolutionary Biol Ctr, Dept Organismal Biol, Uppsala, Sweden. [Labiak, Paulo H.] Univ Fed Parana, Dept Bot, Curitiba, Parana, Brazil. [Leon, Blanca; Yatskievych, George] Univ Texas Austin, Plant Resources Ctr, Austin, TX 78712 USA. [Li, Chun-Xiang; Miao, Xin-Yuan] Chinese Acad Sci, Nanjing Inst Geol & Palaeontol, State Key Lab Palaeobiol & Stratig, Beijing, Peoples R China. [Link-Perez, Melanie] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Liu, Hong-Mei] Chinese Acad Sci, Fairylake Bot Garden, Shenzhen Key Lab Southern Subtrop Plant Divers, Beijing, Peoples R China. [Ngan Thi Lu] Vietnam Acad Sci & Technol, Vietnam Natl Museum Nat, Dept Bot, Hanoi, Vietnam. [Meza-Torres, Esteban I.] Univ Nacl Nordeste, Consejo Nacl Invest Cient & Tecn, Inst Bot Nordeste, Corrientes, Argentina. [Moran, Robbin] New York Bot Garden, Bronx, NY 10458 USA. [Mynssen, Claudine Massi] Inst Pesquisas Jardim Bot Rio de Janeiro, Inst Pesquisa, Diretoria Pesquisa, Rio De Janeiro, Brazil. [Nagalingum, Nathalie] Royal Bot Gardens & Domain Trust, Natl Herbarium New South Wales, Sydney, NSW, Australia. [Ollgaard, Benjamin] Aarhus Univ, Sect Ecoinformat & Biodivers, Aarhus, Denmark. [Pereira, Jovani B. de S.; Schulz, Christian] Ruhr Univ Bochum, Dept Evolut & Biodivers Plants, Bochum, Germany. [Ponce, Monica] Consejo Nacl Invest Cient & Tecn, Inst Bot Darwin, Buenos Aires, DF, Argentina. [Ranker, Tom A.] Univ Hawaii Manoa, Dept Bot, Honolulu, HI 96822 USA. [Shinohara, Wataru] Kagawa Univ, Fac Educ, Takamatsu, Kagawa, Japan. [Shmakov, Alexander] Altai State Univ, South Siberian Bot Garden, Barnaul, Russia. [Sylvestre, Lana da Silva] Univ Fed Rio de Janeiro, Dept Bot, Rio De Janeiro, Brazil. [Triana-Moreno, Luz Amparo] Univ Caldas, Dept Ciencias Biol, Manizales, Colombia. [Valdespino, Ivan A.] Univ Panama, Dept Bot, Panama City, Panama. [Vasco, Alejandra] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City, DF, Mexico. [Weakley, Alan] Univ North Carolina Chapel Hill, North Carolina Bot Garden, UNC Herbarium, Chapel Hill, NC USA. [Wei, Ran; Zhang, Xian-Chun] Chinese Acad Sci, Inst Bot, Beijing, Peoples R China. [Wolf, Paul G.] Utah State Univ, Dept Biol, Logan, UT 84322 USA. [Yan, Yue-Hong] Chinese Acad Sci, Shanghai Chenshan Plant Sci Res Ctr, Shanghai Chenshan Bot Garden, Beijing, Peoples R China. [Zhang, Liang] Chinese Acad Sci, Kunming Inst Bot, Beijing, Peoples R China. RP Schuettpelz, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA.; Schneider, H (reprint author), Sun Yat Sen Univ, Sch Life Sci, Inst Ecol & Evolut, Guangzhou, Guangdong, Peoples R China.; Schneider, H (reprint author), Nat Hist Museum, Dept Life Sci, London, England. EM schuettpelze@si.edu; haralds@mail.sysu.edu.cn RI Kessler, Michael/A-3605-2009; Hirai, Regina/K-3913-2013; Prado, Jefferson/C-4766-2012; OI Prado, Jefferson/0000-0003-4783-3125; Hovenkamp, Peter/0000-0002-4124-2175; Gabriel y Galan, Jose Maria/0000-0003-2786-0062 NR 319 TC 0 Z9 0 U1 16 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD NOV PY 2016 VL 54 IS 6 SI SI BP 563 EP 603 DI 10.1111/jse.12229 PG 41 WC Plant Sciences SC Plant Sciences GA EF4TB UT WOS:000390323800002 ER PT J AU Sigel, EM AF Sigel, Erin M. TI Genetic and genomic aspects of hybridization in ferns SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Review DE allopolyploidy; fixed heterozygosity; gene expression; genome evolution; homoploid hybrids; introgression; multiple origins; sterile hybrids ID APPALACHIAN ASPLENIUM COMPLEX; DRYOPTERIS SPINULOSA COMPLEX; POLYPODIUM-VULGARE COMPLEX; EASTERN NORTH-AMERICA; NUCLEAR-DNA AMOUNTS; RETICULATE EVOLUTION; ELECTROPHORETIC EVIDENCE; CHLOROPLAST DNA; HOMOSPOROUS FERNS; HYBRID SPECIATION AB The morphological and ecological intermediacy of hybrid taxa has long interested and challenged fern biologists, resulting in numerous systematic contributions focused on disentangling relationships within reticulate species complexes. From a genetic perspective, hybrid ferns are especially interesting because they represent the union of divergent parental genomes in unique evolutionary entities. This review summarizes advances in our knowledge of the genetic and genomic aspects of hybridization in ferns from the mid-20th century to the present. The different organismal products of hybridization, evolutionary aspects of additive and non-additive gene expression in allopolyploids, genetic and genomic mechanisms leading to gene silencing and loss, the roles of multiple origins and introgression for imparting genetic variation to hybrid fern taxa and their progenitors, and the utility of allopolyploid ferns to investigate mechanisms of genome evolution in the homosporous ferns are discussed. Comparisons are made to other plant lineages and important future research directions are highlighted, with the goal of stimulating additional research on hybrid ferns. C1 [Sigel, Erin M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166 POB 37012, Washington, DC 20013 USA. RP Sigel, EM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166 POB 37012, Washington, DC 20013 USA. EM SigelEM@si.edu FU Peter Buck Postdoctoral Fellowship at the National Museum of Natural History, Smithsonian Institution FX The author is grateful to A. Grusz, E. Schuettpelz, and C. Taylor for their helpful comments on this manuscript, and to R. Everly and the Smithsonian Libraries for help obtaining research materials. Two anonymous reviewers provided valuable comments and edits. This work was funded by a Peter Buck Postdoctoral Fellowship at the National Museum of Natural History, Smithsonian Institution. NR 234 TC 1 Z9 1 U1 9 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1674-4918 EI 1759-6831 J9 J SYST EVOL JI J. Syst. Evol. PD NOV PY 2016 VL 54 IS 6 SI SI BP 638 EP 655 DI 10.1111/jse.12226 PG 18 WC Plant Sciences SC Plant Sciences GA EF4TB UT WOS:000390323800006 ER PT J AU Lucking, R Nelsen, MP Aptroot, A Benatti, MN Binh, NQ Gueidan, C Gutierrez, MC Jungbluth, P Lumbsch, HT Marcelli, MP Moncada, B Naksuwankul, K Orozco, T Salazar-Allen, N Upreti, DK AF Luecking, Robert Nelsen, Matthew P. Aptroot, Andre Benatti, Michel N. Nguyen Quoc Binh Gueidan, Cecile Cecilia Gutierrez, Martha Jungbluth, Patricia Lumbsch, H. Thorsten Marcelli, Marcelo P. Moncada, Bibiana Naksuwankul, Khwanruan Orozco, Thelma Salazar-Allen, Noris Upreti, Dalip K. TI A pot-pourri of new species of Trypetheliaceae resulting from molecular phylogenetic studies SO LICHENOLOGIST LA English DT Article DE Brazil; Colombia; Fiji; lichen; New Caledonia; Panama; taxonomy; Vietnam ID LICHEN; FOREST; GENUS AB Based on separately obtained and analyzed molecular data and within the framework of a global revision of the family Trypetheliaceae, 21 new species are described, from the Neotropics and tropical Asia, in the genera Architrypethelium (1), Astrothelium (15), Bathelium (1), Nigrovothelium (1), Trypethelium (1), and Viridothelium (2), namely: Architrypethelium lauropaluanum Lucking, M. P. Nelsen & Marcelli sp. nov., differing from A. hyalinum in the perithecia immersed between coarse thallus verrucae and in the additional ascospore septa; Astrothelium aurantiacocinereum Lucking, Naksuwankul & Lumbsch sp. nov., differing from A. aeneum in the prominent, well-delimited, trypethelioid pseudostromata and the absence of pigment on the thallus surface, as well as in the barely lichenized thallus; A. carassense Lucking, M. P. Nelsen & Marcelli sp. nov., differing from A. purpurascens in orange, K+ red pseudostroma pigment and the slightly larger ascospores; A. cryptolucens Lucking, M. P. Nelsen & N. Salazar sp. nov., differing from A. carrascoense in the inspersed hymenium; A. fijiense Lucking, Naksuwankul & Lumbsch sp. nov., differing from A. cinereorosellum in the presence of lichexanthone on the well-delimited pseudostromata and in the slightly shorter ascospores; A. laevithallinum Lucking, M. P. Nelsen & Marcelli sp. nov., differing from A. endochryseum in the smooth thallus; A. leucosessile Lucking, M. P. Nelsen& Aptroot sp. nov., differing from A. phlyctaena in the conspicuous, sessile pseudostromata; A. macrostomoides Lucking, M. P. Nelsen & Benatti sp. nov., differing from A. macrostomum in the larger ascospores; A. megacrypticum Lucking, M. P. Nelsen & N. Salazar sp. nov., differing from A. longisporum in the single-spored asci and larger ascospores; A. nicaraguense Lucking, M. P. Nelsen & T. Orozco sp. nov., differing from A. gigantosporum in the smaller ascospores; A. norisianum Lucking, M. P. Nelsen & Aptroot sp. nov., differing from A. sepultum in the distinct, well-delimited pseudostromata; A. obtectum Lucking, M. P. Nelsen & Benatti sp. nov., differing from A. nigrocacuminum in the smaller ascospores; A. sordithecium Lucking, M. P. Nelsen & Marcelli sp. nov., differing from A. leucothelium in the inspersed hymenium and the absence of lichexanthone from the thallus surface outside the pseudostromata; A. subendochryseum Lucking, M. P. Nelsen & Marcelli sp. nov., differing from A. endochryseum in the absence of pigment in the pseudostromata and the lateral thallus cover of the pseudostromata; A. subinterjectum Lucking, M. P. Nelsen & Jungbluth sp. nov., differing from A. obtectum in the smaller pseudostromata and smaller ascospores, and from A. interjectum in the diffuse pseudostromata and smaller ascospores; Bathelium porinosporum Lucking, M. P. Nelsen & Gueidan sp. nov., differing from other Bathelium species in the 3-septate, euseptate ascospores; Nigrovothelium bullatum Lucking, Upreti & Lumbsch sp. nov., differing from N. tropicum in the bullate thallus; Trypethelium tolimense Lucking, Moncada & M. Gut. sp. nov., differing from T. xanthoplatystomum in the absence of a yellow-orange pigment on the pseudostromata and the K+ yellow (not K+ red) medullary pigment; Viridothelium tricolor Lucking, M. P. Nelsen & N. Salazar sp. nov., characterized by black perithecia with a lateral ostiole immersed in white pseudostromata strongly contrasting with the surrounding brown thallus, in combination with 2-spored asci and large, muriform ascospores; and V. vonkonratii Lucking, Naksuwankul & Lumbsch sp. nov., differing from V. virens in larger ascospores and mostly solitary ascomata. All species are illustrated and their taxonomy and phylogenetic relationships are discussed. ITS barcoding sequences are reported for five specimens of Bathelium porinosporum. C1 [Luecking, Robert] Bot Garden & Bot Museum Berlin, Konigin Luise Str 6-8, D-14195 Berlin, Germany. [Luecking, Robert; Nelsen, Matthew P.; Lumbsch, H. Thorsten] Field Museum, Integrat Res Ctr, 1400 South Lake Shore, Chicago, IL 60605 USA. [Aptroot, Andre] ABL Herbarium, Gvd Veenstr 107, NL-3762 XK Soest, Netherlands. [Benatti, Michel N.; Marcelli, Marcelo P.] Nucleo Pesquisa Micol, Inst Bot, Caixa Postal 68041, BR-04045972 Sao Paulo, Brazil. [Nguyen Quoc Binh] Vietnam Natl Museum Nat, Vietnam Acad Sci & Technol, Dept Biol, 18 Hoang Quoc Viet St, Hanoi, Vietnam. [Gueidan, Cecile] Nat Hist Museum, Dept Life Sci, Cromwell Rd, London SW7 5BD, England. [Gueidan, Cecile] CSIRO, Australian Natl Herbarium, Natl Facil & Collect, Natl Res Collect Australia, GPO Box 1600, Canberra, ACT 2601, Australia. [Cecilia Gutierrez, Martha] Univ Dist Francisco Jose de Caldas, Ingn Ambiental, Carrera 5 Este 15-82,Av Circunvalar, Bogota, Colombia. [Jungbluth, Patricia] Univ Fed Santa Maria, Dept Zooctenia & Ciencias Biol, Av Idependencia 3751, BR-98300000 Palmeira Das Missoes, RS, Brazil. [Moncada, Bibiana] Univ Dist Francisco Jose de Caldas, Cra 4 26D-54, Bogota, Colombia. [Moncada, Bibiana] Field Museum, Sci & Educ, 1400 South Lake Shore, Chicago, IL 60605 USA. [Naksuwankul, Khwanruan] Mahasarakham Univ, Dept Biol, Kantarawichai 44150, Maha Sarakham P, Thailand. [Naksuwankul, Khwanruan] Mahasarakham Univ, Nat Med Mushroom Museum, Fac Sci, Kantarawichai 44150, Maha Sarakham P, Thailand. [Salazar-Allen, Noris] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. [Orozco, Thelma] Univ Cent Amer, Herbario Nacl Nicaragua, Apartado 69, Managua, Nicaragua. [Upreti, Dalip K.] Natl Bot Res Inst CSIR, Rana Pratap Marg, Lucknow 226001, Uttar Pradesh, India. RP Lucking, R (reprint author), Bot Garden & Bot Museum Berlin, Konigin Luise Str 6-8, D-14195 Berlin, Germany.; Lucking, R (reprint author), Field Museum, Integrat Res Ctr, 1400 South Lake Shore, Chicago, IL 60605 USA. EM r.luecking@bgbm.org FU National Science Foundation [NSF-DEB 0715660, DEB-1025861, DEB-1145898]; Caterpillar(R) Company; Committee on Evolutionary Biology (University of Chicago); American Society of Plant Taxonomists; Brown Family Fellowship through the Field Museum; William Harper Rainey Fellowship through the University of Chicago; National Geographic Committee for Research and Exploration [8247-07]; Thai Research Fund; Mahasarakham University [RSA 5580045]; Mohamed bin Zayed Species Conservation Fund [11253111]; Negaunee Foundation; Universidad Distrital Francisco Jose de Caldas in Bogota, Colombia FX We are grateful to the National Science Foundation for funding aspects of this work through the grant NSF-DEB 0715660 "Neotropical Epiphytic Microlichens An Innovative Inventory of a Highly Diverse yet Little Known Group of Symbiotic Organisms" to The Field Museum (PI Robert Lucking). The Caterpillar (R) Company provided additional funds to study lichens from Panama. MN was further supported through a grant from the Committee on Evolutionary Biology (University of Chicago), a Graduate Student Research Grant from The American Society of Plant Taxonomists, and a Brown Family Fellowship through the Field Museum, as well as a William Harper Rainey Fellowship through the University of Chicago. Field support in Panama was provided by the University of Panama (Department of Botany) in the development of two lichen seminars (2009, 2011) during which the lichens were collected. Thanks also to Park authorities and rangers of Parque Nacional Altos de Campana during the field trips and to the Ministry of the Environment (formerly A.N.A.M.) for collection and export permits. In Colombia, logistical support was provided by the Universidad Distrital Francisco Jose de Caldas and the Cardenas Herrera family for access to their Finca El Santuario. For field support in Brazil, we thank the Universidade Estadual Paulista, campus Botucatu, and the administration of the Santuario do Caraca, as well as the owners of Fazenda Palmeira da Serra in Sao Paulo State. Work on Fiji was supported by the National Geographic Committee for Research and Exploration, Grant No. 8247-07. For field work in New Caledonia, we thank the Thai Research Fund and Mahasarakham University for providing financial assistance (K. Papong RSA 5580045), the National Science Foundation (Awards No. DEB-1025861 and DEB-1145898), the Mohamed bin Zayed Species Conservation Fund (Award No. 11253111), and the Negaunee Foundation. We also thank 'Direction du developpement economique et de l'environnement de la Province Nord', and 'Direction de l'environnement de la Province Sud' for plant permits to both provinces. KN also thanks Mahasarakham University, Thailand. The Universidad Distrital Francisco Jose de Caldas in Bogota, Colombia, is thanked for providing support to BM as part of the program 'Movilidad Academica' for professors. NR 21 TC 3 Z9 3 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0024-2829 EI 1096-1135 J9 LICHENOLOGIST JI Lichenologist PD NOV PY 2016 VL 48 IS 6 BP 639 EP 660 DI 10.1017/S0024282916000475 PG 22 WC Plant Sciences; Mycology SC Plant Sciences; Mycology GA EF5IT UT WOS:000390364600003 ER PT J AU Lucking, R Nelsen, MP Aptroot, A Barillas De Klee, R Bawingan, PA Benatti, MN Binh, NQ Bungartz, F Caceres, MES Canez, LD Chaves, JL Ertz, D Esquivel, RE Ferraro, LI Grijalva, A Gueidan, C Hernandez, JE Knight, A Lumbsch, HT Marcelli, MP Mercado-Diaz, JA Moncada, B Morales, EA Naksuwankul, K Orozco, T Parnmen, S Rivas Plata, E Salazar-Allen, N Spielmann, AA Ventura, N AF Luecking, Robert Nelsen, Matthew P. Aptroot, Andre Barillas De Klee, Roselvira Bawingan, Paulina A. Benatti, Michel N. Nguyen Quoc Binh Bungartz, Frank Caceres, Marcela E. S. Canez, Luciana da Silva Chaves, Jose-Luis Ertz, Damien Esmeralda Esquivel, Rhina Itati Ferraro, Lidia Grijalva, Alfredo Gueidan, Cecile Hernandez, Jesus E. Knight, Allison Lumbsch, H. Thorsten Marcelli, Marcelo P. Mercado-Diaz, Joel A. Moncada, Bibiana Morales, Eduardo A. Naksuwankul, Khwanruan Orozco, Thelma Parnmen, Sittiporn Rivas Plata, Eimy Salazar-Allen, Noris Spielmann, Adriano A. Ventura, Nohemy TI A phylogenetic framework for reassessing generic concepts and species delimitation in the lichenized family Trypetheliaceae (Ascomycota: Dothideomycetes) SO LICHENOLOGIST LA English DT Article DE evolution; genus concepts; lichenized fungi; phenotypic characters; species concepts ID MICROPROBE MASS-SPECTROMETRY; FLUORESCENCE MICROSCOPY; OSTROPALES GRAPHIDACEAE; PYRENOCARPOUS LICHENS; MOLECULAR-DATA; RIBOSOMAL DNA; GENUS; CLASSIFICATION; EVOLUTION; ALIGNMENT AB We provide an expanded and updated, 2-locus phylogeny (mtSSU, nuLSU) of the lichenized fungal family Trypetheliaceae, with a total of 196 ingroup OTUs, in order to further refine generic delimitations and species concepts in this family. As a result, the following 15 clades are recognized as separate genera, including five newly established genera: Aptrootia, Architrypethelium, Astrothelium (including the bulk of corticate species with astrothelioid ascospores; synonyms: Campylothelium, Cryptothelium, Laurera), Bathelium s. str. (excluding B. degenerans and relatives which fall into Astrothelium), the reinstated Bogoriella (for tropical, lichenized species previously placed in Mycomicrothelia), Constrictolumina gen. nov. (for tropical, lichenized species of Arthopyrenia), Dictyomeridium gen. nov. (for a subgroup of species with muriform ascospores previously placed in Polymeridium), Julella (provisionally, as the type species remains unsequenced), Marcelaria (Laurera purpurina complex), Nigrovothelium gen. nov. (for the Trypethelium tropicum group), Novomicrothelia gen. nov. (for an additional species previously placed in Mycomicrothelia), Polymeridium s. str., Pseudopyrenula, Trypethelium s. str. (T. eluteriae group), and Viridothelium gen. nov. (for the Trypethelium virens group). All recognized genera are phenotypically characterized and a discussion on the evolution of phenotypic features in the family is given. Based on the obtained phylogeny, species delimitations are revised and the importance of characters such as thallus morphology, hymenial inspersion, and secondary chemistry for taxonomic purposes is discussed, resulting in a refined species concept. C1 [Luecking, Robert] Bot Garden & Bot Museum Berlin, Konigin Luise Str 6-8, D-14195 Berlin, Germany. [Luecking, Robert; Nelsen, Matthew P.; Lumbsch, H. Thorsten; Mercado-Diaz, Joel A.; Rivas Plata, Eimy] Field Museum, Integrat Res Ctr, 1400 South Lake Shore Dr, Chicago, IL 60605 USA. [Mercado-Diaz, Joel A.] Univ Chicago, Comm Evolutionary Biol, 1025 E 57th St, Chicago, IL 60637 USA. [Aptroot, Andre] ABL Herbarium, Gvd Veenstr 107, NL-3762 XK Soest, Netherlands. [Barillas De Klee, Roselvira] Univ San Carlos, Fac Ciencias Quim & Farm, Escuela Biol, Zona 12, Guatemala City, Guatemala. [Bawingan, Paulina A.] St Louis Univ, Sch Nat Sci, Baguio, Philippines. [Benatti, Michel N.; Marcelli, Marcelo P.] Nucleo Pesquisa Micol, Inst Bot, Caixa Postal 68041, BR-04045972 Sao Paulo, Brazil. [Nguyen Quoc Binh] Vietnam Natl Museum Nat, Vietnam Acad Sci & Technol, Dept Biol, 18 Hoang Quoc Viet St, Hanoi, Vietnam. [Bungartz, Frank] Fdn Charles Darwin, Santa Cruz, Galapagos, Ecuador. [Bungartz, Frank] Schedestr 8, D-53113 Bonn, Germany. [Caceres, Marcela E. S.] Univ Fed Sergipe, Dept Biociencias, BR-49500000 Itabaiana, Sergipe, Brazil. [Canez, Luciana da Silva; Spielmann, Adriano A.] Univ Fed Mato Grosso do Sul, Ctr Ciencias Biol & Saude, Lab Liquenol, Cidade Univ,Caixa Postal 549, BR-79070900 Campo Grande, MS, Brazil. [Chaves, Jose-Luis] Inst Nacl Biodiversidad INBio, Lab Hongos, Apdo 22-3100, Santo Domingo De Heredia, Costa Rica. [Ertz, Damien] Bot Garden Meise, Dept Bryophytes Thallophytes BT, Nieuwelaan 38, B-1860 Meise, Belgium. [Esmeralda Esquivel, Rhina; Ventura, Nohemy] Univ El Salvador, Fac Ciencias Nat & Matemat, Escuela Biol, Ciudad Univ,Final Av Heroes & Martires 30 Julio, San Salvador, El Salvador. [Itati Ferraro, Lidia] Inst Bot Nordeste IBONE, Casilla Correo 209, RA-3400 Corrientes, Argentina. [Grijalva, Alfredo; Orozco, Thelma] Univ Cent Amer, Herbario Nacl Nicaragua, Apartado 69, Managua, Nicaragua. [Gueidan, Cecile] Nat Hist Museum, Dept Life Sci, Cromwell Rd, London SW7 5BD, England. [Gueidan, Cecile] CSIRO, Australian Natl Herbarium, Natl Facil & Collect, Natl Res Collect Australia, GPO Box 1600, Canberra, ACT 2601, Australia. [Hernandez, Jesus E.] Cent Univ Venezuela, Inst Expt Jardin Bot Dr Tobias Lasser, Caracas, Venezuela. [Knight, Allison] Univ Otago, Dept Bot, POB 56, Dunedin, New Zealand. [Moncada, Bibiana] Univ Dist Francisco Jose de Caldas, Biol, Torre Labs, Cra 4 26D-54, Bogota, Colombia. [Moncada, Bibiana] Field Museum, Sci & Educ, 1400 South Lake Shore, Chicago, IL 60605 USA. [Morales, Eduardo A.] Herbario Criptogam Univ Catolica Boliviana, Ingn Ambiental, Casilla Correos 5381, Cochabamba, Bolivia. [Naksuwankul, Khwanruan] Mahasarakham Univ, Dept Biol, Kantarawichai 44150, Maha Sarakham P, Thailand. [Naksuwankul, Khwanruan] Mahasarakham Univ, Nat Med Mushroom Museum, Fac Sci, Kantarawichai 44150, Maha Sarakham P, Thailand. [Parnmen, Sittiporn] Minist Publ Hlth, Dept Med Sci, Toxicol & Biochem Sect, Nonthaburi 11000, Thailand. [Salazar-Allen, Noris] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. RP Lucking, R (reprint author), Bot Garden & Bot Museum Berlin, Konigin Luise Str 6-8, D-14195 Berlin, Germany.; Lucking, R (reprint author), Field Museum, Integrat Res Ctr, 1400 South Lake Shore Dr, Chicago, IL 60605 USA. EM r.luecking@bgbm.org RI Caceres, Marcela/H-7039-2012 FU NSF-DEB [0715660]; Committee on Evolutionary Biology (University of Chicago); Caterpillar(R) Company; American Society of Plant Taxonomists; University of Chicago; Brown Family Fellowship through the Field Museum; William Harper Rainey Fellowship through the University of Chicago; CNPq (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico) [311706/2012-6, 563342/2010-2]; Bay and Paul Foundations; Erwin Warth Stiftung, NSF [DEB 0841405]; Mohamed bin Zayed Species Conservation Fund [152510692]; Universidad Distrital Francisco Jose de Caldas in Bogota, Colombia; Natural History Museum in London FX We are grateful to a number of organizations for funding including: NSF-DEB 0715660 "Neotropical Epiphytic Microlichens - An Innovative Inventory of a Highly Diverse yet Little Known Group of Symbiotic Organisms" to The Field Museum (PI Robert Lucking), a grant from the Committee on Evolutionary Biology (University of Chicago) to MN, and the Caterpillar (R) Company provided funds to study lichens from Panama. The American Society of Plant Taxonomists is also acknowledged for a Graduate Student Research Grant awarded to MN. Additionally, MN's work was supported the University of Chicago and by a Brown Family Fellowship through the Field Museum, as well as by a William Harper Rainey Fellowship through the University of Chicago. The CNPq (Conselho Nacional de Desenvolvimento Cientifico e Tecnologico) is thanked for a research grant and field trip funding (Processos 311706/2012-6 and CNPq-Sisbiota Processo 563342/2010-2) to MESC. As part of the Census of Galapagos Biodiversity, the Galapagos Lichen Inventory received funds from several donors (for a detailed list see http://www.darwinfoundation.org/datazone/checklists). The lichen inventory in particular received funds from The Bay and Paul Foundations, the Erwin Warth Stiftung, NSF (grant no. DEB 0841405) and, most recently, the Mohamed bin Zayed Species Conservation Fund, project no. 152510692. This publication is contribution number 2143 of the Charles Darwin Foundation for the Galapagos Islands. We especially thank Galo Quedaza and Victor Carrion from the Galapagos National Park for technical support and specimen export permits for Galapagos material analyzed in this study. Logistical support was provided by the University of Panama (Department of Botany) in the development of two lichen seminars (2009, 2011) under the program Neotropical Epiphytic Microlichens in which the lichens were collected. Thanks also to Park authorities and rangers from Parque Nacional Altos de Campana during the field trips and to the Ministry of the Environment (former A.N.A.M.) for collection and export permits. The Universidad Distrital Francisco Jose de Caldas in Bogota, Colombia, is thanked for providing support to BM as part of the program 'Mobilidad Academica' for professors. The Natural History Museum in London is thanked for research and travel funds to CG and the Vietnam National Museum of Nature in Hanoi for organizing the fieldwork. NR 85 TC 6 Z9 6 U1 3 U2 3 PU CAMBRIDGE UNIV PRESS PI CAMBRIDGE PA EDINBURGH BLDG, SHAFTESBURY RD, CB2 8RU CAMBRIDGE, ENGLAND SN 0024-2829 EI 1096-1135 J9 LICHENOLOGIST JI Lichenologist PD NOV PY 2016 VL 48 IS 6 BP 739 EP 762 DI 10.1017/S0024282916000505 PG 24 WC Plant Sciences; Mycology SC Plant Sciences; Mycology GA EF5IT UT WOS:000390364600008 ER PT J AU DeCaluwe, HB Wielebnowski, NC Howard, J Pelican, KM Ottinger, MA AF DeCaluwe, Heather B. Wielebnowski, Nadja C. Howard, JoGayle Pelican, Katharine M. Ottinger, Mary Ann TI Characterization of Multiple Pathways Modulating Aggression in the Male Clouded Leopard (Neofelis nebulosa) SO ZOO BIOLOGY LA English DT Article DE glucocorticoids; androgens; GnRH agonist; tricyclic antidepressant; serotonergic regulation ID GNRH ANALOG DESLORELIN; CHALLENGE HYPOTHESIS; TRICYCLIC ANTIDEPRESSANTS; TERRITORIAL AGGRESSION; ADRENAL ACTIVITY; AXIS ACTIVITY; MICE LACKING; MALE-RATS; BEHAVIOR; TESTOSTERONE AB Breeding clouded leopards (Neofelis nebulosa) ex situ has been a challenge, primarily due to extreme and often fatal male aggression toward females. This study's aim was to determine the degree to which two possible mechanisms-serotonergic pathways and circulating testosterone levels-affect aggressive behavior. Male clouded leopard behavioral and hormonal data were collected during a series of behavior tests administered before and after treatment with either an anxiety-reducing tricyclic antidepressant (clomipramine) or a GnRH agonist (deslorelin). Results showed that clomipramine treatment decreased "overall activity" (P = 0.054) and increased "lying down" (P = 0.0043) and hiding in a "nest box" (P = 0.0023). Clomipramine treatment also decreased the incidence of "growling" during a mirror image stimulation test, relative to non-test periods (P<0.0001 pre-drug treatment; P = 0.242 peri-drug treatment), indicating reduced aggression. Suppression of the reproductive axis via deslorelin treatment resulted in significant decreases in circulating androgen (P<0.0001) and glucocorticoid (P<0.0001), accompanied by decreased aggressive behaviors, including "swatting" (P = 0.0476), "tail flicking" (P = 0.0409), and "growling" during the behavior reaction tests: mirror image stimulation (P<0.0001 pre-drug treatment: P = 0.7098 peri-drug treatment) and unfamiliar people test (P<0.0001 pre-drug treatment: P = 0.2666 peri-drug treatment) relative to non-test periods. Both drug treatments provide evidence that multiple mechanisms modulate aggressive behavior in the male clouded leopard, suggesting that serotonergic modulation coupled with circulating androgens may aid in the formation of successful breeding pairs. (C) 2016 Wiley Periodicals, Inc. C1 [DeCaluwe, Heather B.] Univ Maryland, Dept Anim & Avian Sci, College Pk, MD 20742 USA. [DeCaluwe, Heather B.; Howard, JoGayle] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Wielebnowski, Nadja C.] Oregon Zoo, Dept Conservat & Res, Portland, OR USA. [Pelican, Katharine M.] Univ Minnesota, Coll Vet Med, Dept Vet Preventat Med, Minneapolis, MN 55455 USA. [Ottinger, Mary Ann] Univ Houston, Dept Biol & Biochem, Houston, TX 77204 USA. RP Ottinger, MA (reprint author), Univ Houston, Dept Biol & Biochem, Houston, TX 77204 USA. EM maotting@central.uh.edu FU Conservation Grants Fund [08-801] FX Grant sponsor: Conservation Grants Fund; grant number: #08-801. NR 66 TC 0 Z9 0 U1 2 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 EI 1098-2361 J9 ZOO BIOL JI Zoo Biol. PD NOV-DEC PY 2016 VL 35 IS 6 BP 474 EP 486 DI 10.1002/zoo.21319 PG 13 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA EE2VK UT WOS:000389443000002 PM 27588696 ER PT J AU Zellmer, GF Pistone, M Iizuka, Y Andrews, BJ Gomez-Tuena, A Straub, SM Cottrell, E AF Zellmer, Georg F. Pistone, Mattia Iizuka, Yoshiyuki Andrews, Benjamin J. Gomez-Tuena, Arturo Straub, Susanne M. Cottrell, Elizabeth TI Petrogenesis of antecryst-bearing arc basalts from the Trans-Mexican Volcanic Belt: Insights into along-arc variations in magma-mush ponding depths, H2O contents, and surface heat flux SO AMERICAN MINERALOGIST LA English DT Article DE Subduction; geobarometry; arc basalts; magma-mush zones; glomerocrysts; melt ascent; hygrometry; degassing ID SOUFRIERE HILLS VOLCANO; CALC-ALKALINE-LAVAS; MELT INCLUSIONS; SILICATE MELTS; CRYSTAL MUSHES; MANTLE WEDGE; FRONT STRATOVOLCANOES; GEOCHEMICAL EVIDENCE; THERMODYNAMIC MODEL; MAGNESIAN ANDESITE AB The Trans-Mexican Volcanic Belt (TMVB) is known for the chemical diversity in its erupted products. We have analyzed the olivine, pyroxene, and plagioclase mineral chemistry of 30 geochemically well-characterized mafic eruptives from Isla Maria at the western end of the arc to Palma Sola in the east. The mineral major oxide data indicate the dominance of open system processes such as antecryst uptake, and the scarcity of mineral-mineral and mineral-melt equilibria suggests that apart from forming microlites, erupted melts do not significantly crystallize during ascent. A combination of plagioclase antecryst chemistry and MELTS thermodynamic modeling of H2O-saturated isobaric fractional crystallization was employed to develop a pressure sensor aimed at determining the ponding depths of the co-genetic magmas from which the erupted plagioclase crystal assemblage originates. We show that the depth of magma-mush reservoirs increase eastward along the TMVB. We suggest that magma ponding is triggered by degassing-induced crystallization during magma ascent, and that the pressure sensor can also be regarded as a degassing sensor, with more hydrous melts beginning to degas at greater depths. Modeled initial magma H2O contents at the Moho range from similar to 4 to similar to 9 wt%. Magma-mush ponding depth variations fully explain the observed westward increase of average surface heat flux along the TMVB, supporting a new model of mafic arc magma ascent, where rapidly rising, initially aphyric melts pick up their antecrystic crystal cargo from a restricted crustal depth range, in which small unerupted batches of previously risen co-genetic magmas typically stall and solidify. This implies that, globally, mafic arc magmas may be used to constrain the depths of degassing and mush zone formation, as well as the amount of H2O in the primary melts. C1 [Zellmer, Georg F.] Massey Univ, Inst Agr & Environm, Palmerston North 4442, New Zealand. [Zellmer, Georg F.; Pistone, Mattia; Andrews, Benjamin J.; Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Iizuka, Yoshiyuki] Acad Sinica, Inst Earth Sci, 128 Acad Rd Sect 2, Taipei 11529, Taiwan. [Gomez-Tuena, Arturo] Univ Nacl Autonoma Mexico, Ctr Geociencias, Queretaro 76230, Mexico. [Straub, Susanne M.] Columbia Univ, Lamont Doherty Earth Observ, 61 Route 9W, Palisades, NY 10964 USA. RP Zellmer, GF (reprint author), Massey Univ, Inst Agr & Environm, Palmerston North 4442, New Zealand.; Zellmer, GF (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM g.f.zellmer@massey.ac.nz OI Pistone, Mattia/0000-0001-7560-3146; Zellmer, Georg/0000-0001-5450-9353 FU Smithsonian Institution-Global Volcanism Program FX Leslie Hale provided valuable on-site help in identifying relevant samples from Jim Luhr's Mexican Volcanic Belt collection of the National Museum of Natural History of the Smithsonian Institution. We are indebted to Hui-Ho Hsieh from Academia Sinica and Timothy Gooding and Timothy Rose from the National Museum of Natural History for valuable assistance with sample preparation and microprobe analysis. We thank Laura Waters for early access to the recently published plagioclase-liquid hygrometer-thermometer. This contribution benefitted from constructive input by John Adam, Mark Bebbington, Fred Davis, Szabolcs Kosik, and Laura Waters, and from thoughtful reviews by Scott Bryan and Chiara Petrone. G.F.Z. acknowledges a Smithsonian Institution visiting fellowship for February-July 2013 and July 2015, funded through the Smithsonian Institution-Global Volcanism Program (http://volcano.si.edu/), and travel support by Massey University. NR 122 TC 0 Z9 0 U1 3 U2 3 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD NOV PY 2016 VL 101 IS 11 BP 2405 EP 2422 DI 10.2138/am-2016-5701 PG 18 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA EC8BP UT WOS:000388365300004 ER PT J AU Pasteels, JM Deparis, O Mouchet, SR Windsor, DM Billen, J AF Pasteels, Jacques M. Deparis, Olivier Mouchet, Sebastien R. Windsor, Donald M. Billen, Johan TI Structural and physical evidence for an endocuticular gold reflector in the tortoise beetle, Charidotella ambita SO ARTHROPOD STRUCTURE & DEVELOPMENT LA English DT Article DE Elytra; Ultrastructure; Structural color; Gold reflector; Tortoise beetle; Chrysomelidae ID DEFENSIVE SECRETION; CARDIAC-GLYCOSIDES; COLEOPTERA; CUTICLE; IDENTIFICATION; IRIDESCENCE; CHITIN; SILVER; GREEN; PUPAE AB Charidotella ambita offers a unique opportunity for unambiguously locating its gold reflector by comparing the structure of reflecting and non-reflecting cuticle of the elytron and pronotum. Using light microscopy and TEM, the reflector was located underneath the macrofiber endocuticle just above the epidermis. The reflector is a multilayer comprising up to 50 bilayers alternating high and low density layers parallel to the surface of the cuticle. It is chirped, i.e., showing a progressive decrease in layer thickness from approximately 150 nm-100 nm across its depth. The high density layers in contact with the endocuticle fuse to the last macrofiber when the reflector is interrupted by a trabecula, demonstrating their cuticular nature. Simulated reflectance spectra from models of the multilayer matched the reflection spectra measured on the major gold patch of the elytron of living specimens. Previous reports in adult insects exhibiting metallic colors located their reflector in the upper strata and structures of the cuticle, i.e., epicuticle, exocuticle, scales and hairs. Thus, the endocuticular location of the reflector in C. ambita (and other tortoise beetles) appears unique for adult insects. Gold reflection appears in C ambita only when the synthesis of the macrolayer endocuticle is complete, which may take up to 2 weeks. The development of the gold reflector coincides with the start of mating behavior, possibly suggesting a signaling function in conspecific recognition once sexual maturity has been reached. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Pasteels, Jacques M.] Univ Libre Bruxelles, Evolutionary Biol & Ecol, CP 160-12,Ave FD Roosevelt 50, B-1050 Brussels, Belgium. [Deparis, Olivier; Mouchet, Sebastien R.] Univ Namur UNamur, Dept Phys Phys Matter & Radiat PMR, Rue Bruxelles 61, B-5000 Namur, Belgium. [Mouchet, Sebastien R.] Univ Exeter, Coll Engn Math & Phys Sci, Stocker Rd, Exeter EX4 4QL, Devon, England. [Windsor, Donald M.] Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. [Billen, Johan] Katholieke Univ Leuven, Inst Zool, Naamsestr 59,Box 2466, B-3000 Leuven, Belgium. RP Billen, J (reprint author), Katholieke Univ Leuven, Inst Zool, Naamsestr 59,Box 2466, B-3000 Leuven, Belgium. EM jmpastee@ulb.ac.be; olivier.deparis@unamur.be; sebastien.mouchet@unamur.be; windsordm@gmail.com; johan.billen@kuleuven.be OI Mouchet, Sebastien/0000-0001-6611-3794 FU Belgian National Fund for Scientific Research; Wallonia-Brussels International (WBI) through a Postdoctoral Fellowship for Excellence program WBI.WORLD FX We are very grateful to An Vandoren for her help in section preparation, and to R.A. Steinbrecht and two anonymous reviewers for valuable comments on the manuscript. SRM was supported by the Belgian National Fund for Scientific Research (F.R.S.-FNRS) as a Research Fellow and by Wallonia-Brussels International (WBI) through a Postdoctoral Fellowship for Excellence program WBI.WORLD. JMP and DMW received important logistical support from STRI during field work in Panama. NR 30 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1467-8039 EI 1873-5495 J9 ARTHROPOD STRUCT DEV JI Arthropod Struct. Dev. PD NOV PY 2016 VL 45 IS 6 BP 509 EP 518 DI 10.1016/j.asd.2016.10.008 PG 10 WC Entomology SC Entomology GA ED7ZS UT WOS:000389092000001 PM 27725254 ER PT J AU Michel, APM Miller, DJ Sun, K Tao, L Stanton, L Zondlo, MA AF Michel, Anna P. M. Miller, David J. Sun, Kang Tao, Lei Stanton, Levi Zondlo, Mark A. TI Long-Path Quantum Cascade Laser-Based Sensor for Methane Measurements SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID ATMOSPHERIC AMMONIA MEASUREMENTS; ABSORPTION-SPECTROSCOPY; FTIR SPECTROSCOPY; FLUX MEASUREMENTS; NATURAL-GAS; EMISSIONS; BUDGET; N2O AB A long-path methane (CH4) sensor was developed and field deployed using an 8-mm quantum cascade laser. The high optical power (40 mW) of the laser allowed for path-integrated measurements of ambient CH4 at total pathlengths from 100 to 1200 m with the use of a retroreflector. Wavelength modulation spectroscopy was used to make high-precision measurements of atmospheric pressure-broadened CH4 absorption over these long distances. An in-line reference cell with higher harmonic detection provided metrics of system stability in rapidly changing and harsh environments. The system consumed less than 100 W of power and required no consumables. The measurements intercompared favorably (typically less than 5% difference) with a commercial in situ methane sensor when accounting for the different spatiotemporal scales of the measurements. The sensor was field deployed for 2 weeks at an arctic lake to examine the robustness of the approach in harsh field environments. Shortterm precision over a 458-m pathlength was 10 ppbv at 1Hz, equivalent to a signal from a methane enhancement above background of 5 ppmv in a 1-m length. The sensor performed well in a range of harsh environmental conditions, including snow, rain, wind, and changing temperatures. These field measurements demonstrate the capabilities of the approach for use in detecting large but highly variable emissions in arctic environments. C1 [Michel, Anna P. M.; Miller, David J.; Sun, Kang; Tao, Lei; Stanton, Levi; Zondlo, Mark A.] Princeton Univ, Midinfrared Technol Hlth & Environm, Princeton, NJ 08544 USA. [Miller, David J.; Sun, Kang; Tao, Lei; Stanton, Levi; Zondlo, Mark A.] Princeton Univ, Dept Civil & Environm Engn, Princeton, NJ 08544 USA. [Michel, Anna P. M.] Woods Hole Oceanog Inst, Appl Ocean Phys & Engn Dept, 266 Woods Hole Rd,MS 7, Woods Hole, MA 02543 USA. [Miller, David J.] Brown Univ, Inst Brown Environm & Soc, Providence, RI 02912 USA. [Sun, Kang] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. [Tao, Lei] NEC Labs Amer, Princeton, NJ USA. [Stanton, Levi] Sonoma Technol Inc, Petaluma, CA USA. RP Michel, APM (reprint author), Woods Hole Oceanog Inst, Appl Ocean Phys & Engn Dept, 266 Woods Hole Rd,MS 7, Woods Hole, MA 02543 USA. EM amichel@whoi.edu OI Zondlo, Mark/0000-0003-2302-9554 FU MIRTHE through NSF-ERC Grant [EEC-0540832]; National Science Foundation [DGE-0646086]; NASA [IIP-1263579] FX The authors gratefully acknowledge funding for this work by MIRTHE through NSF-ERC Grant EEC-0540832. The authors wish to thank Professor Claire F. Gmachl and her research group and Professor James Smith and his research group for the valuable support and feedback. We specifically thank Mary Lynn Baeck for access to the Princeton University Broadmead site for field measurements and the supporting meteorological data from the site. We also thank Matthew Reid for assisting with the GC measurements and Victor Fu for work on the initial sensor development and field testing, and LI-COR Biosciences for use of the LI-7700 CH4 analyzer. Finally, we are grateful for the help and support of the NSF Toolik Field Station staff for use of their facilities and for logistical assistance with the field measurements in Alaska. D. J. Miller acknowledges support by the National Science Foundation Graduate Research Fellowship under Grant DGE-0646086. K. Sun acknowledges support by the NASA Earth and Space Science Fellowship IIP-1263579. NR 37 TC 0 Z9 0 U1 8 U2 8 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0739-0572 EI 1520-0426 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD NOV PY 2016 VL 33 IS 11 BP 2373 EP 2384 DI 10.1175/JTECH-D-16-0024.1 PG 12 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA ED4HG UT WOS:000388808000007 ER PT J AU Thornhill, AH Mishler, BD Knerr, NJ Gonzalez-Orozco, CE Costion, CM Crayn, DM Laffan, SW Miller, JT AF Thornhill, Andrew H. Mishler, Brent D. Knerr, Nunzio J. Gonzalez-Orozco, Carlos E. Costion, Craig M. Crayn, Darren M. Laffan, Shawn W. Miller, Joseph T. TI Continental-scale spatial phylogenetics of Australian angiosperms provides insights into ecology, evolution and conservation SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Australian flora; CANAPE; conservation; neo-endemism; observed richness; palaeo-endemism; phylogenetic diversity; phylogenetic endemism; spatial phylogenetics ID RAIN-FOREST; BIODIVERSITY HOTSPOTS; MOLECULAR PHYLOGENIES; MONSOON TROPICS; ZONE BIOTA; DIVERSITY; ENDEMISM; FLORA; HISTORY; BIRDS AB Aim Biodiversity studies typically use species, or more recently phylogenetic diversity (PD), as their analysis unit and produce a single map of observed diversity. However, observed biodiversity is not necessarily an indicator of significant biodiversity and therefore should not be used alone. By applying a small number of additional metrics to PD, with associated statistical tests, we can determine whether more or less of the phylogeny occurs in an area, whether branch lengths in an area are longer or shorter, and whether more long or short-branched endemism occurs in an area, than expected under a null model. Location Australian continent. Methods We used a phylogeny sampling 90% of Australia's angiosperm genera, and 3.4 million georeferenced plant specimens downloaded from Australia's Virtual Herbarium (AVH), to calculate PD, relative phylogenetic diversity (RPD) and relative phylogenetic endemism (RPE). Categorical analysis of neo-and palaeo-endemism (CANAPE) and randomization tests were performed to determine statistical significance. Results We identify several combinations of significant PD and endemism across the continent that are not seen using observed diversity patterns alone. Joint interpretation of these combinations complements the previous interpretations of Australia's plant evolutionary history. Of conservation concern, only 42% of the significant endemism cells found here overlap with existing nature reserves. Main conclusions These spatial phylogenetic methods are feasible to apply to a whole flora at the continental scale. Observed richness or PD is inadequate to fully understand the patterns of biodiversity. The combination of statistical tests applied here can be used to better explain biodiversity patterns and the evolutionary and ecological processes that have created them. The spatial phylogenetic methods used in this paper can be also be used to identify conservation priorities at any geographical scale or taxonomic level. C1 [Thornhill, Andrew H.; Knerr, Nunzio J.; Miller, Joseph T.] CSIRO Natl Res Collect, Ctr Australian Natl Biodivers Res, Canberra, ACT, Australia. [Thornhill, Andrew H.; Costion, Craig M.; Crayn, Darren M.] James Cook Univ, Australian Trop Herbarium, Cairns, Qld 4870, Australia. [Thornhill, Andrew H.; Mishler, Brent D.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Thornhill, Andrew H.; Mishler, Brent D.] Univ Calif Berkeley, Jepson Herbaria, Berkeley, CA 94720 USA. [Gonzalez-Orozco, Carlos E.] Univ Canberra, Inst Appl Ecol, Canberra, ACT 2601, Australia. [Gonzalez-Orozco, Carlos E.] Univ Canberra, Collaborat Res Network Murray Darling Basin Futur, Canberra, ACT 2601, Australia. [Gonzalez-Orozco, Carlos E.] Corpoica, Corp Colombiana Invest Agr, Km 17 Via Puerto Lopez, Meta, Colombia. [Costion, Craig M.] Smithsonian Inst, MRC 166, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA. [Laffan, Shawn W.] Univ New South Wales, Sch Biol Earth & Environm Sci, Ctr Ecosyst Sci, Sydney, NSW 2052, Australia. [Miller, Joseph T.] Natl Sci Fdn, Div Environm Biol, Arlington, VA 22230 USA. RP Thornhill, AH (reprint author), CSIRO Natl Res Collect, Ctr Australian Natl Biodivers Res, Canberra, ACT, Australia. EM andrew.thornhill@gmail.com RI Thornhill, Andrew/I-3363-2012; OI Thornhill, Andrew/0000-0002-0325-5725; Laffan, Shawn/0000-0002-5996-0570 FU CSIRO (Australia); NSF [DEB-1354552] FX This manuscript includes work by Joe Miller while serving at the National Science Foundation. The views expressed in this paper do not necessarily reflect those of the National Science Foundation or the United States Government. CSIRO (Australia) provided a Distinguished Visiting Scientist Award to Brent Mishler. Brendan Lepschi and Anna Monro provided the species list of the Australian Plant Census on which genetic and spatial sampling was based. NSF grant DEB-1354552 provided partial support for the UC Berkeley portion of this project. We thank the two anonymous referees who provided comments that helped improve the manuscript. NR 65 TC 1 Z9 1 U1 12 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD NOV PY 2016 VL 43 IS 11 BP 2085 EP 2098 DI 10.1111/jbi.12797 PG 14 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA ED5CH UT WOS:000388868700001 ER PT J AU Simpson, LA Ambrosio, LJ Baeza, JA AF Simpson, Lunden A. Ambrosio, Louis J. Baeza, J. Antonio TI SEXUAL DIMORPHISM AND ALLOMETRIC GROWTH IN THE ENIGMATIC PYGMY CRAB PETRAMITHRAX PYGMAEUS (BELL, 1836) (DECAPODA: BRACHYURA: MITHRACIDAE), WITH A FORMAL TEST OF RENSCH'S RULE IN SPIDER CRABS (SUPERFAMILY MAJOIDEA) SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE allometry; body size; dwarfism; evolutionary ecology; evolutionary trends ID MULTIPLE SEQUENCE ALIGNMENT; ALTERNATIVE MATING STRATEGIES; SOUTHEASTERN BRAZILIAN COAST; SIZE DIMORPHISM; FIDDLER-CRAB; BODY-SIZE; RELATIVE GROWTH; PHYLOGENETIC ANALYSES; ONTOGENIC SHIFTS; UCA-URUGUAYENSIS AB Rensch's rule, a well-studied macroevolutionary pattern of sexual size dimorphism (SSD), predicts, in monophyletic taxa in which males are the larger sex, that as the body size of the species in the Glade increases, SSD increases as well. We tested Rensch's rule in the superfamily Majoidea, a diverse Glade of 'spider crabs.' Considering that having the widest range of data available is important when testing macroevolutionary hypotheses, we first explored SSD in the pygmy spider crab Petramithrax pygmaeus (Bell, 1836), one of the smallest spider crabs in the superfamily. Petramithrax pygmaeus exhibits an unusual pattern of sexual dimorphism, with females displaying a larger average carapace width than males, yet males attain a larger overall body size. This type of SSD is unusual for spider crabs, with most species displaying male-biased sexual size dimorphism for both mean and overall body size. Hierarchical cluster and discriminant analyses demonstrated the existence of two distinct ontogenetic phases in P. pygmaeus (juvenile/prepubertal and adult/postpubertal). We used our data on body size of P. pygmaeus along with previously published body-size data for 11 other species within the superfamily Majoidea to test for Rensch's rule. Using raw data, phylogenetic independent contrasts generated from maximum likelihood (ML) and Bayesian inference (BI) phylogenetic trees, and reduced major axis regression analyses, we determined that for the tested species in the Majoidea that the predictions of Rensch's rule were not upheld. Macroevoultionary patterns such as Rensch's rule are not well studied in marine invertebrate systems; looking at how these rules compare between vertebrate and invertebrate and terrestrial and aquatic animals will help us to understand the differences and factors that could influence size and growth in these systems. C1 [Simpson, Lunden A.; Ambrosio, Louis J.; Baeza, J. Antonio] Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA. [Baeza, J. Antonio] Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. [Baeza, J. Antonio] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. RP Baeza, JA (reprint author), Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA.; Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA.; Baeza, JA (reprint author), Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. EM jbaezam@clemson.edu NR 104 TC 0 Z9 0 U1 9 U2 9 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 EI 1937-240X J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD NOV PY 2016 VL 36 IS 6 BP 792 EP 803 DI 10.1163/1937240X-00002486 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA ED8IN UT WOS:000389115300004 ER PT J AU Connette, G Oswald, P Songer, M Leimgruber, P AF Connette, Grant Oswald, Patrick Songer, Melissa Leimgruber, Peter TI Mapping Distinct Forest Types Improves Overall Forest Identification Based on Multi-Spectral Landsat Imagery for Myanmar's Tanintharyi Region SO REMOTE SENSING LA English DT Article DE remote sensing; forest types; forest classification; Landsat 8 OLI; satellite imagery; wildlife habitat; tropical forest; mangrove ID SOUTHEAST-ASIA; COVER CLASSIFICATION; BRAZILIAN AMAZON; LOGGED FORESTS; CLOUD SHADOW; COSTA-RICA; DEFORESTATION; CONSERVATION; BIODIVERSITY; DEGRADATION AB We investigated the use of multi-spectral Landsat OLI imagery for delineating mangrove, lowland evergreen, upland evergreen and mixed deciduous forest types in Myanmar's Tanintharyi Region and estimated the extent of degraded forest for each unique forest type. We mapped a total of 16 natural and human land use classes using both a Random Forest algorithm and a multivariate Gaussian model while considering scenarios with all natural forest classes grouped into a single intact or degraded category. Overall, classification accuracy increased for the multivariate Gaussian model with the partitioning of intact and degraded forest into separate forest cover classes but slightly decreased based on the Random Forest classifier. Natural forest cover was estimated to be 80.7% of total area in Tanintharyi. The most prevalent forest types are upland evergreen forest (42.3% of area) and lowland evergreen forest (21.6%). However, while just 27.1% of upland evergreen forest was classified as degraded (on the basis of canopy cover <80%), 66.0% of mangrove forest and 47.5% of the region's biologically-rich lowland evergreen forest were classified as degraded. This information on the current status of Tanintharyi's unique forest ecosystems and patterns of human land use is critical to effective conservation strategies and land-use planning. C1 [Connette, Grant; Songer, Melissa; Leimgruber, Peter] Smithsonian Conservat Biol Inst, Myanmar Program, Conservat Ecol Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. [Oswald, Patrick] Fauna & Flora Int, 35 Shan Kone St, San Chaung Township 11111, Yangon, Myanmar. RP Connette, G (reprint author), Smithsonian Conservat Biol Inst, Myanmar Program, Conservat Ecol Ctr, 1500 Remount Rd, Front Royal, VA 22630 USA. EM grmcco@gmail.com; patrick.oswald@fauna-flora.org; songerm@si.edu; leimgruberp@si.edu FU Leona M. and Harry B. Helmsley Charitable Trust FX We thank our editors and several anonymous reviewers for constructive feedback on this manuscript. We are also grateful to Saw Htun, Kyaw Thinn Latt, and Robert Tizard (Wildlife Conservation Society), as well as Frank Momberg and Mark Grindley (Fauna & Flora International) for their comments and insight on this project. We also thank Nyi Nyi Kyaw and Soe Thiha of the Myanmar Forest Department for facilitating field data collection and providing their expert input. We thank Ko Zaw Myo, Ko Hein, Ko Khin Zaw Moe, Ko Aung Myint, Ko Tu Tu and Saw War Mei Sai for assistance with field visits to the Tanintharyi Nature Reserve. Funding for this research was provided by The Leona M. and Harry B. Helmsley Charitable Trust. NR 61 TC 1 Z9 1 U1 21 U2 21 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD NOV PY 2016 VL 8 IS 11 AR 882 DI 10.3390/rs8110882 PG 15 WC Remote Sensing SC Remote Sensing GA ED4DS UT WOS:000388798400003 ER PT J AU Connette, KJL Connette, G Bernd, A Phyo, P Aung, KH Tun, YL Thein, ZM Horning, N Leimgruber, P Songer, M AF Connette, Katherine J. LaJeunesse Connette, Grant Bernd, Asja Phyo, Paing Aung, Kyaw Htet Tun, Ye Lin Thein, Zaw Min Horning, Ned Leimgruber, Peter Songer, Melissa TI Assessment of Mining Extent and Expansion in Myanmar Based on Freely-Available Satellite Imagery SO REMOTE SENSING LA English DT Article DE mining; change detection; Myanmar; Landsat; Google Earth ID CLOUD SHADOW; LAND; AREA; RECLAMATION; MINES; INDIA AB Using freely-available data and open-source software, we developed a remote sensing methodology to identify mining areas and assess recent mining expansion in Myanmar. Our country-wide analysis used Landsat 8 satellite data from a select number of mining areas to create a raster layer of potential mining areas. We used this layer to guide a systematic scan of freely-available fine-resolution imagery, such as Google Earth, in order to digitize likely mining areas. During this process, each mining area was assigned a ranking indicating our certainty in correct identification of the mining land use. Finally, we identified areas of recent mining expansion based on the change in albedo, or brightness, between Landsat images from 2002 and 2015. We identified 90,041 ha of potential mining areas in Myanmar, of which 58% (52,312 ha) was assigned high certainty, 29% (26,251 ha) medium certainty, and 13% (11,478 ha) low certainty. Of the high-certainty mining areas, 62% of bare ground was disturbed (had a large increase in albedo) since 2002. This four-month project provides the first publicly-available database of mining areas in Myanmar, and it demonstrates an approach for large-scale assessment of mining extent and expansion based on freely-available data. C1 [Connette, Katherine J. LaJeunesse; Connette, Grant; Leimgruber, Peter; Songer, Melissa] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, 1500 Remt Rd, Front Royal, VA 22630 USA. [Connette, Katherine J. LaJeunesse; Bernd, Asja; Phyo, Paing; Aung, Kyaw Htet; Tun, Ye Lin; Thein, Zaw Min] EcoDev ALARM, Kamaryut Township 11041, Yangon, Myanmar. [Bernd, Asja] Univ Bayreuth, Dept Biogeog, Univ Str 30, D-95447 Bayreuth, Germany. [Phyo, Paing; Aung, Kyaw Htet; Tun, Ye Lin] Univ Bern, Ctr Dev & Environm, One Map Myanmar, 18D Sein Lei Yeik Thar St, Yankin Township 11081, Yangon, Myanmar. [Horning, Ned] Amer Museum Nat Hist, New York, NY 10024 USA. RP Connette, KJL (reprint author), Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, 1500 Remt Rd, Front Royal, VA 22630 USA.; Connette, KJL (reprint author), EcoDev ALARM, Kamaryut Township 11041, Yangon, Myanmar. EM lajeune@gmail.com; grmcco@gmail.com; asja.bernd@gmail.com; paingphyo.77.pp@gmail.com; kyawhtetaung.bfor.2013@gmail.com; yelinnhtun93@gmail.com; zawmintheinzmt@gmail.com; horning@amnh.org; LeimgruberP@si.edu; SongerM@si.edu FU European Union's Forest Law Enforcement, Governance and Trade (FLEGT) initiative; U.S. Agency for International Development (USAID); FHI project through the Myanmar NGO Advancing Life and Regenerating the Motherland (ALARM) [360]; Helmsley Charitable Trust through the Smithsonian Institution FX Funding for this research was provided by European Union's Forest Law Enforcement, Governance and Trade (FLEGT) initiative, U.S. Agency for International Development (USAID), and FHI 360 project through the Myanmar NGO Advancing Life and Regenerating the Motherland (ALARM), and by the Helmsley Charitable Trust through the Smithsonian Institution. We would like to thank U Win Myo Thu, Richard Holloway, Tony Neil, and Khay Mar Aye at ALARM for their support of this project and the Myanmar Information Management Unit (MIMU) for hosting the data and for providing geospatial base data. We also thank the editors at Remote Sensing and three anonymous reviewers for their input on the manuscript. We give special thanks to the Civil Society Organization members who assisted in our validation data collection efforts in Kayah State, Mandalay Region, Tanintharyi Region and Shan State. NR 43 TC 0 Z9 0 U1 7 U2 7 PU MDPI AG PI BASEL PA ST ALBAN-ANLAGE 66, CH-4052 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD NOV PY 2016 VL 8 IS 11 AR 912 DI 10.3390/rs8110912 PG 14 WC Remote Sensing SC Remote Sensing GA ED4DS UT WOS:000388798400033 ER PT J AU Gunther, L Lopez, MD Knornschild, M Reid, K Nagy, M Mayer, F AF Guenther, Linus Lopez, Marlena D. Knoernschild, Mirjam Reid, Kyle Nagy, Martina Mayer, Frieder TI From resource to female defence: the impact of roosting ecology on a bat's mating strategy SO Royal Society Open Science LA English DT Article DE male territoriality; site-dependent dominance; social dispersion; resource-defence polygyny; female-defence polygyny; Rhynchonycteris naso ID TENT-MAKING BAT; SOCIAL-ORGANIZATION; SACCOPTERYX-BILINEATA; INTRASPECIFIC VARIATION; EMBALLONURID BATS; SEXUAL SELECTION; ARTIBEUS-JAMAICENSIS; PIPISTRELLUS-NANUS; FRUIT BAT; CHIROPTERA AB With their extraordinary species richness and diversity in ecological traits and social systems, bats are a promising taxon for testing socio-ecological hypotheses in order to get new insights into the evolution of animal social systems. Regarding its roosting habits, proboscis bats form an extreme by occupying sites which are usually completely exposed to daylight (e.g. tree trunks, vines or rocks). This is accompanied by morphological and behavioural adaptations to remain cryptic in exposed day roosts. With long-term behavioural observations and genetic parentage analyses of individually marked proboscis bats, we assessed its social dispersion and male mating strategy during day and night. Our results reveal nocturnal male territoriality-a strategy which most closely resembles a resource-defence polygyny that is frequent also in other tropical bats. Its contrasting clumped social dispersion during the day is likely to be the result of strong selection for crypsis in exposed roosts and is accompanied by direct female defence in addition to male territoriality. To the best of our knowledge, such contrasting male mating strategies within a single day-night cycle have not been described in a vertebrate species so far and illustrate a possible evolutionary trajectory from resource-defence to female-defence strategy by small ecologically driven evolutionary steps. C1 [Guenther, Linus; Mayer, Frieder] Leibniz Inst Res Evolut & Biodivers, Museum Nat Kunde, Invalidenstr 43, D-10115 Berlin, Germany. [Lopez, Marlena D.] Univ Melbourne, Fac Vet & Agr Sci, Werribee, Vic, Australia. [Knoernschild, Mirjam] Free Univ Berlin, Inst Biol, Anim Behav Lab, Takustr 6, D-14195 Berlin, Germany. [Knoernschild, Mirjam] Smithsonian Trop Res Inst, Roosevelt Ave,Tupper Bldg 401, Balboa, Panama. [Reid, Kyle] Univ Illinois, Dept Biol Sci, Chicago, IL 60680 USA. [Nagy, Martina] Friedrich Alexander Univ Erlangen Nuremberg, Dept Sensor Technol, Paul Gordan Str 3-5, D-91052 Erlangen, Germany. RP Gunther, L (reprint author), Leibniz Inst Res Evolut & Biodivers, Museum Nat Kunde, Invalidenstr 43, D-10115 Berlin, Germany. EM linus.guenther@mfn-berlin.de FU Deutsche Forschungsgemeinschaft (DFG) [MA1737/4, KN935 3-1]; National Geographic Society (NGS); German Academic Exchange Service (DAAD); Elsa-Neumann-Fellowship; Ilse & Dr Alexander Mayer Stiftung; Baden-Wurttemberg Stiftung; National Science Foundation; Louis Stokes Alliances for Minority Participation (NSF-LSAMP) FX This work was funded by the Deutsche Forschungsgemeinschaft (DFG, F.M.: MA1737/4; M.K.: DFG, KN935 3-1), the National Geographic Society (NGS), by grants to M.N. and L.G. from the German Academic Exchange Service (DAAD), the Elsa-Neumann-Fellowship (L.G.), the Ilse & Dr Alexander Mayer Stiftung (M.N.), the Baden-Wurttemberg Stiftung (Eliteprogramme for Postdocs, M.K.) and partnership of the National Science Foundation and Louis Stokes Alliances for Minority Participation (NSF-LSAMP, M.D.L. and K.R.). NR 77 TC 0 Z9 0 U1 9 U2 9 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 2054-5703 J9 ROY SOC OPEN SCI JI R. Soc. Open Sci. PD NOV PY 2016 VL 3 IS 11 AR 160503 DI 10.1098/rsos.160503 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EE0DR UT WOS:000389244400029 PM 28018637 ER PT J AU Dalling, JW Cernusak, LA Winter, K Aranda, J Garcia, M Virgo, A Cheesman, AW Baresch, A Jaramillo, C Turner, BL AF Dalling, James W. Cernusak, Lucas A. Winter, Klaus Aranda, Jorge Garcia, Milton Virgo, Aurelio Cheesman, Alexander W. Baresch, Andres Jaramillo, Carlos Turner, Benjamin L. TI Two tropical conifers show strong growth and water-use efficiency responses to altered CO2 concentration SO ANNALS OF BOTANY LA English DT Article DE Araucaria heterophylla; Podocarpus guatemalensis; Tabebuia rosea; Chrysophyllum cainito; tropical conifer; angiosperm dominance; water-use efficiency; relative growth rate; nitrate assimilation; elevated CO2 ID ELEVATED CO2; ATMOSPHERIC CO2; RAIN-FOREST; NITRATE ASSIMILATION; ARAUCARIA-ANGUSTIFOLIA; STOMATAL CONDUCTANCE; ISOTOPIC COMPOSITION; ANGIOSPERM TREES; CLIMATE-CHANGE; SOIL AB Background and Aims Conifers dominated wet lowland tropical forests 100 million years ago (MYA). With a few exceptions in the Podocarpaceae and Araucariaceae, conifers are now absent from this biome. This shift to angiosperm dominance also coincided with a large decline in atmospheric CO2 concentration (c(a)). We compared growth and physiological performance of two lowland tropical angiosperms and conifers at c(a) levels representing pre-industrial (280 ppm), ambient (400 ppm) and Eocene (800 ppm) conditions to explore how differences in c(a) affect the growth and water-use efficiency (WUE) of seedlings from these groups. Methods Two conifers (Araucaria heterophylla and Podocarpus guatemalensis) and two angiosperm trees (Tabebuia rosea and Chrysophyllum cainito) were grown in climate-controlled glasshouses in Panama. Growth, photosynthetic rates, nutrient uptake, and nutrient use and water-use efficiencies were measured. Key Results Podocarpus seedlings showed a stronger (66 %) increase in relative growth rate with increasing c(a) relative to Araucaria (19 %) and the angiosperms (no growth enhancement). The response of Podocarpus is consistent with expectations for species with conservative growth traits and low mesophyll diffusion conductance. While previous work has shown limited stomatal response of conifers to c(a), we found that the two conifers had significantly greater increases in leaf and whole-plant WUE than the angiosperms, reflecting increased photosynthetic rate and reduced stomatal conductance. Foliar nitrogen isotope ratios (delta N-15) and soil nitrate concentrations indicated a preference in Podocarpus for ammonium over nitrate, which may impact nitrogen uptake relative to nitrate assimilators under high c(a). Significance Podocarps colonized tropical forests after angiosperms achieved dominance and are now restricted to infertile soils. Although limited to a single species, our data suggest that higher c(a) may have been favourable for podocarp colonization of tropical South America 60 MYA, while plasticity in photosynthetic capacity and WUE may help account for their continued persistence under large changes in c(a) since the Eocene. C1 [Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Dalling, James W.; Winter, Klaus; Aranda, Jorge; Garcia, Milton; Virgo, Aurelio; Jaramillo, Carlos; Turner, Benjamin L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Cernusak, Lucas A.; Cheesman, Alexander W.] James Cook Univ, Coll Sci & Engn, Cairns, Qld 4870, Australia. [Baresch, Andres] Stanford Univ, Sch Earth Energy & Environm Sci, Stanford, CA 94305 USA. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA.; Dalling, JW (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM dallingj@life.illinois.edu RI Cheesman, Alexander/H-5918-2013; Turner, Benjamin/E-5940-2011; Cernusak, Lucas/A-6859-2011 OI Cheesman, Alexander/0000-0003-3931-5766; Turner, Benjamin/0000-0002-6585-0722; Cernusak, Lucas/0000-0002-7575-5526 NR 63 TC 1 Z9 1 U1 10 U2 10 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 EI 1095-8290 J9 ANN BOT-LONDON JI Ann. Bot. PD NOV PY 2016 VL 118 IS 6 BP 1113 EP 1125 DI 10.1093/aob/mcw162 PG 13 WC Plant Sciences SC Plant Sciences GA ED0TM UT WOS:000388554900005 PM 27582361 ER PT J AU Brown, AGA Vallenari, A Prusti, T de Bruijne, JHJ Mignard, F Drimmel, R Babusiaux, C Bailer-Jones, CAL Bastian, U Biermann, M Evans, DW Eyer, L Jansen, F Jordi, C Katz, D Klioner, SA Lammers, U Lindegren, L Luri, X O'Mullane, W Panem, C Pourbaix, D Randich, S Sartoretti, P Siddiqui, HI Soubiran, C Valette, V van Leeuwen, F Walton, NA Aerts, C Arenou, F Cropper, M Hog, E Lattanzi, MG Grebel, EK Holland, AD Huc, C Passot, X Perryman, M Bramante, L Cacciari, C Castaneda, J Chaoul, L Cheek, N De Angeli, F Fabricius, C Guerra, R Hernandez, J Jean-Antoine-Piccolo, A Masana, E Messineo, R Mowlavi, N Nienartowicz, K Ordonez-Blanco, D Panuzzo, P Portell, J Richards, PJ Riello, M Seabroke, GM Tanga, P Thevenin, F Torra, J Els, SG Gracia-Abril, G Comoretto, G Garcia-Reinaldos, M Lock, T Mercier, E Altmann, M Andrae, R Astraatmadja, TL Bellas-Velidis, I Benson, K Berthier, J Blomme, R Busso, G Carry, B Cellino, A Clementini, G Cowell, S Creevey, O Cuypers, J Davidson, M De Ridder, J de Torres, A Delchambre, L Dell'Oro, A Ducourant, C Fremat, Y Garcia-Torres, M Gosset, E Halbwachs, JL Hambly, NC Harrison, DL Hauser, M Hestroffer, D Hodgkin, ST Huckle, HE Hutton, A Jasniewicz, G Jordan, S Kontizas, M Korn, AJ Lanzafame, AC Manteiga, M Moitinho, A Muinonen, K Osinde, J Pancino, E Pauwels, T Petit, JM Recio-Blanco, A Robin, AC Sarro, LM Siopis, C Smith, M Smith, KW Sozzetti, A Thuillot, W van Reeven, W Viala, Y Abbas, U Aramburu, AA Accart, S Aguado, JJ Allan, PM Allasia, W Altavilla, G Alvarez, MA Alves, J Anderson, RI Andrei, AH Varela, EA Antiche, E Antoja, T Anton, S Arcay, B Bach, N Baker, SG Balaguer-Nunez, L Barache, C Barata, C Barbier, A Barblan, F Navascues, DBY Barros, M Barstow, MA Becciani, U Bellazzini, M Garcia, AB Belokurov, V Bendjoya, P Berihuete, A Bianchi, L Bienayme, O Billebaud, F Blagorodnova, N Blanco-Cuaresma, S Boch, T Bombrun, A Borrachero, R Bouquillon, S Bourda, G Bouy, H Bragaglia, A Breddels, MA Brouillet, N Brusemeister, T Bucciarelli, B Burgess, P Burgon, R Burlacu, A Busonero, D Buzzi, R Caffau, E Cambras, J Campbell, H Cancelliere, R Cantat-Gaudin, T Carlucci, T Carrasco, JM Castellani, M Charlot, P Charnas, J Chiavassa, A Clotet, M Cocozza, G Collins, RS Costigan, G Crifo, F Cross, NJG Crosta, M Crowley, C Dafonte, C Damerdji, Y Dapergolas, A David, P David, M De Cat, P de Felice, F de Laverny, P De Luise, F De March, R de Martino, D de Souza, R Debosscher, J del Pozo, E Delbo, M Delgado, A Delgado, HE Di Matteo, P Diakite, S Distefano, E Dolding, C Dos Anjos, S Drazinos, P Duran, J Dzigan, Y Edvardsson, B Enke, H Evans, NW Bontemps, GE Fabre, C Fabrizio, M Faigler, S Falcao, AJ Casas, MF Federici, L Fedorets, G Fernandez-Hernaandez, J Fernique, P Fienga, A Figueras, F Filippi, F Findeisen, K Fonti, A Fouesneau, M Fraile, E Fraser, M Fuchs, J Gai, M Galleti, S Galluccio, L Garabato, D Garcia-Sedano, F Garofalo, A Garralda, N Gavras, P Gerssen, J Geyer, R Gilmore, G Girona, S Giuffrida, G Gomes, M Gonzalez-Marcos, A Gonzalez-Nunez, J Gonzalez-Vidal, JJ Granvik, M Guerrier, A Guillout, P Guiraud, J Gurpide, A Gutierrez-Sanchez, R Guy, LP Haigron, R Hatzidimitriou, D Haywood, M Heiter, U Helmi, A Hobbs, D Hofmann, W Holl, B Holland, G Hunt, JAS Hypki, A Icardi, V Irwin, M de Fombelle, GJ Jofre, P Jonker, PG Jorissen, A Julbe, F Karampelas, A Kochoska, A Kohley, R Kolenberg, K Kontizas, E Koposov, SE Kordopatis, G Koubsky, P Krone-Martins, A Kudryashova, M Kull, I Bachchan, RK Lacoste-Seris, F Lanza, AF Lavigne, JB Le Poncin-Lafitte, C Lebreton, Y Lebzelter, T Leccia, S Leclerc, N Lecoeur-Taibi, I Lemaitre, V Lenhardt, H Leroux, F Liao, S Licata, E Lindstrom, HEP Lister, TA Livanou, E Lobel, A Loffler, W Lopez, M Lorenz, D MacDonald, I Fernandes, TM Managau, S Mann, RG Mantelet, G Marchal, O Marchant, JM Marconi, M Marinoni, S Marrese, PM Marschalko, G Marshall, DJ Martin-Fleitas, JM Martino, M Mary, N Matijevic, G Mazeh, T McMillan, PJ Messina, S Michalik, D Millar, NR Miranda, BMH Molina, D Molinaro, R Molinaro, M Molnar, L Moniez, M Montegriffo, P Mor, R Mora, A Morbidelli, R Morel, T Morgenthaler, S Morris, D Mulone, AF Muraveva, T Musella, I Narbonne, J Nelemans, G Nicastro, L Noval, L Ordenovic, C Ordieres-Mere, J Osborne, P Pagani, C Pagano, I Pailler, F Palacin, H Palaversa, L Parsons, P Pecoraro, M Pedrosa, R Pentikainen, H Pichon, B Piersimoni, AM Pincau, FX Plachy, E Plum, G Poujoulet, E Prsa, A Pulone, L Ragaini, S Rago, S Rambaux, N Ramos-Lerate, M Ranalli, P Rauw, G Read, A Regibo, S Reyle, C Ribeiro, RA Rimoldini, L Ripepi, V Riva, A Rixon, G Roelens, M Romero-Gomez, M Rowell, N Royer, F Ruiz-Dern, L Sadowski, G Selles, TS Sahlmann, J Salgado, J Salguero, E Sarasso, M Savietto, H Schultheis, M Sciacca, E Segol, M Segovia, JC Segransan, D Shih, IC Smareglia, R Smart, RL Solano, E Solitro, F Sordo, R Nieto, SS Souchay, J Spagna, A Spoto, F Stampa, U Steele, IA Steidelmuller, H Stephenson, CA Stoev, H Suess, FF Suveges, M Surdej, J Szabados, L Szegedi-Elek, E Tapiador, D Taris, F Tauran, G Taylor, MB Teixeira, R Terrett, D Tingley, B Trager, SC Turon, C Ulla, A Utrilla, E Valentini, G van Elteren, A Van Hemelryck, E van Leeuwen, M Varadi, M Vecchiato, A Veljanoski, J Via, T Vicente, D Vogt, S Voss, H Votruba, V Voutsinas, S Walmsley, G Weiler, M Weingrill, K Wevers, T Wyrzykowski, L Yoldas, A Zerjal, M Zucker, S Zurbach, C Zwitter, T Alecu, A Allen, M Prieto, CA Amorim, A Anglada-Escude, G Arsenijevic, V Azaz, S Balm, P Beck, M Bernstein, HH Bigot, L Bijaoui, A Blasco, C Bonfigli, M Bono, G Boudreault, S Bressan, A Brown, S Brunet, PM Bunclark, P Buonanno, R Butkevich, AG Carret, C Carrion, C Chemin, L Chereau, F Corcione, L Darmigny, E de Boer, KS de Teodoro, P de Zeeuw, PT Delle Luche, C Domingues, CD Dubath, P Fodor, F Frezouls, B Fries, A Fustes, D Fyfe, D Gallardo, E Gallegos, J Gardiol, D Gebran, M Gomboc, A Gomez, A Grux, E Gueguen, A Heyrovsky, A Hoar, J Iannicola, G Parache, YI Janotto, AM Joliet, E Jonckheere, A Keil, R Kim, DW Klagyivik, P Klar, J Knude, J Kochukhov, O Kolka, I Kos, J Kutka, A Lainey, V LeBouquin, D Liu, C Loreggia, D Makarov, VV Marseille, MG Martayan, C Martinez-Rubi, O Massart, B Meynadier, F Mignot, S Munari, U Nguyen, AT Nordlander, T Ocvirk, P O'Flaherty, KS Sanz, AO Ortiz, P Osorio, J Oszkiewicz, D Ouzounis, A Palmer, M Park, P Pasquato, E Peltzer, C Peralta, J Peturaud, F Pieniluoma, T Pigozzi, E Poels, J Prat, G Prod'homme, T Raison, F Rebordao, JM Risquez, D Rocca-Volmerange, B Rosen, S Ruiz-Fuertes, MI Russo, F Sembay, S Vizcaino, IS Short, A Siebert, A Silva, H Sinachopoulos, D Slezak, E Soffel, M Sosnowska, D Straizys, V ter Linden, M Terrell, D Theil, S Tiede, C Troisi, L Tsalmantza, P Tur, D Vaccari, M Vachier, F Valles, P Van Hamme, W Veltz, L Virtanen, J Wallut, JM Wichmann, R Wilkinson, MI Ziaeepour, H Zschocke, S AF Brown, A. G. A. Vallenari, A. Prusti, T. de Bruijne, J. H. J. Mignard, F. Drimmel, R. Babusiaux, C. Bailer-Jones, C. A. L. Bastian, U. Biermann, M. Evans, D. W. Eyer, L. Jansen, F. Jordi, C. Katz, D. Klioner, S. A. Lammers, U. Lindegren, L. Luri, X. O'Mullane, W. Panem, C. Pourbaix, D. Randich, S. Sartoretti, P. Siddiqui, H. I. Soubiran, C. Valette, V. van Leeuwen, F. Walton, N. A. Aerts, C. Arenou, F. Cropper, M. Hog, E. Lattanzi, M. G. Grebel, E. K. Holland, A. D. Huc, C. Passot, X. Perryman, M. Bramante, L. Cacciari, C. Castaneda, J. Chaoul, L. Cheek, N. De Angeli, F. Fabricius, C. Guerra, R. Hernandez, J. Jean-Antoine-Piccolo, A. Masana, E. Messineo, R. Mowlavi, N. Nienartowicz, K. Ordonez-Blanco, D. Panuzzo, P. Portell, J. Richards, P. J. Riello, M. Seabroke, G. M. Tanga, P. Thevenin, F. Torra, J. Els, S. G. Gracia-Abril, G. Comoretto, G. Garcia-Reinaldos, M. Lock, T. Mercier, E. Altmann, M. Andrae, R. Astraatmadja, T. L. Bellas-Velidis, I. Benson, K. Berthier, J. Blomme, R. Busso, G. Carry, B. Cellino, A. Clementini, G. Cowell, S. Creevey, O. Cuypers, J. Davidson, M. De Ridder, J. de Torres, A. Delchambre, L. Dell'Oro, A. Ducourant, C. Fremat, Y. Garcia-Torres, M. Gosset, E. Halbwachs, J. -L. Hambly, N. C. Harrison, D. L. Hauser, M. Hestroffer, D. Hodgkin, S. T. Huckle, H. E. Hutton, A. Jasniewicz, G. Jordan, S. Kontizas, M. Korn, A. J. Lanzafame, A. C. Manteiga, M. Moitinho, A. Muinonen, K. Osinde, J. Pancino, E. Pauwels, T. Petit, J. -M. Recio-Blanco, A. Robin, A. C. Sarro, L. M. Siopis, C. Smith, M. Smith, K. W. Sozzetti, A. Thuillot, W. van Reeven, W. Viala, Y. Abbas, U. Aramburu, A. Abreu Accart, S. Aguado, J. J. Allan, P. M. Allasia, W. Altavilla, G. Alvarez, M. A. Alves, J. Anderson, R. I. Andrei, A. H. Varela, E. Anglada Antiche, E. Antoja, T. Anton, S. Arcay, B. Bach, N. Baker, S. G. Balaguer-Nunez, L. Barache, C. Barata, C. Barbier, A. Barblan, F. Barrado y Navascues, D. Barros, M. Barstow, M. A. Becciani, U. Bellazzini, M. Garcia, A. Bello Belokurov, V. Bendjoya, P. Berihuete, A. Bianchi, L. Bienayme, O. Billebaud, F. Blagorodnova, N. Blanco-Cuaresma, S. Boch, T. Bombrun, A. Borrachero, R. Bouquillon, S. Bourda, G. Bouy, H. Bragaglia, A. Breddels, M. A. Brouillet, N. Bruesemeister, T. Bucciarelli, B. Burgess, P. Burgon, R. Burlacu, A. Busonero, D. Buzzi, R. Caffau, E. Cambras, J. Campbell, H. Cancelliere, R. Cantat-Gaudin, T. Carlucci, T. Carrasco, J. M. Castellani, M. Charlot, P. Charnas, J. Chiavassa, A. Clotet, M. Cocozza, G. Collins, R. S. Costigan, G. Crifo, F. Cross, N. J. G. Crosta, M. Crowley, C. Dafonte, C. Damerdji, Y. Dapergolas, A. David, P. David, M. De Cat, P. de Felice, F. de laverny, P. De Luise, F. De March, R. de Martino, D. de Souza, R. Debosscher, J. del Pozo, E. Delbo, M. Delgado, A. Delgado, H. E. Di Matteo, P. Diakite, S. Distefano, E. Dolding, C. Dos Anjos, S. Drazinos, P. Duran, J. Dzigan, Y. Edvardsson, B. Enke, H. Evans, N. W. Bontemps, G. Eynard Fabre, C. Fabrizio, M. Faigler, S. Falcao, A. J. Casas, M. Farras Federici, L. Fedorets, G. Fernandez-Hernandez, J. Fernique, P. Fienga, A. Figueras, F. Filippi, F. Findeisen, K. Fonti, A. Fouesneau, M. Fraile, E. Fraser, M. Fuchs, J. Gai, M. Galleti, S. Galluccio, L. Garabato, D. Garcia-Sedano, F. Garofalo, A. Garralda, N. Gavras, P. Gerssen, J. Geyer, R. Gilmore, G. Girona, S. Giuffrida, G. Gomes, M. Gonzalez-Marcos, A. Gonzalez-Nunez, J. Gonzalez-Vidal, J. J. Granvik, M. Guerrier, A. Guillout, P. Guiraud, J. Gurpide, A. Gutierrez-Sanchez, R. Guy, L. P. Haigron, R. Hatzidimitriou, D. Haywood, M. Heiter, U. Helmi, A. Hobbs, D. Hofmann, W. Holl, B. Holland, G. Hunt, J. A. S. Hypki, A. Icardi, V. Irwin, M. de Fombelle, G. Jevardat Jofre, P. Jonker, P. G. Jorissen, A. Julbe, F. Karampelas, A. Kochoska, A. Kohley, R. Kolenberg, K. Kontizas, E. Koposov, S. E. Kordopatis, G. Koubsky, P. Krone-Martins, A. Kudryashova, M. Kull, I. Bachchan, R. K. Lacoste-Seris, F. Lanza, A. F. Lavigne, J. -B. Le Poncin-Lafitte, C. Lebreton, Y. Lebzelter, T. Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Lemaitre, V. Lenhardt, H. Leroux, F. Liao, S. Licata, E. Lindstrom, H. E. P. Lister, T. A. Livanou, E. Lobel, A. Loeffler, W. Lopez, M. Lorenz, D. MacDonald, I. Fernandes, T. Magalhacs Managau, S. Mann, R. G. Mantelet, G. Marchal, O. Marchant, J. M. Marconi, M. Marinoni, S. Marrese, P. M. Marschalko, G. Marshall, D. J. Martin-Fleitas, J. M. Martino, M. Mary, N. Matijevic, G. Mazeh, T. McMillan, P. J. Messina, S. Michalik, D. Millar, N. R. Miranda, B. M. H. Molina, D. Molinaro, R. Molinaro, M. Molnar, L. Moniez, M. Montegriffo, P. Mor, R. Mora, A. Morbidelli, R. Morel, T. Morgenthaler, S. Morris, D. Mulone, A. F. Muraveva, T. Musella, I. Narbonne, J. Nelemans, G. Nicastro, L. Noval, L. Ordenovic, C. Ordieres-Mere, J. Osborne, P. Pagani, C. Pagano, I. Pailler, F. Palacin, H. Palaversa, L. Parsons, P. Pecoraro, M. Pedrosa, R. Pentikainen, H. Pichon, B. Piersimoni, A. M. Pincau, F. -X. Plachy, E. Plum, G. Poujoulet, E. Prsa, A. Pulone, L. Ragaini, S. Rago, S. Rambaux, N. Ramos-Lerate, M. Ranalli, P. Rauw, G. Read, A. Regibo, S. Reyle, C. Ribeiro, R. A. Rimoldini, L. Ripepi, V. Riva, A. Rixon, G. Roelens, M. Romero-Gomez, M. Rowell, N. Royer, F. Ruiz-Dern, L. Sadowski, G. Selles, T. Sagrista Sahlmann, J. Salgado, J. Salguero, E. Sarasso, M. Savietto, H. Schultheis, M. Sciacca, E. Segol, M. Segovia, J. C. Segransan, D. Shih, I. -C. Smareglia, R. Smart, R. L. Solano, E. Solitro, F. Sordo, R. Nieto, S. Soria Souchay, J. Spagna, A. Spoto, F. Stampa, U. Steele, I. A. Steidelmueller, H. Stephenson, C. A. Stoev, H. Suess, F. F. Suveges, M. Surdej, J. Szabados, L. Szegedi-Elek, E. Tapiador, D. Taris, F. Tauran, G. Taylor, M. B. Teixeira, R. Terrett, D. Tingley, B. Trager, S. C. Turon, C. Ulla, A. Utrilla, E. Valentini, G. van Elteren, A. Van Hemelryck, E. van Leeuwen, M. Varadi, M. Vecchiato, A. Veljanoski, J. Via, T. Vicente, D. Vogt, S. Voss, H. Votruba, V. Voutsinas, S. Walmsley, G. Weiler, M. Weingrill, K. Wevers, T. Wyrzykowski, L. Yoldas, A. Zerjal, M. Zucker, S. Zurbach, C. Zwitter, T. Alecu, A. Allen, M. Prieto, C. Allende Amorim, A. Anglada-Escude, G. Arsenijevic, V. Azaz, S. Balm, P. Beck, M. Bernstein, H. -H. Bigot, L. Bijaoui, A. Blasco, C. Bonfigli, M. Bono, G. Boudreault, S. Bressan, A. Brown, S. Brunet, P. -M. Bunclark, P. Buonanno, R. Butkevich, A. G. Carret, C. Carrion, C. Chemin, L. Chereau, F. Corcione, L. Darmigny, E. de Boer, K. S. de Teodoro, P. de Zeeuw, P. T. Delle Luche, C. Domingues, C. D. Dubath, P. Fodor, F. Frezouls, B. Fries, A. Fustes, D. Fyfe, D. Gallardo, E. Gallegos, J. Gardiol, D. Gebran, M. Gomboc, A. Gomez, A. Grux, E. Gueguen, A. Heyrovsky, A. Hoar, J. Iannicola, G. Parache, Y. Isasi Janotto, A. -M. Joliet, E. Jonckheere, A. Keil, R. Kim, D. -W. Klagyivik, P. Klar, J. Knude, J. Kochukhov, O. Kolka, I. Kos, J. Kutka, A. Lainey, V. LeBouquin, D. Liu, C. Loreggia, D. Makarov, V. V. Marseille, M. G. Martayan, C. Martinez-Rubi, O. Massart, B. Meynadier, F. Mignot, S. Munari, U. Nguyen, A. -T. Nordlander, T. Ocvirk, P. O'Flaherty, K. S. Sanz, A. Olias Ortiz, P. Osorio, J. Oszkiewicz, D. Ouzounis, A. Palmer, M. Park, P. Pasquato, E. Peltzer, C. Peralta, J. Peturaud, F. Pieniluoma, T. Pigozzi, E. Poels, J. Prat, G. Prod'homme, T. Raison, F. Rebordao, J. M. Risquez, D. Rocca-Volmerange, B. Rosen, S. Ruiz-Fuertes, M. I. Russo, F. Sembay, S. Vizcaino, I. Serraller Short, A. Siebert, A. Silva, H. Sinachopoulos, D. Slezak, E. Soffel, M. Sosnowska, D. Straizys, V. ter Linden, M. Terrell, D. Theil, S. Tiede, C. Troisi, L. Tsalmantza, P. Tur, D. Vaccari, M. Vachier, F. Valles, P. Van Hamme, W. Veltz, L. Virtanen, J. Wallut, J. -M. Wichmann, R. Wilkinson, M. I. Ziaeepour, H. Zschocke, S. CA Gaia Collaboration TI Gaia Data Release 1 Summary of the astrometric, photometric, and survey properties SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE catalogs; astrometry; parallaxes; proper motions; surveys ID OPEN CLUSTERS; SKY SURVEY; ALL-SKY; CATALOG; PARALLAXES; BAND AB Context. At about 1000 days after the launch of Gaia we present the first Gaia data release, Gaia DR1, consisting of astrometry and photometry for over 1 billion sources brighter than magnitude 20.7. Aims. A summary of Gaia DR1 is presented along with illustrations of the scientific quality of the data, followed by a discussion of the limitations due to the preliminary nature of this release. Methods. The raw data collected by Gaia during the first 14 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into an astrometric and photometric catalogue. Results. Gaia DR1 consists of three components: a primary astrometric data set which contains the positions, parallaxes, and mean proper motions for about 2 million of the brightest stars in common with the HIPPARCOS and Tycho-2 catalogues - a realisation of the Tycho-Gaia Astrometric Solution (TGAS) - and a secondary astrometric data set containing the positions for an additional 1.1 billion sources. The second component is the photometric data set, consisting of mean G-band magnitudes for all sources. The G-band light curves and the characteristics of similar to 3000 Cepheid and RR Lyrae stars, observed at high cadence around the south ecliptic pole, form the third component. For the primary astrometric data set the typical uncertainty is about 0.3 mas for the positions and parallaxes, and about 1 mas yr(-1) for the proper motions. A systematic component of similar to 0.3 mas should be added to the parallax uncertainties. For the subset of similar to 94 000 HIPPARCOS stars in the primary data set, the proper motions are much more precise at about 0.06 mas yr(-1). For the secondary astrometric data set, the typical uncertainty of the positions is similar to 10 mas. The median uncertainties on the mean G-band magnitudes range from the mmag level to similar to 0.03 mag over the magnitude range 5 to 20.7. Conclusions. Gaia DR1 is an important milestone ahead of the next Gaia data release, which will feature five-parameter astrometry for all sources. Extensive validation shows that Gaia DR1 represents a major advance in the mapping of the heavens and the availability of basic stellar data that underpin observational astrophysics. Nevertheless, the very preliminary nature of this first Gaia data release does lead to a number of important limitations to the data quality which should be carefully considered before drawing conclusions from the data. C1 [Brown, A. G. A.; Costigan, G.; Hypki, A.; van Elteren, A.; de Zeeuw, P. T.; Prod'homme, T.; Risquez, D.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Vallenari, A.; Cantat-Gaudin, T.; Sordo, R.; Munari, U.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Prusti, T.; de Bruijne, J. H. J.; Perryman, M.; Antoja, T.; Allen, M.; Azaz, S.; Short, A.] European Space Res & Technol Ctr ESA ESTEC, Directorate Sci, Sci Support Off, Keplerlaan 1, NL-2201AZ Noordwijk, Netherlands. [Mignard, F.; Tanga, P.; Thevenin, F.; Carry, B.; Creevey, O.; Recio-Blanco, A.; Bendjoya, P.; Chiavassa, A.; de laverny, P.; Delbo, M.; Galluccio, L.; Kordopatis, G.; Ordenovic, C.; Pichon, B.; Schultheis, M.; Spoto, F.; Bigot, L.; Bijaoui, A.; Massart, B.; Slezak, E.] Univ Nice Sophia Antipolis, Lab Lagrange, Observ Cote dAzur, CNRS, CS 34229, F-06304 Nice, France. [Drimmel, R.; Lattanzi, M. G.; Cellino, A.; Sozzetti, A.; Abbas, U.; Bucciarelli, B.; Busonero, D.; Buzzi, R.; Crosta, M.; Gai, M.; Liao, S.; Morbidelli, R.; Rago, S.; Riva, A.; Sarasso, M.; Smart, R. L.; Spagna, A.; Vecchiato, A.; Corcione, L.; Gardiol, D.; Loreggia, D.; Russo, F.] Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, TO, Italy. [Babusiaux, C.; Katz, D.; Sartoretti, P.; Arenou, F.; Panuzzo, P.; Viala, Y.; Caffau, E.; Crifo, F.; Di Matteo, P.; Findeisen, K.; Gavras, P.; Haigron, R.; Haywood, M.; Lebreton, Y.; Leclerc, N.; Marchal, O.; Plum, G.; Royer, F.; Ruiz-Dern, L.; Shih, I. -C.; Turon, C.; Chereau, F.; Delle Luche, C.; Gomez, A.; Gueguen, A.; Meynadier, F.; Mignot, S.; Peturaud, F.] Univ Paris Diderot, PSL Res Univ, CNRS, GEPI,Observ Paris,Sorbonne Paris Cite, 5 Pl Jules Janssen, F-92190 Meudon, France. [Bailer-Jones, C. A. L.; Andrae, R.; Astraatmadja, T. L.; Smith, K. W.; Fouesneau, M.; Kim, D. -W.; Liu, C.; Tiede, C.; Tsalmantza, P.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Bastian, U.; Biermann, M.; Grebel, E. K.; Els, S. G.; Mercier, E.; Altmann, M.; Hauser, M.; Jordan, S.; Bruesemeister, T.; Hofmann, W.; Lenhardt, H.; Loeffler, W.; Mantelet, G.; Selles, T. Sagrista; Stampa, U.; Bernstein, H. -H.] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Evans, D. W.; van Leeuwen, F.; Walton, N. A.; De Angeli, F.; Riello, M.; Busso, G.; Cowell, S.; Harrison, D. L.; Hodgkin, S. T.; Belokurov, V.; Blagorodnova, N.; Burgess, P.; Campbell, H.; Delgado, A.; Evans, N. W.; Fraser, M.; Gilmore, G.; Holland, G.; Irwin, M.; Jofre, P.; Koposov, S. E.; Millar, N. R.; Osborne, P.; Rixon, G.; Suess, F. F.; van Leeuwen, M.; Wyrzykowski, L.; Yoldas, A.; Alecu, A.; Brown, S.; Bunclark, P.; Peltzer, C.; Wilkinson, M. I.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Eyer, L.; Mowlavi, N.; Anderson, R. I.; Barblan, F.; Blanco-Cuaresma, S.; Holl, B.; Palaversa, L.; Roelens, M.; Segransan, D.; Varadi, M.; Park, P.; Sosnowska, D.] Univ Geneva, Dept Astron, Chemin Maillettes 51, CH-1290 Versoix, Switzerland. [Jansen, F.] European Space Res & Technol Ctr ESA ESTEC, Directorate Sci, Operat Dept, Mission Operat Div, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Jordi, C.; Luri, X.; Castaneda, J.; Fabricius, C.; Masana, E.; Portell, J.; Torra, J.; Gracia-Abril, G.; Antiche, E.; Balaguer-Nunez, L.; Borrachero, R.; Carrasco, J. M.; Clotet, M.; Casas, M. Farras; Figueras, F.; Garralda, N.; Gonzalez-Vidal, J. J.; Gurpide, A.; Julbe, F.; Molina, D.; Mor, R.; Romero-Gomez, M.; Nieto, S. Soria; Voss, H.; Weiler, M.; Anglada-Escude, G.; Fries, A.; Gallardo, E.; Gebran, M.; Parache, Y. Isasi; Martinez-Rubi, O.; Palmer, M.; Valles, P.] Univ Barcelona, Inst Ciencies Cosmos, IEEC UB, Marti Franques 1, E-08028 Barcelona, Spain. [Klioner, S. A.; Geyer, R.; Steidelmueller, H.; Butkevich, A. G.; Soffel, M.; Zschocke, S.] Tech Univ Dresden, Lohrmann Observ, Mommsenstr 13, D-01062 Dresden, Germany. [Lammers, U.; O'Mullane, W.; Guerra, R.; Hernandez, J.; Garcia-Reinaldos, M.; Lock, T.; Kohley, R.; Sahlmann, J.; Hoar, J.] European Space Astron Ctr ESA ESAC, Camino Bajo dell Castillo S-N, Madrid 28692, Spain. [Lindegren, L.; Hobbs, D.; Bachchan, R. K.; McMillan, P. J.; Michalik, D.; Ranalli, P.] Lund Univ, Dept Astron & Theoret Phys, Lund Observ, Box 43, S-22100 Lund, Sweden. [Panem, C.; Valette, V.; Huc, C.; Passot, X.; Chaoul, L.; Jean-Antoine-Piccolo, A.; Burlacu, A.; Guiraud, J.; Pailler, F.; Walmsley, G.; Brunet, P. -M.; Darmigny, E.; Fodor, F.; Frezouls, B.; Janotto, A. -M.; Nguyen, A. -T.; Wallut, J. -M.] CNES Ctr Spatial Toulouse, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Pourbaix, D.; Siopis, C.; Jorissen, A.; Sadowski, G.; Pasquato, E.] Univ Libre Bruxelles, Inst Astron & Astrophys, CP 226,Blvd Triomphe, B-1050 Brussels, Belgium. [Pourbaix, D.; Gosset, E.] FRS FNRS, Rue Egmont 5, B-1000 Brussels, Belgium. [Randich, S.; Dell'Oro, A.; Pancino, E.] Osserv Astrofis Arcetri, INAF, Largo Enrico Fermi 5, I-50125 Florence, Italy. [Siddiqui, H. I.; Comoretto, G.; Gutierrez-Sanchez, R.; Parsons, P.; Stephenson, C. A.; Balm, P.] Telespazio Vega UK Ltd, ESA ESAC, Camino Bajo del Castillo, Madrid 28692, Spain. [Soubiran, C.; Ducourant, C.; Billebaud, F.; Blanco-Cuaresma, S.; Bourda, G.; Brouillet, N.; Charlot, P.; Jofre, P.; Chemin, L.] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18N,Allee Geoffroy St Hilaire, F-33615 Pessac, France. [Aerts, C.; De Ridder, J.; Debosscher, J.; Kolenberg, K.; Nelemans, G.; Regibo, S.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. [Aerts, C.; Jonker, P. G.; Nelemans, G.; Wevers, T.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Cropper, M.; Seabroke, G. M.; Benson, K.; Huckle, H. E.; Smith, M.; Baker, S. G.; Dolding, C.; Hunt, J. A. S.; Prieto, C. Allende; Boudreault, S.; Rosen, S.] Univ Coll London, Mullard Space Sci Lab, Surrey RH5 6NT, England. [Hog, E.; Lindstrom, H. E. P.; Knude, J.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. [Holland, A. D.; Burgon, R.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. [Bramante, L.; Messineo, R.; De March, R.; Filippi, F.; Fonti, A.; Icardi, V.; Martino, M.; Mulone, A. F.; Solitro, F.; Pigozzi, E.] ALTEC Spa, Corso Marche 79, I-10146 Turin, Italy. [Cacciari, C.; Clementini, G.; Altavilla, G.; Bellazzini, M.; Bragaglia, A.; Cocozza, G.; Federici, L.; Galleti, S.; Garofalo, A.; Montegriffo, P.; Muraveva, T.; Ragaini, S.] Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. [Cheek, N.; Varela, E. Anglada; Fernandez-Hernandez, J.; Gonzalez-Nunez, J.; Segovia, J. C.; de Teodoro, P.; Gallegos, J.] Serco Gest Negocios ESA ESAC, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Nienartowicz, K.; Ordonez-Blanco, D.; Charnas, J.; Guy, L. P.; de Fombelle, G. Jevardat; Lecoeur-Taibi, I.; Rimoldini, L.; Suveges, M.; Beck, M.; Dubath, P.; Ruiz-Fuertes, M. I.] Univ Geneva, Dept Astron, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. [Richards, P. J.; Allan, P. M.; Terrett, D.] Rutherford Appleton Lab, STFC, Didcot OX11 0QX, Oxon, England. [Els, S. G.; Gracia-Abril, G.; Mercier, E.] ESAC, Gaia DPAC Project Off, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Altmann, M.; Andrei, A. H.; Barache, C.; Bouquillon, S.; Carlucci, T.; Le Poncin-Lafitte, C.; Souchay, J.; Taris, F.; Meynadier, F.] UPMC Univ Paris 06, PSL Res Univ, CNRS, SYRTE,Observ Paris,Sorbonne Univ,LNE, 61 Ave Observ, F-75014 Paris, France. [Bellas-Velidis, I.; Dapergolas, A.; Gavras, P.; Karampelas, A.; Kontizas, E.; Sinachopoulos, D.] Natl Observ Athens, Athens 15236, Greece. [Berthier, J.; Carry, B.; Hestroffer, D.; Thuillot, W.; David, P.; Kudryashova, M.; Rambaux, N.; Lainey, V.; Vachier, F.] UPMC Univ Paris 06, PSL Res Univ, IMCCE, Observ Paris,CNRS,Sorbonne Univ,Univ Lille, 77 Av Denfert Rochereau, F-75014 Paris, France. [Blomme, R.; Cuypers, J.; Fremat, Y.; Pauwels, T.; De Cat, P.; Lobel, A.; Van Hemelryck, E.; Jonckheere, A.; Martayan, C.] Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium. [Creevey, O.; Veltz, L.] Univ Paris XI, CNRS, Inst Astrophys Spatiale, UMR 8617, Batiment 121, F-91405 Orsay, France. [Davidson, M.; Hambly, N. C.; Collins, R. S.; Cross, N. J. G.; MacDonald, I.; Mann, R. G.; Morris, D.; Rowell, N.; Voutsinas, S.; Heyrovsky, A.; Ouzounis, A.] Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [de Torres, A.; Bombrun, A.; Crowley, C.; Joliet, E.; ter Linden, M.] ESA ESAC, HE Space Operat BV, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Delchambre, L.; Gosset, E.; Damerdji, Y.; Morel, T.; Rauw, G.; Surdej, J.; Poels, J.] Univ Liege, Inst Astrophys & Geophys, 19c,Allee 6 Aout, B-4000 Liege, Belgium. [Garcia-Torres, M.] Univ Pablo de Olavide, Area Lenguajes & Sistemas Informat, Ctra Utrera,Km 1, Seville 41013, Spain. [Halbwachs, J. -L.; Bienayme, O.; Boch, T.; Fernique, P.; Guillout, P.; Pincau, F. -X.; Ocvirk, P.; Siebert, A.] Univ Strasbourg, Observ Astron Strasbourg, CNRS, UMR 7550, 11 Rue Univ, F-67000 Strasbourg, France. [Harrison, D. L.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Hutton, A.; van Reeven, W.; Bach, N.; del Pozo, E.; Martin-Fleitas, J. M.; Mora, A.; Utrilla, E.] ESA ESAC, Aurora Technol, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Jasniewicz, G.; Zurbach, C.] Univ Montpellier, Lab Univers & Particules Montpellier, Pl Eugene Bataillon,CC72, F-34095 Montpellier 05, France. [Kontizas, M.; Drazinos, P.; Gavras, P.; Hatzidimitriou, D.; Karampelas, A.; Livanou, E.] Univ Athens, Dept Astrophys Astron & Mech, Athens 15783, Greece. [Korn, A. J.; Edvardsson, B.; Heiter, U.; Kochukhov, O.; Nordlander, T.] Uppsala Univ, Div Astron & Space Phys, Dept Phys & Astron, Box 516, S-75120 Uppsala, Sweden. [Lanzafame, A. C.] Univ Catania, Dipartimento Fis & Astron, Sez Astrofis, Via S Sofia 78, I-95123 Catania, Italy. [Lanzafame, A. C.; Becciani, U.; Distefano, E.; Lanza, A. F.; Messina, S.; Pagano, I.; Sciacca, E.] Osserv Astrofis Catania, INAF, Via S Sofia 78, I-95123 Catania, Italy. [Manteiga, M.; Alvarez, M. A.; Arcay, B.; Dafonte, C.; Garabato, D.; Fustes, D.] Univ A Coruna, Fac Informat, Campus Elvina S-N, La Coruna 15071, Spain. [Moitinho, A.; Barata, C.; Barros, M.; Gomes, M.; Krone-Martins, A.; Miranda, B. M. H.; Amorim, A.; Arsenijevic, V.] Univ Lisbon, CENTRA, FCUL, Edif C8, P-1749016 Lisbon, Portugal. [Muinonen, K.; Fedorets, G.; Granvik, M.; Pentikainen, H.; Oszkiewicz, D.; Pieniluoma, T.; Virtanen, J.] Univ Helsinki, Dept Phys, POB 64, FIN-00014 Helsinki, Finland. [Muinonen, K.; Virtanen, J.] Finnish Geospatial Res Inst FGI, Geodeetinrinne 2, Masala 02430, Finland. [Osinde, J.; Varela, E. Anglada; Duran, J.; Salgado, J.; Salguero, E.] ESA ESAC, Isdefe, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Pancino, E.; Fabrizio, M.; Giuffrida, G.; Marinoni, S.; Marrese, P. M.; Troisi, L.] ASI Sci Data Ctr, Via Politecn SNC, I-00133 Rome, Italy. [Petit, J. -M.; Robin, A. C.; Diakite, S.; Reyle, C.; Grux, E.; Ziaeepour, H.] Univ Bourgogne Franche Comte, OSU THETA Franche Comte Bourgogne, CNRS, Inst UTINAM UMR6213, F-25000 Besancon, France. [Sarro, L. M.; Aguado, J. J.; Delgado, H. E.; Garcia-Sedano, F.; Carrion, C.] UNED, Dept Inteligencia Artificial, C Juan del Rosal 16, Madrid 28040, Spain. [Aramburu, A. Abreu] ESA ESAC, Elecnor Deimos Space, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Accart, S.; Barbier, A.; Bontemps, G. Eynard; Guerrier, A.; Lacoste-Seris, F.; Lavigne, J. -B.; Lemaitre, V.; Leroux, F.; Managau, S.; Mary, N.; Narbonne, J.; Noval, L.; Palacin, H.; Tauran, G.; Delle Luche, C.; LeBouquin, D.; Marseille, M. G.; Massart, B.] CNES Ctr Spatial Toulouse, Thales Serv, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Allasia, W.; Bianchi, L.; Licata, E.; Pecoraro, M.] EURIX Srl, Via Carcano 26, I-10153 Turin, Italy. [Alves, J.; Lebzelter, T.; Lorenz, D.] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. [Anderson, R. I.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Andrei, A. H.] ON MCTI BR, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Andrei, A. H.] OV UFRJ BR, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, RJ, Brazil. [Anton, S.; Osorio, J.] Univ Porto, Fac Ciencias, Dept Matemat, Rua Campo Alegre 687, P-4169007 Oporto, Portugal. [Anton, S.] Univ Lisbon, Inst Astrofis & Ciencias Espaco, Fac Ciencias, P-1749016 Lisbon, Portugal. [Barrado y Navascues, D.; Bouy, H.; Lopez, M.; Solano, E.] ESA ESAC, Ctr Astrobiol CSIC INTA, Dept Astrofis, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Barstow, M. A.; Pagani, C.; Read, A.; Fyfe, D.; Ortiz, P.; Rosen, S.; Sembay, S.; Wilkinson, M. I.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. [Garcia, A. Bello] Univ Oviedo, Campus Univ, Gijon 33203, Spain. [Berihuete, A.] Univ Cadiz, Avd Univ, Cadiz 11002, Spain. [Breddels, M. A.; Helmi, A.; Trager, S. C.; Veljanoski, J.] Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands. [Cambras, J.; Via, T.; Tur, D.] Univ Catalunya, Consorci Serv, C Gran Capita 2-4 3rd Floor, Barcelona 08034, Spain. [Cancelliere, R.] Univ Turin, Dept Comp Sci, Corso Svizzera 185, I-10149 Turin, Italy. [Castellani, M.; Marinoni, S.; Marrese, P. M.; Pulone, L.; Bono, G.; Buonanno, R.; Iannicola, G.] Osserv Astron Roma, INAF, Via Frascati 33, I-00078 Rome, Italy. [Damerdji, Y.] CRAAG, Route Observ,BP 63 Bouzareah, Algiers 16340, Algeria. [David, M.] Univ Antwerp, Onderzoeksgrp Toegepaste Wiskunde, Middelheimlaan 1, B-2020 Antwerp, Belgium. [de Felice, F.] Univ Padua, Dept Phys & Astron, Via Marzolo 8, I-35131 Padua, Italy. [De Luise, F.; Fabrizio, M.; Piersimoni, A. M.; Valentini, G.; Bonfigli, M.] Osservatorio Astron Teramo, INAF, Via Mentore Maggini, I-64100 Teramo, Italy. [de Martino, D.; Leccia, S.; Marconi, M.; Molinaro, R.; Musella, I.; Ripepi, V.] Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. [de Souza, R.; Dos Anjos, S.; Teixeira, R.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao,1226 Cidade Univ, BR-05508900 Sao Paulo, SP, Brazil. [Dzigan, Y.; Zucker, S.] Tel Aviv Univ, Dept Geosci, IL-6997801 Tel Aviv, Israel. [Dzigan, Y.] Univ Amsterdam, Astron Inst Anton Pannekoek, POB 94249, NL-1090 GE Amsterdam, Netherlands. [Enke, H.; Gerssen, J.; Kordopatis, G.; Matijevic, G.; Weingrill, K.; Klar, J.; Ocvirk, P.; Siebert, A.; Veltz, L.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. [Fabre, C.] CNES Ctr Spatial Toulouse, ATOS, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Faigler, S.; Kull, I.; Mazeh, T.] Tel Aviv Univ, Sch Phys & Astron, IL-6997801 Tel Aviv, Israel. [Falcao, A. J.; Fernandes, T. Magalhacs; Ribeiro, R. A.; Silva, H.] UNINOVA CTS, Campus FCT UNL, P-2829516 Caparica, Portugal. [Fienga, A.] Univ Nice Sophia Antipolis, Lab Geoazur, UMR 7329, CNRS,Observ Cote dAzur, 250 Rue A Einstein, F-06560 Valbonne, France. [Fraile, E.] ESA ESAC, RHEA, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Fuchs, J.; Koubsky, P.; Votruba, V.; Kutka, A.] Acad Sci Czech Republic, Astron Inst, Fricova 298, Ondrejov 25165, Czech Republic. [Girona, S.; Vicente, D.] Barcelona Supercomp Ctr, Centro Nacl Supercomp, C Jordi Girona 29,Ed Nexus 2, Barcelona 08034, Spain. [Gonzalez-Marcos, A.] Univ La Rioja, Dept Mech Engn, C San Jose de Calasanz 31, Logrono 26004, La Rioja, Spain. [Gonzalez-Nunez, J.] Univ Vigo, ETSE Telecomunicac, Campus Lagoas Marcosende, Vigo 36310, Galicia, Spain. [Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. [Kochoska, A.; Zerjal, M.; Zwitter, T.; Gomboc, A.; Kos, J.] Univ Ljubljana, Fac Math & Phys, Jadranska Ulica 19, Ljubljana 1000, Slovenia. [Kolenberg, K.] Univ Antwerp, Dept Phys, Groenenborgerlaan 171, B-2020 Antwerp, Belgium. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lebreton, Y.] Univ Rennes 1, Inst Phys Rennes, F-35042 Rennes, France. [Liao, S.] Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. [Lindstrom, H. E. P.] CSC Danmark AS, Retortvej 8, DK-2500 Valby, Denmark. [Lister, T. A.] Las Cumbres Observ Global Telescope Network Inc, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Marchant, J. M.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Marschalko, G.; Molnar, L.; Plachy, E.; Szabados, L.; Szegedi-Elek, E.; Varadi, M.; Klagyivik, P.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. [Marschalko, G.] Univ Szeged, Baja Observ, Szegedi Ut 3-70, H-6500 Baja, Hungary. [Marshall, D. J.] Univ Paris Diderot, CEA Saclay, CEA DSM CNRS, IRFU,Serv Astrophys,Lab AIM, Bat 709, F-91191 Gif Sur Yvette, France. [Molinaro, M.; Smareglia, R.] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34143 Trieste, Italy. [Moniez, M.] Univ Paris Saclay, CNRS IN2P3, Univ Paris Sud, Lab Accelerateur Lineaire, F-91898 Orsay, France. [Morgenthaler, S.] Ecole Polytech Fed Lausanne, SB MATHAA STAP, MA B1 473,Batiment MA,Stn 8, CH-1015 Lausanne, Switzerland. [Nicastro, L.] INAF IASF Bologna, Via P Gobetti 101, I-40129 Bologna, Italy. [Ordieres-Mere, J.] Tech Univ Madrid, Jose Gutierrez Abascal 2, Madrid 28006, Spain. [Pedrosa, R.; Carret, C.] CNES Ctr Spatial Toulouse, EQUERT Int, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Poujoulet, E.] CNES Ctr Spatial Toulouse, AKKA, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Prsa, A.] Villanova Univ, Dept Astrophys & Planetary Sci, 800 E Lancaster Ave, Villanova, PA 19085 USA. [Ramos-Lerate, M.] ESA ESAC, Vitrociset Belgium, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Savietto, H.] Fork Res, Rua Cruzado Osberno,Lt 1,9 Esq, Lisbon, Portugal. [Segol, M.] CNES Ctr Spatial Toulouse, APAVE SUDEUROPE SAS, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Solano, E.] Spanish Virtual Observ, Granada, Spain. [Stoev, H.] INAF, Fdn Galileo Galilei, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, Santa Cruz De T, Spain. [Tapiador, D.] ESA ESAC, INSA, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Tapiador, D.] Univ Complutense Madrid, Dept Arquitectura Comp & Automat, Fac Informat, C Prof Jose Garcia Santesmases S-N, E-28040 Madrid, Spain. [Taylor, M. B.] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Tingley, B.] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, 120 Ny Munkegade,Bldg 1520, DK-8000 Aarhus C, Denmark. [Ulla, A.] Univ Vigo, Dept Appl Phys, Vigo 36310, Spain. [Vogt, S.] ESA ESTEC, HE Space Operat BV, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Wyrzykowski, L.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Prieto, C. Allende] Inst Astrofis Canarias, Tenerife 38205, Spain. [Prieto, C. Allende] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain. [Blasco, C.] ESA ESTEC, RHEA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Boudreault, S.] Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. [Bressan, A.] SISSA, Via Bonomea 265, I-34136 Trieste, Italy. [Chemin, L.] Minist Ciencia Tecnol, Inst Nacl Pesquisas Espaciais, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [de Boer, K. S.] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. [de Zeeuw, P. T.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Domingues, C. D.; Rebordao, J. M.] Univ Lisbon, Lab Opt Lasers & Syst, Fac Sci, Campus Lumiar,Estr Paco Lumiar 22, P-1649038 Lisbon, Portugal. [Gebran, M.] Notre Dame Univ, Dept Phys & Astron, POB 72, Zouk Mikael, Lebanon. [Gomboc, A.] Univ Nova Gorica, Vipavska 13, Nova Gorica 5000, Slovenia. [Gueguen, A.; Raison, F.] OPINAS, Max Planck Inst Extraterr Phys, Giessenbachstr, D-85741 Garching, Germany. [Joliet, E.] CALTECH, NASA IPAC Infrared Sci Arch, Mail Code 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA. [Keil, R.] Univ Bremen, Ctr Appl Space Technol & Micrograv ZARM, Fallturm 1, D-28359 Bremen, Germany. [Keil, R.] ESA ESOC, RHEA Syst, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Kolka, I.] Tartu Observ, EE-61602 Toravere, Estonia. [Kos, J.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Kutka, A.] Slovak Org Space Activ, Zamocka 18, Bratislava 85101, Slovakia. [Liu, C.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Makarov, V. V.] US Naval Observ, Astrometry Dept, 3450 Massachusetts Ave NW, Washington, DC 20392 USA. [Martayan, C.] European Southern Observ, Alonso de Cordova 3107, Casilla 19001, Santiago De Chi, Chile. [Massart, B.] Airbus Def & Space SAS, 31 Rue Cosmonautes, F-31402 Toulouse 4, France. [O'Flaherty, K. S.] ESA ESTEC, EJR Quartz BV, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Sanz, A. Olias] ESA ESAC, Server Labs, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Oszkiewicz, D.] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Ul Sloneczna 36, PL-60286 Poznan, Poland. [Prat, G.] CNES Ctr Spatial Toulouse, CS Syst Informat, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Prod'homme, T.] European Space Res & Technol Ctr ESA ESTEC, Directorate Sci, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Raison, F.] ESA ESAC, Praesepe BV, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Rocca-Volmerange, B.] UPMC, Sorbonne Univ, F-75014 Paris, France. [Rocca-Volmerange, B.] Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Vizcaino, I. Serraller] ESA ESAC, GMV, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Straizys, V.] Vilnius Univ, Inst Theoret Phys & Astron, Sauletekio Al 3, LT-10222 Vilnius, Lithuania. [ter Linden, M.] S&T Corp, POB 608, NL-2600 AP Delft, Netherlands. [Terrell, D.] Southwest Res Inst SwRI, Dept Space Studies, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. [Theil, S.] Inst Space Syst, Deutsch Zentrum Luft & Raumfahrt, Fallturm 1, D-28359 Bremen, Germany. [Tiede, C.] Univ Appl Sci Munich, Karlstr 6, D-80333 Munich, Germany. [Troisi, L.] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. [Vaccari, M.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Cape Town, South Africa. [Vaccari, M.] INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. [Van Hamme, W.] Florida Int Univ, Dept Phys, 11200 SW 8th St, Miami, FL 33199 USA. [Wichmann, R.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. RP Brown, AGA (reprint author), Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. EM brown@strw.leidenuniv.nl RI Arenou, Frederic/B-1846-2014; Bellas-Velidis, Ioannis/K-4615-2013; Koposov, Sergey/F-2754-2012; Gavras, Panagiotis/C-4485-2015; Rebordao, Jose Manuel/M-3269-2013; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; Votruba, Viktor/G-9058-2014; Koubsky, Pavel/G-9031-2014; OI de Martino, Domitilla/0000-0002-5069-4202; Arenou, Frederic/0000-0003-2837-3899; Koposov, Sergey/0000-0003-2644-135X; Gavras, Panagiotis/0000-0002-4383-4836; Rebordao, Jose Manuel/0000-0002-7418-0345; Barrado Navascues, David/0000-0002-5971-9242; Taylor, Mark/0000-0002-4209-1479; Garabato, Daniel/0000-0002-7133-6623; Cellino, Alberto/0000-0002-6645-334X; Moitinho de Almeida, Andre/0000-0003-0822-5995; Fabricius, Claus/0000-0003-2639-1372; Lanza, Antonino Francesco/0000-0001-5928-7251; McMillan, Paul/0000-0002-8861-2620; Alvarez, Marco/0000-0002-6786-2620; Berihuete, Angel/0000-0002-8589-4423; Alves, Joao/0000-0002-4355-0921; Nelemans, Gijs/0000-0002-0752-2974; Krone-Martins, Alberto/0000-0002-2308-6623 FU Algerian Centre de Recherche en Astronomie, Astrophysique et Geophysique of Bouzareah Observatory; Austrian FWF Hertha Firnberg Programme [T359, P20046, P23737]; BELgian federal Science Policy Office (BELSPO) through various PROgramme de Developpement d'EXperiences scientifiques (PRODEX) grants; Brazil-France exchange programme FAPESP-COFECUB; Brazil-France exchange programme CAPES-COFECUB; Chinese National Science Foundation [NSFC 11573054]; Czech-Republic Ministry of Education, Youth, and Sports [L.G. 15010]; Danish Ministry of Science; Estonian Ministry of Education and Research [IUT40-1]; European Commission [MRTN-CT-2006-033481, PIOF-GA-2009-255267, MTKD-CT-2004-014188, FP7-606740, 264895]; European Research Council (ERC) [320360]; European Research Council (ERC) through the European Union's Horizon research and innovation programme [670519]; European Science Foundation (ESF); European Space Agency; European Space Agency Plan for European Cooperating States (PECS) programme; Czech Space Office through ESA PECS [98058]; Academy of Finland; Magnus Ehrnrooth Foundation; French Centre National de la Recherche Scientifique (CNRS) through action "Defi MASTODONS"; French Centre National d'Etudes Spatiales (CNES); French Agence Nationale de la Recherche (ANR) [ANR-10-IDEX-0001-02]; Region Aquitaine; Universite de Bordeaux; French Utinam Institute of the Universite de Franche-Comte - Region de Franche-Comte; Institut des Sciences de l'Univers (INSU); German Aerospace Agency (Deutsches Zentrum fur Luft- und Raumfahrt e.V., DLR) [50QG0501, 50QG0601, 50QG0602, 50QG0701, 50QG0901, 50QG1001, 50QG1101, 50QG140, 50QG1401, 50QG1402, 50QG1404]; Hungarian Academy of Sciences through Lendulet Programme [LP2014-17]; Hungarian National Research, Development, and Innovation Office [NKFIH K-115709, PD-116175]; Israel Ministry of Science and Technology [3-9082]; Agenzia Spaziale Italiana (ASI) [I/037/08/0, I/058/10/0, 2014-025-R.0, 2014-025-R.1.2015, I/008/10/0, 2013/030/I.0]; Italian Istituto Nazionale di Astrofisica (INAF); Netherlands Organisation for Scientific Research (NWO) [NWO-M-614.061.414]; Netherlands Research School for Astronomy (NOVA); Polish National Science Centre through HARMONIA grant [2015/18/M/ST9/00544]; Portugese Fundacao para a Ciencia e a Tecnologia (FCT) [PTDC/CTE-SPA/118692/2010, PDCTE/CTE-AST/81711/2003, SFRH/BPD/74697/2010]; Slovenian Research Agency; Spanish Ministry of Economy MINECO-FEDER [AyA2014-55216, AyA2011-24052, ESP2013-48318-C2-R, ESP2014-55996-C2-R]; ICCUB (Unidad de Excelencia Maria de Maeztu) [MDM-2014-0369]; Swedish National Space Board (SNSB/Rymdstyrelsen); Swiss State Secretariat for Education, Research, and Innovation; Swiss National Science Foundation; Early Postdoc.Mobility fellowship; United Kingdom Rutherford Appleton Laboratory; United Kingdom Science and Technology Facilities Council (STFC) [PP/C506756/1, ST/I00047X/1]; United Kingdom Space Agency (UKSA) [ST/K000578/1, ST/N000978/1]; Robert Martin Ayers Sciences Fund; National Aeronautics and Space Administration; National Science Foundation; [PEst-OE/AMB/UI4006/2011]; [UID/FIS/00099/2013]; [UID/EEA/00066/2013] FX This work has made use of results from the European Space Agency (ESA) space mission Gaia, the data from which were processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Gaia mission website is http://www.cosmos.esa.int/gaia. The authors are current or past members of the ESA Gaia mission team and of the Gaia DPAC. This work has received financial supported from the Algerian Centre de Recherche en Astronomie, Astrophysique et Geophysique of Bouzareah Observatory; the Austrian FWF Hertha Firnberg Programme through grants T359, P20046, and P23737; the BELgian federal Science Policy Office (BELSPO) through various PROgramme de Developpement d'EXperiences scientifiques (PRODEX) grants; the Brazil-France exchange programmes FAPESP-COFECUB and CAPES-COFECUB; the Chinese National Science Foundation through grant NSFC 11573054; the Czech-Republic Ministry of Education, Youth, and Sports through grant L.G. 15010; the Danish Ministry of Science; the Estonian Ministry of Education and Research through grant IUT40-1; the European Commission's Sixth Framework Programme through the European Leadership in Space Astrometry (ELSA) Marie Curie Research Training Network (MRTN-CT-2006-033481), through Marie Curie project PIOF-GA-2009-255267 (SAS-RRL), and through a Marie Curie Transfer-of-Knowledge (ToK) fellowship (MTKD-CT-2004-014188); the European Commission's Seventh Framework Programme through grant FP7-606740 (FP7-SPACE-2013-1) for the Gaia European Network for Improved data User Services (GENIUS) and through grant 264895 for the Gaia Research for European Astronomy Training (GREAT-ITN) network; the European Research Council (ERC) through grant 320360 and through the European Union's Horizon 2020 research and innovation programme through grant agreement 670519 (Mixing and Angular Momentum tranSport of massIvE stars - MAMSIE); the European Science Foundation (ESF), in the framework of the Gaia Research for European Astronomy Training Research Network Programme (GREAT-ESF); the European Space Agency in the framework of the Gaia project; the European Space Agency Plan for European Cooperating States (PECS) programme through grants for Slovenia; the Czech Space Office through ESA PECS contract 98058; the Academy of Finland; the Magnus Ehrnrooth Foundation; the French Centre National de la Recherche Scientifique (CNRS) through action "Defi MASTODONS"; the French Centre National d'Etudes Spatiales (CNES); the French Agence Nationale de la Recherche (ANR) "investissements d'avenir" Initiatives D'EXcellence (IDEX) programme PSL* through grant ANR-10-IDEX-0001-02; the Region Aquitaine; the Universite de Bordeaux; the French Utinam Institute of the Universite de Franche-Comte, supported by the Region de Franche-Comte and the Institut des Sciences de l'Univers (INSU); the German Aerospace Agency (Deutsches Zentrum fur Luft- und Raumfahrt e.V., DLR) through grants 50QG0501, 50QG0601, 50QG0602, 50QG0701, 50QG0901, 50QG1001, 50QG1101, 50QG140, 50QG1401, 50QG1402, and 50QG1404; the Hungarian Academy of Sciences through Lendulet Programme LP2014-17; the Hungarian National Research, Development, and Innovation Office through grants NKFIH K-115709 and PD-116175; the Israel Ministry of Science and Technology through grant 3-9082; the Agenzia Spaziale Italiana (ASI) through grants I/037/08/0, I/058/10/0, 2014-025-R.0, and 2014-025-R.1.2015 to INAF and contracts I/008/10/0 and 2013/030/I.0 to ALTEC S.p.A.; ; the Italian Istituto Nazionale di Astrofisica (INAF); the Netherlands Organisation for Scientific Research (NWO) through grant NWO-M-614.061.414 and through a VICI grant to A. Helmi; the Netherlands Research School for Astronomy (NOVA); the Polish National Science Centre through HARMONIA grant 2015/18/M/ST9/00544; the Portugese Fundacao para a Ciencia e a Tecnologia (FCT) through grants PTDC/CTE-SPA/118692/2010, PDCTE/CTE-AST/81711/2003, and SFRH/BPD/74697/2010; the Strategic Programmes PEst-OE/AMB/UI4006/2011 for SIM, UID/FIS/00099/2013 for CENTRA, and UID/EEA/00066/2013 for UNINOVA; the Slovenian Research Agency; the Spanish Ministry of Economy MINECO-FEDER through grants AyA2014-55216, AyA2011-24052, ESP2013-48318-C2-R, and ESP2014-55996-C2-R and MDM-2014-0369 of ICCUB (Unidad de Excelencia Maria de Maeztu); the Swedish National Space Board (SNSB/Rymdstyrelsen); the Swiss State Secretariat for Education, Research, and Innovation through the ESA PRODEX programme, the Mesures d'Accompagnement, and the Activites Nationales Complementaires; the Swiss National Science Foundation, including an Early Postdoc.Mobility fellowship; the United Kingdom Rutherford Appleton Laboratory; the United Kingdom Science and Technology Facilities Council (STFC) through grants PP/C506756/1 and ST/I00047X/1; and the United Kingdom Space Agency (UKSA) through grants ST/K000578/1 and ST/N000978/1. We acknowledge the valuable advice provided by Vincenzo Innocente (CERN) during two pre-launch reviews of DPAC. This research has made use of the Set of Identifications, Measurements, and Bibliography for Astronomical Data (Wenger et al. 2000) and of the "Aladin sky atlas" (Bonnarel et al. 2000; Boch & Fernique 2014), which are developed and operated at Centre de Donnees astronomiques de Strasbourg (CDS), France. Some of the figures in this paper were made with TOPCAT (http://www.starlink.ac.uk/topcat/) or through the use of the STIL library (http://www.starlink.ac.uk/stil). This research made use of the AAVSO Photometric All-Sky Survey (APASS, https://www.aavso.org/apass), funded by the Robert Martin Ayers Sciences Fund. This publication made use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. We thank the anonymous referee for suggestions that helped improve this paper. NR 44 TC 37 Z9 37 U1 8 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A2 DI 10.1051/0004-6361/201629512 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500136 ER PT J AU Cruz, P Barrado, D Lillo-Box, J Diaz, M Birkby, J Lopez-Morales, M Fortney, JJ AF Cruz, Patricia Barrado, David Lillo-Box, Jorge Diaz, Marcos Birkby, Jayne Lopez-Morales, Mercedes Fortney, Jonathan J. TI Detection of the secondary eclipse of Qatar-1b in the Ks band SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: individual: Qatar-1b; techniques: photometric ID INFRARED THERMAL EMISSION; GROUND-BASED DETECTION; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; IN HABITABLE ZONES; MASS M-STARS; TERRESTRIAL EXOPLANETS; HOT JUPITERS; WASP-12B; RADIUS AB Aims. Qatar-1b is a close-orbiting hot Jupiter (R-p similar or equal to 1.18 RJ, M-p similar or equal to 1.33 M-J) around a metal-rich K-dwarf, with orbital separation and period of 0.023 AU and 1.42 days. We have observed the secondary eclipse of this exoplanet in the Ks band with the objective of deriving a brightness temperature for the planet and providing further constraints to the orbital configuration of the system. Methods. We obtained near-infrared photometric data from the ground by using the OMEGA2000 instrument at the 3.5 m telescope at Calar Alto (Spain) in staring mode, with the telescope defocused. We have used principal component analysis (PCA) to identify correlated systematic trends in the data. A Markov chain Monte Carlo analysis was performed to model the correlated systematics and fit for the secondary eclipse of Qatar-1b using a previously developed occultation model. We adopted the prayer bead method to assess the effect of red noise on the derived parameters. Results. We measured a secondary eclipse depth of 0.196% (+0.071%)(-0.051%),which indicates a brightness temperature in the Ks band for the planet of 1885(-168)(+212) K. We also measured a small deviation in the central phase of the secondary eclipse of -0.0079(-0.0043)(+0.0162), which leads to a value for e cos omega of 0.012(-0.0067)(+0.0252). However, this last result needs to be confirmed with more data. C1 [Cruz, Patricia; Diaz, Marcos] Univ Sao Paulo IAG USP, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo, Brazil. [Cruz, Patricia; Barrado, David; Lillo-Box, Jorge] CSIC, INTA, Ctr Astrobiol, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Villanueva De La Canada 28692, Spain. [Lillo-Box, Jorge] ESO, Alonso Cordova 3107,Vitacura,Casilla 19001, Santiago, Chile. [Birkby, Jayne; Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. RP Cruz, P (reprint author), Univ Sao Paulo IAG USP, Inst Astron Geofis & Ciencias Atmosfer, Sao Paulo, Brazil.; Cruz, P (reprint author), CSIC, INTA, Ctr Astrobiol, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Villanueva De La Canada 28692, Spain. EM patricia.cruz@usp.br RI Barrado Navascues, David/C-1439-2017 OI Barrado Navascues, David/0000-0002-5971-9242 FU Spanish grants [AYA2012-38897-C02-01, PRICIT-S2009/ESP-1496]; RoPACS network during this research, a Marie Curie Initial Training Network - European Commissions Seventh Framework Programme; European Commission; NASA through the Sagan Fellowship Program FX This research has been funded by Spanish grants AYA2012-38897-C02-01, and PRICIT-S2009/ESP-1496. P.C., D.B., and J.B. have received support from the RoPACS network during this research, a Marie Curie Initial Training Network funded by the European Commissions Seventh Framework Programme. J.L.-B. acknowledges financial support from the Marie Curie Actions of the European Commission (FP7-COFUND) and the Spanish grant AYA2012-38897-C02-01. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This article is based on data collected under Service Time program at the Calar Alto Observatory, the German-Spanish Astronomical Center, Calar Alto, jointly operated by the Max-Planck-Institut fur Astronomie Heidelberg and the Instituto de Astrofisica de Andalucia (CSIC). We are very grateful to the CAHA staff for the superb quality of the observations. This work has made use of the ALADIN interactive sky atlas and the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. NR 21 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A61 DI 10.1051/0004-6361/201526333 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500008 ER PT J AU Garraffo, C Drake, JJ Cohen, O AF Garraffo, Cecilia Drake, Jeremy J. Cohen, Ofer TI The missing magnetic morphology term in stellar rotation evolution (Research Note) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); stars: activity; stars: rotation ID LOW-MASS STARS; SOLAR-TYPE STARS; PRE-MAIN-SEQUENCE; SUN-LIKE STARS; ANGULAR-MOMENTUM; DIFFERENTIAL ROTATION; SPIN-DOWN; CYCLE 23; FIELDS; WIND AB Aims. This study examines the relationship between magnetic field complexity and mass and angular momentum losses. Observations of open clusters have revealed a bimodal distribution of the rotation periods of solar-like stars that has proven difficult to explain under the existing rubric of magnetic braking. Recent studies suggest that magnetic complexity can play an important role in controlling stellar spin-down rates. However, magnetic morphology is still neglected in most rotation evolution models due to the difficulty of properly accounting for its effects on wind driving and angular momentum loss. Methods. Using state-of-the-art magnetohydrodynamical magnetized wind simulations we study the effect that different distributions of the magnetic flux at different levels of geometrical complexity have on mass and angular momentum loss rates. Results. Angular momentum loss rates depend strongly on the level of complexity of the field but are independent of the way this complexity is distributed. We deduce the analytical terms representing the magnetic field morphology dependence of mass and angular momentum loss rates. We also define a parameter that best represents complexity for real stars. As a test, we use these analytical methods to estimate mass and angular momentum loss rates for 8 stars with observed magnetograms and compare them to the simulated results. Conclusions. Magnetic field complexity provides a natural physical basis for stellar rotation evolution models requiring a rapid transition between weak and strong spin-down modes. C1 [Garraffo, Cecilia; Drake, Jeremy J.; Cohen, Ofer] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Garraffo, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cgarraffo@cfa.harvard.edu FU SI Grand Challenges grant "Lessons from Mars: are habitable atmospheres on planets around M dwarfs viable?"; SI CGPS grant "Can exoplanets around red dwarfs maintain habitable atmospheres?"; "Living with a star" grant [NNX16AC11G]; NASA [NAS8-03060]; NASA HEC Pleiades system [SMD-13-4526] FX We thank anonymous referee for helpful comments and discussion that allowed us to significantly improve this work. C.G. and O.C. were supported by SI Grand Challenges grant "Lessons from Mars: are habitable atmospheres on planets around M dwarfs viable?". O.C. was also supported by SI CGPS grant "Can exoplanets around red dwarfs maintain habitable atmospheres?" and "Living with a star" grant NNX16AC11G. J.J.D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center. The authors thank Vinay Kashyap for helpful discussions. Numerical simulations were performed on the NASA HEC Pleiades system under award SMD-13-4526, and on the Smithsonian Institution High Performance Cluster (SI/HPC). NR 44 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A110 DI 10.1051/0004-6361/201628367 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500039 ER PT J AU Ginsburg, A Goss, WM Goddi, C Galvan-Madrid, R Dale, JE Bally, J Battersby, CD Youngblood, A Sankrit, R Smith, R Darling, J Kruijssen, JMD Liu, HB AF Ginsburg, A. Goss, W. M. Goddi, C. Galvan-Madrid, R. Dale, J. E. Bally, J. Battersby, C. D. Youngblood, A. Sankrit, R. Smith, R. Darling, J. Kruijssen, J. M. D. Liu, H. B. TI Toward gas exhaustion in the W51 high-mass protoclusters SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE H II regions; circumstellar matter; radio continuum: ISM; radio lines: ISM; stars: massive; stars: protostars ID H-II REGIONS; GIANT MOLECULAR CLOUD; STAR-FORMING REGIONS; YOUNG STELLAR OBJECTS; R-CORONAE-AUSTRALIS; RHO-OPHIUCHI CLOUD; FORMALDEHYDE EMISSION; CLUSTER PROGENITORS; CONTINUUM EMISSION; RADIO-CONTINUUM AB We present new JVLA observations of the high-mass cluster-forming region W51A from 2 to 16 GHz with resolution theta(fwhm) approximate to 0.3-0.5 ''. The data reveal a wealth of observational results: (1) Currently forming, very massive (proto-O) stars are traced by o-H2CO 2(1,1)-2(1,2) emission, suggesting that this line can be used efficiently as a massive protostar tracer; (2) there is a spatially distributed population of. less than or similar to mJy continuum sources, including hypercompact H II regions and candidate colliding wind binaries, in and around the W51 proto-clusters; and (3) there are two clearly detected protoclusters, W51e and W51 IRS2, that are gas-rich but may have most of their mass in stars within their inner. 0.05 pc. The majority of the bolometric luminosity in W51 most likely comes from a third population of OB stars between these clusters. The presence of a substantial population of exposed O-stars coincident with a population of still-forming massive stars, together with a direct measurement of the low mass loss rate via ionized gas outflow from W51 IRS2, implies that feedback is ineffective at halting star formation in massive protoclusters. Instead, feedback may shut off the large-scale accretion of diffuse gas onto the W51 protoclusters, implying that they are evolving toward a state of gas exhaustion rather than gas expulsion. Recent theoretical models predict gas exhaustion to be a necessary step in the formation of gravitationally bound stellar clusters, and our results provide an observational validation of this process. C1 [Ginsburg, A.; Liu, H. B.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Goddi, C.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Goddi, C.] Leiden Univ, Leiden Observ, ALLEGRO, POB 9513, NL-2300 RA Leiden, Netherlands. [Galvan-Madrid, R.] UNAM, Inst Radioastron & Astrofis, AP 3-72, Morelia 58089, Michoacan, Mexico. [Dale, J. E.] Univ Observ Excellence Cluster Universe, Scheinerstr 1, D-81679 Munich, Germany. [Bally, J.; Darling, J.] Univ Colorado, CASA, 389 UCB, Boulder, CO 80309 USA. [Battersby, C. D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Youngblood, A.] Univ Colorado, LASP, 600 UCB, Boulder, CO 80309 USA. [Sankrit, R.] NASA, Ames Res Ctr, SOFIA Sci Ctr, M-S 232-12, Moffett Field, CA 94035 USA. [Smith, R.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Oxford Rd, Manchester M13 9PL, Lancs, England. [Kruijssen, J. M. D.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Kruijssen, J. M. D.] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. RP Ginsburg, A (reprint author), European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM Adam.Ginsburg@eso.org FU Deutsche Forschungsgemeinschaft (DFG) [KR4801/1-1] FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. J.M.D.K. gratefully acknowledges financial support in the form of a Gliese Fellowship and an Emmy Noether Research Group from the Deutsche Forschungsgemeinschaft (DFG), grant number KR4801/1-1. This research made use of: APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com, Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), ds9, a tool for data visualization supported by the Chandra X-ray Science Center (CXC) and the High Energy Astrophysics Science Archive Center (HEASARC) with support from the JWST Mission office at the Space Telescope Science Institute for 3D visualization, myRadex, an alternative implementation of RADEX (http://home.strw.leidenuniv.nl/similar to moldata/radex.html), pvextractor, a tool to extract position-velocity diagrams along arbitrary directions from data cubes, pyradex, a python wrapper of RADEX (http://home.strw.leidenuniv.nl/similar to moldata/radex.html), pyspeckit, an open-source spectral analysis and plotting package for Python hosted at http://pyspeckit.bitbucket.org (Ginsburg & Mirocha 2011), spectralcube, a library for astronomical spectral data cubes, and wcsaxes, an open-source plotting library for Python hosted at https://wcsaxes.readthedocs.io/en/latest/. NR 102 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A27 DI 10.1051/0004-6361/201628318 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500037 ER PT J AU Jackson, N Tagore, A Deller, A Moldon, J Varenius, E Morabito, L Wucknitz, O Carozzi, T Conway, J Drabent, A Kapinska, A Orru, E Brentjens, M Blaauw, R Kuper, G Sluman, J Schaap, J Vermaas, N Iacobelli, M Cerrigone, L Shulevski, A ter Veen, S Fallows, R Pizzo, R Sipior, M Anderson, J Avruch, IM Bell, ME van Bemmel, I Bentum, MJ Best, P Bonafede, A Breitling, F Broderick, JW Brouw, WN Bruggen, M Ciardi, B Corstanje, A de Gasperin, F de Geus, E Eisloffel, J Engels, D Falcke, H Garrett, MA Griessmeier, JM Gunst, AW van Haarlem, MP Heald, G Hoeft, M Horandel, J Horneffer, A Intema, H Juette, E Kuniyoshi, M van Leeuwen, J Loose, GM Maat, P McFadden, R McKay-Bukowski, D McKean, JP Mulcahy, DD Munk, H Pandey-Pommier, M Polatidis, AG Reich, W Rottgering, HJA Rowlinson, A Scaife, AMM Schwarz, DJ Steinmetz, M Swinbank, J Thoudam, S Toribio, MC Vermeulen, R Vocks, C van Weeren, RJ Wise, MW Yatawatta, S Zarka, P AF Jackson, N. Tagore, A. Deller, A. Moldon, J. Varenius, E. Morabito, L. Wucknitz, O. Carozzi, T. Conway, J. Drabent, A. Kapinska, A. Orru, E. Brentjens, M. Blaauw, R. Kuper, G. Sluman, J. Schaap, J. Vermaas, N. Iacobelli, M. Cerrigone, L. Shulevski, A. ter Veen, S. Fallows, R. Pizzo, R. Sipior, M. Anderson, J. Avruch, I. M. Bell, M. E. van Bemmel, I. Bentum, M. J. Best, P. Bonafede, A. Breitling, F. Broderick, J. W. Brouw, W. N. Brueggen, M. Ciardi, B. Corstanje, A. de Gasperin, F. de Geus, E. Eisloeffel, J. Engels, D. Falcke, H. Garrett, M. A. Griessmeier, J. M. Gunst, A. W. van Haarlem, M. P. Heald, G. Hoeft, M. Horandel, J. Horneffer, A. Intema, H. Juette, E. Kuniyoshi, M. van Leeuwen, J. Loose, G. M. Maat, P. McFadden, R. McKay-Bukowski, D. McKean, J. P. Mulcahy, D. D. Munk, H. Pandey-Pommier, M. Polatidis, A. G. Reich, W. Rottgering, H. J. A. Rowlinson, A. Scaife, A. M. M. Schwarz, D. J. Steinmetz, M. Swinbank, J. Thoudam, S. Toribio, M. C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wise, M. W. Yatawatta, S. Zarka, P. TI LBCS: The LOFAR Long-Baseline Calibrator Survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE instrumentation: interferometers; techniques: interferometric; surveys; galaxies: active; radio continuum: galaxies ID FREQUENCY SKY SURVEY; RADIO-SOURCES; ARRAY; INTERFEROMETER; VLBI AB We outline the LOFAR Long-Baseline Calibrator Survey (LBCS), whose aim is to identify sources suitable for calibrating the highest-resolution observations made with the International LOFAR Telescope, which include baselines > 1000 km. Suitable sources must contain significant correlated flux density (greater than or similar to 50 - 100 mJy) at frequencies around 110-190 MHz on scales of a few hundred milliarcseconds. At least for the 200-300-km international baselines, we find around 1 suitable calibrator source per square degree over a large part of the northern sky, in agreement with previous work. This should allow a randomly selected target to be successfully phase calibrated on the international baselines in over 50% of cases. Products of the survey include calibrator source lists and fringe-rate and delay maps of wide areas-typically a few degrees-around each source. The density of sources with significant correlated flux declines noticeably with baseline length over the range 200-600 km, with good calibrators on the longest baselines appearing only at the rate of 0.5 per sq. deg. Coherence times decrease from 1-3 min on 200-km baselines to about 1 min on 600-km baselines, suggesting that ionospheric phase variations contain components with scales of a few hundred kilometres. The longest median coherence time, at just over 3 min, is seen on the DE609 baseline, which at 227 km is close to being the shortest. We see median coherence times of between 80 and 110 s on the four longest baselines (580-600 km), and about 2 min for the other baselines. The success of phase transfer from calibrator to target is shown to be influenced by distance, in a manner that suggests a coherence patch at 150-MHz of the order of 1 deg. Although source structures cannot be measured in these observations, we deduce that phase transfer is affected if the calibrator source structure is not known. We give suggestions for calibration strategies and choice of calibrator sources, and describe the access to the online catalogue and data products. C1 [Jackson, N.; Tagore, A.; Moldon, J.; Mulcahy, D. D.; Scaife, A. M. M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Deller, A.; Moldon, J.; Orru, E.; Brentjens, M.; Blaauw, R.; Kuper, G.; Sluman, J.; Schaap, J.; Vermaas, N.; Iacobelli, M.; Cerrigone, L.; Shulevski, A.; ter Veen, S.; Fallows, R.; Pizzo, R.; Sipior, M.; Bentum, M. J.; Broderick, J. W.; Brouw, W. N.; de Geus, E.; Falcke, H.; Garrett, M. A.; Gunst, A. W.; van Haarlem, M. P.; Heald, G.; van Leeuwen, J.; Loose, G. M.; Maat, P.; McFadden, R.; McKean, J. P.; Munk, H.; Polatidis, A. G.; Rowlinson, A.; Toribio, M. C.; Vermeulen, R.; Wise, M. W.; Yatawatta, S.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Varenius, E.; Carozzi, T.; Conway, J.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Morabito, L.; de Gasperin, F.; Garrett, M. A.; Intema, H.; Rottgering, H. J. A.; Toribio, M. C.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Wucknitz, O.; Eisloeffel, J.; Horneffer, A.; Reich, W.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Drabent, A.; Hoeft, M.] Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. [Kapinska, A.] Univ Portsmouth, Winston Churchill Ave, Portsmouth PO1 2UP, Hants, England. [Kapinska, A.] Univ Western Australia, ICRAR, Crawley, WA, Australia. [Kapinska, A.] Arc Ctr Excellence All Sky Astrophys, CAASTRO, Sydney, NSW 2006, Australia. [Anderson, J.] Helmholtz Zentrum Potsdam, Deutsch GeoForschungsZentrum GFZ, Dept Geodesy & Remote Sensing 1, Telegrafenberg A17, D-14473 Potsdam, Germany. [Avruch, I. M.] SRON Netherlands Insitute Space Res, POB 800, NL-9700 Groningen, Netherlands. [Avruch, I. M.; Brouw, W. N.; Heald, G.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 Groningen, Netherlands. [Bell, M. E.; Heald, G.] CSIRO Astron & Space Sci, 26 Dick Perry Ave, Kensington, WA 6151, Australia. [van Bemmel, I.] Joint Inst VLBI Europe, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Bentum, M. J.] Univ Twente, NL-7522 NB Enschede, Netherlands. [Best, P.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.] Univ Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Breitling, F.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. [Ciardi, B.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. [Corstanje, A.; Falcke, H.; Horandel, J.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [de Geus, E.] SmarterVision BV, Oostersingel 5, NL-9401 JX Assen, Netherlands. [Engels, D.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Griessmeier, J. M.] Univ Orleans CNRS, LPC2E, F-450751 Orleans 2, France. [Griessmeier, J. M.] Univ Orleans, OSUC, CNRS INSU USR 704, Stn Radioastron Nancay,Observ Paris, Route Souesmes, F-18330 Nancay, France. [Intema, H.] Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA. [Juette, E.] Ruhr Univ Bochum, Astronom Inst, Univ Str 150, D-44780 Bochum, Germany. [Kuniyoshi, M.] Natl Astron Observ Japan, Tokyo, Japan. [van Leeuwen, J.; Rowlinson, A.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Tahtelantie 62, Sodankyla 99600, Finland. [McKay-Bukowski, D.; Vermeulen, R.] STFC Rutherford Appleton Lab, Harwell Sci & Innovat Campus, Didcot OX11 0QX, Oxon, England. [Munk, H.] Radboud Univ Nijmegen, Radio Lab, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, 9 Ave Charles Andre, F-69561 St Genis Laval, France. [Schwarz, D. J.] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany. [Swinbank, J.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Zarka, P.] LESIA, Pl J Janssen, F-92195 Meudon, France. [Zarka, P.] PSL SU UPMC UPD SPC, CNRS, Observ Paris, USN, Pl J Janssen, F-92195 Meudon, France. RP Jackson, N (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. EM neal.jackson@manchester.ac.uk OI Varenius, Eskil/0000-0002-3248-9467 FU European Commission [283393, 617-199]; STFC; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020] FX LOFAR, the Low Frequency Array designed and constructed by ASTRON, has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (ILT) foundation under a joint scientific policy. The research leading to these results has received funding from the European Commission Seventh Framework Programme (FP/2007-2013) under grant agreements No. 283393 (RadioNet3), in the form of a travel grant to N.J. to support data analysis, and 617-199 (ALERT). A.T. acknowledges receipt of an STFC postdoctoral fellowship. ADK acknowledges financial support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. NR 28 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A86 DI 10.1051/0004-6361/201629016 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500098 ER PT J AU Jorgensen, JK van der Wiel, MHD Coutens, A Lykke, JM Muller, HSP van Dishoeck, EF Calcutt, H Bjerkeli, P Bourke, TL Drozdovskaya, MN Favre, C Fayolle, EC Garrod, RT Jacobsen, SK Oberg, KI Persson, MV Wampfler, SF AF Jorgensen, J. K. van der Wiel, M. H. D. Coutens, A. Lykke, J. M. Mueller, H. S. P. van Dishoeck, E. F. Calcutt, H. Bjerkeli, P. Bourke, T. L. Drozdovskaya, M. N. Favre, C. Fayolle, E. C. Garrod, R. T. Jacobsen, S. K. Oberg, K. I. Persson, M. V. Wampfler, S. F. TI The ALMA Protostellar Interferometric Line Survey (PILS) First results from an unbiased submillimeter wavelength line survey of the Class 0 protostellar binary IRAS 16293-2422 with ALMA SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; stars: protostars; ISM: molecules; ISM: individual objects: IRAS 16293-2422; submillimeter: ISM ID LOW-MASS PROTOSTAR; SOLAR-TYPE PROTOSTAR; COMPLEX ORGANIC-MOLECULES; STAR-FORMING REGIONS; GRAIN-SURFACE-CHEMISTRY; WATER DEUTERIUM FRACTIONATION; INTERSTELLAR HEAVY-WATER; YOUNG STELLAR OBJECTS; HOT-CORE; ETHYLENE-GLYCOL AB Context. The inner regions of the envelopes surrounding young protostars are characterized by a complex chemistry, with prebiotic molecules present on the scales where protoplanetary disks eventually may form. The Atacama Large Millimeter/submillimeter Array (ALMA) provides an unprecedented view of these regions zooming in on solar system scales of nearby protostars and mapping the emission from rare species. Aims. The goal is to introduce a systematic survey, the Protostellar Interferometric Line Survey (PILS), of the chemical complexity of one of the nearby astrochemical templates, the Class 0 protostellar binary IRAS 16293 2422, using ALMA in order to understand the origin of the complex molecules formed in its vicinity. In addition to presenting the overall survey, the analysis in this paper focuses on new results for the prebiotic molecule glycolaldehyde, its isomers, and rarer isotopologues and other related molecules. Methods. An unbiased spectral survey of IRAS 16293 2422 covering the full frequency range from 329 to 363 GHz (0.8 mm) has been obtained with ALMA, in addition to a few targeted observations at 3.0 and 1.3 mm. The data consist of full maps of the protostellar binary system with an angular resolution of 0.5 '' (60 AU diameter), a spectral resolution of 0.2 km s(-1), and a sensitivity of 4-5 mJy beam(-1) km s(-1), which is approximately two orders of magnitude better than any previous studies. Results. More than 10 000 features are detected toward one component in the protostellar binary, corresponding to an average line density of approximately one line per 3 km s(-1). Glycolaldehyde; its isomers, methyl formate and acetic acid; and its reduced alcohol, ethylene glycol, are clearly detected and their emission well-modeled with an excitation temperature of 300 K. For ethylene glycol both lowest state conformers, aGg' and gGg', are detected, the latter for the first time in the interstellar medium (ISM). The abundance of glycolaldehyde is comparable to or slightly larger than that of ethylene glycol. In comparison to the Galactic Center these two species are over-abundant relative to methanol, possibly an indication of formation of the species at low temperatures in CO-rich ices during the infall of the material toward the central protostar. Both C-13 and the deuterated isotopologues of glycolaldehyde are detected, also for the first time ever in the ISM. For the deuterated species, a D/H ratio of approximate to 5% is found with no differences between the deuteration in the different functional groups of glycolaldehyde, in contrast to previous estimates for methanol and recent suggestions of significant equilibration between water and-OH functional groups at high temperatures. Measurements of the C-13-species lead to a C-12:C-13 ratio of approximate to 30, lower than the typical ISM value. This low ratio may reflect an enhancement of (CO)-C-13 in the ice due to either ion-molecule reactions in the gas before freeze-out or to differences in the temperatures where (CO)-C-12 and (CO)-C-13 ices sublimate. Conclusions. The results reinforce the importance of low-temperature grain surface chemistry for the formation of prebiotic molecules seen here in the gas after sublimation of the entire ice mantle. Systematic surveys of the molecules thought to be chemically related, as well as the accurate measurements of their isotopic composition, hold strong promise for understanding the origin of prebiotic molecules in the earliest stages of young stars. C1 [Jorgensen, J. K.; van der Wiel, M. H. D.; Lykke, J. M.; Calcutt, H.; Bjerkeli, P.; Jacobsen, S. K.] Univ Copenhagen, Niels Bohr Inst & Nat Hist, Museum Denmark, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. [Coutens, A.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Mueller, H. S. P.] Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany. [van Dishoeck, E. F.; Drozdovskaya, M. N.; Persson, M. V.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, Giessenbachstr 1, D-85748 Garching, Germany. [Bjerkeli, P.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Bourke, T. L.] SKA Org, Jodrell Bank Observ, Macclesfield SK11 9DL, Cheshire, England. [Favre, C.] Univ Grenoble Alpes, F-38000 Grenoble, France. [Favre, C.] CNRS, IPAG, F-38000 Grenoble, France. [Fayolle, E. C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Garrod, R. T.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Garrod, R. T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Wampfler, S. F.] Univ Bern, CSH, Sidlerstr 5, CH-3012 Bern, Switzerland. RP Jorgensen, JK (reprint author), Univ Copenhagen, Niels Bohr Inst & Nat Hist, Museum Denmark, Ctr Star & Planet Format, Oster Voldgade 5-7, DK-1350 Copenhagen K, Denmark. EM jeskj@nbi.ku.dk OI Persson, Magnus Vilhelm/0000-0002-1100-5734 FU Lundbeck Foundation Group Leader Fellowship; European Research Council (ERC) under the European Union's Horizon research and innovation programme through ERC Consolidator Grant "S4F" [646908]; Danish National Research Foundation; STFC grant; COST action CM1401 "Our Astrochemical History"; A-ERC [291141] FX We are grateful to the staff at the Nordic ALMA Regional Center (ARC) node at Onsala Space Observatory, in particular, Ivan Marti-Vidal and Sebastien Muller, for their support in setting up the program and for assistance with the data reduction. We also thank the anonymous referee for many comments that helped improve the presentation. Thanks also go to G. Fedoseev, K.-J. Chuang, and H. Linnartz for experimental information and discussions on the formation of glycolaldehyde and ethylene glycol in ices at low temperatures. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2012.1.00712.S and ADS/JAO.ALMA#2013.1.00278.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The group of J.K.J. acknowledges support from a Lundbeck Foundation Group Leader Fellowship as well as the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 646908) through ERC Consolidator Grant "S4F". Research at the Centre for Star and Planet Formation is funded by the Danish National Research Foundation. The work of AC was funded by a STFC grant. AC thanks the COST action CM1401 "Our Astrochemical History" for additional financial support. The group of EvD acknowledges A-ERC grant 291141 CHEMPLAN. NR 193 TC 3 Z9 3 U1 6 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A117 DI 10.1051/0004-6361/201628648 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500059 ER PT J AU Lallement, R Snowden, S Kuntz, KD Dame, TM Koutroumpa, D Grenier, I Casandjian, JM AF Lallement, R. Snowden, S. Kuntz, K. D. Dame, T. M. Koutroumpa, D. Grenier, I. Casandjian, J. M. TI On the distance to the North Polar Spur and the local CO-H-2 factor SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: ISM; radio lines: ISM; local insterstellar matter; ISM: bubbles; dust, extinction; Galaxy: center ID MILKY-WAY; GALACTIC-CENTER; FERMI BUBBLES; RADIO; MAPS; EXTINCTION; GALAXY; STARS; MODEL; WIND AB Aims. Most models identify the X-ray bright North Polar Spur (NPS) with a hot interstellar (IS) bubble in the Sco-Cen star-forming region at similar or equal to 130 pc. An opposite view considers the NPS as a distant structure associated with Galactic nuclear outflows. Constraints on the NPS distance can be obtained by comparing the foreground IS gas column inferred from X-ray absorption to the distribution of gas and dust along the line of sight. Absorbing columns toward shadowing molecular clouds simultaneously constrain the CO-H-2 conversion factor. Methods. We derived the columns of X-ray absorbing matter N-Habs from spectral fitting of dedicated XMM-Newton observations toward the NPS southern terminus (l(II) similar or equal to 29 degrees, b(II) similar or equal to + 5 to + 11 degrees). The distribution of the IS matter was obtained from absorption lines in new stellar spectra, 3D dust maps, and emission data, including high spatial resolution CO measurements recorded for this purpose. Results. N-Habs varies from similar or equal to 4.3 to similar or equal to 1.3 x 10(21) cm(-2) along the 19 fields. Relationships between X-ray brightness, absorbing column, and hardness ratio demonstrate a brightness increase with latitude that is governed by increasing absorption. The comparison with absorption data and local and large-scale dust maps rules out an NPS source near-side closer than 300 pc. The correlation between N-Habs and the reddening increases with the sightline length from 300 pc to 4 kpc and is the tightest with Planck tau(353GHz)-based reddening, suggesting a much larger distance. N(H)/E(B-V)(tau) similar or equal to 4.1 x 10(21) cm(-2) mag(-1), close to Fermi-Planck determinations. N-Habs absolute values are compatible with HI-CO clouds at -5 <= V-LSR <= +25 to +45 km s(-1) and an NPS potentially far beyond the Local Arm. A shadow cast by a b = +9 degrees molecular cloud constrains X-CO in that direction to <= 1.0 x 10(20) cm(-2) K-1 km(-1) s. The average X-CO over the fields is <= 0.75 x 10(20) cm(-2) K-1 km(-1) s. C1 [Lallement, R.] GEPI Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. [Snowden, S.] NASA GSFC, Greenbelt, MD 20771 USA. [Kuntz, K. D.] Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Dame, T. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Koutroumpa, D.] Univ Versailles St Quentin, LATMOS IPSL, INSU CNRS, 11 Bd DAlembert, F-78280 Guyancourt, France. [Grenier, I.] Univ Paris Diderot, AIM, F-91191 Gif Sur Yvette, France. [Casandjian, J. M.] CEA Saclay DSM Irfu SAp, F-91191 Gif Sur Yvette, France. RP Lallement, R (reprint author), GEPI Observ Paris, 5 Pl Jules Janssen, F-92195 Meudon, France. EM rosine.lallement@obspm.fr FU NASA [NNX15AG24G]; French National Research Agency (ANR) through the STILISM project; CNRS program (Programme National de Physique et Chimie du Milieu Interstellaire) FX K.K. acknowledges support from NASA grant NNX15AG24G. R.L. and I.G. acknowledge support from the French National Research Agency (ANR) through the STILISM project. R.L. acknowledges telescope time funding by the CNRS program (Programme National de Physique et Chimie du Milieu Interstellaire) and thanks the TBL-Narval team at Pic du Midi for their efficient support and excellent service observing. NR 54 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A131 DI 10.1051/0004-6361/201629453 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500133 ER PT J AU Prusti, T de Bruijne, JHJ Brown, AGA Vallenari, A Babusiaux, C Bailer-Jones, CAL Bastian, U Biermann, M Evans, DW Eyer, L Jansen, F Jordi, C Klioner, SA Lammers, U Lindegren, L Luri, X Mignard, F Milligan, DJ Panem, C Poinsignon, V Pourbaix, D Randich, S Sarri, G Sartoretti, P Siddiqui, HI Soubiran, C Valette, V van Leeuwen, F Walton, NA Aerts, C Arenou, F Cropper, M Drimmel, R Hog, E Katz, D Lattanzi, MG O'Mullane, W Grebel, EK Holland, AD Huc, C Passot, X Bramante, L Cacciari, C Castaneda, J Chaoul, L Cheek, N De Angeli, F Fabricius, C Guerra, R Hernandez, J Jean-Antoine-Piccolo, A Masana, E Messineo, R Mowlavi, N Nienartowicz, K Ordonez-Blanco, D Panuzzo, P Portell, J Richards, PJ Riello, M Seabroke, GM Tanga, P Thevenin, F Torra, J Els, SG Gracia-Abril, G Comoretto, G Garcia-Reinaldos, M Lock, T Mercier, E Altmann, M Andrae, R Astraatmadja, TL Bellas-Velidis, I Benson, K Berthier, J Blomme, R Busso, G Carry, B Cellino, A Clementini, G Cowell, S Creevey, O Cuypers, J Davidson, M De Ridder, J de Torres, A Delchambre, L Dell'Oro, A Ducourant, C Fremat, Y Garcia-Torres, M Gosset, E Halbwachs, JL Hambly, NC Harrison, DL Hauser, M Hestroffer, D Hodgkin, ST Huckle, HE Hutton, A Jasniewicz, G Jordan, S Kontizas, M Korn, AJ Lanzafame, AC Manteiga, M Moitinho, A Muinonen, K Osinde, J Pancino, E Pauwels, T Petit, JM Recio-Blanco, A Robin, AC Sarro, LM Siopis, C Smith, M Smith, KW Sozzetti, A Thuillot, W van Reeven, W Viala, Y Abbas, U Aramburu, AA Accart, S Aguado, JJ Allan, PM Allasia, W Altavilla, G Alvarez, MA Alves, J Anderson, RI Andrei, AH Varela, EA Antiche, E Antoja, T Anton, S Arcay, B Atzei, A Ayache, L Bach, N Baker, SG Balaguer-Nunez, L Barache, C Barata, C Barbier, A Barblan, F Baroni, M Navascues, DY Barros, M Barstow, MA Becciani, U Bellazzini, M Bellei, G Garcia, AB Belokurov, V Bendjoya, P Berihuete, A Bianchi, L Bienayme, O Billebaud, F Blagorodnova, N Blanco-Cuaresma, S Boch, T Bombrun, A Borrachero, R Bouquillon, S Bourda, G Bouy, H Bragaglia, A Breddels, MA Brouillet, N Brusemeister, T Bucciarelli, B Budnik, F Burgess, P Burgon, R Burlacu, A Busonero, D Buzzi, R Au, ECF Cambras, J Campbell, H Cancelliere, R Cantat-Gaudin, T Carlucci, T Carrasco, JM Castellani, M Charlot, P Charnas, J Charvet, P Chassat, F Chiavassa, A Clotet, M Cocozza, G Collins, RS Collins, P Costigan, G Crifo, F Cross, NJG Crosta, M Crowley, C Dafonte, C Damerdji, Y Dapergolas, A David, P David, M De Cat, P de Felice, F de Laverny, P De Luise, F De March, R de Martino, D de Souza, R Debosscher, J del Pozo, E Delbo, M Delgado, A Delgado, HE di Marco, F Di Matteo, P Diakite, S Distefano, E Dolding, C Dos Anjos, S Drazinos, P Duran, J Dzigan, Y Ecale, E Edvardsson, B Enke, H Erdmann, M Escolar, D Espina, M Evans, NW Bontemps, GE Fabre, C Fabrizio, M Faigler, S Falcao, AJ Casas, MF Faye, F Federici, L Fedorets, G Fernandez-Hernandez, J Fernique, P Fienga, A Figueras, F Filippi, F Findeisen, K Fonti, A Fouesneau, M Fraile, E Fraser, M Fuchs, J Furnell, R Gai, M Galleti, S Galluccio, L Garabato, D Garcia-Sedano, F Gare, P Garofalo, A Garralda, N Gavras, P Gerssen, J Geyer, R Gilmore, G Girona, S Giuffrida, G Gomes, M Gonzalez-Marcos, A Gonzalez-Nunez, J Gonzalez-Vidal, JJ Granvik, M Guerrier, A Guillout, P Guiraud, J Gurpide, A Gutierrez-Sanchez, R Guy, LP Haigron, R Hatzidimitriou, D Haywood, M Heiter, U Helmi, A Hobbs, D Hofmann, W Holl, B Holland, G Hunt, JAS Hypki, A Icardi, V Irwin, M de Fombelle, GJ Jofre, P Jonker, PG Jorissen, A Julbe, F Karampelas, A Kochoska, A Kohley, R Kolenberg, K Kontizas, E Koposov, SE Kordopatis, G Koubsky, P Kowalczyk, A Krone-Martins, A Kudryashova, M Kull, I Bachchan, RK Lacoste-Seris, F Lanza, AF Lavigne, JB Le Poncin-Lafitte, C Lebreton, Y Lebzelter, T Leccia, S Leclerc, N Lecoeur-Taibi, I Lemaitre, V Lenhardt, H Leroux, F Liao, S Licata, E Lindstrom, HEP Lister, TA Livanou, E Lobel, A Loffler, W Lopez, M Lopez-Lozano, A Lorenz, D Loureiro, T MacDonald, I Fernandes, TM Managau, S Mann, RG Mantelet, G Marchal, O Marchant, JM Marconi, M Marie, J Marinoni, S Marrese, PM Marschalko, G Marshall, DJ Martin-Fleitas, JM Martino, M Mary, N Matijevic, G Mazeh, T McMillan, PJ Messina, S Mestre, A Michalik, D Millar, NR Miranda, BMH Molina, D Molinaro, R Molinaro, M Molnar, L Moniez, M Montegriffo, P Monteiro, D Mor, R Mora, A Morbidelli, R Morel, T Morgenthaler, S Morley, T Morris, D Mulone, AF Muraveva, T Musella, I Narbonne, J Nelemans, G Nicastro, L Noval, L Ordenovic, C Ordieres-Mere, J Osborne, P Pagani, C Pagano, I Pailler, F Palacin, H Palaversa, L Parsons, P Paulsen, T Pecoraro, M Pedrosa, R Pentikainen, H Pereira, J Pichon, B Piersimoni, AM Pineau, FX Plachy, E Plum, G Poujoulet, E Prsa, A Pulone, L Ragaini, S Rago, S Rambaux, N Ramos-Lerate, M Ranalli, P Rauw, G Read, A Regibo, S Renk, F Reyle, C Ribeiro, RA Rimoldini, L Ripepi, V Riva, A Rixon, G Roelens, M Romero-Gomez, M Rowell, N Royer, F Rudolph, A Ruiz-Dern, L Sadowski, G Selles, TS Sahlmann, J Salgado, J Salguero, E Sarasso, M Savietto, H Schnorhk, A Schultheis, M Sciacca, E Segol, M Segovia, JC Segransan, D Serpell, E Shih, IC Smareglia, R Smart, RL Smith, C Solano, E Solitro, F Sordo, R Nieto, SS Souchay, J Spagna, A Spoto, F Stampa, U Steele, IA Steidelmuller, H Stephenson, CA Stoev, H Suess, FF Suveges, M Surdej, J Szabados, L Szegedi-Elek, E Tapiador, D Taris, F Tauran, G Taylor, MB Teixeira, R Terrett, D Tingley, B Trager, SC Turon, C Ulla, A Utrilla, E Valentini, G van Elteren, A Van Hemelryck, E van Leeuwen, M Varadi, M Vecchiato, A Veljanoski, J Via, T Vicente, D Vogt, S Voss, H Votruba, V Voutsinas, S Walmsley, G Weiler, M Weingrill, K Werner, D Wevers, T Whitehead, G Wyrzykowski, L Yoldas, A Zerjal, M Zucker, S Zurbach, C Zwitter, T Alecu, A Allen, M Prieto, CA Amorim, A Anglada-Escude, G Arsenijevic, V Azaz, S Balm, P Beck, M Bernstein, HH Bigot, L Bijaoui, A Blasco, C Bonfigli, M Bono, G Boudreault, S Bressan, A Brown, S Brunet, PM Bunclark, P Buonanno, R Butkevich, AG Carret, C Carrion, C Chemin, L Chereau, F Corcione, L Darmigny, E de Boer, KS de Teodoro, P de Zeeuw, PT Delle Luche, C Domingues, CD Dubath, P Fodor, F Frezouls, B Fries, A Fustes, D Fyfe, D Gallardo, E Gallegos, J Gardiol, D Gebran, M Gomboc, A Gomez, A Grux, E Gueguen, A Heyrovsky, A Hoar, J Iannicola, G Parache, YI Janotto, AM Joliet, E Jonckheere, A Keil, R Kim, DW Klagyivik, P Klar, J Knude, J Kochukhov, O Kolka, I Kos, J Kutka, A Lainey, V LeBouquin, D Liu, C Loreggia, D Makarov, VV Marseille, MG Martayan, C Martinez-Rubi, O Massart, B Meynadier, F Mignot, S Munari, U Nguyen, AT Nordlander, T Ocvirk, P O'Flaherty, KS Sanz, AO Ortiz, P Osorio, J Oszkiewicz, D Ouzounis, A Palmer, M Park, P Pasquato, E Peltzer, C Peralta, J Peturaud, F Pieniluoma, T Pigozzi, E Poels, J Prat, G Prod'homme, T Raison, F Rebordao, JM Risquez, D Rocca-Volmerange, B Rosen, S Ruiz-Fuertes, MI Russo, F Sembay, S Vizcaino, IS Short, A Siebert, A Silva, H Sinachopoulos, D Slezak, E El, MSF Sosnowska, D Straizys, V ter Linden, M Terrell, D Theil, S Tiede, C Troisi, L Tsalmantza, P Tur, D Vaccari, M Vachier, F Valles, P Van Hamme, W Veltz, L Virtanen, J Wallut, JM Wichmann, R Wilkinson, MI Ziaeepour, H Zschocke, S AF Prusti, T. de Bruijne, J. H. J. Brown, A. G. A. Vallenari, A. Babusiaux, C. Bailer-Jones, C. A. L. Bastian, U. Biermann, M. Evans, D. W. Eyer, L. Jansen, F. Jordi, C. Klioner, S. A. Lammers, U. Lindegren, L. Luri, X. Mignard, F. Milligan, D. J. Panem, C. Poinsignon, V. Pourbaix, D. Randich, S. Sarri, G. Sartoretti, P. Siddiqui, H. I. Soubiran, C. Valette, V. van Leeuwen, F. Walton, N. A. Aerts, C. Arenou, F. Cropper, M. Drimmel, R. Hog, E. Katz, D. Lattanzi, M. G. O'Mullane, W. Grebel, E. K. Holland, A. D. Huc, C. Passot, X. Bramante, L. Cacciari, C. Castaneda, J. Chaoul, L. Cheek, N. De Angeli, F. Fabricius, C. Guerra, R. Hernandez, J. Jean-Antoine-Piccolo, A. Masana, E. Messineo, R. Mowlavi, N. Nienartowicz, K. Ordonez-Blanco, D. Panuzzo, P. Portell, J. Richards, P. J. Riello, M. Seabroke, G. M. Tanga, P. Thevenin, F. Torra, J. Els, S. G. Gracia-Abril, G. Comoretto, G. Garcia-Reinaldos, M. Lock, T. Mercier, E. Altmann, M. Andrae, R. Astraatmadja, T. L. Bellas-Velidis, I. Benson, K. Berthier, J. Blomme, R. Busso, G. Carry, B. Cellino, A. Clementini, G. Cowell, S. Creevey, O. Cuypers, J. Davidson, M. De Ridder, J. de Torres, A. Delchambre, L. Dell'Oro, A. Ducourant, C. Fremat, Y. Garcia-Torres, M. Gosset, E. Halbwachs, J. -L. Hambly, N. C. Harrison, D. L. Hauser, M. Hestroffer, D. Hodgkin, S. T. Huckle, H. E. Hutton, A. Jasniewicz, G. Jordan, S. Kontizas, M. Korn, A. J. Lanzafame, A. C. Manteiga, M. Moitinho, A. Muinonen, K. Osinde, J. Pancino, E. Pauwels, T. Petit, J. -M. Recio-Blanco, A. Robin, A. C. Sarro, L. M. Siopis, C. Smith, M. Smith, K. W. Sozzetti, A. Thuillot, W. van Reeven, W. Viala, Y. Abbas, U. Aramburu, A. Abreu Accart, S. Aguado, J. J. Allan, P. M. Allasia, W. Altavilla, G. Alvarez, M. A. Alves, J. Anderson, R. I. Andrei, A. H. Varela, E. Anglada Antiche, E. Antoja, T. Anton, S. Arcay, B. Atzei, A. Ayache, L. Bach, N. Baker, S. G. Balaguer-Nunez, L. Barache, C. Barata, C. Barbier, A. Barblan, F. Baroni, M. Barrado y Navascues, D. Barros, M. Barstow, M. A. Becciani, U. Bellazzini, M. Bellei, G. Garcia, A. Bello Belokurov, V. Bendjoya, P. Berihuete, A. Bianchi, L. Bienayme, O. Billebaud, F. Blagorodnova, N. Blanco-Cuaresma, S. Boch, T. Bombrun, A. Borrachero, R. Bouquillon, S. Bourda, G. Bouy, H. Bragaglia, A. Breddels, M. A. Brouillet, N. Bruesemeister, T. Bucciarelli, B. Budnik, F. Burgess, P. Burgon, R. Burlacu, A. Busonero, D. Buzzi, R. Au, E. Ca Ff Cambras, J. Campbell, H. Cancelliere, R. Cantat-Gaudin, T. Carlucci, T. Carrasco, J. M. Castellani, M. Charlot, P. Charnas, J. Charvet, P. Chassat, F. Chiavassa, A. Clotet, M. Cocozza, G. Collins, R. S. Collins, P. Costigan, G. Crifo, F. Cross, N. J. G. Crosta, M. Crowley, C. Dafonte, C. Damerdji, Y. Dapergolas, A. David, P. David, M. De Cat, P. de Felice, F. de Laverny, P. De Luise, F. De March, R. de Martino, D. de Souza, R. Debosscher, J. del Pozo, E. Delbo, M. Delgado, A. Delgado, H. E. di Marco, F. Di Matteo, P. Diakite, S. Distefano, E. Dolding, C. Dos Anjos, S. Drazinos, P. Duran, J. Dzigan, Y. Ecale, E. Edvardsson, B. Enke, H. Erdmann, M. Escolar, D. Espina, M. Evans, N. W. Bontemps, G. Eynard Fabre, C. Fabrizio, M. Faigler, S. Falcao, A. J. Farras Casas, M. Faye, F. Federici, L. Fedorets, G. Fernandez-Hernandez, J. Fernique, P. Fienga, A. Figueras, F. Filippi, F. Findeisen, K. Fonti, A. Fouesneau, M. Fraile, E. Fraser, M. Fuchs, J. Furnell, R. Gai, M. Galleti, S. Galluccio, L. Garabato, D. Garcia-Sedano, F. Gare, P. Garofalo, A. Garralda, N. Gavras, P. Gerssen, J. Geyer, R. Gilmore, G. Girona, S. Giuffrida, G. Gomes, M. Gonzalez-Marcos, A. Gonzalez-Nunez, J. Gonzalez-Vidal, J. J. Granvik, M. Guerrier, A. Guillout, P. Guiraud, J. Gurpide, A. Gutierrez-Sanchez, R. Guy, L. P. Haigron, R. Hatzidimitriou, D. Haywood, M. Heiter, U. Helmi, A. Hobbs, D. Hofmann, W. Holl, B. Holland, G. Hunt, J. A. S. Hypki, A. Icardi, V. Irwin, M. de Fombelle, G. Jevardat Jofre, P. Jonker, P. G. Jorissen, A. Julbe, F. Karampelas, A. Kochoska, A. Kohley, R. Kolenberg, K. Kontizas, E. Koposov, S. E. Kordopatis, G. Koubsky, P. Kowalczyk, A. Krone-Martins, A. Kudryashova, M. Kull, I. Bachchan, R. K. Lacoste-Seris, F. Lanza, A. F. Lavigne, J. -B. Le Poncin-Lafitte, C. Lebreton, Y. Lebzelter, T. Leccia, S. Leclerc, N. Lecoeur-Taibi, I. Lemaitre, V. Lenhardt, H. Leroux, F. Liao, S. Licata, E. Lindstrom, H. E. P. Lister, T. A. Livanou, E. Lobel, A. Loeffler, W. Lopez, M. Lopez-Lozano, A. Lorenz, D. Loureiro, T. MacDonald, I. Magalhaes Fernandes, T. Managau, S. Mann, R. G. Mantelet, G. Marchal, O. Marchant, J. M. Marconi, M. Marie, J. Marinoni, S. Marrese, P. M. Marschalko, G. Marshall, D. J. Martin-Fleitas, J. M. Martino, M. Mary, N. Matijevic, G. Mazeh, T. McMillan, P. J. Messina, S. Mestre, A. Michalik, D. Millar, N. R. Miranda, B. M. H. Molina, D. Molinaro, R. Molinaro, M. Molnar, L. Moniez, M. Montegriffo, P. Monteiro, D. Mor, R. Mora, A. Morbidelli, R. Morel, T. Morgenthaler, S. Morley, T. Morris, D. Mulone, A. F. Muraveva, T. Musella, I. Narbonne, J. Nelemans, G. Nicastro, L. Noval, L. Ordenovic, C. Ordieres-Mere, J. Osborne, P. Pagani, C. Pagano, I. Pailler, F. Palacin, H. Palaversa, L. Parsons, P. Paulsen, T. Pecoraro, M. Pedrosa, R. Pentikainen, H. Pereira, J. Pichon, B. Piersimoni, A. M. Pineau, F. -X. Plachy, E. Plum, G. Poujoulet, E. Prsa, A. Pulone, L. Ragaini, S. Rago, S. Rambaux, N. Ramos-Lerate, M. Ranalli, P. Rauw, G. Read, A. Regibo, S. Renk, F. Reyle, C. Ribeiro, R. A. Rimoldini, L. Ripepi, V. Riva, A. Rixon, G. Roelens, M. Romero-Gomez, M. Rowell, N. Royer, F. Rudolph, A. Ruiz-Dern, L. Sadowski, G. Selles, T. Sagrista Sahlmann, J. Salgado, J. Salguero, E. Sarasso, M. Savietto, H. Schnorhk, A. Schultheis, M. Sciacca, E. Segol, M. Segovia, J. C. Segransan, D. Serpell, E. Shih, I-C. Smareglia, R. Smart, R. L. Smith, C. Solano, E. Solitro, F. Sordo, R. Nieto, S. Soria Souchay, J. Spagna, A. Spoto, F. Stampa, U. Steele, I. A. Steidelmueller, H. Stephenson, C. A. Stoev, H. Suess, F. F. Suveges, M. Surdej, J. Szabados, L. Szegedi-Elek, E. Tapiador, D. Taris, F. Tauran, G. Taylor, M. B. Teixeira, R. Terrett, D. Tingley, B. Trager, S. C. Turon, C. Ulla, A. Utrilla, E. Valentini, G. van Elteren, A. Van Hemelryck, E. van Leeuwen, M. Varadi, M. Vecchiato, A. Veljanoski, J. Via, T. Vicente, D. Vogt, S. Voss, H. Votruba, V. Voutsinas, S. Walmsley, G. Weiler, M. Weingrill, K. Werner, D. Wevers, T. Whitehead, G. Wyrzykowski, L. Yoldas, A. Zerjal, M. Zucker, S. Zurbach, C. Zwitter, T. Alecu, A. Allen, M. Allende Prieto, C. Amorim, A. Anglada-Escude, G. Arsenijevic, V. Azaz, S. Balm, P. Beck, M. Bernstein, H. -H. Bigot, L. Bijaoui, A. Blasco, C. Bonfigli, M. Bono, G. Boudreault, S. Bressan, A. Brown, S. Brunet, P. -M. Bunclark, P. Buonanno, R. Butkevich, A. G. Carret, C. Carrion, C. Chemin, L. Chereau, F. Corcione, L. Darmigny, E. de Boer, K. S. de Teodoro, P. de Zeeuw, P. T. Delle Luche, C. Domingues, C. D. Dubath, P. Fodor, F. Frezouls, B. Fries, A. Fustes, D. Fyfe, D. Gallardo, E. Gallegos, J. Gardiol, D. Gebran, M. Gomboc, A. Gomez, A. Grux, E. Gueguen, A. Heyrovsky, A. Hoar, J. Iannicola, G. Parache, Y. Isasi Janotto, A. -M. Joliet, E. Jonckheere, A. Keil, R. Kim, D. -W. Klagyivik, P. Klar, J. Knude, J. Kochukhov, O. Kolka, I. Kos, J. Kutka, A. Lainey, V. LeBouquin, D. Liu, C. Loreggia, D. Makarov, V. V. Marseille, M. G. Martayan, C. Martinez-Rubi, O. Massart, B. Meynadier, F. Mignot, S. Munari, U. Nguyen, A. -T. Nordlander, T. Ocvirk, P. O'Flaherty, K. S. Sanz, A. Olias Ortiz, P. Osorio, J. Oszkiewicz, D. Ouzounis, A. Palmer, M. Park, P. Pasquato, E. Peltzer, C. Peralta, J. Peturaud, F. Pieniluoma, T. Pigozzi, E. Poels, J. Prat, G. Prod'homme, T. Raison, F. Rebordao, J. M. Risquez, D. Rocca-Volmerange, B. Rosen, S. Ruiz-Fuertes, M. I. Russo, F. Sembay, S. Vizcaino, I. Serraller Short, A. Siebert, A. Silva, H. Sinachopoulos, D. Slezak, E. El, M. So Ff Sosnowska, D. Straizys, V. ter Linden, M. Terrell, D. Theil, S. Tiede, C. Troisi, L. Tsalmantza, P. Tur, D. Vaccari, M. Vachier, F. Valles, P. Van Hamme, W. Veltz, L. Virtanen, J. Wallut, J. -M. Wichmann, R. Wilkinson, M. I. Ziaeepour, H. Zschocke, S. CA Gaia Collaboration TI The Gaia mission SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE space vehicles: instruments; Galaxy: structure; astrometry; parallaxes; proper motions; telescopes ID FGK BENCHMARK STARS; GENERAL-RELATIVISTIC MODEL; COVARIANCE EXPANSION MODEL; CCD RADIATION-DAMAGE; CA-II TRIPLET; ASTROMETRIC SOLUTION; STANDARD STARS; SOLAR-SYSTEM; ERROR CHARACTERIZATION; GRAVITATIONAL-FIELD AB Gaia is a cornerstone mission in the science programme of the European Space Agency (ESA). The spacecraft construction was approved in 2006, following a study in which the original interferometric concept was changed to a direct-imaging approach. Both the spacecraft and the payload were built by European industry. The involvement of the scientific community focusses on data processing for which the international Gaia Data Processing and Analysis Consortium (DPAC) was selected in 2007. Gaia was launched on 19 December 2013 and arrived at its operating point, the second Lagrange point of the Sun-Earth-Moon system, a few weeks later. The commissioning of the spacecraft and payload was completed on 19 July 2014. The nominal five-year mission started with four weeks of special, ecliptic-pole scanning and subsequently transferred into full-sky scanning mode. We recall the scientific goals of Gaia and give a description of the as-built spacecraft that is currently (mid-2016) being operated to achieve these goals. We pay special attention to the payload module, the performance of which is closely related to the scientific performance of the mission. We provide a summary of the commissioning activities and findings, followed by a description of the routine operational mode. We summarise scientific performance estimates on the basis of in-orbit operations. Several intermediate Gaia data releases are planned and the data can be retrieved from the Gaia Archive, which is available through the Gaia home page. C1 [Prusti, T.; de Bruijne, J. H. J.; Antoja, T.; Allen, M.; Azaz, S.; Short, A.] European Space Res & Technol Ctr ESA ESTEC, Sci Support Off, Directorate Sci, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Brown, A. G. A.; Costigan, G.; Hypki, A.; van Elteren, A.; de Zeeuw, P. T.; Prod'homme, T.; Risquez, D.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Vallenari, A.; Cantat-Gaudin, T.; Sordo, R.; Munari, U.] Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Babusiaux, C.; Sartoretti, P.; Arenou, F.; Katz, D.; Panuzzo, P.; Viala, Y.; Crifo, F.; Di Matteo, P.; Findeisen, K.; Gavras, P.; Haigron, R.; Haywood, M.; Lebreton, Y.; Leclerc, N.; Marchal, O.; Plum, G.; Royer, F.; Ruiz-Dern, L.; Shih, I-C.; Turon, C.; Chereau, F.; Delle Luche, C.; Gomez, A.; Gueguen, A.; Meynadier, F.; Mignot, S.; Peturaud, F.] Univ Paris Diderot, PSL Res Univ, Observ Paris, GEPI,CNRS,Sorbonne Paris Cite, 5 Pl Jules Janssen, F-92190 Meudon, France. [Bailer-Jones, C. A. L.; Andrae, R.; Astraatmadja, T. L.; Smith, K. W.; Fouesneau, M.; Kim, D. -W.; Liu, C.; Tiede, C.; Tsalmantza, P.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Bastian, U.; Biermann, M.; Grebel, E. K.; Els, S. G.; Mercier, E.; Altmann, M.; Hauser, M.; Jordan, S.; Bruesemeister, T.; Hofmann, W.; Lenhardt, H.; Mantelet, G.; Selles, T. Sagrista; Stampa, U.] Heidelberg Univ, Astron Rech Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Evans, D. W.; van Leeuwen, F.; Walton, N. A.; De Angeli, F.; Riello, M.; Busso, G.; Cellino, A.; Cowell, S.; Harrison, D. L.; Hodgkin, S. T.; Atzei, A.; Barbier, A.; Belokurov, V.; Berihuete, A.; Blagorodnova, N.; Bombrun, A.; Bragaglia, A.; Burgess, P.; Burlacu, A.; Campbell, H.; Chiavassa, A.; Dapergolas, A.; Delgado, A.; Evans, N. W.; Fraser, M.; Gilmore, G.; Holland, G.; Irwin, M.; Jofre, P.; Koposov, S. E.; Millar, N. R.; Osborne, P.; Rixon, G.; Suess, F. F.; van Leeuwen, M.; Wyrzykowski, L.; Yoldas, A.; Alecu, A.; Amorim, A.; Bijaoui, A.; Bressan, A.; Brown, S.; Peltzer, C.; Wilkinson, M. I.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Mowlavi, N.; Anderson, R. I.; Barblan, F.; Blanco-Cuaresma, S.; Holl, B.; Palaversa, L.; Roelens, M.; Segransan, D.; Varadi, M.; Park, P.; Sosnowska, D.] Univ Geneva, Dept Astron, Chemin Maillettes 51, CH-1290 Versoix, Switzerland. [Jansen, F.] European Space Res & Technol Ctr ESA ESTEC, Mission Operat Div, Operat Dept, Directorate Sci, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Jordi, C.; Luri, X.; Castaneda, J.; Fabricius, C.; Masana, E.; Portell, J.; Torra, J.; Gracia-Abril, G.; Antiche, E.; Balaguer-Nunez, L.; Borrachero, R.; Carrasco, J. M.; Clotet, M.; Farras Casas, M.; Figueras, F.; Garralda, N.; Gonzalez-Vidal, J. J.; Gurpide, A.; Julbe, F.; Molina, D.; Mor, R.; Romero-Gomez, M.; Nieto, S. Soria; Voss, H.; Anglada-Escude, G.; Fries, A.; Gallardo, E.; Gebran, M.; Parache, Y. Isasi; Martinez-Rubi, O.; Palmer, M.; Valles, P.] Univ Barcelona, IEEC UB, Inst Ciencies Cosmos, Marti Franques 1, E-08028 Barcelona, Spain. [Klioner, S. A.; Geyer, R.; Steidelmueller, H.; Butkevich, A. G.; Zschocke, S.] Tech Univ Dresden, Lohrmann Observ, Mommsenstr 13, D-01062 Dresden, Germany. [Lammers, U.; O'Mullane, W.; Guerra, R.; Hernandez, J.; Garcia-Reinaldos, M.; Lock, T.; Kohley, R.; Sahlmann, J.; Hoar, J.] European Space Astron Ctr ESA ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Lindegren, L.; Hobbs, D.; Bachchan, R. K.; McMillan, P. J.; Ranalli, P.] Lund Univ, Lund Observ, Dept Astron & Theoret Phys, Box 43, S-22100 Lund, Sweden. [Tanga, P.; Thevenin, F.; Carry, B.; Creevey, O.; Recio-Blanco, A.; Bendjoya, P.; Chiavassa, A.; de Laverny, P.; Delbo, M.; Galluccio, L.; Kordopatis, G.; Ordenovic, C.; Pichon, B.; Schultheis, M.; Spoto, F.; Bijaoui, A.; Massart, B.; Slezak, E.] Univ Nice Sophia Antipolis, Observ Cote Azur, Lab Lagrange, CNRS, CS 34229, F-06304 Nice, France. [Milligan, D. J.; Budnik, F.; Collins, P.; Espina, M.; Kowalczyk, A.; Loureiro, T.; Renk, F.; Rudolph, A.; Werner, D.; Whitehead, G.] European Space Operat Ctr ESA ESOC, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Panem, C.; Valette, V.; Huc, C.; Passot, X.; Chaoul, L.; Jean-Antoine-Piccolo, A.; Burlacu, A.; Guiraud, J.; Pailler, F.; Walmsley, G.; Brunet, P. -M.; Darmigny, E.; Fodor, F.; Frezouls, B.; Janotto, A. -M.; Nguyen, A. -T.; Wallut, J. -M.] CNES Ctr Spatial Toulouse, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Poinsignon, V.; Charvet, P.; Chassat, F.; Ecale, E.; Faye, F.; Massart, B.] Airbus Def & Space SAS, 31 Rue Cosmonautes, F-31402 Toulouse 4, France. [Pourbaix, D.; Siopis, C.; Jorissen, A.; Sadowski, G.; Pasquato, E.] Univ Libre Bruxelles, Inst Astron & Astrophys, CP 226,Blvd Triomphe, B-1050 Brussels, Belgium. [Pourbaix, D.; Gosset, E.] FRS FNRS, Rue Egmont 5, B-1000 Brussels, Belgium. [Randich, S.; Dell'Oro, A.; Pancino, E.] Osserv Astrofis Arcetri, INAF, Largo Enrico Fermi 5, I-50125 Florence, Italy. [Sarri, G.; Atzei, A.; Baroni, M.; Erdmann, M.; Escolar, D.; Furnell, R.; Gare, P.; Monteiro, D.; Paulsen, T.; Pereira, J.; Schnorhk, A.; Prod'homme, T.] European Space Res & Technol Ctr ESA ESTEC, Directorate Sci, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Siddiqui, H. I.; Comoretto, G.; Gutierrez-Sanchez, R.; Parsons, P.; Stephenson, C. A.; Balm, P.] Telespazio Vega UK Ltd, ESA ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Aerts, C.; De Ridder, J.; Debosscher, J.; Kolenberg, K.; Nelemans, G.; Regibo, S.] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18N,Allee Geoffroy St Hilaire, F-33615 Pessac, France. [Aerts, C.; De Ridder, J.; Debosscher, J.; Kolenberg, K.; Nelemans, G.; Regibo, S.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. [Aerts, C.; Jonker, P. G.; Nelemans, G.; Wevers, T.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. [Cropper, M.; Seabroke, G. M.; Benson, K.; Huckle, H. E.; Smith, M.; Baker, S. G.; Dolding, C.; Hunt, J. A. S.; Allende Prieto, C.; Boudreault, S.; Rosen, S.] Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. [Drimmel, R.; Lattanzi, M. G.; Cellino, A.; Sozzetti, A.; Abbas, U.; Bucciarelli, B.; Busonero, D.; Buzzi, R.; Crosta, M.; Gai, M.; Liao, S.; Morbidelli, R.; Rago, S.; Riva, A.; Sarasso, M.; Smart, R. L.; Spagna, A.; Vecchiato, A.; Corcione, L.; Gardiol, D.; Loreggia, D.; Russo, F.] Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, TO, Italy. [Hog, E.; Lindstrom, H. E. P.; Knude, J.] Univ Copenhagen, Niels Bohr Inst, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Holland, A. D.; Burgon, R.] Open Univ, Dept Phys Sci, Ctr Elect Imaging, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. [Bramante, L.; Messineo, R.; De March, R.; Filippi, F.; Fonti, A.; Icardi, V.; Martino, M.; Mulone, A. F.; Solitro, F.; Pigozzi, E.] ALTEC Spa, Corso Marche 79, I-10146 Turin, Italy. [Cacciari, C.; Clementini, G.; Altavilla, G.; Bellazzini, M.; Bragaglia, A.; Cocozza, G.; Federici, L.; Galleti, S.; Garofalo, A.; Monteiro, D.; Muraveva, T.; Ragaini, S.] Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. [Cheek, N.; Varela, E. Anglada; Fernandez-Hernandez, J.; Gonzalez-Nunez, J.; Segovia, J. C.; de Teodoro, P.; Gallegos, J.] Serco Gestion Negocios ESA ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Nienartowicz, K.; Ordonez-Blanco, D.; Charnas, J.; Guy, L. P.; de Fombelle, G. Jevardat; Lecoeur-Taibi, I.; Rimoldini, L.; Suveges, M.; Beck, M.; Dubath, P.; Ruiz-Fuertes, M. I.] Univ Geneva, Dept Astron, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. [Richards, P. J.; Allan, P. M.; Terrett, D.] Rutherford Appleton Lab, STFC, Didcot OX11 0QX, Oxon, England. [Els, S. G.; Gracia-Abril, G.; Mercier, E.] ESAC, Gaia DPAC Project Off, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Altmann, M.; Andrei, A. H.; Barache, C.; Bouquillon, S.; Carlucci, T.; Le Poncin-Lafitte, C.; Souchay, J.; Taris, F.; Meynadier, F.] UPMC Univ Paris 06, PSL Res Univ, Sorbonne Univ, SYRTE,Observ Paris,CNRS,LNE, 61 Ave Observ, F-75014 Paris, France. [Bellas-Velidis, I.; Dapergolas, A.; Gavras, P.; Karampelas, A.; Kontizas, E.; Sinachopoulos, D.] Natl Observ Athens, Athens 15236, Greece. [Berthier, J.; Carry, B.; Thuillot, W.; David, P.; Kudryashova, M.; Rambaux, N.; Lainey, V.; Vachier, F.] Univ Lille, UPMC Univ Paris 06, PSL Res Univ, IMCCE,Observ Paris,CNRS,Sorbonne Univ, 77 Av Denfert Rochereau, F-75014 Paris, France. [Blomme, R.; Cuypers, J.; Fremat, Y.; Pauwels, T.; De Cat, P.; Lobel, A.; Van Hemelryck, E.; Jonckheere, A.; Martayan, C.] Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium. [Creevey, O.; Veltz, L.] Univ Paris 11, Inst Astrophys Spatiale, UMR 8617, CNRS, Batiment 121, F-91405 Orsay, France. [Davidson, M.; Hambly, N. C.; Collins, R. S.; Cross, N. J. G.; MacDonald, I.; Mann, R. G.; Morris, D.; Rowell, N.; Voutsinas, S.; Heyrovsky, A.; Ouzounis, A.] Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [de Torres, A.; Bombrun, A.; Crowley, C.; Joliet, E.; ter Linden, M.] HE Space Operat BV ESA ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Delchambre, L.; Gosset, E.; Damerdji, Y.; Morel, T.; Rauw, G.; Surdej, J.] Univ Liege, Inst Astrophys & Geophys, 19c,Allee 6 Aout, B-4000 Liege, Belgium. [Garcia-Torres, M.] Univ Pablo Olavide, Area Lenguajes & Sistemas Informat, Ctra Utrera,Km 1, Seville 41013, Spain. [Halbwachs, J. -L.; Bienayme, O.; Boch, T.; Fernique, P.; Guillout, P.; Pineau, F. -X.; Ocvirk, P.; Siebert, A.] Univ Strasbourg, Observ Astron Strasbourg, CNRS, UMR 7550, 11 Rue Univ, F-67000 Strasbourg, France. [Harrison, D. L.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Hutton, A.; van Reeven, W.; Bach, N.; del Pozo, E.; Martin-Fleitas, J. M.; Mora, A.; Utrilla, E.] Aurora Technol ESA ESAC, Camino Bajo Castillo S-N, Madrid 28692, Spain. [Jasniewicz, G.; Zurbach, C.] Univ Montpellier, Lab Univers & Particules Montpellier, Pl Eugene Bataillon,CC72, F-34095 Montpellier 05, France. [Kontizas, M.; Drazinos, P.; Gavras, P.; Hatzidimitriou, D.; Karampelas, A.; Livanou, E.] Univ Athens, Dept Astrophys Astron & Mech, Athens 15783, Greece. [Korn, A. J.; Edvardsson, B.; Heiter, U.; Kochukhov, O.; Nordlander, T.] Uppsala Univ, Dept Phys & Astron, Div Astron & Space Phys, Box 516, S-75120 Uppsala, Sweden. [Lanzafame, A. C.] Univ Catania, Dipartimento Fis & Astron, Sez Astrofis, Via S Sofia 78, I-95123 Catania, Italy. [Lanzafame, A. C.; Becciani, U.; Distefano, E.; Lanza, A. F.; Messina, S.; Pagano, I.; Sciacca, E.] Osserv Astrofis Catania, INAF, Via S Sofia 78, I-95123 Catania, Italy. [Manteiga, M.; Alvarez, M. A.; Arcay, B.; Dafonte, C.; Garabato, D.; Fustes, D.] Univ A Coruna, Fac Informat, Campus Elvina S-N, La Coruna 15071, Spain. [Moitinho, A.; Barata, C.; Barros, M.; Gomes, M.; Krone-Martins, A.; Miranda, B. M. H.; Amorim, A.; Arsenijevic, V.] Univ Lisbon, CENTRA, FCUL, Campo Grande,Edif C8, P-1749016 Lisbon, Portugal. [Muinonen, K.; Fedorets, G.; Granvik, M.; Pentikainen, H.; Oszkiewicz, D.; Pieniluoma, T.; Virtanen, J.] Univ Helsinki, Dept Phys, POB 64, Helsinki 00014, Finland. [Muinonen, K.; Virtanen, J.] Finnish Geospatial Res Inst FGI, Geodeetinrinne 2, Masala 02430, Finland. [Osinde, J.; Varela, E. Anglada; Duran, J.; Salgado, J.; Salguero, E.] ESA ESAC, Isdefe, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Pancino, E.; Fabrizio, M.; Giuffrida, G.; Marinoni, S.; Marrese, P. M.; Troisi, L.] ASI Sci Data Ctr, Via Politecn SNC, I-00133 Rome, Italy. [Petit, J. -M.; Robin, A. C.; Diakite, S.; Reyle, C.; Grux, E.; Ziaeepour, H.] Univ Bourgogne Franche Comte, OSU THETA Franche Comte Bourgogne, Inst UTINAM UMR6213, CNRS, F-25000 Besancon, France. [Sarro, L. M.; Aguado, J. J.; Delgado, H. E.; Garcia-Sedano, F.; Carrion, C.] UNED, Dpto Inteligencia Artificial, C Juan del Rosal 16, Madrid 28040, Spain. [Aramburu, A. Abreu] ESA ESAC, Elecnor Deimos Space, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Accart, S.; Barbier, A.; Bontemps, G. Eynard; Guerrier, A.; Lacoste-Seris, F.; Lavigne, J. -B.; Lemaitre, V.; Leroux, F.; Managau, S.; Mary, N.; Narbonne, J.; Noval, L.; Palacin, H.; Tauran, G.; Delle Luche, C.; LeBouquin, D.; Marseille, M. G.; Massart, B.] CNES Ctr Spatial Toulouse, Thales Serv, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Allasia, W.; Bianchi, L.; Licata, E.; Pecoraro, M.] EURIX Srl, Via Carcano 26, I-10153 Turin, Italy. [Alves, J.; Lebzelter, T.; Lorenz, D.] Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. [Anderson, R. I.] Johns Hopkins Univ, Dept Phys & Astron, 3400 N Charles St, Baltimore, MD 21218 USA. [Andrei, A. H.] ON MCTI BR, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, Brazil. [Andrei, A. H.] OV UFRJ BR, Ladeira Pedro Antonio 43, BR-20080090 Rio De Janeiro, Brazil. [Anton, S.; Osorio, J.] Univ Porto, Fac Ciencias, Dept Matemat Aplicada, Rua Campo Alegre 687, P-4169007 Oporto, Portugal. [Anton, S.] Univ Lisbon, Fac Ciencias, Inst Astrofis & Ciencias Espaco, Campo Grande, P-1749016 Lisbon, Portugal. [Ayache, L.] Vitrociset Belgium, ESA ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Barrado y Navascues, D.; Bouy, H.; Lopez, M.; Solano, E.] ESA ESAC, CSIC INTA, Ctr Astrobiol, Dept Astrofis, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Barstow, M. A.; Pagani, C.; Read, A.; Fyfe, D.; Ortiz, P.; Rosen, S.; Sembay, S.; Wilkinson, M. I.] Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. [Bellei, G.] ESA ESOC, Deimos Space SLU, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Garcia, A. Bello] Univ Oviedo, Campus Univ, Gijon 33203, Spain. [Berihuete, A.] Univ Cadiz, Avd Univ, Cadiz 11002, Spain. [Breddels, M. A.; Helmi, A.; Trager, S. C.; Veljanoski, J.] Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands. [Cambras, J.; Via, T.; Tur, D.] Univ Catalunya, Consorci Serv, C Gran Capita,2-4 3rd Floor, Barcelona 08034, Spain. [Cancelliere, R.] Univ Turin, Dept Comp Sci, Corso Svizzera 185, I-10149 Turin, Italy. [Castellani, M.; Marinoni, S.; Marrese, P. M.; Pulone, L.; Bono, G.; Buonanno, R.; Iannicola, G.] Osserv Astron Roma, INAF, Via Frascati 33, I-00078 Monte Porzio Catone, Italy. [Damerdji, Y.] CRAAG, Ctr Rech Astron Astrophys & Geophys, Route Observ BP 63, Algiers 16340, Algeria. [David, M.] Univ Antwerp, Onderzoeksgrp Toegepaste Wiskunde, Middelheimlaan 1, B-2020 Antwerp, Belgium. [de Felice, F.] Univ Padua, Dept Phys & Astron, Via Marzolo 8, I-35131 Padua, Italy. [De Luise, F.; Fabrizio, M.; Piersimoni, A. M.; Valentini, G.; Bonfigli, M.] Osservatorio Astron Teramo, INAF, Via Mentore Maggini, I-64100 Teramo, Italy. [de Martino, D.; Leccia, S.; Marconi, M.; Molinaro, R.; Musella, I.; Ripepi, V.] Osserv Astron Capodimonte, INAF, Via Moiariello 16, I-80131 Naples, Italy. [de Souza, R.; Dos Anjos, S.; Teixeira, R.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226,Cidade Univ, BR-05508900 Sao Paulo, Brazil. [di Marco, F.; Morley, T.; Serpell, E.] ESA ESOC, Telespazio Vega Deutschland GmbH, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Dzigan, Y.; Zucker, S.] Tel Aviv Univ, Dept Geosci, IL-6997801 Tel Aviv, Israel. [Dzigan, Y.] Univ Amsterdam, Astron Inst Anton Pannekoek, POB 94249, NL-1090 GE Amsterdam, Netherlands. [Enke, H.; Gerssen, J.; Kordopatis, G.; Matijevic, G.; Weingrill, K.; Klar, J.; Ocvirk, P.; Siebert, A.; Veltz, L.] Leibniz Inst Astrophys Potsdam AIP, An der Sternwarte 16, D-14482 Potsdam, Germany. [Fabre, C.] CNES Ctr Spatial Toulouse, ATOS, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Faigler, S.; Kull, I.; Mazeh, T.] Tel Aviv Univ, Sch Phys & Astron, IL-6997801 Tel Aviv, Israel. [Falcao, A. J.; Magalhaes Fernandes, T.; Ribeiro, R. A.; Silva, H.] UNINOVA CTS, Campus FCT UNL, P-2829516 Caparica, Portugal. [Fienga, A.] Univ Nice Sophia Antipolis, Lab Geoazur, CNRS, UMR 7329,Observ Cote Azur, 250 Eue A Einstein, F-06560 Valbonne, France. [Fraile, E.] RHEA, ESA ESAC, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Fuchs, J.; Koubsky, P.; Votruba, V.; Kutka, A.] Acad Sci Czech Republic, Astron Inst, Fricova 298, Ondrejov 25165, Czech Republic. [Girona, S.; Vicente, D.] Barcelona Supercomp Ctr, Centro Nacl Supercomp, C Jordi Girona 29,Ed Nexus 2, Barcelona 08034, Spain. [Gonzalez-Marcos, A.] Univ La Rioja, Dept Mech Engn, C San Jose de Calasanz 31, Logrono 26004, La Rioja, Spain. [Gonzalez-Nunez, J.] Univ Vigo, ETSE Telecomunicac, Campus Lagoas Marcosende, Vigo 36310, Galicia, Spain. [Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. [Kochoska, A.; Zerjal, M.; Zwitter, T.; Gomboc, A.; Kos, J.] Univ Ljubljana, Fac Math & Phys, Jadranska Ulica 19, Ljubljana 1000, Slovenia. [Kolenberg, K.] Univ Antwerp, Dept Phys, Groenenborgerlaan 171, B-2020 Antwerp, Belgium. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lebreton, Y.] Univ Rennes 1, Inst Phys Rennes, F-35042 Rennes, France. [Liao, S.] Chinese Acad Sci, Shanghai Astron Observ, 80 Nandan Rd, Shanghai 200030, Peoples R China. [Lindstrom, H. E. P.] CSC Danmark AS, Retortvej 8, DK-2500 Valby, Denmark. [Lister, T. A.] Global Telescope Network Inc, Las Cumbres Observ, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Lopez-Lozano, A.] ESA ESOC, CGI, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Marchant, J. M.; Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Marie, J.] LSE Space GmbH, ESA ESOC, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Marschalko, G.; Molnar, L.; Plachy, E.; Szabados, L.; Szegedi-Elek, E.; Varadi, M.; Klagyivik, P.] Hungarian Acad Sci, Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. [Marschalko, G.] Univ Szeged, Baja Observ, Szegedi Ut 3-70, H-6500 Baja, Hungary. [Marshall, D. J.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU,Serv Astrophys,CEA Saclay, Bat 709, F-91191 Gif Sur Yvette, France. [Mestre, A.] ESA ESOC, GMV, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Molinaro, M.; Smareglia, R.] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34143 Trieste, Italy. [Moniez, M.] Univ Paris Saclay, CNRS IN2P3, Univ Paris Sud, Lab Accelerateur Lineaire, F-91898 Orsay, France. [Morgenthaler, S.] Ecole Polytech Fed Lausanne, SB MATHAA STAP, MA B1 473,Batiment MA,Stn 8, CH-1015 Lausanne, Switzerland. [Nicastro, L.] INAF IASF Bologna, Via P Gobetti 101, I-40129 Bologna, Italy. [Ordieres-Mere, J.] Tech Univ Madrid, Jose Gutierrez Abascal 2, Madrid 28006, Spain. [Pedrosa, R.; Carret, C.] CNES Ctr Spatial Toulouse, EQUERT Int, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Poujoulet, E.] CNES Ctr Spatial Toulouse, AKKA, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Prsa, A.] Villanova Univ, Dept Astrophys & Planetary Sci, 800 Lancaster Ave, Villanova, PA 19085 USA. [Ramos-Lerate, M.] ESA ESAC, Vitrociset Belgium, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Savietto, H.] Fork Res, Rua Cruzado Osberno,Lt 1,9 Esq, Lisbon, Portugal. [Segol, M.] APAVE SUDEUROPE SAS, CNES Ctr Spatial Toulouse, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Smith, C.] Serco Serv GmbH, ESA ESOC, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Solano, E.] Spanish Virtual Observ, Madrid, Spain. [Stoev, H.] Fdn Galileo Galilei, INAF, Rambla Jose Ana Fernandez Perez 7, Brena Baja 38712, Santa Cruz De T, Spain. [Tapiador, D.] ESA ESAC, INSA, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Tapiador, D.] Univ Complutense Madrid, Dept Arquitectura Comp & Automat, Fac Informat, C Prof Jose Garcia Santesmases S-N, E-28040 Madrid, Spain. [Taylor, M. B.] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Tingley, B.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, 120 Ny Munkegade,Bldg 1520, DK-8000 Aarhus C, Denmark. [Ulla, A.] Univ Vigo, Dept Appl Phys, Vigo 36310, Spain. [Vogt, S.] ESA ESTEC, HE Space Operat BV, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Wyrzykowski, L.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Allende Prieto, C.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Allende Prieto, C.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Blasco, C.] ESA ESTEC, RHEA, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Boudreault, S.] Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany. [Bressan, A.] SISSA, Via Bonomea 265, I-34136 Trieste, Italy. [Chemin, L.] Minist Ciencia Tecnol, Inst Nacl Pesquisas Espaciais, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP, Brazil. [de Boer, K. S.] Univ Bonn, Argelander Inst Astron, Hugel 171, D-53121 Bonn, Germany. [de Zeeuw, P. T.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Domingues, C. D.; Rebordao, J. M.] Univ Lisbon, Fac Sci, Lab Opt Lasers & Syst, Campus Lumiar,Estr Paco Lumiar 22, P-1649038 Lisbon, Portugal. [Gebran, M.] Notre Dame Univ, Dept Phys & Astron, POB 72, Louaize, Zouk Mikael, Lebanon. [Gomboc, A.] Univ Nova Gorica, Vipavska 13, Nova Gorica 5000, Slovenia. [Gueguen, A.; Raison, F.] Max Planck Inst Extraterr Phys, OPINAS, Giessenbachstr, D-85741 Garching, Germany. [Joliet, E.] CALTECH, NASA IPAC Infrared Sci Arch, Mail Code 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA. [Keil, R.] Univ Bremen, Ctr Appl Space Technol & Micrograv ZARM, Fallturm 1, D-28359 Bremen, Germany. [Keil, R.] ESA ESOC, RHEA Syst, Robert Bosch Str 5, D-64293 Darmstadt, Germany. [Kolka, I.] Tartu Observ, EE-61602 Toravere, Estonia. [Kos, J.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Kutka, A.] Slovak Org Space Act, Zamocka 18, Bratislava 85101, Slovakia. [Liu, C.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Makarov, V. V.] US Naval Observ, Astrometry Dept, 3450 Massachusetts Ave NW, Washington, DC 20392 USA. [Martayan, C.] European Southern Observ, Alonso de Cordova 3107, Casilla 19001, Santiago De Chi, Chile. [O'Flaherty, K. S.] ESA ESTEC, EJR Quartz BV, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. [Sanz, A. Olias] ESA ESAC, Server Labs, Camino bajo Castillo S-N, Madrid 28692, Spain. [Oszkiewicz, D.] Adam Mickiewicz Univ, Fac Phys, Astron Observ Inst, Ul Sloneczna 36, PL-60286 Poznan, Poland. [Prat, G.] CNES Ctr Spatial Toulouse, CS Syst Informat, 18 Ave Edouard Belin, F-31401 Toulouse 9, France. [Raison, F.] ESA ESAC, Praesepe BV, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Rocca-Volmerange, B.] Sorbonne Univ UPMC, F-75014 Paris, France. [Rocca-Volmerange, B.] Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Vizcaino, I. Serraller] ESA ESAC, GMV, Camino Bajo del Castillo S-N, Madrid 28692, Spain. [Straizys, V.] Vilnius Univ, Inst Theoret Phys & Astron, Sauletekio Al 3, LT-10222 Vilnius, Lithuania. [ter Linden, M.] S&T Corp, POB 608, NL-2600 AP Delft, Netherlands. [Terrell, D.] Southwest Res Inst SwRI, Dept Space Studies, 1050 Walnut St,Suite 300, Boulder, CO 80302 USA. [Theil, S.] Deutsch Zentrum Luft & Raumfahrt, Inst Space Syst, Fallturm 1, D-28359 Bremen, Germany. [Tiede, C.] Univ Appl Sci Munich, Karlstr 6, D-80333 Munich, Germany. [Troisi, L.] Univ Roma Tor Vergata, Dipartimento Fis, Via Ric Sci 1, I-00133 Rome, Italy. [Vaccari, M.] Univ Western Cape, Dept Phys & Astron, Robert Sobukwe Rd, ZA-7535 Cape Town, South Africa. [Vaccari, M.] Ist Radioastron, INAF, Via Gobetti 101, I-40129 Bologna, Italy. [Van Hamme, W.] Florida Int Univ, Dept Phys, 11200 SW 8th St, Miami, FL 33199 USA. [Wichmann, R.] Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. RP Prusti, T (reprint author), European Space Res & Technol Ctr ESA ESTEC, Sci Support Off, Directorate Sci, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM tprusti@cosmos.esa.int RI Arenou, Frederic/B-1846-2014; Bellas-Velidis, Ioannis/K-4615-2013; Koposov, Sergey/F-2754-2012; Gavras, Panagiotis/C-4485-2015; Rebordao, Jose Manuel/M-3269-2013; Barrado Navascues, David/C-1439-2017; Solano, Enrique/C-2895-2017; OI Granvik, Mikael/0000-0002-5624-1888; Krone-Martins, Alberto/0000-0002-2308-6623; Moitinho de Almeida, Andre/0000-0003-0822-5995; Arenou, Frederic/0000-0003-2837-3899; Koposov, Sergey/0000-0003-2644-135X; Gavras, Panagiotis/0000-0002-4383-4836; Rebordao, Jose Manuel/0000-0002-7418-0345; Barrado Navascues, David/0000-0002-5971-9242; Taylor, Mark/0000-0002-4209-1479; Alvarez, Marco/0000-0002-6786-2620; Garabato, Daniel/0000-0002-7133-6623; de Martino, Domitilla/0000-0002-5069-4202; Fabricius, Claus/0000-0003-2639-1372; Lanza, Antonino Francesco/0000-0001-5928-7251; McMillan, Paul/0000-0002-8861-2620; Dafonte, Carlos/0000-0003-4693-7555; Cellino, Alberto/0000-0002-6645-334X; Berihuete, Angel/0000-0002-8589-4423; Fedorets, Grigori/0000-0002-8418-4809; Alves, Joao/0000-0002-4355-0921; Molnar, Laszlo/0000-0002-8159-1599; Nelemans, Gijs/0000-0002-0752-2974 FU DPAC; Algerian Centre de Recherche en Astronomie, Astrophysique et Geophysique of Bouzareah Observatory; Austrian FWF Hertha Firnberg Programme [T359, P20046, P23737]; BELgian federal Science Policy Office (BELSPO) through various PROgramme de Developpement d'Experiences scientifiques (PRODEX) grants; Brazil-France exchange programmes FAPESP-COFECUB; CAPES-COFECUB; Chinese National Science Foundation [NSFC 11573054]; Czech-Republic Ministry of Education, Youth, and Sports [LG 15010]; Danish Ministry of Science; Estonian Ministry of Education and Research [IUT40-1]; European Commission [MRTN-CT-2006-033481, PIOF-GA-2009-255267, MTKD-CT-2004-014188, FP7-606740, 264895]; European Research Council (ERC) [320360]; European Research Council (ERC) through the European Union's Horizon research and innovation programme [670519]; European Science Foundation (ESF); European Space Agency; European Space Agency Plan for European Cooperating States (PECS) programme; Czech Space Office through ESA PECS [98058]; Academy of Finland; Magnus Ehrnrooth Foundation; French Centre National de la Recherche Scientifique (CNRS) through action "Defi MASTODONS"; French Centre National d'Etudes Spatiales (CNES); French L'Agence Nationale de la Recherche (ANR) investissements d'avenir Initiatives D'EXcellence (IDEX) programme PSL* [ANR-10-IDEX-0001-02]; Region Aquitaine; Universite de Bordeaux; French Utinam Institute of the Universite de Franche-Comte - Region de Franche-Comte; French Utinam Institute of the Universite de Franche-Comte - Institut des Sciences de l'Univers (INSU); German Aerospace Agency (Deutsches Zentrum fur Luft-und Raumfahrt e.V., DLR) [50QG0501, 50QG0601, 50QG0602, 50QG0701, 50QG0901, 50QG1001, 50QG1101, 50QG140, 50QG1401, 50QG1402, 50QG1404]; Hungarian Academy of Sciences through Lendulet Programme [LP2014-17]; Hungarian National Research, Development, and Innovation Office [NKFIH K-115709, PD-116175]; Israel Ministry of Science and Technology [3-9082]; Agenzia Spaziale Italiana (ASI) [I/037/08/0, I/058/10/0, 2014-025-R.0, 2014-025-R.1.2015, I/008/10/0, 2013/030/I.0]; Italian Istituto Nazionale di Astrofisica (INAF); Netherlands Organisation for Scientific Research (NWO) [NWO-M-614.061.414]; Netherlands Research School for Astronomy (NOVA); Polish National Science Centre through HARMONIA grant [2015/18/M/ST9/00544]; Portugese Fundacao para a Ciencia e a Tecnologia (FCT) [PTDC/CTE-SPA/118692/2010, PDCTE/CTE-AST/81711/2003, SFRH/BPD/74697/2010]; Slovenian Research Agency; Spanish Ministry of Economy MINECO-FEDER [AyA2014-55216, AyA2011-24052, ESP2013-48318-C2-R, ESP2014-55996-C2-R]; ICCUB (Unidad de Excelencia Maria de Maeztu) [MDM-2014-0369]; Swedish National Space Board (SNSB/Rymdstyrelsen); Swiss State Secretariat for Education, Research, and Innovation through the ESA PRODEX programme; Mesures d'Accompagnement; Activites Nationales Complementaires; Swiss National Science Foundation, Early Postdoc. Mobility fellowship; United Kingdom Rutherford Appleton Laboratory; United Kingdom Science and Technology Facilities Council (STFC) [PP/C506756/1, ST/I00047X/1]; United Kingdom Space Agency (UKSA) [ST/K000578/1, ST/N000978/1]; ESO programmes [092.B-0165, 093.B-0236, 094.B-0181, 095.B-0046, 096.B-0162, 097.B-0304]; United Kingdom Science and Technology Facilities Council; [PEst-OE/AMB/UI4006/2011]; [UID/FIS/00099/2013]; [UID/EEA/00066/2013] FX This work has made use of results from the European Space Agency (ESA) space mission Gaia, the data from which were processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The Gaia mission website is http://www.cosmos.esa.int/gaia. The authors are current or past members of the ESA and Airbus DS Gaia mission teams and of the Gaia DPAC. This work has financially been supported by: the Algerian Centre de Recherche en Astronomie, Astrophysique et Geophysique of Bouzareah Observatory; the Austrian FWF Hertha Firnberg Programme through grants T359, P20046, and P23737; the BELgian federal Science Policy Office (BELSPO) through various PROgramme de Developpement d'Experiences scientifiques (PRODEX) grants; the Brazil-France exchange programmes FAPESP-COFECUB and CAPES-COFECUB; the Chinese National Science Foundation through grant NSFC 11573054; the Czech-Republic Ministry of Education, Youth, and Sports through grant LG 15010; the Danish Ministry of Science; the Estonian Ministry of Education and Research through grant IUT40-1; the European Commission's Sixth Framework Programme through the European Leadership in Space Astrometry (ELSA) Marie Curie Research Training Network (MRTN-CT-2006-033481), through Marie Curie project PIOF-GA-2009-255267 (SAS-RRL), and through a Marie Curie Transfer-of-Knowledge (ToK) fellowship (MTKD-CT-2004-014188); the European Commission's Seventh Framework Programme through grant FP7-606740 (FP7-SPACE-2013-1) for the Gaia European Network for Improved data User Services (GENIUS) and through grant 264895 for the Gaia Research for European Astronomy Training (GREAT-ITN) network; the European Research Council (ERC) through grant 320360 and through the European Union's Horizon 2020 research and innovation programme through grant agreement 670519 (Mixing and Angular Momentum tranSport of massIvE stars - MAMSIE); the European Science Foundation (ESF), in the framework of the Gaia Research for European Astronomy Training Research Network Programme (GREAT-ESF); the European Space Agency in the framework of the Gaia project; the European Space Agency Plan for European Cooperating States (PECS) programme through grants for Slovenia; the Czech Space Office through ESA PECS contract 98058; the Academy of Finland; the Magnus Ehrnrooth Foundation; the French Centre National de la Recherche Scientifique (CNRS) through action "Defi MASTODONS"; the French Centre National d'Etudes Spatiales (CNES); the French L'Agence Nationale de la Recherche (ANR) investissements d'avenir Initiatives D'EXcellence (IDEX) programme PSL* through grant ANR-10-IDEX-0001-02; the Region Aquitaine; the Universite de Bordeaux; the French Utinam Institute of the Universite de Franche-Comte, supported by the Region de Franche-Comte and the Institut des Sciences de l'Univers (INSU); the German Aerospace Agency (Deutsches Zentrum fur Luft-und Raumfahrt e.V., DLR) through grants 50QG0501, 50QG0601, 50QG0602, 50QG0701, 50QG0901, 50QG1001, 50QG1101, 50QG140, 50QG1401, 50QG1402, and 50QG1404; the Hungarian Academy of Sciences through Lendulet Programme LP2014-17; the Hungarian National Research, Development, and Innovation Office through grants NKFIH K-115709 and PD-116175; the Israel Ministry of Science and Technology through grant 3-9082; the Agenzia Spaziale Italiana (ASI) through grants I/037/08/0, I/058/10/0, 2014-025-R.0, and 2014-025-R.1.2015 to INAF and contracts I/008/10/0 and 2013/030/I.; 0 to ALTEC S.p.A.; the Italian Istituto Nazionale di Astrofisica (INAF); the Netherlands Organisation for Scientific Research (NWO) through grant NWO-M-614.061.414 and through a VICI grant to A. Helmi; the Netherlands Research School for Astronomy (NOVA); the Polish National Science Centre through HARMONIA grant 2015/18/M/ST9/00544; the Portugese Fundacao para a Ciencia e a Tecnologia (FCT) through grants PTDC/CTE-SPA/118692/2010, PDCTE/CTE-AST/81711/2003, and SFRH/BPD/74697/2010; the Strategic Programmes PEst-OE/AMB/UI4006/2011 for SIM, UID/FIS/00099/2013 for CENTRA, and UID/EEA/00066/2013 for UNINOVA; the Slovenian Research Agency; the Spanish Ministry of Economy MINECO-FEDER through grants AyA2014-55216, AyA2011-24052, ESP2013-48318-C2-R, and ESP2014-55996-C2-R and MDM-2014-0369 of ICCUB (Unidad de Excelencia Maria de Maeztu); the Swedish National Space Board (SNSB/Rymdstyrelsen); the Swiss State Secretariat for Education, Research, and Innovation through the ESA PRODEX programme, the Mesures d'Accompagnement, and the Activites Nationales Complementaires; the Swiss National Science Foundation, including an Early Postdoc. Mobility fellowship; the United Kingdom Rutherford Appleton Laboratory; the United Kingdom Science and Technology Facilities Council (STFC) through grants PP/C506756/1 and ST/I00047X/1; and the United Kingdom Space Agency (UKSA) through grants ST/K000578/1 and ST/N000978/1. The GBOT programme uses observations collected at (i) the European Organisation for Astronomical Research in the Southern Hemisphere with the VLT Survey Telescope (VST), under ESO programmes 092.B-0165, 093.B-0236, 094.B-0181, 095.B-0046, 096.B-0162, and 097.B-0304; (ii) the Liverpool Telescope, which is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the United Kingdom Science and Technology Facilities Council; and (iii) telescopes of the Las Cumbres Observatory Global Telescope Network. In addition to the authors of this paper, there are numerous people who have made essential contributions to Gaia, for instance those employed in the design, manufacturing, integration, and testing of the spacecraft and its modules, subsystems, and units. Many of those will remain unnamed yet spent countless hours, occasionally during nights, weekends, and public holidays, in cold offices and dark clean rooms.; At the risk of being incomplete, we specifically name, in alphabetical order, from Airbus DS (Toulouse): Alexandre Affre, Marie-Therese Aime, Audrey Albert, Aurelien Albert-Aguilar, Hania Arsalane, Arnaud Aurousseau, Denis Bassi, Franck Bayle, Pierre-Luc Bazin, Emmanuelle Benninger, Philippe Bertrand, Jean-Bernard Biau, Francois Binter, Cedric Blanc, Eric Blonde, Patrick Bonzom, Bernard Bories, Jean-Jacques Bouisset, Joel Boyadjian, Isabelle Brault, Corinne Buge, Bertrand Calvel, Jean-Michel Camus, France Canton, Lionel Carminati, Michel Carrie, Didier Castel, Fabrice Cherouat, Ludovic Chirouze, Michel Choquet, Claude Coatantiec, Emmanuel Collados, Philippe Corberand, Christelle Dauga, Robert Davancens, Catherine Deblock, Eric Decourbey, Charles Dekhtiar, Michel Delannoy, Michel Delgado, Damien Delmas, Victor Depeyre, Isabelle Desenclos, Christian Dio, Kevin Downes, Marie-Ange Duro, Omar Emam, Elizabeth Estrada, Coralie Falgayrac, Benjamin Farcot, Claude Faubert, Sebastien Finana, Gregory Flandin, Loic Floury, Gilles Fongy, Michel Fruit, Florence Fusero, Christophe Gabilan, Jeremie Gaboriaud, Cyril Gallard, Damien Galy, Benjamin Gandon, Patrick Gareth, Eric Gelis, Andre Gellon, Laurent Georges, Philippe-Marie Gomez, Jose Goncalves, Frederic Guedes, Vincent Guillemier, Thomas Guilpain, Stephane Halbout, Marie Hanne, Gregory Hazera, Daniel Herbin, Tommy Hercher, Claude Hoarau le Papillon, Matthias Holz, Philippe Humbert, Sophie Jallade, Gregory Jonniaux, Frederic Juillard, Philippe Jung, Charles Koeck, Julien L'Hermitte, Rene Laborde, Anouk Laborie, Jerome Lacoste-Barutel, Baptiste Laynet, Virginie Le Gall, Marc Le Roy, Christian Lebranchu, Didier Lebreton, Patrick Lelong, Jean-Luc Leon, Stephan Leppke, Franck Levallois, Philippe Lingot, Laurant Lobo, Celine Lopez, Jean-Michel Loupias, Carlos Luque, Sebastien Maes, Bruno Mamdy, Denis Marchais, Alexandre Marson, Remi Mauriac, Philippe Mayo, Caroline Meisse, Herve Mercereau, Olivier Michel, Florent Minaire, Xavier Moisson, Denis Montperrus, Boris Niel, Cedric Papot, Jean-Francois Pasquier, Gareth Patrick, Pascal Paulet, Martin Peccia, Sylvie Peden, Sonia Penalva, Michel Pendaries, Philippe Peres, Gregory Personne, Dominique Pierot, Jean-Marc Pillot, Lydie Pinel, Fabien Piquemal, Maxime Pomelec, Andre Porras, Pierre Pouny, Severin Provost, Sebastien Ramos, Fabienne Raux, Florian Reuscher, Nicolas Riguet, Mickael Roche, Gilles Rougier, Stephane Roy, Jean-Paul Ruffie, Frederic Safa, Claudie Serris, Andre Sobeczko, Jean-Francois Soucaille, Philippe Tatry, Theo Thomas, Pierre Thoral, Dominique Torcheux, Vincent Tortel, Stephane Touzeau, Didier Trantoul, Cyril Vetel, Jean-Axel Vatinel, Jean-Paul Vormus, Marc Zanoni, from ESA: Ricard Abello, Ivan Aksenov, Salim Ansari, Philippe Armbruster, Jean-Pierre Balley, Rainer Bauske, Thomas Beck, Pier Mario Besso, Carlos Bielsa, Gerhard Billig, Andreas Boosz, Thierry Bru, Joe Bush, Marco Butkovic, Jacques Candee, David Cano, Carlos Casas, Francesco Castellini, David Chapmann, Nebil Cinar, Mark Clements, Giovanni Colangelo, Ana Colorado McEvoy, Vincente Companys, Federico Cordero, Sylvain Damiani, Paolo de Meo, Fabio de Santis, Fabienne Delhaise, Gianpiero Di Girolamo, Yannis Diamantidis, John Dodsworth, Ernesto Dolling, Jane Douglas, Jean Doutreleau, Dominic Doyle, Mark Drapes, Frank Dreger, Peter Droll, Gerhard Drolshagen, Bret Durrett, Christina Eilers, Yannick Enginger, Alessandro Ercolani, Robert Ernst, Hugh Evans, Fabio Favata, Stefano Ferreri, Daniel Firre, Michael Flegel, Melanie Flentge, Alan Flowers, Jens Freihofer, Cesar Gomez Hernandez, Juan Ma; nuel Garcia, Wahida Gasti, Jose Gavira, Frank Geerling, Franck Germes, Gottlob Gienger, Benedicte Girouart, Bernard Godard, Nick Godfrey, Roy Gouka, Cosimo Greco, Robert Guilanya, Kester Habermann, Manfred Hadwiger, Ian Harrison, Angela Head, Martin Hechler, Kjeld Hjortnaes, Jacolien Hoek, Frank Hoffmann, Justin Howard, Arjan Hulsbosch, Jose Jimenez, Simon Kellett, Andrea Kerruish, Kevin Kewin, Oliver Kiddle, Sabine Kielbassa, Volker Kirschner, Holger Krag, Benoiit Laine, Markus Landgraf, Mathias Lauer, Robert Launer, Santiago Llorente, Guillermo Lorenzo, James Madison, Filip Marinic, Arturo Martin Polegre, Ander Martinez, Marco Massaro, Luca Michienzi, Ali Mohammadzadeh, Richard Morgan-Owen, Prisca Muhlmann, Michael Muller, Pablo Munoz, Petteri Nieminen, Alfred Nillies, Wilfried Nzoubou, Alistair O'Connell, Oscar Pace, Mohini Parameswaran, Ramon Pardo, Taniya Parikh, Panos Partheniou, Dario Pellegrinetti, Jose-Louis Pellon-Bailon, Michael Perryman, Christian Philippe, Alex Popescu, Alfonso Rivero, Andrew Robson, Gerd Rossling, Martina Rossmann, Markus Ruckert, Jamie Salt, Giovanni Santin, Rui Santos, Stefano Scaglioni, Melanie Schabe, Dominic Schafer, Micha Schmidt, Rudolf Schmidt, Jean Schutz, Klaus-Jurgen Schulz, Julia Schwartz, Andreas Scior, Jorg Seifert, Gunther Sessler, Felicity Sheasby, Heike Sillack, Swamy Siram, Claudio Sollazzo, Steven Straw, Mark Thompson, Raffaele Tosellini, Irren Tsu-Silva, Livio Tucci, Aileen Urwin, Jean-Baptiste Valet, Helma van de Kamp-Glasbergen, Martin Vannier, Kees van't Klooster, Enrico Vassallo, David Verrier, Sam Verstaen, Rudiger Vetter, Jose Villalvilla, Raffaele Vitulli, Mildred Vogele, Sergio Volonte, Catherine Watson, Karsten Weber, Gavin Williams, Alistair Winton, Michael Witting, Peter Wright, Karlie Yeung, Igor Zayer, and from CERN: Vincenzo Innocente. We thank the referee, Joss Bland-Hawthorn, for constructive feedback that helped to clarify several items in the text. NR 123 TC 24 Z9 24 U1 5 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A1 DI 10.1051/0004-6361/201629272 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500125 ER PT J AU Willson, M Kraus, S Kluska, J Monnier, JD Ireland, M Aarnio, A Sitko, ML Calvet, N Espaillat, C Wilner, DJ AF Willson, M. Kraus, S. Kluska, J. Monnier, J. D. Ireland, M. Aarnio, A. Sitko, M. L. Calvet, N. Espaillat, C. Wilner, D. J. TI Sparse aperture masking interferometry survey of transitional discs Search for substellar-mass companions and asymmetries in their parent discs SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; planets and satellites: formation; planets and satellites: detection; techniques: interferometric stars: pre-main sequence ID T-TAURI STARS; MAIN-SEQUENCE STARS; INFRARED SPECTROGRAPH SPECTRA; H ALPHA-EMISSION; PROTOPLANETARY DISK; YOUNG STARS; PRETRANSITIONAL DISKS; IMAGE-RECONSTRUCTION; CIRCUMSTELLAR DISKS; GIANT PLANETS AB Context. Transitional discs are a class of circumstellar discs around young stars with extensive clearing of dusty material within their inner regions on 10s of au scales. One of the primary candidates for this kind of clearing is the formation of planet(s) within the disc that then accrete or clear their immediate area as they migrate through the disc. Aims. The goal of this survey was to search for asymmetries in the brightness distribution around a selection of transitional disc targets. We then aimed to determine whether these asymmetries trace dynamically-induced structures in the disc or the gap-opening planets themselves. Methods. Our sample included eight transitional discs. Using the Keck/NIRC2 instrument we utilised the Sparse Aperture Masking ( SAM) interferometry technique to search for asymmetries indicative of ongoing planet formation. We searched for close-in companions using both model fitting and interferometric image reconstruction techniques. Using simulated data, we derived diagnostics that helped us to distinguish between point sources and extended asymmetric disc emission. In addition, we investigated the degeneracy between the contrast and separation that appear for marginally resolved companions. Results. We found FP Tau to contain a previously unseen disc wall, and DMTau, LkH ff 330, and TWHya to contain an asymmetric signal indicative of point source-like emission. We placed upper limits on the contrast of a companion in RXJ 1842.9-3532 and V2246 Oph. We ruled the asymmetry signal in RXJ 1615.3-3255 and V2062 Oph to be false positives. In the cases where our data indicated a potential companion we computed estimates for the value of McMc and found values in the range of 10(-5)-10(-3) M-J(2) yr(-1). Conclusions. We found significant asymmetries in four targets. Of these, three were consistent with companions. We resolved a previously unseen gap in the disc of FP Tau extending inwards from approximately 10 au. C1 [Willson, M.; Kraus, S.; Kluska, J.] Univ Exeter, Astrophys Grp, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England. [Monnier, J. D.; Aarnio, A.; Calvet, N.] Univ Michigan, Dept Astron, 311 West Hall,1085 South Univ Ave, Ann Arbor, MI 48109 USA. [Ireland, M.] Res Sch Astron & Astrophys, Mt Stromlo Observ Cotter Rd, Weston, ACT 2611, Australia. [Sitko, M. L.] Univ Cincinnati, Dept Phys, Cincinnati, OH 45221 USA. [Sitko, M. L.] Space Sci Inst, 475 Walnut St,Suite 205, Boulder, CO 80301 USA. [Espaillat, C.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-78, Cambridge, MA 02138 USA. RP Willson, M (reprint author), Univ Exeter, Astrophys Grp, Sch Phys, Stocker Rd, Exeter EX4 4QL, Devon, England. EM mwillson@astro.ex.ac.uk FU STFC Rutherford Fellowship and Grant [ST/J004030/1, ST/K003445/1]; Marie Sklodowska-Curie CIG grant [618910]; Philip Leverhulme Prize [PLP-2013-110]; NASA KPDA grants [JPL-1452321, 1474717, 1485953, 1496788]; W.M. Keck Foundation FX We acknowledge support from a STFC Rutherford Fellowship and Grant (ST/J004030/1, ST/K003445/1), Marie Sklodowska-Curie CIG grant (Ref. 618910), and Philip Leverhulme Prize (PLP-2013-110). We additionally acknowledge support from NASA KPDA grants (JPL-1452321, 1474717, 1485953, 1496788). The authors wish to recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. NR 68 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD NOV PY 2016 VL 595 AR A9 DI 10.1051/0004-6361/201628859 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ED0ZP UT WOS:000388573500087 ER PT J AU Markson, S Rittenhouse, ST Schmidt, R Shaffer, JP Sadeghpour, HR AF Markson, Samuel Rittenhouse, Seth T. Schmidt, Richard Shaffer, James P. Sadeghpour, H. R. TI Theory of Ultralong-Range Rydberg Molecule Formation Incorporating Spin-Dependent Relativistic Effects: Cs(6s)-Cs(np) as Case Study SO CHEMPHYSCHEM LA English DT Article DE cold molecules; dipole moments; relativistic effects; Rydberg systems; vibrational spectroscopy ID HYPERFINE-STRUCTURE; SHAPE RESONANCES; DIPOLE-MOMENTS; STATES; DIMERS; ATOMS; CS AB We calculate vibrational spectra of ultralong-range Cs(32p) Rydberg molecules that form in an ultracold gas of Cs atoms. We account for the partial-wave scattering of the Rydberg electrons from the Cs perturber atoms by including the full set of spin-resolved S-1,3(J) and P-1,3(J) scattering phase shifts, and allow for the mixing of singlet (S=0) and triplet (S=1) spin states through Rydberg electron spin-orbit and ground state electron hyperfine interactions. Excellent agreement with observed data in Sa ss mannshausen etal. [Phys. Rev. Lett. 2015, 113, 133201] in line positions and profiles is obtained. We also determine the spin-dependent permanent electric dipole moments for these molecules. This is the first such calculation of ultralong-range Rydberg molecules for which all of the relativistic contributions are accounted. C1 [Markson, Samuel; Schmidt, Richard; Sadeghpour, H. R.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Markson, Samuel] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Rittenhouse, Seth T.] US Naval Acad, Dept Phys, Annapolis, MD 21402 USA. [Shaffer, James P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73072 USA. RP Markson, S (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.; Markson, S (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM smarkson@cfa.harvard.edu FU FAS Division of Science, Research Computing Group at Harvard University; NSF Graduate Research Fellow grant; Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University; Smithsonian Astrophysical Observatory; NSF [PHY-1516421, PHY-1607296]; Smitsonian Astrophysical Observatory; Cottrell College Science Award through the Research Corporation for Scientific Advancement FX The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. S.M. is supported by an NSF Graduate Research Fellow grant, the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University, and the Smithsonian Astrophysical Observatory. R.S. is supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and the Smitsonian Astrophysical Observatory. S.T.R. acknowledges support from NSF Grant No. PHY-1516421 and from a Cottrell College Science Award through the Research Corporation for Scientific Advancement. J.S. acknowledges support from NSF Grant No. PHY-1607296. This article is a contribution of the U.S. Government and is not subject to U.S. copyright. NR 31 TC 1 Z9 1 U1 2 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 1439-4235 EI 1439-7641 J9 CHEMPHYSCHEM JI ChemPhysChem PD NOV PY 2016 VL 17 IS 22 BP 3683 EP 3691 DI 10.1002/cphc.201600932 PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA ED1SK UT WOS:000388625000013 PM 27712011 ER PT J AU Tonra, CM Sager-Fradkin, K Marra, PP AF Tonra, Christopher M. Sager-Fradkin, Kimberly Marra, Peter P. TI Barriers to salmon migration impact body condition, offspring size, and life history variation in an avian consumer SO ECOGRAPHY LA English DT Article ID DIPPERS CINCLUS-MEXICANUS; MARINE-DERIVED NUTRIENTS; SPAWNING PACIFIC SALMON; AMERICAN DIPPERS; FRESH-WATER; FOOD WEBS; DAM REMOVAL; ALTITUDINAL MIGRATION; STREAM PRODUCTIVITY; SOUTHEASTERN ALASKA AB The impacts of barriers, such as dams, and associated stream effects on the migration of salmon have been well documented, but there is much less information on consequences for terrestrial vertebrates in these freshwater systems. Salmon themselves provide food resources to higher trophic levels and deposit rich marine-derived nutrients (MDN) that benefit the base of freshwater food webs. We studied a higher-order terrestrial consumer of aquatic prey, the American dipper Cinclus mexicanus, in a riparian food web, to test the hypothesis that barriers to salmon migration negatively impact body condition, and ultimately life history. We predicted that, compared to dippers breeding above barriers, those in areas with salmon would receive MDN and thus be in better condition, have greater breeding effort (frequency of multiple brood attempts), produce larger offspring in better condition, be more likely to maintain year-round territories, and have higher annual survival. Using stable isotopes as signatures of MDN, we found that C-13 and N-15 were more enriched in dippers below barriers, confirming access to MDN. Female dippers below barriers had greater mass corrected for body size, were more likely to attempt multiple broods within a season and produced larger female offspring. Furthermore, dippers below barriers were more likely to maintain year-round territories and had higher annual survival. Our results demonstrate how river barriers such as dams influence vital rates and life histories of higher-order consumers. C1 [Tonra, Christopher M.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [Tonra, Christopher M.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Sager-Fradkin, Kimberly] Lower Elwha Klallam Tribe, Dept Nat Resources, Port Angeles, WA USA. RP Tonra, CM (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. EM tonra.1@osu.edu FU USFWS Tribal Wildlife Research grant [WA U-26-NA-1]; Smithsonian Stable Isotope Research Fellowship; George Didden Conservation Biology Fellowship from the National Zoo; Olympic National Forest; Clallam County Parks; Washington Dept of Fish and Wildlife; Dungeness State Hatchery FX This study was funded by a USFWS Tribal Wildlife Research grant to Marra and Sager-Fradkin (WA U-26-NA-1), and a Smithsonian Stable Isotope Research Fellowship and George Didden Conservation Biology Fellowship from the National Zoo to CMT. For providing support as well as access to study sites, we are extremely grateful to Olympic National Park, particularly Patti Happe and Jerry Freilich; Olympic National Forest; Clallam County Parks; Washington Dept of Fish and Wildlife, including staff at the Elwha Chinook rearing channel and the Dungeness State Hatchery; and several private land owners. We wish to thank James Adelman, Dave Manson, Rebecca Paradis, and especially Sara Cendejas-Zarelli for their assistance in the field. We are grateful to Christine France for her assistance with stable isotope analysis and to Rob Fleischer and Nancy Rotzel McInerney for assistance with DNA analysis and access to facilities. Ray Danner and Colin Studds provided assistance with analysis and frequent discussions of the topics of this study, and we thank Barbara Blackie, Jeff Duda, Sarah Morley, and the Natural Resources staff of the Lower Elwha Klallam Tribe for sharing their knowledge of this system and for assistance with identifying study sites. All of our field methods were approved by the Smithsonian Inst. Animal Care and Use Committee (Protocol #11-01). NR 67 TC 1 Z9 1 U1 11 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0906-7590 EI 1600-0587 J9 ECOGRAPHY JI Ecography PD NOV PY 2016 VL 39 IS 11 BP 1056 EP 1065 DI 10.1111/ecog.02014 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA ED1DK UT WOS:000388584000004 ER PT J AU Sangil, C Guzman, HM AF Sangil, Carlos Guzman, Hector M. TI Macroalgal communities on multi-stressed coral reefs in the Caribbean: Long-term changes, spatial variations, and relationships with environmental variables SO JOURNAL OF SEA RESEARCH LA English DT Article DE Coral reef macroalgae; Community structure; Time series; Lobophora variegata; Halimeda opuntia; Echinometra viridis ID GREAT-BARRIER-REEF; NORTHWESTERN HAWAIIAN-ISLANDS; BOCAS DEL TORO; DIADEMA-ANTILLARUM; CLIMATE-CHANGE; MASS MORTALITY; PHASE-SHIFTS; REDUNDANCY ANALYSIS; BENTHIC COMMUNITY; WAVE EXPOSURE AB Long-term changes in macroalgal cover, spatial variation between macroalgal communities, and relationships with environmental variables and benthic groups were assessed in coral reefs along the Caribbean coast of Panama. Sampling was conducted in two regions: Western and Central. Data collected between 2000 and 2012 showed a continuous increase in macroalgal abundance, although patterns differed according to region and site. There were differences in macroalgal communities between regions, as well as within regions between different wave-exposure levels. There were also differences between sites within regions exposed to the same level of wave action. Multivariate analysis found that wave exposure along with herbivore density (Echinometra viridis) and sedimentation were the variables that explained most of the variability between communities. Other variables such as Echinometra lucunter and Diadema antillarum densities, fish density, productivity, and live coral cover had significant relationships with community structure, but explained less of the variability. (C) 2016 Elsevier B.V. All rights reserved. C1 [Sangil, Carlos] Univ La Laguna, Dept Bot Ecol & Plant Physiol, San Cristobal la Laguna 38071, Canary Islands, Spain. [Sangil, Carlos] Univ La Laguna, Dept Anim Biol Soil Sci & Geol, Canary Isl, Spain. [Guzman, Hector M.] Smithsonian Inst, Smithsonian Trop Res Inst, Panama City, Panama. RP Sangil, C (reprint author), Univ La Laguna, Dept Bot Ecol & Plant Physiol, San Cristobal la Laguna 38071, Canary Islands, Spain. EM casangil@ull.es FU Smithsonian Tropical Research Institute, Smithsonian Institution; Dr. Manuel Morales Foundation FX Long-term data was produced by the Panama Coral Reef Monitoring Network, a program supported by the Smithsonian Tropical Research Institute, Smithsonian Institution. Special thanks to Carlos Guevara and Marta Rodriguez for field work support and comments and initial review of this manuscript. C. Sangil benefited from a postdoctoral fellowship from the Dr. Manuel Morales Foundation. NR 80 TC 0 Z9 0 U1 10 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1385-1101 EI 1873-1414 J9 J SEA RES JI J. Sea Res. PD NOV PY 2016 VL 117 BP 7 EP 19 DI 10.1016/j.seares.2016.09.001 PG 13 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA ED3VR UT WOS:000388777100002 ER PT J AU Krishnadas, M Kumar, A Comita, LS AF Krishnadas, Meghna Kumar, Ajith Comita, Liza S. TI Environmental gradients structure tropical tree assemblages at the regional scale SO JOURNAL OF VEGETATION SCIENCE LA English DT Article DE Community assembly; Environmental filtering; Habitat classification; Indicator species; Multivariate regression trees; Niche breadth; Tropical forest; Western Ghats ID RAIN-FOREST TREES; BETA-DIVERSITY; HABITAT ASSOCIATIONS; DENSITY-DEPENDENCE; SPATIAL SCALES; CLIMATE-CHANGE; WESTERN-GHATS; FLORISTIC COMPOSITION; SPECIES ASSEMBLAGES; BIODIVERSITY CHANGE AB Questions: Environmental filtering and niche differences influence assembly of tree communities at multiple spatial scales. At regional scales, determining the environmental variables that primarily influence compositional variation in species assemblages reveals ecologically relevant habitat types for conservation. Strength of species' association with these habitats and differences in species occurrence along environmental gradients lend credence to niche-based assembly and help estimate responses of tree communities to natural or human-mediated environmental change. Location: Western Ghats, India. Methods: We analysed an openly available data set of ca. 62 000 trees (>10 cm DBH) in 96 1-ha plots across a 22 000 km(2) landscape, using multivariate regression trees (MRT) to identify compositional groups related to combinations of temperature, rainfall and soil type. Next, we conducted indicator species analysis to assess species associations with habitats. We then compared species richness and diversity among habitats. Finally, to discern niche overlap we assessed pair-wise differences between species in their abundance distributions along environmental gradients. Results: Environmental gradients clearly influenced landscape-scale tree assemblages in this region. Nine ecological habitat types were identified: annual rainfall was the most important variable driving compositional differences, followed by temperature, seasonality and soils. Approximately 17% of 398 species tested were associated with single habitats. Number of species associations and local diversity varied significantly among habitats. Between 29 and 50% of species pairs showed significant differences in their distributions along environmental gradients considered. Conclusions: Relating compositionally defined tree assemblages to combinations of abiotic variables allows ecologically robust recognition of habitat types for conservation planning. Compositional differences structured by annual rainfall and temperature suggests that climate change can impact species persistence and tree community composition in the Western Ghats. Specifically, future research should assess drought response of forests by examining recruitment and survival of species in different combinations of rainfall, temperature and human disturbances. C1 [Krishnadas, Meghna; Comita, Liza S.] Yale Sch Forestry & Environm Studies, 205 Prospect St, New Haven, CT 06511 USA. [Kumar, Ajith] Wildlife Conservat Soc India, Ctr Wildlife Studies, Bangalore, Karnataka, India. [Kumar, Ajith] Natl Ctr Biol Sci, Bellary Rd, Bangalore 560065, Karnataka, India. [Comita, Liza S.] Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. RP Krishnadas, M (reprint author), Yale Sch Forestry & Environm Studies, 205 Prospect St, New Haven, CT 06511 USA. EM meghna.krishnadas@yale.edu; ajith@ncbs.res.in; liza.comita@yale.edu OI Krishnadas, Meghna/0000-0003-2231-9787 NR 80 TC 0 Z9 0 U1 15 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1100-9233 EI 1654-1103 J9 J VEG SCI JI J. Veg. Sci. PD NOV PY 2016 VL 27 IS 6 BP 1117 EP 1128 DI 10.1111/jvs.12438 PG 12 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA ED7RG UT WOS:000389066400005 ER PT J AU Huang, DW Arrigoni, R Benzoni, F Fukami, H Knowlton, N Smith, ND Stolarski, J Chou, LM Budd, AF AF Huang, Danwei Arrigoni, Roberto Benzoni, Francesca Fukami, Hironobu Knowlton, Nancy Smith, Nathan D. Stolarski, Jaroslaw Chou, Loke Ming Budd, Ann F. TI Taxonomic classification of the reef coral family Lobophylliidae (Cnidaria: Anthozoa: Scleractinia) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Faviina; Indo-Pacific; integrative taxonomy; marine invertebrates; morphological phylogenetics; Mussidae; systematics ID BAYESIAN PHYLOGENETIC INFERENCE; MOLECULAR PHYLOGENY; MAXIMUM-LIKELIHOOD; ORDER SCLERACTINIA; MIXED MODELS; GENUS; FAVIIDAE; GENERA; RECONSTRUCTION; MERULINIDAE AB Lobophylliidae is a family-level clade of corals within the 'robust' lineage of Scleractinia. It comprises species traditionally classified as Indo-Pacific 'mussids', 'faviids', and 'pectiniids'. Following detailed revisions of the closely related families Merulinidae, Mussidae, Montastraeidae, and Diploastraeidae, this monograph focuses on the taxonomy of Lobophylliidae. Specifically, we studied 44 of a total of 54 living lobophylliid species from all 11 genera based on an integrative analysis of colony, corallite, and subcorallite morphology with molecular sequence data. By examining coral skeletal features at three distinct levels - macromorphology, micromorphology, and microstructure we built a morphological matrix comprising 46 characters. Data were analysed via maximum parsimony and transformed onto a robust molecular phylogeny inferred using two nuclear (histone H3 and internal transcribed spacers) and one mitochondrial (cytochrome c oxidase subunit I) DNA loci. The results suggest that micromorphological characters exhibit the lowest level of homoplasy within Lobophylliidae. Molecular and morphological trees show that Symphyllia, Parascolymia, and Australomussa should be considered junior synonyms of Lobophyllia, whereas Lobophyllia pachysepta needs to be transferred to Acanthastrea. Our analyses also lend strong support to recent revisions of Acanthastrea, which has been reorganized into five separate genera (Lobophyllia, Acanthastrea, Homophyllia, Sclerophyllia, and Micromussa), and to the establishment of Australophyllia. Cynarina and the monotypic Moseleya remain unchanged, and there are insufficient data to redefine Oxypora, Echinophyllia, and Echinomorpha. Finally, all lobophylliid genera are diagnosed under the phylogenetic classification system proposed here, which will facilitate the placement of extinct taxa on the scleractinian tree of life. (C) 2016 The Linnean Society of London C1 [Huang, Danwei; Chou, Loke Ming] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Huang, Danwei; Chou, Loke Ming] Natl Univ Singapore, Trop Marine Sci Inst, Singapore 117543, Singapore. [Arrigoni, Roberto] King Abdullah Univ Sci & Technol, Div Biol & Environm Sci & Engn, Red Sea Res Ctr, Thuwal 239556900, Saudi Arabia. [Arrigoni, Roberto; Benzoni, Francesca] Univ Milano Bicocca, Dept Biotechnol & Biosci, Piazza Sci 2, I-20126 Milan, Italy. [Fukami, Hironobu] Miyazaki Univ, Dept Marine Biol & Environm Sci, Miyazaki 8892192, Japan. [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Smith, Nathan D.] Nat Hist Museum Los Angeles Cty, Dinosaur Inst, 900 Exposit Blvd, Los Angeles, CA 90007 USA. [Stolarski, Jaroslaw] Polish Acad Sci, Inst Paleobiol, Twarda 51-55, PL-00818 Warsaw, Poland. [Budd, Ann F.] Univ Iowa, Dept Earth & Environm Sci, Iowa City, IA 52242 USA. RP Huang, DW (reprint author), Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore.; Huang, DW (reprint author), Natl Univ Singapore, Trop Marine Sci Inst, Singapore 117543, Singapore.; Arrigoni, R (reprint author), King Abdullah Univ Sci & Technol, Div Biol & Environm Sci & Engn, Red Sea Res Ctr, Thuwal 239556900, Saudi Arabia.; Arrigoni, R (reprint author), Univ Milano Bicocca, Dept Biotechnol & Biosci, Piazza Sci 2, I-20126 Milan, Italy. EM huangdanwei@nus.edu.sg; roberto.arrigoni@kaust.edu.sa RI Benzoni, Francesca/G-1304-2010 OI Benzoni, Francesca/0000-0001-8906-1309 FU US National Science Foundation [DEB-1145043, 1331980]; National University of Singapore [R-154-000-671-133] FX For comments on taxonomy, we thank S. D. Cairns, B. W. Hoeksema, and B. R. Rosen. We appreciate the following for assistance with museum loans, cataloguing information, and specimen photographs: T. S. Adrain (SUI), K. S. Chua and S. K. Tan (ZRC), A. J. Baldinger (MCZ), A. Andouche and P. Lozouet (MNHN), C. C. Wallace, B. J. Done, and P. R. Muir (MTQ), J. G. Darrell, K. G. Johnson, N. Santodomingo, and H. Taylor (NHMUK), G. Paulay (UF), W. Y. Licuanan and K. S. Luzon (UP), S. D. Cairns, T. Coffer, and T. C. Walter (USNM), Z. T. Richards (WAM), C. Lueter, K. Loch, and W. Loch (ZMB), and M. V. Sorensen and M. T. Tottrup (ZMUC). We also thank M. L. Berumen (King Abdullah University of Science and Technology) for samples from the Red Sea, E. Karsenti (European Molecular Biology Laboratory), E. Bourgois (Tara Oceans Expeditions), and the OCEANS consortium for sampling in Gambier Island and Djibouti during the Tara Oceans Expeditions, A. H. Baird and M. O. Hoogenboom (James Cook University) for specimens from Australia, C. Payri and B. Dreyfus (IRD) for collections in New Caledonia, and the Niugini Biodiversity Expedition and P. Bouchet (MNHN) for specimens from Papua New Guinea, as well as E. Dutrieux (CREOCEAN) and C. H. Chaineau (Total SA) for samples from Yemen. M. Wortel of the Department of Earth & Environmental Sciences Petrographic Facilities at the University of Iowa prepared thin sections. Scanning electron microscopy was performed at the University of Iowa Central Microscopy Research Facility, and also at USNM aided by Caitlin Baker. Y. X. Tee helped to verify the references. Funds were provided by the US National Science Foundation Grants DEB-1145043, 1331980, as well as the National University of Singapore Start-up Grant R-154-000-671-133. Data reported here are available as Supporting Information and in the Corallosphere database. NR 198 TC 0 Z9 0 U1 2 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD NOV PY 2016 VL 178 IS 3 BP 436 EP 481 DI 10.1111/zoj.12391 PG 46 WC Zoology SC Zoology GA ED1RW UT WOS:000388623600001 ER PT J AU Rauhut, OWM Carrano, MT AF Rauhut, Oliver W. M. Carrano, Matthew T. TI The theropod dinosaur Elaphrosaurus bambergi Janensch, 1920, from the Late Jurassic of Tendaguru, Tanzania SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Abelisauroidea; Africa; Gondwana; Noasauridae; theropod evolution ID ABELISAUROID DINOSAURIA; PHYLOGENETIC POSITION; TYRANNOSAURUS-REX; PATAGONIA; OSTEOLOGY; EVOLUTION; CERATOSAUR; ARGENTINA; MOROCCO; AFRICA AB Theropod dinosaurs from the Late Jurassic of Gondwana are still poorly known, with Elaphrosaurus bambergi Janensch, 1920, from the late Kimmeridgian of Tendaguru, Tanzania, being the only taxon represented by more than isolated remains from Africa. Having long been considered a coelurosaurian, more specifically an ornithomimosaur, Elaphrosaurus is currently regarded as a basal ceratosaur. Here, we revise the osteology and phylogenetic position of this important taxon. Elaphrosaurus shows many unusual osteological characters, including extremely elongated and constricted cervical vertebrae, an expansive shoulder girdle with strongly modified forelimbs, a relatively small ilium, and elongate hindlimbs with a very small ascending process of the astragalus that is fused to the tibia. We found this taxon to share many derived characters with noasaurids, such as: strongly elongate cervical and dorsal vertebrae; low, rectangular neural spines in the mid-caudal vertebrae; presence of only an anterior centrodiapophyseal lamina in anterior caudal vertebrae; presence of a wide, U-shaped notch between the glenoid and the anteroventral hook in the coracoid; a laterally flared postacetabular blade of the ilium; a flat anterior side of the distal tibia; and a reduced shaft of metatarsal II. Our analysis placed Elaphrosaurus within a dichotomous Noasauridae as part of a Jurassic subclade, here termed Elaphrosaurinae, that otherwise includes taxa from eastern Asia. These results underscore the long and complex evolutionary history of abelisauroids, which is still only beginning to be understood. (C) 2016 The Linnean Society of London C1 [Rauhut, Oliver W. M.] Ludwig Maximilians Univ Munchen, Dept Earth & Environm Sci, Bayer Staatssammlung Palaontol & Geol, GeoBioCtr,SNSB, Richard Wagner Str 10, D-80333 Munich, Germany. [Carrano, Matthew T.] Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. RP Rauhut, OWM (reprint author), Ludwig Maximilians Univ Munchen, Dept Earth & Environm Sci, Bayer Staatssammlung Palaontol & Geol, GeoBioCtr,SNSB, Richard Wagner Str 10, D-80333 Munich, Germany. EM o.rauhut@lrz.uni-muenchen.de FU Deutsche Forschungsgemeinschaft [RA 1012/1-1]; Volkswagen Foundation [I/84 640] FX First of all, the curators who made the study of Elaphrosaurus possible during this long-term project deserve our special thanks: Wolf-Dieter Heinrich, David Unwin, and Daniela Schwarz. Likewise, we thank Kristian Remes who supervised the remounting of the Tendaguru dinosaurs for the new exhibition in the Natural History Museum in Berlin, and helped in many other ways. Many colleagues provided access to material for comparative purposes, and all of this help is gratefully acknowledged, especially to Xu Xing, Li Kui, Ronan Allain, and Paul Sereno. We thank Adriana Lopez-Arbarello, Wolf-Dieter Heinrich, Christian Foth, and Diego Pol for useful discussions. Mario Bronzati is thanked for taking the measurements of the femoral circumference of Elaphrosaurus, and Martine Focke, Georg Janssen, and Manuela Schellenberger helped with processing the photographs. Steve Brusatte and Phil Currie deserve thanks for carefully reviewing the manuscript and providing many useful comments. This project was financially supported by the Deutsche Forschungsgemeinschaft under grant RA 1012/1-1 and the Volkswagen Foundation under grant I/84 640 (both to O.R.), which is gratefully acknowledged. English translations of Accarie et al. (1995), Bonaparte (1986), Janensch (1925), Lapparent (1960), Novas (1992), and Stromer (1915, 1931) are available from The Polyglot Paleontologist website (www.paleoglot.org). NR 163 TC 1 Z9 1 U1 3 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD NOV PY 2016 VL 178 IS 3 BP 546 EP 610 DI 10.1111/zoj.12425 PG 65 WC Zoology SC Zoology GA ED1RW UT WOS:000388623600005 ER PT J AU Parsons, AW Bland, C Forrester, T Baker-Whatton, MC Schuttler, SG McShea, WJ Costello, R Kays, R AF Parsons, Arielle Waldstein Bland, Christina Forrester, Tavis Baker-Whatton, Megan C. Schuttler, Stephanie G. McShea, William J. Costello, Robert Kays, Roland TI The ecological impact of humans and dogs on wildlife in protected areas in eastern North America SO BIOLOGICAL CONSERVATION LA English DT Article DE Camera traps; Coyote; Hikers; Domestic dog; Protected areas; Risk-disturbance ID DOMESTIC DOGS; FLIGHT RESPONSES; DEER; POPULATIONS; CARNIVORES; UNGULATE; PREDATOR; GROWTH; FOREST; PARKS AB The establishment of protected areas is a key strategy for preserving biodiversity. However, human use of protected areas can cause disturbance to wildlife, especially in areas that allow hunting and if humans are accompanied by dogs (Canis familiaris). We used citizen-science run camera traps to investigate how humans, dogs and coyotes (Canis latrans) used 33 protected areas and analyzed behavioral responses by three prey species: white-tailed deer (Odocoileus virginianus), eastern gray squirrel (Sciurus carolinensis) and northern raccoon (Procyon lotor). We obtained 52,863 detections of native wildlife, 162,418 detections of humans and 23,332 detections of dogs over 42,874 camera nights. Most dogs (99%) were on the trail, and 89% of off-trail dogs were accompanied by humans. Prey avoided dogs, humans and coyotes temporally, but did not avoid them spatially, or greatly increase vigilance. Our results indicate that humans are perceived as a greater risk than coyotes, and this increases when dogs accompany their owners. The concentration of dogs on the trail with their owners, and relatively minor behavioral impacts on prey, contrasts the strong negative ecological effects found in studies of free ranging dogs. We found dog management to be effective: prohibiting dogs in protected areas reduced their use of an area by a factor of 10 and leash laws increased leashing rates by 21%. Although millions of dogs use natural areas in North America each year, regulations enacted by protected areas combined with responsible management of dog behavior greatly reduce the ecological impact of man's best friend. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Parsons, Arielle Waldstein; Schuttler, Stephanie G.; Kays, Roland] North Carolina Museum Nat Sci, 11 West Jones St, Raleigh, NC 27601 USA. [Bland, Christina; Kays, Roland] North Carolina State Univ, Dept Forestry & Environm Resources, 2800 Faucette Blvd, Raleigh, NC 27607 USA. [Costello, Robert; Kays, Roland] Smithsonians Natl Museum Nat Hist, 10th St & Constitut Ave NW, Washington, DC 20560 USA. [Forrester, Tavis; McShea, William J.] Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. [Forrester, Tavis] Oregon Dept Fish & Wildlife, 1401 Gekeler Lane, La Grande, OR 97850 USA. [Baker-Whatton, Megan C.] Nature Conservancy, 4245 Fairfax Dr, Arlington, VA 22203 USA. RP Parsons, AW (reprint author), NC Museum Nat Sci, 11 West Jones St, Raleigh, NC 27601 USA. EM arielle.parsons@naturalsciences.org FU National Science Foundation [1232442, 1319293]; US Forest Service [13-JV-11330101-021]; North Carolina Museum of Natural Sciences; Smithsonian Institution FX We thank our 376 volunteers for their hard work collecting camera trap data for this study. For their field assistance and volunteer coordination we thank the staff of the NPS, USFWS, USFS, TNC, NC, SC, VA, MD and TN State Parks, NCWRC, TNDF, VDGIF, WVWA, the WNF, and RPRCR We thank A. Mash, N. Fuentes, S. Higdon, T. Perkins, L. Gatens, R. Owens, R. Gayle, C. Backman, K. Clark, J. Grimes and J. Simkins for their help reviewing photographs. We thank P. Jansen and M. Cove for early discussions of AAR This work was conducted with funding from the National Science Foundation [grant #1232442 and #1319293], the US Forest Service [grant #13-JV-11330101-021], the North Carolina Museum of Natural Sciences and the Smithsonian Institution. NR 41 TC 1 Z9 1 U1 53 U2 53 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD NOV PY 2016 VL 203 BP 75 EP 88 DI 10.1016/j.biocon.2016.09.001 PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EC5EO UT WOS:000388156100009 ER PT J AU Buuveibaatar, B Mueller, T Strindberg, S Leimgruber, P Kaczensky, P Fuller, TK AF Buuveibaatar, Bayarbaatar Mueller, Thomas Strindberg, Samantha Leimgruber, Peter Kaczensky, Petra Fuller, Todd K. TI Human activities negatively impact distribution of ungulates in the Mongolian Gobi SO BIOLOGICAL CONSERVATION LA English DT Article DE Spatial modelling; Equus hemionus; Mining development; Gobi desert; Mongolia; Gazella subgutturosa ID CENTRAL-ASIA; SAIGA ANTELOPE; GAZELLES; SELECTION; WILDLIFE; ECOLOGY AB The Southern Gobi of Mongolia is an iconic ungulate stronghold that supports the world's largest populations of Asiatic wild ass (or khulan - Equus hemionus) and goitered gazelle (Gazella subgutturosa). A growing human population, intensifying exploitation of natural resources, and the development of infrastructure in the region place increasing pressure on these species and their habitats. During 2012-2015, we studied factors influencing the distribution of these two ungulate species in the Southern Gobi to better inform management. We built Generalized Linear Mixed Models (GLMMs) to predict the location of suitable habitat for the two species using environmental and human-associated factors. These models were validated using independent telemetry data for each species. The GLMMs, suggest that the probability of ungulate presence decreased with increasing human influence and increased in areas with intermediate values of elevation and Normalized Difference Vegetation Index (except for goitered gazelle). Notably, human-associated factors were more important than environmental variables in explaining the distribution of the two species. Habitat models predicted between 45 and 55% of the study area to be suitable for khulan and between 50 and 55% suitable for goitered gazelles during 2012-2015. Models for both species had good predictive power, as nearly 90% of khulan and 100% of goitered gazelle telemetry locations from separate data sets were found within the predicted preferred areas. Our approach quantifies the key drivers of their distribution and our findings are useful for policy makers, managers, and industry to plan mitigation measures to reduce the impacts of development. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Buuveibaatar, Bayarbaatar] Mongolia Program, Wildlife Conservat Soc, Ulaanbaatar, Mongol Peo Rep. [Buuveibaatar, Bayarbaatar; Fuller, Todd K.] Univ Massachusetts, Dept Environm Conservat, Amherst, MA 01003 USA. [Mueller, Thomas] Goethe Univ Frankfurt, Senckenberg Biodivers & Climate Res Ctr, Frankfurt, Germany. [Mueller, Thomas] Goethe Univ Frankfurt, Dept Biol Sci, Frankfurt, Germany. [Strindberg, Samantha] Global Conservat Program, Wildlife Conservat Soc, Bronx, NY USA. [Leimgruber, Peter] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Kaczensky, Petra] Univ Vet Med, Res Inst Wildlife Ecol, Vienna, Austria. RP Buuveibaatar, B (reprint author), Mongolia Program, Wildlife Conservat Soc, Ulaanbaatar, Mongol Peo Rep. EM buuveibaatar@wcs.org FU Robert Bosch Foundation; WCS FX We would like to thank B. Chimeddorj, G. Naranbaatar, T. Munkhzul, S. Amarsaikhan, B. Dashnyam, T. Purevsuren and many other field survey team members. The logistical and administrative support of A. Otgonsuren, T. Dashzeveg, S. Enlchtuvshin from Wildlife Conservation Society (WCS), B. Nyamdorj from Sustainability East Asia (SEA), and D.A. Hosack from Oyu Tolgoi (OT) is greatly appreciated. T. Mueller was funded by the Robert Bosch Foundation. Capture of khulan was made possible by C. Walzer. We are grateful to WCS for the project funding administered through a cooperative agreement with SEA and originating from OT. NR 40 TC 1 Z9 1 U1 5 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD NOV PY 2016 VL 203 BP 168 EP 175 DI 10.1016/j.biocon.2016.09.013 PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EC5EO UT WOS:000388156100020 ER PT J AU Kuntner, M Gregoric, M Cheng, RC Li, DQ AF Kuntner, Matjaz Gregoric, Matjaz Cheng, Ren-Chung Li, Daiqin TI Leaf masquerade in an orb web spider SO JOURNAL OF ARACHNOLOGY LA English DT Article DE Passive defenses; anachoresis; crypsis; Poltys; Araneidae ID ARANEIDAE CAEROSTRIS; ARANEAE ARANEIDAE; GENUS POLTYS; CAMOUFLAGE; PHYLOGENY AB Leaf masquerade-an animal resembling leaves that are inedible for predators or innocuous for prey-is well known in insects but less so in arachnids. We report a case of a striking morphological and behavioral adaptation that can be labeled as leaf masquerade in an undescribed spider species (Poltys C. L. Koch, 1843, Araneidae) from southwest China. The female abdomen has anatomical analogues of a leaf pedicel and venation, and its color is both green and brown, thus resembling both live and dry leaves. The spider camouflages itself with pulled dead leaves among live ones. This novel natural history in a spider adds an arachnid model to the growing literature on animal masquerade. C1 [Kuntner, Matjaz; Gregoric, Matjaz; Cheng, Ren-Chung] Biol Inst ZRC SAZU, Evolutionary Zool Lab, Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore, Singapore. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. RP Kuntner, M (reprint author), Biol Inst ZRC SAZU, Evolutionary Zool Lab, Ljubljana, Slovenia.; Kuntner, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA.; Kuntner, M (reprint author), Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. EM kuntner@gmail.com RI Li, Daiqin/D-6922-2013 OI Li, Daiqin/0000-0001-8269-7734 NR 28 TC 0 Z9 0 U1 5 U2 5 PU AMER ARACHNOLOGICAL SOC PI COLLEGE PARK PA UNIV MARYLAND, DEPT ENTOMOLOGY, 4112 PLANT SCIENCES BLDG, COLLEGE PARK, MD 20742-4454 USA SN 0161-8202 EI 1937-2396 J9 J ARACHNOL JI J. Arachnol. PD NOV PY 2016 VL 44 IS 3 BP 397 EP 400 PG 4 WC Entomology SC Entomology GA EC9SD UT WOS:000388483600009 ER PT J AU Grealy, A Douglass, K Haile, J Bruwer, C Gough, C Bunce, M AF Grealy, Alicia Douglass, Kristina Haile, James Bruwer, Chriselle Gough, Charlotte Bunce, Michael TI Tropical ancient DNA from bulk archaeological fish bone reveals the subsistence practices of a historic coastal community in southwest Madagascar SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Ancient DNA; Archaeology; Biodiversity; Bulk-bone; Fish; Madagascar; Metabarcoding; Subsistence ID PACIFIC-NORTHWEST COAST; BRITISH-COLUMBIA; SPECIES IDENTIFICATION; BIODIVERSITY; ASSEMBLAGES; ECOSYSTEMS; EVOLUTION; REMAINS AB Taxonomic identification of archaeological fish bones provides important insights into the subsistence practices of ancient coastal peoples. However, it can be difficult to execute robust morphological identification of fish bones from species-rich fossil assemblages, especially from post-cranial material with few distinguishing features. Fragmentation, weathering and burning further impede taxonomic identification, resulting in large numbers of unidentifiable bones from archaeological sites. This limitation can be somewhat mitigated by taking an ancient DNA (aDNA) bulk-bone metabarcoding (BBM) approach to faunal identification, where DNA from non-diagnostic bone fragments is extracted and sequenced in parallel. However, a large proportion of fishing communities (both past and present) live in tropical regions that have sub-optimal conditions for long-term aDNA preservation. To date, the BBM method has never been applied to fish bones before, or to fossils excavated from an exposed context within a tropical climate. Here, we demonstrate that morphologically indistinct bulk fish bone from the tropics can be identified by sequencing aDNA extracted from 100 to 300 ya archaeological midden material in southwest Madagascar. Despite the biases of the approach, we rapidly obtained family, genus, and species level assemblage information, and used this to describe a subset of the ichthyofauna exploited by an 18th century fishing community. We identified 23 families of fish, including benthic, pelagic, and coral dwelling fishes, suggesting a reliance on a variety of marine and brackish habitats. When possible, BBM should be used alongside osteological approaches to address the limitations of both; however, this study highlights how genetic methods can nevertheless be a valuable tool for helping resolve faunal assemblages when morphological identification is hindered by taphonomic processes, lack of adequate comparative collections, and time constraints, and can provide a temporal perspective on fish biodiversity in the context of accelerated exploitation of the marine environment. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Grealy, Alicia; Bunce, Michael] Curtin Univ, Dept Environm & Agr, Trace & Environm DNA TrEnD Lab, Perth, WA 6102, Australia. [Douglass, Kristina] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Haile, James] Univ Oxford, Res Lab Archaeol & Hist Art, PalaeoBARN, Oxford OX1 2JD, England. [Bruwer, Chriselle] Univ South Africa, Dept Anthropol & Archaeol, Pretoria, South Africa. [Bruwer, Chriselle] Arc Maps & Graph, Pretoria, South Africa. [Gough, Charlotte] Blue Ventures Conservat, London N7 9DP, England. RP Grealy, A (reprint author), Curtin Univ, Dept Environm & Agr, Trace & Environm DNA TrEnD Lab, Perth, WA 6102, Australia. EM alicia.grealy@uqconnect.edu.au FU National Science Foundation; P.E.O. Scholar Award; Yale Institute of Biospheric Studies; Yale MacMillan Centre for International and Area Studies; Yale Council on Archaeological Studies; University of Toliara; Yale University; Australian Research Council [DP160104473] FX The archaeological investigations carried out in the Velondriake Marine Protected Area, were made possible with funding from the National Science Foundation Graduate Research Fellowship Program, the P.E.O. Scholar Award, the Yale Institute of Biospheric Studies, the Yale MacMillan Centre for International and Area Studies and the Yale Council on Archaeological Studies. Research permissions were granted by the Ministere de l'Enseignement Superieur et de la Recherche Scientifique, Autorisation Numero 128/13-MESupReS/SG/DGRP and by the Centre de Documentation et de Recherche sur l'Art et les Traditions Orales Malgaches (CEDRATOM), under the auspices of the Memorandum of Understanding between the University of Toliara, under the direction of Dr. Barthelemy Manjakahery, Director of the CEDRATOM, and Yale University, under the direction of Dr. Roderick McIntosh, Professor of Anthropology. Local permission to carry out archaeological research was granted by the Office du Maire, Commune de Befandefa and by the Chefs de Fokontany of Andavadoaka, Nosy Ve, Antsaragnagnangy, Lamboara, Ampasilava and Salary. Permits for the export of archaeological materials for the purposes of laboratory analysis were granted by the Secretariat General of the Ministere de l'Artisanat de la Culture et des Patrimoines, Direction Regionale de la Culture et du Patrimoine Atsimo Andrefana, Visas de Sorties Numero 09/06-MCP/SG/DRCP.AA; Numero 05/14-MACP/SG/DRCP.AA; Numero 08/14-MACP/SG/DRCP.AA in accordance with Avis Numero 375, 02/02/1978. We acknowledge the support of the Australian Research Council Discovery Project grant DP160104473 (MB). NR 60 TC 0 Z9 0 U1 11 U2 11 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD NOV PY 2016 VL 75 BP 82 EP 88 DI 10.1016/j.jas.2016.10.001 PG 7 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA EC6LL UT WOS:000388247500007 ER PT J AU Crichton, EG Malo, C Pukazhenthi, BS Nagy, P Skidmore, JA AF Crichton, Elizabeth G. Malo, Clara Pukazhenthi, Budhan S. Nagy, Peter Skidmore, Julian A. TI Evaluation of cholesterol-treated dromedary camel sperm function by heterologous IVF and AI SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Dromedary camel; Cholesterol; Spermatozoa; Goat oocytes; IVF; AI ID LOADED CYCLODEXTRINS PRIOR; IN-VITRO FERTILIZATION; FREE HAMSTER EGGS; ZONA-FREE EGGS; BOAR SPERMATOZOA; ARTIFICIAL-INSEMINATION; IMPROVES CRYOSURVIVAL; REDUCED GLUTATHIONE; ACROSOME REACTION; POSTTHAW QUALITY AB Cholesterol (cholesterol-loaded cyclodextrins: CLC) treatment of dromedary camel sperm prior to freezing enhances cryosurvival. The present study first validated the efficacy of a heterologous zona-free goat oocyte assay (n =115 oocytes) to evaluate camel sperm function in vitro (Experiment 1: n = 6 bulls), then examined the effects of CLC treatment (1.5 mgimL CLC; CLC+) versus no treatment (0 CLC) of fresh (Experiment 2: n=4 bulls) and frozen-thawed (Experiment 3: n =5 bulls) camel sperm to penetrate, de-condense and form pro-nuclei in in vitro-matured goat oocytes. Finally, the ability of fresh 0 CLC and CLC+ sperm to fertilize in vivo was studied by artificially inseminating super-ovulated females (n = 7-9 per treatment) and examining embryo production (Experiment 4: n=4-5 bulls/treatment). Camel spermatozoa penetrated (60%) and formed pro-nuclei (33%) in goat oocytes demonstrating the utility of this heterologous system for assessing sperm function in vitro. For fresh spermatozoa, 0 CLC-treated sperm performed better than their CLC+ counterparts for all parameters measured (P< 0.05). In contrast, cryopreservation resulted in a sharp decline in sperm-oocyte interaction in 0 CLC aliquots but remained unaltered in CLC+ aliquots demonstrating a protective effect of cholesterol treatment. There was no difference between treatments in the in vitro fertilizing ability of frozen-thawed sperm or in the numbers of embryos retrieved following AI with fresh 0 CLC or CLC+ sperm. We conclude that although CLC treatment of dromedary camel sperm improves sperm motility it fails to confer an advantage to them in terms of improved in vitro sperm-oocyte interaction or in vivo fertilization under the conditions tested. (C) 2016 Elsevier B.V. All rights reserved. C1 [Crichton, Elizabeth G.; Malo, Clara; Skidmore, Julian A.] Camel Reprod Ctr, POB 79914, Dubai, U Arab Emirates. [Pukazhenthi, Budhan S.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Nagy, Peter] EICMP, Dubai, U Arab Emirates. RP Crichton, EG (reprint author), Camel Reprod Ctr, POB 79914, Dubai, U Arab Emirates. EM bethiberg@aol.com NR 57 TC 0 Z9 0 U1 5 U2 5 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 EI 1873-2232 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD NOV PY 2016 VL 174 BP 20 EP 28 DI 10.1016/j.anireprosci.2016.08.013 PG 9 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA EC3YF UT WOS:000388062300004 PM 27622555 ER PT J AU Pushpakumara, PGA Rajapakse, RC Perera, BMAO Brown, JL AF Pushpakumara, P. G. A. Rajapakse, R. C. Perera, B. M. A. O. Brown, J. L. TI Reproductive performance of the largest captive Asian elephant (Elephas maximus) population in Sri Lanka SO ANIMAL REPRODUCTION SCIENCE LA English DT Article DE Elephant; Pregnancy; Reproduction; Sex ratio; Inter-birth interval ID LOXODONTA-AFRICANA; MORTALITY; DEMOGRAPHY; PREGNANCY; BEHAVIOR; ZOOS AB The Pinnawela Elephant Orphanage (PEO) in Sri Lanka maintains one of the largest captive Asian elephant (Elephas maximus maximus) populations in the world, with a total of 79 animals (45 females and 34 males) at present. It was established in 1975 as an orphanage for rescued wild calves, and commenced natural breeding under controlled conditions when they reached breeding age. This study summarizes reproductive data of 65 live births from 38 years of records at PEO. The age at first calving (n =31) was 14.6 +/- 0.7 years, and the numbers of females giving birth two, three, four and five times were 21, 8, 4 and 2, with corresponding inter-birth intervals (IBI) of 4.9 +/- 0.3, 4.8 +/- 0.5, 7.9 +/- 1.9 and 5.7 +/- 0.5 years, respectively. Females giving birth to males (5.7 +/- 2.2 years) had longer IBIs compared to birthing female calves (4.7 +/- 1.1 years). The average gestation for 18 pregnancies with known conception dates was 667 11 days. The average birth weight was similar for male (83.1 +/- 4.6 kg; n =14) and female (82.8 +/- 8.4 kg; n = 6) calves. Sex ratio for live births was 36 male:29 female and not different from 1:1; however, more males (10/14) were born after a second parity. Calf mortality and stillbirth rates were low: 7.6% and 4.4%, respectively. This study highlights the successful breeding program at the PEO, providing baseline reproductive data that can aid in improving breeding of other elephants managed under captive conditions. (C) 2016 Elsevier B.V. All rights reserved. C1 [Pushpakumara, P. G. A.] Univ Peradeniya, Dept Farm Anim Prod & Hlth, Fac Vet Med & Anim Sci, Peradeniya, Sri Lanka. [Rajapakse, R. C.] Elephant Orphanage, Pinnawela, Sri Lanka. [Perera, B. M. A. O.] Wildlife Hlth Ctr, Peradeniya, Sri Lanka. [Brown, J. L.] Smithsonian Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. RP Pushpakumara, PGA (reprint author), Univ Peradeniya, Dept Farm Anim Prod & Hlth, Fac Vet Med & Anim Sci, Peradeniya, Sri Lanka. EM pganil@pdn.ac.lk NR 49 TC 0 Z9 0 U1 10 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4320 EI 1873-2232 J9 ANIM REPROD SCI JI Anim. Reprod. Sci. PD NOV PY 2016 VL 174 BP 93 EP 99 DI 10.1016/j.anireprosci.2016.09.010 PG 7 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA EC3YF UT WOS:000388062300013 PM 27665491 ER PT J AU Bergin, EA Du, F Cleeves, LI Blake, GA Schwarz, K Visser, R Zhang, K AF Bergin, Edwin A. Du, Fujun Cleeves, L. Ilsedore Blake, G. A. Schwarz, K. Visser, R. Zhang, K. TI HYDROCARBON EMISSION RINGS IN PROTOPLANETARY DISKS INDUCED BY DUST EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; molecular processes; planet-disk interactions; planetary systems; planets and satellites: atmospheres ID T-TAURI STARS; LY-ALPHA RADIATION; CIRCUMSTELLAR DISKS; DM-TAURI; MOLECULAR CLOUDS; ALMA OBSERVATIONS; H-2 FLUORESCENCE; PLANETARY SYSTEM; GRAIN-GROWTH; SOLAR NEBULA AB We report observations of resolved C2H emission rings within the gas-rich protoplanetary disks of TW Hya and DM Tau using the Atacama Large Millimeter Array. In each case the emission ring is found to arise at the edge of the observable disk of millimeter-sized grains (pebbles) traced by submillimeter-wave continuum emission. In addition, we detect a C3H2 emission ring with an identical spatial distribution to C2H in the TW. Hya disk. This suggests that these are hydrocarbon rings (i.e., not limited to C2H). Using a detailed thermo-chemical model we show that reproducing the emission from C2H requires a strong UV field and C/O > 1 in the upper disk atmosphere and outer disk, beyond the edge of the pebble disk. This naturally arises in a disk where the ice-coated dust mass is spatially stratified due to the combined effects of coagulation, gravitational settling and drift. This stratification causes the disk surface and outer disk to have a greater permeability to UV photons. Furthermore the concentration of ices that transport key volatile carriers of oxygen and carbon in the midplane, along with photochemical erosion of CO, leads to an elemental C/O ratio that exceeds unity in the UV-dominated disk. Thus the motions of the grains, and not the gas, lead to a rich hydrocarbon chemistry in disk surface layers and in the outer disk midplane. C1 [Bergin, Edwin A.; Du, Fujun; Schwarz, K.; Zhang, K.] Univ Michigan, Dept Astron, 311 West Hall,1085 S Univ Ave, Ann Arbor, MI 48109 USA. [Cleeves, L. Ilsedore] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, MC 150-21,1200 E Calif Blvd, Pasadena, CA 91125 USA. [Visser, R.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. RP Bergin, EA (reprint author), Univ Michigan, Dept Astron, 311 West Hall,1085 S Univ Ave, Ann Arbor, MI 48109 USA. RI zhang, ke/A-3898-2009; OI zhang, ke/0000-0002-0661-7517; Cleeves, L. Ilsedore/0000-0003-2076-8001 FU National Science Foundation [AST-1514670, AST-1344133]; NASA XRP grant [NNX16AB48G] FX This work was supported by funding from the National Science Foundation grant AST-1514670 and AST-1344133 (INSPIRE) along with NASA XRP grant NNX16AB48G. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00198.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 109 TC 2 Z9 2 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 101 DI 10.3847/0004-637X/831/1/101 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC0KD UT WOS:000387788600044 ER PT J AU Li, G Holman, MJ Tao, M AF Li, Gongjie Holman, Matthew J. Tao, Molei TI UNCOVERING CIRCUMBINARY PLANETARY ARCHITECTURAL PROPERTIES FROM SELECTION BIASES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; celestial mechanics; planetary systems ID DYNAMICAL MASS ESTIMATE; SOLAR-TYPE STARS; HIGH-INCLINATION; EXTRASOLAR PLANETS; BINARY-SYSTEMS; 3-BODY PROBLEM; KEPLER; ORBITS; STABILITY; EVOLUTION AB Studying newly discovered circumbinary planetary systems improves our understanding of planetary system formation. Learning the architectural properties of these systems is essential for constraining the different formation mechanisms. We first revisit the stability limit of circumbinary planets. Next, we focus on eclipsing stellar binaries and obtain an analytical expression for the transit probability in a realistic setting, where a finite observation period and planetary orbital precession are included. Our understanding of the architectural properties of the currently observed transiting systems is then refined, based on Bayesian analysis and a series of tested hypotheses. We find that (1) it is not a selection bias that the innermost planets reside near the stability limit for eight of the nine observed systems, and this pile-up is consistent with a log uniform distribution of the planetary semimajor axis; (2) it is not a selection bias that the planetary and stellar orbits are nearly coplanar (less than or similar to 3 degrees), and this-along with previous studies-may imply an occurrence rate of circumbinary planets similar to that of single star systems; (3) the dominance of observed circumbinary systems with only one transiting planet may be caused by selection effects; (4) formation mechanisms involving Lidov-Kozai oscillations, which may produce misalignment and large separation between planets and stellar binaries, are consistent with the lack of transiting circumbinary planets around short-period stellar binaries, in agreement with previous studies. As a consequence of (4), eclipse timing variations may better suit the detection of planets in such configurations. C1 [Li, Gongjie; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Tao, Molei] Georgia Inst Technol, Sch Math, 686 Cherry St, Atlanta, GA 30332 USA. RP Li, G (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. OI Li, Gongjie/0000-0001-8308-0808 FU NSF [DMS-1521667]; Harvard William F Milton Award FX The authors would like to thank the anonymous referee for giving constructive comments that substantially improved the quality of this paper. In addition, the authors would like to thank Yanqin Wu and Josh Winn for helpful discussions. This work and M.T. were supported in part by NSF DMS-1521667. G.L. was supported in part by Harvard William F Milton Award. NR 79 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 96 DI 10.3847/0004-637X/831/1/96 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC0KD UT WOS:000387788600039 ER PT J AU Rodriguez, JE Stassun, KG Cargile, P Shappee, BJ Siverd, RJ Pepper, J Lund, MB Kochanek, CS James, D Kuhn, RB Beatty, TG Gaudi, BS Weintraub, DA Stanek, KZ Holoien, TWS Prieto, JL Feldman, DM Espaillat, CC AF Rodriguez, Joseph E. Stassun, Keivan G. Cargile, Phillip Shappee, Benjamin J. Siverd, Robert J. Pepper, Joshua Lund, Michael B. Kochanek, Christopher S. James, David Kuhn, Rudolf B. Beatty, Thomas G. Gaudi, B. Scott Weintraub, David A. Stanek, Krzysztof Z. Holoien, Thomas W. -S. Prieto, Jose L. Feldman, Daniel M. Espaillat, Catherine C. TI DM ORI: A YOUNG STAR OCCULTED BY A DISTURBANCE IN ITS PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (DM Ori); stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be ID T-TAURI STARS; RW AURIGAE; MAGNETOSPHERIC ACCRETION; CIRCUMSTELLAR DISK; SPECTRAL-ANALYSIS; EPSILON-AURIGAE; SPACED DATA; AA TAURI; NGC 2264; VARIABILITY AB In some planet formation theories, protoplanets grow gravitationally within a young star's protoplanetary disk, a signature of which may be a localized disturbance in the disk's radial and/or vertical structure. Using time-series photometric observations by the Kilodegree Extremely Little Telescope South project and the All-Sky Automated Survey for SuperNovae, combined with archival observations, we present the discovery of two extended dimming events of the young star, DM Ori. This young system faded by similar to 1.5 mag from 2000 March to 2002 August and then again in 2013 January until 2014 September (depth similar to 1.7 mag). We constrain the duration of the 2000-2002 dimming to be < 860 days, and the event in 2013-2014 to be < 585 days, separated by similar to 12.5 years. A model of the spectral energy distribution indicates a large infrared excess consistent with an extensive circumstellar disk. Using basic kinematic arguments, we propose that DM Ori is likely being periodically occulted by a feature (possibly a warp or perturbation) in its circumstellar disk. In this scenario, the occulting feature is located >6 au from the host star, moving at similar to 14.6 km s(-1). and is similar to 4.9 au in width. This localized structure may indicate a disturbance such as that which. may be caused by a protoplanet early in its formation. C1 [Rodriguez, Joseph E.; Stassun, Keivan G.; Lund, Michael B.; Weintraub, David A.] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, 1000 17th Ave North, Nashville, TN 37208 USA. [Cargile, Phillip] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Shappee, Benjamin J.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Siverd, Robert J.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA. [Pepper, Joshua] Lehigh Univ, Dept Phys, 16 Mem Dr East, Bethlehem, PA 18015 USA. [Kochanek, Christopher S.; Gaudi, B. Scott; Stanek, Krzysztof Z.; Holoien, Thomas W. -S.] Ohio State Univ, Dept Astron, 174 W 18th Ave, Columbus, OH 43210 USA. [Kochanek, Christopher S.; Stanek, Krzysztof Z.; Holoien, Thomas W. -S.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, 191 W Woodruff Ave, Columbus, OH 43210 USA. [James, David] Cerro Tololo InterAmer Observ, Casilla 603, La Serena, Chile. [Kuhn, Rudolf B.] South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa. [Beatty, Thomas G.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Beatty, Thomas G.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA. [Prieto, Jose L.] Univ Diego Portales, Fac Ingn, Av Ejercito 441, Santiago, Chile. [Prieto, Jose L.] Millennium Inst Astrophys, Santiago, Chile. [Feldman, Daniel M.; Espaillat, Catherine C.] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. RP Rodriguez, JE (reprint author), Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA. OI Rodriguez, Joseph/0000-0001-8812-0565; Pepper, Joshua/0000-0002-3827-8417; Stassun, Keivan/0000-0002-3481-9052 FU NASA [NNG04GO70G, NAS 5-26555, NNX13AI46G]; Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics; NSF CAREER Grant [AST-1056524]; NSF PAARE grant [AST-1358862]; NASA - Space Telescope Science Institute [HF-51348.001]; NSF [AST-1515876, AST-1515927, AST-0908816]; DOE Computational Science Graduate Fellowship [DE-FG02-97ER25308]; National Aeronautics and Space Administration [NNG05GF22G]; U.S. National Science Foundation [AST-0909182, AST-1313422]; CCAPP at the Ohio State University; Center for Cosmology and AstroParticle Physics (CCAPP) at OSU; Mt. Cuba Astronomical Foundation; Robert Martin Ayers Sciences Fund FX Early work on KELT-North was supported by NASA Grant NNG04GO70G. J.A.P. and K.G.S. acknowledge support from the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics. This work has made use of NASA's Astrophysics Data System and the SIMBAD database operated at CDS, Strasbourg, France.; Work by BSG was partially supported by NSF CAREER Grant AST-1056524. Work by K.G.S. was supported by NSF PAARE grant AST-1358862. B.J.S. is supported by NASA through Hubble Fellowship grant HF-51348.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. C.S.K. and K.Z.S. are supported by NSF grants AST-1515876 and AST-1515927. T.W.-S.H. is supported by the DOE Computational Science Graduate Fellowship, grant number DE-FG02-97ER25308. P.C. is supported by the NASA grant NNX13AI46G.; The CSS survey is funded by the National Aeronautics and Space Administration under grant No. NNG05GF22G issued through the Science Mission Directorate Near-Earth Objects Observations Program. The CRTS survey is supported by the U.S. National Science Foundation under grants AST-0909182 and AST-1313422.; Development of ASAS-SN has been supported by NSF grant AST-0908816 and CCAPP at the Ohio State University. ASAS-SN is supported by NSF grant AST-1515927, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Mt. Cuba Astronomical Foundation, George Skestos, and the Robert Martin Ayers Sciences Fund. NR 59 TC 1 Z9 1 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 74 DI 10.3847/0004-637X/831/1/74 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC0KD UT WOS:000387788600017 ER PT J AU Bayliss, MB Ruel, J Stubbs, CW Allen, SW Applegate, DE Ashby, MLN Bautz, M Benson, BA Bleem, LE Bocquet, S Brodwin, M Capasso, R Carlstrom, JE Chang, CL Chiu, I Cho, HM Clocchiatti, A Crawford, TM Crites, AT de Haan, T Desai, S Dietrich, JP Dobbs, MA Doucouliagos, AN Foley, RJ Forman, WR Garmire, GP George, EM Gladders, MD Gonzalez, AH Gupta, N Halverson, NW Hlavacek-Larrondo, J Hoekstra, H Holder, GP Holzapfel, WL Hou, Z Hrubes, JD Huang, N Jones, C Keisler, R Knox, L Lee, AT Leitch, EM von der Linden, A Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Meyer, SS Mocanu, LM Mohr, JJ Murray, SS Padin, S Pryke, C Rapetti, D Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Schrabback, T Shirokoff, E Song, J Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, KT Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zenteno, A AF Bayliss, M. B. Ruel, J. Stubbs, C. W. Allen, S. W. Applegate, D. E. Ashby, M. L. N. Bautz, M. Benson, B. A. Bleem, L. E. Bocquet, S. Brodwin, M. Capasso, R. Carlstrom, J. E. Chang, C. L. Chiu, I. Cho, H-M. Clocchiatti, A. Crawford, T. M. Crites, A. T. de Haan, T. Desai, S. Dietrich, J. P. Dobbs, M. A. Doucouliagos, A. N. Foley, R. J. Forman, W. R. Garmire, G. P. George, E. M. Gladders, M. D. Gonzalez, A. H. Gupta, N. Halverson, N. W. Hlavacek-Larrondo, J. Hoekstra, H. Holder, G. P. Holzapfel, W. L. Hou, Z. Hrubes, J. D. Huang, N. Jones, C. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. von der Linden, A. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Meyer, S. S. Mocanu, L. M. Mohr, J. J. Murray, S. S. Padin, S. Pryke, C. Rapetti, D. Reichardt, C. L. Rest, A. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Schrabback, T. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. T. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zenteno, A. TI SPT-GMOS: A GEMINI/GMOS-SOUTH SPECTROSCOPIC SURVEY OF GALAXY CLUSTERS IN THE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: clusters: general; galaxies: distances and redshifts; techniques: spectroscopic ID POLE TELESCOPE SURVEY; GRAVITATIONALLY LENSED GALAXY; DIGITAL SKY SURVEY; LYMAN-BREAK GALAXIES; SIMILAR-TO 2; ZELDOVICH EFFECT SURVEY; REGION NEARBY SURVEY; 720 SQUARE DEGREES; GIANT ARCS SURVEY; GREATER-THAN 1 AB We present the results of SPT-GMOS, a spectroscopic survey with the Gemini Multi-Object Spectrograph (GMOS) on Gemini South. The targets of SPT-GMOS are galaxy clusters identified in the SPT-SZ survey, a millimeter-wave survey of 2500 deg(2) of the southern sky using the South Pole Telescope (SPT). Multi-object spectroscopic observations of 62 SPT-selected galaxy clusters were performed between 2011 January and 2015 December, yielding spectra with radial velocity measurements for 2595 sources. We identify 2243 of these sources as galaxies, and 352 as stars. Of the galaxies, we identify 1579 as members of SPT-SZ galaxy clusters. The primary goal of these observations was to obtain spectra of cluster member galaxies to estimate cluster redshifts and velocity dispersions. We describe the full spectroscopic data set and resulting data products, including galaxy redshifts, cluster redshifts, and velocity dispersions, and measurements of several well-known spectral indices for each galaxy: the equivalent width, W, of [O II] lambda lambda 3727, 3729 and H-delta, and the 4000 angstrom break strength, D4000. We use the spectral indices to classify galaxies by spectral type (i.e., passive, post-starburst, star-forming), and we match the spectra against photometric catalogs to characterize spectroscopically observed cluster members as a function of brightness (relative to m*). Finally, we report several new measurements of redshifts for ten bright, strongly lensed background galaxies in the cores of eight galaxy clusters. Combining the SPT-GMOS data set with previous spectroscopic follow-up of SPT-SZ galaxy clusters results in spectroscopic measurements for >100 clusters, or similar to 20% of the full SPT-SZ sample. C1 [Bayliss, M. B.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Bayliss, M. B.; Stubbs, C. W.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Bayliss, M. B.] Colby Coll, Dept Phys & Astron, 5100 Mayflower Hill Dr, Waterville, ME 04901 USA. [Allen, S. W.; Keisler, R.; von der Linden, A.; Mantz, A.; Story, K. T.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. [Allen, S. W.; Hlavacek-Larrondo, J.; Keisler, R.; von der Linden, A.; Mantz, A.; Story, K. T.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. [Applegate, D. E.; Schrabback, T.] Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Clocchiatti, A.; Crawford, T. M.; Gladders, M. D.; Leitch, E. M.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Shirokoff, E.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Benson, B. A.; Bleem, L. E.; Bocquet, S.; Carlstrom, J. E.; Chang, C. L.; Clocchiatti, A.; Crawford, T. M.; Gladders, M. D.; Hou, Z.; Keisler, R.; Leitch, E. M.; Mantz, A.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Rest, A.; Schaffer, K. K.; Shirokoff, E.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Bleem, L. E.; Carlstrom, J. E.; Clocchiatti, A.; Hou, Z.; Keisler, R.; Meyer, S. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Bocquet, S.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Aty 8rgonne, Argonne, IL 60439 USA. [Bocquet, S.; Capasso, R.; Chiu, I.; Clocchiatti, A.; Dietrich, J. P.; Gupta, N.; Mohr, J. J.; Rapetti, D.; Saro, A.] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Bocquet, S.; Capasso, R.; Chiu, I.; Dietrich, J. P.; Gupta, N.; Mohr, J. J.; Rapetti, D.; Saro, A.] Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, 5110 Rockhill Rd, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H-M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrosifis, Santiago, Region Metropol, Chile. [Crites, A. T.; Padin, S.; Williamson, R.] CALTECH, Pasadena, CA 91125 USA. [de Haan, T.; George, E. M.; Holzapfel, W. L.; Huang, N.; Lee, A. T.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Dobbs, M. A.] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada. [Doucouliagos, A. N.; Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Vieira, J. D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Garmire, G. P.] Huntingdon Inst Xray Astron LLC, Huntingdon, PA USA. [George, E. M.; Mohr, J. J.] Max Planck Inst Extraterrestrial Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.; Sayre, J. T.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.; Sayre, J. T.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hlavacek-Larrondo, J.] Univ Montreal, Dept Phys, Montreal, PQ H3T 1J4, Canada. [Hlavacek-Larrondo, J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [von der Linden, A.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [von der Linden, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen, Denmark. [Marrone, D. P.] Univ Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Song, J.] Korea Astron & Space Sci Inst, Daejeon 305348, South Korea. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. [Zenteno, A.] Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Desai, S.] IIT Hyderabad, Dept Phys, Sangareddy 502285, Telangana, India. [Foley, R. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Bayliss, MB (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA.; Bayliss, MB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Bayliss, MB (reprint author), Colby Coll, Dept Phys & Astron, 5100 Mayflower Hill Dr, Waterville, ME 04901 USA. EM mbbayliss@cfa.harvard.edu OI Bocquet, Sebastian/0000-0002-4900-805X; Stubbs, Christopher/0000-0003-0347-1724; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [AST-1009012, PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; NSF [AST-1009649, MRI-0723073]; Alfred P. Sloan Foundation; U.S. Department of Energy [DE-AC02-06CH11357]; Fermi Research Alliance, LLC [DE-AC02-07CH11359]; United States Department of Energy; NASA through Space Telescope Science Institute [HST-GO-13412.004-A]; NASA [NAS 5-26555]; [GS-2011A-C-03]; [GS-2011A-C-04]; [GS-2011B-C-06]; [GS-2011B-C-33]; [GS-2012A-Q-04]; [GS-2012A-Q-37]; [GS-2012B-Q-29]; [GS-2012B-Q-59]; [GS-2013A-Q-05]; [GS-2013A-Q-45]; [GS-2013B-Q-25]; [GS-2013B-Q-72]; [GS-2014B-Q-31]; [GS-2014B-Q-64]; [13412] FX We thank the anonymous referee for helpful and thoughtful feedback that improved this paper. This work is supported by the National Science Foundation through Grant AST-1009012. The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support was also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. R.J.F. gratefully acknowledges support from the Alfred P. Sloan Foundation. Argonne National Laboratory work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. BB is supported by the Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the United States Department of Energy. Support for program #HST-GO-13412.004-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.; The data presented here were taken with the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: The United States, Canada, Chile, Australia, Brazil, and Argentina. Gemini data used in this work was taken as a part of the following Gemini programs: GS-2011A-C-03, GS-2011A-C-04, GS-2011B-C-06, GS-2011B-C-33, GS-2012A-Q-04, GS-2012A-Q-37, GS-2012B-Q-29, GS-2012B-Q-59, GS-2013A-Q-05, GS-2013A-Q-45, GS-2013B-Q-25, GS-2013B-Q-72, GS-2014B-Q-31, and GS-2014B-Q-64. Additional supporting data were obtained with the 6.5m Magellan Telescopes, which are located at the Las Campanas Observatory in Chile. This work is also partly based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555; these observations are associated with program #13412. NR 111 TC 0 Z9 0 U1 6 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD NOV PY 2016 VL 227 IS 1 AR 3 DI 10.3847/0067-0049/227/1/3 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC5VO UT WOS:000388205600002 ER PT J AU Pomar, L Haq, BU AF Pomar, Luis Haq, Bilal U. TI Decoding depositional sequences in carbonate systems: Concepts vs experience SO GLOBAL AND PLANETARY CHANGE LA English DT Review ID CORALLINE RED ALGAE; SEA-LEVEL CHANGES; INTERNAL WAVES; HIGH-FREQUENCY; UPPER MIOCENE; FACIES ARCHITECTURE; IBERIAN BASIN; NORTH-SEA; NE SPAIN; STRATIGRAPHIC SEQUENCES AB Efficacy of sequence stratigraphic concepts in siliciclastic systems has been proven by successful applications in both academia and the industry over the past four decades. However, experience has demonstrated repeatedly that the relatively simple advective transportational approach of these models is less than successful when applied to the more complex carbonate systems and can lead to erroneous interpretations. Instead, an approach that includes the use of the changes in the biotic components of carbonate deposits to infer the sea-level trajectory and thereby placing it in the proper sequence framework is deemed to be more meaningful. This is exemplified with several well-studied examples that illustrate the variety of ways in which the biotic components can build carbonate platforms, and how these have changed through the ages prompted by biological evolution. This extended review discusses carbonate production, source to sink transportation influenced by sea-level changes, surface waves, as well as the less understood and under-appreciated internal waves, and the resulting variety of platforms that can be built by the interaction of these factors, as well as the changing patterns of biotic components with time. Their effect on the carbonate reservoir is considerable, understanding of which is the ultimate objective of carbonate research for applications in the industry. Key elements in the carbonate environments that differ from the siliciclastic systems are: 1) intrabasinal conditions (nutrients, salinity, temperature, water energy, transparency) are important controls on carbonate production and therefore also control in-situ accommodation and how it may be filled; 2) depositional accommodation can be both physical (controlled by hydrodynamics) and ecological (in the building-up above the base level mode); 3) because carbonates are products of biological activity, their production modes have been changing with time as their biotic components have evolved; 4) seafloor morphology determines the size and efficiency of the carbonate factory; 5) several carbonate factories may coexist or alternate, in-phase, out-of-phase with or independently of the sea level changes. The complexity and interplay of all of these governing factors contribute to very diverse carbonate production styles and edifices. Consequently, sequence-stratigraphic interpretations in carbonates are more meaningful when seen through the lens of process-product relationships, rather than simply through bedding patterns and bounding surfaces characterization. (C) 2016 Elsevier B.V. All rights reserved. C1 [Pomar, Luis] Univ Balearic Isl, Palma De Mallorca, Spain. [Haq, Bilal U.] Smithsonian Inst, Washington, DC 20560 USA. [Haq, Bilal U.] Univ Paris 06, Sorbonne, Paris, France. RP Haq, BU (reprint author), Smithsonian Inst, Washington, DC 20560 USA.; Haq, BU (reprint author), Univ Paris 06, Sorbonne, Paris, France. EM bhaq@inbox.com OI Pomar, Luis/0000-0001-7074-3959 FU Spanish Ministerio de Economia y Competitividad [CGL2014-52096-P] FX Funding from Spanish Ministerio de Economia y Competitividad Project CGL2014-52096-P is acknowledged. This paper represents a long process of evolution of ideas, to which many of our colleagues have contributed. Jim Hendry (Tullow Oil), and Chris Kendall have brought alive some of the ideas developed here in previous publications. Comments and suggestions by Christian Gorini and an anonymous reviewer also contributed to the improvement of the manuscript. NR 222 TC 1 Z9 1 U1 3 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 EI 1872-6364 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD NOV PY 2016 VL 146 BP 190 EP 225 DI 10.1016/j.gloplacha.2016.10.001 PG 36 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EC3TR UT WOS:000388049700016 ER PT J AU Montanez, IP McElwain, JC Poulsen, CJ White, JD DiMichele, WA Wilson, JP Griggs, G Hren, MT AF Montanez, Isabel P. McElwain, Jennifer C. Poulsen, Christopher J. White, Joseph D. DiMichele, William A. Wilson, Jonathan P. Griggs, Galen Hren, Michael T. TI Climate, p(CO2) and terrestrial carbon cycle linkages during late Palaeozoic glacial-interglacial cycles SO NATURE GEOSCIENCE LA English DT Article ID TRANSFER SCHEME LSX; ATMOSPHERIC CO2; ICE-AGE; FOSSIL CUTICLE; RECORD; MODEL; LEAVES; SEQUESTRATION; PLEISTOCENE; TEMPERATURE AB Earth's last icehouse, 300 million years ago, is considered the longest-lived and most acute of the past half-billion years, characterized by expansive continental ice sheets(1,2) and possibly tropical low-elevation glaciation(3). This atypical climate has long been attributed to anomalous radiative forcing promoted by a 3% lower incident solar luminosity(4) and sustained low atmospheric p(CO2) (<= 300 ppm)(5). Climate models(6), however, indicate a CO2 sensitivity of ice-sheet distribution and sea-level response that questions this long-standing climate paradigm by revealing major discrepancy between hypothesized ice distribution, pCO(2), andgeologic records of glacioeustasy(2,6). Here we present a high-resolution record of atmospheric pCO(2) for 16 million years of the late Palaeozoic, developed using soil carbonate-based and fossil leaf-based proxies, that resolves the climate conundrum. Palaeo-fluctuations on the 10(5)-yr scale occur within the CO2 range predicted for anthropogenic change and co-vary with substantial change in sea level and ice volume. We further document coincidence between pCO(2) changes and repeated restructuring of Euramerican tropical forests that, in conjunction with modelled vegetation shifts, indicate a more dynamic carbon sequestration history than previously considered(7,8) and a major role for terrestrial vegetation-CO2 feedbacks in driving eccentricity-scale climate cycles of the late Palaeozoic icehouse. C1 [Montanez, Isabel P.; Griggs, Galen] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [McElwain, Jennifer C.] Univ Coll Dublin, Sch Biol & Environm Sci, Earth Inst, Dublin 4, Ireland. [Poulsen, Christopher J.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA. [White, Joseph D.] Baylor Univ, Dept Biol, Waco, TX 76798 USA. [DiMichele, William A.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Wilson, Jonathan P.] Haverford Coll, Dept Biol, Haverford, PA 19041 USA. [Hren, Michael T.] Univ Connecticut, Ctr Integrat Geosci, Storrs, CT 06269 USA. RP Montanez, IP (reprint author), Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA.; McElwain, JC (reprint author), Univ Coll Dublin, Sch Biol & Environm Sci, Earth Inst, Dublin 4, Ireland. EM ipmontanez@ucdavis.edu; Jennifer.McElwain@ucd.ie FU NSF [EAR-1338281, EAR-1338200, EAR-1338247, EAR-1338256]; ERC; [279962-OXYEVOL] FX We thank D. Breecker for discussion and comments on this work, and R. Barclay, J. Antognini, D. Garello, A. Byrd, R. Chen, C. Marquardt and D. Rauh for assistance in the research, D. Horton for access to palaeoclimate model results, and N. Tabor for a subset of stable isotopic analyses. This work was funded by NSF grants EAR-1338281 (I.P.M.), EAR-1338200 (C.J.P.), EAR-1338247 (J.D.W.), and EAR-1338256 (M.T.H.), and ERC-2011-StG and 279962-OXYEVOL to J.C.M. NR 59 TC 2 Z9 2 U1 14 U2 14 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD NOV PY 2016 VL 9 IS 11 BP 824 EP + DI 10.1038/ngeo2822 PG 8 WC Geosciences, Multidisciplinary SC Geology GA EB9ME UT WOS:000387718200009 ER PT J AU Pineda-Munoz, S Evans, AR Alroy, J AF Pineda-Munoz, Silvia Evans, Alistair R. Alroy, John TI The relationship between diet and body mass in terrestrial mammals SO PALEOBIOLOGY LA English DT Article ID FOSSIL MAMMALS; CLIMATE-CHANGE; COPES RULE; SIZE; HERBIVORES; EVOLUTION; PATTERNS; DISTRIBUTIONS; ENVIRONMENT; CENOGRAMS AB Diet and body mass are highly important factors in mammalian ecology, and they have also proven to be powerful paleoecological indicators. Our previous research has proposed a new classification scheme for mammals with more dietary divisions that emphasizes the primary resource in a given diet. We analyzed a database summarizing the dietary preferences of 139 species of marsupial and placental terrestrial mammals (including 14 orders) and their average body masses in order to explore whether this new classification better highlights ecomorphological differences between species. Additionally, the dietary diversity of every species in the data set was quantified by applying the inverse Simpson index to stomach content percentages. We observed a decrease in maximum dietary diversity with increasing body mass. Having lower requirements for energy and nutrients per unit of body weight or ecological advantages such as larger home ranges allows larger mammals to feed on less nutritive feeding resources (i.e., structural plant material). Our results also suggest that body-size ranges are different across dietary specializations. Smaller mammals (<1 kg) are mainly insectivores, granivores, or mixed feeders, while bigger animals (>30 kg) are usually either carnivores or herbivores that feed specifically on grasses and leaves. The medium-size range (1-30 kg) is mostly composed of frugivorous species that inhabit tropical and subtropical rain forests. Thus, the near absence of medium-sized mammals in open environments such as savannas can be linked to the decreasing density of fruit trees needed to support a pure frugivorous diet year-round. In other words, seasonality of precipitation prevents species from specializing on a totally frugivorous diet. Our results suggest that this new classification scheme correlates well with body mass, one of the most studied morphological variables in paleoecology and ecomorphology. Therefore, the classification should serve as a useful basis for future paleoclimatological studies. C1 [Pineda-Munoz, Silvia; Alroy, John] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. [Pineda-Munoz, Silvia] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Evans, Alistair R.] Monash Univ, Sch Biol Sci, Clayton, Vic 3800, Australia. RP Pineda-Munoz, S (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia.; Pineda-Munoz, S (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. EM silvia.pineda-munoz@students.mq.edu.au; arevans@fastmail.fm; john.alroy@mq.edu.au RI Evans, Alistair/D-4239-2011 OI Evans, Alistair/0000-0002-4078-4693 FU Macquarie University's HDR Project Support Funds; Peter Buck Predoctoral Research Fellowship from Smithsonian NMNH; Australian Research Council; Monash University FX We thank M. McCurry and Xuan Zhu for assistance with GIS analysis. We also thank Nick Chan, David M. Alba, colleagues at Macquarie University and National Museum of Natural History Smithsonian Institution, and two anonymous reviewers for comments and suggestions. S.P.-M. was supported by Macquarie University's HDR Project Support Funds and a Peter Buck Predoctoral Research Fellowship from Smithsonian NMNH. A.E. acknowledges the support of the Australian Research Council and Monash University. This is the Evolution of Terrestrial Ecosystems Program publication number 339. NR 58 TC 0 Z9 0 U1 12 U2 12 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD NOV PY 2016 VL 42 IS 4 BP 659 EP 669 DI 10.1017/pab.2016.6 PG 11 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA EC2PO UT WOS:000387966000007 ER PT J AU Raouafi, NE Patsourakos, S Pariat, E Young, PR Sterling, AC Savcheva, A Shimojo, M Moreno-Insertis, F DeVore, CR Archontis, V Torok, T Mason, H Curdt, W Meyer, K Dalmasse, K Matsui, Y AF Raouafi, N. E. Patsourakos, S. Pariat, E. Young, P. R. Sterling, A. C. Savcheva, A. Shimojo, M. Moreno-Insertis, F. DeVore, C. R. Archontis, V. Torok, T. Mason, H. Curdt, W. Meyer, K. Dalmasse, K. Matsui, Y. TI Solar Coronal Jets: Observations, Theory, and Modeling SO SPACE SCIENCE REVIEWS LA English DT Review DE Plasmas; Sun: activity; Sun: corona; Sun: magnetic fields; Sun: UV radiation; Sun: X-rays ID X-RAY JETS; ENERGETIC PARTICLE EVENTS; H-ALPHA SURGES; MAGNETIC RECONNECTION MODEL; MICHELSON DOPPLER IMAGER; TRANSITION REGION; MASS EJECTIONS; FLUX EMERGENCE; PHYSICAL PARAMETERS; BLOWOUT JET AB Coronal jets represent important manifestations of ubiquitous solar transients, which may be the source of significant mass and energy input to the upper solar atmosphere and the solar wind. While the energy involved in a jet-like event is smaller than that of "nominal" solar flares and coronal mass ejections (CMEs), jets share many common properties with these phenomena, in particular, the explosive magnetically driven dynamics. Studies of jets could, therefore, provide critical insight for understanding the larger, more complex drivers of the solar activity. On the other side of the size-spectrum, the study of jets could also supply important clues on the physics of transients close or at the limit of the current spatial resolution such as spicules. Furthermore, jet phenomena may hint to basic process for heating the corona and accelerating the solar wind; consequently their study gives us the opportunity to attack a broad range of solar-heliospheric problems. C1 [Raouafi, N. E.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. [Patsourakos, S.] Univ Ioannina, Dept Phys, Ioannina, Greece. [Pariat, E.; Dalmasse, K.] Observ Paris, LESIA, Meudon, France. [Young, P. R.] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA. [Young, P. R.] NASA Goddard Space Flight Ctr, Code 671, Greenbelt, MD 20771 USA. [Sterling, A. C.] NASA Marshall Space Flight Ctr, Huntsville, AL USA. [Savcheva, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Shimojo, M.] Natl Astron Observ Japan, Mitaka, Tokyo, Japan. [Moreno-Insertis, F.] Inst Astrofis Canarias, Tenerife, Spain. [DeVore, C. R.] NASA Goddard Space Flight Ctr, Heliophys Sci Div, Greenbelt, MD USA. [Archontis, V.] Univ St Andrews, Sch Math & Stat, St Andrews, Fife, Scotland. [Torok, T.] Predict Sci Inc, 9990 Mesa Rim Rd,Ste 170, San Diego, CA 92121 USA. [Mason, H.] Univ Cambridge, Ctr Math Sci, DAMTP, Cambridge, England. [Curdt, W.] Max Planck Inst Sonnensyst Forsch, Gottingen, Germany. [Meyer, K.] Abertay Univ, Div Comp & Math, Dundee, Scotland. [Dalmasse, K.] NCAR, CISL HAO, POB 3000, Boulder, CO 80307 USA. [Matsui, Y.] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo, Japan. RP Raouafi, NE (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM NourEddine.Raouafi@jhuapl.edu RI Shimojo, Masumi/J-2605-2016 OI Shimojo, Masumi/0000-0002-2350-3749 FU FP7 Marie Curie Grant [FP7-PEOPLE-2010-RG/268288]; European Union (European Social Fund-ESF); Greek national funds through the Operational Program "Education and Lifelong Learning" of the National Strategic Reference Framework (NSRF)-Research Funding Program: Thales; Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program; Hinode Project Office at NASA/MSFC; National Science Foundation [AGS-1159353]; NASA; Computational and Information Systems Laboratory; HAO; AFOSR [FA9550-15-1-0030]; Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract FX The "Solar Jets" team members are grateful for the International Space Science Institute (ISSI, Bern, Switzerland) that hosted two meetings on March 2013 and March 2014 within the frame of the international team on the "Solar Coronal Jets (http://www.issibern.ch/teams/solarjets)". This work benefited greatly from discussions held at these meetings. S. Patsourakos acknowledges support from an FP7 Marie Curie Grant (FP7-PEOPLE-2010-RG/268288) as well as European Union (European Social Fund-ESF) and Greek national funds through the Operational Program" Education and Lifelong Learning" of the National Strategic Reference Framework (NSRF)-Research Funding Program: Thales. Investing in knowledge society through the European Social Fund. A.C. Sterling thanks R.L. Moore for useful discussions. A.C. Sterling was supported by funding from the Heliophysics Division of NASA's Science Mission Directorate through the Living With a Star Targeted Research and Technology Program, and by funding from the Hinode Project Office at NASA/MSFC. P.R. Young acknowledges funding from National Science Foundation grant AGS-1159353. T. Torok was supported by NASA's HSR and LWS programs. K. Dalmasse acknowledges support from the Computational and Information Systems Laboratory and from the HAO, as well as support from the AFOSR under award FA9550-15-1-0030.; The SOHO is a mission of international cooperation between ESA and NASA. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as a domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with the ESA and NSC (Norway). The STEREO/SECCHI data used here are produced by an international consortium of the NRL (USA), LM-SAL (USA), NASA GSFC (USA), RAL (UK), Univ. Birmingham (UK), MPS (Germany), CSL (Belgium), IOTA (France), and IAS (France). SDO is the first mission to be launched for NASA's Living With a Star (LWS) Program. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. NR 219 TC 5 Z9 5 U1 12 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD NOV PY 2016 VL 201 IS 1-4 BP 1 EP 53 DI 10.1007/s11214-016-0260-5 PG 53 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EC0DE UT WOS:000387767300001 ER PT J AU Evans, MEK Merow, C Record, S McMahon, SM Enquist, BJ AF Evans, Margaret E. K. Merow, Cory Record, Sydne McMahon, Sean M. Enquist, Brian J. TI Towards Process-cased Range Modeling of Many Species SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID INTEGRAL PROJECTION MODELS; CLIMATE-CHANGE; ENVIRONMENTAL-CHANGE; FUNCTIONAL TRAITS; BIOTIC INTERACTIONS; NORTH-AMERICA; FOREST MODEL; VITAL-RATES; FOOD-WEB; POPULATION AB Understanding and forecasting species' geographic distributions in the face of global change is a central priority in biodiversity science. The existing view is that one must choose between correlative models for many species versus process-based models for few species. We suggest that opportunities exist to produce process-based range models for many species, by using hierarchical and inverse modeling to borrow strength across species, fill data gaps, fuse diverse data sets, and model across biological and spatial scales. We review the statistical ecology and population and range modeling literature, illustrating these modeling strategies in action. A variety of large, coordinated ecological datasets that can feed into these modeling solutions already exist, and we highlight organisms that seem ripe for the challenge. C1 [Evans, Margaret E. K.] Univ Arizona, Lab Tree Ring Res, Tucson, AZ 85721 USA. [Evans, Margaret E. K.; Enquist, Brian J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Merow, Cory] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Record, Sydne] Bryn Mawr Coll, Dept Biol, Bryn Mawr, PA 19010 USA. [McMahon, Sean M.] Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. [Enquist, Brian J.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Enquist, Brian J.] Ctr Environm Studies, Aspen, CO 81611 USA. RP Evans, MEK (reprint author), Univ Arizona, Lab Tree Ring Res, Tucson, AZ 85721 USA.; Evans, MEK (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. EM mekevans@email.arizona.edu FU Berkeley Initiative on Global Change Biology; NSF [DEB-1632706, DEB-1137366]; USDA-AFRI grant [2016-67003-24944]; USDA-NRI [DEB-1137366, 2008-35615-19014]; Smithsonian Institution's Center for Tropical Forest Science-Forest Global Earth Observatory; Aspen Center for Environmental Studies; NSF DBI-ABI [1565118] FX The authors benefited from discussions surrounding an Organized Oral Session titled 'Novel Approaches for Process Based Species Distribution Models' at the 2014 annual meeting of the Ecological Society of America, and a workshop 'Ecological insights from integrating diverse data with hierarchical models' sponsored by the Berkeley Initiative on Global Change Biology in October, 2014. In particular, the authors gratefully acknowledge discussions with Tom Miller, Rob Salguero-GOmez, Mark Vanderwel, Matt Talluto, Jorn Pagel, Frank Schurr, Katy Prudic, Andrew Rominger, Dominic LaRoche, Regis Ferriere, Kent McFarland, Dave Moore, Jeff Oliver, and Noah Charney. John Shaw (Interior West-Forest Inventory and Analysis, USDA Forest Service) and Andrew Gray (Pacific Northwest-Forest Inventory and Analysis, USDA Forest Service) provided data on the abundance of U.S.A. tree species. We thank Ben Olimpio for his assistance producing panel (B) in Box 2. MEKE acknowledges the support of NSF grant DEB-1632706 and USDA-AFRI grant 2016-67003-24944. CM acknowledges funding from USDA-NRI grant 2008-35615-19014 and DEB-1137366. SMM and CM acknowledge funding support from NSF DEB-1137366 and Smithsonian Institution's Center for Tropical Forest Science-Forest Global Earth Observatory. BJE acknowledges support from a fellowship from the Aspen Center for Environmental Studies and from NSF DBI-ABI 1565118. NR 100 TC 0 Z9 0 U1 22 U2 22 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD NOV PY 2016 VL 31 IS 11 BP 860 EP 871 DI 10.1016/j.tree.2016.08.005 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA EA6LO UT WOS:000386740900007 PM 27663835 ER PT J AU Benedict, GF Henry, TJ Franz, OG McArthur, BE Wasserman, LH Jao, WC Cargile, PA Dieterich, SB Bradley, AJ Nelan, EP Whipple, AL AF Benedict, G. F. Henry, T. J. Franz, O. G. McArthur, B. E. Wasserman, L. H. Jao, Wei-Chun Cargile, P. A. Dieterich, S. B. Bradley, A. J. Nelan, E. P. Whipple, A. L. TI THE SOLAR NEIGHBORHOOD. XXXVII. THE MASS-LUMINOSITY RELATION FOR MAIN-SEQUENCE M DWARFS SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; binaries : close; stars : distances; stars : late-type; techniques : interferometric; echniques : radial velocities ID TELESCOPE TRIGONOMETRIC PARALLAXES; NAVAL OBSERVATORY PARALLAXES; HYDROGEN-BURNING LIMIT; FINE GUIDANCE SENSORS; SKY SURVEY 2MASS; NEARBY M DWARFS; SYSTEM LHS 1070; FIELD M-DWARFS; M-CIRCLE-DOT; ECLIPSING BINARY AB We present a mass-luminosity relation (MLR) for red dwarfs spanning a range of masses from 0.62 M-circle dot to the end of the stellar main sequence at 0.08 M-circle dot. The relation is based on 47 stars for which dynamical masses have been determined, primarily using astrometric data from Fine Guidance Sensors (FGS) 3 and 1r, white-light interferometers on the Hubble Space Telescope (HST), and radial velocity data from McDonald Observatory. For our HST/FGS sample of 15 binaries, component mass errors range from 0.4% to 4.0% with a median error of 1.8%. With these and masses from other sources, we construct a V-band MLR for the lower main sequence with 47 stars. and a K-band MLR with 45 stars with fit residuals half of those of the V. band. We use GJ 831. AB as an example, obtaining an absolute trigonometric parallax,pi(abs) = 125.3 +/- 0.3 mas, with orbital elements yielding. M-A=0.270 +/- 0.004 M-circle dot and M-B = 0.145 +/- 0.002 M-circle dot. The mass precision rivals that derived for eclipsing binaries. A remaining major task is the interpretation of the intrinsic cosmic scatter in the observed MLR for low-mass stars in terms of physical effects. In the meantime, useful mass values can be estimated from the MLR for the ubiquitous red dwarfs that account for 75% of all stars, with applications ranging from the characterization of exoplanet host stars to the contribution of red dwarfs to the mass of the universe. C1 [Benedict, G. F.; McArthur, B. E.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Henry, T. J.] RECONS Inst, Chambersburg, PA 17201 USA. [Franz, O. G.; Wasserman, L. H.] Lowell Observ, 1400 West Mars Hill Rd, Flagstaff, AZ 86001 USA. [Jao, Wei-Chun] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Cargile, P. A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Dieterich, S. B.] Carnegie Inst Sci, Washington, DC 20005 USA. [Bradley, A. J.] Spacecraft Syst Engn Serv, POB 91, Annapolis Jct, MD 20701 USA. [Nelan, E. P.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Whipple, A. L.] Conceptual Analyt LLC, Greenbelt, MD 20771 USA. [Henry, T. J.; Jao, Wei-Chun; Dieterich, S. B.] CTIO, Vicuna, Coquimbo Region, Chile. RP Benedict, GF (reprint author), Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. OI Benedict, George/0000-0003-2852-3279 FU NASA from the Space Telescope Science Institute [GTO NAG5-1603, GO-6036, 6047, 6566, 6764, 6882, 6883, 6884, 7491, 7493, 7894, 8292, 8728, 8729, 8774, 9234, 9408, 9972, 10104, 10613, 10773, 10929, 11299, 12629]; NASA [NAS5-26555]; National Science Foundation [AST 05-07711, AST 09-08402, AST 14-12026]; NSF FX Support for this work was provided by NASA through grants GTO NAG5-1603, GO-6036, 6047, 6566, 6764, 6882, 6883, 6884, 7491, 7493, 7894, 8292, 8728, 8729, 8774, 9234, 9408, 9972, 10104, 10613, 10773, 10929, 11299, and 12629 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. The RECONS program has been supported by the National Science Foundation through grants AST 05-07711, AST 09-08402, and AST 14-12026.; This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. This research has made use of the SIMBAD and Vizier databases and Aladin, operated at CDS, Strasbourg, France, the NASA/IPAC Extragalactic Database (NED) which is operated by JPL, California Institute of Technology, under contract with the NASA, and NASA's Astrophysics Data System Abstract Service. NR 128 TC 2 Z9 2 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2016 VL 152 IS 5 AR 141 DI 10.3847/0004-6256/152/5/141 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB3HP UT WOS:000387255000002 ER PT J AU Van Eylen, V Albrecht, S Gandolfi, D Dai, F Winn, JN Hirano, T Narita, N Bruntt, H Prieto-Arranz, J Bejar, VJS Nowak, G Lund, MN Palle, E Ribas, I Sanchis-Ojeda, R Yu, L Arriagada, P Butler, RP Crane, JD Handberg, R Deeg, H Jessen-Hansen, J Johnson, JA Nespral, D Rogers, L Ryu, T Shectman, S Shrotriya, T Slumstrup, D Takeda, Y Teske, J Thompson, I Vanderburg, A Wittenmyer, R AF Van Eylen, Vincent Albrecht, Simon Gandolfi, Davide Dai, Fei Winn, Joshua N. Hirano, Teriyuki Narita, Norio Bruntt, Hans Prieto-Arranz, Jorge Bejar, Victor J. S. Nowak, Grzegorz Lund, Mikkel N. Palle, Enric Ribas, Ignasi Sanchis-Ojeda, Roberto Yu, Liang Arriagada, Pamela Butler, R. Paul Crane, Jeffrey D. Handberg, Rasmus Deeg, Hans Jessen-Hansen, Jens Johnson, John A. Nespral, David Rogers, Leslie Ryu, Tsuguru Shectman, Stephen Shrotriya, Tushar Slumstrup, Ditte Takeda, Yoichi Teske, Johanna Thompson, Ian Vanderburg, Andrew Wittenmyer, Robert TI THE K2-ESPRINT PROJECT. V. A SHORT-PERIOD GIANT PLANET ORBITING A SUBGIANT STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: dynamical evolution and stability; stars: fundamental parameters; stars: individual (K2-39) ID SOLAR-TYPE STARS; K2 MISSION; RED GIANT; EXTRASOLAR PLANETS; HOT JUPITERS; KEPLER-432 B; SUPER-EARTH; MASS STARS; OSCILLATIONS; ASTEROSEISMOLOGY AB We report on the discovery and characterization of the transiting planet K2-39b (EPIC 206247743b). With an orbital period of 4.6 days, it is the shortest-period planet orbiting a subgiant star known to date. Such planets are rare, with only a handful of known cases. The reason for this is poorly understood but may reflect differences in planet occurrence around the relatively high-mass stars that have been surveyed, or may be the result of tidal destruction of such planets. K2-39 (EPIC 206247743) is an evolved star with a spectroscopically derived stellar radius and mass of 3.88(-0.42)(+0.48) R-circle dot and 1.53(-0.13)(+0.13) M-circle dot, respectively, and a very close-in transiting planet, with a/R-* = 3.4. Radial velocity (RV) follow-up using the HARPS, FIES, and PFS instruments leads to a planetary mass of 50.3(-9.4)(+9.7) M-circle plus. In combination with a radius measurement of 8.3 +/- 1.1, this results in a mean planetary density of 0.50(-0.17)(+0.29) g cm(-3). We furthermore discover a long-term RV trend, which may be caused by a long-period planet or stellar companion. Because K2-39b has a short orbital period, its existence makes it seem unlikely that tidal destruction is wholly responsible for the differences in planet populations around subgiant and main-sequence stars. Future monitoring of the transits of this system may enable the detection of period decay and constrain the tidal dissipation rates of subgiant stars. C1 [Van Eylen, Vincent; Albrecht, Simon; Bruntt, Hans; Lund, Mikkel N.; Handberg, Rasmus; Jessen-Hansen, Jens; Shrotriya, Tushar; Slumstrup, Ditte] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Gandolfi, Davide] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy. [Gandolfi, Davide] Heidelberg Univ, Zentrum Astron, Landessternwarte Konigstuhl, Konigstuhl 12, D-69117 Heidelberg, Germany. [Dai, Fei; Winn, Joshua N.; Yu, Liang] MIT, Dept Phys, Cambridge, MA 02139 USA. [Dai, Fei; Winn, Joshua N.; Yu, Liang] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hirano, Teriyuki] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan. [Narita, Norio; Ryu, Tsuguru; Takeda, Yoichi] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Narita, Norio; Ryu, Tsuguru] SOKENDAI Grad Univ Adv Studies, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Narita, Norio; Ryu, Tsuguru] Natl Inst Nat Sci, Astrobiol Ctr, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Prieto-Arranz, Jorge; Bejar, Victor J. S.; Nowak, Grzegorz; Palle, Enric; Deeg, Hans; Nespral, David] IAC, E-38205 Tenerife, Spain. [Prieto-Arranz, Jorge; Bejar, Victor J. S.; Nowak, Grzegorz; Palle, Enric; Deeg, Hans; Nespral, David] ULL, Dept Astrofis, E-38206 Tenerife, Spain. [Lund, Mikkel N.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Ribas, Ignasi] CSIC, IEEC, Inst Ciencies Espai, Campus UAB, E-08193 Barcelona, Spain. [Sanchis-Ojeda, Roberto] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Arriagada, Pamela; Butler, R. Paul; Teske, Johanna] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Crane, Jeffrey D.; Shectman, Stephen; Teske, Johanna; Thompson, Ian] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Johnson, John A.; Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rogers, Leslie] CALTECH, Dept Astron, MC249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. [Rogers, Leslie] CALTECH, Div Geol & Planetary Sci, MC249-17,1200 East Calif Blvd, Pasadena, CA 91125 USA. [Wittenmyer, Robert] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia. [Wittenmyer, Robert] Univ New South Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Wittenmyer, Robert] Univ Southern Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. RP Van Eylen, V (reprint author), Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. EM vincent@phys.au.dk RI Butler, Robert/B-1125-2009; OI Gandolfi, Davide/0000-0001-8627-9628; Handberg, Rasmus/0000-0001-8725-4502; Lund, Mikkel Norup/0000-0001-9214-5642 FU Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan [25247026]; Spanish Ministry of Economy and Competitiveness (MINECO); Fondo Europeo de Desarrollo Regional (FEDER) [ESP2013-48391-C4-1-R, ESP2014-57495-C2-2-R]; NSF Graduate Research Fellowship [DGE 1144152]; NASA through the Sagan Fellowship Program; Danish National Research Foundation [DNRF106]; ASTERISK project - European Research Council [267864]; European Union Seventh Framework Programme (FP7) [312430] FX We thank the referee, Alexander Santerne, for helpful comments and suggestions which significantly improved this manuscript. We thank Saul Rappaport for helpful comments during the early stages of this project. We acknowledge kind help by Masayuki Kuzuhara for the analysis of Subaru IRCS data. N.N. acknowledges support from the NAOJ Fellowship, Inoue Science Research Award, and Grant-in-Aid for Scientific Research (A) (No. 25247026) from the Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan. I.R. acknowledges support from the Spanish Ministry of Economy and Competitiveness (MINECO) and the Fondo Europeo de Desarrollo Regional (FEDER) through grants ESP2013-48391-C4-1-R and ESP2014-57495-C2-2-R. A.V. is supported by the NSF Graduate Research Fellowship, Grant No. DGE 1144152. This work was performed (in part) under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. This article is based on observations obtained with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Further observations made with the 1.55m Carlos Sanchez Telescope operated on the island of Tenerife by the Instituto de Astrofisica de Canarias in the Spanish Observatorio del Teide. Observations with the HARPS spectrograph at ESO's La Silla observatory (095.C-0718(A)). Data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no.: 267864). We acknowledge A.S.K. for covering travels in relation to this publication. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2013-2016) under grant agreement No. 312430 (OPTICON). This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. NR 66 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2016 VL 152 IS 5 AR 143 DI 10.3847/0004-6256/152/5/143 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB3HP UT WOS:000387255000004 ER PT J AU Zhou, G Rodriguez, JE Collins, KA Beatty, T Oberst, T Heintz, TM Stassun, KG Latham, DW Kuhn, RB Bieryla, A Lund, MB Labadie-Bartz, J Siverd, RJ Stevens, DJ Gaudi, BS Pepper, J Buchhave, LA Eastman, J Colon, K Cargile, P James, D Gregorio, J Reed, PA Jensen, ELN Cohen, DH McLeod, KK Tan, TG Zambelli, R Bayliss, D Bento, J Esquerdo, GA Berlind, P Calkins, ML Blancato, K Manner, M Samulski, C Stockdale, C Nelson, P Stephens, D Curtis, I Kielkopf, J Fulton, BJ DePoy, DL Marshall, JL Pogge, R Gould, A Trueblood, M Trueblood, P AF Zhou, George Rodriguez, Joseph E. Collins, Karen A. Beatty, Thomas Oberst, Thomas Heintz, Tyler M. Stassun, Keivan G. Latham, David W. Kuhn, Rudolf B. Bieryla, Allyson Lund, Michael B. Labadie-Bartz, Jonathan Siverd, Robert J. Stevens, Daniel J. Gaudi, B. Scott Pepper, Joshua Buchhave, Lars A. Eastman, Jason Colon, Knicole Cargile, Phillip James, David Gregorio, Joao Reed, Phillip A. Jensen, Eric L. N. Cohen, David H. McLeod, Kim K. Tan, T. G. Zambelli, Roberto Bayliss, Daniel Bento, Joao Esquerdo, Gilbert A. Berlind, Perry Calkins, Michael L. Blancato, Kirsten Manner, Mark Samulski, Camile Stockdale, Christopher Nelson, Peter Stephens, Denise Curtis, Ivan Kielkopf, John Fulton, Benjamin J. DePoy, D. L. Marshall, Jennifer L. Pogge, Richard Gould, Andy Trueblood, Mark Trueblood, Pat TI KELT-17B: A HOT-JUPITER TRANSITING AN A-STAR IN A MISALIGNED ORBIT DETECTED WITH DOPPLER TOMOGRAPHY SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: individual (KELT-17b); stars:individual (KELT-17, BD+14 1881, TYC 807-903-1) ID RAPIDLY ROTATING STARS; MAIN-SEQUENCE STARS; DIFFERENTIAL ROTATION; STELLAR MASS; GIANT STARS; F-STARS; EXTRASOLAR PLANETS; IMAGE SUBTRACTION; KEPLER STARS; LIGHT CURVES AB We present the discovery of a hot. Jupiter transiting the V =9.23 mag main-sequence A-star KELT-17(BD+14 1881). KELT-17b is a 1.31(-0.29)(+0.28)M(J), 1.525(-0.060) (+0.065) R-J hot-Jupiter in a 3.08-day period orbit misaligned at -115 degrees.9 +/- 4.degrees 1 to the rotation axis of the star. The planet is confirmed via both the detection of the radial velocity orbit, and the Doppler tomographic detection of the shadow of the planet during two transits. The nature of the spin-orbit misaligned transit geometry allows us to place a constraint on the level of differential rotation in the host star; we find that KELT-17 is consistent with both rigid-body rotation and solar differential rotation rates (alpha < 0.30 at 2 sigma significance). KELT-17 is only the fourth A-star with a confirmed transiting planet, and with a mass of 1.635 M-+0.066(-0.061)circle dot, an effective temperature of 7454 +/- 49 K, and a projected rotational velocity of nu sin I-* = 44.2(-1.3)(+1.5) km S-1 it is among the most massive, hottest, and most rapidly rotating of known planet hosts. C1 [Zhou, George; Latham, David W.; Bieryla, Allyson; Eastman, Jason; Cargile, Phillip; Esquerdo, Gilbert A.; Berlind, Perry; Calkins, Michael L.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Rodriguez, Joseph E.; Collins, Karen A.; Stassun, Keivan G.; Lund, Michael B.; Manner, Mark] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr, Nashville, TN 37235 USA. [Collins, Karen A.; Stassun, Keivan G.] Fisk Univ, Dept Phys, 1000 17th Ave North, Nashville, TN 37208 USA. [Beatty, Thomas] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Beatty, Thomas] Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA. [Oberst, Thomas; Heintz, Tyler M.] Westminster Coll, Dept Phys, New Wilmington, PA 16172 USA. [Kuhn, Rudolf B.] South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa. [Labadie-Bartz, Jonathan; Pepper, Joshua] Lehigh Univ, Dept Phys, 16 Mem Dr East, Bethlehem, PA 18015 USA. [Siverd, Robert J.] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA. [Stevens, Daniel J.; Gaudi, B. Scott; Pogge, Richard; Gould, Andy] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Colon, Knicole] NASA Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. [Colon, Knicole] Bay Area Environm Res Inst, 625 2nd St Ste 209, Petaluma, CA 94952 USA. [James, David] Cerro Tololo InterAmer Observ, Casilla 603, La Serena, Chile. [Gregorio, Joao] Atalaia Grp & Crow Observ, Portalegre, Portugal. [Reed, Phillip A.] Kutztown State Univ, Dept Phys Sci, Kutztown, PA 19530 USA. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Cohen, David H.; McLeod, Kim K.; Blancato, Kirsten; Samulski, Camile] Wellesley Coll, Wellesley, MA 02481 USA. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Zambelli, Roberto] Societ Astronom Lunae, Via Montefrancio 77, I-19030 Castelnuovo Magra, Italy. [Bayliss, Daniel] Univ Geneva, Astron Observ, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. [Bento, Joao] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Stockdale, Christopher] Hazelwood Observ, Hazelwood South, Vic, Australia. [Nelson, Peter] Ellinbank Observ, Ellinbank, Vic, Australia. [Stephens, Denise] BYU Dept Phys & Astron, N486 ESC, Provo, UT 84602 USA. [Curtis, Ivan] ICO, Adelaide, SA, Australia. [Kielkopf, John] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Fulton, Benjamin J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [DePoy, D. L.; Marshall, Jennifer L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [DePoy, D. L.; Marshall, Jennifer L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Trueblood, Mark; Trueblood, Pat] Winer Observ, Sonoita, AZ 85637 USA. RP Zhou, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM george.zhou@cfa.harvard.edu OI Rodriguez, Joseph/0000-0001-8812-0565; Tan, Thiam-Guan/0000-0001-5603-6895; Pepper, Joshua/0000-0002-3827-8417; Latham, David/0000-0001-9911-7388; Stassun, Keivan/0000-0002-3481-9052 FU Theodore Dunham, Jr. Grant of the Fund for Astronomical Research; National Science Foundation Graduate Research Fellowship [2014184874]; NSF CAREER Grant [AST-1056524] FX The authors thank the referee for insightful comments. K.K.M. acknowledges the Theodore Dunham, Jr. Grant of the Fund for Astronomical Research for the purchase of the SDSS filters used at Whitin Observatory. B.J.F. notes that this material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 2014184874. Work by B.S.G. and D.J.S. was partially supported by NSF CAREER Grant AST-1056524. Any opinion, findings, and conclusions or recommendations expressed in this material are those of the authors(s) and do not necessarily reflect the views of the National Science Foundation. NR 94 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2016 VL 152 IS 5 AR 136 DI 10.3847/0004-6256/152/5/136 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB0LX UT WOS:000387036400002 ER PT J AU Bulbul, E Markevitch, M Foster, A Miller, E Bautz, M Loewenstein, M Randall, SW Smith, RK AF Bulbul, Esra Markevitch, Maxim Foster, Adam Miller, Eric Bautz, Mark Loewenstein, Mike Randall, Scott W. Smith, Randall K. TI SEARCHING FOR THE 3.5 keV LINE IN THE STACKED SUZAKU OBSERVATIONS OF GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: general; large-scale structure of universe; line: identification ID DARK-MATTER; EMISSION-LINE; NEUTRINOS; IONS AB We perform a detailed study of the stacked Suzaku observations of 47 galaxy clusters, spanning a redshift range of 0.01-0.45, to search for the unidentified 3.5 keV line. This sample provides an independent test for the previously detected line. We detect a 2s-significant spectral feature at 3.5 keV in the spectrum of the full sample. When the sample is divided into two subsamples (cool-core and non-cool core clusters), the cool-core subsample shows no statistically significant positive residuals at the line energy. A very weak (similar to 2 sigma confidence) spectral feature at 3.5 keV is permitted by the data from the non-cool-core clusters sample. The upper limit on a neutrino decay mixing angle of sin(2)(2 theta) = 6.1 x 10(-11) from the full Suzaku sample is consistent with the previous detections in the stacked XMM-Newton sample of galaxy clusters (which had a higher statistical sensitivity to faint lines), M31, and Galactic center, at a 90% confidence level. However, the constraint from the present sample, which does not include the Perseus cluster, is in tension with previously reported line flux observed in the core of the Perseus cluster with XMM-Newton and Suzaku. C1 [Bulbul, Esra; Miller, Eric; Bautz, Mark] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Markevitch, Maxim; Loewenstein, Mike] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Foster, Adam; Randall, Scott W.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Bulbul, E (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM ebulbul@mit.edu OI Smith, Randall/0000-0003-4284-4167 FU NASA [NX14AF78G, NNX13AE77G, NNX15AC76G, NNX15AE16G]; Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution FX The authors thank Keith Arnaud for providing help with response remapping, and the anonymous referee for useful comments on the draft. Support for this work was provided by NASA through contracts NNX14AF78G, NNX13AE77G, and NNX15AC76G. E.M. and M. B. acknowledge support from NASA grants NNX13AE77G and NNX15AC76G. A. F. acknowledges NASA grant NNX15AE16G. Support for SWR was provided by the Chandra X-ray Center through NASA contract NAS8-03060 and the Smithsonian Institution. NR 24 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 55 DI 10.3847/0004-637X/831/1/55 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB2YU UT WOS:000387229300018 ER PT J AU Schanche, NE Reeves, KK Webb, DF AF Schanche, Nicole E. Reeves, Katharine K. Webb, David F. TI THE BLOB CONNECTION: SEARCHING FOR LOW CORONAL SIGNATURES OF SOLAR POST-CME BLOBS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: coronal mass ejections (CMEs); Sun: corona ID EJECTION CURRENT SHEET; MASS EJECTION; MAGNETIC RECONNECTION; FLARE; PLASMOIDS; HINODE; EUV; DYNAMICS; ERUPTION; WAKE AB Bright linear structures, thought to be indicators of a current sheet (CS), are often seen in Large Angle and Spectrometric Coronagraph (LASCO) on the Solar and Heliospheric Observatory (SOHO) white-light data in the wake of coronal mass ejections (CMEs). In a subset of these post-CME structures, relatively bright blobs are seen moving outward along the rays. These blobs have been interpreted as consequences of the plasmoid instability in the CS, and can help us. to understand the dynamics of the reconnection. We examine several instances, taken largely from the SOHO/LASCO CME-rays Catalog, where these blobs are clearly visible in white-light data. Using radially filtered, difference, wavelet enhanced, and multiscale Gaussian normalized images to visually inspect Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA) data in multiple wavelengths, we look for signatures of material that correspond. both temporally and spatially to the later appearance of the blobs in LASCO/C2. Constraints from measurements of the blobs allow us to predict the expected count rates in DN pixel(-1) s(-1) for each AIA channel. The resulting values would make the blobs bright enough to be detectable at 1.2 R-circle dot. However, we do not. see conclusive evidence for corresponding blobs in the AIA data in any of the events. We do the same calculation for the "cartwheel CME," an event in which blobs were seen in X-rays, and find that our estimated count rates are close to those observed. We suggest several possibilities for the absence of the EUV blobs including the. formation of the blob higher than the AIA field of view, blob coalescence, and overestimation of blob densities. C1 [Schanche, Nicole E.; Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 58, Cambridge, MA 02138 USA. [Webb, David F.] ISR Boston Coll, Chestnut Hill, MA 02467 USA. RP Schanche, NE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 58, Cambridge, MA 02138 USA. EM nschanche@cfa.harvard.edu OI Reeves, Katharine/0000-0002-6903-6832 FU NASA [NNX13AG54G, NNM07AB07C]; Lockheed-Martin [SP02H1701R] FX This work was supported by NASA grant NNX13AG54G and contracts SP02H1701R from Lockheed-Martin to SAO and NNM07AB07C from NASA to SAO. LASCO/C2 data courtesy of SOHO/LASCO consortium. SOHO is a project of international cooperation between ESA and NASA. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies incooperation with ESA and NSC (Norway). N.S. would like to thank J. Raymond and N. Murphy for useful discussions and P. McCauley for his image processing help and advice. NR 41 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 47 DI 10.3847/0004-637X/831/1/47 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB2YU UT WOS:000387229300010 ER PT J AU Stassun, KG Torres, G AF Stassun, Keivan G. Torres, Guillermo TI EVIDENCE FOR A SYSTEMATIC OFFSET OF-0.25 mas IN THE GAIA DR1 PARALLAXES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: eclipsing; parallaxes; stars: distances ID CONSTRAINTS; STARS AB We test the parallaxes reported in the Gaia first data release using the sample of eclipsing binaries with accurate, empirical distances from Stassun & Torres. We find an average offset of -0.25 +/- 0.05. mas in the sense of the Gaia parallaxes being too small (i.e., the distances too long). The offset does not depend strongly on obvious parameters such as color or brightness. However, we find with high confidence that the offset may depend on ecliptic latitude: the mean offset is -0.38 +/- 0.06. mas in the ecliptic north and -0.05 +/- 0.09. mas in the ecliptic south. The ecliptic latitude dependence may also be represented by the linear relation, Delta pi approximate to -0.22(+/- 0.05) - 0.003(+/- 0.001) x beta mas (beta in degrees). Finally, there is a possible dependence of the parallax offset on distance, with the offset becoming negligible for pi less than or similar to 1 mas; we discuss whether this could be caused by a systematic error in the eclipsing binary distance scale, and reject this interpretation as unlikely. C1 [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr Lane, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, 1000 17th Ave N, Nashville, TN 37208 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Stassun, KG (reprint author), Vanderbilt Univ, Dept Phys & Astron, 6301 Stevenson Ctr Lane, Nashville, TN 37235 USA.; Stassun, KG (reprint author), Fisk Univ, Dept Phys, 1000 17th Ave N, Nashville, TN 37208 USA. EM keivan.stassun@vanderbilt.edu OI Stassun, Keivan/0000-0002-3481-9052 FU NSF PAARE [AST-1358862]; NSF [AST-1509375] FX This work has made use of the Filtergraph data visualization service at filtergraph.vanderbilt.edu (Burger et al. 2013). K.G.S. acknowledges partial support from NSF PAARE grant AST-1358862. G.T. acknowledges partial support for this work from NSF grant AST-1509375. The authors are grateful to S.. Casertano and A. Riess for sharing their results in advance of publication. We are grateful to the referee for critiques and suggestions that improved the manuscript. This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. NR 13 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD NOV 1 PY 2016 VL 831 IS 1 AR L6 DI 10.3847/2041-8205/831/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB2AM UT WOS:000387158800001 ER PT J AU Zhu, L Jacob, DJ Kim, PS Fisher, JA Yu, K Travis, KR Mickley, LJ Yantosca, RM Sulprizio, MP De Smedt, I Abad, GG Chance, K Li, C Ferrare, R Fried, A Hair, JW Hanisco, TF Richter, D Scarino, AJ Walega, J Weibring, P Wolfe, GM AF Zhu, Lei Jacob, Daniel J. Kim, Patrick S. Fisher, Jenny A. Yu, Karen Travis, Katherine R. Mickley, Loretta J. Yantosca, Robert M. Sulprizio, Melissa P. De Smedt, Isabelle Abad, Gonzalo Gonzalez Chance, Kelly Li, Can Ferrare, Richard Fried, Alan Hair, Johnathan W. Hanisco, Thomas F. Richter, Dirk Scarino, Amy Jo Walega, James Weibring, Petter Wolfe, Glenn M. TI Observing atmospheric formaldehyde (HCHO) from space: validation and intercomparison of six retrievals from four satellites (OMI, GOME2A, GOME2B, OMPS) with SEAC(4)RS aircraft observations over the southeast US SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID OZONE MONITORING INSTRUMENT; SPECTRAL-RESOLUTION LIDAR; ISOPRENE EMISSIONS; PROFILER SUITE; NORTH-AMERICA; MODEL; COLUMNS; TROPOSPHERE; CHEMISTRY; TRANSPORT AB Formaldehyde (HCHO) column data from satellites are widely used as a proxy for emissions of volatile organic compounds (VOCs), but validation of the data has been extremely limited. Here we use highly accurate HCHO aircraft observations from the NASA SEAC4RS (Studies of Emissions, Atmospheric Composition, Clouds and Climate Coupling by Regional Surveys) campaign over the southeast US in August-September 2013 to validate and intercompare six retrievals of HCHO columns from four different satellite instruments (OMI, GOME2A, GOME2B and OMPS; for clarification of these and other abbreviations used in the paper, please refer to Appendix A.) and three different research groups. The GEOS-Chem chemical transport model is used as a common intercomparison platform. All retrievals feature a HCHO maximum over Arkansas and Louisiana, consistent with the aircraft observations and reflecting high emissions of biogenic isoprene. The retrievals are also interconsistent in their spatial variability over the southeast US (r = 0.4-0.8 on a 0.5 degrees x 0.5 degrees grid) and in their day-to-day variability (r = 0.5-0.8). However, all retrievals are biased low in the mean by 20-51 %, which would lead to corresponding bias in estimates of isoprene emissions from the satellite data. The smallest bias is for OMI-BIRA, which has high corrected slant columns relative to the other retrievals and low scattering weights in its air mass factor (AMF) calculation. OMI-BIRA has systematic error in its assumed vertical HCHO shape profiles for the AMF calculation, and correcting this would eliminate its bias relative to the SEAC(4)RS data. Our results support the use of satellite HCHO data as a quantitative proxy for isoprene emission after correction of the low mean bias. There is no evident pattern in the bias, suggesting that a uniform correction factor may be applied to the data until better understanding is achieved. C1 [Zhu, Lei; Jacob, Daniel J.; Yu, Karen; Travis, Katherine R.; Mickley, Loretta J.; Yantosca, Robert M.; Sulprizio, Melissa P.] Harvard Univ, John A Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Jacob, Daniel J.; Kim, Patrick S.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Fisher, Jenny A.] Univ Wollongong, Sch Chem, Ctr Atmospher Chem, Wollongong, NSW, Australia. [Fisher, Jenny A.] Univ Wollongong, Sch Earth & Environm Sci, Wollongong, NSW, Australia. [De Smedt, Isabelle] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Abad, Gonzalo Gonzalez; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Li, Can] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Li, Can; Hanisco, Thomas F.; Wolfe, Glenn M.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Ferrare, Richard; Hair, Johnathan W.] NASA Langley Res Ctr, Hampton, VA 23681 USA. [Fried, Alan; Richter, Dirk; Walega, James; Weibring, Petter] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. [Scarino, Amy Jo] Sci Syst & Applicat Inc, Hampton, VA USA. [Wolfe, Glenn M.] Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21228 USA. RP Zhu, L (reprint author), Harvard Univ, John A Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM leizhu@fas.harvard.edu RI Wolfe, Glenn/D-5289-2011; Chem, GEOS/C-5595-2014 FU US National Aeronautics and Space Administration; University of Wollongong FX We acknowledge contributions from the NASA SEAC4RS science team. We would also like to thank the SEAC4RS flight crews and support staff for their outstanding efforts in the field. This work was funded by the US National Aeronautics and Space Administration. We thank Michel Van Roozendael for helpful discussions. Jenny A. Fisher acknowledges support from a University of Wollongong Vice Chancellor's Postdoctoral Fellowship. We thank three anonymous reviewers who provided thorough and thoughtful comments. NR 51 TC 0 Z9 0 U1 6 U2 6 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD NOV 1 PY 2016 VL 16 IS 21 BP 13477 EP 13490 DI 10.5194/acp-16-13477-2016 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EB1NF UT WOS:000387118600002 ER PT J AU Nash, MC Martin, S Gattuso, JP AF Nash, Merinda C. Martin, Sophie Gattuso, Jean-Pierre TI Mineralogical response of the Mediterranean crustose coralline alga Lithophyllum cabiochae to near-future ocean acidification and warming SO BIOGEOSCIENCES LA English DT Article ID BIOGENIC CARBONATES; SKELETAL MINERALOGY; RED ALGA; TEMPERATURE; DISSOLUTION; SEAWATER; RESOLUTION; DOLOMITE; CALCITE; GROWTH AB Red calcareous coralline algae are thought to be among the organisms most vulnerable to ocean acidification due to the high solubility of their magnesium calcite skeleton. Although skeletal mineralogy is proposed to change as CO2 and temperature continue to rise, there is currently very little information available on the response of coralline algal carbonate mineralogy to near-future changes in pCO(2) and temperature. Here we present results from a 1-year controlled laboratory experiment to test mineralogical responses to pCO(2) and temperature in the Mediterranean crustose coralline alga (CCA) Lithophyllum cabiochae. Our results show that Mg incorporation is mainly constrained by temperature (+1 mol% MgCO3 for an increase of 3 degrees C), and there was no response to pCO(2). This suggests that L. cabiochae thalli have the ability to buffer their calcifying medium against ocean acidification, thereby enabling them to continue to deposit magnesium calcite with a significant mol% MgCO3 under elevated pCO(2). Analyses of CCA dissolution chips showed a decrease in Mg content after 1 year for all treatments, but this was affected neither by pCO(2) nor by temperature. Our findings suggest that biological processes exert a strong control on calcification on magnesium calcite and that CCA may be more resilient under rising CO2 than previously thought. However, previously demonstrated increased skeletal dissolution with ocean acidification will still have major consequences for the stability and maintenance of Mediterranean coralligenous habitats. C1 [Nash, Merinda C.] Australian Natl Univ, Res Sch Phys & Engn, Canberra, ACT, Australia. [Nash, Merinda C.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Martin, Sophie] UPMC Univ Paris 06, Sorbonne Univ, UMR7144, Stn Biol Roscoff, F-29680 Roscoff, France. [Gattuso, Jean-Pierre] CNRS, Lab Adaptat & Diversite Milieu Marin, UMR7144, Stn Biol Roscoff, F-29680 Roscoff, France. [Gattuso, Jean-Pierre] Sci Po, Inst Sustainable Dev & Int Relat, 27 Rue St Guillaume, F-75007 Paris, France. RP Nash, MC (reprint author), Australian Natl Univ, Res Sch Phys & Engn, Canberra, ACT, Australia.; Nash, MC (reprint author), Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. EM merinda.nash@anu.edu.au FU CarboOcean IP of the European Commission [511176-2]; European Community [211384] FX This work was supported by the CarboOcean IP of the European Commission (grant 511176-2) and is a contribution to the European Project on Ocean Acidification (EPOCA), which received funding from the European Community (grant agreement 211384). NR 35 TC 0 Z9 0 U1 33 U2 33 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1726-4170 EI 1726-4189 J9 BIOGEOSCIENCES JI Biogeosciences PD NOV 1 PY 2016 VL 13 IS 21 BP 5937 EP 5945 DI 10.5194/bg-13-5937-2016 PG 9 WC Ecology; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA EB5XZ UT WOS:000387455500001 ER PT J AU Cook, JA Greiman, SE Agosta, SJ Anderson, RP Arbogast, BS Baker, RJ Boeger, W Bradley, RD Brooks, DR Cole, R Demboski, JR Dobson, AP Dunnum, JL Eckerlin, RP Esselstyn, J Galbreath, KE Hawdon, J Hoekstra, HE Kutz, SJ Light, JE Olson, LE Patterson, BD Patton, JL Phillips, AJ Rickart, E Rogers, DS Siddall, ME Tkach, VV Hoberg, EP AF Cook, Joseph A. Greiman, Stephen E. Agosta, Salvatore J. Anderson, Robert P. Arbogast, Brian S. Baker, Robert J. Boeger, Walter Bradley, Robert D. Brooks, Daniel R. Cole, Rebecca Demboski, John R. Dobson, Andrew P. Dunnum, Jonathan L. Eckerlin, Ralph P. Esselstyn, Jacob Galbreath, Kurt E. Hawdon, John Hoekstra, Hopi E. Kutz, Susan J. Light, Jessica E. Olson, Link E. Patterson, Bruce D. Patton, James L. Phillips, Anna J. Rickart, Eric Rogers, Duke S. Siddall, Mark E. Tkach, Vasyl V. Hoberg, Eric P. TI Transformational Principles for NEON Sampling of Mammalian Parasites and Pathogens: A Response to Springer and Colleagues SO BIOSCIENCE LA English DT Editorial Material ID CLIMATE-CHANGE; ECOLOGY; DISEASE; COLLECTIONS C1 [Cook, Joseph A.; Greiman, Stephen E.; Dunnum, Jonathan L.] Univ New Mexico, Museum Southwestern Biol, Albuquerque, NM 87131 USA. [Cook, Joseph A.; Greiman, Stephen E.; Dunnum, Jonathan L.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Agosta, Salvatore J.] Virginia Commonwealth Univ, Ctr Environm Studies, Richmond, VA 23284 USA. [Agosta, Salvatore J.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [Anderson, Robert P.] CUNY City Coll, Dept Biol, 138th St & Convent Ave, New York, NY 10031 USA. [Arbogast, Brian S.] Univ North Carolina Wilmington, Dept Biol & Marine Biol, Wilmington, NC USA. [Baker, Robert J.; Bradley, Robert D.] Texas Tech Univ, Dept Biol, Lubbock, TX 79409 USA. [Baker, Robert J.; Bradley, Robert D.] Texas Tech Univ Museum, Lubbock, TX 79409 USA. [Boeger, Walter] Univ Fed Parana, Curitiba, Parana, Brazil. [Brooks, Daniel R.] Univ Nebraska, HW Manter Lab Parasitol, Lincoln, NE USA. [Cole, Rebecca] US Geol Survey, Natl Wildlife Hlth Ctr, Madison, WI USA. [Demboski, John R.] Denver Museum Nat & Sci, Denver, CO USA. [Dobson, Andrew P.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Eckerlin, Ralph P.] Northern Virginia Community Coll, Math Sci & Engn Div, Annandale, VA USA. [Esselstyn, Jacob] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Esselstyn, Jacob] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Galbreath, Kurt E.] Northern Michigan Univ, Dept Biol, Marquette, MI USA. [Hawdon, John] George Washington Univ, Sch Med & Hlth Sci, Washington, DC 20052 USA. [Hoekstra, Hopi E.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Hoekstra, Hopi E.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Kutz, Susan J.] Univ Calgary, Fac Vet Med, Calgary, AB T2N 1N4, Canada. [Light, Jessica E.] Texas A&M Univ, Dept Wildlife & Fisheries Sci, College Stn, TX 77843 USA. [Light, Jessica E.] Texas A&M Univ, Biodivers Res & Teaching Collect, College Stn, TX USA. [Olson, Link E.] Univ Alaska, Univ Alaska Museum, Fairbanks, AK 99701 USA. [Patterson, Bruce D.] Field Museum Nat Hist, Chicago, IL 60605 USA. [Patton, James L.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Phillips, Anna J.; Hoberg, Eric P.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Hoberg, Eric P.] ARS, USDA, Beltsville, MD USA. [Rickart, Eric] Nat Hist Museum, Salt Lake City, UT USA. [Rogers, Duke S.] Brigham Young Univ, Monte L Bean Life Sci Museum, Provo, UT 84602 USA. [Rogers, Duke S.] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA. [Siddall, Mark E.] Amer Museum Nat Hist, New York, NY 10024 USA. [Tkach, Vasyl V.] Univ North Dakota, Dept Biol, Grand Forks, ND USA. RP Cook, JA (reprint author), Univ New Mexico, Museum Southwestern Biol, Albuquerque, NM 87131 USA.; Cook, JA (reprint author), Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. EM tucojoe@gmail.com OI Demboski, John/0000-0002-5163-4113 NR 13 TC 0 Z9 0 U1 4 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD NOV PY 2016 VL 66 IS 11 BP 917 EP 919 DI 10.1093/biosci/biw123 PG 3 WC Biology SC Life Sciences & Biomedicine - Other Topics GA EB6AU UT WOS:000387463900002 ER PT J AU Haufler, CH Pryer, KM Schuettpelz, E Sessa, EB Farrar, DR Moran, R Schneller, JJ Watkins, JE Windham, MD AF Haufler, Christopher H. Pryer, Kathleen M. Schuettpelz, Eric Sessa, Emily B. Farrar, Donald R. Moran, Robbin Schneller, J. Jakob Watkins, James E., Jr. Windham, Michael D. TI Sex and the Single Gametophyte: Revising the Homosporous Vascular Plant Life Cycle in Light of Contemporary Research SO BIOSCIENCE LA English DT Article DE ferns; breeding systems; life cycles; genetics; botany ID FERN GAMETOPHYTES; DEVELOPMENTAL PHYSIOLOGY; GENETIC-VARIATION; TEMPERATE FERNS; LAND PLANTS; POPULATIONS; DIVERSIFICATION; ANTHERIDIOGEN; HISTORY; SYSTEMS AB Homosporous vascular plants are typically depicted as extreme inbreeders, with bisexual gametophytes that produce strictly homozygous sporophytes. This view is promulgated in textbook life cycles despite ample evidence that natural populations of most species regularly outcross. We review research on a variety of mechanisms, including genetic load, asynchronous production of eggs and sperm, and pheromonal control of gamete production, that actively promote heterozygosity in ferns and lycophytes. Evolution of the land plants cannot be reconstructed without accurate depictions of the unique life cycle that has helped make ferns the second most diverse lineage of vascular plants on Earth. With revised illustrations and definitions, we provide scientists, educators, and students with a contemporary understanding of fern and lycophyte reproduction, revealing them as evolutionarily dynamic and exploiting a wide range of mating systems. C1 [Haufler, Christopher H.] Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. [Pryer, Kathleen M.; Windham, Michael D.] Duke Univ, Dept Biol, Durham, NC USA. [Schuettpelz, Eric] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Sessa, Emily B.] Univ Florida, Dept Biol, Gainesville, FL USA. [Farrar, Donald R.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA USA. [Moran, Robbin] New York Bot Garden, Inst Systemat Bot, Bronx, NY 10458 USA. [Schneller, J. Jakob] Univ Zurich, Inst Systemat Bot, CH-8006 Zurich, Switzerland. [Watkins, James E., Jr.] Colgate Univ, Dept Biol, Hamilton, NY 13346 USA. RP Haufler, CH (reprint author), Univ Kansas, Dept Ecol & Evolutionary Biol, Lawrence, KS 66045 USA. EM vulgare@ku.edu FU OTS FX One of the first courses offered by a fledgling Organization for Tropical Studies (OTS) was on tropical ferns in Costa Rica. Taught in 1967, it was attended by 11 students, all from universities in the United States. After attending the course and completing their degrees, nearly all the students became teachers and researchers, making major contributions to the study of ferns. Their names now read like a who's who in the field of fern research. More than 40 years later, in January 2008, OTS offered its second course in tropical fern biology. Twenty-three students and six faculty members attended from the United States, Brazil, Colombia, Cuba, Spain, and Switzerland. This publication was sparked by lively discussions among that critical mass of fern biologists attending the 2008 course. We are grateful to OTS for re-igniting this course and for sponsoring subsequent courses in 2013 and 2015. We are indebted to Chris Martine and Jae Cantley for providing valuable comments on an early draft of the article and to the anonymous reviewers for helpful critiques of our manuscript. KMP is grateful to David Haig for constructive conversations about the fern life cycle and for helping to develop the new terminology presented here. NR 71 TC 2 Z9 2 U1 27 U2 27 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD NOV PY 2016 VL 66 IS 11 BP 928 EP 937 DI 10.1093/biosci/biw108 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA EB6AU UT WOS:000387463900005 ER PT J AU Griffin, EA Traw, MB Morin, PJ Pruitt, JN Wright, SJ Carson, WP AF Griffin, Eric A. Traw, M. Brian Morin, Peter J. Pruitt, Jonathan N. Wright, S. Joseph Carson, Walter P. TI Foliar bacteria and soil fertility mediate seedling performance: a new and cryptic dimension of niche differentiation SO ECOLOGY LA English DT Article DE niche differentiation; phyllosphere; plant community; plant-microbe interactions; soil resource availability; species coexistence; tree diversity ID LOWLAND TROPICAL FOREST; NEOTROPICAL FOREST; FUNGAL ENDOPHYTES; RAIN-FOREST; TETRACYCLINE ANTIBIOTICS; PHYLLOSPHERE BACTERIA; ARABIDOPSIS-THALIANA; COMMUNITY ECOLOGY; FUNCTIONAL TRAITS; SPECIES-DIVERSITY AB The phyllosphere (comprising the leaf surface and interior) is one of the world's largest microbial habitats and is host to an abundant and diverse array of bacteria. Nonetheless, the degree to which bacterial communities are benign, harmful, or beneficial to plants in situ is unknown. We tested the hypothesis that the net effect of reducing bacterial abundance and diversity would vary substantially among host species (from harmful to beneficial) and this would be strongly mediated by soil resource availability. To test this, we monitored tree seedling growth responses to commercial antibiotics among replicated resource supply treatments (N,P,K) in a tropical forest in Panama for 29months. We applied either antibiotics or control water to replicated seedlings of five common tree species (Alseis blackiana, Desmopsis panamensis, Heisteria concinna, Sorocea affinis, and Tetragastris panamensis). These antibiotic treatments significantly reduced both the abundance and diversity of bacteria epiphytically as well as endophytically. Overall, the effect of antibiotics on performance was highly host specific. Applying antibiotics increased growth for three species by as much as 49% (Alseis, Heisteria, and Tetragastris), decreased growth for a fourth species by nearly 20% (Sorocea), and had no impact on a fifth species (Desmopsis). Perhaps more importantly, the degree to which foliar bacteria were harmful or not varied with soil resource supply. Specifically, applying antibiotics had no effect when potassium was added but increased growth rate by almost 40% in the absence of potassium. Alternatively, phosphorus enrichment caused the effect of bacteria to switch from being primarily beneficial to harmful or vice versa, but this depended entirely on the presence or absence of nitrogen enrichment (i.e., important and significant interactions). Our results are the first to demonstrate that the net effect of reducing the abundance and diversity of bacteria can have very strong positive and negative effects on seedling performance. Moreover, these effects were clearly mediated by soil resource availability. Though speculative, we suggest that foliar bacteria may interact with soil fertility to comprise an important, yet cryptic dimension of niche differentiation, which can have important implications for species coexistence. C1 [Griffin, Eric A.; Traw, M. Brian; Pruitt, Jonathan N.; Carson, Walter P.] Univ Pittsburgh, Dept Biol Sci, A234 Langley Hall,4249 Fifth Ave, Pittsburgh, PA 15260 USA. [Morin, Peter J.] Rutgers State Univ, Dept Ecol Evolut & Nat Resources, 14 Coll Farm Rd, New Brunswick, NJ 08901 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. RP Griffin, EA (reprint author), Univ Pittsburgh, Dept Biol Sci, A234 Langley Hall,4249 Fifth Ave, Pittsburgh, PA 15260 USA. EM eag46@pitt.edu FU National Science Foundation Graduate Research Fellowship; Smithsonian Tropical Research Institute Predoctoral Fellowship; Lewis and Clark Fellowship for Exploration and Field Research; Sigma Xi; University of Pittsburgh; Central Research Development Fund award from University of Pittsburgh FX We thank Omar Hernandez and Rufino Gonzalez for plant identification and help in the field, as well as Severino Fernandez for help with antibiotic applications. We thank Emily Borodkin for help culturing bacteria in the lab and Betsy Arnold and Justin Shaffer for help sequencing bacterial isolates. In addition, we thank Michelle Spicer for input regarding statistical analyses. Moreover, we thank Allen Herre and an anonymous reviewer for comments. We acknowledge financial support from a National Science Foundation Graduate Research Fellowship, a Smithsonian Tropical Research Institute Predoctoral Fellowship, a Lewis and Clark Fellowship for Exploration and Field Research, Sigma Xi Grant-in-Aid of Research, and the University of Pittsburgh, all of which supported E. Griffin's PhD research; a Central Research Development Fund award from the University of Pittsburgh to W. Carson, B. Traw, and E. Griffin. NR 73 TC 1 Z9 1 U1 19 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD NOV PY 2016 VL 97 IS 11 BP 2998 EP 3008 DI 10.1002/ecy.1537 PG 11 WC Ecology SC Environmental Sciences & Ecology GA EB2YJ UT WOS:000387228200011 PM 27870044 ER PT J AU Coldren, GA Barreto, CR Wykoff, DD Morrissey, EM Langley, JA Feller, IC Chapman, SK AF Coldren, G. A. Barreto, C. R. Wykoff, D. D. Morrissey, E. M. Langley, J. A. Feller, I. C. Chapman, S. K. TI Chronic warming stimulates growth of marsh grasses more than mangroves in a coastal wetland ecotone SO ECOLOGY LA English DT Article DE biomass; mangrove; marsh; range shift; warming; climate change ID SALT-MARSH; CLIMATE-CHANGE; AVICENNIA-GERMINANS; PLANT; EXPANSION; WINTER; FORESTS; SHIFTS; PRODUCTIVITY; BIODIVERSITY AB Increasing temperatures and a reduction in the frequency and severity of freezing events have been linked to species distribution shifts. Across the globe, mangrove ranges are expanding toward higher latitudes, likely due to diminishing frequency of freezing events associated with climate change. Continued warming will alter coastal wetland plant dynamics both above- and belowground, potentially altering plant capacity to keep up with sea level rise. We conducted an in situ warming experiment, in northeast Florida, to determine how increased temperature (+2 degrees C) influences co-occurring mangrove and salt marsh plants. Warming was achieved using passive warming with three treatment levels (ambient, shade control, warmed). Avicennia germinans, the black mangrove, exhibited no differences in growth or height due to experimental warming, but displayed a warming-induced increase in leaf production (48%). Surprisingly, Distichlis spicata, the dominant salt marsh grass, increased in biomass (53% in 2013 and 70% in 2014), density (41%) and height (18%) with warming during summer months. Warming decreased plant root mass at depth and changed abundances of anaerobic bacterial taxa. Even while the poleward shift of mangroves is clearly controlled by the occurrences of severe freezes, chronic warming between these freeze events may slow the progression of mangrove dominance within ecotones. C1 [Coldren, G. A.; Barreto, C. R.; Wykoff, D. D.; Langley, J. A.; Chapman, S. K.] Villanova Univ, Villanova, PA 19085 USA. [Morrissey, E. M.] West Virginia Univ, Morgantown, WV 26506 USA. [Feller, I. C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Chapman, SK (reprint author), Villanova Univ, Villanova, PA 19085 USA. EM samantha.chapman@villanova.edu OI Feller, Ilka/0000-0002-6391-1608 FU NASA Kennedy Space Center Environmental and Ecological Programs; National Aeronautics and Space Administration Climate and Biological Response Program [NNX11AO94G, NNX12 AF55G]; National Science Foundation Macrosystems Biology Program [EF 1065821] FX We are grateful to Lynne Phillips and Carlton Hall for continued support from the NASA Kennedy Space Center Environmental and Ecological Programs. Heather Tran, Cheryl Doughty, Richard and Heather Kittredge provided assistance in the field. Funding for this work was provided by grants from the National Aeronautics and Space Administration Climate and Biological Response Program (NNX11AO94G, NNX12 AF55G) and the National Science Foundation Macrosystems Biology Program (EF 1065821). This work was conducted as part of NASA's Climate Adaptation Science Investigators (CASI) Workgroup. We are thankful for the insightful suggestions and comments by two anonymous reviewers that substantially improved this manuscript. NR 46 TC 0 Z9 0 U1 38 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD NOV PY 2016 VL 97 IS 11 BP 3167 EP 3175 DI 10.1002/ecy.1539 PG 9 WC Ecology SC Environmental Sciences & Ecology GA EB2YJ UT WOS:000387228200026 PM 27870028 ER PT J AU Gizis, JE Williams, PKG Burgasser, AJ Libralato, M Nardiello, D Piotto, G Bedin, LR Berger, E Paudel, R AF Gizis, John E. Williams, Peter K. G. Burgasser, Adam J. Libralato, Mattia Nardiello, Domenico Piotto, Giampaolo Bedin, Luigi R. Berger, Edo Paudel, Rishi TI WISEP J060738.65+242953.4: A NEARBY POLE-ON L8 BROWN DWARF WITH RADIO EMISSION SO ASTRONOMICAL JOURNAL LA English DT Article DE brown dwarfs; solar neighborhood; stars: activity; stars: individual (WISEP J060738.65+242953.4); starspots ID SPITZER-SPACE-TELESCOPE; LOW-MASS STARS; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; EXTRASOLAR GIANT PLANETS; ELECTRON-CYCLOTRON MASER; MAGNETIC-FIELD TOPOLOGY; INFRARED ARRAY CAMERA; T-DWARFS; ULTRACOOL DWARFS; X-RAY AB We present a simultaneous, multi-wavelength campaign targeting the nearby (7.2 pc) L8/L9 (optical/nearinfrared) dwarf WISEP J060738.65+242953.4 in the mid-infrared, radio, and optical. Spitzer Space Telescope observations show no variability at the 0.2% level over 10 hr each in the 3.6 and 4.5 mu m bands. Kepler K2 monitoring over 36 days in Campaign 0 rules out stable periodic signals in the optical with amplitudes greater than 1.5% and periods between 1.5 hr and 2 days. Non-simultaneous Gemini optical spectroscopy detects lithium, constraining this L dwarf to be less than similar to 2 Gyr old, but no Balmer emission is observed. The low measured projected rotation velocity (v sin i < 6 km s(-1)) and lack of variability are very unusual compared to other brown dwarfs, and we argue that this substellar object is likely viewed pole-on. We detect quiescent (non-bursting) radio emission with the Very Large Array. Among radio-detected L and T dwarfs, it has the lowest observed L-v and the lowest v. sin. i. We discuss the implications of a pole-on detection for various proposed radio emission scenarios. C1 [Gizis, John E.; Paudel, Rishi] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Williams, Peter K. G.; Berger, Edo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Burgasser, Adam J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Libralato, Mattia; Nardiello, Domenico; Piotto, Giampaolo] Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy. [Libralato, Mattia; Nardiello, Domenico; Piotto, Giampaolo; Bedin, Luigi R.] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. RP Gizis, JE (reprint author), Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. OI Williams, Peter/0000-0003-3734-3587; Piotto, Giampaolo/0000-0002-9937-6387 FU NASA Science Mission directorate; NASA [NNX15AV664G]; National Science Foundation [AST-1008361]; W.M. Keck Foundation; National Aeronautics and Space Administration's Earth Science Technology Office [NCC5-626] FX This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The material is based in part upon work supported by NASA under award No. NNX15AV664G. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. EB acknowledges support from the National Science Foundation through Grant AST-1008361. This work is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and CONICET (Argentina). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; This research has made use of NASA's Astrophysics Data System, the VizieR catalog access tool, CDS, Strasbourg, France, IRAF, PyQt, and Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013). IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. This work made use of PyKE (Still & Barclay 2012), a software package for the reduction and analysis of Kepler data. This open-source software project is developed and distributed by the NASA Kepler Guest Observer Office. This research made use of Montage, funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com NR 76 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD NOV PY 2016 VL 152 IS 5 AR 123 DI 10.3847/0004-6256/152/5/123 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA4VU UT WOS:000386614500004 ER PT J AU Guzik, JA Houdek, G Chaplin, WJ Smalley, B Kurtz, DW Gilliland, RL Mullally, F Rowe, JF Bryson, ST Still, MD Antoci, V Appourchaux, T Basu, S Bedding, TR Benomar, O Garcia, RA Huber, D Kjeldsen, H Latham, DW Metcalfe, TS Papics, PI White, TR Aerts, C Ballot, J Boyajian, TS Briquet, M Bruntt, H Buchhave, LA Campante, TL Catanzaro, G Christensen-Dalsgaard, J Davies, GR Dogan, G Dragomir, D Doyle, AP Elsworth, Y Frasca, A Gaulme, P Gruberbauer, M Handberg, R Hekker, S Karoff, C Lehmann, H Mathias, P Mathur, S Miglio, A Molenda-Zakowicz, J Mosser, B Murphy, SJ Regulo, C Ripepi, V Salabert, D Sousa, SG Stello, D Uytterhoeven, K AF Guzik, J. A. Houdek, G. Chaplin, W. J. Smalley, B. Kurtz, D. W. Gilliland, R. L. Mullally, F. Rowe, J. F. Bryson, S. T. Still, M. D. Antoci, V. Appourchaux, T. Basu, S. Bedding, T. R. Benomar, O. Garcia, R. A. Huber, D. Kjeldsen, H. Latham, D. W. Metcalfe, T. S. Papics, P. I. White, T. R. Aerts, C. Ballot, J. Boyajian, T. S. Briquet, M. Bruntt, H. Buchhave, L. A. Campante, T. L. Catanzaro, G. Christensen-Dalsgaard, J. Davies, G. R. Dogan, G. Dragomir, D. Doyle, A. P. Elsworth, Y. Frasca, A. Gaulme, P. Gruberbauer, M. Handberg, R. Hekker, S. Karoff, C. Lehmann, H. Mathias, P. Mathur, S. Miglio, A. Molenda-Zakowicz, J. Mosser, B. Murphy, S. J. Regulo, C. Ripepi, V. Salabert, D. Sousa, S. G. Stello, D. Uytterhoeven, K. TI DETECTION OF SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, AND STELLAR MODELS FOR theta CYG, THE BRIGHTEST STAR OBSERVED BY THE KEPLER MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE asteroseismology; stars: fundamental parameters; stars: interiors; stars: solar-type ID MAIN-SEQUENCE STARS; GAMMA DORADUS STARS; F-TYPE STARS; EXOPLANET HOST STARS; INFRARED FLUX METHOD; EFFECTIVE TEMPERATURES; NEARBY STARS; DELTA SCT; A-TYPE; SPECTROSCOPIC PARAMETERS AB theta Cygni is an F3 spectral type magnitude V = 4.48 main-sequence star that was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were first obtained during Quarter 6 ( 2010 June-September). and subsequently in Quarters 8 and 12-17. We present analyses of solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 modes with frequencies of 1000-2700 mu Hz, a large frequency separation of 83.9 +/- 0.4 mu Hz, and maximum oscillation amplitude at frequency nu(max) = 1829 +/- 54 mu Hz. We also present analyses of new ground-based spectroscopic observations, which, combined with interferometric angular diameter measurements, give T-eff = 6697 +/- 78 K, radius 1.49 +/- 0.03 Re-circle dot, [Fe/H] = -0.02 +/- 0.06 dex, and log g = 4.23 +/- 0.03. We calculate stellar models matching these constraints using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses of 1.35-1.39 M-circle dot and ages of 1.0-1.6 Gyr. theta Cyg's T-eff and log g place it cooler than the red edge of the gamma Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The pulsation models show gamma Dor gravity modes driven by the convective blocking mechanism, with frequencies of 1-3 cycles per day (11 to 33 mu Hz). However, gravity modes were not seen in Kepler data; one signal at 1.776 cycles per day (20.56 mu Hz) may be attributable to a faint, possibly background, binary. C1 [Guzik, J. A.] Los Alamos Natl Lab, XTD NTA, MS T-082, Los Alamos, NM 87545 USA. [Houdek, G.; Chaplin, W. J.; Antoci, V.; Bedding, T. R.; Huber, D.; Kjeldsen, H.; White, T. R.; Bruntt, H.; Campante, T. L.; Christensen-Dalsgaard, J.; Davies, G. R.; Dogan, G.; Elsworth, Y.; Handberg, R.; Hekker, S.; Karoff, C.; Miglio, A.; Murphy, S. J.; Stello, D.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Chaplin, W. J.; Campante, T. L.; Davies, G. R.; Elsworth, Y.; Miglio, A.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Smalley, B.; Doyle, A. P.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Kurtz, D. W.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Gilliland, R. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Mullally, F.; Rowe, J. F.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bryson, S. T.; Still, M. D.] NASA, Ames Res Ctr, Bldg 244,MS-244-30, Moffett Field, CA 94035 USA. [Still, M. D.] Bay Area Environm Res Inst, 560 Third St W, Sonoma, CA 95476 USA. [Appourchaux, T.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, Batiment 121, F-91405 Orsay, France. [Basu, S.; Boyajian, T. S.] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. [Bedding, T. R.; Benomar, O.; Huber, D.; White, T. R.; Murphy, S. J.; Stello, D.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Benomar, O.] New York Univ Abu Dhabi, Ctr Space Sci, NYUAD Inst, POB 129188, Abu Dhabi, U Arab Emirates. [Garcia, R. A.; Davies, G. R.; Salabert, D.] Univ Paris Diderot, Lab AIM, CEA, DRF,CNRS,IRFU,SAp,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Metcalfe, T. S.; Mathur, S.] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. [Papics, P. I.; Aerts, C.] Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. [White, T. R.] Australian Astron Observ, POB 915, N Ryde, NSW 1670, Australia. [Aerts, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Ballot, J.; Mathias, P.] Univ Toulouse, UPS OMP, IRAP, F-65000 Tarbes, France. [Briquet, M.] Univ Liege, Inst Astrophys & Geophys, Quartier Agora, Allee 6 Aout 19C, B-4000 Liege, Belgium. [Bruntt, H.] Aarhus Katedralskole, Skolegyde 1, DK-8000 Aarhus C, Denmark. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Catanzaro, G.; Frasca, A.] INAF Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy. [Dogan, G.; Karoff, C.] Aarhus Univ, Dept Geosci, Hoegh Guldbergs Gade 2, DK-8000 Aarhus C, Denmark. [Dogan, G.] Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. [Dragomir, D.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Doyle, A. P.] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England. [Gaulme, P.] Sloan Digital Sky Survey, Apache Point Observ, POB 59, Sunspot, NM 88349 USA. [Gaulme, P.] New Mexico State Univ, Dept Astron, POB 30001, Las Cruces, NM 88003 USA. [Gruberbauer, M.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Hekker, S.] Max Planck Inst Solar Syst Res, SAGE Res Grp, Justus von Liebig Weg 3, D-37077 Gttingen, Germany. [Lehmann, H.] TLS, Sternwarte 5, D-07778 Tautenburg, Germany. [Mathias, P.] CNRS, IRAP, 57 Ave Azereix,BP 826, F-65008 Tarbes, France. [Molenda-Zakowicz, J.] Uniwersytetu Wroclawskiego, Inst Astron, Ul Kopernika 11, PL-51622 Wroclaw, Poland. [Mosser, B.] Univ Paris Diderot, Univ Paris 06, Sorbonne Paris Cite, LESIA,Observ Paris,CNRS,Sorbonne Univ, Paris, France. [Regulo, C.; Uytterhoeven, K.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Regulo, C.; Uytterhoeven, K.] Univ La Laguna, Dept Astron, E-38205 Tenerife, Spain. [Ripepi, V.] INAF Osservatorio Astron Capodimonte, Via Moiariello 16, I-80131 Naples, Italy. [Sousa, S. G.] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Oporto, Portugal. RP Guzik, JA (reprint author), Los Alamos Natl Lab, XTD NTA, MS T-082, Los Alamos, NM 87545 USA. OI Guzik, Joyce/0000-0003-1291-1533; Karoff, Christoffer/0000-0003-2009-7965 FU Kepler Guest Observer [KEPLER08-0013]; NASA Astrophysics Theory Program [12-ATP12-0130]; KITP Asteroseismology Institute at U.C. Santa Barbara; Austrian FWF Project [P21205-N16]; European Community's Seventh Framework Program (FP7) [269194]; Spanish National Plan of RD [AYA2010-17803]; NSF [AST-1514676, AST-1105930]; NASA [NNX16AI09G, NNX13AE70G, NNX12AE17G]; Belgian Science Policy Office (BELSPO) [C90309]; European Research Council under the European Community's Seventh Framework Programme (FP7)/ERC [338251]; Polish Ministry grant [NCN 2014/13/B/ST9/00902]; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) - European Research Council [267864]; Fundao para a Cincia e Tecnologia (Portugal) [SFRH/BPD/47611/2008]; European Community's Seventh Framework Programme (FP7) [312844]; ANR (Agence Nationale de la Recherche, France) program IDEE [ANR-12-BS05-0008]; CNES; Kepler mission under NASA Cooperative [NNX11AB99A, NNX13AB58A]; Smithsonian Astrophysical Observatory FX We are grateful to the Kepler Guest Observer program for observing theta Cyg with a custom aperture. We thank the referee for helpful comments and suggestions. J.A.G. acknowledges support from Kepler Guest Observer grant KEPLER08-0013, NASA Astrophysics Theory Program grant 12-ATP12-0130, and the KITP Asteroseismology Institute at U.C. Santa Barbara in 2011 December. G.H. acknowledges support from the Austrian FWF Project P21205-N16. R.A.G., G.R.D., and K.U. have received funding from the European Community's Seventh Framework Program (FP7/2007-2013) under grant agreement no. 269194. K.U. acknowledges support by the Spanish National Plan of R&D for 2010, project AYA2010-17803. S.B. acknowledges support from NSF grants AST-1514676 and AST-1105930, and NASA grants NNX16AI09G and NNX13AE70G. P.I.P. is a Postdoctoral Fellow of The Research Foundation-Flanders (FWO), Belgium, and he also acknowledges funding from the Belgian Science Policy Office (BELSPO, C90309: CoRoT Data Exploitation). S.H. acknowledges funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ ERC grant agreement number 338251 (StellarAges). J.M.-Z. acknowledges the Polish Ministry grant No. NCN 2014/13/B/ST9/00902. Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no.: 267864). S.G.S. acknowledges support from the Fundao para a Cincia e Tecnologia (Portugal) in the form of the grant SFRH/BPD/47611/2008. R.A.G. received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 312844 (SPACEINN). B.M. and R.A.G. received funding from the ANR (Agence Nationale de la Recherche, France) program IDEE (n ANR-12-BS05-0008) "Interaction Des Etoiles et des Exoplanetes." R.A.G., G.R.D., and D.S. acknowledge support from the CNES. S.M. acknowledges support from the NASA grant NNX12AE17G. D.W.L. acknowledges partial support from the Kepler mission under NASA Cooperative Agreements NNX11AB99A and NNX13AB58A with the Smithsonian Astrophysical Observatory. NR 178 TC 0 Z9 0 U1 6 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 17 DI 10.3847/0004-637X/831/1/17 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA7FG UT WOS:000386794900011 ER PT J AU Kenyon, SJ Najita, JR Bromley, BC AF Kenyon, Scott J. Najita, Joan R. Bromley, Benjamin C. TI ROCKY PLANET FORMATION: QUICK AND NEAT SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; planets and satellites: formation; protoplanetary disks; stars: formation ID SUN-LIKE STARS; T-TAURI STARS; SCORPIUS OB ASSOCIATION; DUSTY DEBRIS DISKS; PRE-MAIN-SEQUENCE; SOLAR-TYPE STARS; LOW-MASS STARS; PICTORIS CIRCUMSTELLAR DISK; FALSE-POSITIVE RATE; SPECTRAL ENERGY-DISTRIBUTIONS AB We reconsider the commonly held assumption that warm debris disks are tracers of terrestrial planet formation. The high occurrence rate inferred for Earth-mass planets around mature solar-type stars based on exoplanet surveys (similar to 20%) stands in stark contrast to the low incidence rate (<= 2%-3%) of warm dusty debris around solar-type stars during the expected epoch of terrestrial planet assembly (similar to 10 Myr). If Earth-mass planets at au distances are a common outcome of the planet formation process, this discrepancy suggests that rocky planet formation occurs more quickly and/or is much neater than traditionally believed, leaving behind little in the way of a dust signature. Alternatively, the incidence rate of terrestrial planets has been overestimated, or some previously unrecognized physical mechanism removes warm dust efficiently from the terrestrial planet region. A promising removal mechanism is gas drag in a residual gaseous disk with a surface density >= 10(-5) of the minimum-mass solar nebula. C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Najita, Joan R.] Natl Opt Astron Observ, 950 Cherry Ave, Tucson, AZ 85719 USA. [Bromley, Benjamin C.] Univ Utah, Dept Phys & Astron, 201 JFB, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X; Bromley, Benjamin/0000-0001-7558-343X FU NASA Outer Planets program [NNX11AM37G]; National Science Foundation [PHY-1066293]; NASA [NXX15AD94G] FX We acknowledge a generous allotment of computer time on the NASA "discover" cluster. We thank G. Herczeg for valuable discussions of stellar accretion rates. Comments from and discussions with S. Andrews, J. Carpenter, M. Geller, A. Glassgold, G. Kennedy, N. Murray, I. Pascucci, D. Wilner, and an anonymous referee improved our presentation. Portions of this project were supported by the NASA Outer Planets program through grant NNX11AM37G. The work of J. N. was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. J.N. also acknowledges the stimulating research environment supported by NASA Agreement No. NXX15AD94G to the Earths in Other Solar Systems program. NR 271 TC 1 Z9 1 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 8 DI 10.3847/0004-637X/831/1/8 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA7FG UT WOS:000386794900002 ER PT J AU Sandquist, EL Jessen-Hansen, J Shetrone, MD Brogaard, K Meibom, S Leitner, M Stello, D Bruntt, H Antoci, V Orosz, JA Grundahl, F Frandsen, S AF Sandquist, Eric L. Jessen-Hansen, J. Shetrone, Matthew D. Brogaard, Karsten Meibom, Soren Leitner, Marika Stello, Dennis Bruntt, Hans Antoci, Victoria Orosz, Jerome A. Grundahl, Frank Frandsen, Soren TI THE AGE AND DISTANCE OF THE KEPLER OPEN CLUSTER NGC 6811 FROM AN ECLIPSING BINARY, TURNOFF STAR PULSATION, AND GIANT ASTEROSEISMOLOGY SO ASTROPHYSICAL JOURNAL LA English DT Article DE asteroseismology; binaries: eclipsing; binaries: spectroscopic; open clusters and associations: individual (NGC 6811); stars: distances; stars: variables: delta Scuti ID STELLAR POPULATION SYNTHESIS; ATMOSPHERIC VELOCITY-FIELDS; SOLAR CHEMICAL-COMPOSITION; HOBBY-EBERLY TELESCOPE; F-TYPE STARS; RED GIANTS; ABSOLUTE DIMENSIONS; MAIN-SEQUENCE; DELTA-SCUTI; AM STARS AB We present the analysis of an eccentric, partially eclipsing long-period (P = 19.23 days) binary system KIC 9777062 that contains main-sequence stars near the turnoff of the intermediate-age open cluster NGC 6811. The primary is a metal-lined Am star with a possible convective blueshift to its radial velocities, and one star (probably the secondary) is likely to be a gamma Dor pulsator. The component masses are 1.603 +/- 0.006(stat.) +/- 0.016(sys.) and 1.419 +/- 0.003 +/- 0.008 M-circle dot, and the radii are 1.744 +/- 0.004 +/- 0.002 and 1.544 +/- 0.002 +/- 0.002 R-circle dot. The isochrone ages of the stars are mildly inconsistent: the age from the mass-radius combination for the primary (1.05. +/- 0.05 +/- 0.09 Gyr, where the last quote was systematic uncertainty from models and metallicity) is smaller than that from the secondary (1.21 +/- 0.05 +/- 0.15 Gyr) and is consistent with the inference from the color-magnitude diagram (1.00 +/- 0.05 Gyr). We have improved the measurements of the asteroseismic parameters Delta(nu) and nu(max) for helium-burning stars in the cluster. The masses of the stars appear to be larger (or alternately, the radii appear to be smaller) than predicted from isochrones using the ages derived from the eclipsing stars. The majority of stars near the cluster turnoff are pulsating stars: we identify a sample of 28 delta Sct, 15 gamma Dor, and 5 hybrid types. We used the period-luminosity relation for high-amplitude d Sct stars to fit the ensemble of the strongest frequencies for the cluster members, finding (m- M)(V) = 10.37 +/- 0.03. This is larger than most previous determinations, but smaller than values derived from the eclipsing binary (10.47 +/- 0.05). C1 [Sandquist, Eric L.; Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Jessen-Hansen, J.; Brogaard, Karsten; Bruntt, Hans] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. [Shetrone, Matthew D.] Univ Texas, McDonald Observ, HC75 Box 1337-L, Ft Davis, TX 79734 USA. [Brogaard, Karsten; Antoci, Victoria; Grundahl, Frank; Frandsen, Soren] Univ Victoria, Dept Phys & Astron, POB 3055, Victoria, BC V8W 3P6, Canada. [Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leitner, Marika] Humboldt State Univ, Dept Phys & Astron, 1 Harpst St, Arcata, CA 95521 USA. [Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. RP Sandquist, EL (reprint author), San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. EM esandquist@mail.sdsu.edu; jjh@phys.au.dk; shetrone@astro.as.utexas.edu; kfb@phys.au.dk; smeibom@cfa.harvard.edu; rika.six@gmail.com; stello@physics.usyd.edu.au; bruntt@gmail.com; antoci@phys.au.dk; jorosz@mail.sdsu.edu; fgj@phys.au.dk; srf@phys.au.dk OI Stello, Dennis/0000-0002-4879-3519 FU Danish National Research Foundation [NDRF106]; ASTERISK project - European Research Council [267864]; National Science Foundation [AST 09-08536]; National Aeronautics and Space Administration [NNX13AC19G]; Research Experiences for Undergraduates site at San Diego State University - National Science Foundation [AST-0850564]; Carlsberg Foundation; Villum Foundation; NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX E.L.S. is grateful to the Stellar Astrophysics Centre at Aarhus University for their generosity and hospitality during his sabbatical stay, during which part of this work was completed. Funding for the Stellar Astrophysics Center is provided by the Danish National Research Foundation (grant agreement no. NDRF106) with research supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement no. 267864). Our work has been funded through grant AST 09-08536 from the National Science Foundation and grant NNX13AC19G from the National Aeronautics and Space Administration to E.L.S. M.L. was supported as part of the Research Experiences for Undergraduates site at San Diego State University, funded by the National Science Foundation under grant AST-0850564 to E.L.S. K.B. acknowledges support from the Carlsberg Foundation and the Villum Foundation. We would also like to thank S. Brunker, E. Rich, C. Curtin, M. Lapid, J. Mascoop, and J. Pautzke for assisting in the acquistion of ground-based photometric observations, and staff and student support astronomers at the NOT (T. Augusteijn, A. A. Djupvik, T. Pursimo, J. Telting, F. S. Kiaeerad, G. Barisevicius, J. Lehtinen, O. Smirnova, S. Geier, T. Kangas, J. Kajava, and Y. Martinez-Osori) for assisting in the acquisition of FIES observations.; We are very grateful to the Kepler team for the opportunity to work with such a precise and extensive data set for detecting variable stars. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France; the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; the WEBDA database, operated at the Institute for Astronomy of the University of Vienna; Astropy, a community-developed core Python package for astronomy (Astropy Collaboration, 2013); and the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration, including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 143 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD NOV 1 PY 2016 VL 831 IS 1 AR 11 DI 10.3847/0004-637X/831/1/11 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA7FG UT WOS:000386794900005 ER PT J AU Bewick, S Agusto, F Calabrese, JM Muturi, EJ Fagan, WF AF Bewick, Sharon Agusto, Folashade Calabrese, Justin M. Muturi, Ephantus J. Fagan, William F. TI Epidemiology of La Crosse Virus Emergence, Appalachia Region, United States SO EMERGING INFECTIOUS DISEASES LA English DT Article ID WESTERN NORTH-CAROLINA; AEDES-ALBOPICTUS; CALIFORNIA ENCEPHALITIS; DIPTERA-CULICIDAE; MOSQUITOS; TRANSMISSION; TRISERIATUS; JAPONICUS; VECTOR; TENNESSEE AB La Crosse encephalitis is a viral disease that has emerged in new locations across the Appalachian region of the United States. Conventional wisdom suggests that ongoing emergence of La Crosse virus (LACV) could stem from the invasive Asian tiger (Aedes albopictus) mosquito. Efforts to prove this, however, are complicated by the numerous transmission routes and species interactions involved in LACV dynamics. To analyze LACV transmission by Asian tiger mosquitoes, we constructed epidemiologic models. These models accurately predict empirical infection rates. They do not, however, support the hypothesis that Asian tiger mosquitoes are responsible for the recent emergence of LACV at new foci. Consequently, we conclude that other factors, including different invasive mosquitoes, changes in climate variables, or changes in wildlife densities, should be considered as alternative explanations for recent increases in La Crosse encephalitis. C1 [Bewick, Sharon; Fagan, William F.] Univ Maryland, 1210 Biol Psychol Bldg, College Pk, MD 20742 USA. [Agusto, Folashade] Univ Kansas, Lawrence, KS 66045 USA. [Calabrese, Justin M.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Muturi, Ephantus J.] Illinois Nat Hist Survey, Champaign, IL 61820 USA. RP Bewick, S (reprint author), Univ Maryland, 1210 Biol Psychol Bldg, College Pk, MD 20742 USA. EM sharon_bewick@hotmail.com RI Calabrese, Justin/B-9131-2012 FU US National Science Foundation [DMS-1225917]; Strategic Environmental Research and Development Program [RC-2639] FX This research was supported by the US National Science Foundation under grant DMS-1225917 (to W.F.F.) and by the Strategic Environmental Research and Development Program under grant RC-2639 (to S.B.). NR 41 TC 0 Z9 0 U1 1 U2 1 PU CENTERS DISEASE CONTROL PI ATLANTA PA 1600 CLIFTON RD, ATLANTA, GA 30333 USA SN 1080-6040 EI 1080-6059 J9 EMERG INFECT DIS JI Emerg. Infect. Dis PD NOV PY 2016 VL 22 IS 11 BP 1921 EP 1929 DI 10.3201/eid2211.160308 PG 9 WC Immunology; Infectious Diseases SC Immunology; Infectious Diseases GA EA3XS UT WOS:000386543200008 PM 27767009 ER PT J AU Gonzalez, VL Kayal, E Halloran, M Shrestha, Y Harasewych, MG AF Gonzalez, Vanessa L. Kayal, Ehsan Halloran, Margaret Shrestha, Yesha Harasewych, M. G. TI The complete mitochondrial genome of the land snail Cerion incanum (Gastropoda: Stylommatophora) and the phylogenetic relationships of Cerionidae within Panpulmonata SO JOURNAL OF MOLLUSCAN STUDIES LA English DT Article ID PROTEIN-SEQUENCE ALIGNMENTS; PULMONATA-STYLOMMATOPHORA; EVOLUTION; CLASSIFICATION; HYBRIDIZATION; SYSTEMATICS; MOLLUSCA; PROGRAM; FLORIDA; DNA AB The complete mitochondrial genome of the neotype of Cerion incanum (Leidy, 1851) was sequenced using high-throughput sequencing and found to be a circular genome 15,117 bp in length with a GC content of 34.3%. It is the largest mitogenome presently known in Stylommatophora, with the difference in size due primarily to intergenic regions and to a lesser extent to larger sizes of individual genes. Gene content is identical to that of other stylommatophorans, but differs in having the tRNA-Gln gene situated on the major coding strand. Gene order of C. incanum was similar to that in Helicidae, differing in the regions between COX1 and NADH5, and between tRNA-Ser2 and tRNA-Ile. The potential origin of replication was located in a 50-bp noncoding region between COX3 and tRNA-Ile. Phylogenetic analyses using Bayesian inference and maximum-likelihood analyses of nucleotide data for all protein-coding and large and small ribosomal genes resulted in a well-resolved tree. This tree was similar to trees derived from nuclear or a combination of nuclear and mitochondrial genes, differing from previous phylogenetic reconstructions based on mitogenomes in the placement of Hygrophila. The phylogenetic position of Cerionidae as sister taxon to Helicoidea is consistent with previous findings after allowing for more limited taxon sampling in the mitogenome tree. The mitogenome tree is sufficiently populated to refute the inclusion of Cerionidae in Clausiloidea, as advocated by some authors, but at present lacks the representatives of the Orthalicoidea or Urocoptoidea needed to resolve more precisely its relationships with those taxa. C1 [Gonzalez, Vanessa L.; Kayal, Ehsan; Halloran, Margaret; Shrestha, Yesha; Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM harasewych@si.edu OI Shrestha, Yesha/0000-0002-9714-8516 NR 67 TC 0 Z9 0 U1 5 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0260-1230 EI 1464-3766 J9 J MOLLUS STUD JI J. Molluscan Stud. PD NOV PY 2016 VL 82 BP 525 EP 533 DI 10.1093/mollus/eyw017 PN 4 PG 9 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA EA8QG UT WOS:000386901500005 ER PT J AU Simkanin, C Fofonoff, PW Larson, K Lambert, G Dijkstra, JA Ruiz, GM AF Simkanin, Christina Fofonoff, Paul W. Larson, Kristen Lambert, Gretchen Dijkstra, Jennifer A. Ruiz, Gregory M. TI Spatial and temporal dynamics of ascidian invasions in the continental United States and Alaska (vol 163, pg 163, 2016) SO MARINE BIOLOGY LA English DT Correction C1 [Simkanin, Christina; Fofonoff, Paul W.; Larson, Kristen; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Lambert, Gretchen] Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. [Dijkstra, Jennifer A.] Univ New Hampshire, Ctr Coastal & Ocean Mapping, Durham, NH 03824 USA. RP Simkanin, C (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM csimkanin@gmail.com NR 1 TC 0 Z9 0 U1 4 U2 4 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD NOV PY 2016 VL 163 IS 11 AR 224 DI 10.1007/s00227-016-2995-7 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA EA6WA UT WOS:000386768500003 ER PT J AU Vlckova, K Gomez, A Petrzelkova, KJ Whittier, CA Todd, AF Yeoman, CJ Nelson, KE Wilson, BA Stumpf, RM Modry, D White, BA Leigh, SR AF Vlckova, Klara Gomez, Andres Petrzelkova, Klara J. Whittier, Christopher A. Todd, Angelique F. Yeoman, Carl J. Nelson, Karen E. Wilson, Brenda A. Stumpf, Rebecca M. Modry, David White, Bryan A. Leigh, Steven R. TI Effect of Antibiotic Treatment on the Gastrointestinal Microbiome of Free-Ranging Western Lowland Gorillas (Gorilla g. gorilla) SO MICROBIAL ECOLOGY LA English DT Article DE Gorilla; Antibiotics; Medical treatment; Gastrointestinal microbiome; Illumina MiSeq; Bacteria ID FECAL BACTERIAL DIVERSITY; HUMAN GUT MICROBIOTA; PAN-TROGLODYTES; LARGE-INTESTINE; NATIONAL-PARK; WILD; DISEASE; PHARMACOKINETICS; CHIMPANZEES; PNEUMONIAE AB The mammalian gastrointestinal (GI) microbiome, which plays indispensable roles in host nutrition and health, is affected by numerous intrinsic and extrinsic factors. Among them, antibiotic (ATB) treatment is reported to have a significant effect on GI microbiome composition in humans and other animals. However, the impact of ATBs on the GI microbiome of free-ranging or even captive great apes remains poorly characterized. Here, we investigated the effect of cephalosporin treatment (delivered by intramuscular dart injection during a serious respiratory outbreak) on the GI microbiome of a wild habituated group of western lowland gorillas (Gorilla gorilla gorilla) in the Dzanga Sangha Protected Areas, Central African Republic. We examined 36 fecal samples from eight individuals, including samples before and after ATB treatment, and characterized the GI microbiome composition using Illumina-MiSeq sequencing of the bacterial 16S rRNA gene. The GI microbial profiles of samples from the same individuals before and after ATB administration indicate that the ATB treatment impacts GI microbiome stability and the relative abundance of particular bacterial taxa within the colonic ecosystem of wild gorillas. We observed a statistically significant increase in Firmicutes and a decrease in Bacteroidetes levels after ATB treatment. We found disruption of the fibrolytic community linked with a decrease of Ruminoccocus levels as a result of ATB treatment. Nevertheless, the nature of the changes observed after ATB treatment differs among gorillas and thus is dependent on the individual host. This study has important implications for ecology, management, and conservation of wild primates. C1 [Vlckova, Klara; Modry, David] Univ Vet & Pharmaceut Sci Brno, Fac Vet Med, Dept Pathol & Parasitol, Palackeho Tr 1-3, Brno 61242, Czech Republic. [Gomez, Andres; Nelson, Karen E.] J Craig Venter Inst, 4120 Capricorn Lane, La Jolla, CA 92037 USA. [Gomez, Andres; Wilson, Brenda A.; Stumpf, Rebecca M.; White, Bryan A.; Leigh, Steven R.] Univ Illinois, Carl R Woese Inst Genom Biol, 1206 West Gregory Dr, Urbana, IL 61801 USA. [Petrzelkova, Klara J.] Acad Sci Czech Republic, Inst Vertebrate Biol, Kvetna 8, CS-60365 Brno, Czech Republic. [Petrzelkova, Klara J.] Liberec Zoo, Masarykova 1347-31, Liberec 46001, Czech Republic. [Petrzelkova, Klara J.; Modry, David] Acad Sci Czech Republic, Inst Parasitol, Ctr Biol, Branisovska 31, CR-37005 Ceske Budejovice, Czech Republic. [Whittier, Christopher A.] Tufts Univ, Cummings Sch Vet Med, 200 Westboro Rd, North Grafton, MA 01536 USA. [Whittier, Christopher A.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Dept Wildlife Hlth Sci, 3001 Connecticut Ave Northwest, Washington, DC 20008 USA. [Todd, Angelique F.] Dzanga Sangha Protected Areas, WWF, BP 1053, Bangui, Cent Afr Republ. [Yeoman, Carl J.] Montana State Univ, Dept Anim & Range Sci, POB 172900, Bozeman, MT 59717 USA. [Nelson, Karen E.] J Craig Venter Inst, 9704 Med Ctr Dr, Rockville, MD 20850 USA. [Wilson, Brenda A.] Univ Illinois, Dept Microbiol, 601 South Goodwin Ave, Urbana, IL 61801 USA. [Stumpf, Rebecca M.] Univ Illinois, Dept Anthropol, 601 South Goodwin Ave, Urbana, IL 61801 USA. [Modry, David] Univ Vet & Pharmaceut Sci Brno, CEITEC VFU, Palackeho Tr 1-3, Brno 61242, Czech Republic. [Leigh, Steven R.] Univ Colorado, Dept Anthropol, 1350 Pleasant St, Boulder, CO 80309 USA. RP Vlckova, K (reprint author), Univ Vet & Pharmaceut Sci Brno, Fac Vet Med, Dept Pathol & Parasitol, Palackeho Tr 1-3, Brno 61242, Czech Republic. EM klari.vlckova@gmail.com; agomez@jcvi.org; petrzelkova@ivb.cz; chris.whittier@tufts.edu; angeliqueftodd@gmail.com; carl.yeoman@montana.edu; kenelson@jcvi.org; bawilson@life.illinois.edu; rstumpf@illinois.edu; modryd@vfu.cz; bwhite44@illinois.edu; Steven.Leigh@colorado.edu RI Petrzelkova, Klara/G-7111-2014 FU Zoo Liberec; Internal Grant Agency of University of Veterinary and Pharmaceutical Sciences [Brno 47/2013/FVL]; Institute of Vertebrate Biology, Academy of Sciences of the Czech Republic [RVO 68081766]; European Social Fund; State Budget of the Czech Republic [OPVK CZ.1.07/2.3.00/20.0300]; US National Science Foundation (NSF) [0935347]; University of Illinois at Urbana-Champaign FX We express our gratitude to the Government of the Central African Republic and to the World Wildlife Fund for granting permission to conduct our research in the Central African Republic, the Primate Habituation Programme (Dzanga-Ndoki National Park, Dzanga-Sangha Protected Areas) for the logistical support in the field, and all local trackers and assistants from Bai Hokou for their help with sample collection. Moreover, we would like to thank to Zoo Liberec for the financial support during ATB treatment of gorillas. We thank to the Roy J. Carver Biotechnology Center, High-Throughput Sequencing and Genotyping Unit, University of Illinois at Urbana-Champaign for providing the amplicon sequencing using Illumina MiSeq Platform. This publication derives from the HPI-Lab, Laboratory for Infectious Diseases Common to Humans and (Non-Human) Primates, Czech Republic. This work was financially supported by the Internal Grant Agency of University of Veterinary and Pharmaceutical Sciences Brno 47/2013/FVL, by the institutional support of the Institute of Vertebrate Biology, Academy of Sciences of the Czech Republic (RVO 68081766), and co-financed from European Social Fund and State Budget of the Czech Republic (project OPVK CZ.1.07/2.3.00/20.0300). Sequencing was supported by the US National Science Foundation (NSF) 0935347 and the University of Illinois at Urbana-Champaign. NR 63 TC 1 Z9 1 U1 40 U2 40 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 EI 1432-184X J9 MICROB ECOL JI Microb. Ecol. PD NOV PY 2016 VL 72 IS 4 SI SI BP 943 EP 954 DI 10.1007/s00248-016-0745-5 PG 12 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA EA6YS UT WOS:000386775700021 PM 26984253 ER PT J AU Chaves, JA Cooper, EA Hendry, AP Podos, J De Leon, LF Raeymaekers, JAM Macmillan, WO Uy, JAC AF Chaves, Jaime A. Cooper, Elizabeth A. Hendry, Andrew P. Podos, Jeffrey De Leon, Luis F. Raeymaekers, Joost A. M. Macmillan, W. Owen Uy, J. Albert C. TI Genomic variation at the tips of the adaptive radiation of Darwin's finches SO MOLECULAR ECOLOGY LA English DT Article DE adaptive radiation; beak size; Darwin's finches; genomic regions; RAD-seq ID WIDE ASSOCIATION; GENE FLOW; BEAK SHAPE; HAPLOTYPE RECONSTRUCTION; REPRODUCTIVE ISOLATION; ECOLOGICAL SPECIATION; NATURAL-SELECTION; SYMPATRIC MORPHS; COLOR PATTERN; DIVERGENCE AB Adaptive radiation unfolds as selection acts on the genetic variation underlying functional traits. The nature of this variation can be revealed by studying the tips of an ongoing adaptive radiation. We studied genomic variation at the tips of the Darwin's finch radiation; specifically focusing on polymorphism within, and variation among, three sympatric species of the genus Geospiza. Using restriction site-associated DNA (RAD-seq), we characterized 32 569 single-nucleotide polymorphisms (SNPs), from which 11 outlier SNPs for beak and body size were uncovered by a genomewide association study (GWAS). Principal component analysis revealed that these 11 SNPs formed four statistically linked groups. Stepwise regression then revealed that the first PC score, which included 6 of the 11 top SNPs, explained over 80% of the variation in beak size, suggesting that selection on these traits influences multiple correlated loci. The two SNPs most strongly associated with beak size were near genes associated with beak morphology across deeper branches of the radiation: delta-like 1 homologue (DLK1) and high-mobility group AT-hook 2 (HMGA2). Our results suggest that (i) key adaptive traits are associated with a small fraction of the genome (11 of 32 569 SNPs), (ii) SNPs linked to the candidate genes are dispersed throughout the genome (on several chromosomes), and (iii) micro-and macro-evolutionary variation (roots and tips of the radiation) involve some shared and some unique genomic regions. C1 [Chaves, Jaime A.; Cooper, Elizabeth A.; Uy, J. Albert C.] Univ Miami, Dept Biol, Coral Gables, FL 33146 USA. [Chaves, Jaime A.] USFQ, Colegio Ciencias Biol & Ambientales & Extens Gala, Campus Cumbaya, Quito, Ecuador. [Cooper, Elizabeth A.] Clemson Univ, Dept Biochem & Genet, Clemson, SC 29634 USA. [Hendry, Andrew P.] McGill Univ, Dept Biol, Redpath Museum, Montreal, PQ, Canada. [Podos, Jeffrey] Univ Massachusetts, Dept Biol, Amherst, MA 01003 USA. [De Leon, Luis F.] Inst Invest Cient & Serv Alta Tecnol INDICASAT AI, Ctr Biodiversidad & Descubrimiento Drogas, Panama City, Panama. [De Leon, Luis F.] Univ Massachusetts, Dept Biol, 100 Morrissey Blvd, Boston, MA 02125 USA. [Raeymaekers, Joost A. M.] Univ Leuven, Lab Biodivers & Evolutionary Genom, B-3000 Leuven, Belgium. [Raeymaekers, Joost A. M.] Norwegian Univ Sci & Technol, Dept Biol, Ctr Biodivers Dynam, N-7491 Trondheim, Norway. [Macmillan, W. Owen] Smithsonian Trop Res Inst, Panama City, Panama. RP Chaves, JA (reprint author), Univ Miami, Dept Biol, Coral Gables, FL 33146 USA.; Chaves, JA (reprint author), USFQ, Colegio Ciencias Biol & Ambientales & Extens Gala, Campus Cumbaya, Quito, Ecuador. EM jachaves@usfq.edu.ec RI Raeymaekers, Joost/J-9538-2014; OI Raeymaekers, Joost/0000-0003-2732-7495; De Leon, Luis Fernando/0000-0001-9317-420X FU Marie Curie fellowship [IEF 300256]; GAIAS-USFQ Grant; SENACYT GRANT; College of Arts and Sciences of the University of Miami; Aresty Chair in Tropical Ecology FX Logistical support and permits (Research Permit #56123) were provided by the Galapagos National Park Service and the Charles Darwin Foundation. For assistance in the field, we thank D. Sharpe, K. Gotanda, K. Cottenie, C. McMillan, J. Sardell, R. Sardell, F. Uy, S. Knutie, A. Leon, J. Koop and D. Hanson. For initial laboratory efforts, we are grateful to Oscar Puebla and Eldredge Bermingham at STRI. We thank W. Hulme and the staff of the Hussman Institute of Human Genetics for performing the sequencing used in this study. We also thank both the University of Miami Center for Computational Science and the Clemson Computing and Information Technology Center for providing many of the computing resources used in our analyses. We thank A. Comeault for helpful discussions and guidance with the implementation and interpretation of GEMMA analyses and M. Roesti, D. Bolnick, D. Presgraves, Patrik Nosil and Searcy/Uy laboratory members for important comments on earlier drafts. We thank Dan Garrigan for his assistance with implementing POPBAM program. Field work was funded in part by a Marie Curie fellowship (IEF 300256) to JAMR, GAIAS-USFQ Grant to JACH, SENACYT GRANT TO LFD, and the genomic work was funded by the College of Arts and Sciences of the University of Miami (JAC, EAC & JACU) and Aresty Chair in Tropical Ecology (JACU). NR 89 TC 5 Z9 5 U1 59 U2 59 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD NOV PY 2016 VL 25 IS 21 BP 5282 EP 5295 DI 10.1111/mec.13743 PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA EA1LH UT WOS:000386353200003 PM 27363308 ER PT J AU Chiang, JM Spasojevic, MJ Muller-Landau, HC Sun, IF Lin, YC Su, SH Chen, ZS Chen, CT Swenson, NG McEwan, RW AF Chiang, Jyh-Min Spasojevic, Marko J. Muller-Landau, Helene C. Sun, I-Fang Lin, Yiching Su, Sheng-Hsin Chen, Zueng-Sang Chen, Chien-Teh Swenson, Nathan G. McEwan, Ryan W. TI Functional composition drives ecosystem function through multiple mechanisms in a broadleaved subtropical forest SO OECOLOGIA LA English DT Article DE Complementarity hypothesis; Forest carbon dynamics; Functional diversity; Functional trait; Mass-ratio effect ID CARBON STOCKS; ABOVEGROUND BIOMASS; SPECIES-DIVERSITY; SPATIAL STRUCTURE; TROPICAL FORESTS; PLANT DIVERSITY; PRODUCTIVITY; BIODIVERSITY; TRAITS; COMPLEMENTARITY AB Understanding the role of biodiversity (B) in maintaining ecosystem function (EF) is a foundational scientific goal with applications for resource management and conservation. Two main hypotheses have emerged that address B-EF relationships: niche complementarity (NC) and the mass-ratio (MR) effect. We tested the relative importance of these hypotheses in a subtropical old-growth forest on the island nation of Taiwan for two EFs: aboveground biomass (ABG) and coarse woody productivity (CWP). Functional dispersion (FDis) of eight plant functional traits was used to evaluate complementarity of resource use. Under the NC hypothesis, EF will be positively correlated with FDis. Under the MR hypothesis, EF will be negatively correlated with FDis and will be significantly influenced by community-weighted mean (CWM) trait values. We used path analysis to assess how these two processes (NC and MR) directly influence EF and may contribute indirectly to EF via their influence on canopy packing (stem density). Our results indicate that decreasing functional diversity and a significant influence of CWM traits were linked to increasing AGB for all eight traits in this forest supporting the MR hypothesis. Interestingly, CWP was primarily influenced by NC and MR indirectly via their influence on canopy packing. Maximum height explained more of the variation in both AGB and CWP than any of the other plant functional traits. Together, our results suggest that multiple mechanisms operate simultaneously to influence EF, and understanding their relative importance will help to elucidate the role of biodiversity in maintaining ecosystem function. C1 [Chiang, Jyh-Min; Lin, Yiching] Tunghai Univ, Dept Life Sci, Taichung 40704, Taiwan. [Spasojevic, Marko J.] Univ Calif Riverside, Dept Biol, Riverside, CA 92521 USA. [Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. [Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 97401, Taiwan. [Su, Sheng-Hsin] Taiwan Forestry Res Inst, Taipei 10066, Taiwan. [Chen, Zueng-Sang] Natl Taiwan Univ, Dept Agr Chem, Taipei 10617, Taiwan. [Chen, Chien-Teh] Natl Chung Hsin Univ, Dept Agron, Taichung 402, Taiwan. [Swenson, Nathan G.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [McEwan, Ryan W.] Univ Dayton, Dept Biol, Dayton, OH 45469 USA. RP Chiang, JM (reprint author), Tunghai Univ, Dept Life Sci, Taichung 40704, Taiwan. EM jyhmin@thu.edu.tw OI Chiang, Jyh-Min/0000-0002-6293-1551 FU National Science Council of Taiwan [102-2313-B-029-003-MY3, 98-2313-B-029-001-MY3]; US National Science Foundation [DEB-1046113]; Smithsonian Center for Tropical Forest Science Research Grants Program; Council of Agriculture; National Science Council of Taiwan FX We gratefully acknowledge the financial support of the National Science Council of Taiwan (102-2313-B-029-003-MY3, 98-2313-B-029-001-MY3 to J-MC), the US National Science Foundation (DEB-1046113), and the Smithsonian Center for Tropical Forest Science Research Grants Program (to RWM). The establishment and two tree censuses of the Fushan plot were financially supported by the Council of Agriculture and the National Science Council of Taiwan. We gratefully acknowledge Ryan Chisholm, John Dwyer, and two anonymous reviewers for their comments that improved the previous versions of this manuscript. JMC wants to thank his father, Mr. Tien-Chin Chiang, for the long-time support of his academic career. He was actively involved in the discussion of this project from a farmer's point-of-view before he passed away on the 6th of March, 2016. None of the authors has any conflict of interest. NR 58 TC 0 Z9 0 U1 28 U2 28 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD NOV PY 2016 VL 182 IS 3 BP 829 EP 840 DI 10.1007/s00442-016-3717-z PG 12 WC Ecology SC Environmental Sciences & Ecology GA DZ2ME UT WOS:000385675100017 PM 27632194 ER PT J AU de Hoogh, K Gulliver, J van Donkelaar, A Martin, RV Marshall, JD Bechle, MJ Cesaroni, G Pradas, MC Dedele, A Eeftens, M Forsberg, B Galassi, C Heinrich, J Hoffmann, B Jacquemin, B Katsouyanni, K Korek, M Kunzli, N Lindley, SJ Lepeule, J Meleux, F de Nazelle, A Nieuwenhuijsen, M Nystad, W Raaschou-Nielsen, O Peters, A Peuch, VH Rouil, L Udvardy, O Slama, R Stempfelet, M Stephanou, EG Tsai, MY Yli-Tuomi, T Weinmayr, G Brunekreef, B Vienneau, D Hoek, G AF de Hoogh, Kees Gulliver, John van Donkelaar, Aaron Martin, Randall V. Marshall, Julian D. Bechle, Matthew J. Cesaroni, Giulia Cirach Pradas, Marta Dedele, Audrius Eeftens, Marloes Forsberg, Bertil Galassi, Claudia Heinrich, Joachim Hoffmann, Barbara Jacquemin, Benedicte Katsouyanni, Klea Korek, Michal Kunzli, Nino Lindley, Sarah J. Lepeule, Johanna Meleux, Frederik de Nazelle, Audrey Nieuwenhuijsen, Mark Nystad, Wenche Raaschou-Nielsen, Ole Peters, Annette Peuch, Vincent-Henri Rouil, Laurence Udvardy, Orsolya Slama, Remy Stempfelet, Morgane Stephanou, Euripides G. Tsai, Ming Y. Yli-Tuomi, Tarja Weinmayr, Gudrun Brunekreef, Bert Vienneau, Danielle Hoek, Gerard TI Development of West-European PM2.5 and NO2 land use regression models incorporating satellite-derived and chemical transport modelling data SO ENVIRONMENTAL RESEARCH LA English DT Article DE Air pollution; Exposure; Spatial modelling; Fine particulate matter; Nitrogen dioxide ID FINE PARTICULATE MATTER; AEROSOL OPTICAL DEPTH; AIR-POLLUTION; EXPOSURE ASSESSMENT; MACC REANALYSIS; ESCAPE PROJECT; AREAS; PM10; ABSORBENCY; PMCOARSE AB Satellite-derived (SAT) and chemical transport model (CTM) estimates of PM2.5 and NO2 are increasingly used in combination with Land Use Regression (LUR) models. We aimed to compare the contribution of SAT and CTM data to the performance of LUR PM2.5 and NO2 models for Europe. Four sets of models, all including local traffic and land use variables, were compared (LUR without SAT or CTM, with SAT only, with CTM only, and with both SAT and CTM). LUR models were developed using two monitoring data sets: PM2.5 and NO2 ground level measurements from the European Study of Cohorts for Air Pollution Effects (ESCAPE) and from the European AIRBASE network. LUR PM2.5 models including SAT and SAT+CTM explained similar to 60% of spatial variation in measured PM2.5 concentrations, substantially more than the LUR model without SAT and CTM (adjR(2): 0.33-0.38). For NO2 CTM improved prediction modestly (adjR2: 0.58) compared to models without SAT and CTM (adjR2: 0.47-0.51). Both monitoring networks are capable of producing models explaining the spatial variance over a large study area. SAT and CTM estimates of PM2.5 and NO2 significantly improved the performance of high spatial resolution LUR models at the European scale for use in large epidemiological studies. (C) 2016 Elsevier Inc. All rights reserved. C1 [de Hoogh, Kees; Eeftens, Marloes; Kunzli, Nino; Tsai, Ming Y.; Vienneau, Danielle] Swiss Trop & Publ Hlth Inst, Socinstr 57, CH-4051 Basel, Switzerland. [de Hoogh, Kees; Eeftens, Marloes; Kunzli, Nino; Tsai, Ming Y.; Vienneau, Danielle] Univ Basel, Peterspl 1, CH-4001 Basel, Switzerland. [Gulliver, John] Imperial Coll London, Dept Epidemiol & Biostat, MRC PHE Ctr Environm & Hlth, St Marys Campus,Norfolk Pl, London W2 1PG, England. [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, 6310 Coburg Rd, Halifax, NS B3H 4R2, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Marshall, Julian D.; Bechle, Matthew J.] Univ Washington, John R Kiely Prof Civil & Environm Engn, Wilcox 268, Seattle, WA 98195 USA. [Cesaroni, Giulia] Lazio Reg Hlth Serv, Dept Epidemiol, Via Cristoforo Colombo 112, I-00147 Rome, Italy. [Cirach Pradas, Marta; Nieuwenhuijsen, Mark] Ctr Res Environm Epidemiol CREAL, Doctor Aiguader 88, E-08003 Barcelona, Spain. [Cirach Pradas, Marta; Nieuwenhuijsen, Mark] CIBERESP, Ave Monforte Lemos,3-5 Pabellon 11 Planta 0, Madrid 28029, Spain. [Dedele, Audrius] Vytauto Didziojo Univ, Dept Environm Sci, K Donelaicio 58, LT-44248 Kaunas, Lithuania. [Forsberg, Bertil] Umea Univ, Dept Publ Hlth & Clin Med Occupat & Environm Med, SE-90187 Umea, Sweden. [Galassi, Claudia] Citta Salute & Sci Univ Hosp, Canc Epidemiol Unit, Corso Bramante 88, I-10126 Turin, Italy. [Galassi, Claudia] Ctr Canc Prevent, Corso Bramante 88, I-10126 Turin, Italy. [Heinrich, Joachim] Univ Munich, Univ Hosp, Munich Inst, Ziemssenstr 1, D-80336 Munich, Germany. [Heinrich, Joachim] Outpatient Clin Occupat Social & Environm Med, Ziemssenstr 1, D-80336 Munich, Germany. [Heinrich, Joachim] Helmholtz Zentrum Munchen, German Res Ctr Environm Hlth, Inst Epidemiol 1, Ingolstadter Landstr 1, D-85764 Neuherberg, Germany. [Hoffmann, Barbara] Univ Dusseldorf, IUF Leibniz Res Inst Environm Med, Aufm Hennekamp 50, D-40225 Dusseldorf, Germany. [Hoffmann, Barbara] Univ Dusseldorf, Fac Med, Univ Str 1, D-40225 Dusseldorf, Germany. [Jacquemin, Benedicte] INSERM, U1168, VIMA Aging & Chron Dis Epidemiol & Publ Hlth Appr, 16 Ave Paul Vaillant Couturier, F-94807 Villejuif, France. [Jacquemin, Benedicte] Univ Versailles St Quentin En Yvelines, UMR S 1168, 2 Ave Source Bievre, F-78180 Montigny Le Bretonneux, France. [Jacquemin, Benedicte] Univ Pompeu Fabra, Placa Merce 10-12, Barcelona 08002, Spain. [Katsouyanni, Klea] Univ Athens, Sch Med, Dept Hyg Epidemiol & Med Stat, 75 Mikras Asias St, GR-11527 Athens, Greece. [Katsouyanni, Klea] Kings Coll London, Dept Primary Care & Publ Hlth Sci, Franklin Wilkins Bldg,150 Stamford St, London SE1 9NH, England. [Katsouyanni, Klea] Kings Coll London, Environm Res Grp, Franklin Wilkins Bldg,150 Stamford St, London SE1 9NH, England. [Korek, Michal] Karolinska Inst, Inst Environm Med, Nobels Vag 13, S-17165 Stockholm, Sweden. [Lindley, Sarah J.] Univ Manchester, Sch Environm Educ & Dev, Geog, Manchester M13 3PL, Lancs, England. [Lepeule, Johanna] INSERM, F-38000 Grenoble, France. [Lepeule, Johanna] Univ Grenoble Alpes, IAB, U1209, Team Environm Epidemiol, F-38000 Grenoble, France. [Meleux, Frederik] Natl Inst Ind Environm & Risks INERIS, Parc Technol ALATA, F-60550 Verneuil En Halatte, France. [de Nazelle, Audrey] Imperial Coll London, Ctr Environm Policy, South Kensington Campus, London SW7 2AZ, England. [Nieuwenhuijsen, Mark] Hosp del Mar, Res Inst, IMIM, Dr Aiguader 88, Barcelona 08003, Spain. [Nystad, Wenche] Norwegian Inst Publ Hlth, Div Environm Med, POB 4404, N-0403 Oslo, Norway. [Raaschou-Nielsen, Ole] Danish Canc Soc Res Ctr, Strandboulevarden 49, DK-2100 Copenhagen, Denmark. [Raaschou-Nielsen, Ole] Aarhus Univ, Dept Environm Sci, Frederiksborgvej 399,POB 358, DK-4000 Roskilde, Denmark. [Peters, Annette] German Res Ctr Environm Hlth, Helmholtz Zentrum Munchen, Inst Epidemiol 2, Ingolstadter Landstr 1, D-85764 Neuherberg, Germany. [Peuch, Vincent-Henri] ECMWF, Shinfield Pk, Reading RG2 9AX, Berks, England. [Udvardy, Orsolya] Natl Publ Hlth Ctr, Albert Florian Ut 2-6, H-1097 Budapest, Hungary. [Stempfelet, Morgane] French Inst Publ Hlth, 12 Rue Val dOsne, F-94415 St Maurice, France. [Stephanou, Euripides G.] Univ Crete, Dept Chem, ECPL, Iraklion 71003, Greece. [Tsai, Ming Y.] Univ Washington, Dept Environm & Occupat Hlth Sci, Box 357234, Seattle, WA 98195 USA. [Yli-Tuomi, Tarja] Natl Inst Hlth & Welf THL, Dept Hlth Protect, Living Environm & Hlth Unit, POB 95, FI-70701 Kuopio, Finland. [Weinmayr, Gudrun] Univ Ulm, Inst Epidemiol & Med Biometry, Helmholtzstr 22, D-89081 Ulm, Germany. [Brunekreef, Bert; Hoek, Gerard] Univ Utrecht, Inst Risk Assessment Sci, Yalelaan 2, NL-3584 CM Utrecht, Netherlands. [Brunekreef, Bert] Univ Med Ctr Utrecht, Julius Ctr Hlth Sci & Primary Care, Uni Weg 100, NL-3584 CM Utrecht, Netherlands. RP de Hoogh, K (reprint author), Swiss Trop & Publ Hlth Inst, Socinstr 57, CH-4051 Basel, Switzerland.; de Hoogh, K (reprint author), Univ Basel, Peterspl 1, CH-4001 Basel, Switzerland. EM c.dehoogh@unibas.ch; j.gulliver@imperial.ac.uk; kelaar@Dal.Ca; Randall.Martin@Dal.Ca; julian@umn.edu; bechl002@umn.edu; g.cesaroni@deplazio.it; mcirach@creal.cat; a.dedele@gmf.vdu.lt; Marloes.eeftens@unibas.ch; bertil.forsberg@envmed.umu.se; claudia.galassi@cpo.it; heinrich@helmholtz-muenchen.de; Barbara.Hoffmann@IUF-Duesseldorf.de; benedicte.jacquemin@inserm.fr; kkatsouy@med.uoa.gr; Michal.Korek@ki.se; Nino.kuenzli@unibas.ch; sarah.lindley@manchester.ac.uk; johanna.lepeule@ujf-grenoble.fr; Frederik.MELEUX@ineris.fr; anazelle@imperial.ac.uk; mnieuwenhuijsen@creal.cat; Wenche.Nystad@fhi.no; ole@cancer.dk; peters@helmholtz-muenchen.de; Vincent-Henri.Peuch@ecmwf.int; Laurence.ROUIL@ineris.fr; udvardy.orsolya@oki.antsz.hu; remy.slama@ujf-grenoble.fr; m.stempfelet@invs.sante.fr; Euripides.Stephanou@gmail.com; m.tsai@unibas.ch; tarja.yli-tuomi@thl.fi; gudrun.weinmayr@uni-ulm.de; B.Brunekreef@uu.nl; Danielle.vienneau@unibas.ch; G.Hoek@uu.nl RI Nieuwenhuijsen, Mark/C-3914-2017; Kunzli, Nino/F-7195-2014; OI Nieuwenhuijsen, Mark/0000-0001-9461-7981; Kunzli, Nino/0000-0001-8360-080X; Slama, Remy/0000-0002-8980-8529; Yli-Tuomi, Tarja/0000-0001-9332-2241; Peters, Annette/0000-0001-6645-0985 FU European Community [FP7 308610, FP7 211250]; European Commission under the EU Seventh Research Framework Programme (MACC II) [283576] FX The research was supported by funding from the European Community's Seventh Framework Program EXPOsOMICS and ESCAPE studies under Grant agreement numbers: FP7 308610 and FP7 211250 respectively. The Air quality modelling data were produced within MACC projects funded by the European Commission under the EU Seventh Research Framework Programme (Grant agreement no. 283576, MACC II). NR 23 TC 1 Z9 1 U1 19 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0013-9351 EI 1096-0953 J9 ENVIRON RES JI Environ. Res. PD NOV PY 2016 VL 151 BP 1 EP 10 DI 10.1016/j.envres.2016.07.005 PG 10 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA EA2HO UT WOS:000386413600001 PM 27447442 ER PT J AU Smith, EF Nelson, LL Strange, MA Eyster, AE Rowland, SM Schrag, DP Macdonald, FA AF Smith, E. F. Nelson, L. L. Strange, M. A. Eyster, A. E. Rowland, S. M. Schrag, D. P. Macdonald, F. A. TI The end of the Ediacaran: Two new exceptionally preserved body fossil assemblages from Mount Dunfee, Nevada, USA SO GEOLOGY LA English DT Article ID PRECAMBRIAN-CAMBRIAN BOUNDARY; WHITE-INYO REGION; GAOJIASHAN LAGERSTATTE; EASTERN CALIFORNIA; SOUTHERN SHAANXI; WESTERN NEVADA; SHELLY FAUNA; EXTINCTION; EVOLUTION; CLOUDINA AB Evaluation of hypotheses that relate environmental to evolutionary change across the Ediacaran-Cambrian transition has been hampered by a dearth of sections that preserve both the last appearance of Ediacaran body fossils and the first appearance of Treptichnus pedum within carbonate-rich strata suitable for chemostratigraphic studies. Here, we report two new exceptionally preserved latest Ediacaran fossil assemblages from the Deep Spring Formation at Mount Dunfee, Nevada (USA). Further, we report these occurrences in a high-resolution carbon isotope chemostratigraphic framework, permitting correlation on a regional and global scale. The lower of the two horizons, at the base of the Deep Spring Formation, hosts a body fossil assemblage that includes Gaojiashania, other vermiform body fossils, and possible Wutubus annularis interbedded with Cloudina shell beds. The upper of the two fossil horizons, in the Esmeralda Member of the Deep Spring Formation, contains Conotubus and occurs within the basal Cambrian negative carbon isotope excursion, establishing it as the youngest Ediacaran fossil assemblage discovered to date. This is the first report of Gaojiashania, Conotubus, and Wutubus in Laurentia, extending the known stratigraphic ranges and biogeographic distributions of these taxa to a global scale. These data refine the relative ages of defining characteristics of the Ediacaran-Cambrian boundary and confirm that a large perturbation to the carbon cycle and surface ocean conditions coincided with the extinction of Ediacaran organisms. C1 [Smith, E. F.] Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. [Nelson, L. L.; Eyster, A. E.; Schrag, D. P.; Macdonald, F. A.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Rowland, S. M.] Univ Nevada, Dept Geosci, 4505 S Maryland Pkwy, Las Vegas, NV 89154 USA. RP Smith, EF (reprint author), Smithsonian Inst, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. FU National Science Foundation Graduate Research Fellowship Program; Massachusetts Institute of Technology NASA Astrobiology Institute FX We thank the National Science Foundation Graduate Research Fellowship Program and the Massachusetts Institute of Technology NASA Astrobiology Institute for support; E. Hodgin and F. Liu for assistance in the field; E. Sperling, L. Tarhan, D. Erwin, and S. Tweedt for advice and stimulating discussions; and J. Schiffbauer, M. Laflamme, and two anonymous reviewers for improving this manuscript. NR 36 TC 2 Z9 2 U1 9 U2 9 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 EI 1943-2682 J9 GEOLOGY JI Geology PD NOV PY 2016 VL 44 IS 11 BP 911 EP 914 DI 10.1130/G38157.1 PG 4 WC Geology SC Geology GA DZ8LF UT WOS:000386121200008 ER PT J AU Lucas, M Forero, D Basset, Y AF Lucas, Maxime Forero, Dimitri Basset, Yves TI Diversity and recent population trends of assassin bugs (Hemiptera: Reduviidae) on Barro Colorado Island, Panama SO INSECT CONSERVATION AND DIVERSITY LA English DT Article DE Assassin bug; light trap; monitoring; Panstrongylus geniculatus; predation; rainfall; temperature; Triatominae ID TROPICAL RAIN-FORESTS; BIODIVERSITY LOSS; ASSEMBLAGES; ABUNDANCE; IMPACTS; CLIMATE; COMMUNITIES; INSECTS; TREES AB 1. In tropical rainforests, most assassin bugs (Hemiptera: Reduviidae) represent important predators preying on other arthropods. Apart from the hematophagous Triatominae of medical importance, Reduviidae remain poorly known. 2. Here, we address the importance of Reduviidae for long-term monitoring of secondary consumers in tropical rainforests, using data from Barro Colorado Island (BCI), Panama. First, we demonstrate that light traps allow catching a wide and representative diversity of Reduviidae, and are more efficient than other collection methods tested. 3. Second, we present one of the very first checklists of Reduviidae for a tropical locality, including 118 species. These baseline data will be necessary for interpreting any long-term changes in reduviid populations on BCI. 4. Last, we show that the low abundance of Reduviidae collected at light remains challenging for statistical analyses of long-term population trends. During a 7-year period (2009-2015), we observed no significant changes in the short-term population dynamics of most reduviid taxa, although these results do not account for the complexity of the intra-annual population dynamics of each species. In particular, the population of the rather abundant Panstrongylus geniculatus, which is a known vector of Chagas' disease, appears to be fluctuating but so far is stable. 5. Daily maximum temperature and rainfall were negatively correlated with the overall abundance of Reduviidae during light traps surveys. During the past 25 years, global warming has induced significant increases in annual temperature and rainfall in Panama. Therefore, we conclude that reduviid populations on BCI may be vulnerable in the future to these global effects. C1 [Lucas, Maxime] AgroParisTech, Gest Environm Ecosyst & Forets Trop, 648,Rue Jean Francois Breton,BP 7355, F-34086 Montpellier 4, France. [Forero, Dimitri] Pontificia Univ Javeriana, Dept Biol, Lab Entomol, UNESIS, Bogota, Colombia. [Basset, Yves] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Basset, Yves] Univ Panama, Maestria Entomol, Panama City, Panama. [Basset, Yves] Univ South Bohemia, Fac Sci, Ceske Budejovice, Czech Republic. RP Lucas, M (reprint author), AgroParisTech, Gest Environm Ecosyst & Forets Trop, 648,Rue Jean Francois Breton,BP 7355, F-34086 Montpellier 4, France. EM max.lucasdc@gmail.com OI Forero, Dimitri/0000-0002-6358-757X FU Czech Science Foundation GACR grant [14-36098G] FX We thank Hector Barrios and Donald Windsor for granting us access to their Malaise trap data. Grants from the Smithsonian Institution Barcoding Opportunity FY012 and FY013 and in-kind help from the Canadian Centre for DNA Barcoding via Paul Hebert and Alex Borisenko at the Biodiversity Institute of Ontario allowed to sequence many of reduviid specimens collected recently on BCI. YB was supported by Czech Science Foundation GACR grant 14-36098G and is a member of the Sistema Nacional de Investigacion, SENACYT, Panama. NR 60 TC 0 Z9 0 U1 15 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1752-458X EI 1752-4598 J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD NOV PY 2016 VL 9 IS 6 BP 546 EP 558 DI 10.1111/icad.12191 PG 13 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA EA1MC UT WOS:000386355400007 ER PT J AU Ames, CL Macrander, J AF Ames, Cheryl Lewis Macrander, Jason TI Evidence for an Alternative Mechanism of Toxin Production in the Box Jellyfish Alatina alata SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article ID CARYBDEA-MARSUPIALIS CNIDARIA; RNA-SEQ DATA; CHIRONEX-FLECKERI; REFERENCE GENOME; VENOM PROTEOME; SEQUENCE DATA; CUBOZOA; NEMATOCYST; TRANSCRIPTOME; EVOLUTION AB Cubozoans (box jellyfish) have a reputation as the most venomous animals on the planet. Herein, we provide a review of cubozoan prey capture and digestion informed by the scientific literature. Like all cnidarians, box jellyfish envenomation originates from structures secreted within nematocyte post-Golgi vesicles called nematocysts. When tentacles come in contact with prey or would-be predators, a cocktail of toxins is rapidly deployed from nematocysts via a long spiny tubule that serves to immobilize the target organism. The implication has long been that toxin peptides and proteins making up the venom within the nematocyst capsule are secreted directly by nematocytes during nematogenesis. However, our combined molecular and morphological analysis of the venomous box jellyfish Alatina alata suggests that gland cells with possible dual roles in secreting toxins and toxic-like enzymes are found in the gastric cirri. These putative gland cell assemblages might be functionally important internally (digestion of prey) as well as externally (envenomation) in cubozoans. Despite the absence of nematocysts in the gastric cirri of mature A. alata medusae, this area of the digestive system appears to be the region of the body where venom-implicated gene products are found in highest abundance, challenging the idea that in cnidarians venom is synthesized exclusively in, or nearby, nematocysts. In an effort to uncover evidence for a central area enriched in gland cells associated with the gastric cirri we provide a comparative description of the morphology of the digestive structures of A. alata and Carybdea box jellyfish species. Finally, we conduct a multi-faceted analysis of the gene ontology terms associated with venom-implicated genes expressed in the tentacle/pedalium and gastric cirri, with a particular emphasis on zinc metalloprotease homologs and genes encoding other bioactive proteins that are abundant in the A. alata transcriptome. C1 [Ames, Cheryl Lewis] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Ames, Cheryl Lewis] Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. [Macrander, Jason] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43215 USA. RP Ames, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA.; Ames, CL (reprint author), Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. EM amesc@si.edu NR 80 TC 1 Z9 1 U1 19 U2 19 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD NOV PY 2016 VL 56 IS 5 BP 973 EP 988 DI 10.1093/icb/icw113 PG 16 WC Zoology SC Zoology GA DZ7XD UT WOS:000386081100023 ER PT J AU Ledo, A Illian, JB Schnitzer, SA Wright, SJ Dalling, JW Burslem, DFRP AF Ledo, Alicia Illian, Janine B. Schnitzer, Stefan A. Wright, S. Joseph Dalling, James W. Burslem, David F. R. P. TI Lianas and soil nutrients predict fine-scale distribution of above-ground biomass in a tropical moist forest SO JOURNAL OF ECOLOGY LA English DT Article DE above-ground biomass spatial distribution; carbon dynamics; carbon stocks; INLA approach; liana; resource competition; soil nutrients; spatial statistics ID BARRO COLORADO ISLAND; TREE GROWTH; NEOTROPICAL FOREST; AMAZONIAN FOREST; RAIN-FOREST; HABITAT ASSOCIATIONS; PERVASIVE ALTERATION; SPATIAL-PATTERNS; CARBON STOCKS; DIVERSITY AB Prediction of carbon dynamics in response to global climate change requires an understanding of the processes that govern the distribution of carbon stocks. Above-ground biomass (AGB) in tropical forests is regulated by variation in soil fertility, climate, species composition and topography at regional scales, but the drivers of fine-scale variation in tropical forest AGB are poorly understood. The factors that control the growth and mortality of individual trees may be obscured by the low resolution of studies at regional scales. In this paper, we evaluated the effects of soil nutrients, topography and liana abundance on the fine-scale spatial distribution of AGB and density of trees for a lowland tropical moist forest in Panama using additive regression models. Areas with larger values of AGB were negatively associated with the presence of lianas, which may reflect competition with lianas and/or the association of lianas with disturbed or open-canopy patches within forests. AGB was positively associated with soils possessing higher pH and K concentrations, reflecting the importance of below-ground resource availability on AGB independently of stem density.Synthesis. Our results shed new light on the factors that influence fine-scale tree AGB and carbon stocks in tropical forests: liana abundance is the strongest predictor, having a negative impact on tree AGB. The availability of soil nutrients was also revealed as an important driver of fine-scale spatial variation in tree AGB. C1 [Ledo, Alicia; Burslem, David F. R. P.] Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. [Illian, Janine B.] Univ St Andrews, Ctr Res Ecol & Environm Modelling, Sch Math & Stat, Observ Buchanan Gardens, St Andrews KY16 9LZ, Fife, Scotland. [Illian, Janine B.] Norwegian Univ Sci & Technol, Dept Math Sci, NO-7491 Trondheim, Norway. [Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, POB 1881, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.; Wright, S. Joseph; Dalling, James W.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. [Dalling, James W.] Univ Illinois, Dept Plant Biol, 265 Morrill Hall,505 S Goodwin, Urbana, IL 61801 USA. RP Ledo, A (reprint author), Univ Aberdeen, Sch Biol Sci, Aberdeen AB24 3UU, Scotland. EM alicialedo@gmail.com OI Burslem, David/0000-0001-6033-0990 FU Marie-Curie Action - SPATFOREST [FP7-PEOPLE-2013-IEF]; US National Science Foundation [DEB-0613666, DEB-0845071, DEB-1019436]; National Science Foundation [DEB021104, DEB021115, DEB0212284, DEB0212818] FX This study was supported by the FP7-PEOPLE-2013-IEF Marie-Curie Action - SPATFOREST. Tree data from BCI were provided by the Center for Tropical Forest Science of the Smithsonian Tropical Research Institute and the primary granting agencies that have supported the BCI plot tree census. Data for the liana censuses were supported by the US National Science Foundation grants DEB-0613666, DEB-0845071 and DEB-1019436 (to SAS). Soil data were funded by the National Science Foundation grants DEB021104, DEB021115, DEB0212284 and DEB0212818 supporting soils mapping in the BCI plot. We thank Helene Muller-Landau for providing some data on tree height for some BCI trees. We also thank all the people who contributed to obtaining the data. NR 91 TC 2 Z9 2 U1 17 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 EI 1365-2745 J9 J ECOL JI J. Ecol. PD NOV PY 2016 VL 104 IS 6 BP 1819 EP 1828 DI 10.1111/1365-2745.12635 PG 10 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA DZ5PY UT WOS:000385915200029 ER PT J AU Zeder, MA Spitzer, MD AF Zeder, Melinda A. Spitzer, Megan D. TI New insights into broad spectrum communities of the Early Holocene Near East: The birds of Hallan Cemi SO QUATERNARY SCIENCE REVIEWS LA English DT Article DE Broad Spectrum Revolution; Early Holocene; Avifauna; Eastern Fertile Crescent ID EPIPALAEOLITHIC SITE; REVOLUTION; ASIA; DIVERSITY; EMERGENCE; ISRAEL; BP AB The Early Holocene in Near East was a pivotal transitional period that witnessed dramatic changes in climate and environment, human settlement, major changes in subsistence strategies focusing on a broad range of different plant and animal resources, and a radical restructuring of social relations, The remarkable corpus of avifauna from the Early Holocene site of Hallan Cemi in southeastern Turkey sheds new light on key issues about this dynamic period that has been termed the "Broad Spectrum Revolution". The avifauna from this important site demonstrate how Hallan Cemi occupants took advantage of the site's strategic location at the junction of multiple environmental zones by extracting a diverse range of seasonally available resources from both near-by and more distant eco-zones to cobble together a stable subsistence economy capable of supporting this small community throughout the year. They give testimony to the impacts of resource utilization over time, especially on species unable to rebound from sustained human hunting. At the same time, they show how Hallan Cemi residents mitigated these impacts by replacing depleted resources with alternative, more resilient ones that could be more sustainably harvested. They open a window onto the growing investment in feasting and ritual activity that helped bind this community together. In so doing they provide a means of empirically evaluating the efficacy of contrasting explanatory frameworks for the Broad Spectrum Revolution that gave rise to the subsequent domestication of plant and animals in the Near East. Contrary to frameworks that cast these developments as responses to resource depression, lessons learned from the Hallan Cemi avifauna lend support to frameworks that emphasize the human capacity to strategically target, capitalize, and improve upon circumscribed resource rich environments in a way that permits more permanent occupation of these niches. And they underscore the degree to which social and ritual activities work together with ecological and economic facets of the lives of these people to both perpetuate and reshape these communities on the threshold of domestication and the emergence of agriculture. Published by Elsevier Ltd. C1 [Zeder, Melinda A.] Santa Fe Inst, Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol,Dept Anthropol, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. [Spitzer, Megan D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Washington, DC 20560 USA. RP Zeder, MA (reprint author), Santa Fe Inst, Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol,Dept Anthropol, 1399 Hyde Pk Rd, Santa Fe, NM 87501 USA. EM zederm@si.edu FU Wenner Gren Foundation for Anthropological Research [8619]; National Geographic Society (CRE) - Smithsonian Institution Scholarly Studies Program [9313-13] FX This research was supported by funding from the Wenner Gren Foundation for Anthropological Research (Gr. 8619), The National Geographic Society (CRE Grant Number: 9313-13) funded by the Smithsonian Institution Scholarly Studies Program. Ximena Lemoine performed a preliminary sorting of the avifauan prior to Spitzer's analysis. The authors thank Richard Redding, Michael Rosenberg, Bruce Smith and Reuven Yeshurun for helpful comments, and Hanneke Meijer for providing photographs of specimens at the Senckenberg Natural History Museum. NR 63 TC 0 Z9 0 U1 4 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD NOV 1 PY 2016 VL 151 BP 140 EP 159 DI 10.1016/j.quascirev.2016.08.024 PG 20 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EA2DZ UT WOS:000386404300009 ER PT J AU Krzemien, L Lukomski, M Bratasz, L Kozlowski, R Mecklenburg, MF AF Krzemien, Leszek Lukomski, Michal Bratasz, Lukasz Kozlowski, Roman Mecklenburg, Marion F. TI Mechanism of craquelure pattern formation on panel paintings SO STUDIES IN CONSERVATION LA English DT Article DE Craquelure pattern; Crack formation; Fracture saturation; Panel paintings; Gesso layer; Dimensional change; Drying shrinkage; Relative humidity cycles AB The drying shrinkage accumulation from exposure of freshly prepared gesso layers to relative humidity (RH) cycles was determined to elucidate the mechanism of craquelure pattern formation on panel paintings. The progresive drying shrinkage of the gesso is observed only under the cycles going to high RH levels which bring about transitions from brittle to ductile state of the material. The first incidence of fracture on the gesso layers occurred after a limited number of cycles ranging between a few and 100 for a range of layer thickness between 0.5 and 1mm. The craquelure patterns stabilised also after a limited number of cycles (30 for the 1-mm thick layer). Upon increase in the gesso layer thickness, the strength of the layer is reduced and the spacing of shrinkage fractures increases. The study demonstrated that craquelure patterns, mimicking historical ones, can be realistically produced in laboratory conditions. Such studies would provide useful information for preparing specimens simulating historic panel paintings and would inform the current efforts on automatic, computer-aided classifications of crack formations on paintings. C1 [Krzemien, Leszek; Lukomski, Michal; Bratasz, Lukasz; Kozlowski, Roman] Polish Acad Sci, Jerzy Haber Inst Catalysis & Surface Chem, Ul Niezapominajek 8, PL-30239 Krakow, Poland. [Bratasz, Lukasz] Natl Museum Krakow, Krakow, Poland. [Mecklenburg, Marion F.] Smithsonian Museum, Conservat Inst, Washington, DC USA. RP Krzemien, L (reprint author), Polish Acad Sci, Jerzy Haber Inst Catalysis & Surface Chem, Ul Niezapominajek 8, PL-30239 Krakow, Poland. EM nckrzemi@cyf-kr.edu.pl OI Bratasz, Lukasz/0000-0002-5277-2606 FU Polish National Science Centre [2011/01/B/HS2/02586] FX This research was supported by Grant 2011/01/B/HS2/02586 from the Polish National Science Centre. NR 11 TC 0 Z9 0 U1 6 U2 6 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0039-3630 EI 2047-0584 J9 STUD CONSERV JI Stud. Conserv. PD NOV PY 2016 VL 61 IS 6 BP 324 EP 330 DI 10.1080/00393630.2016.1140428 PG 7 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA DZ7SQ UT WOS:000386067300003 ER PT J AU Melo, BF Ochoa, LE Vari, RP Oliveira, C AF Melo, Bruno F. Ochoa, Luz E. Vari, Richard P. Oliveira, Claudio TI Cryptic species in the Neotropical fish genus Curimatopsis (Teleostei, Characiformes) SO ZOOLOGICA SCRIPTA LA English DT Article ID TAMBAQUI COLOSSOMA-MACROPOMUM; AMAZON BASIN; MOLECULAR PHYLOGENY; ECONOMICALLY IMPORTANT; SOUTH-AMERICA; RIO NEGRO; CHARACIDAE; OSTARIOPHYSI; PHYLOGEOGRAPHY; CURIMATIDAE AB Detritivores of the fish family Curimatidae are assigned to eight genera, one of which, the Curimatopsis, with only five species, is the least speciose genus and sister to other seven genera in the family. Ongoing morphological investigations reveal, however, the likely existence of additional species. In this study, fifty-one specimens of Curimatopsis from multiple rivers of the Amazon, Paraguay and Suriname drainages were identified morphologically according to the present species concepts and then barcoded using the universal cytochrome c oxidase subunit I (COI) mitochondrial marker. Species delimitation analyses were conducted using Bayesian methods through the general mixed Yule-coalescent analysis combined with conventional likelihood, genetic distance and haplotypic diversity approaches. We found eleven well-supported clusters that represent four of the named species and seven cryptic, undescribed species of Curimatopsis. Our results show a clear delimitation of species boundaries constrained by distinct Amazonian river ecotones that may have promoted intrageneric lineage diversification. This is the first of a series of genetic studies applicable to future taxonomic, phylogenetic and evolutionary studies across the Curimatidae. C1 [Melo, Bruno F.; Ochoa, Luz E.; Oliveira, Claudio] Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Dist Rubiao Jr S-N, BR-18618970 Sao Paulo, Brazil. [Melo, Bruno F.; Vari, Richard P.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, MCR 159,POB 37012, Washington, DC 20013 USA. RP Melo, BF (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Morfol, Dist Rubiao Jr S-N, BR-18618970 Sao Paulo, Brazil. EM melo@ibb.unesp.br; luzeocho@gmail.com; claudio@ibb.unesp.br RI Gesseff, Ednilson/A-3019-2017 FU FAPESP [10/17009-2, 11/08374-1, 13/16436-2, 14/06853-8]; CNPq PDJ [40258/2014-7]; NSF DEB [1257898]; Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, Division of Fishes, National Museum of Natural History; 'South American Characiformes Inventory' Thematic Project of FAPESP (FAPESP) [11/50282-7] FX We thank Francisco Langeani (DZSJRP), Lucia R. Py-Daniel and Renildo R. Oliveira (INPA), and Alessio Datovo and Michel D. Gianeti (MZUSP), for making available comparative material of Curimatopsis. Thanks to Brian Sidlauskas and Kendra Hoekzema (OSU) who provided essential sequences and to Jorge E. Garcia-Melo for photography of specimens and assistance with the editing of Fig. 2. Authors were funded by FAPESP #10/17009-2, FAPESP #11/08374-1, FAPESP #13/16436-2 and CNPq PDJ 40258/2014-7 (BFM), FAPESP #14/06853-8 (LEO), NSF DEB 1257898 (RPV, CO) and the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, Division of Fishes, National Museum of Natural History (RPV). This project also received support from the 'South American Characiformes Inventory' Thematic Project of FAPESP (FAPESP #11/50282-7). NR 79 TC 1 Z9 2 U1 5 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0300-3256 EI 1463-6409 J9 ZOOL SCR JI Zool. Scr. PD NOV PY 2016 VL 45 IS 6 BP 650 EP 658 DI 10.1111/zsc.12178 PG 9 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA DZ7VI UT WOS:000386075500007 ER PT J AU Maas, B Karp, DS Bumrungsri, S Darras, K Gonthier, D Huang, JCC Lindell, CA Maine, JJ Mestre, L Michel, NL Morrison, EB Perfecto, I Philpott, SM Sekerciogiu, CH Silva, RM Taylor, PJ Tscharntke, T Van Bael, SA Whelan, CJ Williams-Guillen, K AF Maas, Bea Karp, Daniel S. Bumrungsri, Sara Darras, Kevin Gonthier, David Huang, Joe C. -C. Lindell, Catherine A. Maine, Josiah J. Mestre, Laia Michel, Nicole L. Morrison, Emily B. Perfecto, Ivette Philpott, Stacy M. Sekerciogiu, Cagan H. Silva, Roberta M. Taylor, Peter J. Tscharntke, Teja Van Bael, Sunshine A. Whelan, Christopher J. Williams-Guillen, Kimberly TI Bird and bat predation services in tropical forests and agroforestry landscapes SO BIOLOGICAL REVIEWS LA English DT Article DE agricultural landscapes; arthropod suppression; bird and bat ecology; cacao; coffee; ecosystem services; exclosure experiments; flying vertebrates; food webs; pest suppression ID INSECTIVOROUS BIRDS; AGRICULTURAL LANDSCAPES; TROPHIC CASCADES; PEST-CONTROL; FUNCTIONAL DIVERSITY; ECOSYSTEM SERVICES; COFFEE FARMS; BIODIVERSITY CONSERVATION; POLLINATION ECOLOGY; LEAF DAMAGE AB Understanding distribution patterns and multitrophic interactions is critical for managing bat- and bird-mediated ecosystem senzices such as the suppression of pest and non-pest arthropods. Despite the ecological and economic importance of bats and birds in tropical forests, a.grotbrestry systems, and agricultural systems mixed with natural forest, a systematic review of their impact is still missing. A growing number of bird and bat exclosure experiments has improved our knowledge allowing new conclusions regarding their roles in food Webs and associated ecosystem seivices. Here, 1,ye review the distribution patterns of insectivorous birds and bats, their local and landscape drivers, and their effects on trophic cascades in tropical ecosystems. We report that for birds but not bats comanmity composition and relative importance of functional groups changes conspicuously from forests to habitats including both agricultural areas and forests, here termed 'forest-agri' habitats, with reduced representation of insectivores in the latter. In contrast to previous theory regarding trophic cascade strength, we find that birds and bats reduce the density and biomass of arthropods in the tropics with effect sizes similar to those in temperate and boreal communities. The relative importance of birds versus bats in regulating pest abundances varies with s(ason, geography and management. Birds and bats may even suppress tropical arthropod outbreaks, although positive effects on plant growth are not always report,ed. As both bats and birds are major ag,ents of pest suppression, a better understanding of the local and landscape factoi-s driving the variability of their impact is needed. C1 [Maas, Bea; Darras, Kevin; Tscharntke, Teja] Univ Gottingen, Agroecol, Grisebachstr 6, D-37077 Gottingen, Germany. [Maas, Bea] Univ Vienna, Dept Bot & Biodivers Res, Div Trop Ecol & Anim Biodivers, A-1030 Vienna, Austria. [Karp, Daniel S.; Gonthier, David] Nature Conservancy, 201 Mission St,4th Floor, San Francisco, CA 94105 USA. [Karp, Daniel S.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Mulford Hall,130 Hilgard Way, Berkeley, CA 94720 USA. [Bumrungsri, Sara] Prince Songkla Univ, Fac Sci, Dept Biol, Thailand 15 Karnjanavanich Rd, Hat Yai 90110, Songkhla, Thailand. [Gonthier, David; Perfecto, Ivette; Williams-Guillen, Kimberly] Univ Michigan, Sch Nat Resources & Environm, 440 Church St, Ann Arbor, MI 48109 USA. [Huang, Joe C. -C.] Texas Tech Univ, Dept Biol Sci, Box 43131, Lubbock, TX 79409 USA. [Huang, Joe C. -C.] Texas Tech Univ, Dept Biol Sci, Southeast Asian Bat Conservat & Res Unit, Box 43131, Lubbock, TX 79409 USA. [Lindell, Catherine A.; Morrison, Emily B.] Michigan State Univ, Dept Integrat Biol, Ctr Global Change & Earth Observat, 288 Farm Lane RM 203, E Lansing, MI 48824 USA. [Maine, Josiah J.] Southern Illinois Univ, Dept Zool, Ctr Ecol, Cooperat Wildlife Res Lab, 1125 Lincoln Dr, Carbondale, IL 62901 USA. [Mestre, Laia] CREAF, Carretera Bellaterra Autonomo S-N, Barcelona 08193, Spain. [Mestre, Laia] Univ Autonoma Barcelona, Dept Biol Anim Biol Vegetal & Ecol, Carretera Bellaterra Autonomo S-N, E-08193 Barcelona, Spain. [Mestre, Laia] Swedish Univ Agr Sci, Dept Ecol, Box 7044, S-75007 Uppsala, Sweden. [Michel, Nicole L.] Univ Saskatchewan, Sch Environm & Sustainabil, 117 Sci Pl, Saskatoon, SK S7N 5C8, Canada. [Philpott, Stacy M.] Univ Calif Santa Cruz, Dept Environm Studies, 1156 High St, Santa Cruz, CA 95062 USA. [Sekerciogiu, Cagan H.] Univ Utah, Dept Biol, 257 South 1400 East,Rm 201, Salt Lake City, UT 84112 USA. [Sekerciogiu, Cagan H.] Koc Univ, Coll Sci, TR-34450 Istanbul, Turkey. [Silva, Roberta M.] Univ Estadual Santa Cruz, Programa Posgrad Ecol & Conservacao Biodiversidad, Rodovia Ilheus Itabuna,Km 16, BR-45662900 Ilheus, BA, Brazil. [Taylor, Peter J.] Univ KwaZulu Natal, Sch Life Sci, Private Bag X54001, ZA-4000 Durban, South Africa. [Taylor, Peter J.] Univ Venda, SARChI Chair Biodivers Value & Change, Sch Math & Nat Sci, P Bag X5050, ZA-0950 Thohoyandou, South Africa. [Taylor, Peter J.] Univ Venda, Ctr Invas Biol, Sch Math & Nat Sci, P Bag X5050, ZA-0950 Thohoyandou, South Africa. [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, 6823 St Charles Ave, New Orleans, LA 70118 USA. [Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. [Whelan, Christopher J.] Univ Illinois, Illinois Nat Hist Survey, Biol Sci, 845 West Taylor St, Chicago, IL 60607 USA. [Williams-Guillen, Kimberly] Paso Pacifico, POB 1244, Ventura, CA 94302 USA. RP Maas, B (reprint author), Univ Gottingen, Agroecol, Grisebachstr 6, D-37077 Gottingen, Germany.; Maas, B (reprint author), Univ Vienna, Dept Bot & Biodivers Res, Div Trop Ecol & Anim Biodivers, A-1030 Vienna, Austria. EM beamaas@gmx.at RI Philpott, Stacy/F-2330-2011; OI Whelan, Christopher/0000-0001-7511-2603; Darras, Kevin Felix Arno/0000-0002-9013-3784; Sekercioglu, Cagan H./0000-0003-3193-0377; Mestre, Laia/0000-0001-7314-7546 FU DFG [CRC 990 EFForTS]; BMBF; South African National Research Foundation; Department of Science and Technology, University of Venda; Southern African Macadamia Growers' Association; NatureNet Science Fellowship from the Nature Conservancy; Bat Conservation International; Environment Canada; University of Saskatchewan; Spanish Ministry of Research and Innovation (MICINN-FEDER) [CGL2007-64080-C02-01/BOS, CGL2010-18182]; NSF [DBI-0610473, DEB-0349388]; State University of Santa Cruz; Mars Center for Cocoa Science FX We thank all scientists, field assistants, local communities and research Binders supporting ecosystem-service research for their contribution to a better understanding of these complex services and their relationship to human well-being, biodiversity conservation and land-use management. Your hard work and commitment on several field exclosure studies greatly promoted the literature in that field within recent years and not only provides the theoretical background for this review but facilitates real-world implications for land-use management and biodiversity conservation in many areas Worldwide. We wish to thank Ed Turner and one anonymous reviewer for their valuable suggestions. B.M., K.D. and T.T. were supported by the DFG (CRC 990 EFForTS) P.J.T. and T.T. by the BMBF (SPACES: Limpopo Living Landscapes), P.J.T. by the South African National Research Foundation, Department of Science and Technology, University of Venda and Southern African Macadamia Growers' Association, D.S.K. was supported by a NatureNet Science Fellowship from the Nature Conservancy. J.J.M. was supported by a grant from Bat Conservation International. N.L.M. was supported by Environment Canada and the University of Saskatchewan. L.M. was supported by the Spanish Ministry of Research and Innovation (MICINN-FEDER: CGL2007-64080-C02-01/BOS, CGL2010-18182). K.W.G. was supported by NSF grant #DBI-0610473 and Bat Conservation International, as well as by a NSF grant #DEB-0349388 to I.P. R.M.S. was supported by the State University of Santa Cruz and the Mars Center for Cocoa Science. NR 188 TC 5 Z9 5 U1 75 U2 75 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1464-7931 EI 1469-185X J9 BIOL REV JI Biol. Rev. PD NOV PY 2016 VL 91 IS 4 BP 1081 EP 1101 DI 10.1111/brv.12211 PG 21 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DZ1AG UT WOS:000385570300012 PM 26202483 ER PT J AU Ward, PS Brady, SG Fisher, BL Schultz, TR AF Ward, P. S. Brady, S. G. Fisher, B. L. Schultz, T. R. TI Phylogenetic classifications are informative, stable, and pragmatic: the case for monophyletic taxa SO INSECTES SOCIAUX LA English DT Editorial Material ID EVOLUTIONARY; HYMENOPTERA; FORMICIDAE; TAXONOMY C1 [Ward, P. S.; Schultz, T. R.] Univ Calif Davis, Dept Entomol & Nematol, Davis, CA 95616 USA. [Brady, S. G.] Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20560 USA. [Fisher, B. L.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. RP Ward, PS (reprint author), Univ Calif Davis, Dept Entomol & Nematol, Davis, CA 95616 USA. EM psward@ucdavis.edu NR 26 TC 1 Z9 1 U1 3 U2 3 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD NOV PY 2016 VL 63 IS 4 BP 489 EP 492 DI 10.1007/s00040-016-0516-9 PG 4 WC Entomology SC Entomology GA DY6PH UT WOS:000385249100002 PM 27773940 ER PT J AU Guenard, B Shik, JZ Booher, D Lubertazzi, D Alpert, G AF Guenard, B. Shik, J. Z. Booher, D. Lubertazzi, D. Alpert, G. TI Extreme polygyny in the previously unstudied subtropical ant Temnothorax tuscaloosae with implications for the biogeographic study of the evolution of polygyny SO INSECTES SOCIAUX LA English DT Article DE Biogeography; Macroecology; Life history; Polygyny; Formicidae; Temnothorax ID LEPTOTHORAX-RUGATULUS EMERY; NEST-SITE LIMITATION; HYMENOPTERA-FORMICIDAE; SOCIAL INSECTS; ENERGY GRADIENTS; QUEEN NUMBER; COLONY SIZE; CURVISPINOSUS; DIVERSITY; SOCIETIES AB Evolutionary ecologists often seek to explain life history variation at geographical scales. Progress in this regard has been slower in social insects than in unitary organisms, due in part to limited information about species distributions and the complexity of studying colony-level traits. Temnothorax ants have proven useful for investigating associations between ecology and life history traits in ants, because they have small colonies (< 200 workers) with substantial variation in traits like queen number within and across populations. Yet most of these studies have focused on < 10 Temnothorax species from northern latitudes, although the genus contains > 400 species that range from temperate to tropical biomes. Here, we generate the first global map of Temnothorax diversity and demonstrate that previous ecological hypotheses for colony life history variation in the genus are based on data and studies confined to a small part of the overall genus-level distribution. For example, studies of northern-latitude species have suggested that overwintering success is a prominent selective force favoring polygyny but little is known about polygyny in Temnothorax species from other regions. We report the highest observed queen numbers known in the genus in the subtropical species T. tuscaloosae and confirm that all queens in these polygynous colonies are mated and actively laying eggs. Behavioral laboratory experiments further indicate that this species has a fluid nest structure and lacks intraspecific aggression at the whole-forest scale. These results extend the biogeographical extent of life history studies for this genus and point to evolutionary discoveries awaiting comparative research of the global Temnothorax fauna. C1 [Guenard, B.] Univ Hong Kong, Sch Biol Sci, Pok Fu Lam, Hong Kong, Peoples R China. [Shik, J. Z.] Smithsonian Trop Res Inst, Balboa, Panama. [Shik, J. Z.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, Univ Pk 15, DK-2100 Copenhagen, Denmark. [Booher, D.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, 621 Charles E Young Dr S, Los Angeles, CA 90095 USA. [Lubertazzi, D.; Alpert, G.] Harvard Univ, Museum Comparat Zool, 26 Oxford St, Cambridge, MA 02138 USA. RP Guenard, B (reprint author), Univ Hong Kong, Sch Biol Sci, Pok Fu Lam, Hong Kong, Peoples R China. EM bguenard@hku.hk OI /0000-0001-6782-917X FU NC Division of Parks and Recreation; US Forest ServiceDepartment of Energy-Savannah River Operations Office through the U.S. Forest Service Savannah River under Interagency Agreement [DE-AI09-00SR22188] FX We dedicate this paper to E. O. Wilson who described T. tuscaloosae in 1951 in his first taxonomic paper on ants. We would like to thank Tim Linksvayer and Joe MacGown for providing us records, respectively, from Tennessee and Mississippi. Collections in State Parks of North Carolina were supported by a permit from the NC Division of Parks and Recreation. Collections in Georgia National Forests were supported by a permit from the US Forest Service. Collections conducted in Virginia, West Virginia and Lake Raleigh (NC) were performed on private lands with permission from their respective owners. Ed Olson and John Blake for their assistance in locating field sites at Savannah River Site, a National Environmental Research Park. Logistical support was provided by the Department of Energy-Savannah River Operations Office through the U.S. Forest Service Savannah River under Interagency Agreement DE-AI09-00SR22188. Mike Joyce and the U.S. Forest service for permitting research insect collections. NR 70 TC 0 Z9 0 U1 9 U2 9 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD NOV PY 2016 VL 63 IS 4 BP 543 EP 551 DI 10.1007/s00040-016-0498-7 PG 9 WC Entomology SC Entomology GA DY6PH UT WOS:000385249100008 ER PT J AU Warren, RJ Chick, LD DeMarco, B McMillan, A De Stefano, V Gibson, R Pinzone, P AF Warren, R. J., II Chick, L. D. DeMarco, B. McMillan, A. De Stefano, V. Gibson, R. Pinzone, P. TI Climate-driven range shift prompts species replacement SO INSECTES SOCIAUX LA English DT Article DE Aphaenogaster; Rudis complex; Hybridization; Traits; Phenotypic plasticity; Phylogenetics ID ANT HYBRID ZONE; HYMENOPTERA-FORMICIDAE; POLEWARD SHIFTS; POPULATIONS; PHYLOGENY; DIVERSITY; COMPLEX; FIRE; DIFFERENTIATION; SALAMANDERS AB Climate change prompts warm-tolerant species upward and poleward to either displace or replace cold-tolerant species. Warm-tolerant species may replace cold-tolerant individuals with upward migration, or cold-tolerant genes if the species hybridize. We examined genetic and morphological differences between low elevation, warm-tolerant (Aphaenogaster rudis) and high elevation cold-tolerant (A. picea) ant species that form an upward-shifting ecotone in the southern Appalachian Mountains (USA). The A. picea/A. rudis ecotone shifted upward ca. 200 m between the decades 1970 and 2010, and characteristic morphological traits appeared muddled where the species met, suggesting hybridization. However, we found no evidence of genetic hybridization, and the trait most associated with species identity, pigmentation, remained so across the environmental gradients. Conversely, femur length did not differentiate well between species identities, and it shifted across the environmental gradients. These results suggest that the cold tolerant A. picea, associated with high-elevation and high-latitude, was replaced by the warm-tolerant, low elevation A. rudis species. As such, these results suggest that less competitive cold-tolerant species may be replaced by more competitive cold-intolerant species with climate warming. C1 [Warren, R. J., II; McMillan, A.; De Stefano, V.; Gibson, R.; Pinzone, P.] SUNY Buffalo State, Dept Biol, 1300 Elmwood Ave, Buffalo, NY 14222 USA. [Chick, L. D.] Case Western Reserve Univ, Dept Biol, Cleveland, OH 44106 USA. [DeMarco, B.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Warren, RJ (reprint author), SUNY Buffalo State, Dept Biol, 1300 Elmwood Ave, Buffalo, NY 14222 USA. EM hexastylis@gmail.com FU SUNY Buffalo State Office of Undergraduate Research; National Science Foundation [1136703] FX Partial support for this research was provided by the SUNY Buffalo State Office of Undergraduate Research. Additional funding was provided to LDC through National Science Foundation Grant 1136703-Dimensions in Biodiversity: Collaborative Research: The climate cascade: functional and evolutionary consequences of climatic change on species, trait, and genetic diversity in a temperate ant community to PIs: Nate Sanders, Aaron Ellison, Nick Gotelli, Sara Helms Cahan, Bryan Ballif, and Rob Dunn. We also thank Highlands Biological Stations Director Jim Costa and staff for support; Victor Agraz, Deborah Jackson, Mary Schultz, Chris Broecker, Havish Deepnarain, Nicole Dexter, Jesse Helton, Jing Niu, Vidhyaben Patel, Zeph Pendleton, Rachel Power, Paula Reith, Morgan Spinelli for field help. We thank the Georgia Department of Natural Resources Nongame Conservation Section and the US Forest Service Chattahoochee-Oconee National Forest for permission to collect ants. We also thank Georgia Museum of Natural History Curator and Collections Manager Richard Hoebeke for loaning us Aphaenogaster specimens from R. H. Crozier's collections. NR 57 TC 0 Z9 0 U1 19 U2 19 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD NOV PY 2016 VL 63 IS 4 BP 593 EP 601 DI 10.1007/s00040-016-0504-0 PG 9 WC Entomology SC Entomology GA DY6PH UT WOS:000385249100013 ER PT J AU Sperry, JS Wang, YJ Wolfe, BT Mackay, DS Anderegg, WRL McDowell, NG Pockman, WT AF Sperry, John S. Wang, Yujie Wolfe, Brett T. Mackay, D. Scott Anderegg, William R. L. McDowell, Nate G. Pockman, William T. TI Pragmatic hydraulic theory predicts stomatal responses to climatic water deficits SO NEW PHYTOLOGIST LA English DT Article DE climate change drought; hydraulic limitation; modeling climate change impacts; plant drought responses; plant water transport; stomatal regulation; xylem cavitation; xylem transport ID FOREST DIE-OFF; XYLEM EMBOLISM; DROUGHT; CONDUCTANCE; PLANTS; CAVITATION; STRESS; MODEL; SOIL; RESISTANCE AB Ecosystem models have difficulty predicting plant drought responses, partially from uncertainty in the stomatal response to water deficits in soil and atmosphere. We evaluate a supply-demand' theory for water-limited stomatal behavior that avoids the typical scaffold of empirical response functions. The premise is that canopy water demand is regulated in proportion to threat to supply posed by xylem cavitation and soil drying. The theory was implemented in a trait-based soil-plant-atmosphere model. The model predicted canopy transpiration (E), canopy diffusive conductance (G), and canopy xylem pressure (P-canopy) from soil water potential (P-soil) and vapor pressure deficit (D). Modeled responses to D and P-soil were consistent with empirical response functions, but controlling parameters were hydraulic traits rather than coefficients. Maximum hydraulic and diffusive conductances and vulnerability to loss in hydraulic conductance dictated stomatal sensitivity and hence the iso- to anisohydric spectrum of regulation. The model matched wide fluctuations in G and P-canopy across nine data sets from seasonally dry tropical forest and pinon-juniper woodland with <26% mean error. Promising initial performance suggests the theory could be useful in improving ecosystem models. Better understanding of the variation in hydraulic properties along the root-stem-leaf continuum will simplify parameterization. C1 [Sperry, John S.; Wang, Yujie; Anderegg, William R. L.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Wolfe, Brett T.] Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Panama. [Mackay, D. Scott] SUNY Buffalo, Dept Geog, Buffalo, NY 14260 USA. [McDowell, Nate G.] Los Alamos Natl Lab, Earth & Environm Sci Div, Los Alamos, NM 87545 USA. [Pockman, William T.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. RP Sperry, JS (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM j.sperry@utah.edu RI Mackay, Scott/J-7569-2012 OI Mackay, Scott/0000-0003-0477-9755 FU National Science Foundation [IOS-1450650, IOS-1450679]; Department of Energy, Survival Mortality and Next Generation Ecosystem Experiment-Tropics FX Funded by National Science Foundation IOS-1450650, IOS-1450679, and the Department of Energy, Survival Mortality and Next Generation Ecosystem Experiment-Tropics. The manuscript benefited from thorough comments by three anonymous reviewers. NR 67 TC 5 Z9 5 U1 37 U2 37 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD NOV PY 2016 VL 212 IS 3 BP 577 EP 589 DI 10.1111/nph.14059 PG 13 WC Plant Sciences SC Plant Sciences GA DZ4AE UT WOS:000385797800008 PM 27329266 ER PT J AU Delaney, MA Ward, JM Walsh, TF Chinnadurai, SK Kerns, K Kinsel, MJ Treuting, PM AF Delaney, M. A. Ward, J. M. Walsh, T. F. Chinnadurai, S. K. Kerns, K. Kinsel, M. J. Treuting, P. M. TI Response to "Regarding Mole-rats and Cancer" SO VETERINARY PATHOLOGY LA English DT Letter ID HETEROCEPHALUS-GLABER C1 [Delaney, M. A.; Treuting, P. M.] Univ Washington, Dept Comparat Med, Seattle, WA 98195 USA. [Ward, J. M.] Global VetPathol, Montgomery Village, MD USA. [Walsh, T. F.; Kerns, K.] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. [Chinnadurai, S. K.] Chicago Zool Soc, Brookfield, IL USA. [Chinnadurai, S. K.] Brookfield Zoo, Brookfield, IL USA. [Kinsel, M. J.] Univ Illinois, Zool Pathol Program, Maywood, IL USA. RP Delaney, MA (reprint author), Univ Washington, 850 Republican St,N310, Seattle, WA 98109 USA. EM delaney.martha@gmail.com NR 6 TC 0 Z9 0 U1 2 U2 2 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 0300-9858 EI 1544-2217 J9 VET PATHOL JI Vet. Pathol. PD NOV PY 2016 VL 53 IS 6 BP 1266 EP 1267 DI 10.1177/0300985816658773 PG 2 WC Pathology; Veterinary Sciences SC Pathology; Veterinary Sciences GA DZ4HQ UT WOS:000385819700023 PM 27733704 ER PT J AU Noyce, GL Fulthorpe, R Gorgolewski, A Hazlett, P Tran, H Basiliko, N AF Noyce, Genevieve L. Fulthorpe, Roberta Gorgolewski, Adam Hazlett, Paul Honghi Tran Basiliko, Nathan TI Soil microbial responses to wood ash addition and forest fire in managed Ontario forests SO APPLIED SOIL ECOLOGY LA English DT Article DE Wood ash; Microbial communities; Bacteria; Fungi; Amplicon sequencing; Forest soil amendments ID RIBOSOMAL-RNA GENES; COMMUNITY STRUCTURE; BACTERIAL COMMUNITIES; CHEMICAL-PROPERTIES; PLANT DIVERSITY; NUTRIENT-UPTAKE; GROWTH; PH; FERTILIZATION; ECOSYSTEMS AB Wood ash is typically applied to soils to counteract acidification and base cation depletion, but the effects of this ash on the organic layer microbial community are rarely studied. We analyzed microbial responses to ash addition in two field-scale experiments in Ontario, Canada. One experiment was in a young boreal forest soil and the other was in an uneven-aged hardwood north-temperate forest soil. We also investigated the effects of a natural forest fire near the boreal experiment. In both cases, ash addition had no effect on overall microbial biomass and respiration, but increased the phylogenetic diversity of bacterial communities and the relative abundance of Bacteroidetes taxa, though effects on other bacterial taxa were site-specific. Eukaryotic effects also varied by experiment; at the boreal site, ash increased eukaryotic phylogenetic diversity and decreased the fungi:bacteria ribosomal marker ratio, but at the temperate site ash decreased eukaryotic diversity and did not affect the fungi:bacteria ratio. There was limited additional effect on the boreal soil microbial community of increasing ash addition from 0.7 to 5.7 tha(-1), as determined by T-RFLP analysis, though soil pH in both experiments increased with higher addition rates. At the temperate site, ash effects were consistently stronger for fly ash than for bottom ash. In both experiments, only 14 unique bacterial taxa were found after ash addition, and the strongest driver of overall community composition was the forest type, not ash treatment. In contrast, the soil microbial community observed at the forest fire site was clearly different. Overall, these results indicate that wood ash addition has only minimal effects on the composition of the soil microbial community in sites across two distinct global forest biomes. Published by Elsevier B.V. C1 [Noyce, Genevieve L.] Univ Toronto, Dept Geog, 100 St George St, Toronto, ON M5S 3G3, Canada. [Noyce, Genevieve L.; Fulthorpe, Roberta] Univ Toronto Scarborough, Dept Phys & Environm Sci, 1065 Mil Trail, Toronto, ON M1C 1A4, Canada. [Gorgolewski, Adam] Univ Toronto, Fac Forestry, 33 Willcocks St, Toronto, ON M5S 3B3, Canada. [Hazlett, Paul] Canadian Forest Serv, Great Lakes Forestry Ctr, 1219 Queen St E, Sault Ste Marie, ON P6A 2E5, Canada. [Honghi Tran] Univ Toronto, Dept Chem Engn & Appl Chem, 200 Coll St, Toronto, ON M5S 3E5, Canada. [Basiliko, Nathan] Laurentian Univ, Dept Biol, 840 Ramsey Lake Rd, Sudbury, ON P3E 6H5, Canada. [Basiliko, Nathan] Laurentian Univ, Vale Living Lakes Ctr, 840 Ramsey Lake Rd, Sudbury, ON P3E 6H5, Canada. [Basiliko, Nathan] Univ Toronto, Dept Geog, 3359 Mississauga Rd, Mississauga, ON L5L 1C6, Canada. RP Noyce, GL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM noyceg@si.edu FU NSERC Collaborative Research and Development Grant FX This work was supported by a NSERC Collaborative Research and Development Grant to co-authors HT and NB. Haliburton Forest and Wildlife Reserve graciously provided site access. The Island Lake Project is operated and maintained by Natural Resources Canada and the Ontario Ministry of Natural Resources in collaboration with the Northeast Superior Forest Community, Tembec, Inc., and the Northeast Superior Chiefs Forum. We thank Emma Horrigan, Kyle Lewis, and Emily Smenderovac for assisting with plot set-up, sample collection, and laboratory analyses. NR 69 TC 1 Z9 1 U1 28 U2 28 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0929-1393 EI 1873-0272 J9 APPL SOIL ECOL JI Appl. Soil Ecol. PD NOV PY 2016 VL 107 BP 368 EP 380 DI 10.1016/j.apsoil.2016.07.006 PG 13 WC Soil Science SC Agriculture GA DY1MZ UT WOS:000384860400039 ER PT J AU Bluck, AFL Mendel, JT Ellison, SL Patton, DR Simard, L Henriques, BMB Torrey, P Teimoorinia, H Moreno, J Starkenburg, E AF Bluck, Asa F. L. Mendel, J. Trevor Ellison, Sara L. Patton, David R. Simard, Luc Henriques, Bruno M. B. Torrey, Paul Teimoorinia, Hossen Moreno, Jorge Starkenburg, Else TI The impact of galactic properties and environment on the quenching of central and satellite galaxies: a comparison between SDSS, Illustris and L-Galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: kinematics and dynamics; galaxies: star formation; galaxies: structure ID SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; HALO OCCUPATION STATISTICS; STAR-FORMATION HISTORY; STELLAR MASS; HOST GALAXIES; COSMOLOGICAL SIMULATIONS; QUIESCENT GALAXIES; ELLIPTIC GALAXIES; AGN FEEDBACK AB We quantify the impact that a variety of galactic and environmental properties have on the quenching of star formation. We collate a sample of similar to 400 000 central and similar to 100 000 satellite galaxies from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Specifically, we consider central velocity dispersion (sigma(c)), stellar, halo, bulge and disc mass, local density, bulge-to-total ratio, groupcentric distance and galaxy-halo mass ratio. We develop and apply a new statistical technique to quantify the impact on the quenched fraction (f(Quench)) of varying one parameter, while keeping the remaining parameters fixed. For centrals, we find that the f(Quench)-sigma(c) relationship is tighter and steeper than for any other variable considered. We compare to the Illustris hydrodynamical simulation and the Munich semi-analytic model (L-Galaxies), finding that our results for centrals are qualitatively consistent with their predictions for quenching via radio-mode AGN feedback, hinting at the viability of this process in explaining our observational trends. However, we also find evidence that quenching in L-Galaxies is too efficient and quenching in Illustris is not efficient enough, compared to observations. For satellites, we find strong evidence that environment affects their quenched fraction at fixed central velocity dispersion, particularly at lower masses. At higher masses, satellites behave identically to centrals in their quenching. Of the environmental parameters considered, local density affects the quenched fraction of satellites the most at fixed central velocity dispersion. C1 [Bluck, Asa F. L.; Henriques, Bruno M. B.] ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Bluck, Asa F. L.; Ellison, Sara L.; Teimoorinia, Hossen] Univ Victoria, Dept Phys & Astron, 3800 Finnerty Rd, Victoria, BC V8P 1A1, Canada. [Mendel, J. Trevor] Max Planck Inst Extraterr Phys MPE, Giessenbachstr, D-85748 Garching, Germany. [Patton, David R.] Trent Univ, Dept Phys & Astron, 1600 West Bank Dr, Peterborough, ON K9J 7B8, Canada. [Simard, Luc] Natl Res Council Canada, Herzberg Inst Astrophys, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. [Torrey, Paul] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Torrey, Paul; Moreno, Jorge] CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA. [Moreno, Jorge] Calif State Polytech Univ Pomona, Dept Phys & Astron, Pomona, CA 91768 USA. [Moreno, Jorge] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Starkenburg, Else] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. RP Bluck, AFL (reprint author), ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland.; Bluck, AFL (reprint author), Univ Victoria, Dept Phys & Astron, 3800 Finnerty Rd, Victoria, BC V8P 1A1, Canada. EM asa.bluck@phys.ethz.ch OI Henriques, Bruno/0000-0002-1392-489X FU Swiss National Foundation for Sciences; National Science and Engineering Research Council (NSERC) of Canada; NSF [AST-1516364]; Emmy Noether programme from the Deutsche Forschungsgemeinschaft (DFG); Canadian Institute for Advanced Research (CIFAR); AIP Schwarzschild fellowship; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We thank Steven Bamford, Richard Bower, Marcella Carollo, Chris Conselice, Rob Crain, Will Hartley, Lars Hernquist, Simon Lilly, Avi Loeb, Laura Sales and Peter Thomas for helpful discussions on this work. We thank Kevin Schawinski for giving us the green valley test idea. We also thank the referee for many helpful and insightful comments on this work, which have contributed greatly to this version. We gratefully acknowledge funding from the Swiss National Foundation for Sciences and the National Science and Engineering Research Council (NSERC) of Canada, particularly for Discovery Grants awarded to SLE and DRP. JM is supported by NSF grant AST-1516364. ES gratefully acknowledges funding by the Emmy Noether programme from the Deutsche Forschungsgemeinschaft (DFG) as well as funding through a Canadian Institute for Advanced Research (CIFAR) global scholarship and AIP Schwarzschild fellowship.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 108 TC 3 Z9 3 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2016 VL 462 IS 3 BP 2559 EP 2586 DI 10.1093/mnras/stw1665 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XU UT WOS:000384676000020 ER PT J AU O'Connell, R Eisenstein, D Vargas, M Ho, S Padmanabhan, N AF O'Connell, Ross Eisenstein, Daniel Vargas, Mariana Ho, Shirley Padmanabhan, Nikhil TI Large covariance matrices: smooth models from the two-point correlation function SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE large-scale structure of Universe ID MATTER POWER SPECTRUM; BARYON ACOUSTIC-OSCILLATIONS; MOCK GALAXY CATALOGS; COSMOLOGY; PRECISION; Z=0.35 AB We introduce a new method for estimating the covariance matrix for the galaxy correlation function in surveys of large-scale structure. Our method combines simple theoretical results with a realistic characterization of the survey to dramatically reduce noise in the covariance matrix. For example, with an investment of only approximate to 1000 CPU hours we can produce a model covariance matrix with noise levels that would otherwise require similar to 35 000 mocks. Non-Gaussian contributions to the model are calibrated against mock catalogues, after which the model covariance is found to be in impressive agreement with the mock covariance matrix. Since calibration of this method requires fewer mocks than brute force approaches, we believe that it could dramatically reduce the number of mocks required to analyse future surveys. C1 [O'Connell, Ross; Ho, Shirley] Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. [Eisenstein, Daniel] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Vargas, Mariana] Univ Nacl Autonoma Mexico, Inst Fis, Apdo Postal 20-364, Mexico City 04510, DF, Mexico. [Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06511 USA. RP O'Connell, R (reprint author), Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. EM rcoconne@andrew.cmu.edu FU Templeton Foundation; U.S. Department of Energy [DE-SC0013718]; NASA [NNH12ZDA001N- EUCLID]; NSF [AST1412966]; DOE [DE-SC0008080]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX RCO is supported by a grant from the Templeton Foundation. DJE is supported by grant DE-SC0013718 from the U.S. Department of Energy. SH is supported by NASA NNH12ZDA001N- EUCLID and NSF AST1412966. NP is supported in part by DOE DE-SC0008080.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 27 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2016 VL 462 IS 3 BP 2681 EP 2694 DI 10.1093/mnras/stw1821 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XU UT WOS:000384676000027 ER PT J AU Ridolfi, A Freire, PCC Torne, P Heinke, CO Van Den Berg, M Jordan, C Kramer, M Bassa, CG Sarkissian, J D'Amico, N Lorimer, D Camilo, F Manchester, RN Lyne, A AF Ridolfi, A. Freire, P. C. C. Torne, P. Heinke, C. O. van den Berg, M. Jordan, C. Kramer, M. Bassa, C. G. Sarkissian, J. D'Amico, N. Lorimer, D. Camilo, F. Manchester, R. N. Lyne, A. TI Long-term observations of the pulsars in 47 Tucanae - I. A study of four elusive binary systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: general; pulsars: individual: PSR J0024-7204P; pulsars: individual: PSR J0024-7204V; pulsars: individual: PSR J0024-7204W; pulsars: individual: PSR J0024-7201X; globular clusters: individual: 47 Tucanae ID GLOBULAR-CLUSTER 47-TUCANAE; X-RAY BINARIES; VARIABLE MILLISECOND PULSAR; XSS J12270-4859; GLOBULAR-CLUSTER-47 TUCANAE; PSR J1023+0038; 1ST J102347.6+003841; INTERSTELLAR-MEDIUM; RADIO PULSAR; WHITE-DWARFS AB For the past couple of decades, the Parkes radio telescope has been regularly observing the millisecond pulsars in 47 Tucanae (47 Tuc). This long-term timing programme was designed to address a wide range of scientific issues related to these pulsars and the globular cluster where they are located. In this paper, the first of a series, we address one of these objectives: the characterization of four previously known binary pulsars for which no precise orbital parameters were known, namely 47 Tuc P, V, W and X (pulsars 47 Tuc R and Y are discussed elsewhere). We determined the previously unknown orbital parameters of 47 Tuc V and X and greatly improved those of 47 Tuc P and W. For pulsars W and X we obtained, for the first time, full coherent timing solutions across the whole data span, which allowed a much more detailed characterization of these systems. 47 Tuc W, a well-known tight eclipsing binary pulsar, exhibits a large orbital period variability, as expected for a system of its class. 47 Tuc X turns out to be in a wide, extremely circular, 10.9-d long binary orbit and its position is similar to 3.8 arcmin away from the cluster centre, more than three times the distance of any other pulsar in 47 Tuc. These characteristics make 47 Tuc X a very different object with respect to the other pulsars of the cluster. C1 [Ridolfi, A.; Freire, P. C. C.; Torne, P.; Heinke, C. O.; Kramer, M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Heinke, C. O.] Univ Alberta, Dept Phys, CCIS 4-183, Edmonton, AB T6G 2E1, Canada. [van den Berg, M.] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. [van den Berg, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Jordan, C.; Kramer, M.; Lyne, A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Bassa, C. G.] Netherlands Inst Radio Astron, ASTROA, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Sarkissian, J.; Manchester, R. N.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Box 76, Epping, NSW 1710, Australia. [D'Amico, N.] INAF, Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy. [D'Amico, N.] Univ Cagliari, Dipartimento Fis, SP Monserrato Sestu Km 0,7, I-90042 Monserrato, CA, Italy. [Lorimer, D.] West Virginia Univ, Dept Phys & Astron, POB 6315, Morgantown, WV 26506 USA. [Camilo, F.] Sq Kilometre Array South Africa, ZA-7405 Pinelands, South Africa. RP Ridolfi, A; Freire, PCC (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM aridolfi@mpifr-bonn.mpg.de; pfreire@mpifr-bonn.mpg.de FU European Research Council BEACON [279702]; Bonn-Cologne Graduate School of Physics and Astronomy; NSERC; Alexander von Humboldt Fellowship; European Research Council under European Union/ERC [337062] FX AR and PF gratefully acknowledge financial support by the European Research Council for the ERC Starting grant BEACON under contract no. 279702. AR and PT are members of the International Max Planck research school for Astronomy and Astrophysics at the Universities of Bonn and Cologne. AR acknowledges partial support through the Bonn-Cologne Graduate School of Physics and Astronomy. CH acknowledges support from an NSERC Discovery Grant and an Alexander von Humboldt Fellowship, and is grateful for the hospitality of MPIfR. CGB acknowledges support from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. 337062 (DRAGNET; PI: Jason Hessels). We especially thank Ralph Eatough for observations, significant assistance with the data handling and for stimulating discussions on pulsar searches. AR also thanks Golam Shaifullah for nice and useful discussions. We are grateful to the anonymous referee for his comments, which helped improve the manuscript. NR 78 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2016 VL 462 IS 3 BP 2918 EP 2933 DI 10.1093/mnras/stw1850 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XU UT WOS:000384676000044 ER PT J AU Price, DC Clark, MA Barsdell, BR Babich, R Greenhill, LJ AF Price, D. C. Clark, M. A. Barsdell, B. R. Babich, R. Greenhill, L. J. TI Optimizing performance-per-watt on GPUs in high performance computing SO COMPUTER SCIENCE-RESEARCH AND DEVELOPMENT LA English DT Article DE Performance per watt; Power efficiency; Radio astronomy; HPC; GPU; DVFS ID TELESCOPE; VOLTAGE; POWER AB The magnitude of the real-time digital signal processing challenge attached to large radio astronomical antenna arrays motivates use of high performance computing (HPC) systems. The need for high power efficiency at remote observatory sites parallels that in HPC broadly, where efficiency is a critical metric. We investigate how the performance-per-watt of graphics processing units (GPUs) is affected by temperature, core clock frequency and voltage. Our results highlight how the underlying physical processes that govern transistor operation affect power efficiency. In particular, we show experimentally that GPU power consumption increases non-linearly (quadratic) with both temperature and supply voltage, as predicted by physical transistor models. We show lowering GPU supply voltage and increasing clock frequency while maintaining a low die temperature increases the power efficiency of an NVIDIA K20 GPU by up to 37-48 % over default settings when running xGPU, a compute-bound code used in radio astronomy. We discuss how automatic temperature-aware and application-dependent voltage and frequency scaling (T-DVFS and A-DVFS) may provide a mechanism to achieve better power efficiency for a wider range of compute codes running on GPUs. C1 [Price, D. C.; Barsdell, B. R.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 01238 USA. [Clark, M. A.; Babich, R.] NVIDIA, 2701 San Tomas Expy, Santa Clara, CA 95050 USA. RP Price, DC (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 01238 USA. EM dprice@cfa.harvard.edu NR 23 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1865-2034 EI 1865-2042 J9 COMPUT SCI-RES DEV JI Comput. Sci.-Res. Dev. PD NOV PY 2016 VL 31 IS 4 BP 185 EP 193 DI 10.1007/s00450-015-0300-5 PG 9 WC Computer Science, Hardware & Architecture SC Computer Science GA DX5DQ UT WOS:000384400400004 ER PT J AU Hinkle, MAG Flynn, ED Catalano, JG AF Hinkle, Margaret A. G. Flynn, Elaine D. Catalano, Jeffrey G. TI Structural response of phyllomanganates to wet aging and aqueous Mn(II) SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Manganese oxides; Birnessite; Phyllomanganates; Redox reactions ID X-RAY-DIFFRACTION; BIOGENIC MN-OXIDES; CRYSTAL-STRUCTURE DETERMINATIONS; SEDIMENT-WATER INTERFACE; METAL SORBED BIRNESSITE; MARINE BACILLUS SP.; NA-RICH BIRNESSITE; SP STRAIN SG-1; HEXAGONAL BIRNESSITE; REDUCTIVE TRANSFORMATION AB Naturally occurring Mn(IV/III) oxides are often formed through microbial Mn(II) oxidation, resulting in reactive phyllo-manganates with varying Mn(IV), Mn(III), and vacancy contents. Residual aqueous Mn(II) may adsorb in the interlayer of phyllomanganates above vacancies in their octahedral sheets. The potential for interlayer Mn(II)-layer Mn(IV) comproportionation reactions and subsequent formation of structural Mn(III) suggests that aqueous Mn(II) may cause phyllomanganate structural changes that alters mineral reactivity or trace metal scavenging. Here we examine the effects of aging phyllomanganates with varying initial vacancy and Mn(III) content in the presence and absence of dissolved Mn(II) at pH 4 and 7. Three phyllomanganates were studied: two exhibiting turbostratic layer stacking (delta-MnO2 with high vacancy content and hexagonal birnessite with both vacancies and Mn(III) substitutions) and one with rotationally ordered layer stacking (triclinic birnessite containing predominantly Mn(III) substitutions). Structural analyses suggest that during aging at pH 4, Mn(II) adsorbs above vacancies and promotes the formation of phyllomanganates with rotationally ordered sheets and mixed symmetries arranged into supercells, while structural Mn(III) undergoes disproportionation. These structural changes at pH 4 correlate with reduced Mn(II) uptake onto triclinic and hexagonal birnessite after 25 days relative to 48 h of reaction, indicating that phyllomanganate reactivity decreases upon aging with Mn(II), or that recrystallization processes involving Mn(II) uptake occur over 25 days. At pH 7, Mn(II) adsorbs and causes limited structural effects, primarily increasing sheet stacking in delta-MnO2. These results show that aging-induced structural changes in phyllomanganates are affected by aqueous Mn(II), pH, and initial solid-phase Mn(III) content. Such restructuring likely alters manganese oxide reactions with other constituents in environmental and geologic systems, particularly trace metals and redox-active compounds. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Hinkle, Margaret A. G.; Flynn, Elaine D.; Catalano, Jeffrey G.] Washington Univ, Dept Earth & Planetary Sci, 1 Brookings Dr, St Louis, MO 63130 USA. RP Hinkle, MAG (reprint author), Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. EM mhinkle@eps.wustl.edu RI Catalano, Jeffrey/A-8322-2013; OI Catalano, Jeffrey/0000-0001-9311-977X; Hinkle, Margaret/0000-0003-2652-1683 FU U.S. National Science Foundation (NSF), Division of Earth Sciences, Geobiology and Low-Temperature Geochemistry Program [EAR-1056480]; NSF Graduate Research Fellowship program [DGE-1143954]; NSF [ECS-0335765, EAR-1161543]; Northwestern University; E.I. DuPont de Nemours Co.; Dow Chemical Company; DOE Office of Science by Argonne National Laboratory [DE-AC02-06CH11357] FX The U.S. National Science Foundation (NSF), Division of Earth Sciences, Geobiology and Low-Temperature Geochemistry Program supported this research through Grant No. EAR-1056480. Flynn was also supported by the NSF Graduate Research Fellowship program through Grant No. DGE-1143954. The facilities and instruments maintained by the Nano Research Facility at Washington University, supported by the NSF through Award No. ECS-0335765, were used to conduct ICP-OES analyses. XRD patterns were collected with the Bruker D8 Advance XRD instrument at Washington University in St. Louis, supported by the NSF through Award No. EAR-1161543. The pH 7 MES-buffer and pH 4 experiment XAFS spectra in this study were collected at the DuPont-Northwestern-Dow Collaborative Access Team (DND-CAT) located at Sector 5 of the Advanced Photon Source (APS). DND-CAT is supported by Northwestern University, E.I. DuPont de Nemours & Co., and The Dow Chemical Company. The pH 7 XAFS spectra were collected at APS beamline 12-BM-B. The APS is a U.S. Department of Energy (DOE) Office of Science User Facility operated for the DOE Office of Science by Argonne National Laboratory under Contract No. DE-AC02-06CH11357. The authors would particularly like to thank Qing Ma for his help in setting up and collecting XAFS spectra at 5-BM-D and Sungsik Lee and Benjamin Reinhart for their support of data collection at beamline 12-BM-B. NR 83 TC 1 Z9 1 U1 13 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD NOV PY 2016 VL 192 BP 220 EP 234 DI 10.1016/j.gca.2016.07.035 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DX1DK UT WOS:000384105700012 ER PT J AU Vitoria, AP Vieira, TD Camargo, PD Santiago, LS AF Vitoria, Angela Pierre Vieira, Tatiane de Oliveira Camargo, Plinio de Barbosa Santiago, Louis S. TI Using leaf delta C-13 and photosynthetic parameters to understand acclimation to irradiance and leaf age effects during tropical forest regeneration SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Young leaves; Mature leaves; Irradiance gradient; Forest ecophysiology; Carbon isotope composition; Atlantic forest ID CARBON-ISOTOPE DISCRIMINATION; BRAZILIAN ATLANTIC FOREST; WATER-USE EFFICIENCY; RIO-DE-JANEIRO; FRENCH-GUIANA; STABLE-CARBON; RAIN-FOREST; CHLOROPHYLL FLUORESCENCE; PLANT-COMMUNITIES; NITROGEN-CONTENT AB Regenerating forests are important for the maintenance of tropical biodiversity. Forest management in fragments of Atlantic forest in Brazil includes removal of exotic eucalyptus trees that were once part of plantations, in order to reestablish native flora. However, it is unclear how native tree saplings regenerating under former plantations respond to abrupt changes in environmental conditions associated, with exotic tree removal. We used leaf carbon isotope composition (delta C-13) and photosynthetic parameters to evaluate physiological responses of native tree saplings to canopy opening. We analyzed young and mature leaves of the three most representative species of regenerating trees (Byrsonima sericea, Siparuna guianensis, Xylopia sericea) in one secondary forest fragment and three managed areas that form an irradiance gradient (9, 85, 230 and 550 mu mol m(-2) s(-1)) in Brazilian Atlantic forest. Eucalyptus removal increased photosynthetic CO2 assimilation and stomatal conductance in mature leaves of all species, but there was no change in intercellular CO2 concentration. In young leaves, two species showed increasing A and one species showed increasing gs in response to canopy opening. Leaf delta C-13 did not vary significantly among species, but site and age affected delta C-13, as leaves from shaded sites showed lower delta C-13 values (around -33 parts per thousand) than leaves from lighter sites (around -30 parts per thousand), and young leaves showed higher delta C-13 values (around -30 parts per thousand) than mature leaves (around -32 parts per thousand). Mature leaves showed greater photosynthesis and stomatal conductance than young leaves. The sensitivity of young leaf delta C-13 to irradiance increases suggests that delta C-13 in these organs is controlled not only through carbon imported to new leaves during growth, but also through direct responses of stomatal control and carboxylation as these young leaves develop their photosynthetic competency. Young and mature leaves showed decreased total chlorophyll/carotenoids with increasing irradiance, indicating acclimation capacity from early developmental phases. Young leaves in high irradiance sites showed susceptibility to irradiance stress (F-v/F-m, around 0.7), but values for mature leaves did not show high irradiance stress (F-v/F-m around 0.8). In conclusion, forest management affected leaf delta C-13 of the main regenerating understary species, with site effects being more important than species-specific features for photosynthetic performance. The data also indicate that these species are resilient to forest management that includes exotic eucalyptus canopy tree removal. In this context, carbon stable isotopes can be considered as recorders of ecological change and can be used to study the effects of management on forest regeneration and photosynthetic competency. (C) 2016 Elsevier B.V. All rights reserved. C1 [Vitoria, Angela Pierre; Vieira, Tatiane de Oliveira] Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, UENF, CBB, Ave Alberto Lamego 2000,Parque Calif, BR-28013602 Campos Dos Goytacazes, RJ, Brazil. [Camargo, Plinio de Barbosa] Ctr Energia Nucl Agr, Ave Centenario 303, BR-13416000 Piracicaba, SP, Brazil. [Santiago, Louis S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. RP Vitoria, AP (reprint author), Univ Estadual Norte Fluminense, Lab Ciencias Ambientais, UENF, CBB, Ave Alberto Lamego 2000,Parque Calif, BR-28013602 Campos Dos Goytacazes, RJ, Brazil. EM apvitoria@gmail.com RI Camargo, Plinio/D-6635-2012 FU CAPES - Brazil (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior) [5656/14-1]; Botany and Plant Sciences Department at the University of California Riverside; USDA National Institute of Food and Agriculture FX The first author thanks the CAPES - Brazil (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior) for the Estagio Senior Exterior fellowship (process # 5656/14-1), and the last author thanks the Botany and Plant Sciences Department at the University of California Riverside and the USDA National Institute of Food and Agriculture for support. The authors thank Luiz Antonio Martinelli for suggestions in the Introduction section and ReBio Uniao. NR 66 TC 0 Z9 0 U1 34 U2 34 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 EI 1872-7042 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD NOV 1 PY 2016 VL 379 BP 50 EP 60 DI 10.1016/j.foreco.2016.07.048 PG 11 WC Forestry SC Forestry GA DW7FM UT WOS:000383816600006 ER PT J AU Egan, AN Vatanparast, M Cagle, W AF Egan, Ashley N. Vatanparast, Mohammad Cagle, William TI Parsing polyphyletic Pueraria: Delimiting distinct evolutionary lineages through phylogeny SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Character evolution; Fabaceae; Phylogeny; Polyphyly; Pueraria; Taxonomy; Neustanthus; Haymondia; Toxicopueraria; Teyleria ID MULTIPLE SEQUENCE ALIGNMENT; SYSTEMATIC SIGNIFICANCE; COMPOUND INFLORESCENCE; ARABIDOPSIS-THALIANA; CHLOROPLAST CAPTURE; PAPILIONOID LEGUMES; MAXIMUM-LIKELIHOOD; FLOWERING PLANTS; DNA-SEQUENCES; NUCLEAR-DNA AB Several taxonomic and phylogenetic studies have hypothesized polyphyly within Pueraria DC., a genus comprising 19 species (24 with varieties) including the highly invasive Pueraria montana var. lobata (Kudzu) introduced to the U.S.A. about 150 years ago. Previous efforts to investigate monophyly of the genus have been hampered by limited taxon sampling or a lack of comprehensive evolutionary context that would enable definitive taxonomic associations. This work presents a comprehensive phylogenetic investigation of Pueraria within the context of tribe Phaseoleae (Leguminosae). Polyphyly was found to be more extensive than previously thought, with five distinct lineages spread across the tribe and spanning over 25 mya of divergence strongly supported by two chloroplast and one nuclear marker, AS2, presented here as a phylogenetic marker for the first time. Our phylogenies support taxonomic revisions to rectify polyphyly within Pueraria, including the resurrection of Neustanthus, moving one species to Teyleria, and the creation of two new genera, Haymondia and Toxicopueraria (taxonomic revisions published elsewhere). Published by Elsevier Inc. C1 [Egan, Ashley N.; Vatanparast, Mohammad] Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, MRC 166,10th & Constitut Ave NW, Washington, DC 20560 USA. [Cagle, William] East Carolina Univ, Dept Biol, Howell Sci Complex, Greenville, NC 27858 USA. [Cagle, William] Campbell Univ, Sch Osteopath Med, Buies Creek, NC 27506 USA. RP Egan, AN (reprint author), Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, MRC 166,10th & Constitut Ave NW, Washington, DC 20560 USA. EM egana@si.edu FU East Carolina University; Smithsonian Institution National Museum of Natural History; U.S. National Science Foundation [DEB-1352217] FX We express thanks to the curators of the following herbaria for access to or loans of specimens: US, K, P, BKF, GH, E, MO, NY, KUN, CDBI, HZU, and HITBC. Thanks to Xin-Fen Gao, Xu Bo, Tadashi Kajita, Tomoko Otao, Tetsukazu Yahara, Firouzeh Javadi, Luxian Liu, and Chengxin Fu for locality information and logistical support in the field and to two anonymous reviewers who helped improve the manuscript. We sincerely thank East Carolina University and the Smithsonian Institution National Museum of Natural History for support. This work was supported by the U.S. National Science Foundation (DEB-1352217). NR 117 TC 0 Z9 0 U1 34 U2 35 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD NOV PY 2016 VL 104 BP 44 EP 59 DI 10.1016/j.ympev.2016.08.001 PG 16 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA DV8WJ UT WOS:000383217100005 PM 27495827 ER PT J AU Miranda, LS Collins, AG Hirano, YM Mills, CE Marques, AC AF Miranda, Lucilia S. Collins, Allen G. Hirano, Yayoi M. Mills, Claudia E. Marques, Antonio C. TI Comparative internal anatomy of Staurozoa (Cnidaria), with functional and evolutionary inferences SO PEERJ LA English DT Article DE Medusozoa; Stauromedusae; Histology; Morphology; Taxonomy; Nematogenesis; Gonad; Reproduction; Claustrum ID HALICLYSTUS-ANTARCTICUS; CHARACTER EVOLUTION; SESSILE SCYPHOZOAN; PHYLUM-CNIDARIA; NERVOUS-SYSTEM; RDNA DATA; STAUROMEDUSAE; PHYLOGENY; REPRODUCTION; PHYSIOLOGY AB Comparative efforts to understand the body plan evolution of stalked jellyfishes are scarce. Most characters, and particularly internal anatomy, have neither been explored for the class Staurozoa, nor broadly applied in its taxonomy and classification. Recently, a molecular phylogenetic hypothesis was derived for Staurozoa, allowing for the first broad histological comparative study of staurozoan taxa. This study uses comparative histology to describe the body plans of nine staurozoan species, inferring functional and evolutionary aspects of internal morphology based on the current phylogeny of Staurozoa. We document rarely-studied structures, such as ostia between radial pockets, intertentacular lobules, gametoducts, pad-like adhesive structures, and white spots of nematocysts (the last four newly proposed putative synapomorphies for Staurozoa). Two different regions of nematogenesis are documented. This work falsifies the view that the peduncle region of stauromedusae only retains polypoid characters; metamorphosis from stauropolyp to stauromedusa occurs both at the apical region (calyx) and basal region (peduncle). Intertentacular lobules, observed previously in only a small number of species, are shown to be widespread. Similarly, gametoducts were documented in all analyzed genera, both in males and females, thereby elucidating gamete release. Finally, ostia connecting adjacent gastric radial pockets appear to be universal for Staurozoa. Detailed histological studies of medusozoan polyps and medusae are necessary to further understand the relationships between staurozoan features and those of other medusozoan cnidarians. C1 [Miranda, Lucilia S.; Marques, Antonio C.] Univ Sao Paulo, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20560 USA. [Hirano, Yayoi M.] Nat Hist Museum & Inst, Coastal Branch, Katsuura, Chiba, Japan. [Mills, Claudia E.] Univ Washington, Friday Harbor Labs, Washington, DC USA. [Mills, Claudia E.] Univ Washington, Dept Biol, Washington, DC USA. [Marques, Antonio C.] Univ Sao Paulo, Ctr Biol Marinha, Sao Sebastiao, SP, Brazil. RP Miranda, LS (reprint author), Univ Sao Paulo, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. EM mirandals@ib.usp.br RI Miranda, Lucilia/L-4930-2015 FU FAPESP [2010/07362-7, 2015/23695-0, 2010/52324-6, 2011/50242-5, 2013/50484-4]; CNPq [142270/2010-5, 165066/2014-8, 474672/2007-7, 563106/2010-7, 562143/2010-6, 477156/2011-8, 305805/2013-4, 445444/2014-2]; CAPES/PDSE [16499/12-3] FX This study was supported by: FAPESP 2010/07362-7 (LSM), 2015/23695-0 (LSM), 2010/52324-6 (ACM), 2011/50242-5 (ACM), 2013/50484-4 (ACM); CNPq 142270/2010-5 (LSM), 165066/2014-8 (LSM), 474672/2007-7 (ACM), 563106/2010-7 (ACM), 562143/2010-6 (ACM), 477156/2011-8 (ACM), 305805/2013-4 (ACM), 445444/2014-2 (ACM); CAPES/PDSE: 16499/12-3 (LSM). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 83 TC 1 Z9 1 U1 10 U2 10 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD OCT 27 PY 2016 VL 4 AR e2594 DI 10.7717/peerj.2594 PG 83 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB2DQ UT WOS:000387168200005 PM 27812408 ER PT J AU Lyons, SK Miller, JH Amatangel, KL Behrensmeyer, AK Bercovici, A Blois, JL Davis, M DiMichele, W Du, A Eronen, JT Faith, JT Graves, GR Jud, N Labandeira, C Looy, CV McGill, B Patterson, D Pineda-Munoz, S Potts, R Riddle, B Terry, R Toth, A Ulrich, W Villasenor, A Wing, S Anderson, H Anderson, J Gotelli, NJ AF Lyons, S. Kathleen Miller, Joshua H. Amatangel, Kathryn L. Behrensmeyer, Anna K. Bercovici, Antoine Blois, Jessica L. Davis, Matt DiMichele, William Du, Andrew Eronen, Jussi T. Faith, J. Tyler Graves, Gary R. Jud, Nathan Labandeira, Conrad Looy, Cindy V. McGill, Brian Patterson, David Pineda-Munoz, Silvia Potts, Richard Riddle, Brett Terry, Rebecca Toth, Aniko Ulrich, Werner Villasenor, Amelia Wing, Scott Anderson, Heidi Anderson, John Gotelli, Nicholas J. TI How foreign is the past? Reply SO NATURE LA English DT Letter ID CONSERVATION; PLANT C1 [Lyons, S. Kathleen; Bercovici, Antoine; DiMichele, William; Pineda-Munoz, Silvia; Toth, Aniko; Wing, Scott] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Miller, Joshua H.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Amatangel, Kathryn L.] SUNY Coll Brockport, Dept Environm Sci & Biol, Brockport, NY 14420 USA. [Behrensmeyer, Anna K.; Blois, Jessica L.] Univ Calif Merced, Sch Nat Sci, 5200 North Lake Rd, Merced, CA 95343 USA. [Davis, Matt] Yale Univ, Dept Geol & Geophys, POB 6666, New Haven, CT 06520 USA. [Du, Andrew; Patterson, David; Villasenor, Amelia] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Eronen, Jussi T.] Univ Helsinki, Dept Geosci & Geog, FIN-00014 Helsinki, Finland. [Faith, J. Tyler] Univ Queensland, Sch Social Sci, Brisbane, Qld 4072, Australia. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen, Denmark. [Jud, Nathan] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Labandeira, Conrad] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad] Capital Normal Univ, Key Lab Insect Evolut & Environm Changes, Beijing 100048, Peoples R China. [Looy, Cindy V.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Looy, Cindy V.] Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA. [McGill, Brian] Univ Maine, Sch Biol & Ecol & Sustainabil Solut Initiat, Orono, ME 04469 USA. [Potts, Richard] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Dept Anthropol, Washington, DC 20013 USA. [Riddle, Brett] Univ Nevada, Sch Life Sci, Las Vegas, NV 89154 USA. [Terry, Rebecca] Oregon State Univ, Dept Integrat Biol, Corvallis, OR 97731 USA. [Ulrich, Werner] Nicolaus Copernicus Univ, Chair Ecol & Biogeog, Lwowska 1, PL-87100 Torun, Poland. [Anderson, Heidi; Anderson, John] Univ Witwatersrand, Evolutionary Studies Inst, ZA-20150 Johannesburg, South Africa. [Gotelli, Nicholas J.] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. RP Lyons, SK (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM lyonss2@si.edu RI Eronen, Jussi/B-7978-2013; McGill, Brian/A-3476-2008; Blois, Jessica/G-5893-2011; publicationpage, cmec/B-4405-2017 OI Eronen, Jussi/0000-0002-0390-8044; McGill, Brian/0000-0002-0850-1913; Blois, Jessica/0000-0003-4048-177X; NR 7 TC 0 Z9 0 U1 13 U2 13 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD OCT 27 PY 2016 VL 538 IS 7626 BP E3 EP + DI 10.1038/nature20096 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EA5IY UT WOS:000386654400002 PM 27786209 ER PT J AU Chang, B Croson, M Straker, L Gart, S Dove, C Gerwin, J Jung, S AF Chang, Brian Croson, Matthew Straker, Lorian Gart, Sean Dove, Carla Gerwin, John Jung, Sunghwan TI How seabirds plunge-dive without injuries SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE diving; seabirds; buckling; injury; water entry ID NORTHERN GANNETS; SULA-BASSANA; WATER; ACCOMMODATION; UNDERWATER; EVOLUTION; BEHAVIOR; FRACTURE; PURSUIT; OPTICS AB In nature, several seabirds (e.g., gannets and boobies) dive into water at up to 24 m/s as a hunting mechanism; furthermore, gannets and boobies have a slender neck, which is potentially the weakest part of the body under compression during high-speed impact. In this work, we investigate the stability of the bird's neck during plunge-diving by understanding the interaction between the fluid forces acting on the head and the flexibility of the neck. First, we use a salvaged bird to identify plunge-diving phases. Anatomical features of the skull and neck were acquired to quantify the effect of beak geometry and neck musculature on the stability during a plunge-dive. Second, physical experiments using an elastic beam as a model for the neck attached to a skull-like cone revealed the limits for the stability of the neck during the bird's dive as a function of impact velocity and geometric factors. We find that the neck length, neck muscles, and diving speed of the bird predominantly reduce the likelihood of injury during the plunge-dive. Finally, we use our results to discuss maximum diving speeds for humans to avoid injury. C1 [Chang, Brian; Croson, Matthew; Gart, Sean; Jung, Sunghwan] Virginia Polytech Inst & State Univ, Dept Biomed Engn & Mech, Blacksburg, VA 24061 USA. [Straker, Lorian; Dove, Carla] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Straker, Lorian] Univ Fed Rio de Janeiro, Setor Ornitol, Museu Nacl, BR-20940040 Rio De Janeiro, RJ, Brazil. [Gerwin, John] North Carolina Museum Nat Sci, Raleigh, NC 27601 USA. RP Jung, S (reprint author), Virginia Polytech Inst & State Univ, Dept Biomed Engn & Mech, Blacksburg, VA 24061 USA. EM sunnyjsh@vt.edu FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico Grant [246819/2013-8]; Virginia Tech Institute for Critical Technology and Applied Science; National Science Foundation [CBET-1336038, PHYS-1205642] FX We thank Alex Ochs, Grace Ma, Andrew Marino, Thomas Moore, and Yuan-nan Young for their initial contributions. This work was partially supported by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico Grant 246819/2013-8 (to L.S.), Virginia Tech Institute for Critical Technology and Applied Science, and National Science Foundation Grants CBET-1336038 (to B.C., S.G., and S.J.) and PHYS-1205642 (to S.G. and S.J.). NR 39 TC 1 Z9 1 U1 16 U2 16 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD OCT 25 PY 2016 VL 113 IS 43 BP 12006 EP 12011 DI 10.1073/pnas.1608628113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ7ZI UT WOS:000386087100032 PM 27702905 ER PT J AU Yadav, RK Gastine, T Christensen, UR Wolk, SJ Poppenhaeger, K AF Yadav, Rakesh K. Gastine, Thomas Christensen, Ulrich R. Wolk, Scott J. Poppenhaeger, Katja TI Approaching a realistic force balance in geodynamo simulations SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE geodynamo; magnetohydrodynamics; planetary dynamos; turbulence; rotating convection ID ROTATING SPHERICAL-SHELLS; CONVECTION-DRIVEN DYNAMOS; EARTHS INNER-CORE; MAGNETIC-FIELDS; MAGNETOCONVECTION; EVOLUTION; REVERSAL; MODELS; MOTION AB Earth sustains its magnetic field by a dynamo process driven by convection in the liquid outer core. Geodynamo simulations have been successful in reproducing many observed properties of the geomagnetic field. However, although theoretical considerations suggest that flow in the core is governed by a balance between Lorentz force, rotational force, and buoyancy (called MAC balance for Magnetic, Archimedean, Coriolis) with only minute roles for viscous and inertial forces, dynamo simulations must use viscosity values that are many orders of magnitude larger than in the core, due to computational constraints. In typical geodynamo models, viscous and inertial forces are not much smaller than the Coriolis force, and the Lorentz force plays a subdominant role; this has led to conclusions that these simulations are viscously controlled and do not represent the physics of the geodynamo. Here we show, by a direct analysis of the relevant forces, that a MAC balance can be achieved when the viscosity is reduced to values close to the current practical limit. Lorentz force, buoyancy, and the uncompensated (by pressure) part of the Coriolis force are of very similar strength, whereas viscous and inertial forces are smaller by a factor of at least 20 in the bulk of the fluid volume. Compared with nonmagnetic convection at otherwise identical parameters, the dynamo flow is of larger scale and is less invariant parallel to the rotation axis (less geostrophic), and convection transports twice as much heat, all of which is expected when the Lorentz force strongly influences the convection properties. C1 [Yadav, Rakesh K.; Wolk, Scott J.; Poppenhaeger, Katja] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Yadav, Rakesh K.; Gastine, Thomas; Christensen, Ulrich R.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Gastine, Thomas] Univ Paris Diderot, Sorbonne Paris Cite, Inst Phys Globe Paris, UMR CNRS 7154, F-75005 Paris, France. [Poppenhaeger, Katja] Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. RP Yadav, RK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Yadav, RK (reprint author), Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. EM rakesh.yadav@cfa.harvard.edu RI Yadav, Rakesh/E-2169-2017 OI Yadav, Rakesh/0000-0002-9569-2438 FU NASA [GO4-15011X, NAS8-03060]; Deutsche Forschungsgemeinschaft [SFB 963/A17] FX We thank the two anonymous referees for very constructive comments. Funding from NASA (through the Chandra Grant GO4-15011X) and Deutsche Forschungsgemeinschaft (through SFB 963/A17) is acknowledged. S.J.W. was supported by NASA Contract NAS8-03060. Simulations were performed at Gesellschaft fur wissenschaftliche Datenverarbeitung mbH Gottingen (GWDG) and Rechenzentrum Garching der Max-Planck-Gesellschaft (RZG). NR 41 TC 1 Z9 1 U1 3 U2 3 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD OCT 25 PY 2016 VL 113 IS 43 BP 12065 EP 12070 DI 10.1073/pnas.1608998113 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ7ZI UT WOS:000386087100042 PM 27790991 ER PT J AU Presnell, JS Vandepas, LE Warren, KJ Swalla, BJ Amemiya, CT Browne, WE AF Presnell, Jason S. Vandepas, Lauren E. Warren, Kaitlyn J. Swalla, Billie J. Amemiya, Chris T. Browne, William E. TI The Presence of a Functionally Tripartite Through-Gut in Ctenophora Has Implications for Metazoan Character Trait Evolution SO CURRENT BIOLOGY LA English DT Article ID MNEMIOPSIS-LEIDYI; ANIMAL EVOLUTION; ORIGINS; PERSPECTIVE; EXPRESSION; ANTHOZOA; SPONGES; SYSTEM; LOBATE AB The current paradigm of gut evolution assumes that non-bilaterian metazoan lineages either lack a gut (Porifera and Placozoa) or have a sac-like gut (Ctenophora and Cnidaria) and that a through-gut originated within Bilateria [1-8]. An important group for understanding early metazoan evolution is Ctenophora (comb jellies), which diverged very early from the animal stem lineage [9-13]. The perception that ctenophores possess a sac-like blind gut with only one major opening remains a commonly held misconception [4, 5, 7, 14, 15]. Despite descriptions of the ctenophore digestive system dating to Agassiz [16] that identify two openings of the digestive system opposite of the mouth-called "excretory pores" by Chun [17], referred to as an "anus" by Main [18], and coined "anal pores" by Hyman [19]-contradictory reports, particularly prominent in recent literature, posit that waste products are primarily expelled via the mouth [4, 5, 7, 14, 19-23]. Here we demonstrate that ctenophores possess a unidirectional, functionally tripartite through-gut and provide an updated interpretation for the evolution of the metazoan through-gut. Our results resolve lingering questions regarding the functional anatomy of the ctenophore gut and long-standing misconceptions about waste removal in ctenophores. Moreover, our results present an intriguing evolutionary quandary that stands in stark contrast to the current paradigm of gut evolution: either (1) the through-gut has its origins very early in the metazoan stem lineage or (2) the ctenophore lineage has converged on an arrangement of organs functionally similar to the bilaterian through-gut. C1 [Presnell, Jason S.; Warren, Kaitlyn J.] Univ Miami, Dept Biol, Cox Sci Ctr, 1301 Mem Dr, Miami, FL 33146 USA. [Vandepas, Lauren E.; Swalla, Billie J.; Amemiya, Chris T.] Univ Washington, Dept Biol, 24 Kincaid Hall, Seattle, WA 98195 USA. [Swalla, Billie J.] Univ Washington, Friday Harbor Labs, Friday Harbor, WA 98250 USA. [Vandepas, Lauren E.; Amemiya, Chris T.] Virginia Mason, Benaroya Res Inst, 1201 Ninth Ave, Seattle, WA 98107 USA. [Browne, William E.] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. RP Browne, WE (reprint author), Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20013 USA. EM webrowne3@gmail.com RI Browne, William/D-4267-2013 OI Browne, William/0000-0001-8200-6489 FU University of Miami College of Arts and Sciences; National Science Foundation; University of Washington Department of Biology Edmondson Award FX J.S.P. was supported by the University of Miami College of Arts and Sciences. L.E.V. was supported by a Graduate Research Fellowship from the National Science Foundation and the University of Washington Department of Biology Edmondson Award. We thank Kathryn Tosney, James Baker, and Julia Dallman for comments on early versions of this manuscript. We thank Ricardo Cepeda, Joshua Swore, and Michael Rego for additional animal support. NR 48 TC 2 Z9 2 U1 6 U2 6 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 EI 1879-0445 J9 CURR BIOL JI Curr. Biol. PD OCT 24 PY 2016 VL 26 IS 20 BP 2814 EP 2820 DI 10.1016/j.cub.2016.08.019 PG 7 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA EA2DY UT WOS:000386404200050 PM 27568594 ER PT J AU Lapierre, D Alijah, A Kochanov, R Kokoouline, V Tyuterev, V AF Lapierre, David Alijah, Alexander Kochanov, Roman Kokoouline, Viatcheslav Tyuterev, Vladimir TI Lifetimes and wave functions of ozone metastable vibrational states near the dissociation limit in a full-symmetry approach SO PHYSICAL REVIEW A LA English DT Article ID POTENTIAL-ENERGY SURFACES; MASS-INDEPENDENT FRACTIONATION; CW-CRDS SPECTRA; TEMPERATURE-DEPENDENCE; O-16/O-18 ISOTOPOLOGUES; EXCHANGE-REACTION; GROUND-STATE; QUANTUM DYNAMICS; FORMATION RATES; CM(-1) REGION AB Energies and lifetimes (widths) of vibrational states above the lowest dissociation limit of O-16(3) were determined using a previously developed efficient approach, which combines hyperspherical coordinates and a complex absorbing potential. The calculations are based on a recently computed potential energy surface of ozone determined with a spectroscopic accuracy [Tyuterev et al., J. Chem. Phys. 139, 134307 (2013)]. The effect of permutational symmetry on rovibrational dynamics and the density of resonance states in O-3 is discussed in detail. Correspondence between quantum numbers appropriate for short- and long-range parts of wave functions of the rovibrational continuum is established. It is shown, by symmetry arguments, that the allowed purely vibrational (J = 0) levels of O-16(3) and O-18(3), both made of bosons with zero nuclear spin, cannot dissociate on the ground-state potential energy surface. Energies and wave functions of bound states of the ozone isotopologue O-16(3) with rotational angular momentum J = 0 and 1 up to the dissociation threshold were also computed. For bound levels, good agreement with experimental energies is found: The rms deviation between observed and calculated vibrational energies is 1 cm(-1). Rotational constants were determined and used for a simple identification of vibrational modes of calculated levels. C1 [Lapierre, David; Alijah, Alexander; Tyuterev, Vladimir] Univ Reims, CNRS, UMR 7331, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France. [Kochanov, Roman] Tomsk State Univ, Quamer Lab, Tomsk, Russia. [Kochanov, Roman] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, MS50 60 Garden St, Cambridge, MA 02138 USA. [Kokoouline, Viatcheslav] Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA. RP Lapierre, D (reprint author), Univ Reims, CNRS, UMR 7331, Grp Spectrometrie Mol & Atmospher, F-51687 Reims 2, France. RI Kochanov, Roman/E-8679-2014; Alijah, Alexander/A-4079-2013; OI Kochanov, Roman/0000-0001-5165-5099; Alijah, Alexander/0000-0002-4915-0558; Tyuterev, Vladimir/0000-0002-2181-1158 FU CNRS; National Science Foundation [PHY-15-06391]; ROMEO HPC Center at the University of Reims Champagne-Ardenne; Tomsk State University Academic D. Mendeleev funding Program; French LEFE Chat program of the Institut National des Sciences de l'Univers (CNRS); Laboratoire International Franco-Russe SAMIA FX This work is supported by the CNRS through an invited professor position for V.K. at the GSMA, the National Science Foundation, Grant No. PHY-15-06391 and the ROMEO HPC Center at the University of Reims Champagne-Ardenne. The supports from Tomsk State University Academic D. Mendeleev funding Program, from French LEFE Chat program of the Institut National des Sciences de l'Univers (CNRS), and from Laboratoire International Franco-Russe SAMIA are acknowledged. NR 96 TC 1 Z9 1 U1 10 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD OCT 21 PY 2016 VL 94 IS 4 AR 042514 DI 10.1103/PhysRevA.94.042514 PG 15 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DZ7ZW UT WOS:000386088800007 ER PT J AU Hayasaki, K Loeb, A AF Hayasaki, Kimitake Loeb, Abraham TI Detection of Gravitational Wave Emission by Supermassive Black Hole Binaries Through Tidal Disruption Flares SO SCIENTIFIC REPORTS LA English DT Article ID GALACTIC NUCLEI; ACCRETION DISKS; STAR-FORMATION; EVOLUTION; RATES; PERIODICITY; INSTABILITY; CANDIDATE; RADIATION; DYNAMICS AB Galaxy mergers produce supermassive black hole binaries, which emit gravitational waves prior to their coalescence. We perform three-dimensional hydrodynamic simulations to study the tidal disruption of stars by such a binary in the final centuries of its life. We find that the gas stream of the stellar debris moves chaotically in the binary potential and forms accretion disks around both black holes. The accretion light curve is modulated over the binary orbital period owing to relativistic beaming. This periodic signal allows to detect the decay of the binary orbit due to gravitational wave emission by observing two tidal disruption events that are separated by more than a decade. C1 [Hayasaki, Kimitake] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 361763, South Korea. [Hayasaki, Kimitake; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Hayasaki, K (reprint author), Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 361763, South Korea.; Hayasaki, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kimi@cbnu.ac.kr FU Chungbuk National University; NSF [AST-1312034] FX The authors thank to the anonymous referee for fruitful comments and suggestions. The numerical simulations were performed using a high performance computing cluster at the Korea Astronomy and Space Science Institute. This work was supported in part by the research grant of the Chungbuk National University in 2015 [K.H.] and by NSF grant AST-1312034 [A.L.]. NR 51 TC 0 Z9 0 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD OCT 21 PY 2016 VL 6 AR 35629 DI 10.1038/srep35629 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ4LD UT WOS:000385829200001 PM 27767188 ER PT J AU Brinkerink, CD Muller, C Falcke, H Bower, GC Krichbaum, TP Castillo, E Deller, AT Doeleman, SS Fraga-Encinas, R Goddi, C Hernandez-Gomez, A Hughes, DH Kramer, M Leon-Tavares, J Loinard, L Montana, A Moscibrodzka, M Ortiz-Leon, GN Sanchez-Arguelles, D Tilanus, RPJ Wilson, GW Zensus, JA AF Brinkerink, Christiaan D. Mueller, Cornelia Falcke, Heino Bower, Geoffrey C. Krichbaum, Thomas P. Castillo, Edgar Deller, Adam T. Doeleman, Sheperd S. Fraga-Encinas, Raquel Goddi, Ciriaco Hernandez-Gomez, Antonio Hughes, David H. Kramer, Michael Leon-Tavares, Jonathan Loinard, Laurent Montana, Alfredo Moscibrodzka, Monika Ortiz-Leon, Gisela N. Sanchez-Arguelles, David Tilanus, Remo P. J. Wilson, Grant W. Zensus, J. Anton TI Asymmetric structure in Sgr A* at 3 mm from closure phase measurements with VLBA, GBT and LMT SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; techniques: interferometric; galaxies: active-galaxies: jets; radio continuum: galaxies ID EVENT HORIZON SCALES; SAGITTARIUS-A; GALACTIC-CENTER; BLACK-HOLE; GRMHD SIMULATIONS; MILKY-WAY; NRAO 530; 6 CM; WAVELENGTH; SIZE AB We present the results of a closure phase analysis of 3 mm very long baseline interferometry measurements performed on Sagittarius A* (Sgr A*). We have analysed observations made in 2015 May using the Very Long Baseline Array, the Robert C. Byrd Green Bank Telescope and the Large Millimeter Telescope Alfonso Serrano and obtained non-zero closure phase measurements on several station triangles - indicative of a non-point-symmetric source structure. The data are fitted with an asymmetric source structure model in Sgr A*, represented by a simple two-component model, which favours a fainter component due east of the main source. This result is discussed in light of a scattering screen with substructure or an intrinsically asymmetric source. C1 [Brinkerink, Christiaan D.; Mueller, Cornelia; Falcke, Heino; Fraga-Encinas, Raquel; Goddi, Ciriaco; Moscibrodzka, Monika; Tilanus, Remo P. J.] Radboud Univ Nijmegen, IMAPP, Dept Astron, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands. [Mueller, Cornelia; Krichbaum, Thomas P.; Kramer, Michael; Loinard, Laurent; Zensus, J. Anton] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, 645 N Aohoku Pl, Hilo, HI 96720 USA. [Castillo, Edgar; Montana, Alfredo; Sanchez-Arguelles, David] Consejo Nacl Ciencia & Technol, Ave Insurgentes Sur 1582, Del Benito Juarez 03940, DF, Mexico. [Castillo, Edgar; Hughes, David H.; Leon-Tavares, Jonathan; Montana, Alfredo] INAOE, Apartado Postal 51 & 216, Puebla 72000, Mexico. [Deller, Adam T.] ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Doeleman, Sheperd S.] MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. [Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hernandez-Gomez, Antonio; Loinard, Laurent; Ortiz-Leon, Gisela N.] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Leon-Tavares, Jonathan] Univ Ghent, Sterrenkundig Observ, Krijgslaan 281-S9, B-9000 Ghent, Belgium. [Tilanus, Remo P. J.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Wilson, Grant W.] Univ Massachusetts, Dept Astron, LGRT B 619E,710 North Pleasant St, Amherst, MA 01003 USA. RP Brinkerink, CD; Muller, C (reprint author), Radboud Univ Nijmegen, IMAPP, Dept Astron, Heyendaalseweg 135, NL-6525 AJ Nijmegen, Netherlands.; Muller, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM c.brinkerink@astro.ru.nl; c.mueller@astro.ru.nl OI Deller, Adam/0000-0001-9434-3837 FU ERC [610058]; CONACyT, Mexico; DGAPA, UNAM FX We wish to express our gratitude to the MIT Haystack team (Lindy Blackburn, Laura Vertatschitsch, Jason Soohoo), who installed the recording system at LMT and who have played an instrumental role in making VLBI measurements possible at LMT. We thank Frank Ghigo at GBT for his help in obtaining the system temperature measurements. We thank Michael Johnson for illuminating discussions on the scattering screen and on closure phase statistics, and we appreciate the input on the draft we received from Eduardo Ros. This work is supported by the ERC Synergy Grant "BlackHoleCam: Imaging the Event Horizon of Black Holes" (Grant 610058). AH, LL, and GNO-L acknowledge the financial support of CONACyT, Mexico and DGAPA, UNAM. NR 33 TC 1 Z9 1 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 1382 EP 1392 DI 10.1093/mnras/stw1743 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100016 ER PT J AU Rappaport, S Lehmann, H Kalomeni, B Borkovits, T Latham, D Bieryla, A Ngo, H Mawet, D Howell, S Horch, E Jacobs, TL LaCourse, D Sodor, A Vanderburg, A Pavlovski, K AF Rappaport, S. Lehmann, H. Kalomeni, B. Borkovits, T. Latham, D. Bieryla, A. Ngo, H. Mawet, D. Howell, S. Horch, E. Jacobs, T. L. LaCourse, D. Sodor, A. Vanderburg, A. Pavlovski, K. TI A quintuple star system containing two eclipsing binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries : close; binaries: eclipsing; binaries: general; binaries: spectroscopic; binaries: visual ID RADIAL-VELOCITIES; TIDAL FRICTION; MULTIPLE STARS; CLOSE BINARIES; DATA RELEASE; SKY SURVEY; DATA SET; KEPLER; EVOLUTION; CATALOG AB We present a quintuple star system that contains two eclipsing binaries. The unusual architecture includes two stellar images separated by 11 arcsec on the sky: EPIC 212651213 and EPIC 212651234. The more easterly image (212651213) actually hosts both eclipsing binaries which are resolved within that image at 0.09 arcsec, while the westerly image (212651234) appears to be single in adaptive optics (AO), speckle imaging, and radial velocity (RV) studies. The 'A' binary is circular with a 5.1-d period, while the 'B' binary is eccentric with a 13.1-d period. The gamma velocities of the A and B binaries are different by similar to 10 km s(-1). That, coupled with their resolved projected separation of 0.09 arcsec, indicates that the orbital period and separation of the 'C' binary (consisting of A orbiting B) are similar to 65 yr and similar or equal to 25 au, respectively, under the simplifying assumption of a circular orbit. Motion within the C orbit should be discernible via future RV, AO, and speckle imaging studies within a couple of years. The C system (i.e. 212651213) has an RV and proper motion that differ from that of 212651234 by only similar to 1.4 km s(-1) and similar to 3 mas yr(-1). This set of similar space velocities in three dimensions strongly implies that these two objects are also physically bound, making this at least a quintuple star system. C1 [Rappaport, S.; Kalomeni, B.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Rappaport, S.; Kalomeni, B.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Lehmann, H.] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany. [Kalomeni, B.] Ege Univ, Dept Astron & Space Sci, TR-35100 Izmir, Turkey. [Borkovits, T.] Univ Szeged, Baja Astron Observ, Kt 766, H-6500 Baja, Hungary. [Latham, D.; Bieryla, A.; Vanderburg, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Ngo, H.] CALTECH, Div Geol & Planetary Sci, 1200 E Calif Blvd MC 150-21, Pasadena, CA 91125 USA. [Mawet, D.] CALTECH, Dept Astron, MC 249-17,1200 E Calif Blvd, Pasadena, CA 91125 USA. [Mawet, D.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Howell, S.] NASA, Ames Res Ctr, Kepler & Missions K2, POB 1,M-S 244-30, Moffett Field, CA 94035 USA. [Horch, E.] Southern Connecticut State Univ, Dept Phys, New Haven, CT 06515 USA. [Jacobs, T. L.] 12812 SE 69th Pl, Bellevue, WA 98006 USA. [LaCourse, D.] 7507 52nd Pl NE, Marysville, WA 98270 USA. [Sodor, A.] MTA CSFK, Konkoly Observ, Konkoly Thege M Ut 15-17, H-1121 Budapest, Hungary. [Pavlovski, K.] Univ Zagreb, Fac Sci, Dept Phys, Bijenicka Cesta 32, Zagreb 10000, Croatia. RP Rappaport, S (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA.; Rappaport, S (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM sar@mit.edu OI Ngo, Henry/0000-0001-5172-4859 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NSF Graduate Research Fellowship [DGE 1144152]; Turkish Scientific and Technical Research Council [TUBITAK-112T766, TUBITAK-BIDEP 2219]; Croatian HRZZ grant [2014-09-8656]; Hungarian NKFIH Grant [K-115709]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; NKFIH [OTKA K-113117]; Lendulet grant of the Hungarian Academy of Sciences [LP2012-31] FX We are grateful to Mark Everett for help with the WIYN observations. We thank Alan Levine for helpful discussions about this system. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. Based, in part, on data from CMC15 Data Access Service at CAB (INTA-CSIC). This work was based on observations at the W. M. Keck Observatory granted by the California Institute of Technology. We thank the observers who contributed to the measurements reported here and acknowledge the efforts of the Keck Observatory staff. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. AV is supported by the NSF Graduate Research Fellowship, Grant No. DGE 1144152. EH is grateful for support from NASA's Ames Research Center that allowed him to participate in the speckle observations and analysis. BK gratefully acknowledges the support provided by the Turkish Scientific and Technical Research Council (TUBITAK-112T766 and TUBITAK-BIDEP 2219). KP was supported by the Croatian HRZZ grant 2014-09-8656. AS acknowledges the financial support of the Hungarian NKFIH Grant K-115709 and the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. TB and AS acknowledge the financial support of the NKFIH Grant OTKA K-113117. The Konkoly observations were supported by the Lendulet grant LP2012-31 of the Hungarian Academy of Sciences. NR 57 TC 1 Z9 1 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 1812 EP 1825 DI 10.1093/mnras/stw1745 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100046 ER PT J AU Hardcastle, MJ Gurkan, G van Weeren, RJ Williams, WL Best, PN de Gasperin, F Rafferty, DA Read, SC Sabater, J Shimwell, TW Smith, DJB Tasse, C Bourne, N Brienza, M Bruggen, M Brunetti, G Chyzy, KT Conway, J Dunne, L Eales, SA Maddox, SJ Jarvis, MJ Mahony, EK Morganti, R Prandoni, I Rottgering, HJA Valiante, E White, GJ AF Hardcastle, M. J. Gurkan, G. van Weeren, R. J. Williams, W. L. Best, P. N. de Gasperin, F. Rafferty, D. A. Read, S. C. Sabater, J. Shimwell, T. W. Smith, D. J. B. Tasse, C. Bourne, N. Brienza, M. Bruggen, M. Brunetti, G. Chyzy, K. T. Conway, J. Dunne, L. Eales, S. A. Maddox, S. J. Jarvis, M. J. Mahony, E. K. Morganti, R. Prandoni, I. Rottgering, H. J. A. Valiante, E. White, G. J. TI LOFAR/H-ATLAS: a deep low-frequency survey of the Herschel-ATLAS North Galactic Pole field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; infrared: galaxies; radio continuum: galaxies ID STAR-FORMATION HISTORY; INFRARED-RADIO CORRELATION; SCIENCE DEMONSTRATION PHASE; MASS-SELECTED GALAXIES; LESS-THAN 1.0; LUMINOSITY FUNCTION; SKY SURVEY; FORMING GALAXIES; WIDE-FIELD; SDSS-III AB We present Low-Frequency Array (LOFAR) High-Band Array observations of the Herschel-ATLAS North Galactic Pole survey area. The survey we have carried out, consisting of four pointings covering around 142 deg(2) of sky in the frequency range 126-173 MHz, does not provide uniform noise coverage but otherwise is representative of the quality of data to be expected in the planned LOFAR wide-area surveys, and has been reduced using recently developed 'facet calibration' methods at a resolution approaching the full resolution of the data sets (similar to 10 x 6 arcsec) and an rms off-source noise that ranges from 100 mu Jy beam(-1) in the centre of the best fields to around 2 mJy beam(-1) at the furthest extent of our imaging. We describe the imaging, cataloguing and source identification processes, and present some initial science results based on a 5 sigma source catalogue. These include (i) an initial look at the radio/far-infrared correlation at 150 MHz, showing that many Herschel sources are not yet detected by LOFAR; (ii) number counts at 150 MHz, including, for the first time, observational constraints on the numbers of star-forming galaxies; (iii) the 150-MHz luminosity functions for active and star-forming galaxies, which agree well with determinations at higher frequencies at low redshift, and show strong redshift evolution of the star-forming population; and (iv) some discussion of the implications of our observations for studies of radio galaxy life cycles. C1 [Hardcastle, M. J.; Gurkan, G.; Williams, W. L.; Read, S. C.; Smith, D. J. B.] Univ Hertfordshire, Ctr Astrophy Res, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Best, P. N.; Sabater, J.; Bourne, N.; Dunne, L.; Maddox, S. J.] Royal Observ, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [de Gasperin, F.; Shimwell, T. W.; Rottgering, H. J. A.] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Rafferty, D. A.; Bruggen, M.] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. [Tasse, C.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France. [Brienza, M.; Morganti, R.] Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Brienza, M.; Morganti, R.] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [Brunetti, G.; Prandoni, I.] INAF Inst Radioastron, Via P Gobetti 101, I-40129 Bologna, Italy. [Chyzy, K. T.; Eales, S. A.] Jagiellonian Univ, Astron Observ, Ul Orla 171, PL-30244 Krakow, Poland. [Conway, J.] Chalmers, Onsala Space Observ, SE-43992 Onsala, Sweden. [Dunne, L.; Maddox, S. J.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Jarvis, M. J.] Oxford Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. [Jarvis, M. J.] Univ Western Cape, Dept Phys, Private Bag X17, ZA-7535 Bellville, South Africa. [Mahony, E. K.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Mahony, E. K.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW, Australia. [White, G. J.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0NL, Oxon, England. RP Hardcastle, MJ (reprint author), Univ Hertfordshire, Ctr Astrophy Res, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM m.j.hardcastle@herts.ac.uk OI Sabater, Jose/0000-0003-1149-6294; Mahony, Elizabeth/0000-0002-5053-2828; Hardcastle, Martin/0000-0003-4223-1117 FU UK Science and Technology Facilities Council [ST/M001008/1]; University of Hertfordshire; UK STFC [ST/M001229/1]; European Research Council under European Union/ERC [RADIOLIFE-320745]; ERC [321271]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Leverhulme Trust; STFC [ST/P000096/1]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX MJH and WLW acknowledge support from the UK Science and Technology Facilities Council [ST/M001008/1]. GG thanks the University of Hertfordshire for a research studentship. PNB is grateful for support from the UK STFC via grant ST/M001229/1. RM gratefully acknowledges support from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013) ERC Advanced Grant RADIOLIFE-320745. TWS acknowledges support from the ERC Advanced Investigator programme NewClusters 321271. LD and SJM acknowledge support from ERC Advanced and Consolidator grants Cosmic ISM and Cosmic Dust. EKM acknowledges support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. GJW gratefully acknowledges support from the Leverhulme Trust.; This research has made use of the University of Hertfordshire high-performance computing facility (http://stri-cluster.herts.ac.uk/) and the LOFAR-UK computing facility located at the University of Hertfordshire and supported by STFC [ST/P000096/1]. This research made use of ASTROPY, a community-developed core PYTHON package for astronomy (Astropy Collaboration et al. 2013) hosted at http://www.astropy.org/, of APLPY, an open-source astronomical plotting package for PYTHON hosted at http://aplpy.github.com/, and of TOPCAT and STILTS (Taylor 2005).; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 120 TC 4 Z9 4 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2016 VL 462 IS 2 BP 1910 EP 1936 DI 10.1093/mnras/stw1763 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX8XE UT WOS:000384674100053 ER PT J AU Hull, CLH Girart, JM Zhang, QZ AF Hull, Charles L. H. Girart, Josep M. Zhang, Qizhou TI 880 mu m SMA POLARIZATION OBSERVATIONS OF THE QUASAR 3C 286 SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: polarimeters; methods: observational; polarization; quasars: individual (3C 286); techniques: interferometric; techniques: polarimetric ID 5 GHZ; COMPACT; BRIGHT AB For decades, the bright radio quasar 3C 286 has been widely recognized as one of the most reliable polarization calibrators at centimeter wavelengths because of its unchanging polarization position angle and high polarization percentage. However, it has become clear in recent years that the polarization position angle of 3C 286 changes with increasing frequency, increasing from similar to 33 degrees at lambda greater than or similar to 3 cm to similar to 38 degrees at lambda approximate to 1 mm. With the advent of high-sensitivity polarization observations by current and future (sub) millimeter telescopes, knowledge of the position angle of 3C 286 at higher frequencies is critical for calibration. We report the first polarization observations of 3C 286 at submillimeter wavelengths, taken at 880 mu m (340 GHz) with the Submillimeter Array. We find a polarization position angle and percentage of 37 degrees.4 +/- 1 degrees.5 and 15.7% +/- 0.8%, respectively, which is consistent with previous measurements at 1 mm. C1 [Hull, Charles L. H.; Girart, Josep M.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Girart, Josep M.] CSIC IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Cerdanyola Del Valles, Catalonia, Spain. [Hull, Charles L. H.] Natl Radio Astron Observ, Charlottesville, VA USA. RP Hull, CLH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Hull, CLH (reprint author), Natl Radio Astron Observ, Charlottesville, VA USA. EM chat.hull@cfa.harvard.edu OI Hull, Charles/0000-0002-8975-7573 FU MICINN [AYA2014-57369-C3-P]; MECD (Spain) [PRX15/00435]; SI CGPS award, "Magnetic Fields and Massive Star Formation"; [2015BS012] FX The authors thank the anonymous referee for the insightful comments. C.L.H.H. thanks the SMA staff who made the SMA observations possible. He particularly thanks Charlie Qi for his help with MIR data reduction. He also thanks Ram Rao and Dan Marrone for the useful discussion of absolute polarization angle calibration of the SMA. C.L.H.H. thanks Laurence Sabin for kindly allowing us to use data from her project, 2015B-S012, to measure polarization leakage terms that were necessary to calibrate the 3C 286 data. C.L.H.H. acknowledges Dick Plambeck for his help in deriving polarization percentages and uncertainties from the 1 mm CARMA data, and Rick Perley for the discussion of the low-frequency data from Perley & Butler (2013). J.M.G. acknowledges support from MICINN AYA2014-57369-C3-P and the MECD PRX15/00435 grants (Spain). Q.Z. and J.M.G. acknowledge the support of the SI CGPS award, "Magnetic Fields and Massive Star Formation." The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 21 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 124 DI 10.3847/0004-637X/830/2/124 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200027 ER PT J AU Jiang, YF Guillochon, J Loeb, A AF Jiang, Yan-Fei Guillochon, James Loeb, Abraham TI PROMPT RADIATION AND MASS OUTFLOWS FROM THE STREAM-STREAM COLLISIONS OF TIDAL DISRUPTION EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; methods: numerical; quasars: supermassive black holes; radiative transfer ID SUPERMASSIVE BLACK-HOLE; X-RAY OUTBURSTS; STELLAR DISRUPTION; FOLLOW-UP; STAR; SIMULATIONS; ASASSN-14LI; CANDIDATE; GALAXIES; PS1-10JH AB Stream-stream collisions play an important role in the circularization of highly eccentric streams that result from tidal disruption events (TDEs). We perform three-dimensional radiation hydrodynamic simulations to show that stream collisions can contribute significant optical and ultraviolet light to the flares produced by TDEs, and can explain the majority of the observed emission. Our simulations focus on the region near the radiation-pressure-dominated shock produced by a collision and track how the kinetic energy of the stream is dissipated by the associated shock. When the mass flow rate of the stream (M) over dot is a significant fraction of the Eddington accretion rate, greater than or similar to 2% of the initial kinetic energy is converted to radiation as a result of the collision. In this regime, the collision redistributes the specific kinetic energy into the downstream gas and more than 16% of the mass can become unbound. The fraction of unbound gas decreases rapidly as (M) over dot drops significantly below the Eddington limit, with no unbound gas being produced when (M) over dot drops to 1% of Eddington; we find, however, that the radiative efficiency increases slightly to less than or similar to 8% in these cases of low (M) over dot. The effective radiation temperature and size of the photosphere are determined by the stream velocity and (M) over dot, and we find them to be a few times 10(4). K and 10(14). cm in our calculations, comparable to the values inferred for some TDE candidates. The size of the photosphere is directly proportional to (M) over dot, which can explain its rapidly changing size as seen in TDE candidates such as PS1-10jh. C1 [Jiang, Yan-Fei; Guillochon, James; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Jiang, YF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA High-End Computing (HEC) Program through NASA Advanced Supercomputing (NAS) Division at Ames Research Center; Extreme Science and Engineering Discovery Environment (XSEDE); National Science Foundation [ACI-1053575]; NASA through Einstein Postdoctoral Fellowship [PF-140109, PF3-140108]; NSF grant [AST-1312034] FX We thank the anonymous referee for valuable comments that improved the paper. This work was supported by the computational resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center; the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1053575. Y.F.J. and J.G. are supported by NASA through Einstein Postdoctoral Fellowship grant number PF-140109 and PF3-140108. This work was also supported in part by NSF grant AST-1312034. NR 60 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 125 DI 10.3847/0004-637X/830/2/125 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200028 ER PT J AU Kuchner, MJ Silverberg, SM Bans, AS Bhattacharjee, S Kenyon, SJ Debes, JH Currie, T Garcia, L Jung, D Lintott, C McElwain, M Padgett, DL Rebull, LM Wisniewski, JP Nesvold, E Schawinski, K Thaller, ML Grady, CA Biggs, J Bosch, M Cernohous, T Luca, HAD Hyogo, M Wah, LLW Piipuu, A Pineiro, F AF Kuchner, Marc J. Silverberg, Steven M. Bans, Alissa S. Bhattacharjee, Shambo Kenyon, Scott J. Debes, John H. Currie, Thayne Garcia, Luciano Jung, Dawoon Lintott, Chris McElwain, Michael Padgett, Deborah L. Rebull, Luisa M. Wisniewski, John P. Nesvold, Erika Schawinski, Kevin Thaller, Michelle L. Grady, Carol A. Biggs, Joseph Bosch, Milton Cernohous, Tadeas. Luca, Hugo A. Durantini Hyogo, Michiharu Wah, Lily Lau Wan Piipuu, Art Pineiro, Fernanda CA Disk Detective Collaboration TI DISK DETECTIVE: DISCOVERY OF NEW CIRCUMSTELLAR DISK CANDIDATES THROUGH CITIZEN SCIENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; infrared: planetary systems; methods: data analysis; protoplanetary disks; stars: emission line, Be; surveys ID INFRARED-SURVEY-EXPLORER; YOUNG STELLAR OBJECTS; DUSTY DEBRIS DISKS; DIGITAL-SKY-SURVEY; STAR-FORMING REGIONS; EXTRA-SOLAR PLANETS; SPECTROSCOPIC SURVEY; EXOPLANET SYSTEMS; OB ASSOCIATION; BINARY-SYSTEMS AB The Disk Detective citizen science project aims to find new stars with 22 mu m excess emission from circumstellar dust using data from NASA's Wide-field Infrared Survey Explorer (WISE) mission. Initial cuts on the AllWISE catalog provide an input catalog of 277,686 sources. Volunteers then view images of each source online in 10 different bands to identify false positives (galaxies, interstellar matter, image artifacts, etc.). Sources that survive this online vetting are followed up with spectroscopy on the FLWO Tillinghast telescope. This approach should allow us to unleash the full potential of WISE for finding new debris disks and protoplanetary disks. We announce a first list of 37 new disk candidates discovered by the project, and we describe our vetting and follow-up process. One of these systems appears to contain the first debris disk discovered around a star with a white dwarf companion: HD 74389. We also report four newly discovered classical Be stars (HD 6612, HD 7406, HD 164137, and HD 218546) and a new detection of 22 mu m excess around the previously known debris disk host star HD 22128. C1 [Kuchner, Marc J.; McElwain, Michael; Padgett, Deborah L.; Grady, Carol A.] NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 21230 USA. [Silverberg, Steven M.; Wisniewski, John P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Bans, Alissa S.] Valparaiso Univ, Dept Phys & Astron, Neils Sci Ctr, 1610 Campus Dr East, Valparaiso, IN 46383 USA. [Bhattacharjee, Shambo] Int Space Univ, 1 Rue Jean Dominique Cassini, F-67400 Illkirch Graffenstaden, France. [Kenyon, Scott J.] Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. [Debes, John H.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Currie, Thayne] Natl Astron Observ Japan, 650 N Aohokhu Pl, Hilo, HI 96720 USA. [Garcia, Luciano] Univ Nacl Cordoba, Observ Astron Cordoba, Laprida 854,X5000BGR, Cordoba, Argentina. [Jung, Dawoon] Korea Aerosp Res Inst, Lunar Explorat Program Off, 169-84 Gwahak Ro, Daejeon 34133, South Korea. [Lintott, Chris] Denys Wilkinson Bldg Keble Rd, Oxford OX1 3RH, England. [Rebull, Luisa M.] CALTECH, Infrared Proc & Anal Ctr, M-S 314-6 1200 E Calif Blvd, Pasadena, CA 91125 USA. [Nesvold, Erika] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. [Schawinski, Kevin] Swiss Fed Inst Technol, Inst Astron, Wolfgang Pauli Str 27 Bldg HIT, CH-8093 Zurich, Switzerland. [Thaller, Michelle L.] NASA, Headquarters Sci Mission Directorate, 300 E St SW, Washington, DC 20546 USA. [Biggs, Joseph; Bosch, Milton; Cernohous, Tadeas.; Luca, Hugo A. Durantini; Hyogo, Michiharu; Wah, Lily Lau Wan; Piipuu, Art; Pineiro, Fernanda; Disk Detective Collaboration] Disk Detect, Washington, DC USA. RP Kuchner, MJ (reprint author), NASA, Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 21230 USA. EM Marc.Kuchner@nasa.gov; silverberg@ou.edu; alissa.s.bans@gmail.com; shambo.bhattacharjee@community.isunet.edu; skenyon@cfa.harvard.edu; debes@stsci.edu; thayne.currie@gmail.com; lucianog@oac.uncor.edu; dwjung@kari.re.kr; cjl@astro.ox.ac.uk; michael.w.mcelwain@nasa.gov; deborah.l.padgett@nasa.gov; rebull@ipac.caltech.edu; wisniewski@ou.edu; enesvold@carnegiescience.edu; kevin.schawinski@phys.ethz.ch; michelle.thaller@nasa.gov; carol.a.grady@nasa.gov OI Kenyon, Scott/0000-0003-0214-609X FU NASA Astrophysics Data Analysis Program [14-ADAP14-0161]; NASA Astrobiology Program via the Goddard Center for Astrobiology; NASA's Science Innovation Fund; Alfred P. Sloan foundation; Google Global Impact award; NASA; NSF; Smithsonian Astrophysical Observatory; Space Telescope Science Institute under U.S. Government [NAG W-2166]; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We acknowledge support from grant 14-ADAP14-0161 from the NASA Astrophysics Data Analysis Program. M.K. acknowledges funding from the NASA Astrobiology Program via the Goddard Center for Astrobiology and support from NASA's Science Innovation Fund.; Development of the Disk Detectives site was supported by a grant from the Alfred P. Sloan foundation, and the Zooniverse platform is supported by a Google Global Impact award.; WISE is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory (JPL)/California Institute of Technology (Caltech), funded by NASA. 2MASS is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center (IPAC) at Caltech, funded by NASA and the NSF. This paper uses data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory.; The DSS was produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. This work has made use of the BeSS database, operated at LESIA, Observatoire de Meudon, France: http://basebe.obspm.fr.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 109 TC 0 Z9 0 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 84 DI 10.3847/0004-637X/830/2/84 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA1FK UT WOS:000386337700001 ER PT J AU Marchesi, S Lanzuisi, G Civano, F Iwasawa, K Suh, H Comastri, A Zamorani, G Allevato, V Griffiths, R Miyaji, T Ranalli, P Salvato, M Schawinski, K Silverman, J Treister, E Urry, CM Vignali, C AF Marchesi, S. Lanzuisi, G. Civano, F. Iwasawa, K. Suh, H. Comastri, A. Zamorani, G. Allevato, V. Griffiths, R. Miyaji, T. Ranalli, P. Salvato, M. Schawinski, K. Silverman, J. Treister, E. Urry, C. M. Vignali, C. TI THE CHANDRA COSMOS-LEGACY SURVEY: SOURCE X-RAY SPECTRAL PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: nuclei; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; STAR-FORMING GALAXIES; SEYFERT 2 GALAXIES; ABSORBING COLUMN DENSITIES; XMM-NEWTON OBSERVATIONS; EVOLUTION SURVEY COSMOS; HEAVILY OBSCURED AGN; COMPTON-THICK AGN; PHOTOMETRIC REDSHIFTS AB We present the X-ray spectral analysis of the 1855 extragalactic sources in the Chandra COSMOS-Legacy survey catalog having more than 30 net counts in the 0.5-7 keV band. A total of 38% of the sources are optically classified type 1 active galactic nuclei (AGNs), 60% are type 2 AGNs, and 2% are passive, low-redshift galaxies. We study the distribution of AGN photon index Gamma and of the intrinsic absorption N-H,N-z based on the sources' optical classification: type 1 AGNs have a slightly steeper mean photon index Gamma than type 2 AGNs, which, on the other hand, have average N-H,N-z similar to 3 times higher than type 1 AGNs. We find that similar to 15% of type 1 AGNs have N-H,N-z > 10(22) cm(-2), i.e., are obscured according to the X-ray spectral fitting; the vast majority of these sources have L2-10 (keV) > 10(44) erg s(-1). The existence of these objects suggests that optical and X-ray obscuration can be caused by different phenomena, the X-ray obscuration being, for example, caused by dust-free material surrounding the inner part of the nuclei. Approximately 18% of type 2 AGNs have N-H,N-z < 10(22) cm(-2), and most of these sources have low X-ray luminosities (L2-10 (keV) < 10(43) erg s(-1)). We expect a part of these sources to be low-accretion, unobscured AGNs lacking broad emission lines. Finally, we also find a direct proportional trend between N-H,N-z and host-galaxy mass and star formation rate, although part of this trend is due to a redshift selection effect. C1 [Marchesi, S.] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA. [Marchesi, S.; Lanzuisi, G.; Comastri, A.; Zamorani, G.; Vignali, C.] Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. [Lanzuisi, G.; Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, Viale Berti Pichat 6-2, I-40127 Bologna, Italy. [Civano, F.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Iwasawa, K.] Univ Barcelona IEEC UB, ICREA, Marti & Franques 1, E-08028 Barcelona, Spain. [Iwasawa, K.] Univ Barcelona IEEC UB, ICC, Marti & Franques 1, E-08028 Barcelona, Spain. [Suh, H.] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. [Allevato, V.] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2a, FI-00014 Helsinki, Finland. [Griffiths, R.] Univ Hawaii, Div Nat Sci, Dept Phys & Astron, 200 W Kawili St, Hilo, HI 96720 USA. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron Sede Ensenada, Km 103,Carret Tijunana Ensenada, Ensenada, BC, Mexico. [Ranalli, P.] Lund Observ, POB 43, SE-22100 Lund, Sweden. [Salvato, M.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Schawinski, K.] Swiss Fed Inst Technol, Dept Phys, Inst Astron, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. [Silverman, J.] Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Treister, E.] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile. [Treister, E.] Pontificia Univ Catolica Chile, Inst Astrofis, Casilla 306, Santiago 22, Chile. [Urry, C. M.] Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. RP Marchesi, S (reprint author), Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA.; Marchesi, S (reprint author), Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. OI Zamorani, Giovanni/0000-0002-2318-301X; Comastri, Andrea/0000-0003-3451-9970; Marchesi, Stefano/0000-0001-5544-0749 FU NASA Chandra [GO3-14150C, GO3-14150B]; PRIN-INAF "Windy Black Holes Combing Galaxy Evolution"; FP7 Career Integration Grant "eEASy": "Supermassive Black Holes through Cosmic Time: From Current Surveys to eROSITA-Euclid Synergies" [CIG 321913]; Spanish MINECO of ICCUB (Unidad de Excelencia "Maria de Maeztu") [AYA2013-47447-C3-2-P, MDM-2014-0369]; UNAM-DGAPA Grant PAPIIT [IN104216]; CONACyT Grant Cientifica Basica [179662]; Swiss National Science Foundation [PP00P2_138979/1]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; FONDECYT [1120061]; CONICYT Anillo project [ACT1101] FX This work was supported in part by NASA Chandra grant number GO3-14150C and also GO3-14150B (F.C., V.A., M.E.); PRIN-INAF 2014 "Windy Black Holes Combing Galaxy Evolution" (A.C., M.B., G.L., and C.V.); the FP7 Career Integration Grant "eEASy": "Supermassive Black Holes through Cosmic Time: From Current Surveys to eROSITA-Euclid Synergies" (CIG 321913; M.B. and G.L.); the Spanish MINECO under grant AYA2013-47447-C3-2-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia "Maria de Maeztu"; K.I.); UNAM-DGAPA Grant PAPIIT IN104216 and CONACyT Grant Cientifica Basica #179662 (T.M.); the Swiss National Science Foundation Grant PP00P2_138979/1 (K.S.); and the Center of Excellence in Astrophysics and Associated Technologies (PFB 06), by the FONDECYT regular grant 1120061 and by the CONICYT Anillo project ACT1101 (E.T.). NR 97 TC 0 Z9 0 U1 6 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 100 DI 10.3847/0004-637X/830/2/100 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200003 ER PT J AU Shingledecker, CN Bergner, JB Le Gal, R Oberg, KI Hincelin, U Herbst, E AF Shingledecker, Christopher N. Bergner, Jennifer B. Le Gal, Romane Oberg, Karin I. Hincelin, Ugo Herbst, Eric TI ON THE INFERENCE OF THE COSMIC-RAY IONIZATION RATE zeta FROM THE HCO+-to-DCO+ ABUNDANCE RATIO: THE EFFECT OF NUCLEAR SPIN SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; cosmic rays; ISM: abundances; ISM: clouds; ISM: molecules; ISM: supernova remnants ID DENSE INTERSTELLAR CLOUDS; SUPERNOVA REMNANT W51C; GRAIN CHEMICAL-MODELS; ORTHO-PARA CONVERSION; INTER-STELLAR CLOUDS; MOLECULAR CLOUDS; SURFACE-REACTIONS; DARK CLOUDS; NONTHERMAL DESORPTION; NITROGEN HYDRIDES AB The chemistry of dense interstellar regions was analyzed using a time-dependent gas-grain astrochemical simulation and a new chemical network that incorporates deuterated chemistry, taking into account nuclear spin states for the hydrogen chemistry and its deuterated isotopologues. With this new network, the utility of the [HCO+]/[DCO+] abundance ratio as a probe of the cosmic-ray ionization rate has been re-examined, with special attention paid to the effect of the initial value of the ortho-to-para ratio (OPR) of molecular hydrogen. After discussing the use of the probe for cold cores, we compare our results with previous theoretical and observational results for a molecular cloud close to the supernova remnant W51C, which is thought to have an enhanced cosmic-ray ionization rate. caused by the nearby gamma-ray source. In addition, we attempt to use our approach to estimate the cosmic-ray ionization rate for L1174, a dense core with an embedded star. Beyond the previously known sensitivity of [HCO+]/[DCO+] to zeta, we demonstrate its additional dependence on the initial OPR and, secondarily, on the age of the source, its temperature, and its density. We conclude that the usefulness of the [HCO+]/[DCO+] abundance ratio in constraining the cosmic-ray ionization rate in dense regions increases with the age of the source and the ionization rate as the ratio becomes far less sensitive to the initial value of the OPR. C1 [Shingledecker, Christopher N.; Le Gal, Romane; Hincelin, Ugo; Herbst, Eric] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Bergner, Jennifer B.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Oberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Herbst, Eric] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Shingledecker, CN (reprint author), Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. EM shingledecker@virginia.edu FU NSF FX E.H. wishes to thank the National Science Foundation for continuing to support the astrochemistry program at the University of Virginia. He thanks as well the NASA Exobiology and Evolutionary Biology Program through a subcontract from Rensselaer Polytechnic Institute. J.B.B. acknowledges funding from an NSF Graduate Research Fellowship. NR 52 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 151 DI 10.3847/0004-637X/830/2/151 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA4LG UT WOS:000386583400003 ER PT J AU Storm, S Mundy, LG Lee, KI Fernandez-Lopez, M Looney, LW Teuben, P Arce, HG Rosolowsky, EW Meisner, AM Isella, A Kauffmann, J Shirley, YL Kwon, W Plunkett, AL Pound, MW Segura-Cox, DM Tassis, K Tobin, JJ Volgenau, NH Crutcher, RM Testi, L AF Storm, Shaye Mundy, Lee G. Lee, Katherine I. Fernandez-Lopez, Manuel Looney, Leslie W. Teuben, Peter Arce, Hector G. Rosolowsky, Erik W. Meisner, Aaron M. Isella, Andrea Kauffmann, Jens Shirley, Yancy L. Kwon, Woojin Plunkett, Adele L. Pound, Marc W. Segura-Cox, Dominique M. Tassis, Konstantinos Tobin, John J. Volgenau, Nikolaus H. Crutcher, Richard M. Testi, Leonardo TI CARMA LARGE AREA STAR FORMATION SURVEY: DENSE GAS IN THE YOUNG L1451 REGION OF PERSEUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: kinematics and dynamics; ISM: molecules; ISM: structure; stars: formation ID MOLECULAR CLOUDS; DRIVEN TURBULENCE; CLUSTER FORMATION; MAGNETIC-FIELDS; VIRIAL-THEOREM; DUST; CORES; OPHIUCHUS; SERPENS; MODEL AB We present a 3 mm spectral line and continuum survey of L1451 in the Perseus Molecular Cloud. These observations are from the CARMA Large Area Star Formation Survey (CLASSy), which also imaged Barnard. 1, NGC 1333, Serpens Main, and Serpens South. L1451 is the survey region with the lowest level of star formation activity-it contains no confirmed protostars. HCO+, HCN, and N2H+ (J = 1 -> 0). are all detected throughout the region, with HCO+ being the most spatially widespread, and molecular emission seen toward 90% of the area above N(H-2) column densities of 1.9 x 10(21) cm(-2). HCO+ has the broadest velocity dispersion, near 0.3 km s(-1) on average, compared with similar to 0.15 km s(-1) for the other molecules, thus representing a range of subsonic to supersonic gas motions. Our non-binary dendrogram analysis reveals that the dense gas traced by each molecule has a similar hierarchical structure, and that gas surrounding the candidate first hydrostatic core (FHSC), L1451-mm, and other previously detected single-dish continuum clumps has similar hierarchical structure; this suggests that different subregions of L1451 are fragmenting on the pathway to forming young stars. We determined that the three-dimensional morphology of the largest detectable dense-gas structures was relatively ellipsoidal compared with other CLASSy regions, which appeared more flattened at the largest scales. A virial analysis shows that the most centrally condensed dust structures are likely unstable against collapse. Additionally, we identify a new spherical, centrally condensed N2H+ feature that could be a new FHSC candidate. The overall results suggest that L1451 is a young region starting to form its generation of stars within turbulent, hierarchical structures. C1 [Storm, Shaye; Lee, Katherine I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Storm, Shaye; Mundy, Lee G.; Lee, Katherine I.; Teuben, Peter; Pound, Marc W.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Fernandez-Lopez, Manuel; Looney, Leslie W.; Segura-Cox, Dominique M.; Crutcher, Richard M.] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA. [Fernandez-Lopez, Manuel] CCT La Plata CONICET, Inst Argentino Radioastron, CC 5, RA-1894 Villa Elisa, Argentina. [Arce, Hector G.] Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. [Rosolowsky, Erik W.] Univ Alberta, Dept Phys, 4-181 CCIS, Edmonton, AB T6G 2E1, Canada. [Meisner, Aaron M.] Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Meisner, Aaron M.] Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Isella, Andrea] Rice Univ, Dept Phys & Astron, POB 1892, Houston, TX 77251 USA. [Kauffmann, Jens] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Shirley, Yancy L.] Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA. [Kwon, Woojin] Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea. [Plunkett, Adele L.] European Southern Observ, Av Alonso de Cordova 3107, Vitacura, Santiago De Chi, Chile. [Tassis, Konstantinos] Univ Crete, Dept Phys, POB 2208, GR-71003 Iraklion, Crete, Greece. [Tassis, Konstantinos] Univ Crete, Inst Theoret & Computat Phys, POB 2208, GR-71003 Iraklion, Crete, Greece. [Tassis, Konstantinos] Fdn Res & Technol Hellas, IESL, Iraklion 7110, Greece. [Tobin, John J.] Leiden Observ, 540 JH Oort Bldg,Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands. [Volgenau, Nikolaus H.] Las Cumbres Observ Global Telescope Network Inc, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA. [Testi, Leonardo] ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. RP Storm, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; Storm, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM shaye.storm@cfa.harvard.edu RI Tassis, Konstantinos/C-3155-2011; OI Rosolowsky, Erik/0000-0002-5204-2259; Arce, Hector/0000-0001-5653-7817 FU University of Maryland [AST-1139990]; University of Illinois [AST-1139950]; National Science Foundation; CARMA FX The authors would like to thank the referee for encouraging critiques that improved the paper, and all members of the CARMA staff who made these observations possible. CLASSy was supported by AST-1139990 (University of Maryland) and AST-1139950 (University of Illinois). Support for CARMA construction was derived from the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the James S. McDonnell Foundation, the Associates of the California Institute of Technology, the University of Chicago, Illinois, California, and Maryland, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. NR 45 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 127 DI 10.3847/0004-637X/830/2/127 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA3FZ UT WOS:000386488200030 ER PT J AU Irwin, JA Maksym, WP Sivakoff, GR Romanowsky, AJ Lin, DC Speegle, T Prado, I Mildebrath, D Strader, J Liu, JF Miller, JM AF Irwin, Jimmy A. Maksym, W. Peter Sivakoff, Gregory R. Romanowsky, Aaron J. Lin, Dacheng Speegle, Tyler Prado, Ian Mildebrath, David Strader, Jay Liu, Jifeng Miller, Jon M. TI Ultraluminous X-ray bursts in two ultracompact companions to nearby elliptical galaxies SO NATURE LA English DT Article ID GLOBULAR-CLUSTER SYSTEM; ACS VIRGO CLUSTER; DWARF GALAXIES; NGC-5128; FIELD; BINARIES; DISTANCE; FLARES; POPULATION; CENTAURUS AB A flaring X-ray source was found near the galaxy NGC 4697 (ref. 1). Two brief flares were seen, separated by four years. During each flare, the flux increased by a factor of 90 on a timescale of about one minute. There is no associated optical source at the position of the flares(1), but if the source was at the distance of NGC 4697, then the luminosities of the flares were greater than 10(39) erg per second. Here we report the results of a search of archival X-ray data for 70 nearby galaxies looking for similar flares. We found two ultraluminous flaring sources in globular clusters or ultracompact dwarf companions of parent elliptical galaxies. One source flared once to a peak luminosity of 9 x 10(40) erg per second; the other flared five times to 10(40) erg per second. The rise times of all of the flares were less than one minute, and the flares then decayed over about an hour. When not flaring, the sources appear to be normal accreting neutron-star or black-hole X-ray binaries, but they are located in old stellar populations, unlike the magnetars, anomalous X-ray pulsars or soft gamma repeaters that have repetitive flares of similar luminosities. C1 [Irwin, Jimmy A.; Speegle, Tyler; Prado, Ian; Mildebrath, David] Univ Alabama, Dept Phys & Astron, Box 870324, Tuscaloosa, AL 35487 USA. [Maksym, W. Peter] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sivakoff, Gregory R.] Univ Alberta, Dept Phys, CCIS 4-181, Edmonton, AB T6G 2E1, Canada. [Romanowsky, Aaron J.] San Jose State Univ, Dept Phys & Astron, One Washington Sq, San Jose, CA 95192 USA. [Romanowsky, Aaron J.] Univ Calif Observ, 1156 High St, Santa Cruz, CA 95064 USA. [Lin, Dacheng] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Liu, Jifeng] Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, 20A Datun Rd, Beijing 100012, Peoples R China. [Liu, Jifeng] Univ Chinese Acad Sci, Coll Astron & Space Sci, 19A Yuquan Rd, Beijing 100049, Peoples R China. [Miller, Jon M.] Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48103 USA. RP Irwin, JA (reprint author), Univ Alabama, Dept Phys & Astron, Box 870324, Tuscaloosa, AL 35487 USA. EM jairwin@ua.edu FU Chandra grant [AR6-17010X]; NASA ADAP [NNX10AE15G]; NSERC; National Science Foundation [AST-1515084]; NSF [AST-1308124, AST-1514763]; Packard Foundation FX We thank T. Richtler for discussions. J.A.I. was supported by Chandra grant AR6-17010X and NASA ADAP grant NNX10AE15G. G.R.S. acknowledges the support of an NSERC Discovery Grant. A.J.R. was supported by the National Science Foundation grant AST-1515084. J.S. acknowledges support from NSF grants AST-1308124 and AST-1514763 and the Packard Foundation. NR 33 TC 1 Z9 1 U1 3 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD OCT 20 PY 2016 VL 538 IS 7625 BP 356 EP + DI 10.1038/nature19822 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EA5PJ UT WOS:000386673100033 PM 27762351 ER PT J AU Bouwens, RJ Oesch, PA Labbe, I Illingworth, GD Fazio, GG Coe, D Holwerda, B Smit, R Stefanon, M van Dokkum, PG Trenti, M Ashby, MLN Huang, JS Spitler, L Straatman, C Bradley, L Magee, D AF Bouwens, R. J. Oesch, P. A. Labbe, I. Illingworth, G. D. Fazio, G. G. Coe, D. Holwerda, B. Smit, R. Stefanon, M. van Dokkum, P. G. Trenti, M. Ashby, M. L. N. Huang, J. -S. Spitler, L. Straatman, C. Bradley, L. Magee, D. TI THE BRIGHT END OF THE z similar to 9 AND z similar to 10 UV LUMINOSITY FUNCTIONS USING ALL FIVE CANDELS FIELDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: high-redshift ID ULTRA-DEEP FIELD; HUBBLE-SPACE-TELESCOPE; STAR-FORMATION RATE; FORMATION RATE DENSITY; EARLY RELEASE SCIENCE; LYMAN-BREAK GALAXIES; EXTRAGALACTIC LEGACY SURVEY; HIGH-REDSHIFT GALAXIES; SURVEY. SURVEY DESIGN; IRAC SOURCE COUNTS AB The deep, wide-area (similar to 800-900 arcmin(2)) near-infrared/WFC3/IR + Spitzer/IRAC observations over the CANDELS fields have been a remarkable resource for constraining the bright end of high-redshift UV luminosity functions. However, the lack of Hubble Space Telescope (HST) 1.05 mu m observations over the CANDELS fields has made it difficult to identify z similar to 9-10 sources robustly, since such data are needed to confirm the presence of an abrupt Lyman break at 1.2 mu m. Here, we report on the successful identification of many such z similar to 9-10 sources from a new HST program (z9-CANDELS) that targets the highest-probability z similar to 9-10 galaxy candidates with observations at 1.05 mu m, to search for a robust Lyman-break at 1.2 mu m. The potential z similar to 9-10 candidates were preselected from the full HST, Spitzer/IRAC S-CANDELS observations, and the deepest-available ground-based optical+near-infrared observations (CFHTLS-DEEP+HUGS+UltraVISTA+ZFOURGE). We identified 15 credible z similar to 9-10 galaxies over the CANDELS fields. Nine of these galaxies lie at z similar to 9 and five are new identifications. Our targeted follow-up strategy has proven to be very efficient in making use of scarce HST time to secure a reliable sample of z similar to 9-10 galaxies. Through extensive simulations, we replicate the selection process for our sample (both the preselection and follow-up) and use it to improve current estimates for the volume density of bright z similar to 9 and z similar to 10 galaxies. The volume densities we find are 5(-2)(+3)x and 8(-3)(+9)x lower, respectively, than those found at z similar to 8. When compared with the best-fit evolution (i.e., d log(10) rho(UV)/dz = -0.29 +/- 0.02) in the UV luminosity densities from z similar to 8 to z similar to 4 integrated to 0.3L(z=3)* (-20 mag), these luminosity densities are 2.6(-0.9)(+1.5)x and 2.2(-1.1)(+2.0) lower, respectively, than the extrapolated trends. Our new results are broadly consistent with the "accelerated evolution" scenario at z > 8, consistent with that seen in many models. C1 [Bouwens, R. J.; Labbe, I.; Holwerda, B.; Stefanon, M.; Straatman, C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Oesch, P. A.; van Dokkum, P. G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Illingworth, G. D.; Magee, D.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Fazio, G. G.; Ashby, M. L. N.; Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Coe, D.; Bradley, L.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Smit, R.] Dept Phys & Astron, South Rd, Durham DH1 3EE, England. [Trenti, M.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Spitler, L.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. RP Bouwens, RJ (reprint author), Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. FU NASA [NAG5-7697, HST-GO-11563]; NWO vrij competitie grant [600.065.140.11N211] FX We thank Jim Dunlop and Steve Finkelstein for valuable conversations. We thank Steve Willner for providing us with feedback on an earlier draft of this manuscript. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge the support of NASA grant NAG5-7697, NASA grant HST-GO-11563, and a NWO vrij competitie grant 600.065.140.11N211. NR 82 TC 2 Z9 2 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 67 DI 10.3847/0004-637X/830/2/67 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ8MN UT WOS:000386124600013 ER PT J AU McNamara, BR Russell, HR Nulsen, PEJ Hogan, MT Fabian, AC Pulido, F Edge, AC AF McNamara, B. R. Russell, H. R. Nulsen, P. E. J. Hogan, M. T. Fabian, A. C. Pulido, F. Edge, A. C. TI A MECHANISM FOR STIMULATING AGN FEEDBACK BY LIFTING GAS IN MASSIVE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: individual (M87, MS 0735+7421, Abell 2029); X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; BRIGHTEST CLUSTER GALAXIES; COOLING FLOW CLUSTERS; COLD MOLECULAR GAS; X-RAY CAVITIES; HEATING HOT ATMOSPHERES; SUPERMASSIVE BLACK-HOLE; H-ALPHA FILAMENTS; STAR-FORMATION; THERMAL-INSTABILITY AB Observation shows that nebular emission, molecular gas, and young stars in giant galaxies are associated with rising X-ray bubbles inflated by radio jets launched from nuclear black holes. We propose a model where molecular clouds condense from low-entropy gas caught in the updraft of rising X-ray bubbles. The low-entropy gas becomes thermally unstable when it is lifted to an altitude where its cooling time is shorter than the time required to fall to its equilibrium location in the galaxy,. i.e., t(c)/t(I)less than or similar to 1. The infall speed of a cloud is bounded by the lesser of its free-fall and terminal speeds, so that the infall time here can exceed the free-fall time by a significant factor. This mechanism is motivated by Atacama Large Millimeter Array observations revealing molecular clouds lying in the wakes of rising X-ray bubbles with velocities well below their free-fall speeds. Our mechanism would provide cold gas needed to fuel a feedback loop while stabilizing the atmosphere on larger scales. The observed cooling time threshold of similar to 5 x 10(8) yr-the clear-cut signature of thermal instability and the onset of nebular emission and star formation-may result from the limited ability of radio bubbles to lift low-entropy gas to altitudes where thermal instabilities can ensue. Outflowing molecular clouds are unlikely to escape, but instead return to the central galaxy in a circulating flow. We contrast our mechanism to precipitation models where the minimum value of t(c)/t(ff) less than or similar to 10 triggers thermal instability, which we find to be inconsistent with observation. C1 [McNamara, B. R.; Hogan, M. T.; Pulido, F.] Univ Waterloo, Dept Phys & Astron, 200 Univ Ave West, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.; Hogan, M. T.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Russell, H. R.; Fabian, A. C.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Nulsen, P. E. J.] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. [Edge, A. C.] Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England. RP McNamara, BR (reprint author), Univ Waterloo, Dept Phys & Astron, 200 Univ Ave West, Waterloo, ON N2L 3G1, Canada.; McNamara, BR (reprint author), Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. OI Hogan, Michael/0000-0002-7031-721X; Nulsen, Paul/0000-0003-0297-4493 FU Natural Sciences and Engineering Research Council of Canada; Canadian Space Agency; ERC Advanced Grant [340442]; Chandra Award [G05-16134X] FX B.R.M. acknowledges generous financial support from the Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency. H.R.R. and A.C.F. acknowledge support from ERC Advanced Grant 340442. We acknowledge helpful discussions with Mark Voit, Megan Donahue, Prateek Sharma, and the anonymous referee. This work was supported in part by Chandra Award Number G05-16134X. NR 85 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2016 VL 830 IS 2 AR 79 DI 10.3847/0004-637X/830/2/79 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA1PE UT WOS:000386363500004 ER PT J AU Plumptre, AJ Nixon, S Kujirakwinja, DK Vieilledent, G Critchlow, R Williamson, EA Nishuli, R Kirkby, AE Hall, JS AF Plumptre, Andrew J. Nixon, Stuart Kujirakwinja, Deo K. Vieilledent, Ghislain Critchlow, Rob Williamson, Elizabeth A. Nishuli, Radar Kirkby, Andrew E. Hall, Jefferson S. TI Catastrophic Decline of World's Largest Primate: 80% Loss of Grauer's Gorilla (Gorilla beringei graueri) Population Justifies Critically Endangered Status SO PLOS ONE LA English DT Article ID SPECIES DISTRIBUTION MODELS; BIEGA NATIONAL-PARK; SPATIAL AUTOCORRELATION; LOWLAND GORILLAS; DISTRIBUTIONS; CONSERVATION; IMPACTS; DESIGN; FOREST; CENSUS AB Grauer's gorilla (Gorilla beringei graueri), the World's largest primate, is confined to eastern Democratic Republic of Congo (DRC) and is threatened by civil war and insecurity. During the war, armed groups in mining camps relied on hunting bushmeat, including gorillas. Insecurity and the presence of several militia groups across Grauer's gorilla's range made it very difficult to assess their population size. Here we use a novel method that enables rigorous assessment of local community and ranger-collected data on gorilla occupancy to evaluate the impacts of civil war on Grauer's gorilla, which prior to the war was estimated to number 16,900 individuals. We show that gorilla numbers in their stronghold of Kahuzi-Biega National Park have declined by 87%. Encounter rate data of gorilla nests at 10 sites across its range indicate declines of 82-100% at six of these sites. Spatial occupancy analysis identifies three key areas as the most critical sites for the remaining populations of this ape and that the range of this taxon is around 19,700 km(2). We estimate that only 3,800 Grauer's gorillas remain in the wild, a 77% decline in one generation, justifying its elevation to Critically Endangered status on the IUCN Red List of Threatened Species. C1 [Plumptre, Andrew J.; Kujirakwinja, Deo K.; Kirkby, Andrew E.] Wildlife Conservat Soc, 2300 Southern Blvd, Bronx, NY 10460 USA. [Plumptre, Andrew J.] Univ Cambridge, Dept Zool, Conservat Sci Grp, David Attenborough Bldg,Pembroke Rd, Cambridge, England. [Nixon, Stuart] Chester Zoo, North England Zool Soc, Upton By Chester CH2 1LH, Cheshire, England. [Vieilledent, Ghislain] CIRAD, UPR Forets & Soc, F-34398 Montpellier, France. [Critchlow, Rob] Univ York, Dept Biol, York, N Yorkshire, England. [Williamson, Elizabeth A.] Univ Stirling, Fac Nat Sci, Stirling, Scotland. [Nishuli, Radar] ICCN, Bukavu, DEM REP CONGO. [Hall, Jefferson S.] Smithsonian Trop Res Inst, Ave Roosevelt 401, Balboa, Ancon, Panama. RP Plumptre, AJ (reprint author), Wildlife Conservat Soc, 2300 Southern Blvd, Bronx, NY 10460 USA.; Plumptre, AJ (reprint author), Univ Cambridge, Dept Zool, Conservat Sci Grp, David Attenborough Bldg,Pembroke Rd, Cambridge, England. EM aplumptre@wcs.org OI Vieilledent, Ghislain/0000-0002-1685-4997; Plumptre, Andrew/0000-0002-9333-4047 FU Arcus Foundation through the Jane Goodall Institute (Arcus) [1202-03]; Critical Ecosystem Partnership Fund; Frankfurt Zoological Society; KfW; Rainforest Trust; UNESCO; USAID/CARPE; US Fish and Wildlife Service; World Bank FX Support for this analysis was primarily provided by the generous support of the Arcus Foundation through the Jane Goodall Institute (Arcus 1202-03). The surveys referred to in the report were funded by other donors, notably Critical Ecosystem Partnership Fund, Frankfurt Zoological Society, KfW, Rainforest Trust, UNESCO, USAID/CARPE, US Fish and Wildlife Service and World Bank. We are also grateful to Wildlife Conservation Society for supporting Andrew Plumptre and Deo Kujirakwinja to compile and analyse the data; CIRAD, who supported Ghislain Vieilledent to help with the R-analyses, Chester Zoo, who supported Stuart Nixon's time during the writing of this report, and the University of York, who supported Rob Critchlow. NR 33 TC 0 Z9 0 U1 31 U2 31 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 19 PY 2016 VL 11 IS 10 AR e0162697 DI 10.1371/journal.pone.0162697 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ9NW UT WOS:000386204000003 PM 27760201 ER PT J AU Cui, YY Bethoux, O Kondratieff, B Shih, CK Ren, D AF Cui, Yingying Bethoux, Olivier Kondratieff, Boris Shih, Chungkun Ren, Dong TI The first fossil salmonfly (Insecta: Plecoptera: Pteronarcyidae), back to the Middle Jurassic SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID INNER-MONGOLIA; CHINA; NOMENCLATURE; HEMISPHERE; TAXONOMY; LOCALITY; GENERA; AGE AB Background: The fossil record of Plecoptera (stoneflies) is considered relatively complete, with stem-groups of each of the three major lineages, viz. Antarctoperlaria, Euholognatha and Systellognatha (and some of their families) represented in the Mesozoic. However, the family Pteronarcyidae (the salmonflies; including two genera, Pteronarcys and Pteronarcella) has no fossil record to date, and the family has been suggested to have diverged recently. Results: In this paper, we report on a set of specimens belonging to a new fossil species of stonefly, discovered from the Middle Jurassic Daohugou locality (China). Our comparative analysis of wing venation and body characters demonstrates that the new species belongs to the Pteronarcyidae, and is more closely related to Pteronarcys than to Pteronarcella. However, it differs from all known species of the former genus. It is therefore assigned to a new genus and named Pteroliriope sinitshenkovae gen. et sp. nov. under the traditional nomenclatural procedure. The cladotypic nomenclatural procedure is also employed, with the resulting combination Pteroliriope nec Pteronarcys sinitshenkovae sp. nov. Conclusions: The first discovery of a fossil member of the Pteronarcyidae demonstrates that the corresponding lineage is not a very recent offshoot but was already present ca. 165 million years ago. This discovery concurs with the view that divergence of most stonefly families took place very early, probably in the Triassic, or even in the Permian. This contribution demonstrates the need for (re-)investigations of the systematics of fossil stoneflies to refine divergence date estimates for Plecoptera lineages. C1 [Cui, Yingying; Bethoux, Olivier] Univ Paris 06, Sorbonne Univ, CNRS, MNHN,CR2P, Paris, France. [Cui, Yingying; Shih, Chungkun; Ren, Dong] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Kondratieff, Boris] Colorado State Univ, Dept Bioagr Sci & Pest Management, Ft Collins, CO 80523 USA. [Shih, Chungkun] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. EM rendong@mail.cnu.edu.cn FU German Academic Exchange Service (DAAD); Agence Nationale de la Recherche in the program "Investissements d'avenir" [LabEx ANR-10-LABX-0003-BCDiv, ANR-11-IDEX-0004-02]; National Natural Science Foundation of China [31230065, 41272006, 31672323]; Program for Changjiang Scholars and Innovative Research Team in University [IRT13081] FX We thank Kevin Arbuckle, an anonymous reviewer and the editorial board of the journal for constructive comments. This work was supported by the German Academic Exchange Service (DAAD; stay of the first author in Germany from April 2013 to April 2014); this work was supported by a grant from Agence Nationale de la Recherche under the LabEx ANR-10-LABX-0003-BCDiv, in the program "Investissements d'avenir" n ANR-11-IDEX-0004-02; this work was supported by the National Natural Science Foundation of China (No. 31230065, 41272006, 31672323), Program for Changjiang Scholars and Innovative Research Team in University (IRT13081). NR 42 TC 0 Z9 0 U1 7 U2 7 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD OCT 18 PY 2016 VL 16 AR 217 DI 10.1186/s12862-016-0787-9 PG 14 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA DZ7EA UT WOS:000386026200003 PM 27756205 ER PT J AU Mecke, S Kieckbusch, M Hartmann, L Kaiser, H AF Mecke, Sven Kieckbusch, Max Hartmann, Lukas Kaiser, Hinrich TI Historical considerations and comments on the type series of Cyrtodactylus marmoratus Gray, 1831, with an updated comparative table for the bent-toed geckos of the Sunda Islands and Sulawesi SO ZOOTAXA LA English DT Article DE Cyrtodactylus marmoratus; bow-fingered geckos; Reptilia; Squamata; Gekkonidae; type specimens; paratypes; precloacal morphology ID REPTILIA SQUAMATA GEKKONIDAE; INDONESIA; ARCHIPELAGO; JAVA; PHYLOGENY; EAST AB Cyrtodactylus marmoratus Gray, 1831, a species of bent-toed gecko exhibiting a precloacal groove in males, was described on the basis of specimens collected by Heinrich Kuhl and Johan Conrad van Hasselt in Java, Greater Sunda Islands, Indonesia. Kluge (1985) subsequently designated a lectotype for C. marmoratus from a series of these specimens (i.e., syntypes), now housed in the herpetological collection at Naturalis (formerly the Rijksmuseum van Natuurlijke Historie; RMNH), Leiden, the Netherlands. Our work at Naturalis shows that the type series of C. marmoratus at RMNH actually comprises two sets of specimens, and that examination of specimens from one set or the other by different authors, including Kluge (1985), is responsible for some confusion surrounding the type series of this species. As a consequence, we present relevant morphological data for all 14 specimens constituting the type series of C. marmoratus at RMNH for the first time. The type status of two specimens of C. marmoratus in the collection at the Museum National d'Histoire Naturelle, Paris, France, remains unresolved at present. Owing to the inconsistent naming and application of terms for some key characters (e.g., groove, sulcus, pit, hollow, depression) used in the diagnoses of Cyrtodactylus species, we here propose a set of novel and useful definitions that are supported by photographs. We also illustrate the sexually dimorphic expression of this character in C. marmoratus. Finally, we present a revised comparative table for the bent-toad geckos of the Sunda Islands and Sulawesi. C1 [Mecke, Sven; Kieckbusch, Max; Hartmann, Lukas] Univ Marburg, Dept Anim Evolut & Systemat & Zool Collect Marbur, Fac Biol, Karl von Frisch Str 8, D-35032 Marburg, Germany. [Hartmann, Lukas] Goethe Univ Frankfurt, Dept Ecol & Evolut, Biol, Max von Laue Str 13, D-60438 Frankfurt, Germany. [Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA. [Kaiser, Hinrich] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Mecke, S (reprint author), Univ Marburg, Dept Anim Evolut & Systemat & Zool Collect Marbur, Fac Biol, Karl von Frisch Str 8, D-35032 Marburg, Germany. EM meckes@staff.uni-marburg.de FU AMNH collection study grant FX The authors thank Christopher J. Raxworthy, David A. Kizirian, David A. Dickey, and Lauren Vonnahme (AMNH), Patrick Campbell (BMNH), Max Nickerson and Kenneth Krysko (FLMNH), Joseph Martinez and Jose Rosado (MCZ), Raffael Ernst and Markus Auer (MTD), Denis Vallan and Urs Wuest (NMB), Esther Dondorp (RMNH), Gunther Kohler and Linda Mogk (SMF), Kelvin Lim (ZRC), and Frank Glaw (ZSM) for allowing examination of material in their care. Furthermore, we are grateful to Aaron Bauer (Villanova University, Villanova, USA) for providing some of the literature cited in the reference section and Nicolas Vidal (MNHN) for providing information on the C. marmoratus specimens housed in the MNHN. SM and HK thank Marinus S. Hoogmoed for many fruitful discussions. We thank Ka Schuster (Philipps-Universitat Marburg, Germany) for reading and commenting on a draft of this paper, and Michael B. Harvey (Broward College, Fort Lauderdale, USA) and Paul Oliver (Australian National University, Canberra, Australia) for their constructive reviews, which greatly improved the manuscript. This study was supported by an AMNH collection study grant to SM. NR 49 TC 1 Z9 1 U1 2 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 17 PY 2016 VL 4175 IS 4 BP 353 EP 365 DI 10.11646/zootaxa.4175.4.5 PG 13 WC Zoology SC Zoology GA DY6QR UT WOS:000385253400005 PM 27811747 ER PT J AU Hong, T AF Hong, Terry TI The Explosion Chronicles SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 2016 VL 141 IS 17 BP 80 EP 80 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA EJ6SJ UT WOS:000393348800143 ER PT J AU Clyde, WC Ramezani, J Johnson, KR Bowring, SA Jones, MM AF Clyde, William C. Ramezani, Jahandar Johnson, Kirk R. Bowring, Samuel A. Jones, Matthew M. TI Direct high-precision U-Pb geochronology of the end-Cretaceous extinction and calibration of Paleocene astronomical timescales SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE K-Pg boundary; geochronology; magnetostratigraphy; astrochronology; Paleocene; timescale ID FISH CANYON SANIDINE; ZUMAIA BASQUE BASIN; PALEOGENE BOUNDARY; MASS EXTINCTION; EARTH; TIME; USA; ACCURACY; COLORADO; INTERVAL AB The Cretaceous-Paleogene (K-Pg) boundary is the best known and most widely recognized global time horizon in Earth history and coincides with one of the two largest known mass extinctions. We present a series of new high-precision uranium-lead (U-Pb) age determinations by the chemical abrasion isotope dilution thermal ionization mass spectrometry (CA-ID-TIMS) method from volcanic ash deposits within a tightly constrained magnetobiostratigraphic framework across the K-Pg boundary in the Denver Basin, Colorado, USA. This new timeline provides a precise interpolated absolute age for the K-Pg boundary of 66.021 +/- 0.024/0.039/0.081 Ma, constrains the ages of magnetic polarity Chrons C28 to C30, and offers a direct and independent test of early Paleogene astronomical and Ar-40/Ar-39 based timescales. Temporal calibration of paleontological and palynological data from the same deposits shows that the interval between the extinction of the dinosaurs and the appearance of earliest Cenozoic mammals in the Denver Basin lasted similar to 185 ky (and no more than 570 ky) and the 'fern spike' lasted similar to 1 ky (and no more than 71 ky) after the K-Pg boundary layer was deposited, indicating rapid rates of biotic extinction and initial recovery in the Denver Basin during this event. (C) 2016 Elsevier B.V. All rights reserved. C1 [Clyde, William C.; Jones, Matthew M.] Univ New Hampshire, Dept Earth Sci, 56 Coll Rd, Durham, NH 03824 USA. [Ramezani, Jahandar; Bowring, Samuel A.] MIT, Dept Earth Atmospher & Planetary Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Johnson, Kirk R.] Smithsonian Inst, Natl Museum Nat Hist, MRC 106,POB 37012, Washington, DC 20013 USA. [Jones, Matthew M.] Northwestern Univ, Inst Technol, Dept Earth & Planetary Sci, 2145 Sheridan Rd, Evanston, IL 60208 USA. RP Clyde, WC (reprint author), Univ New Hampshire, Dept Earth Sci, 56 Coll Rd, Durham, NH 03824 USA. EM will.clyde@unh.edu; ramezani@mit.edu; johnsonkr@si.edu; matthewjones2012@u.northwestern.edu RI Clyde, William/C-9595-2017; OI Clyde, William/0000-0001-8814-3409; Jones, Matthew/0000-0001-5996-1728 FU NSF [EAR 9805474, EAR 0643158, EAR 0642291, EAR 0642838] FX Property access to the West Bijou and My Lucky Number sites was provided by the Plains Conservation Center; to the Easy to Reach section by Toby Pippin; to the Hass Ranch section by Robert and Dale Haas. The project was supported by NSF grants EAR 9805474 to KRJ and R. Raynolds, EAR 0643158 to SAB, EAR 0642291 to WCC and EAR 0642838 to KRJ. We thank R. Barclay, T. Barnum, R. Dodds, B. Ellis, I. Miller, R. Raynolds and K. Tsukui, for help with field work, lab work and helpful discussions. Thanks to J. Crowley for preliminary U-Pb analyses from the Bowring Pit at MIT. An anonymous reviewer and J. Dinares-Turell provided valuable reviews of the manuscript. NR 50 TC 0 Z9 0 U1 25 U2 25 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD OCT 15 PY 2016 VL 452 BP 272 EP 280 DI 10.1016/j.epsl.2016.07.041 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DV5YE UT WOS:000383005800026 ER PT J AU Silva, GSC Roxo, FF Melo, BF Oliveira, C AF Silva, Gabriel S. C. Roxo, Fabio F. Melo, Bruno F. Oliveira, Claudio TI New species of Curculionichthys (Siluriformes: Loricariidae) from the eastern Guiana Shield SO ZOOTAXA LA English DT Article DE Amazon basin; Cascudinhos; Freshwater fishes; Otothyrini; taxonomy ID BRAZIL; BASIN AB We describe a new species of Curculionichthys from northern Brazil. The new species is known from the rio Cassiporee, an Atlantic coastal river and an unnamed affluent of the rio Jari, left tributary of the Amazon river. It can be distinguished from congeners by (1) the irregular concentration of chromatophores that cover the anal-fin origin and adjacent region, and distal portions of the first unbranched anal-fin ray, (2) lack of dark-brown spots scattered over the body, (3) lack of contrasting dark spots over the anterodorsal region of the body, (4) presence of papillae randomly distributed across the lower lip, (5) small, inconspicuous odontodes that form rows over the head and trunk, (6) anterior profile of the head pointed, (7) higher number of premaxillary and dentary teeth, (8) lack of an unpaired platelet on the dorsal portion of the caudal peduncle, (9) lower number of vertebrae, and (10) higher number of lateral abdomen plates. A discussion on the morphological variation of diagnostic features within Curculionichthys is also provided. C1 [Silva, Gabriel S. C.; Roxo, Fabio F.; Melo, Bruno F.; Oliveira, Claudio] Univ Estadual Paulista, Inst Biociencias, Dept Morfol, R Prof Dr Antonio CW Zanin S-N, BR-18618689 Botucatu, SP, Brazil. [Melo, Bruno F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Roxo, FF (reprint author), Univ Estadual Paulista, Inst Biociencias, Dept Morfol, R Prof Dr Antonio CW Zanin S-N, BR-18618689 Botucatu, SP, Brazil. EM roxoff@hotmail.com.br RI Gesseff, Ednilson/A-3019-2017; Melo, Bruno F./G-1644-2012 OI Melo, Bruno F./0000-0002-0499-567X FU Brazilian agencies FAPESP [2012/01622-2]; FAPESP [2014/05051-5, 2015/00691-9, 2014/26508-3]; MCT/CNPq Universal grant [441347/2014-2]; CNPq PDJ [40258/2014-7] FX We thank Cecile S. Gama (Instituto de Pesquisas Cientificas e Tecnologicas do Amapa) for logistic support during field expeditions in Amapa~. Research was funded by the Brazilian agencies FAPESP grant 2012/01622-2 (GSCS), FAPESP grant 2014/05051-5 and 2015/00691-9 (FFR) and MCT/CNPq Universal grant 441347/2014-2 (coord. FFR), CNPq PDJ 40258/2014-7 (BFM) and FAPESP grant 2014/26508-3 (BFM and CO). NR 13 TC 0 Z9 0 U1 3 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 14 PY 2016 VL 4175 IS 3 BP 281 EP 291 DI 10.11646/zootaxa.4175.3.7 PG 11 WC Zoology SC Zoology GA DY6PW UT WOS:000385251000007 PM 27811766 ER PT J AU Crampton, WGR de Santana, CD Waddell, JC Lovejoy, NR AF Crampton, William G. R. de Santana, Carlos David Waddell, Joseph C. Lovejoy, Nathan R. TI Phylogenetic Systematics, Biogeography, and Ecology of the Electric Fish Genus Brachyhypopomus (Ostariophysi: Gymnotiformes) SO PLOS ONE LA English DT Article ID FRESH-WATER FISHES; LOWLAND AMAZON BASIN; ORGAN DISCHARGES; HISTORICAL BIOGEOGRAPHY; SIGNAL DIVERSITY; HYPOPOMIDAE; TELEOSTEI; COMMUNICATION; EVOLUTION; STERNOPYGIDAE AB A species-level phylogenetic reconstruction of the Neotropical bluntnose knifefish genus Brachyhypopomus (Gymnotiformes, Hypopomidae) is presented, based on 60 morphological characters, approximately 1100 base pairs of the mitochondrial cytb gene, and approximately 1000 base pairs of the nuclear rag2 gene. The phylogeny includes 28 species of Brachyhypopomus and nine outgroup species from nine other gymnotiform genera, including seven in the superfamily Rhamphichthyoidea (Hypopomidae and Rhamphichthyidae). Parsimony and Bayesian total evidence phylogenetic analyses confirm the monophyly of the genus, and identify nine robust species groups. Homoplastic osteological characters associated with diminutive body size and occurrence in small stream habitats, including loss of squamation and simplifications of the skeleton, appear to mislead a phylogenetic analysis based on morphological characters alone-resulting in the incorrect placing of Microsternarchus + Racenisia in a position deeply nested within Brachyhypopomus. Consideration of geographical distribution in light of the total evidence phylogeny indicates an origin for Brachyhypopomus in Greater Amazonia (the superbasin comprising the Amazon, Orinoco and major Guiana drainages), with subsequent dispersal and vicariance in peripheral basins, including the La Plata, the Sao Francisco, and trans-Andean basins of northwest South America and Central America. The ancestral habitat of Brachyhypopomus likely resembled the normoxic, low-conductivity terra firme stream system occupied by many extant species, and the genus has subsequently occupied a wide range of terra firme and floodplain habitats including low-and high-conductivity systems, and normoxic and hypoxic systems. Adaptations for impedance matching to high conductivity, and/or for air breathing in hypoxic systems have attended these habitat transitions. Several species of Brachyhypopomus are eurytopic with respect to habitat occupancy and these generally exhibit wider geographical ranges than stenotopic species. C1 [Crampton, William G. R.; de Santana, Carlos David; Waddell, Joseph C.] Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. [Lovejoy, Nathan R.] Univ Toronto Scarborough, Dept Biol Sci, 1265 Mil Trail, Toronto, ON, Canada. [de Santana, Carlos David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. RP Crampton, WGR (reprint author), Univ Cent Florida, Dept Biol, Orlando, FL 32816 USA. EM crampton@uct.edu FU United States National Science Foundation [DEB-0215388, DEB-0614334, DEB-1146374]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico - Brazil [CNPq 38062/96-2, 381597/97-0]; Ministerio de Ciencia e Tecnologia - Brazil; Instituto de Desenvolvimento Sustentavel Mamiraua - Brazil; Fisheries Society of the British Isles - UK; Crampton Lab (via startup funds from UCF); National Geographic Young Explorers grant [9048-11]; Canadian National Science and Engineering Reseach Council (NSERC) Discovery grants; NSF [DEB-0614334, DEB-1146374] FX WGRC was funded by United States National Science Foundation grants DEB-0215388, DEB-0614334, and DEB-1146374 (and supplements), Conselho Nacional de Desenvolvimento Cientifico e Tecnologico - Brazil (recem doutorado fellowship and grants CNPq 38062/96-2 & 381597/97-0), Ministerio de Ciencia e Tecnologia - Brazil, Instituto de Desenvolvimento Sustentavel Mamiraua - Brazil, and Fisheries Society of the British Isles - UK. CDS was funded by a post-doctoral fellowship from the Crampton Lab (via startup funds to WGRC from UCF). JCW was funded by Research Assistantships from NSF DEB-1146374 and a National Geographic Young Explorers grant (9048-11). NRL was funded by Canadian National Science and Engineering Reseach Council (NSERC) Discovery grants and by sub awards from NSF grants DEB-0614334 and DEB-1146374. NR 125 TC 1 Z9 1 U1 8 U2 8 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 13 PY 2016 VL 11 IS 10 AR e0161680 DI 10.1371/journal.pone.0161680 PG 66 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ0CV UT WOS:000385505800002 PM 27736882 ER PT J AU Midya, B Tomza, M Schmidt, R Lemeshko, M AF Midya, Bikashkali Tomza, Michal Schmidt, Richard Lemeshko, Mikhail TI Rotation of cold molecular ions inside a Bose-Einstein condensate SO PHYSICAL REVIEW A LA English DT Article ID COUPLED-CLUSTER THEORY; POLARIZATION PROPAGATOR; QUANTUM-CHEMISTRY; POLAR-MOLECULES; GROUND-STATE; SPECTROSCOPY; IMPURITY; TRAPS; LASER; TRANSITIONS AB We use recently developed angulon theory [R. Schmidt and M. Lemeshko, Phys. Rev. Lett. 114, 203001 (2015)] to study the rotational spectrum of a cyanide molecular anion immersed into Bose-Einstein condensates of rubidium and strontium. Based on ab initio potential energy surfaces, we provide a detailed study of the rotational Lamb shift and many-body-induced fine structure which arise due to dressing of molecular rotation by a field of phonon excitations. We demonstrate that the magnitude of these effects is large enough in order to be observed in modern experiments on cold molecular ions. Furthermore, we introduce a novel method to construct pseudopotentials starting from the ab initio potential energy surfaces, which provides a means to obtain effective coupling constants for low-energy polaron models. C1 [Midya, Bikashkali; Lemeshko, Mikhail] IST Austria, Campus 1, A-3400 Klosterneuburg, Austria. [Tomza, Michal] Barcelona Inst Sci & Technol, ICFO Inst Ciencies Foton, Barcelona, Spain. [Schmidt, Richard] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Schmidt, Richard] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. RP Midya, B; Lemeshko, M (reprint author), IST Austria, Campus 1, A-3400 Klosterneuburg, Austria.; Tomza, M (reprint author), Barcelona Inst Sci & Technol, ICFO Inst Ciencies Foton, Barcelona, Spain.; Schmidt, R (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.; Schmidt, R (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM bikashkali.midya@ist.ac.at; michal.tomza@icfo.es; richard.schmidt@cfa.harvard.edu; mikhail.lemeshko@ist.ac.at RI Tomza, Michal/B-4791-2012 OI Tomza, Michal/0000-0003-1792-8043 FU NSF; Smithsonian Astrophysical Observatory; People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7) under REA [291734]; EU Marie Curie COFUND action (ICFOnest); EU; Spanish Ministry Grant FOQUS [FIS2013-46768-P]; Spanish Ministry Grant Severo Ochoa [SEV-2015-0522]; Fundacio Cellex; National Science Centre [2015/19/D/ST4/02173]; PL-Grid Infrastructure; Generalitat de Catalunya [SGR 874] FX The work was supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory. B.M. acknowledges financial support received from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007-2013) under REA grant agreement No. 291734. M.T. acknowledges support from the EU Marie Curie COFUND action (ICFOnest), the EU Grants ERC AdG OSYRIS, FP7 SIQS and EQuaM, FETPROACT QUIC, the Spanish Ministry Grants FOQUS (FIS2013-46768-P) and Severo Ochoa (SEV-2015-0522), Generalitat de Catalunya (SGR 874), Fundacio Cellex, the National Science Centre (2015/19/D/ST4/02173), and the PL-Grid Infrastructure. NR 88 TC 2 Z9 2 U1 5 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD OCT 13 PY 2016 VL 94 IS 4 AR 041601 DI 10.1103/PhysRevA.94.041601 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DZ1SA UT WOS:000385618500001 ER PT J AU Mah, CL AF Mah, Christopher L. TI Deep-sea (> 1000 m) Goniasteridae (Valvatida; Asteroidea) from the North Pacific, including an overview of Sibogaster, Bathyceramaster n. gen. and three new species SO ZOOTAXA LA English DT Article DE Deep-sea; bathyal; abyssal; hadal; Echinodermata; Asteroidea; new species ID HIPPASTERINAE GONIASTERIDAE; STARS ASTEROIDEA; ECHINODERMATA; PHYLOGENY; BIOGEOGRAPHY; HOLOTHURIANS; SYSTEMATICS; VALVATACEA; CALIFORNIA; REVISION AB Research cruises by the Monterey Bay Aquarium Research Institute (MBARI) have resulted in the discovery of three new species of asteroids from the lower bathyal/abyssal regions of the North Pacific. A new genus, Bathyceramaster is described to accommodate "Mediaster" elegans Ludwig 1905 and related species. New records and in situ observations are also presented. An identification key and taxonomic account of the deep-sea Goniasteridae known from this region including one new genus and two new species is included. An overview of the genus Sibogaster, including a new widely occurring species, is also included. C1 [Mah, Christopher L.] Smithsonian Inst, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20007 USA. RP Mah, CL (reprint author), Smithsonian Inst, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20007 USA. NR 105 TC 0 Z9 0 U1 6 U2 6 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 13 PY 2016 VL 4175 IS 2 BP 101 EP 141 DI 10.11646/zootaxa.4175.2.1 PG 41 WC Zoology SC Zoology GA DY6PT UT WOS:000385250600001 PM 27811777 ER PT J AU Mulcahy, DG Macdonald, KS Brady, SG Meyer, C Barker, KB Coddington, J AF Mulcahy, Daniel G. Macdonald, Kenneth S., III Brady, Sean G. Meyer, Christopher Barker, Katharine B. Coddington, Jonathan TI Greater than X kb: a quantitative assessment of preservation conditions on genomic DNA quality, and a proposed standard for genome-quality DNA SO PEERJ LA English DT Article DE Agarose gels; DNA extractions; Genomic DNA; Tissue preservation ID TISSUE SAMPLES; SEQUENCE AB Advances in biodiversity genomic sequencing will increasingly depend on the availability of DNA samples-and their quantifiable metadata-preserved in large institutional biorepositories that are discoverable to the scientific community. Improvements in sequencing technology constantly provide longer reads, such that longer fragment length, higher molecular weight, and overall "genome-quality" DNA (gDNA) will be desirable. Ideally, biorepositories should publish numerical scale measurements of DNA quality useful to the user community. However, the most widely used technique to evaluate DNA quality, the classic agarose gel, has yet to be quantified. Here we propose a simple and economical method using open source image analysis software to make gDNA gel images quantifiable, and propose percentage of gDNA "greater than X kb" as a standard of comparison, where X is a band from any widely used DNA ladder with desirably large band sizes. We employ two metadata standards ("DNA Threshold" and "Percent above Threshold") introduced as part of the Global Genome Biodiversity Network (GGBN) Darwin Core extension. We illustrate the method using the traditionally used HindIII ladder and the 9,416 base-pair (bp) band as a standard. We also present data, for two taxa, a vertebrate (fish) and an invertebrate (crab), on how gDNA quality varies with seven tissue preservation methods, time since death, preservation method (i.e. buffers vs. cold temperatures), and storage temperature of various buffers over time. Our results suggest that putting tissue into a buffer prior to freezing may be better than directly into ultra-cold conditions. C1 [Mulcahy, Daniel G.; Barker, Katharine B.; Coddington, Jonathan] Smithsonian Inst, Natl Museum Nat Hist, Global Genome Initiat, Washington, DC 20560 USA. [Macdonald, Kenneth S., III] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20560 USA. [Brady, Sean G.; Coddington, Jonathan] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Meyer, Christopher] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Mulcahy, DG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Global Genome Initiat, Washington, DC 20560 USA. EM MulcahyD@si.edu RI Macdonald, Kenneth/F-9822-2011; OI Brady, Sean/0000-0003-0468-940X FU Smithsonian Institution; National Museum of Natural History's Global Genome Initiative; Laboratories of Analytical Biology (L.A.B.) FX This project was funded by the Smithsonian Institution, National Museum of Natural History's Global Genome Initiative and Laboratories of Analytical Biology (L.A.B.). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 26 TC 0 Z9 0 U1 4 U2 4 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD OCT 11 PY 2016 VL 4 AR e2528 DI 10.7717/peerj.2528 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ1DZ UT WOS:000385580400006 PM 27761327 ER PT J AU Bird, S Rubin, KHR Suresh, J Hernquist, L AF Bird, Simeon Rubin, Kate H. R. Suresh, Joshua Hernquist, Lars TI Simulating the carbon footprint of galactic haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE intergalactic medium; galaxies: formation ID METAL-LINE ABSORPTION; INTERGALACTIC C-IV; GALAXY FORMATION PHYSICS; CIV MASS DENSITY; 10 BILLION YEARS; SIMILAR-TO 6; COSMOLOGICAL SIMULATIONS; STAR-FORMATION; CIRCUMGALACTIC MEDIUM; HYDRODYNAMIC SIMULATIONS AB We compare simulations, including the Illustris simulations, to observations of C IV and C II absorption at z = 2-4. These are the CIV column density distribution function in the column density range 10(12)-10(15) cm(-2), the CIV equivalent width distribution at 0.1-2 angstrom, and the covering fractions and equivalent widths of C IV1548 angstrom and C II 1337 angstrom around damped Lyman alpha systems (DLAs). In the context of the feedback models that we investigate, all CIV observations favour the use of more energetic wind models, which are better able to enrich the gas surrounding haloes. We propose two ways to achieve this: an increased wind velocity and an increase in wind thermal energy. However, even our most energetic wind models do not produce enough absorbers with CIV equivalent width >0.6 angstrom, which in our simulations are associated with the most massive haloes. All simulations are in reasonable agreement with the C II covering fraction and equivalent widths around damped Lyman a absorbers, although there is a moderate deficit in one bin 10-100 kpc from the DLA. Finally, we show that the CIV in our simulations is predominantly photoionized. C1 [Bird, Simeon] Carnegie Mellon Univ, 5000 Forbes Ave, Pittsburgh, PA 15206 USA. [Bird, Simeon] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Rubin, Kate H. R.; Suresh, Joshua; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Bird, S (reprint author), Carnegie Mellon Univ, 5000 Forbes Ave, Pittsburgh, PA 15206 USA.; Bird, S (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA. EM sbird4@jh.edu OI Bird, Simeon/0000-0001-5803-5490 FU NASA through Einstein Postdoctoral Fellowship Award [PF5-160133]; McWilliams Fellowship from Carnegie Mellon University; NASA ATP Award [NNX12AC67G]; NSF [AST-1312095] FX We thank Valentina D'Odorico for sharing her data on the C IV column density function, Ben Oppenheimer and Ali Rahmati for sharing CIV column density tables from their simulations with us, J. X. Prochaska for reading a draft and providing thoughtful comments, and Volker Springel for writing and allowing us to use the AREPO code. We also thank Kathy Cooksey for sharing her data on the C IV equivalent width function, for many interesting discussions and for proof-reading a draft. SB was supported by NASA through Einstein Postdoctoral Fellowship Award Number PF5-160133 and by a McWilliams Fellowship from Carnegie Mellon University. LH is supported by NASA ATP Award NNX12AC67G and NSF grant AST-1312095. NR 63 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 307 EP 322 DI 10.1093/mnras/stw1582 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700048 ER PT J AU Girart, JM Torrelles, JM Estalella, R Curiel, S Anglada, G Gomez, JF Carrasco-Gonzalez, C Canto, J Rodriguez, LF Patel, NA Trinidad, MA AF Girart, J. M. Torrelles, J. M. Estalella, R. Curiel, S. Anglada, G. Gomez, J. F. Carrasco-Gonzalez, C. Canto, J. Rodriguez, L. F. Patel, N. A. Trinidad, M. A. TI SMA observations towards the compact, short-lived bipolar water maser outflow in the LkH alpha 234 region SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE masers; stars: formation; ISM: individual objects: LkH alpha 234-VLA 2; ISM: jets and outflows; ISM: molecules ID LKH-ALPHA 234; YOUNG STELLAR OBJECTS; HERBIG-HARO OBJECTS; MAGNETIC-FIELDS; STAR-FORMATION; PROTOSTELLAR CORES; HIGH-VELOCITY; SIO EMISSION; AFGL 2591; EVOLUTION AB We present Submillimeter Array (SMA) 1.35 mm subarcsecond angular resolution observations towards the LkH alpha 234 intermediate-mass star-forming region. The dust emission arises from a filamentary structure of similar to 5 arcsec (similar to 4500 au) enclosing VLA 1-3 and MM 1, perpendicular to the different outflows detected in the region. The most evolved objects are located at the southeastern edge of the dust filamentary structure and the youngest ones at the northeastern edge. The circumstellar structures around VLA 1, VLA 3, and MM 1 have radii between similar to 200 and similar to 375 au and masses in the similar to 0.08-0.3 M-circle dot range. The 1.35 mm emission of VLA 2 arises from an unresolved (r less than or similar to 135 au) circumstellar disc with a mass of similar to 0.02 M-circle dot. This source is powering a compact (similar to 4000 au), low radial velocity (similar to 7 km s(-1)) SiO bipolar outflow, close to the plane of the sky. We conclude that this outflow is the 'large-scale' counterpart of the short-lived, episodic, bipolar outflow observed through H2O masers at much smaller scales (similar to 180 au), and that has been created by the accumulation of the ejection of several episodic collimated events of material. The circumstellar gas around VLA 2 and VLA 3 is hot (similar to 130 K) and exhibits velocity gradients that could trace rotation. There is a bridge of warm and dense molecular gas connecting VLA 2 and VLA 3. We discuss the possibility that this bridge could trace a stream of gas between VLA 3 and VLA 2, increasing the accretion rate on to VLA 2 to explain why this source has an important outflow activity. C1 [Girart, J. M.; Patel, N. A.] Inst Ciencies Espai CSIC IEEC, Can Magrans S-N, E-08193 Cerdanyola Del Valles, Spain. [Girart, J. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Torrelles, J. M.] Inst Ciencies Espai CSIC IEEC, Marti I Franques 1, E-08028 Barcelona, Catalonia, Spain. [Torrelles, J. M.] Inst Ciencies Cosmos UB IEEC, Marti I Franques 1, E-08028 Barcelona, Catalonia, Spain. [Estalella, R.] Univ Barcelona, Dept Fis Quant & Astrofis, Marti I Franques 1, E-08028 Barcelona, Catalonia, Spain. [Estalella, R.] Univ Barcelona, Inst Ciencies Cosmos IEEC UB, Marti I Franques 1, E-08028 Barcelona, Catalonia, Spain. [Curiel, S.; Canto, J.] Univ Nacl Autonoma Mexico, Inst Astron, Apartado 70-264, Mexico City 04510, DF, Mexico. [Anglada, G.; Gomez, J. F.] CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain. [Carrasco-Gonzalez, C.; Rodriguez, L. F.] Inst Radioastron & Astrofis UNAM, Morelia 58089, Michoacan, Mexico. [Trinidad, M. A.] Univ Guanajuato, Dept Astron, Apdo Postal 144, Guanajuato 36000, Mexico. RP Girart, JM (reprint author), Inst Ciencies Espai CSIC IEEC, Can Magrans S-N, E-08193 Cerdanyola Del Valles, Spain.; Girart, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM girart@ieec.cat FU MINECO (Spain) [AYA2014-57369-C3]; FEDER funds; MECD grant (Spain) [PRX15/00435]; SI CGPS award, 'Magnetic Fields and Massive Star Formation'; DGAPA (Mexico); UNAM (Mexico); CONACyT (Mexico) FX GA, RE, JMG, JFG, and JMT acknowledge support from MINECO (Spain) AYA2014-57369-C3 grant (co-funded with FEDER funds). JMG also acknowledges support from the MECD PRX15/00435 grant (Spain) and from the SI CGPS award, 'Magnetic Fields and Massive Star Formation'. RE also acknowledges MDM-2014-0369 of ICCUB (Unidad de Excelencia 'Maria de Maeztu'). SC acknowledges the support of DGAPA, UNAM, and CONACyT (Mexico). NR 36 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 352 EP 361 DI 10.1093/mnras/stw1660 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700052 ER PT J AU Gereb, K Catinella, B Cortese, L Bekki, K Moran, SM Schiminovich, D AF Gereb, K. Catinella, B. Cortese, L. Bekki, K. Moran, S. M. Schiminovich, D. TI GASS 3505: the prototype of HI-excess, passive galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: interactions; radio lines: galaxies ID I-RICH GALAXIES; FAST ALPHA SURVEY; SIMILAR-TO 0; ARECIBO SDSS SURVEY; DIGITAL SKY SURVEY; STAR-FORMATION; NEUTRAL-HYDROGEN; SCALING-RELATIONS; MASSIVE GALAXIES; NEARBY GALAXIES AB We present our multiwavelength analysis of a prototype HI-excess galaxy, GASS 3505, selected based on having a large gas content (M-HI = 10(9.9) M-circle dot) compared to its little associated star formation activity (similar to 0.1 M-circle dot yr(-1)) in the GALEX Arecibo SDSS Survey (GASS). Very Large Array observations show that the HI in GASS 3505 is distributed in a regularly rotating, extended (similar to 50 kpc radius) gas ring. In the SDSS optical image GASS 3505 appears as a bulge-dominated galaxy, however deep optical imaging reveals low surface brightness (greater than or similar to 25 mag arcsec(-2)) stellar emission around the central bulge. Direct evidence for accretion is detected in form of an extended (similar to 60 kpc) stellar stream, showing that GASS 3505 has experienced a minor merger in the recent past. We investigate the possibility that the HI ring in GASS 3505 was accreted in such a merger event using N-body and smoothed particle hydrodynamic simulations. The best model that reproduces the general properties (i.e. gas distribution and kinematics, stellar morphology) of the galaxy involves a merger between the central bulge and a gas-rich (M-star = 10(9) M-circle dot and M-HI/M-star = 10) disc galaxy. However, small discrepancies in the observed and modelled properties could suggest that other sources of gas have to be involved in the build-up of the gas reservoir. This work is the first step towards a larger program to investigate the physical mechanisms that drive the large scatter in the gas scaling relations of nearby galaxies. C1 [Gereb, K.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Catinella, B.; Cortese, L.; Bekki, K.] Univ Western Australia, M468, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia. [Moran, S. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Schiminovich, D.] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. RP Gereb, K (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM kgereb@swin.edu.au; barbara.catinella@uwa.edu.au OI Cortese, Luca/0000-0002-7422-9823 FU Australian Research Council [FT120100660, DP130100664, DP150101734] FX We thank the anonymous referee for the useful comments that helped us to improve the manuscript. KG thanks Tobias Brown, Virginia Kilborn, and Katharina Lutz for helpful discussions on this project. BC is the recipient of an Australian Research Council Future Fellowship (FT120100660). BC, KB and LC acknowledge support from the Australian Research Council's Discovery Projects funding scheme (DP130100664 and DP150101734). BC thanks Jacqueline van Gorkom and Baerbel Koribalski for help with the preliminary reduction of VLA data used in this paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 81 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 382 EP 394 DI 10.1093/mnras/stw1675 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700054 ER PT J AU Black, CS Fesen, RA Parrent, JT AF Black, C. S. Fesen, R. A. Parrent, J. T. TI Progressive redshifts in the late-time spectra of Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE line formation; radiative transfer; supernovae: general ID SN 2011FE; NEBULAR SPECTRA; DELAYED-DETONATION; OPTICAL SPECTROSCOPY; ASYMMETRIC EXPLOSION; LINE-PROFILES; LIGHT CURVES; EMISSION; MODELS; CARBON AB We examine the evolution of late-time, optical nebular features of Type Ia supernovae (SNe Ia) using a sample consisting of 160 spectra of 27 normal SNe Ia taken from the literature as well as unpublished spectra of SN 2008Q and ASASSN-141p. Particular attention was given to nebular features between 4000 and 6000 angstrom in terms of temporal changes in width and central wavelength. Analysis of the prominent late-time 4700 angstrom feature shows a progressive central wavelength shift from similar to 4600 angstrom to longer wavelengths out to at least day +300 for our entire sample. We find no evidence for the feature's redward shift slowing or halting at an [Ferry] blend centroid similar to 4700 angstrom as has been proposed. The width of this feature also steadily increases with a FWHM similar to 170 angstrom at day +100 growing to 200 angstrom or more by day +350. Two weaker adjacent features at around 4850 and 5000 A exhibit similar redshifts to that of the 4700 angstrom feature but show no change in width until very late times. We discuss possible causes for the observed redshifts of these late-time optical features including contribution from [Co II] emission at early nebular epochs and the emergence of additional features at later times. We conclude that the ubiquitous redshift of these common late-time SN Ia spectral features is not mainly due to a decrease in line velocities of forbidden Fe emissions, but the result of decreasing line velocities and opacity of permitted Fe absorption lines. C1 [Black, C. S.; Fesen, R. A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Parrent, J. T.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Black, CS (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. EM christine.black.gr@dartmouth.edu OI Black, Christine/0000-0002-4471-9960 FU Dartmouth's School of Graduate and Advanced Studies; NASA/STScI [12609, 13471] FX The authors wish to thank the referee for providing useful comments and suggestions, M. Modjaz and P. Challis for obtaining the Keck and MMT data on SN 2008Q. We also wish to thank L. Dessert and S. Blondin for making public their model spectra and the staff of MDM Observatory for their assistance in making these observations possible. CSB's supernova research is supported in part by a Fellowship from Dartmouth's School of Graduate and Advanced Studies. RAF's Type Ia supernova research is funded in part by NASA/STScI grants 12609 and 13471. This work was made possible by contributions to the Supernova Spectrum Archive (Richardson et al. 2001), the Weizmann Interactive Supernova data REPository (WISeREP Yaron & Gal-Yam 2012), and the Berkeley SN Ia Program (BSNIP Silverman et al. 2012). Several model spectra, as well as some of the data that were not available on WISeREP at the time of our initial study were obtained with the help of the graph digitizer software, GRAPHCLICK.3 NR 74 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 649 EP 662 DI 10.1093/mnras/stw1680 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700075 ER PT J AU Garcia, JA Fabian, AC Kallman, TR Dauser, T Parker, ML McClintock, JE Steiner, JF Wilms, J AF Garcia, Javier A. Fabian, Andrew C. Kallman, Timothy R. Dauser, Thomas Parker, Michael L. McClintock, Jeffrey E. Steiner, James F. Wilms, Joern TI The effects of high density on the X-ray spectrum reflected from accretion discs around black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; atomic processes; line: formation; radiative transfer; relativistic processes; X-rays: general ID ACTIVE GALACTIC NUCLEI; K-SHELL PHOTOABSORPTION; ENERGY-DISTRIBUTIONS; SUZAKU OBSERVATIONS; XMM-NEWTON; GX 339-4; SOFT EXCESS; HARD STATE; CYGNUS X-1; IRON LINES AB Current models of the spectrum of X-rays reflected from accretion discs around black holes and other compact objects are commonly calculated assuming that the density of the disc atmosphere is constant within several Thomson depths from the irradiated surface. An important simplifying assumption of these models is that the ionization structure of the gas is completely specified by a single, fixed value of the ionization parameter xi, which is the ratio of the incident flux to the gas density. The density is typically fixed at n(e) = 10(15) cm(-3). Motivated by observations, we consider higher densities in the calculation of the reflected spectrum. We show by computing model spectra for n(e) greater than or similar to 10(17) cm(-3) that high-density effects significantly modify reflection spectra. The main effect is to boost the thermal continuum at energies less than or similar to 2 keV. We discuss the implications of these results for interpreting observations of both active galactic nuclei and black hole binaries. We also discuss the limitations of our models imposed by the quality of the atomic data currently available. C1 [Garcia, Javier A.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fabian, Andrew C.; Parker, Michael L.] Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Kallman, Timothy R.] NASA Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. [Dauser, Thomas; Wilms, Joern] Univ Erlangen Nurnberg, Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany. [Dauser, Thomas; Wilms, Joern] Univ Erlangen Nurnberg, ECAP, Sternwartstr 7, D-96049 Bamberg, Germany. [Steiner, James F.] MIT, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. RP Garcia, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; acf@ast.cam.ac.uk RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 FU CGPS grant from the Smithsonian Institution; ERC [340442]; Einstein Fellowship [PF5-160144] FX We thank the anonymous referee for their positive and useful comments, and Laura Brenneman for insightful discussions. JG and JEM acknowledge the support of a CGPS grant from the Smithsonian Institution. ACF acknowledges ERC Advanced Grant 340442 Feedback. JFS has been supported by the Einstein Fellowship grant PF5-160144. NR 73 TC 3 Z9 3 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 751 EP 760 DI 10.1093/mnras/stw1696 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700083 ER PT J AU Zenteno, A Mohr, JJ Desai, S Stalder, B Saro, A Dietrich, JP Bayliss, M Bocquet, S Chiu, I Gonzalez, AH Gangkofner, C Gupta, N Hlavacek-Larrondo, J McDonald, M Reichardt, C Rest, A AF Zenteno, A. Mohr, J. J. Desai, S. Stalder, B. Saro, A. Dietrich, J. P. Bayliss, M. Bocquet, S. Chiu, I. Gonzalez, A. H. Gangkofner, C. Gupta, N. Hlavacek-Larrondo, J. McDonald, M. Reichardt, C. Rest, A. TI Galaxy populations in the 26 most massive galaxy clusters in the South Pole Telescope SPT-SZ survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: formation; cosmology: observations ID BAND LUMINOSITY FUNCTION; SIMILAR-TO 1; ATACAMA COSMOLOGY TELESCOPE; COLOR-MAGNITUDE RELATION; ZELDOVICH EFFECT SURVEY; 720 SQUARE DEGREES; RED-SEQUENCE; X-RAY; STELLAR MASS; RADIAL-DISTRIBUTION AB We present a study of the optical properties of the 26 most massive galaxy clusters within the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) 2500 deg(2) survey spanning the redshift range 0.10 < z < 1.13. We measure the radial profiles, the luminosity functions (LFs), and the halo occupation numbers (HONs) using optical data of typical depth m* + 2. The stacked radial profiles are consistent with a Navarro-Frenk-White profile of concentration 2.84(-0.37)(+0.40) for the red sequence (RS) and 2.36(-0.35)(+0.38) for the total population. Stacking the data in multiple redshift bins shows slight redshift evolution in the concentration when both the total population is used, and when only RS galaxies are used (at 2.1 sigma and 2.8 sigma, respectively). The stacked LF shows a faint end slope alpha = -1.06(-0.03)(+0.04) for the total and a = -0.80(-0.03)(+0.04) for the RS population. The redshift evolution of m* is consistent with a passively evolving composite stellar population (CSP) model. Adopting the CSP model predictions, we explore the redshift evolution of the Schechter parameters alpha and phi*. We find alpha for the total population to be consistent with no evolution (0.3 sigma), and mildly significant evidence of evolution for the red galaxies (1.1-2.1 sigma). The data show that the density phi*/E-2(z) decreases with redshift, in tension with the self-similar expectation at a 2.4 sigma level for the total population. The measured HON-mass relation has a lower normalization than previous low redshift studies. Finally, our data support HON redshift evolution at a 2.1 sigma level, with clusters at higher redshift containing fewer galaxies than their low-z counterparts. C1 [Zenteno, A.] Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Zenteno, A.; Mohr, J. J.; Desai, S.; Saro, A.; Dietrich, J. P.; Bocquet, S.; Chiu, I.; Gangkofner, C.; Gupta, N.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Mohr, J. J.; Desai, S.; Saro, A.; Dietrich, J. P.; Bocquet, S.; Chiu, I.; Gangkofner, C.; Gupta, N.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Desai, S.] Indian Inst Technol Hyderabad, Dept Phys, Kandi 502285, Telangana, India. [Stalder, B.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Stalder, B.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Bayliss, M.] Colby Coll, Dept Phys & Astron, 5800 Mayflower Hill, Waterville, ME 04901 USA. [Bayliss, M.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Chiu, I.] ASIAA, 11F AS NTU Astron Math Bldg,1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hlavacek-Larrondo, J.] Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Reichardt, C.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Rest, A.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Zenteno, A (reprint author), Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile.; Zenteno, A (reprint author), Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. EM azenteno@ctio.noao.edu FU DFG Cluster of Excellence 'Origin and Structure of the Universe'; Transregio Program 'The Dark Universe' [TR33]; Ludwig-Maximilians-Universitat; National Science Foundation [PLR-1248097]; NSF Physics Frontier Center [PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation [GBMF 947]; Australian Research Council [DP150103208] FX We acknowledge the support by the DFG Cluster of Excellence 'Origin and Structure of the Universe', the Transregio Program TR33 'The Dark Universe' and the Ludwig-Maximilians-Universitat. The data processing has been carried out on the computing facilities of the Computational Center for Particle and Astrophysics (C2PAP), located at the Leibniz Supercomputer Center (LRZ). The South Pole Telescope is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation grant GBMF 947. CR acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208). This paper includes data gathered with the Blanco 4-m telescope, located at the Cerro Tololo Inter-American Observatory in Chile, which is part of the US National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), under contract with the National Science Foundation. Other data come from the European Southern Observatory telescopes on La Silla and Paranal. We are very grateful for the efforts of the CTIO, La Silla, and Paranal support staff without whom this paper would not be possible. NR 116 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 830 EP 843 DI 10.1093/mnras/stw1649 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700089 ER PT J AU Riseley, CJ Scaife, AMM Hales, CA Harrison, I Birkinshaw, M Battye, RA Beswick, RJ Brown, ML Casey, CM Chapman, SC Demetroullas, C Hung, CL Jackson, NJ Muxlow, T Watson, B AF Riseley, C. J. Scaife, A. M. M. Hales, C. A. Harrison, I. Birkinshaw, M. Battye, R. A. Beswick, R. J. Brown, M. L. Casey, C. M. Chapman, S. C. Demetroullas, C. Hung, C. -L. Jackson, N. J. Muxlow, T. Watson, B. TI Deep observations of the Super-CLASS supercluster at 325 MHz with the GMRT: the low-frequency source catalogue SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; radio continuum: general ID SPECTRUM RADIO-SOURCES; VLA-COSMOS SURVEY; ALL-SKY SURVEY; FLUX-DENSITY MEASUREMENTS; LARGE-SCALE STRUCTURE; FREE-FREE ABSORPTION; SOURCE COUNTS; SOURCE POPULATION; 610-MHZ SURVEY; DATA RELEASE AB We present the results of 325 MHz Giant Metrewave Radio Telescope observations of a supercluster field, known to contain five Abell clusters at redshift z similar to 0.2. We achieve a nominal sensitivity of 34 mu Jy beam(-1) towards the phase centre. We compile a catalogue of 3257 sources with flux densities in the range 183 mu Jy-1.5 Jy within the entire similar to 6.5 deg(2) field of view. Subsequently, we use available survey data at other frequencies to derive the spectral index distribution for a sub-sample of these sources, recovering two distinct populations - a dominant population which exhibit spectral index trends typical of steep-spectrum synchrotron emission, and a smaller population of sources with typically flat or rising spectra. We identify a number of sources with ultrasteep spectra or rising spectra for further analysis, finding two candidate high-redshift radio galaxies and three gigahertz-peaked-spectrum radio sources. Finally, we derive the Euclidean-normalized differential source counts using the catalogue compiled in this work, for sources with flux densities in excess of 223 mu Jy. Our differential source counts are consistent with both previous observations at this frequency and models of the low-frequency source population. These represent the deepest source counts yet derived at 325 MHz. Our source counts exhibit the well-known flattening at mJy flux densities, consistent with an emerging population of star-forming galaxies; we also find marginal evidence of a downturn at flux densities below 308 mu Jy, a feature so far only seen at 1.4 GHz. C1 [Riseley, C. J.; Scaife, A. M. M.; Harrison, I.; Battye, R. A.; Beswick, R. J.; Brown, M. L.; Demetroullas, C.; Jackson, N. J.; Muxlow, T.; Watson, B.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Riseley, C. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hales, C. A.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA. [Birkinshaw, M.] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Birkinshaw, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Casey, C. M.; Hung, C. -L.] Univ Texas Austin, Dept Astron, 2515 Speedway Blvd,Stop C1400, Austin, TX 78712 USA. [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Coburg Rd, Halifax, NS B3H 1A6, Canada. RP Riseley, CJ (reprint author), Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England.; Riseley, CJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM c.j.riseley@manchester.ac.uk RI Hales, Christopher/J-6048-2014; OI Hales, Christopher/0000-0002-3733-2565; Riseley, Christopher/0000-0002-3369-1085 FU NASA; United Kingdom Science and Technology Facilities Council (STFC); European Research Council [ERC-2012-StG-307215 LODESTONE]; European Research Council through EC [280127]; STFC [ST/I005129/1] FX This work has made use of the NASA/IPAC Extragalactic Database (NED), operated by JPL under contract with NASA, as well as NASA's Astrophysics Data System (ADS) and the Cosmological Calculator developed by Wright (2006). This work has also used data from the Owens Valley Radio Observatory (OVRO) blazar monitoring data base, available at http://www.astro.caltech.edu/ovroblazars/.; CJR gratefully acknowledges funding support from the United Kingdom Science and Technology Facilities Council (STFC). AMS gratefully acknowledges support from the European Research Council under grant ERC-2012-StG-307215 LODESTONE. IH, MLB and CD are grateful to the European Research Council for support through EC FP7 grant number 280127. MLB also thanks the STFC for the award of Advanced and Halliday fellowships (grant number ST/I005129/1). NR 118 TC 1 Z9 1 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2016 VL 462 IS 1 BP 917 EP 940 DI 10.1093/mnras/stw1734 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3BI UT WOS:000383516700096 ER PT J AU Kreisch, CD Machacek, ME Jones, C Randall, SW AF Kreisch, C. D. Machacek, M. E. Jones, C. Randall, S. W. TI MERGER HYDRODYNAMICS OF THE LUMINOUS CLUSTER RX J1347.5-1145 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (RX J1347.5-1145); galaxies: interactions; X-rays: galaxies: clusters ID KELVIN-HELMHOLTZ INSTABILITIES; DEEP CHANDRA OBSERVATIONS; RELAXED GALAXY CLUSTERS; XMM-NEWTON OBSERVATION; SLOSHING COLD FRONTS; X-RAY DATA; MASS-DISTRIBUTION; COOLING FLOWS; GAS; CORES AB We present an analysis of the complex gas hydrodynamics in the X-ray-luminous galaxy cluster RX J1347.5-1145 caught in the act of merging with a subcluster to its southeast using a combined. 186. ks Chandra exposure,. 2.5. times greater than previous analyses. The primary cluster hosts a sloshing cold front spiral traced by four surface brightness edges. 5 ''.85(-0.03)(+0.04) west,. 7 ''.10(-0.03)(+0.07) southeast,. 11 ''.5(-1.2)(+1.3) east, and 16 ''.7(-0.5)(+0.3) northeast from the primary central dominant galaxy, suggesting. that the merger is in the plane of the sky. We measure temperature and density ratios across these edges, confirming that. they are sloshing cold fronts. We observe the eastern edge of the subcluster infall shock, confirming that the observed subcluster is traveling from the southwest to the northeast in a clockwise orbit. We measure a shock density contrast of. 1.38(-0.15)(+0.16) and infer a Mach number of 1.25 +/- 0.08 and a shock velocity of 2810(-240)(+210) km s(-1). Temperature and entropy maps show cool, low-entropy gas trailing the subcluster in a southwestern tail, consistent with core shredding. Simulations suggest that a perturber in the plane of the sky on a clockwise orbit would produce a sloshing spiral winding counterclockwise, opposite to that observed. The most compelling solution to this discrepancy is that the observed southeastern subcluster is on its first passage, shock-heating gas during its clockwise infall, while the main cluster's clockwise cold front spiral formed from earlier encounters with a second perturber orbiting counterclockwise. C1 [Kreisch, C. D.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Kreisch, C. D.] Washington Univ, Dept Phys, One Brookings Dr, St Louis, MO 63130 USA. [Machacek, M. E.; Jones, C.; Randall, S. W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Kreisch, CD (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany.; Kreisch, CD (reprint author), Washington Univ, Dept Phys, One Brookings Dr, St Louis, MO 63130 USA. EM ckreisch@wustl.edu OI Kreisch, Christina/0000-0002-5061-7805 FU NASA CXC grant [GO2-13148X]; Smithsonian Institution; Smithsonian Institution Minority Awards Program; National Aeronautics and Space Administration FX This work was supported in part by NASA CXC grant GO2-13148X and the Smithsonian Institution. C.K. gratefully acknowledges support from the Smithsonian Institution Minority Awards Program. This research has made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog. and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa. This work has made use of the NASA/IPAC Extragalactic Database (NED),. which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We would like to thank Maxim Markevitch for helpful discussions and use of his multivariate chi2 minimization code for fitting the surface brightness profiles, Brian Mason for use of his SZ contours, Jeremy Sanders for help with his GGM filtering technique, Sherry Suyu for useful strong-lensing discussions, and the anonymous referee for exceptionally helpful comments. NR 57 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2016 VL 830 IS 1 BP 1 EP 15 AR 39 DI 10.3847/0004-637X/830/1/39 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ8ML UT WOS:000386124400001 ER PT J AU Kane, SR Hill, ML Kasting, JF Kopparapu, RK Quintana, EV Barclay, T Batalha, NM Borucki, WJ Ciardi, DR Haghighipour, N Hinkel, NR Kaltenegger, L Selsis, F Torres, G AF Kane, Stephen R. Hill, Michelle L. Kasting, James F. Kopparapu, Ravi Kumar Quintana, Elisa V. Barclay, Thomas Batalha, Natalie M. Borucki, William J. Ciardi, David R. Haghighipour, Nader Hinkel, Natalie R. Kaltenegger, Lisa Selsis, Franck Torres, Guillermo TI A CATALOG OF KEPLER HABITABLE ZONE EXOPLANET CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; astronomical databases: miscellaneous; planetary systems; techniques: photometric ID MAIN-SEQUENCE STARS; FALSE-POSITIVE PROBABILITIES; CARBON-DIOXIDE CLOUDS; EARTH-LIKE PLANETS; INNER EDGE; STELLAR MULTIPLICITY; TERRESTRIAL PLANETS; EXTRASOLAR PLANETS; SYSTEMS. I.; MASS STARS AB The NASA Kepler mission has discovered thousands of new planetary candidates, many of which have been confirmed through follow-up observations. A primary goal of the mission is to determine the occurrence rate of terrestrial-size planets within the Habitable Zone (HZ) of their host stars. Here we provide a list of HZ exoplanet candidates from the Kepler Q1-Q17 Data Release 24 data-vetting process. This work was undertaken as part of the Kepler HZ Working Group. We use a variety of criteria regarding HZ boundaries and planetary sizes to produce complete lists of HZ candidates, including a catalog of 104 candidates within the optimistic HZ and 20 candidates with radii less than two Earth radii within the conservative HZ. We cross-match our HZ candidates with the stellar properties and confirmed planet properties from Data Release 25 to provide robust stellar parameters and candidate dispositions. We also include false-positive probabilities recently calculated by Morton et al. for each of the candidates within our catalogs to aid in their validation. Finally, we performed dynamical analysis simulations for multi-planet systems that contain candidates with radii less than two Earth radii as a step toward validation of those systems. C1 [Kane, Stephen R.; Hill, Michelle L.; Hinkel, Natalie R.] San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. [Kasting, James F.] Penn State Univ, Dept Geosci, 443 Deike Bldg, University Pk, PA 16802 USA. [Kopparapu, Ravi Kumar] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Mail Stop 699-0 Bldg 34, Greenbelt, MD 20771 USA. [Quintana, Elisa V.; Barclay, Thomas; Batalha, Natalie M.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ciardi, David R.] NASA, Exoplanet Sci Inst, CALTECH, MS 100-22,770 South Wilson Ave, Pasadena, CA 91125 USA. [Haghighipour, Nader] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Hinkel, Natalie R.] Arizona State Univ, Sch Earth Space Explorat, Tempe, AZ 85287 USA. [Kaltenegger, Lisa] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA. [Selsis, Franck] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18N, Allee Geoffroy St Hilaire, F-33615 Pessac, France. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Kane, SR (reprint author), San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. EM skane@sfsu.edu OI Ciardi, David/0000-0002-5741-3047; Kasting, James/0000-0003-4042-2067 FU NASA ADAP grant [NNX13AF20G]; NASA Astrobiology Institute; NASA [NNH05ZDA001C]; NASA Habitable Worlds grant [NNH14ZDA001N-HW]; agency's Science Mission Directorate FX The authors would like to thank the anonymous referee, whose comments greatly improved the quality of the paper. The authors also thank Douglas Caldwell and Timothy Morton for enlightening discussions regarding Kepler candidate validation. Nader Haghighipour acknowledges support from NASA ADAP grant NNX13AF20G. James Kasting and Ravi Kopparapu gratefully acknowledge funding from the NASA Astrobiology Institute's lead team, supported by NASA under cooperative agreement NNH05ZDA001C. Ravi Kopparapu also acknowledges support from NASA Habitable Worlds grant NNH14ZDA001N-HW. Kepler is NASA's 10th Discovery Mission and was funded by the agency's Science Mission Directorate. This research has made use of the NASA Exoplanet Archive and the ExoFOP site, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has also made use of the Habitable Zone Gallery at hzgallery.org. The results reported herein benefited from collaborations and/or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate. NR 88 TC 1 Z9 1 U1 15 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2016 VL 830 IS 1 AR 1 DI 10.3847/0004-637X/830/1/1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ2EP UT WOS:000385655400001 ER PT J AU Bu, HL Wang, F McShea, WJ Lu, Z Wang, DJ Li, S AF Bu, Hongliang Wang, Fang McShea, William J. Lu, Zhi Wang, Dajun Li, Sheng TI Spatial Co-Occurrence and Activity Patterns of Mesocarnivores in the Temperate Forests of Southwest China SO PLOS ONE LA English DT Article ID CAT PRIONAILURUS-BENGALENSIS; MESOPREDATOR RELEASE; BIODIVERSITY CONSERVATION; SUBTROPICAL FOREST; MARTES-FLAVIGULA; CENTRAL THAILAND; SMALL CARNIVORES; TROPICAL FOREST; SOUTHERN TAIWAN; DIETARY SHIFTS AB Understanding the interactions between species and their coexistence mechanisms will help explain biodiversity maintenance and enable managers to make sound conservation decisions. Mesocarnivores are abundant and diverse mid-sized carnivores and can have profound impacts on the function, structure and dynamics of ecosystem after the extirpation of apex predators in many ecosystems. The moist temperate forests of Southwest China harbor a diverse community of mesocarnivores in the absence of apex predators. Sympatric species tend to partition limited resources along time, diet and space to facilitate coexistence. We determined the spatial and temporal patterns for five species of mesocarnivores. We used detection histories from a large camera-trap dataset collected from 2004-2015 with an extensive effort of 23,313 camera-days from 495 camera locations. The five mesocarnivore species included masked palm civet Paguma larvata, leopard cat Prionailurus bengalensis, hog badger Arctonyx collaris, yellow-throated marten Martes flavigula, and Siberian weasel Mustela sibirica. Only the masked palm civet and hog badger tended to avoid each other; while for other pairs of species, they occurred independently of each other, or no clear pattern observed. With regard to seasonal activity, yellow-throated marten was most active in winter, opposite the pattern observed for masked palm civet, leopard cat and hog badger. For diel activity, masked palm civet, leopard cat and hog badger were primarily nocturnal and crepuscular; yellow-throated marten was diurnal, and Siberian weasel had no clear pattern for most of the year (March to November), but was nocturnal in the winter (December to February). The seasonal shift of the Siberian weasel may be due to the high diet overlap among species in winter. Our results provided new facts and insights into this unique community of mesocarnivores of southwest China, and will facilitate future studies on the mechanism determining coexistence of animal species within complex system. C1 [Bu, Hongliang; Lu, Zhi; Wang, Dajun; Li, Sheng] Peking Univ, Sch Life Sci, Beijing 100871, Peoples R China. [Wang, Fang] Michigan State Univ, Ctr Syst Integrat & Sustainabil, E Lansing, MI 48823 USA. [McShea, William J.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Wang, DJ; Li, S (reprint author), Peking Univ, Sch Life Sci, Beijing 100871, Peoples R China. EM djwang@pku.edu.cn; shengli@pku.edu.cn FU Sichuan Nature Conservancy Foundation [SNCF/PU092013] FX This work was funded by the Sichuan Nature Conservancy Foundation, grant number: SNCF/PU092013 NR 61 TC 1 Z9 1 U1 24 U2 24 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 10 PY 2016 VL 11 IS 10 AR e0164271 DI 10.1371/journal.pone.0164271 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ0CF UT WOS:000385504100038 PM 27723772 ER PT J AU Cetina, M Jag, M Lous, RS Fritsche, I Walraven, JTM Grimm, R Levinsen, J Parish, MM Schmidt, R Knap, M Demler, E AF Cetina, Marko Jag, Michael Lous, Rianne S. Fritsche, Isabella Walraven, Jook T. M. Grimm, Rudolf Levinsen, Jesper Parish, Meera M. Schmidt, Richard Knap, Michael Demler, Eugene TI Ultrafast many-body interferometry of impurities coupled to a Fermi sea SO SCIENCE LA English DT Article ID DYNAMICS; POLARONS; OPTICS; ATOMS; GAS AB The fastest possible collective response of a quantum many-body system is related to its excitations at the highest possible energy. In condensed matter systems, the time scale for such "ultrafast" processes is typically set by the Fermi energy. Taking advantage of fast and precise control of interactions between ultracold atoms, we observed nonequilibrium dynamics of impurities coupled to an atomic Fermi sea. Our interferometric measurements track the nonperturbative quantum evolution of a fermionic many-body system, revealing in real time the formation dynamics of quasi-particles and the quantum interference between attractive and repulsive states throughout the full depth of the Fermi sea. Ultrafast time-domain methods applied to strongly interacting quantum gases enable the study of the dynamics of quantum matter under extreme nonequilibrium conditions. C1 [Cetina, Marko; Jag, Michael; Lous, Rianne S.; Fritsche, Isabella; Walraven, Jook T. M.; Grimm, Rudolf] Austrian Acad Sci, Inst Quantenopt & Quanteninformat, A-6020 Innsbruck, Austria. [Cetina, Marko; Jag, Michael; Lous, Rianne S.; Fritsche, Isabella; Grimm, Rudolf] Univ Innsbruck, Inst Expt Phys, A-6020 Innsbruck, Austria. [Walraven, Jook T. M.] Univ Amsterdam, Inst Phys, Van der Waals Zeeman Inst, NL-1098 XH Amsterdam, Netherlands. [Levinsen, Jesper; Parish, Meera M.] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia. [Schmidt, Richard] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA. [Schmidt, Richard; Demler, Eugene] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Tech Univ Munich, Walter Schottky Inst, Dept Phys, D-85748 Garching, Germany. [Knap, Michael] Tech Univ Munich, Inst Adv Study, D-85748 Garching, Germany. [Cetina, Marko] Univ Maryland, College Pk, MD 20740 USA. RP Grimm, R (reprint author), Austrian Acad Sci, Inst Quantenopt & Quanteninformat, A-6020 Innsbruck, Austria.; Grimm, R (reprint author), Univ Innsbruck, Inst Expt Phys, A-6020 Innsbruck, Austria. EM rudolf.grimm@uibk.ac.at RI Grimm, Rudolf/D-2864-2009; Knap, Michael/H-3344-2011 OI Grimm, Rudolf/0000-0003-1085-5558; Knap, Michael/0000-0002-7093-9502 FU NSF through a grant for ITAMP at Harvard University; Smithsonian Astrophysical Observatory; Technical University of Munich-Institute for Advanced Study; German Excellence Initiative and the European Union FP7 [291763]; Harvard-MIT Center for Ultracold Atoms, NSF [DMR-1308435]; Air Force Office of Scientific Research Quantum Simulation Multidisciplinary University Research Initiative (MURI); Army Research Office MURI on Atomtronics, M. Rossler; Walter Haefner Foundation; ETH Foundation; Simons Foundation; Austrian Science Fund (FWF) within the SFB FoQuS [F4004-N23]; DK ALM [W1259-N27] FX We thank M. Baranov, F. Schreck, G. Bruun, N. Davidson, and R. Folman for stimulating discussions. Supported by NSF through a grant for ITAMP at Harvard University and the Smithsonian Astrophysical Observatory (R.S.); the Technical University of Munich-Institute for Advanced Study, funded by the German Excellence Initiative and the European Union FP7 under grant agreement 291763 (M.K.); the Harvard-MIT Center for Ultracold Atoms, NSF grant DMR-1308435, the Air Force Office of Scientific Research Quantum Simulation Multidisciplinary University Research Initiative (MURI), the Army Research Office MURI on Atomtronics, M. Rossler, the Walter Haefner Foundation, the ETH Foundation, and the Simons Foundation (E.D.); and the Austrian Science Fund (FWF) within the SFB FoQuS (F4004-N23) and within the DK ALM (W1259-N27). NR 31 TC 10 Z9 10 U1 5 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 7 PY 2016 VL 354 IS 6308 SI SI BP 96 EP 99 DI 10.1126/science.aaf5134 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EC0GT UT WOS:000387777900037 PM 27846498 ER PT J AU Nguyen, TL McCaslin, L McCarthy, MC Stanton, JF AF Thanh Lam Nguyen McCaslin, Laura McCarthy, Michael C. Stanton, John F. TI Communication: Thermal unimolecular decomposition of syn-CH3CHOO: A kinetic study SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CRIEGEE INTERMEDIATE CH2OO; CONFORMER-DEPENDENT REACTIVITY; MASTER EQUATION ANALYSIS; TRANSITION-STATE THEORY; REACTION-RATE CONSTANTS; OH RADICAL PRODUCTS; GAS-PHASE; ABSORPTION-SPECTRUM; CHEMICAL-KINETICS; MULTIPLE-WELL AB The thermal decomposition of syn-ethanal-oxide (syn-CH3CHOO) through vinyl hydrogen peroxide (VHP) leading to hydroxyl radical is characterized using a modification of the HEAT thermochemical protocol. The isomerization step of syn-CH3CHOO to VHP via a 1,4 H-shift, which involves a moderate barrier of 72 kJ/mol, is found to be rate determining. A two-dimensional master equation approach, in combination with semi-classical transition state theory, is employed to calculate the time evolution of various species as well as to obtain phenomenological rate coefficients. This work suggests that, under boundary layer conditions in the atmosphere, thermal unimolecular decomposition is the most important sink of syn-CH3CHOO. Thus, the title reaction should be included into atmospheric modeling. The fate of cold VHP, the intermediate stabilized by collisions with a third body, has also been investigated. Published by AIP Publishing. C1 [Thanh Lam Nguyen; McCaslin, Laura; Stanton, John F.] Univ Texas Austin, Dept Chem, Austin, TX 78712 USA. [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Stanton, JF (reprint author), Univ Texas Austin, Dept Chem, Austin, TX 78712 USA. EM jfstanton@mail.utexas.edu OI Nguyen, Thanh Lam/0000-0002-7794-9439 FU Robert A. Welch Foundation [F-1283]; U.S. Department of Energy, Office of Basic Energy Sciences [DE-FG02-07ER15884]; National Science Foundation [CHE-1058063, CHE-1566266] FX We would like to thank two anonymous reviewers for helpful comments that improved the quality of the paper. J.F.S. and T.L.N. are supported by the Robert A. Welch Foundation (Grant No. F-1283). This material is based on work supported by the U.S. Department of Energy, Office of Basic Energy Sciences under Award No. DE-FG02-07ER15884. M.C.M. is supported by National Science Foundation Grant Nos. CHE-1058063 and CHE-1566266. NR 61 TC 2 Z9 2 U1 20 U2 20 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD OCT 7 PY 2016 VL 145 IS 13 AR 131102 DI 10.1063/1.4964393 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA DZ8XP UT WOS:000386156200003 PM 27782412 ER PT J AU Marx, FG Fordyce, RE AF Marx, Felix G. Fordyce, R. Ewan TI A Link No Longer Missing: New Evidence for the Cetotheriid Affinities of Caperea SO PLOS ONE LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; CETACEA MYSTICETI; BALEEN WHALE; NEW-ZEALAND; PLIOCENE; GENUS; MORPHOLOGY; OLIGOCENE; ANATOMY; FOSSIL AB The origins of the enigmatic pygmy right whale Caperea marginata, the only living member of its subfamily (Neobalaeninae), are an outstanding mystery of cetacean evolution. Its strikingly disparate morphology sets Caperea apart from all other whales, and has turned it into a wildcard taxon that holds the key to understanding modern baleen whale diversity. Morphological cladistics generally ally this species with right whales, whereas molecular analyses consistently cluster it with rorquals and grey whales (Balaenopteroidea). A recent study potentially resolved this conflict by proposing that Caperea belongs with the otherwise extinct Cetotheriidae, but has been strongly criticised on morphological grounds. Evidence from the neobalaenine fossil record could potentially give direct insights into morphological transitions, but is currently limited to just a single species: the Late Miocene Miocaperea pulchra, from Peru. We show that Miocaperea has a highly unusual morphology of the auditory region, resulting from a-presumably feeding-related-strengthening of the articulation of the hyoid apparatus with the skull. This distinctive arrangement is otherwise only found in the extinct Cetotheriidae, which makes Miocaperea a 'missing link" that demonstrates the origin of pygmy right whales from cetotheriids, and confirms the latter's resurrection from the dead. C1 [Marx, Felix G.] Monash Univ, Sch Biol Sci, 25 Rainforest Walk, Clayton, Vic 3800, Australia. [Marx, Felix G.] Museum Victoria, Geosci, Melbourne, Vic, Australia. [Marx, Felix G.] Royal Belgian Inst Nat Sci, Directorate Earth & Hist Life, Brussels, Belgium. [Fordyce, R. Ewan] Univ Otago, Dept Geol, Dunedin, New Zealand. [Fordyce, R. Ewan] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Fordyce, R. Ewan] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Marx, FG (reprint author), Monash Univ, Sch Biol Sci, 25 Rainforest Walk, Clayton, Vic 3800, Australia.; Marx, FG (reprint author), Museum Victoria, Geosci, Melbourne, Vic, Australia.; Marx, FG (reprint author), Royal Belgian Inst Nat Sci, Directorate Earth & Hist Life, Brussels, Belgium. EM felix.marx@monash.edu OI Marx, Felix Georg/0000-0002-1029-4001 FU European Commission [656010] FX This research was supported by a European Commission Horizon 2020 Marie Sklodowska-Curie Global Postdoctoral fellowship to FGM (grant ID 656010). NR 33 TC 0 Z9 0 U1 6 U2 6 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 6 PY 2016 VL 11 IS 10 AR e0164059 DI 10.1371/journal.pone.0164059 PG 26 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DZ2UR UT WOS:000385697600071 PM 27711216 ER PT J AU Ramos-Tafur, GE Lemaitre, R AF Ramos-Tafur, Gabriel E. Lemaitre, Rafael TI A new species of symbiotic palaemonid shrimp of the genus Pseudocoutierea Holthuis, 1951 (Decapoda: Caridea: Palaemonidae) from the eastern Gulf of Mexico, with an updated key for the identification of species of the genus SO ZOOTAXA LA English DT Article DE Gulf of Mexico; Pseudocoutierea stephanieae; new species; Decapoda; Caridea; Palaemonidae AB A new species of symbiotic palaemonid shrimp of the genus Pseudocoutierea Holthuis, 1951, is described based on a specimen collected in the eastern Gulf of Mexico, off the southwest coast of Florida. Pseudocoutierea stephanieae sp. nov., is the seventh known in this genus, and morphologically most similar to P. antillensis Chace, 1972, and P. conchae Criales, 1981, from the western Atlantic, and P. elegans Holthuis, 1952, from the eastern Pacific, all sharing an expanded rostral base or eaves that terminate supra-distally in an acute tooth. This new species can be separated by: the presence of an epigastric knob or tubercle on the anterior mid-dorsal third of the carapace, which is absent in all other congeneric species; the shape of the pterygostomial sinus, which is shallow in this new species, whereas it is deep and well defined in all other congeneric species. An updated dichotomous key to species of Pseudocoutierea is presented. C1 [Ramos-Tafur, Gabriel E.] Univ Florida, Florida Museum Nat Hist, Ichthyol Dept, Dickinson Hall,Newell Dr & Museum Rd,POB 117800, Gainesville, FL 32611 USA. [Ramos-Tafur, Gabriel E.] Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, 100 8th Ave SE, Petersburg, FL 33701 USA. [Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. RP Ramos-Tafur, GE (reprint author), Univ Florida, Florida Museum Nat Hist, Ichthyol Dept, Dickinson Hall,Newell Dr & Museum Rd,POB 117800, Gainesville, FL 32611 USA.; Ramos-Tafur, GE (reprint author), Florida Fish & Wildlife Conservat Commiss, Fish & Wildlife Res Inst, 100 8th Ave SE, Petersburg, FL 33701 USA. EM Gabriel.Ramos@myFWC.com; lemaitrr@si.edu FU U.S. Department of the Interior U.S. Fish and Wildlife Service Federal Sportfish Restoration Grant [F-123] FX We are deeply grateful to: Joan Herrera, Laura Wiggins and Rob Lasley (FWRI), for allowing the study of the specimen and providing information; Tammy Cullings for sorting the crustaceans, and taking photographs of fresh coloration. Thanks are due to other staff of FIM and FWRI, especially Ryan Jones and Chris Stafford for their work during survey cruises, providing information on other organisms collected, and physico-chemical data. Thanks are also extended to: SEAMAP staff on cruises aboard the R/V Tommy Munro; Micah Bakenhaster (Fish and Wildlife Health), kindly loaned GERT his personal Leitz SM-Lux compound microscope and drawing equipment; Ted Switzer for his kind collaboration and providing SEAMAP papers; FIM supervisors Bob McMichael (retired) and Deb Leffler, for GERT to work on this paper; Julianne "Joolz" Knight and Brittany "Bossy" Hall, Fish Feeding Ecology Lab or Gut Lab, for their kind collaboration; Sammy De Grave, Oxford University Museum of Natural History, U.K., and Cedric d'Udekem d'Acoz, Royal Belgian Institute of Natural Sciences, Brussels, Belgium, for providing pertinent literature; Charles H.J.M. Fransen and Gabriel Olthof, from Naturalis Biodiversity Center, The Netherlands, kindly provided comments to an earlier draft of the manuscript. We thank the anonymous reviewers for their comments to improve the manuscript. Funding for this project was provided to GERT by the U.S. Department of the Interior U.S. Fish and Wildlife Service Federal Sportfish Restoration Grant F-123. NR 24 TC 0 Z9 0 U1 2 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 6 PY 2016 VL 4173 IS 5 BP 475 EP 482 DI 10.11646/zootaxa.4173.5.4 PG 8 WC Zoology SC Zoology GA DY6OZ UT WOS:000385248200004 PM 27811822 ER PT J AU Mccallum, AW Cabezas, P Andreakis, N AF Mccallum, Anna W. Cabezas, Patricia Andreakis, Nikos TI Deep-sea squat lobsters of the genus Paramunida Baba, 1988 (Crustacea: Decapoda: Munididae) from north-western Australia: new records and description of three new species SO ZOOTAXA LA English DT Article DE Crustacea; Decapoda; Anomura; Munididae; squat lobster; Paramunida; new species; key; Western Australia; Australia; taxonomy; mitochondrial genes ID GALATHEIDAE; ANOMURA; CHIROSTYLIDAE; PACIFIC; MODELS; GENERA; FIJI AB Six species of Paramunida are reported from the continental margin of north-western Australia. Three species are new to science: Paramunida christinae sp. nov., P. ioannis sp. nov., and P. spiniantennata sp. nov. Two species are reported for the first time from Australian waters, P. evexa Macpherson, 1996 and P. tricarinata (Alcock, 1894). These species were confirmed by molecular evidence from the mitochondrial markers ND1 and 16S. We also examine phylogenetic relationships within the genus, and provide an identification key for all known Paramunida species. C1 [Mccallum, Anna W.] Museum Victoria, GPO Box 666, Melbourne, Vic 3001, Australia. [Cabezas, Patricia] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. [Andreakis, Nikos] Australian Inst Marine Sci, PMB 3, Townsville, Qld 4810, Australia. RP Mccallum, AW (reprint author), Museum Victoria, GPO Box 666, Melbourne, Vic 3001, Australia. EM amccallum@museum.vic.gov.au FU Australian Biological Resources Study (ABRS); National Environmental Research Program (NERP); Australian Government initiative supporting world class, public good research; Commonwealth Department of the Environment; CSIRO "Wealth from Oceans" Flagship FX We are grateful to Joanne Taylor (Museum Victoria) for collection management support, Karen Gowlett-Holmes (CSIRO) for permission to reproduce her colour images of squat lobsters, and the Commonwealth Department of the Environment and the CSIRO "Wealth from Oceans" Flagship for funding for the laboratory components of the "Voyages of Discovery" program. We sincerely thank Enrique Macpherson for examining material from the Museum national d'Histoire Naturelle, Paris, and for his comments on the manuscript. Thanks also to Keiji Baba for his comments on the manuscript. The first author was supported by a Postdoctoral Fellowship from the Australian Biological Resources Study (ABRS). The third author was supported by the National Environmental Research Program (NERP), an Australian Government initiative supporting world class, public good research. The NERP Marine Biodiversity Hub is a collaborative partnership between the University of Tasmania, CSIRO Wealth from Oceans Flagship, Geoscience Australia, Australian Institute of Marine Science, Museum Victoria, Charles Darwin University and the University of Western Australia (www.nerpmarine.edu.au). NR 57 TC 0 Z9 0 U1 3 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 5 PY 2016 VL 4173 IS 3 BP 201 EP 224 DI 10.11646/zootaxa.4173.3.1 PG 24 WC Zoology SC Zoology GA DX6VD UT WOS:000384521300001 PM 27701181 ER PT J AU Jamangape, JA Velazquez-Velazquez, E Martinez-Ramirez, E Anzueto-Calvo, MJ Gomez, EL Dominguez-Cisneros, SE Mcmahan, CD Matamoros, WA AF Jamangape O, Jose A. Velazquez-Velazquez, Ernesto Martinez-Ramirez, Emilio Anzueto-Calvo, Manuel J. Gomez, Eyda L. Dominguez-Cisneros, Sara E. Mcmahan, Caleb D. Matamoros, Wilfredo A. TI Validity and Redescription of Profundulus balsanus Ahl, 1935 (Cyprinodontiformes: Profundulidae) SO ZOOTAXA LA English DT Article DE meristic; fish systematics; taxonomy; southern Mexico; synonyms ID EVOLUTIONARY HISTORY; FISH AB Profundulus balsanus was described by Ahl in 1935 and later placed in synonymy with P. punctatus. Recent molecular studies have demonstrated that specimens identified as P. balsanus belong to a distinct taxon. Herein we used a combination of morphometric, meristic, coloration and osteological data in order to demonstrate the distinctiveness of P. balsanus. Additionally, we used molecular data to reconstruct a phylogeny to place P. balsanus in a systematic context. Profundulus balsanus belongs to the punctatus clade within the genus Profundulus. It can be distinguished from P. oaxacae based on scale count in the lateral line and from P. punctatus based on differences in coloration in the anal fin. We provide a taxonomic key to all Mexican species of Profundulus. C1 [Jamangape O, Jose A.; Dominguez-Cisneros, Sara E.; Matamoros, Wilfredo A.] Univ Ciencias & Artes Chiapas, Inst Ciencias Biol, Colecc Ictiol, Tuxtla Gutierrez 29039, Chiapas, Mexico. [Martinez-Ramirez, Emilio] Inst Politecn Nacl, Unidad Oaxaca, Ctr Interdisciplinario Invest Desarrollo Integral, Area Acuacultura,Dept Invest, Hornos 1003, Oaxaca 71230, Mexico. [Gomez, Eyda L.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Mcmahan, Caleb D.] Field Museum Nat Hist, 1400 S Lake Shore Dr, Chicago, IL 60605 USA. RP Matamoros, WA (reprint author), Univ Ciencias & Artes Chiapas, Inst Ciencias Biol, Colecc Ictiol, Tuxtla Gutierrez 29039, Chiapas, Mexico. EM wilmatamoros@yahoo.com NR 20 TC 0 Z9 0 U1 2 U2 2 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD OCT 3 PY 2016 VL 4173 IS 1 BP 55 EP 65 DI 10.11646/zootaxa.4173.1.5 PG 11 WC Zoology SC Zoology GA DX3PO UT WOS:000384285200005 PM 27701203 ER PT J AU Droege, G Barker, K Seberg, O Coddington, J Benson, E Berendsohn, WG Bunk, B Butler, C Cawsey, EM Deck, J Doring, M Flemons, P Gemeinholzer, B Guntsch, A Hollowell, T Kelbert, P Kostadinov, I Kottmann, R Lawlor, RT Lyal, C Mackenzie-Dodds, J Meyer, C Mulcahy, D Nussbeck, SY O'Tuama, E Orrell, T Petersen, G Robertson, T Sohngen, C Whitacre, J Wieczorek, J Yilmaz, P Zetzsche, H Zhang, Y Zhou, X AF Droege, G. Barker, K. Seberg, O. Coddington, J. Benson, E. Berendsohn, W. G. Bunk, B. Butler, C. Cawsey, E. M. Deck, J. Doring, M. Flemons, P. Gemeinholzer, B. Guentsch, A. Hollowell, T. Kelbert, P. Kostadinov, I. Kottmann, R. Lawlor, R. T. Lyal, C. Mackenzie-Dodds, J. Meyer, C. Mulcahy, D. Nussbeck, S. Y. O'Tuama, E. Orrell, T. Petersen, G. Robertson, T. Soehngen, C. Whitacre, J. Wieczorek, J. Yilmaz, P. Zetzsche, H. Zhang, Y. Zhou, X. TI The Global Genome Biodiversity Network (GGBN) Data Standard specification SO DATABASE-THE JOURNAL OF BIOLOGICAL DATABASES AND CURATION LA English DT Article ID SAMPLE PREANALYTICAL CODE; MINIMUM INFORMATION; BIOSPECIMENS; AMPLIFICATION; PHENOTYPES; GENOTYPES; SEARCH; DBGAP; SPREC; TOOL AB Genomic samples of non-model organisms are becoming increasingly important in a broad range of studies from developmental biology, biodiversity analyses, to conservation. Genomic sample definition, description, quality, voucher information and metadata all need to be digitized and disseminated across scientific communities. This information needs to be concise and consistent in today's ever-increasing bioinformatic era, for complementary data aggregators to easily map databases to one another. In order to facilitate exchange of information on genomic samples and their derived data, the Global Genome Biodiversity Network (GGBN) Data Standard is intended to provide a platform based on a documented agreement to promote the efficient sharing and usage of genomic sample material and associated specimen information in a consistent way. The new data standard presented here build upon existing standards commonly used within the community extending them with the capability to exchange data on tissue, environmental and DNA sample as well as sequences. The GGBN Data Standard will reveal and democratize the hidden contents of biodiversity biobanks, for the convenience of everyone in the wider biobanking community. Technical tools exist for data providers to easily map their databases to the standard. C1 [Droege, G.; Berendsohn, W. G.; Guentsch, A.; Kelbert, P.] Free Univ Berlin, Bot Garden & Bot Museum Berlin Dahlem, Konigin Luise Str 6-8, D-14195 Berlin, Germany. [Barker, K.; Coddington, J.; Butler, C.; Hollowell, T.; Meyer, C.; Mulcahy, D.; Orrell, T.; Whitacre, J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Seberg, O.; Petersen, G.] Univ Copenhagen, Nat Hist Museum Denmark, Solvgade 83, DK-1307 Copenhagen, Denmark. [Benson, E.] Damar Res Scientists, Drum Rd, Cuparmuir KY15 5RJ, Fife, Scotland. [Bunk, B.; Soehngen, C.] Leibniz Inst DSMZ, German Collect Microorganisms & Cell Cultures, Inhoffenstr 7B, D-38124 Braunschweig, Germany. [Cawsey, E. M.] CSIRO Natl Res Collect Australia, Australian Natl Wildlife Collect, Canberra, ACT, Australia. [Deck, J.] Univ Calif Berkeley, Berkeley Nat Hist Museums, Berkeley, CA 94720 USA. [Doring, M.; O'Tuama, E.; Robertson, T.] Global Biodivers Informat Facil Secretariat, Univ PK 15, DK-2100 Copenhagen, Denmark. [Flemons, P.] Australian Museum, Sydney, NSW 2010, Australia. [Gemeinholzer, B.] Univ Giessen, Systemat Bot, D-35392 Giessen, Germany. [Kostadinov, I.] Jacobs Univ Bremen gGmbH, Dept Life Sci & Chem, Campus Ring 1, D-28759 Bremen, Germany. [Kottmann, R.; Yilmaz, P.] Max Planck Inst Marine Microbiol, Microbial Genom & Bioinformat Res Grp, Celsiusstr 1, D-28359 Bremen, Germany. [Lawlor, R. T.] Univ Verona, Dept Pathol & Diagnost, ARC Net Appl Res Canc Ctr, I-37134 Verona, Italy. [Lyal, C.; Mackenzie-Dodds, J.] Nat Hist Museum, Cromwell Rd, London SW7 5BD, England. [Nussbeck, S. Y.] Univ Med Ctr Gottingen, Dept Med Informat, Robert Koch Str 40, D-37075 Gottingen, Germany. [Nussbeck, S. Y.] Univ Med Ctr Gottingen, UMG Biobank, Robert Koch Str 40, D-37075 Gottingen, Germany. [Whitacre, J.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. [Zetzsche, H.] JKI, Fed Res Ctr Cultivated Plants, Inst Resistance Res & Stress Tolerance, Erwin Baur Str 27, D-06484 Quedlinburg, Germany. [Zhang, Y.; Zhou, X.] BGI Shenzhen, China Natl GeneBank, Shenzhen 518083, Guangdong, Peoples R China. RP Droege, G (reprint author), Free Univ Berlin, Bot Garden & Bot Museum Berlin Dahlem, Konigin Luise Str 6-8, D-14195 Berlin, Germany. EM g.droege@bgbm.org RI Petersen, Gitte/H-1903-2011; OI Petersen, Gitte/0000-0002-2325-0059; lawlor, Rita/0000-0003-3160-0634 FU DFG (German Research Foundation); European Commission [312253]; German Research Foundation: DFG-GGBN [GU 1109/5-1, GE 1242/13-1]; DFG-DNA-Bank-Netzwerk [INST 1039/11, INST 17818/11, INST 427/1-1, INST 599/1-1]; DFG-GFBio [GU1109/3-1]; DFG-BiNHum [BE 2283/8-1]; National Museum of Natural History (Smithsonian Institution) Global Genome Initiative FX Funding for open access charge: DFG (German Research Foundation)-funded Open Access Publication Fund of the Freie Universitat Berlin. Project Funding: European Commission: SYNTHESYS III (312253); German Research Foundation: DFG-GGBN (GU 1109/5-1, GE 1242/13-1), DFG-DNA-Bank-Netzwerk (INST 1039/11, INST 17818/11, INST 427/1-1, INST 599/1-1), DFG-GFBio (GU1109/3-1) and DFG-BiNHum (BE 2283/8-1); National Museum of Natural History (Smithsonian Institution) Global Genome Initiative. NR 46 TC 1 Z9 1 U1 12 U2 12 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1758-0463 J9 DATABASE-OXFORD JI Database PD OCT 2 PY 2016 AR baw125 DI 10.1093/database/baw125 PG 11 WC Mathematical & Computational Biology SC Mathematical & Computational Biology GA DY7EC UT WOS:000385291400001 ER PT J AU Bernal, JL Verde, L Riess, AG AF Bernal, Jose Luis Verde, Licia Riess, Adam G. TI The trouble with H-0 SO JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS LA English DT Article DE cosmological parameters from CMBR; cosmological parameters from LSS; dark energytheory ID BARYON ACOUSTIC-OSCILLATIONS; HUBBLE CONSTANT; DARK-MATTER; COSMOLOGICAL PARAMETERS; LOCAL VALUE; PLANCK; DISTANCE; GALAXIES; CONSTRAINTS; RADIATION AB We perform a comprehensive cosmological study of the H-0 tension between the direct local measurement and the model-dependent value inferred from the Cosmic Microwave Background. With the recent measurement of H-0 this tension has raised to more than 3 sigma. We consider changes in the early time physics without modifying the late time cosmology. We also reconstruct the late time expansion history in a model independent way with minimal assumptions using distances measures from Baryon Acoustic Oscillations and Type Ia Supernovae, finding that at z < 0.6 the recovered shape of the expansion history is less than 5% different than that of a standard Lambda CDM model. These probes also provide a model insensitive constraint on the low-redshift standard ruler, measuring directly the combination r(s)h where H-0= h x 100 Mpc(-1) km/s and r(s) is the sound horizon at radiation drag (the standard ruler), traditionally constrained by CMB observations. Thus r(s) and H-0 provide absolute scales for distance measurements (anchors) at opposite ends of the observable Universe. We calibrate the cosmic distance ladder and obtain a model-independent determination of the standard ruler for acoustic scale, r(s). The tension in H-0 reflects a mismatch between our determination of r(s) and its standard, CMB-inferred value. Without including high-l Planck CMB polarization data (i.e., only considering the "recommended baseline" low-l polarisation and temperature and the high l temperature data), a modification of the early-time physics to include a component of dark radiation with an effective number of species around 0.4 would reconcile the CMB-inferred constraints, and the local H-0 and standard ruler determinations. The inclusion of the "preliminary" high-l Planck CMB polarisation data disfavours this solution. C1 [Bernal, Jose Luis; Verde, Licia] Univ Barcelona, IEEC UB, ICC, Marti i Franques 1, E-08028 Barcelona, Spain. [Bernal, Jose Luis] Univ Barcelona, Dept Fis Quant & Astrofis, Marti i Franques 1, E-08028 Barcelona, Spain. [Verde, Licia] ICREA, Pg Lluis Companys 23, Barcelona 08010, Spain. [Verde, Licia] Harvard Univ, Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [Verde, Licia] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Verde, Licia] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. RP Bernal, JL (reprint author), Univ Barcelona, IEEC UB, ICC, Marti i Franques 1, E-08028 Barcelona, Spain.; Bernal, JL (reprint author), Univ Barcelona, Dept Fis Quant & Astrofis, Marti i Franques 1, E-08028 Barcelona, Spain. EM joseluis.bernal@icc.ub.edu; liciaverde@icc.ub.edu; ariess@stsci.edu FU Spanish MINECO [BES-2015-071307]; ESF; Spanish MINECO of ICCUB (Unidad de Excelencia Maria de Maeztu) [AYA2014-58747-P, MDM-2014-0369]; ESA Member States, NASA, and Canada; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX We thank Graeme Addison, Alan Heavens and Antonio J. Cuesta for valuable discussion during the development of this study, which helped to improve this work. JLB is supported by the Spanish MINECO under grant BES-2015-071307, co-funded by the ESF. Funding for this work was partially provided by the Spanish MINECO under projects AYA2014-58747-P and MDM-2014-0369 of ICCUB (Unidad de Excelencia Maria de Maeztu). JLB acknowledges hospitality of Radcliffe Institute for Advanced Study, Harvard University.; Based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 80 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1475-7516 J9 J COSMOL ASTROPART P JI J. Cosmol. Astropart. Phys. PD OCT PY 2016 IS 10 AR 019 DI 10.1088/1475-7516/2016/10/019 PG 27 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA EL4FZ UT WOS:000394578400004 ER PT J AU Nkrumah, EE Vallo, P Klose, SM Ripperger, SP Badu, EK Gloza-Rausch, F Drosten, C Kalko, EKV Tschapka, M Oppong, SK AF Nkrumah, Evans E. Vallo, Peter Klose, Stefan M. Ripperger, Simon P. Badu, Ebenezer K. Gloza-Rausch, Florian Drosten, Christian Kalko, Elisabeth K. V. Tschapka, Marco Oppong, Samuel K. TI Foraging Behavior and Habitat Selection of Noack's Round-Leaf Bat (Hipposideros aff. ruber) and Conservation Implications SO TROPICAL CONSERVATION SCIENCE LA English DT Article DE agro-environment; cocoa farms; fallow lands; seminatural habitats; sub-Saharan Africa ID HOME-RANGE; UTILIZATION DISTRIBUTIONS; INSECTIVOROUS BATS; GEOMETRID MOTHS; EMERGENCE TIME; FOREST; CHIROPTERA; LANDSCAPE; DIVERSITY; ECHOLOCATION AB In sub-Saharan Africa, anthropogenic activities such as cocoa (Theobroma cacao) farming have replaced the natural forest vegetation, making agricultural environments more readily available to some species of bats. To augment bat conservation in such highly modified agro-environments, we evaluated the foraging decisions of the widely distributed Noack's round-leaf bat (Hipposideros aff. ruber) in a Ghanaian agro-environment for two factors: (a) foraging durations and (b) habitat selection from radio telemetry data collected from 13 bats. We hypothesized that it opportunistically selects foraging habitats in proportion to its availability. Our compositional analysis revealed, however, a nonrandom use of habitats. A ranking matrix indicated Hipposideros aff. ruber uses all available habitats but strongly preferred seminatural habitats dominated by fallow lands. Cocoa farms were predominantly used as flight paths for commuting between roosts and other nearby habitats during foraging. We observed a mean foraging duration of 109 min (SD = 62 min) per night for the species. In conclusion, our data suggest that (a) they are flexible in selecting all habitat types in the agro-environment but strongly preferred fallow matrices, (b) the provision of canopy trees within the agro-environment serves as flight paths for commuting from roost to habitats offering higher prey densities, and (3) the maintenance of fallow matrices as conservation units in sub-Saharan agro-environments helps augment conservation efforts of the species. C1 [Nkrumah, Evans E.; Badu, Ebenezer K.; Oppong, Samuel K.] Kwame Nkrumah Univ Sci & Technol, Dept Wildlife & Range Management, Kumasi, Ghana. [Vallo, Peter; Klose, Stefan M.; Ripperger, Simon P.; Kalko, Elisabeth K. V.; Tschapka, Marco] Univ Ulm, Evolutionary Ecol & Conservat Gen, Ulm, Germany. [Vallo, Peter] Acad Sci Czech Republic, Inst Vertebrate Biol, Brno, Czech Republic. [Gloza-Rausch, Florian] Noctalis Ctr Bat Protect & Informat, Bad Segeberg, Germany. [Drosten, Christian] Univ Bonn, Med Ctr, Inst Virol, Bonn, Germany. [Kalko, Elisabeth K. V.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. RP Oppong, SK (reprint author), Kwame Nkrumah Univ Sci & Technol, Dept Wildlife & Range Management, Kumasi, Ghana. EM kobbyoppong@yahoo.com RI Vallo, Peter/F-9650-2014 FU German Research Foundation (DFG) [KA 1241/18-1] FX The author(s) disclosed receipt of the following financial support for the research, authorship, and/or publication of this article: The study was supported with funds from the German Research Foundation (DFG) awarded to E.K.V.K. (KA 1241/18-1). NR 52 TC 0 Z9 0 U1 4 U2 4 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 1940-0829 J9 TROP CONSERV SCI JI Trop. Conserv. Sci. PD OCT-DEC PY 2016 VL 9 IS 4 DI 10.1177/1940082916680428 PG 11 WC Biodiversity Conservation SC Biodiversity & Conservation GA EJ4SS UT WOS:000393207800019 ER PT J AU Songer, M Aung, M Allendorf, TD Calabrese, JM Leimgruber, P AF Songer, Melissa Aung, Myint Allendorf, Teri D. Calabrese, Justin M. Leimgruber, Peter TI Drivers of Change in Myanmar's Wild Elephant Distribution SO TROPICAL CONSERVATION SCIENCE LA English DT Article DE Asian elephants; geographic distribution; Myanmar; habitat loss; deforestation; edge effects ID ASIAN ELEPHANTS; POPULATION-SIZE; FOREST COVER; MAXIMUS; CONSERVATION; BURMA AB Myanmar is considered as a stronghold for wild elephants, though past estimates varied widely from 3,000 to 10,000. Results of a 2004 expert workshop showed estimates between 1,430 and 2,065. Building on surveys from 1990 to 1992, we conducted new expert interviews in townships throughout the range, with questions focusing on numbers of elephants living in townships and threats to and from elephants. We used general linear models to analyze characteristics of townships with and without elephants and to understand factors influencing changes in elephant presence. Our results show a major decrease in the geographic distribution of wild elephants in Myanmar between 1992 and 2006 with deforestation being the major driver. While forest cover is important for elephant presence, continuity with other elephant populations had a stonger influence on elephant persistence between surveys. Fragmentation of elephant populations is also a major driver of decline. Increases in forest cover increased elephant presence, while increases in edge and human population had the reverse effect. Deforestation and fragmentation lead to increased human-elephant conflict in some areas, sometimes concluding with the capture of elephants for timber operations and further draining wild populations. A national elephant action plan that includes monitoring of elephant status and threats is urgently needed and critical for Myanmar's wild elephants, particularly as more than 50 years of political isolation are rapidly ending and pressure on the country's natural resources is increasing exponentially. C1 [Songer, Melissa; Calabrese, Justin M.; Leimgruber, Peter] Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. [Aung, Myint] Friends Wildlife, Yangon, Myanmar. [Allendorf, Teri D.] Univ Wisconsin Madison, Madison, WI USA. RP Songer, M (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM songerm@si.edu FU Friends of the National Zoo FX The author(s) disclosed receipt of the following financial support for the research, authorship, and/or publication of this article: Partial funding for this research was provided by the Friends of the National Zoo. NR 26 TC 0 Z9 0 U1 5 U2 5 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 1940-0829 J9 TROP CONSERV SCI JI Trop. Conserv. Sci. PD OCT-DEC PY 2016 VL 9 IS 4 DI 10.1177/1940082916673749 PG 10 WC Biodiversity Conservation SC Biodiversity & Conservation GA EJ4SS UT WOS:000393207800009 ER PT J AU Suarez-Rubio, M Aung, T Oo, SSL Shwe, NM Hlaing, NM Naing, KM Oo, T Sein, MM Renner, SC AF Suarez-Rubio, Marcela Aung, Thein Oo, Sai Sein Lin Shwe, Nay Myo Hlaing, Nay Myo Naing, Kyaw Myo Oo, Tun Sein, Mie Mie Renner, Swen C. TI Nonbreeding Bird Communities Along an Urban-Rural Gradient of a Tropical City in Central Myanmar SO TROPICAL CONSERVATION SCIENCE LA English DT Article DE bird diversity; Mandalay; point counts; urbanization; Myanmar ID LAND-USE; URBANIZATION; BIODIVERSITY; DIVERSITY; HOMOGENIZATION; RICHNESS; PATTERNS; AVIFAUNA; ANIMALS AB Urbanization is known to be a major driver in abundance and species richness of birds. However, how birds respond to urbanization in tropical cities is understudied in general and entirely absent from Myanmar. We conducted a study in and around Mandalay, a large city in central Myanmar to gather first data on birds and their response to urbanization. We selected four habitats with 10 sampling points each in November 2015. We made 1,536 observations of 68 bird species. The number of species and diversity significantly differed between the four localities. Mandalay Hill and Downtown Mandalay had the lowest number of species and diversity, whereas the University Campus and Paddy Fields had the highest. The highest number of observations was in Downtown Mandalay (1,003 counts) and the lowest on Mandalay Hill (103). Nonmetric multidimensional scaling ordination techniques showed that the four habitat types had significantly different bird species composition. Our results indicate a large effect of urbanization on species diversity, species richness, and species composition of birds. C1 [Suarez-Rubio, Marcela; Renner, Swen C.] Univ Nat Resources & Life Sci, Inst Zool, Vienna, Austria. [Aung, Thein] Wild Wings, Yangon, Myanmar. [Oo, Sai Sein Lin; Hlaing, Nay Myo; Naing, Kyaw Myo; Sein, Mie Mie] Univ Mandalay, Dept Zool, Mandalay, Myanmar. [Shwe, Nay Myo] Fauna & Flora Int, Yangon, Myanmar. [Oo, Tun] Indo Myanmar Conservat, Yangon, Myanmar. [Renner, Swen C.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Renner, SC (reprint author), Univ Nat Resources & Life Sci, Inst Zool, Vienna, Austria. EM swen.renner@boku.ac.at FU Rufford Foundation [17058-1] FX The author(s) disclosed receipt of the following financial support for the research, authorship, and/or publication of this article: The authors thank Rufford Foundation (http://www.rufford.org/) for funding the training workshop (Renner #17058-1). NR 36 TC 0 Z9 0 U1 1 U2 1 PU SAGE PUBLICATIONS INC PI THOUSAND OAKS PA 2455 TELLER RD, THOUSAND OAKS, CA 91320 USA SN 1940-0829 J9 TROP CONSERV SCI JI Trop. Conserv. Sci. PD OCT-DEC PY 2016 VL 9 IS 4 DI 10.1177/1940082916675961 PG 9 WC Biodiversity Conservation SC Biodiversity & Conservation GA EJ4SS UT WOS:000393207800011 ER PT J AU Davenport, JRA Kipping, DM Sasselov, D Matthews, JM Cameron, C AF Davenport, James R. A. Kipping, David M. Sasselov, Dimitar Matthews, Jaymie M. Cameron, Chris TI MOST OBSERVATIONS OF OUR NEAREST NEIGHBOR: FLARES ON PROXIMA CENTAURI SO Astrophysical Journal Letters LA English DT Article DE stars: flare; stars: individual (Proxima Cen); stars: low-mass ID DIGITAL SKY SURVEY; STELLAR ACTIVITY; M-DWARFS; HABITABLE ZONES; COOL STARS; PLANETS; PHOTOMETRY; ASTROMETRY; MISSION; SEARCH AB We present a study of white-light flares from the active M5.5 dwarf Proxima Centauri using the Canadian microsatellite Microvariability and Oscillations of STars. Using 37.6 days of monitoring data from 2014 to 2015, we have detected 66 individual flare events, the largest number of white-light flares observed to date on Proxima Cen. Flare energies in our sample range from 10(29) to 10(31.5) erg. The flare rate is lower than that of other classic flare stars of a similar spectral type, such as UV Ceti, which may indicate Proxima Cen had a higher flare rate in its youth. Proxima Cen does have an unusually high flare rate given its slow rotation period, however. Extending the observed power-law occurrence distribution down to 10(28) erg, we show that flares with flux amplitudes of 0.5% occur 63 times per day, while superflares with energies of 10(33) erg occur similar to 8 times per year. Small flares may therefore pose a great difficulty in searches for transits from the recently announced 1.27M circle plus Proxima b, while frequent large flares could have significant impact on the planetary atmosphere. C1 [Davenport, James R. A.] Western Washington Univ, Dept Phys & Astron, 516 High St, Bellingham, WA 98225 USA. [Kipping, David M.] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Matthews, Jaymie M.] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, 1250 Grand Lake Rd, Sydney, NS B1P 6L2, Canada. RP Davenport, JRA (reprint author), Western Washington Univ, Dept Phys & Astron, 516 High St, Bellingham, WA 98225 USA. OI Davenport, James/0000-0002-0637-835X FU NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1501418] FX The authors thank the anonymous referee for their helpful comments that improved this manuscript. J.R.A.D. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1501418. NR 50 TC 3 Z9 3 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2016 VL 829 IS 2 AR L31 DI 10.3847/2041-8205/829/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EJ7XF UT WOS:000393435300001 ER PT J AU Aliu, E Archambault, S Archer, A Arlen, T Aune, T Barnacka, A Behera, B Beilicke, M Benbow, W Berger, K Bird, R Bottcher, M Bouvier, A Buchovecky, M Buckley, JH Bugaev, V Cardenzana, JV Cerruti, M Cesarini, A Chen, X Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dumm, J Eisch, JD Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hutten, M Hakansson, N Holder, J Hughes, G Humensky, TB Johnson, CA Kaaret, P Kar, P Kelley-Hoskins, N Kertzman, M Khassen, Y Kieda, D Krause, M Krawczynski, H Krennrich, F Lang, MJ Madhavan, AS Maier, G McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Orr, M Otte, AN Pandel, D Park, N Pelassa, V Perkins, JS Pichel, A Pohl, M Popkow, A Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rousselle, J Rovero, AC Saxon, DB Sembroski, GH Shahinyan, K Sheidaei, F Skole, C Smith, AW Staszak, D Telezhinsky, I Theiling, M Todd, NW Tucci, JV Tyler, J Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Weiner, OM Weinstein, A Welsing, R Wilhelm, A Williams, DA Zitzer, B Baring, MG Gonzalez, JB Cillis, AN Horan, D Paneque, D AF Aliu, E. Archambault, S. Archer, A. Arlen, T. Aune, T. Barnacka, A. Behera, B. Beilicke, M. Benbow, W. Berger, K. Bird, R. Bottcher, M. Bouvier, A. Buchovecky, M. Buckley, J. H. Bugaev, V. Cardenzana, J. V. Cerruti, M. Cesarini, A. Chen, X. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dumm, J. Eisch, J. D. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Huetten, M. Hakansson, N. Holder, J. Hughes, G. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kelley-Hoskins, N. Kertzman, M. Khassen, Y. Kieda, D. Krause, M. Krawczynski, H. Krennrich, F. Lang, M. J. Madhavan, A. S. Maier, G. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Pandel, D. Park, N. Pelassa, V. Perkins, J. S. Pichel, A. Pohl, M. Popkow, A. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rousselle, J. Rovero, A. C. Saxon, D. B. Sembroski, G. H. Shahinyan, K. Sheidaei, F. Skole, C. Smith, A. W. Staszak, D. Telezhinsky, I. Theiling, M. Todd, N. W. Tucci, J. V. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Weiner, O. M. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Zitzer, B. Baring, M. G. Gonzalez, J. Becerra Cillis, A. N. Horan, D. Paneque, D. CA Veritas Collaboration TI Very high energy outburst of Markarian 501 in May 2009 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE BL Lacertae objects: individual: Mrk 501; gamma rays: galaxies ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; GAMMA-RAY EMISSION; OPTICAL POLARIZATION PROPERTIES; EXTRAGALACTIC RADIO-SOURCES; ACTIVE GALACTIC NUCLEI; X-RAY; MULTIWAVELENGTH OBSERVATIONS; SPECTRAL VARIABILITY; INTERNAL SHOCKS AB The very high energy (VHE; E > 100 GeV) blazar Markarian 501 was observed between April 17 and May 5 (MJD 54 938-54 956), 2009, as part of an extensive multiwavelength campaign from radio to VHE. Strong VHE yray activity was detected on May 1st with Whipple and VERITAS, when the flux (E > 400 GeV) increased to 10 times the preflare baseline flux (3.9 x 10(-11) ph cm(-2) s(-1)), reaching five times the flux of the Crab Nebula. This coincided with a decrease in the optical polarization and a rotation of the polarization angle by 15. This VHE flare showed a fast flux variation with an increase of a factor similar to 4 in 25 min, and a falling time of similar to 50 min. We present the observations of the quiescent state previous to the flare and of the high state after the flare, focusing on the flux and spectral variability from Whipple, VERITAS, Fermi-LAT, RXTE, and Swift combined with optical and radio data. C1 [Aliu, E.; Mukherjee, R.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; McCann, A.; Ragan, K.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Krawczynski, H.; Todd, N. W.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Arlen, T.; Aune, T.; Buchovecky, M.; Ong, R. A.; Popkow, A.; Rousselle, J.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Behera, B.; Chen, X.; Federici, S.; Fleischhack, H.; Huetten, M.; Hughes, G.; Kelley-Hoskins, N.; Krause, M.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, Platanenallee 6, D-15738 Zeuthen, Germany. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Pelassa, V.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Collins-Hughes, E.; Khassen, Y.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bottcher, M.] North West Univ, Ctr Space Res, Private Bag X6001, ZA-2520 Potchefstroom, South Africa. [Bouvier, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Cardenzana, J. V.; Eisch, J. D.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland. [Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; McArthur, S.; Sembroski, G. H.; Theiling, M.; Tucci, J. V.; Varlotta, A.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Furniss, A.] Calif State Univ East Bay, Dept Phys, Hayward, CA 94542 USA. [Gall, D.; Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA. [Humensky, T. B.; Nieto, D.; Weiner, O. M.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kar, P.; Kieda, D.; Sheidaei, F.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Meagher, K.; Otte, A. N.] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, 1100 East 5th St, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin Rd, Galway, Ireland. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Park, N.; Staszak, D.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Perkins, J. S.; Gonzalez, J. Becerra; Cillis, A. N.] NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. [Pichel, A.; Rovero, A. C.; Cillis, A. N.] Inst Astron & Fis Espacio, Casilla Correo 67,Sucursal 28,C1428ZAA, Buenos Aires, DF, Argentina. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Phys Sci, Cork, Ireland. [Smith, A. W.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Zitzer, B.] Univ Maryland, College Pk, MD 20742 USA. [Zitzer, B.] NASA, GSFC, College Pk, MD 20742 USA. [Baring, M. G.] Rice Univ, Dept Phys & Astron, POB 1892, Houston, TX 77251 USA. [Gonzalez, J. Becerra] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Gonzalez, J. Becerra] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Paneque, D.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Paneque, D.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. RP Pichel, A (reprint author), Inst Astron & Fis Espacio, Casilla Correo 67,Sucursal 28,C1428ZAA, Buenos Aires, DF, Argentina. EM anapichel@iafe.uba.ar OI Pandel, Dirk/0000-0003-2085-5586; Krause, Maria/0000-0001-7595-0914 FU US Department of Energy Office of Science; US National Science Foundation; Smithsonian Institution; NSERC in Canada; South African Research Chairs Initiative (SARChI) by National Research Foundation; Department of Science and Technology of South Africa FX This research is supported by grants from the US Department of Energy Office of Science, the US National Science Foundation and the Smithsonian Institution, and by NSERC in Canada. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. The VERITAS Collaboration is grateful to Trevor Weekes for his seminal contributions and leadership in the field of VHE gamma-ray astrophysics, which made this study possible. The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the National Space Board in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. M.B. acknowledges support through the South African Research Chairs Initiative (SARChI) by the National Research Foundation and the Department of Science and Technology of South Africa. NR 86 TC 0 Z9 0 U1 2 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A76 DI 10.1051/0004-6361/201628744 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200085 ER PT J AU Alvarado-Gomez, JD Hussain, GAJ Cohen, O Drake, JJ Garraffo, C Grunhut, J Gombosi, TI AF Alvarado-Gomez, J. D. Hussain, G. A. J. Cohen, O. Drake, J. J. Garraffo, C. Grunhut, J. Gombosi, T. I. TI Simulating the environment around planet-hosting stars II. Stellar winds and inner astrospheres SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: winds, outflows; stars: mass-loss; stars: magnetic field; stars: late-type; magnetohydrodynamics (MHD) ID LOCAL INTERSTELLAR-MEDIUM; SOLAR-LIKE STARS; ANGULAR-MOMENTUM EVOLUTION; MAIN-SEQUENCE STARS; X-RAY-EMISSION; CORONAL MASS EJECTIONS; EARTH-LIKE EXOPLANETS; MHZ RADIO-EMISSION; IN HABITABLE ZONES; SUN-LIKE STARS AB We present the results of a comprehensive numerical simulation of the environment around three exoplanet-host stars (HD 1237, HD22049, and HD147513). Our simulations consider one of the latest models currently used for space weather studies in the Heliosphere, with turbulent Alfven wave dissipation as the source of coronal heating and stellar wind acceleration. Large-scale magnetic field maps, recovered with two implementations of the tomographic technique of Zeeman-Doppler imaging, serve to drive steady-state solutions in each system. This paper contains the description of the stellar wind and inner astrosphere, while the coronal structure was discussed in a previous paper. The analysis includes the magneto-hydrodynamical properties of the stellar wind, the associated mass and angular momentum loss rates, as well as the topology of the astrospheric current sheet in each system. A systematic comparison among the considered cases is performed, including two reference solar simulations covering activity minimum and maximum. For HD1237, we investigate the interactions between the structure of the developed stellar wind, and a possible magnetosphere around the Jupiter-mass planet in this system. We find that the process of particle injection into the planetary atmosphere is dominated by the density distribution rather than the velocity profile of the stellar wind. In this context, we predict a maximum exoplanetary radio emission of 12 mJy at 40 MHz in this system, assuming the crossing of a high-density streamer during periastron passage. Furthermore, in combination with the analysis performed in the first paper of this study, we obtain for the first time a fully simulated mass loss-activity relation. This relation is compared and discussed in the context of the previously proposed observational counterpart, derived from astrospheric detections. Finally, we provide a characterisation of the global 3D properties of the stellar wind of these systems, at the inner edges of their habitable zones. C1 [Alvarado-Gomez, J. D.; Hussain, G. A. J.; Grunhut, J.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Alvarado-Gomez, J. D.] Univ Munich, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. [Hussain, G. A. J.] Univ Toulouse, Inst Rech Astrophys & Planetol, UPS OMP, F-31400 Toulouse, France. [Cohen, O.; Drake, J. J.; Garraffo, C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, 2455 Hayward St, Ann Arbor, MI 48109 USA. RP Alvarado-Gomez, JD (reprint author), European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany.; Alvarado-Gomez, JD (reprint author), Univ Munich, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. EM jalvarad@eso.org RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Alvarado Gomez, Julian David/0000-0001-5052-3473; Cohen, Ofer/0000-0003-3721-0215 FU DFG Cluster of Excellence "Origin and Structure of the Universe" FX We would like to thank the referee for their constructive comments which helped to improve the quality of this paper. This work was carried out using the SWMF/BATSRUS tools developed at The University of Michigan Center for Space Environment Modeling (CSEM) and made available through the NASA Community Coordinated Modeling Center (CCMC). We acknowledge the support by the DFG Cluster of Excellence "Origin and Structure of the Universe". We are grateful for the support by A. Krukau through the Computational Center for Particle and Astrophysics (C2PAP). NR 135 TC 2 Z9 2 U1 2 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A95 DI 10.1051/0004-6361/201628988 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200106 ER PT J AU McGuire, C Fuller, GA Peretto, N Zhang, Q Traficante, A Avison, A Jimenez-Serra, I AF McGuire, C. Fuller, G. A. Peretto, N. Zhang, Q. Traficante, A. Avison, A. Jimenez-Serra, I. TI The structure and early evolution of massive star forming regions Substructure in the infrared dark cloud SDC13 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: clouds; stars: massive; stars: protostars ID HIERARCHICAL FRAGMENTATION; PROTOSTELLAR CANDIDATES; STELLAR EVOLUTION; MOLECULAR CLOUDS; DUST CONTINUUM; CO OUTFLOWS; CYGNUS-X; CORES; PROTOSTARS; EMISSION AB Context. Investigations into the substructure of massive star forming regions are essential for understanding the observed relationships between core mass distributions and mass distributions in stellar clusters, differentiating between proposed mechanisms of massive star formation. Aims. We study the substructure in the two largest fragments (i.e. cores) MM1 and MM2, in the infrared dark cloud complex SDC13. As MM1 appears to be in a later stage of evolution than MM2, comparing their substructure provides an insight in to the early evolution of massive clumps. Methods. We report the results of high resolution SMA dust continuum observations towards MM1 and MM2. Combining these data with Herschel observations, we carry out RADMC-3D radiative transfer modelling to characterise the observed substructure. Results. SMA continuum data indicates 4 sub-fragments in the SDC13 region. The nature of the second brightest sub-fragment (B) is uncertain as it does not appear as prominent at the lower MAMBO resolution or at radio wavelengths. Statistical analysis indicates that it is unlikely to be a background source, an AGB star, or the free-free emission of a HII region. It is plausible that B is a runaway object ejected from MM1. MM1, which is actively forming stars, consists of two sub-fragments A and C. This is confirmed by 70 mu m Herschel data. While MM1 and MM2 appear quite similar in previous low resolution observations, at high resolution, the sub-fragment at the centre of MM2 (D) is much fainter than sub-fragment at the centre of MM1 (A). RADMC-3D models of MM1 and MM2 are able to reproduce these results, modelling MM2 with a steeper density profile and higher mass than is required for MM1. The relatively steep density profile of MM2 depends on a significant temperature decrease in its centre, justified by the lack of star formation in MM2. A final stellar population for MM1 was extrapolated, indicating a star formation efficiency typical of regions of core and cluster formation. Conclusions. The proximity of MM1 and MM2 suggests they were formed at the similar times, however, despite having a larger mass and steeper density profile, the absence of stars in MM2 indicates that it is in an earlier stage of evolution than MM1. This suggests that the density profiles of such cores become shallower as they start to form stars and that evolutionary timescales are not solely dependent on initial mass. Some studies also indicate that the steep density profile of MM2 makes it more likely to form a single massive central object, highlighting the importance of the initial density profile in determining the fragmentation behaviour in massive star forming regions. C1 [McGuire, C.; Fuller, G. A.; Traficante, A.; Avison, A.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. [Fuller, G. A.; Avison, A.] Univ Manchester, UK ALMA Reg Ctr Node, Manchester M13 9PL, Lancs, England. [Peretto, N.] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Jimenez-Serra, I.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. RP McGuire, C (reprint author), Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. EM catherine.mcguire@postgrad.manchester.ac.uk; Nicolas.Peretto@astro.cf.ac.uk OI Zhang, Qizhou/0000-0003-2384-6589 NR 74 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A118 DI 10.1051/0004-6361/201527062 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200029 ER PT J AU Polito, V Del Zanna, G Dudik, J Mason, HE Giunta, A Reeves, KK AF Polito, V. Del Zanna, G. Dudik, J. Mason, H. E. Giunta, A. Reeves, K. K. TI Density diagnostics derived from the O IV and S IV intercombination lines observed by IRIS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: transition region; Sun: UV radiation; techniques: spectroscopic; atomic data ID SOLAR ACTIVE REGIONS; BORON-LIKE IONS; ELECTRON-IMPACT EXCITATION; IONIZATION EQUILIBRIUM; DIELECTRONIC RECOMBINATION; NONEQUILIBRIUM IONIZATION; ENERGY-LEVELS; ATOMIC DATA; N-III; TRANSITION REGION AB The intensity of the O IV 2s(2) 2p P-2-2s2p(2) P-4 and S IV 3 s(2) 3p P-2-3s 3p(2) (4) P intercombination lines around 1400 angstrom observed with the Interface Region Imaging Spectrograph (IRIS) provide a useful tool to diagnose the electron number density (N-e) in the solar transition region plasma. We measure the electron number density in a variety of solar features observed by IRIS, including an active region (AR) loop, plage and brightening, and the ribbon of the 22-June-2015 M 6.5 class flare. By using the emissivity ratios of O IV and S IVv lines, we find that our observations are consistent with the emitting plasma being near isothermal (logT[K] approximate to 5) and iso-density (N-e approximate to 10(10.6) cm(-3)) in the AR loop. Moreover, high electron number densities (N-e approximate to 10(13) cm(-3)) are obtained during the impulsive phase of the flare by using the S IV line ratio. We note that the S IV lines provide a higher range of density sensitivity than the O IV lines. Finally, we investigate the effects of high densities (N-e greater than or similar to 10(11) cm(-3)) on the ionization balance. In particular, the fractional ion abundances are found to be shifted towards lower temperatures for high densities compared to the low density case. We also explored the effects of a non-Maxwellian electron distribution on our diagnostic method. C1 [Polito, V.; Del Zanna, G.; Mason, H. E.] Univ Cambridge, CMS, Dept Appl Math & Theoret Phys, Wilberforce Rd, Cambridge CB3 0WA, England. [Dudik, J.] Acad Sci Czech Republic, Astron Inst, Ondrejov 25165, Czech Republic. [Giunta, A.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 01238 USA. RP Polito, V (reprint author), Univ Cambridge, CMS, Dept Appl Math & Theoret Phys, Wilberforce Rd, Cambridge CB3 0WA, England. EM vp323@cam.ac.uk FU Isaac Newton Studentship; Cambridge Trust; IRIS team at Harvard Smithsonian Centre for Astrophysics; RS Newton Alumni Programme; STFC; Grant Agency of the Czech Republic [P209/12/1652]; Science and Technology Facilities Council; Lockheed-Martin [8100002705]; Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract FX We thank the referee for the useful suggestions which helped improving the manuscript. V.P. acknowledges support from the Isaac Newton Studentship, the Cambridge Trust, the IRIS team at Harvard Smithsonian Centre for Astrophysics and the RS Newton Alumni Programme. G.D.Z. and H.E.M. acknowledge support from the STFC and the RS Newton Alumni Programme. J.D. acknowledges support from the RS Newton Alumni Programme. J.D. also acknowledges support from the Grant No. P209/12/1652 of the Grant Agency of the Czech Republic. A.G. acknowledges the in house research support provided by the Science and Technology Facilities Council. K.R. is supported by contract 8100002705 from Lockheed-Martin to SAO. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research Center and major contributions to downlink communications funded by the Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract. AIA data are courtesy of NASA/SDO and the respective science teams. CHIANTI is a collaborative project involving researchers at the universities of Cambridge (UK), George Mason and Michigan (USA). ADAS is a project managed at the University of Strathclyde (UK) and funded through memberships universities and astrophysics and fusion laboratories in Europe and worldwide. NR 77 TC 0 Z9 0 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2016 VL 594 AR A64 DI 10.1051/0004-6361/201628965 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ4MG UT WOS:000385832200103 ER PT J AU Gostel, MR Weeks, A Raharimampionona, J Phillipson, PB AF Gostel, Morgan R. Weeks, Andrea Raharimampionona, Jeannie Phillipson, Peter B. TI A Partial Taxonomic Revision of the Rhynchocarpa Clade of Commiphora (Burseraceae) Endemic to Madagascar SO SYSTEMATIC BOTANY LA English DT Article DE IUCN Red List; Malagasy biodiversity; morphology; new species; stellate pubescence; taxonomy ID CONSERVATION; RADIATIONS; GENUS AB Recent molecular phylogenetic studies of Commiphora (Burseraceae) have revealed a complex history of species evolution in this genus, which includes four separate invasions of Madagascar. Two of these invasions have resulted in radiations of species that are not well-characterized taxonomically due in part to a lack of sufficient herbarium collections. Recent work has also revealed that morphological characters that have been used historically to circumscribe species of this genus have proven insufficient for distinguishing the closely related Malagasy species of these radiations. In this study we present a partial taxonomic revision for the most species-rich of these clades, the 'Rhynchocarpa' clade, which contains at least 26 species united by numerous molecular synapomorphies yet lack a shared, derived suite of morphological traits. Here, we revise seven 'Rhynchocarpa' species that are united by the presence of stellate pubescence on vegetative and reproductive parts of the plant, a trait that is uncommon in the genus and a practical metric for limiting the scope of the revisionary work. We include five new species, including four new names (Commiphora andranovoryensis, Commiphora elliptica, Commiphora morondavensis, and Commiphora razakamalalae) and a name currently in use, correctly published (Commiphora falcata). We provide morphological descriptions, distributional information, and conservation assessments for these as well as Commiphora aprevalii and Commiphora stellulata. We designate a lectotype for Commiphora stellulata. A key to the seven species is included. We envision this contribution as the first in a series of clade-based revisions that clarify the taxonomy of Malagasy Commiphora. C1 [Gostel, Morgan R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. [Weeks, Andrea] George Mason Univ, Dept Biol, 4400 Univ Dr,MSN 3E1, Fairfax, VA 22030 USA. [Weeks, Andrea] George Mason Univ, Ted R Bradley Herbarium, 4400 Univ Dr,MSN 3E1, Fairfax, VA 22030 USA. [Raharimampionona, Jeannie] Missouri Bot Garden, BP 3391, Antananarivo 101, Madagascar. [Phillipson, Peter B.] Missouri Bot Garden, POB 299, St Louis, MO 63166 USA. [Phillipson, Peter B.] Sorbonne Univ, Inst Systemat Evolut & Biodiversite, Museum Natl Hist Nat, UMR 7205,Univ Pierre & Marie Curie,CNRS, CP 39,57 Rue Cuvier, F-75231 Paris 05, France. RP Gostel, MR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM gostelm@si.edu FU National Science Foundation [DEB 0919179]; Thomas and Kate Jeffress Memorial Foundation; American Society for Plant Taxonomists FX We thank the curators of MO, P, TAN, and TEF for access to collections either by loans or visits; Porter P. Lowry II (MBG), Richard Razakamalala (MBG-Madagascar), Charles Rakotavao (MBG-Madagascar), Christian Camara (MBG-Madagascar), Jackie Andriantiana (TAN) and Hanta Razafindrabe (TAN) for assistance with fieldwork and organizational planning; and Zachary Rogers (MBG) for generous assistance with herbarium material including specimen gifts. Douglas Daly and an anonymous reviewer provided constructive feedback on earlier versions of this manuscript. We also thank the Parc Botanique et Zoologique de Tsimbazaza and the rest of the MBG staff in Antananarivo for their assistance. We express our gratitude to Bobbi Angell for providing richly detailed illustrations of the species newly described in this article. Additional thanks to Jasper Nijdam and the Georgetown University GNuLab for access to and assistance with scanning electron microscopy. This work was funded partially by the National Science Foundation (DEB 0919179), the Thomas and Kate Jeffress Memorial Foundation (AW) and a graduate research grant from the American Society for Plant Taxonomists (MRG). NR 15 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 2016 VL 41 IS 4 BP 1004 EP 1019 DI 10.1600/036364416X694134 PG 16 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA EH4HQ UT WOS:000391732700022 ER PT J AU Stine, JK AF Stine, Jeffrey K. TI Bulldozer: Demolition and Clearance of the Postwar Landscape SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 [Stine, Jeffrey K.] Smithsonian Inst, Natl Museum Amer Hist, Environm Hist, Washington, DC 20560 USA. RP Stine, JK (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Environm Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0007-6805 EI 2044-768X J9 BUS HIST REV JI Bus. Hist. Rev. PD OCT PY 2016 VL 90 IS 3 SI SI BP 603 EP 605 DI 10.1017/S0007680516000969 PG 4 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA EG8ED UT WOS:000391287800029 ER PT J AU Daemmrich, A AF Daemmrich, Arthur TI The Lock and Key of Medicine: Monoclonal Antibodies and the Transformation of Healthcare SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 [Daemmrich, Arthur] Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. RP Daemmrich, A (reprint author), Smithsonian Inst, Lemelson Ctr Study Invent & Innovat, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0007-6805 EI 2044-768X J9 BUS HIST REV JI Bus. Hist. Rev. PD OCT PY 2016 VL 90 IS 3 SI SI BP 615 EP 617 DI 10.1017/S000768051600101X PG 4 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA EG8ED UT WOS:000391287800034 ER PT J AU Franse, J Bulbul, E Foster, A Boyarsky, A Markevitch, M Bautz, M Iakubovskyi, D Loewenstein, M McDonald, M Miller, E Randall, SW Ruchayskiy, O Smith, RK AF Franse, Jeroen Bulbul, Esra Foster, Adam Boyarsky, Alexey Markevitch, Maxim Bautz, Mark Iakubovskyi, Dmytro Loewenstein, Mike McDonald, Michael Miller, Eric Randall, Scott W. Ruchayskiy, Oleg Smith, Randall K. TI RADIAL PROFILE OF THE 3.5 keV LINE OUT TO R-200 IN THE PERSEUS CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; elementary particles; galaxies: clusters: individual (Perseus Cluster); line: identification; X-rays: galaxies: clusters ID X-RAY-EMISSION; DARK-MATTER; GALAXY CLUSTERS; GALACTIC-CENTER; SUZAKU; SPECTROSCOPY; CONSTRAINTS; COSMOLOGY; FILAMENTS; SPECTRA AB The recent discovery of the unidentified emission line at 3.5 keV in galaxies and clusters has attracted great interest from the community. As the origin of the line remains uncertain, we study the surface brightness distribution of the line in the Perseus cluster since that information can be used to identify its origin. We examine the flux distribution of the 3.5 keV line in the deep Suzaku observations of the Perseus cluster in detail. The 3.5 keV line is observed in three concentric annuli in the central observations, although the observations of the outskirts of the cluster did not reveal such a signal. We establish that these detections and the upper limits from the non-detections are consistent with a dark matter decay origin. However, absence of positive detection in the outskirts is also consistent with some unknown astrophysical origin of the line in the dense gas of the Perseus core, as well as with a dark matter origin with a steeper dependence on mass than the dark matter decay. We also comment on several recently published analyses of the 3.5 keV line. C1 [Franse, Jeroen] Leiden Univ, Leiden Observ, Niels Bohrweg 2, Leiden, Netherlands. [Franse, Jeroen; Boyarsky, Alexey] Leiden Univ, Inst Lorentz Theoret Phys, Niels Bohrweg 2, Leiden, Netherlands. [Bulbul, Esra; Bautz, Mark; McDonald, Michael; Miller, Eric] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Foster, Adam; Randall, Scott W.; Smith, Randall K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Markevitch, Maxim] NASA, Goddard Space Flight Ctr, 880 Greenbelt Rd, Greenbelt, MD 20771 USA. [Iakubovskyi, Dmytro; Ruchayskiy, Oleg] Niels Bohr Inst, Discovery Ctr, Blegdamsvej 17, Copenhagen, Denmark. [Iakubovskyi, Dmytro] Bogolyubov Inst Theoret Phys, Str 14-b, UA-03680 Kiev, Ukraine. [Loewenstein, Mike] NASA, CRESST, Greenbelt, MD 20771 USA. [Loewenstein, Mike] NASA, Xray Astrophys Lab, GSFC, Greenbelt, MD 20771 USA. [Loewenstein, Mike] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Franse, J (reprint author), Leiden Univ, Leiden Observ, Niels Bohrweg 2, Leiden, Netherlands.; Franse, J (reprint author), Leiden Univ, Inst Lorentz Theoret Phys, Niels Bohrweg 2, Leiden, Netherlands. FU De Sitter program at Leiden University; NWO; NASA [NNX14AF78G, NNX123AE77G, NNX15AE16G]; VILLUM FONDEN FX The authors thank Ondrej Urban for kindly sharing with us the coordinates of point sources detected in the Suzaku field-of-view; Larry David, Stefano Ettori, and Felipe Andrade-Santos for providing useful suggestions. The work of J.F. was supported by the De Sitter program at Leiden University with funds from NWO. This research is part of the Fundamentals of Science program at Leiden University. E.B. acknowledges support by NASA through contracts NNX14AF78G and NNX123AE77G. The work of R.S. was funded in part by NASA Grant NNX15AE16G. The work of D.I. was supported by a research grant from VILLUM FONDEN. NR 48 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 124 DI 10.3847/0004-637X/829/2/124 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EF7BI UT WOS:000390484700004 ER PT J AU Brounce, M Kelley, KA Stern, R Martinez, F Cottrell, E AF Brounce, Maryjo Kelley, Katherine A. Stern, Robert Martinez, Fernando Cottrell, Elizabeth TI The Fina Nagu volcanic complex: Unusual submarine arc volcanism in the rapidly deforming southern Mariana margin SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article ID OXIDATION-STATE; OXYGEN FUGACITY; SUBDUCTION ZONES; UPPER-MANTLE; ISLAND-ARC; MAGMAS; BASALTS; TROUGH; WATER; DIFFERENTIATION AB In the Mariana convergent margin, large arc volcanoes disappear south of Guam even though the Pacific plate continues to subduct and instead, small cones scatter on the seafloor. These small cones could form either due to decompression melting accompanying back-arc extension or flux melting, as expected for arc volcanoes, or as a result of both processes. Here, we report the major, trace, and volatile element compositions, as well as the oxidation state of Fe, in recently dredged, fresh pillow lavas from the Fina Nagu volcanic chain, an unusual alignment of small, closely spaced submarine calderas and cones southwest of Guam. We show that Fina Nagu magmas are the consequence of mantle melting due to infiltrating aqueous fluids and sediment melts sourced from the subducting Pacific plate into a depleted mantle wedge, similar in extent of melting to accepted models for arc melts. Fina Nagu magmas are not as oxidized as magmas elsewhere along the Mariana arc, suggesting that the subduction component responsible for producing arc magmas is either different or not present in the zone of melt generation for Fina Nagu, and that amphibole or serpentine mineral destabilization reactions are key in producing oxidized arc magmas. Individual Fina Nagu volcanic structures are smaller in volume than Mariana arc volcanoes, although the estimated cumulative volume of the volcanic chain is similar to nearby submarine arc volcanoes. We conclude that melt generation under the Fina Nagu chain occurs by similar mechanisms as under Mariana arc volcanoes, but that complex lithospheric deformation in the region distributes the melts among several small edifices that get younger to the northeast. C1 [Brounce, Maryjo] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Brounce, Maryjo] Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. [Kelley, Katherine A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. [Stern, Robert] Univ Texas Dallas, Dept Geosci, Richardson, TX 75083 USA. [Martinez, Fernando] Univ Hawaii Manoa, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Cottrell, Elizabeth] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Brounce, M (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA.; Brounce, M (reprint author), Univ Calif Riverside, Dept Earth Sci, Riverside, CA 92521 USA. EM mbrounce@ucr.edu FU US Department of Energy [DE-AC02-98CH10886]; NSF [OCE-0961811, OCE-0961559, EAR-1258940, EAR-0841006, OCE-0961352] FX We would like to thank Frances Jenner and two anonymous reviewers for their careful attention to our paper. We would like to thank the captain and crew aboard the Thomas G. Thompson during expedition TN273, and aboard the NOAA vessel Okeanos Explorer and ROV Deep Discoverer during expedition EX1605L1. We thank M. Lytle, B. Covellone, J. Ribeiro, W. Lieu, and E. Jordan for leadership and assistance during dredging operations for TN273. We thank A. Lanzirotti, W. Rao, and S. Wirick for assistance in beamline operations at NSLS BNL. Access to NSLS BNL was supported by the US Department of Energy under contract DE-AC02-98CH10886. We acknowledge support from NSF grant OCE-0961811 to Martinez, NSF OCE-0961559 and NSF EAR-1258940 to Kelley, NSF EAR-0841006 to Cottrell, and NSF OCE-0961352 to Stern. NSF OCE-1258771 provides curatorial support for marine geological samples at the University of Rhode Island. Supporting data are included as data tables in a supporting information file. Additional information may be obtained from the first author at mbrounce@ucr.edu. NR 61 TC 0 Z9 0 U1 3 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD OCT PY 2016 VL 17 IS 10 BP 4078 EP 4091 DI 10.1002/2016GC006457 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA ED2QZ UT WOS:000388694600015 ER PT J AU Correa-Metrio, A Velez, MI Escobar, J St-Jacques, JM Lopez-Perez, M Curtis, J Cosford, J AF Correa-Metrio, Alexander Velez, Maria I. Escobar, Jaime St-Jacques, Jeannine-Marie Lopez-Perez, Minerva Curtis, Jason Cosford, Jason TI Mid-elevation ecosystems of Panama: future uncertainties in light of past global climatic variability SO JOURNAL OF QUATERNARY SCIENCE LA English DT Article DE biodiversity; climate change; Little Ice Age; Medieval Climate Anomaly; precipitation seasonality ID ICE-AGE; CENTRAL-AMERICA; HOLOCENE; OSCILLATION; PERSPECTIVE; VEGETATION; LOWLANDS; VELOCITY; DROUGHT; HISTORY AB Modern changes in regional climates will result in high ecosystem turnover and substantial biodiversity rearrangements. Understanding these changes requires palaeoecological studies at temporal resolutions comparable to the time window at which modern climate change is occurring. Here we present a multi-proxy, high-resolution record of forest and lake ecosystem change that occurred during the last 1100 years at middle elevations in Panama. From similar to 900 to 1400 CE, regional forest and lake ecosystems were characterized by high seasonality, probably associated with both high El Nino activity and higher global temperatures. At similar to 1400 CE, an abrupt transition marked the decoupling of forest and lake responses, with forest responding mostly to local patterns of human occupation, and lake trophic status being controlled mostly by the regional precipitation-evaporation balance, possibly associated with solar irradiance. Factors that played important roles in shaping regional ecosystems during the last 1100 years will probably again play critical roles within the coming decades, i.e. higher precipitation seasonality and higher temperatures. Past responses of the system, together with pervasive human activities, suggest that future conditions will simplify mid-elevation forests. Given the importance of these geographical locations as hotspots of biological diversity, substantial losses of global biodiversity are foreseen. Copyright (C) 2016 John Wiley & Sons, Ltd. C1 [Correa-Metrio, Alexander] Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04510, DF, Mexico. [Velez, Maria I.; Cosford, Jason] Univ Regina, Dept Geol, Regina, SK S4S 7H9, Canada. [Escobar, Jaime] Univ Norte, Dept Ingn Civil & Ambiental, Barranquilla, Colombia. [Escobar, Jaime] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Box 0843-03092, Balboa, Panama. [St-Jacques, Jeannine-Marie] Univ Regina, Prairie Adaptat Res Collaborat, Regina, SK S4S 0A2, Canada. [Lopez-Perez, Minerva] Univ Nacl Autonoma Mexico, Posgrad Ciencias Biol, Mexico City 04510, DF, Mexico. [Curtis, Jason] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. RP Correa-Metrio, A (reprint author), Univ Nacl Autonoma Mexico, Inst Geol, Mexico City 04510, DF, Mexico. EM acorrea@geologia.unam.mx FU Inter-American Institute for Global Change Research (IAI) [CRN3038]; US National Science Foundation [GEO-1128040]; University of Regina FX We thank the community of San Carlos for granting us access to the lake. We thank C. Jaramillo from Smithsonian Tropical Research Institute for facilitating field logistics. We are grateful to W. Gosling and two anonymous reviewers for constructive discussion on the original manuscript. Financial support came from the Inter-American Institute for Global Change Research (IAI, grant no. CRN3038), the US National Science Foundation (grant GEO-1128040), and the University of Regina start-up funds to M. Velez. NR 50 TC 0 Z9 0 U1 6 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0267-8179 EI 1099-1417 J9 J QUATERNARY SCI JI J. Quat. Sci. PD OCT PY 2016 VL 31 IS 7 BP 731 EP 740 DI 10.1002/jqs.2899 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA EC9BF UT WOS:000388437800008 ER PT J AU Porter, ET Breitburg, DL AF Porter, Elka T. Breitburg, Denise L. TI Eastern oyster, Crassostrea virginica, valve gape behavior under diel-cycling hypoxia SO MARINE BIOLOGY LA English DT Article ID EARLY WARNING SYSTEM; MYTILUS-EDULIS; BENTHIC MACROFAUNA; CHESAPEAKE BAY; FOOD AVAILABILITY; ANODONTA-CYGNEA; MACOMA-BALTHICA; METABOLIC-RATE; DEAD ZONES; RESPONSES AB Hypoxia and anoxia in many estuaries worldwide can cause a wide range of negative effects on animals that are directly exposed or indirectly influenced by food web interactions. Typically, experimental studies focus on animal behavior as a function of continuous exposure to low dissolved oxygen (DO) conditions rather than short-term fluctuations. Dissolved oxygen concentrations [DO] can, however, vary throughout the day, and water can become hypoxic for minutes to hours, often during the late night/early morning hours in the summer. Valve gape of 1-year-old eastern oysters, Crassostrea virginica, from Maryland, USA, was continuously measured while exposed to diel-cycling DO in aquaria during normoxic, hypoxic, and supersaturated phases of the cycle over several 2-day periods (July-August 2012). Severe hypoxia (0.6 mg DO L-1) induced oysters to close for significantly longer times than normoxic (7.3 mg DO L-1) conditions. Oysters exposed to mild hypoxia (1.7 mg DO L-1) closed for a similar amount of time as oysters held at normoxia and severe hypoxia. At severe hypoxia, more than one-third of the oysters closed simultaneously and closed immediately when they encountered severe hypoxia while oysters at mild hypoxia often closed later in the low oxygen phase of the cycles. When normoxia was reintroduced after severe hypoxia, most oysters opened immediately and gaped throughout the period. The results indicate that while 1-year-old oysters responded negatively to diel-cycling low [DO], especially to severe hypoxia, they rapidly opened during the normoxic period that followed, potentially reducing any negative effects of a fluctuating environment. C1 [Porter, Elka T.] Univ Baltimore, Yale Gordon Coll Arts & Sci, 1420 N Charles St, Baltimore, MD 21201 USA. [Breitburg, Denise L.] Smithsonian Inst, 664 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Porter, ET (reprint author), Univ Baltimore, Yale Gordon Coll Arts & Sci, 1420 N Charles St, Baltimore, MD 21201 USA. EM eporter@ubalt.edu FU National Oceanic and Atmospheric Administration Center for Sponsored Coastal Ocean Research [NA10NOS4780138]; Smithsonian Hunterdon Fund; Faculty Enhancement Grant by Washington College FX We thank Andrew Keppel, Virginia Clark, and Rebecca Burrell for maintaining the did cycling hypoxia conditions throughout this experiment. We thank F. Scott Porter who built the valve gape apparatus. Oysters were purchased from Marinetics, Cambridge, Maryland. The hypoxia experiments were funded by a National Oceanic and Atmospheric Administration Center for Sponsored Coastal Ocean Research grant No. NA10NOS4780138 and by the Smithsonian Hunterdon Fund to Denise Breitburg. The valve gape measurements during the hypoxia experiments were funded by a Faculty Enhancement Grant by Washington College to Elka T. Porter. We would also like to thank three anonymous reviewers for valuable suggestions that improved the manuscript. NR 68 TC 0 Z9 0 U1 2 U2 2 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD OCT PY 2016 VL 163 IS 10 AR 218 DI 10.1007/s00227-016-2980-1 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA EA1MJ UT WOS:000386356100022 ER PT J AU Sherman, CDH Lotterhos, KE Richardson, MF Tepolt, CK Rollins, LA Palumbi, SR Miller, AD AF Sherman, C. D. H. Lotterhos, K. E. Richardson, M. F. Tepolt, C. K. Rollins, L. A. Palumbi, S. R. Miller, A. D. TI What are we missing about marine invasions? Filling in the gaps with evolutionary genomics SO MARINE BIOLOGY LA English DT Review ID CHINESE MITTEN CRAB; CTENOPHORE MNEMIOPSIS-LEIDYI; ALGA CAULERPA-TAXIFOLIA; MUSSELS GENUS MYTILUS; EUROPEAN GREEN CRAB; LONG NONCODING RNAS; LOCAL ADAPTATION; DNA METHYLATION; NEXT-GENERATION; GENETIC DIVERSITY AB Research on invasion biology has been largely dominated by studies on the ecological effects of invasion events, although recently, evolutionary processes have been shown to be important to invasion success. This is largely attributed to novel genomic tools that provide new opportunities to unravel the natural history, taxonomy, and invasion pathways of invasive species, as well as the genetic basis of adaptive traits that allow them to expand within and beyond their native range. Despite these advances and the growing literature of genomic research on terrestrial pests, these tools have not been widely applied to marine invasive species. This is in part due to the perception that high levels of dispersal and connectivity in many invasive marine species can limit the opportunity for local adaptation. However, there is growing evidence that even in species with high dispersal potential, significant site-specific adaptation can occur. We review how these "omic" tools provide unprecedented opportunities to characterise the role of adaptive variation, physiological tolerance, and epigenetic processes in determining the success of marine invaders. Yet, rapid range expansion in invasions can confound the analysis of genomic data, so we also review how data should be properly analysed and carefully interpreted under such circumstances. Although there are a limited number of studies pioneering this research in marine systems, this review highlights how future studies can be designed to integrate ecological and evolutionary information. Such datasets will be imperative for the effective management of marine pests. C1 [Sherman, C. D. H.; Richardson, M. F.; Rollins, L. A.; Miller, A. D.] Deakin Univ, Sch Life & Environm Sci, Ctr Integrat Ecol, Waurn Ponds Campus,75 Pigdons Rd,Locked Bag 20000, Geelong, Vic 3220, Australia. [Lotterhos, K. E.] Northeastern Univ, Ctr Marine Sci, Dept Marine & Environm Sci, 430 Nahant Rd, Nahant, MA 01908 USA. [Tepolt, C. K.] Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. [Palumbi, S. R.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [Miller, A. D.] Univ Melbourne, Sch BioSci, Pest & Environm Adaptat Res Grp, Parkville, Vic 3010, Australia. RP Sherman, CDH (reprint author), Deakin Univ, Sch Life & Environm Sci, Ctr Integrat Ecol, Waurn Ponds Campus,75 Pigdons Rd,Locked Bag 20000, Geelong, Vic 3220, Australia. EM craig.sherman@deakin.edu.au OI Sherman, Craig/0000-0003-2099-0462 FU Centre for Integrative Ecology, Deakin University FX Research support was provided by funding from the Centre for Integrative Ecology, Deakin University to CDHS, ADM, MFR, and LAR. NR 279 TC 1 Z9 1 U1 20 U2 20 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD OCT PY 2016 VL 163 IS 10 AR 198 DI 10.1007/s00227-016-2961-4 PG 24 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA EA1MJ UT WOS:000386356100002 ER PT J AU Schachat, SR Gibbs, G AF Schachat, Sandra R. Gibbs, GeorgeW. TI Variable wing venation in Agathiphaga (Lepidoptera: Agathiphagidae) is key to understanding the evolution of basal moths SO Royal Society Open Science LA English DT Article DE Amphiesmenoptera; development; disparity; morphology; phenotypic variation; polymorphism ID INSECTA LEPIDOPTERA; ARAUCARIACEAE MACROFOSSILS; MORPHOLOGY; PHYLOGENY; GELECHIOIDEA; TORTRICIDAE; AUSTRALIA; PATTERN; FAMILY; RECORD AB Details of the ancestral groundplan of wing venation in moths remain uncertain, despite approximately a century of study. Here, we describe a 3-branched subcostal vein, a 5-branched medial vein and a 2-branched cubitus posterior vein on the forewing of Agathiphaga vitiensis Dumbleton 1952 from Vanuatu. Such veins had not previously been described in any Lepidoptera. Because wing veins are typically lost during lepidopteran evolutionary history, rarely-if ever-to be regained, the venation of A. vitiensis probably represents the ancestral character state for moths. Wing venation is often used to identify fossil insects as moths, because wing scales are not always preserved; the presence of a supposedly trichopteran 3-branched subcostal vein in crown Lepidoptera may decrease the certainty with which certain amphiesmenopteran fossils from the Mesozoic can be classified. And because plesiomorphic veins can influence the development of lepidopteran wing patterns even if not expressed in the adult wing, the veins described here may determine the location of wing pattern elements in many lepidopteran taxa. C1 [Schachat, Sandra R.] Mississippi Entomol Museum, Mississippi State, MS 39762 USA. [Schachat, Sandra R.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Gibbs, GeorgeW.] Victoria Univ, Sch Biol Sci, POB 600, Wellington 6140, New Zealand. RP Schachat, SR (reprint author), Mississippi Entomol Museum, Mississippi State, MS 39762 USA.; Schachat, SR (reprint author), Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. EM schachatsr@si.edu OI Schachat, Sandra/0000-0003-3237-5619 FU Graduate Research Opportunities Worldwide, a initiative of Australian National University; Sigma Xi [G201503151194219]; National Science Foundation [DGE-1125191]; Graduate Research Opportunities Worldwide, a initiative of National Science Foundation FX S.R.S. received funding as follows. Travel to Australia: Graduate Research Opportunities Worldwide, a joint initiative of Australian National University and the National Science Foundation. Travel to New Zealand: Sigma Xi Grant-in-Aid of Research, grant no. G201503151194219. Graduate research: National Science Foundation Graduate Research Fellowship, grant no. DGE-1125191. NR 63 TC 2 Z9 2 U1 3 U2 3 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 2054-5703 J9 ROY SOC OPEN SCI JI R. Soc. Open Sci. PD OCT PY 2016 VL 3 IS 10 AR 160453 DI 10.1098/rsos.160453 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EE0CS UT WOS:000389241700030 PM 27853559 ER PT J AU Mecke, S Mader, F Kieckbusch, M Kaiser, H Bohme, W Ernst, R AF Mecke, Sven Mader, Felix Kieckbusch, Max Kaiser, Hinrich Boehme, Wolfgang Ernst, Raffael TI Tracking a syntype of the Australian skink Anomalopus leuckartii (WEIN LAND, 1862): 'lost' treasures in the Senckenberg Natural History Collections Dresden highlight the importance of reassessing and safe-guarding natural history collections SO VERTEBRATE ZOOLOGY LA English DT Article DE Scincidae; Lygosominae; Anomalopus leuckartii; Australia; taxonomy; syntype; lectotype; morphology; natural history collections; museums ID BENT-TOED GECKO; SQUAMATA GEKKONIDAE; MUSEUM; CYRTODACTYLUS; SPECIMENS; INDONESIA; JAVA AB We here report the rediscovery of a type specimen of the Australian skink Anomalopus leuckartii (WEINLAND, 1862) in the Museum of Zoology (Museum far Tierkunde), Senckenberg Natural History Collections Dresden (accession number MTKD 10205), heretofore presumed lost during World War II. Eidonomic data for the specimen conform to the original species description, and combined with the specimen's history, we are able to unequivocally identify it as part of the original syntype series. WEINLAND'S description was based on two specimens, one of which does indeed appear to be lost. Consequently, MTKD 10205 is designated as lectotype of A. leuckartii. This find invalidates the subsequent designation of AM R 44677 (Australian Museum, Sydney) as neotype for the species. The rediscovery highlights the importance of maintaining natural history collections, not merely as static archives but rather as dynamic and lively databases. This in combination with optimal taxonomic expertise as bedrock guarantees an environment, in which new discoveries are not impeded but actively promoted, thereby inevitably advancing modern biodiversity research. C1 [Mecke, Sven; Kieckbusch, Max] Philipps Univ Marburg, Fachbereich Biol, AG Evolut & Systemat Tiere & Zool Sammlung Marbur, Karl von Frisch Str 8, D-35032 Marburg, Germany. [Mader, Felix] Janusstr 5, D-93051 Regensburg, Germany. [Kaiser, Hinrich] Victor Valley Coll, Dept Biol, 18422 Bear Valley Rd, Victorville, CA 92395 USA. [Kaiser, Hinrich] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Boehme, Wolfgang] Forsch Museum Alexander Koenig, Sekt Herpetol, Adenauer Allee 160, D-53113 Bonn, Germany. [Ernst, Raffael] Senckenberg Nat Hist Sammlungen Dresden, Museum Tierkunde, Sekt Herpetol, Konigsbrucker Landstr 159, D-01109 Dresden, Germany. RP Mecke, S (reprint author), Philipps Univ Marburg, Fachbereich Biol, AG Evolut & Systemat Tiere & Zool Sammlung Marbur, Karl von Frisch Str 8, D-35032 Marburg, Germany. EM meckes@staff.uni-marburg.de NR 71 TC 0 Z9 0 U1 0 U2 0 PU STAATLICHES MUSEUM TIERKUNDE DRESDEN PI DRESDEN PA KOENIGSBRUECKER LANDSTRASSE 159, DRESDEN, 00000, GERMANY SN 1864-5755 J9 VERTEBR ZOOL JI Vertebr. Zool. PD OCT PY 2016 VL 66 IS 2 BP 169 EP 177 PG 9 WC Zoology SC Zoology GA EA6NH UT WOS:000386745400007 ER PT J AU Hilton, EJ Dillman, CB Zhang, T Zhang, LZ Zhuang, P AF Hilton, Eric J. Dillman, Casey B. Zhang, Tao Zhang, Longzhen Zhuang, Ping TI The skull of the Chinese sturgeon, Acipenser sinensis (Acipenseridae) SO ACTA ZOOLOGICA LA English DT Article DE Acipenseriformes; Actinopterygii; anatomy; cranium; osteologyi ID ORDER ACIPENSERIFORMES; MOLECULAR PHYLOGENY; PADDLEFISH; BIOGEOGRAPHY; CONSERVATION; SYSTEMATICS; SPECIMENS; BIOLOGY; ANATOMY AB The Chinese sturgeon, Acipenser sinensis, is a large member of Acipenseridae now found only in the Yangtze River and the Yellow and East China seas. The goal of this paper was to describe the skull of A. sinensis in the context of recent anatomical and systematic studies of sturgeons. Five specimens (354-670 mm standard length) were prepared as skeletons. The left and right parietals and frontals are broadly separated by a median fontanelle. The lateral-most lateral extrascapular variably supports the confluence of the supratemporal, occipital and trunk lateral lines. There is no distinct ventral supraorbital process as found in other sturgeons. The anterodorsal portion of the snout is unique among Acipenseridae by having a single large anamestic dorsal rostral bone instead of a series of separate dorsal rostral bones. There are 0-2 lateral rostral bones on each side positioned anterior to but not in contact with the horizontal arm of the jugal. The dorsal surface of the neurocranium lacks a pineal opening, and its anterior tip is sharply pointed in the smaller specimens examined and gently curved in larger specimens. The anteromedial arm of the palatopterygoid is broad relative to other acipenserids. These new morphological data are discussed and compared among Acipenseridae. C1 [Hilton, Eric J.; Dillman, Casey B.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. [Zhang, Tao; Zhang, Longzhen; Zhuang, Ping] Chinese Acad Fishery Sci, East China Sea Fisheries Res Inst, 300 Jun Gong Rd, Shanghai 200090, Peoples R China. [Dillman, Casey B.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Hilton, EJ (reprint author), Virginia Inst Marine Sci, Coll William & Mary, Dept Fisheries Sci, Gloucester Point, VA 23062 USA. EM ehilton@vims.edu FU U.S. National Science Foundation [DEB-0841691]; National Nature Science Foundation of China [31101881] FX We are grateful to Zhao Feng, Hou Junli, Wang Rui-Fang, Wang Yu and Yang Gang for assistance in preparation of specimens during a visit by EJH and CBD to Shanghai. This research was supported in part by the U.S. National Science Foundation (DEB-0841691, to EJH and CBD) and the National Nature Science Foundation of China (31101881; to PZ). This is contribution number 3484 of the Virginia Institute of Marine Science, College of William & Mary. NR 33 TC 1 Z9 1 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0001-7272 EI 1463-6395 J9 ACTA ZOOL-STOCKHOLM JI Acta Zool. PD OCT PY 2016 VL 97 IS 4 BP 419 EP 432 DI 10.1111/azo.12136 PG 14 WC Anatomy & Morphology; Zoology SC Anatomy & Morphology; Zoology GA EC8RY UT WOS:000388411500003 ER PT J AU Dell'Aglio, DD Stevens, M Jiggins, CD AF Dell'Aglio, Denise D. Stevens, Martin Jiggins, Chris D. TI Avoidance of an aposematically coloured butterfly by wild birds in a tropical forest SO ECOLOGICAL ENTOMOLOGY LA English DT Article DE Aposematism; artificial models; Heliconius; memory; predation ID MULLERIAN MIMICRY; HELICONIUS-BUTTERFLIES; WARNING COLORATION; PREDATOR AVOIDANCE; DIETARY CONSERVATISM; RECEIVER PSYCHOLOGY; NATURAL-SELECTION; SIGNALS; EVOLUTION; MEMORY AB 1. Birds are considered to be the primary selective agents for warning colouration in butterflies, and select for aposematic mimicry by learning to avoid brightly coloured prey after unpleasant experiences. It has long been thought that bright colouration plays an important role in promoting the avoidance of distasteful prey by birds. 2. The hypothesis that warning colouration facilitates memorability and promotes predator avoidance was tested by means of a field experiment using distasteful model butterflies. Artificial butterflies with a Heliconius colour pattern unknown to local birds were generated using bird vision models, either coloured or achromatic, and hung in tree branches in a tropical forest. Two sequential trials were conducted at each site to test avoidance by naive and experienced predators. 3. There was a significant reduction in predation in the second trial. Also, coloured models were attacked less than achromatic models. Specifically, coloured butterflies were attacked significantly less in the second trial, but there was no significant decrease in predation on achromatic models. 4. The present results imply an important role for colour in enhancing aversion of aposematic butterflies. It has also been demonstrated that previous experience of distasteful prey can lead to enhanced avoidance in subsequent trials, supporting mimicry theory. C1 [Dell'Aglio, Denise D.; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Butterfly Genet Grp, Cambridge, England. [Dell'Aglio, Denise D.; Jiggins, Chris D.] Smithsonian Trop Res Inst, Panama City, Panama. [Stevens, Martin] Univ Exeter, Coll Life & Environm Sci, Ctr Ecol & Conservat, Penryn, England. RP Dell'Aglio, DD (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM ddd23@cam.ac.uk FU CAPES (Brazil); Cambridge Trust (UK); Biotechnology and Biological Sciences Research Council (BBSRC) [BB/G022887/1] FX This study was supported by CAPES (Brazil) and Cambridge Trust (UK) to D.D.D, and by Biotechnology and Biological Sciences Research Council (BBSRC) David Phillips Research Fellowship (BB/G022887/1) to M.S. NR 49 TC 1 Z9 1 U1 27 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6946 EI 1365-2311 J9 ECOL ENTOMOL JI Ecol. Entomol. PD OCT PY 2016 VL 41 IS 5 BP 627 EP 632 DI 10.1111/een.12335 PG 6 WC Entomology SC Entomology GA EC7HU UT WOS:000388308600014 PM 27708481 ER PT J AU Fujihara, M Yamamizu, K Wildt, DE Songsasen, N AF Fujihara, M. Yamamizu, K. Wildt, D. E. Songsasen, N. TI Expression pattern of matrix metalloproteinases changes during folliculogenesis in the cat ovary SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Article ID RIBONUCLEIC-ACID EXPRESSION; TISSUE INHIBITOR; FOLLICULAR DEVELOPMENT; RAT OVARY; EXTRACELLULAR-MATRIX; GROWTH-FACTORS; MOUSE OVARY; IN-VITRO; FOLLICLES; SYSTEM AB Matrix metalloproteinase (MMP) has been implicated as having roles in ovarian folliculogenesis. Here, we determined the expression pattern of six MMPs (MMP1, MMP2, MMP3, MMP7, MMP9 and MMP13) and their endogenous tissue inhibitor, TIMP1, during cat follicle growth. Different developmental stage follicles were mechanically isolated and gene expression analysed by real-time qPCR while MMP1, 2, 9 and 13 localization was determined by immunohistochemistry. With the exception of MMP13, the amount of MMP mRNA was lowest in primordial follicles and increased thereafter. Peak levels were detected in early antral follicles for MMP1 (72.2-fold increase above primordial follicle amount), MMP2 (10-fold), MMP3 (57-fold) and MMP9 (2.8-fold). MMP7 transcripts increased 2-fold by the primary follicle stage and then plateaued. MMP13 mRNA peaked in primary follicles (2.5-fold) and was lower in more advanced counterparts. TIMP1 sharply increased (6-fold) in secondary follicles and gradually declined in the later stages. MMP1 and MMP9 expression were expressed in the granulosa cells of all follicle stages. MMP2 was immunoreactive in early and antral follicles, especially at granulosa cells adjacent to the antral cavity. By contrast, the MMP13 was weakly detected in primary follicles onward. In summary, there are distinctive and consistent changes in MMPs and TIMP1 expression during follicle development, suggesting that these enzymes play one or more roles in cat folliculogenesis. In particular, high mRNA and protein expression levels of MMP1 and MMP2, especially at the antral stage, indicate that these enzymes likely are involved in antrum formation and expansion. C1 [Fujihara, M.; Wildt, D. E.; Songsasen, N.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Fujihara, M.] Kyoto Univ, Wildlife Res Ctr, Kyoto, Japan. [Yamamizu, K.] Kyoto Univ, Ctr iPS Cell Res & Applicat CiRA, Kyoto, Japan. RP Songsasen, N (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. EM songsasenn@si.edu FU Japanese Society for Promotion of Sciences; Smithsonian Institution FX The authors thank veterinary hospitals in Front Royal, Stephens City, Harrisonburg and Purcellville, Virginia for providing cat ovaries. The authors also acknowledge Dr. Budhan Pukazhenthi (Smithsonian Conservation Biology Institute) for technical advice and Drs. Jennifer Nagashima and Chommanart Thongkittidilok (Smithsonian Conservation Biology Institute) for technical supports. This research was supported by the Japanese Society for Promotion of Sciences (MF) and Smithsonian Institution. NR 52 TC 0 Z9 0 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0936-6768 EI 1439-0531 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD OCT PY 2016 VL 51 IS 5 BP 717 EP 725 DI 10.1111/rda.12736 PG 9 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA EC7PZ UT WOS:000388334100011 PM 27484055 ER PT J AU Franz, K AF Franz, Kathleen TI Packaged Pleasures: How Technology and Marketing Revolutionized Desire. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Franz, Kathleen] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Franz, K (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X EI 1097-3729 J9 TECHNOL CULT JI Technol. Cult. PD OCT PY 2016 VL 57 IS 4 BP 1027 EP 1028 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA EC5FA UT WOS:000388157300029 ER PT J AU Afshari, M Peres, G Jibben, PR Petralia, A Reale, F Weber, M AF Afshari, M. Peres, G. Jibben, P. R. Petralia, A. Reale, F. Weber, M. TI X-RAYING THE DARK SIDE OF VENUS-SCATTER FROM VENUS' MAGNETOTAIL? SO ASTRONOMICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (Venus); planets and satellites: terrestrial planets; Sun: UV radiation; Sun: X-rays, gamma rays ID TELESCOPE XRT; DECONVOLUTION; TRANSIT; CHANDRA; RAYS AB We analyze significant X-ray, EUV, and UV emission coming from the dark side of Venus observed with Hinode/XRT and Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) during a transit across the solar disk that. occurred in 2012. As a check we have analyzed an analogous Mercury transit that. occurred in 2006. We have used the latest version of the Hinode/XRT point spread function to deconvolve Venus and Mercury X-ray images, to remove instrumental scattering. After deconvolution, the flux from Venus' shadow remains significant while that of Mercury becomes negligible. Since stray light contamination affects the XRT Ti-poly filter data we use, we performed the same analysis with XRT Al-mesh filter data, not affected by the light leak. Even the latter data show residual flux. We have also found significant EUV (304 angstrom, 193 angstrom, 335 angstrom) and UV (1700 angstrom) flux in Venus' shadow, measured with SDO/AIA. The EUV emission from Venus' dark side is reduced, but still significant, when deconvolution is applied. The light curves of the average flux of the shadow in the X-ray, EUV, and UV bands appear different as Venus crosses the solar disk, but in any of them the flux is, at any time, approximately proportional to the average flux in a ring surrounding Venus, and therefore proportional to that of the solar regions around Venus' obscuring disk line of sight. The proportionality factor depends on the band. This phenomenon has no clear origin; we suggest that. it may be due to scatter occurring in the very long magnetotail of Venus. C1 [Afshari, M.; Peres, G.; Petralia, A.; Reale, F.] Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy. [Afshari, M.; Peres, G.; Petralia, A.; Reale, F.] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. [Jibben, P. R.; Weber, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Peres, G (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy.; Peres, G (reprint author), INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. EM peres@astropa.unipa.it OI PERES, Giovanni/0000-0002-6033-8180; Reale, Fabio/0000-0002-1820-4824 FU Italian Ministero dell'Universita e Ricerca; MSFC/NASA [NNM07AB07C] FX We thank the. anonymous referee for suggestions and comments on EUV deconvolution. M.A., G.P., A.P., and F.R. acknowledge support from Italian Ministero dell'Universita e Ricerca; P.J. and M.W. were supported under contract NNM07AB07C from MSFC/NASA to SAO. Some of the routines for the data analysis and some early evaluations were kindly supplied by A.F. Gambino. SDO data were supplied courtesy of the SDO/AIA consortia. SDO is the first mission to be launched for NASA's Living With a Star Program. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and the NSC (Norway). NR 23 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2016 VL 152 IS 4 AR 107 DI 10.3847/0004-6256/152/4/107 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ3LQ UT WOS:000385749000005 ER PT J AU Espinoza, N Bayliss, D Hartman, JD Bakos, GA Jordan, A Zhou, G Mancini, L Brahm, R Ciceri, S Bhatti, W Csubry, Z Rabus, M Penev, K Bento, J de Val-Borro, M Henning, T Schmidt, B Suc, V Wright, DJ Tinney, CG Tan, TG Noyes, R AF Espinoza, N. Bayliss, D. Hartman, J. D. Bakos, G. A. Jordan, A. Zhou, G. Mancini, L. Brahm, R. Ciceri, S. Bhatti, W. Csubry, Z. Rabus, M. Penev, K. Bento, J. de Val-Borro, M. Henning, T. Schmidt, B. Suc, V. Wright, D. J. Tinney, C. G. Tan, T. G. Noyes, R. TI HATS-25B THROUGH HATS-30B: A HALF-DOZEN NEW INFLATED TRANSITING HOT JUPITERS FROM THE HATSOUTH SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: individual (HATS-25, HATS-26, HATS-27, HATS-28, HATS-29, HATS-30) ID EXTRASOLAR PLANETARY SYSTEMS; OHMIC DISSIPATION; SUPER-NEPTUNE; GIANT PLANETS; KEPLER FIELD; STAR; STELLAR; EXOPLANETS; SPECTROGRAPH; ATMOSPHERES AB We report six new inflated hot Jupiters (HATS-25b through HATS-30b) discovered using the HATSouth global network of automated telescopes. The planets orbit stars with V magnitudes in the range of similar to 12-14 and have masses in the largely populated 0.5M(J)-0.7M(J) region of parameter space but span a wide variety of radii, from 1.17R(J) to 1.75R(J). HATS-25b, HATS-28b, HATS-29b, and HATS-30b are typical inflated hot Jupiters (R-p = 1.17-1.26R(J)) orbiting G-type stars in short period (P = 3.2-4.6 days) orbits. However, HATS-26b (R-p = 1.75R(J), P = 3.3024 days) and HATS-27b (R-p = 1.50R(J), P = 4.6370 days) stand out as highly inflated planets orbiting slightly evolved F stars just after and in the turn-off points, respectively, which are among the least dense hot Jupiters, with densities of 0.153 g cm(-3) and 0.180 g cm(-3), respectively. All the presented exoplanets but HATS-27b are good targets for future atmospheric characterization studies, while HATS-27b is a prime target for Rossiter-McLaughlin monitoring in order to determine its spin-orbit alignment given the brightness (V = 12.8) and stellar rotational velocity (v sin i approximate to 9.3 km s(-1)) of the host star. These discoveries significantly increase the number of inflated hot Jupiters known, contributing to our understanding of the mechanism(s) responsible for hot Jupiter inflation. C1 [Espinoza, N.; Jordan, A.; Brahm, R.; Rabus, M.; Suc, V.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. [Espinoza, N.; Jordan, A.; Brahm, R.] Millennium Inst Astrophys, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. [Bayliss, D.] Univ Geneva, Observ Astron, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. [Hartman, J. D.; Bakos, G. A.; Bhatti, W.; Csubry, Z.; Penev, K.; de Val-Borro, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Zhou, G.; Noyes, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Mancini, L.; Ciceri, S.; Rabus, M.; Henning, T.] Max Planck Inst Astron, Heidelberg, Germany. [Bento, J.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Wright, D. J.; Tinney, C. G.] UNSW Australia, Sch Phys, Exoplanetary Sci UNSW, Sydney, NSW 20152, Australia. [Wright, D. J.; Tinney, C. G.] UNSW Australia, Australian Ctr Astrobiol, Sydney, NSW 20152, Australia. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. RP Espinoza, N (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile.; Espinoza, N (reprint author), Millennium Inst Astrophys, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. EM nespino@astro.puc.cl OI Schmidt, Brian/0000-0001-6589-1287; Bakos, Gaspar/0000-0001-7204-6727; Espinoza Perez, Nestor/0000-0001-9513-1449; Tan, Thiam-Guan/0000-0001-5603-6895; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI [NSF/AST-0723074]; NASA [NNX09AB29G, NNX12AH91H]; CONICYT-PCHA/Doctorado Nacional; FONDECYT [1130857]; BASAL CATA [PFB-06]; Millenium Science Initiative, Chilean Ministry of Economy [IC120009]; ARC Laureate Fellowship [FL0992131]; ARC Discovery Project [DP130102695]; Robert Martin Ayers Sciences Fund; SIMBAD database; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G and NNX12AH91H, and follow-up observations receive partial support from grant NSF/AST-1108686. N.E. is supported by CONICYT-PCHA/Doctorado Nacional. A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. acknowledge support from project IC120009 " Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. This work is based on observations made with ESO Telescopes at the La Silla Observatory. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. Work at UNSW is supported by ARC Discovery Project DP130102695. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. Operations at the MPG. 2.2 m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. The imaging system GROND has been built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO. We thank the MPG. 2.2 m telescope support team for their technical assistance during observations. We thank Helmut Steinle and Jochen Greiner for supporting the GROND observations presented in this manuscript. Observing time were obtained through proposals CN2013-B55, CN2014A-104, CN2014B-571, and ESO 096.C-0544. We are grateful to P. Sackett for her help in the early phase of the HATSouth project. NR 59 TC 0 Z9 0 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2016 VL 152 IS 4 AR 108 DI 10.3847/0004-6256/152/4/108 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ3LQ UT WOS:000385749000006 ER PT J AU MacDonald, MG Ragozzine, D Fabrycky, DC Ford, EB Holman, MJ Isaacson, HT Lissauer, JJ Lopez, ED Mazeh, T Rogers, L Rowe, JF Steffen, JH Torres, G AF MacDonald, Mariah G. Ragozzine, Darin Fabrycky, Daniel C. Ford, Eric B. Holman, Matthew J. Isaacson, Howard T. Lissauer, Jack J. Lopez, Eric D. Mazeh, Tsevi Rogers, Leslie Rowe, Jason F. Steffen, Jason H. Torres, Guillermo TI A DYNAMICAL ANALYSIS OF THE KEPLER-80 SYSTEM OF FIVE TRANSITING PLANETS SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; planets and satellites: dynamical evolution and stability; stars: individual (Kepler-80) ID MEAN MOTION RESONANCES; BVRI PHOTOMETRIC SYSTEMS; MAIN-SEQUENCE STARS; LOW-DENSITY PLANETS; DIGITAL SKY SURVEY; EXOPLANETARY SYSTEMS; TRANSFORMATION EQUATIONS; COLOR TRANSFORMATIONS; TERRESTRIAL PLANETS; TIMING OBSERVATIONS AB Kepler. has discovered hundreds of systems with multiple transiting exoplanets which hold tremendous potential both individually and collectively for understanding the formation and evolution of planetary systems. Many of these systems consist of multiple small planets with periods less than similar to 50 days known as Systems with Tightly spaced Inner Planets, or STIPs. One especially intriguing STIP, Kepler-80 (KOI-500), contains five transiting planets: f, d, e, b, and c with periods of 1.0, 3.1, 4.6, 7.1, and 9.5 days, respectively. We provide measurements of transit times and a transit timing variation (TTV) dynamical analysis. We find that TTVs cannot reliably detect eccentricities for this system, though mass estimates are not affected. Restricting the eccentricity to a reasonable range, we infer masses for the outer four planets (d, e, b, and c) to be 6.75(-0.51)(+0.69), 4.13(-0.95)(+0.81), 6.93(-0.70)(+1.05), and 6.74(-0.86)(+1.23) Earth masses, respectively. The similar masses but different radii are consistent with terrestrial compositions for d and e and similar to 2% H/He envelopes for b and c. We confirm that the outer four planets are in a rare dynamical configuration with four interconnected three-body resonances that are librating with few degree amplitudes. We present a formation model that can reproduce the observed configuration by starting with a multi-resonant chain and introducing dissipation. Overall, the information-rich Kepler-80 planets provide an important perspective into exoplanetary systems. C1 [MacDonald, Mariah G.; Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, 150 West Univ Blvd, Melbourne, FL 32940 USA. [Ragozzine, Darin] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Ragozzine, Darin; Holman, Matthew J.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.; Rogers, Leslie] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA. [Ford, Eric B.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Ford, Eric B.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA. [Isaacson, Howard T.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Lissauer, Jack J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. [Lopez, Eric D.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Blackford Hill, Edinburgh, Midlothian, Scotland. [Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Steffen, Jason H.] Univ Nevada, Dept Phys & Astron, 4505 S Maryland Pkwy,Box 454002, Las Vegas, NV 89154 USA. RP MacDonald, MG (reprint author), Florida Inst Technol, Dept Phys & Space Sci, 150 West Univ Blvd, Melbourne, FL 32940 USA. EM mmacdonald2012@my.fit.edu; darin.ragozzine@gmail.com OI Ragozzine, Darin/0000-0003-1080-9770; Rogers, Leslie/0000-0003-0638-3455; Isaacson, Howard/0000-0002-0531-1073; /0000-0001-6545-639X NR 104 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2016 VL 152 IS 4 AR 105 DI 10.3847/0004-6256/152/4/105 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ3LQ UT WOS:000385749000003 ER PT J AU Rota, CT Ferreira, MAR Kays, RW Forrester, TD Kalies, EL McShea, WJ Parsons, AW Millspaugh, JJ AF Rota, Christopher T. Ferreira, Marco A. R. Kays, Roland W. Forrester, Tavis D. Kalies, Elizabeth L. McShea, William J. Parsons, Arielle W. Millspaugh, Joshua J. TI A multispecies occupancy model for two or more interacting species SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE community; competition; eMammal; interspecific interactions; multinomial logit; multinomial probit; multivariate Bernoulli; occupancymodelling; predation ID LARGE DATA SETS; COOCCURRENCE PATTERNS; BAYESIAN-ANALYSIS; RANGE USE; SELECTION; HABITAT; PARAMETERIZATION; FEAR AB 1. Species occurrence is influenced by environmental conditions and the presence of other species. Current approaches for multispecies occupancy modelling are practically limited to two interacting species and often require the assumption of asymmetric interactions. We propose amultispecies occupancymodel that can accommodate two ormore interacting species. 2. We generalize the single-species occupancy model to two or more interacting species by assuming the latent occupancy state is a multivariate Bernoulli random variable. We propose modelling the probability of each potential latent occupancy state with both a multinomial logit and a multinomial probit model and present details of aGibbs sampler for the latter. 3. As an example, we model co-occurrence probabilities of bobcat (Lynx rufus), coyote (Canis latrans), grey fox (Urocyon cinereoargenteus) and red fox (Vulpes vulpes) as a function of human disturbance variables throughout 6 Mid-Atlantic states in the eastern United States. We found evidence for pairwise interactions among most species, and the probability of some pairs of species occupying the same site varied along environmental gradients; for example, occupancy probabilities of coyote and grey fox were independent at sites with little human disturbance, but these two species were more likely to occur together at sites with high human disturbance. 4. Ecological communities are composed of multiple interacting species. Our proposed method improves our ability to draw inference from such communities by permitting modelling of detection/non-detection data from an arbitrary number of species, without assuming asymmetric interactions. Additionally, our proposed method permits modelling the probability two or more species occur together as a function of environmental variables. These advancements represent an important improvement in our ability to draw community-level inference from multiple interacting species that are subject to imperfect detection. C1 [Rota, Christopher T.] West Virginia Univ, Sch Nat Resources, Morgantown, WV 26506 USA. [Rota, Christopher T.; Millspaugh, Joshua J.] Univ Missouri, Dept Fisheries & Wildlidfe Sci, Columbia, MO 65211 USA. [Ferreira, Marco A. R.] Virginia Tech, Dept Stat, Blacksburg, VA 24061 USA. [Kays, Roland W.; Parsons, Arielle W.] North Carolina Museum Nat Sci, Raleigh, NC 27601 USA. [Kays, Roland W.] North Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Forrester, Tavis D.; McShea, William J.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Kalies, Elizabeth L.] Nature Conservancy, Durham, NC 27701 USA. RP Rota, CT (reprint author), West Virginia Univ, Sch Nat Resources, Morgantown, WV 26506 USA.; Rota, CT (reprint author), Univ Missouri, Dept Fisheries & Wildlidfe Sci, Columbia, MO 65211 USA. EM christopher.rota@mail.wvu.edu FU National Science Foundation [1232442, 1319293]; VWR Foundation; US Forest Service; North Carolina Museum of Natural Sciences; Smithsonian Institution FX We thank our 376 volunteers for their hard work collecting camera trap data for this study. For their field assistance and volunteer coordination, we thank the staff of the NPS, USFWS, USFS, TNC, NC, SC, VA, MD and TN State Parks, NCWRC, TNDF, VDGIF, WVWA, the WNF and RPRCR. We thank N. Fuentes, S. Higdon, T. Perkins, L. Gatens, R. Owens, R. Gayle, C. Backman, K. Clark, J. Grimes and J. Simkins for their help reviewing photographs. This work was conducted with funding from the National Science Foundation grant #1232442 and #1319293, the VWR Foundation, the US Forest Service, the North Carolina Museum of Natural Sciences and the Smithsonian Institution. We thank M. Baker for conversations about study design, training and managing volunteers in WV, VA and MD, and for reviewing, cleaning and managing data from the project. We thank R. Dorazio, R. O'Hara and an anonymous reviewer for helpful comments on early versions of this manuscript. NR 42 TC 0 Z9 0 U1 38 U2 38 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD OCT PY 2016 VL 7 IS 10 BP 1164 EP 1173 DI 10.1111/2041-210X.12587 PG 10 WC Ecology SC Environmental Sciences & Ecology GA EB8VZ UT WOS:000387670700004 ER PT J AU Sigovini, M Keppel, E Tagliapietra, D AF Sigovini, Marco Keppel, Erica Tagliapietra, Davide TI Open Nomenclature in the biodiversity era SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Review DE biodiversity informatics; biomonitoring; controlled vocabulary; primary biodiversity data; semantic tools; species/abundance matrices; taxonomic databases; taxonomy; uncertainty; zoology ID MEDITERRANEAN SEA; INFORMATICS; TAXONOMY; CONSERVATION; CHALLENGES; PRIORITIES; DIVERSITY; KNOWLEDGE; QUALITY; NAMES AB 1. The uncertainty or the provisional status of a taxonomic identification can be expressed by a set of terms and abbreviations known as Open Nomenclature (ON) qualifiers. This approach is widely applied across biological disciplines, and a high amount of biodiversity data left in ON can be found in literature and data bases. However, there is no consensus about ON qualifiers and their meaning. 2. The use of ON qualifiers has been reviewed in order to provide a summary and guide to current practice in zoology. Some recommendation is given to avoid inconsistencies or vagueness. A flow chart is proposed to clarify the sources of uncertainties during identification and to facilitate the application of ON qualifiers. 3. This review provides a guide for taxonomists and ecologists currently involved in biomonitoring and biodiversity programmes, as well as for researchers dealing with biodiversity data infrastructures and tools, offering a starting point for a methodological harmonization. C1 [Sigovini, Marco; Keppel, Erica; Tagliapietra, Davide] CNR Natl Res Council Italy, ISMAR Marine Sci Inst, Arsenale Tesa 104,Castello 2737-F, I-30122 Venice, Italy. [Keppel, Erica] Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. RP Sigovini, M (reprint author), CNR Natl Res Council Italy, ISMAR Marine Sci Inst, Arsenale Tesa 104,Castello 2737-F, I-30122 Venice, Italy. EM marco.sigovini@ve.ismar.cnr.it OI Keppel, Erica/0000-0002-3969-7947; Tagliapietra, Davide/0000-0002-3394-4089 FU National Flagship Project RITMARE - MIUR [SP3_WP2_AZ1_UO03] FX We sincerely thank Prof. A. Minelli (University of Padua, Italy), Dr. C. Glasby (MAGNT, Darwin, Australia), Dr. P. Palma (University of Bournemouth, UK), Dr. A. Ceregato, Dr. I. Guarneri and Dr. S. Menegon (CNR-ISMAR, Venice, Italy), for providing valuable suggestions. Also we would like to thank A. Bracco (Genova, Italy) for assistance with Latin etymologies. Finally, we thank the anonymous referees for their constructive remarks that greatly improved the quality of the manuscript. We gratefully acknowledge the support from the National Flagship Project RITMARE (SP3_WP2_AZ1_UO03) funded by MIUR. NR 61 TC 0 Z9 0 U1 4 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD OCT PY 2016 VL 7 IS 10 BP 1217 EP 1225 DI 10.1111/2041-210X.12594 PG 9 WC Ecology SC Environmental Sciences & Ecology GA EB8VZ UT WOS:000387670700010 ER PT J AU Henry, TJ Howard, SZ AF Henry, Thomas J. Howard, Samuel Z. TI REVISION OF THE NEOTROPICAL PLANT BUG GENUS SINERVUS STAL (HETEROPTERA: MIRIDAE: BRYOCORINAE: ECCRITOTARSINI), WITH THE DESCRIPTION OF FOUR NEW SPECIES AND A CLOSELY RELATED NEW GENUS SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Insecta; Hemiptera; Miridae; Bryocorinae; new genus; new species; new combinations; Neotropics AB The eccritotarsine plant bug genus Sinervus Stal is revised and the species S. apicalis, n. sp. from Honduras and S. cunealis, n. sp. and S. egeri, n. sp. from Brazil are described, bringing the total species in the genus to 11. Sinervus and the nine previously known species are diagnosed and the three new species are described. The genus Sinervaspartus, n. gen. is described to accommodate Spartacus discovittatus Carvalho, new combination (as the type species), Sinervus espartacoides Carvalho and Gomes, new combination, Spartacus venezuelanus Carvalho, new combination, and Sinervaspartus marginalis, n. sp. from Peru. Color dorsal images for all species, male genitalia for the new species, selected SEM micrographs, and keys to help distinguish Sinervus and Sinervaspartus and all included species are provided. Relationships with the New World genus Spartacus Distant and certain Old World genera are discussed. C1 [Henry, Thomas J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012, Washington, DC 20013 USA. [Howard, Samuel Z.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Howard, Samuel Z.] 42 Castro St,Apt 5, San Francisco, CA 94114 USA. RP Henry, TJ (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov NR 21 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2016 VL 118 IS 4 BP 533 EP 554 DI 10.4289/0013-8797.118.4.533 PG 22 WC Entomology SC Entomology GA EB9SX UT WOS:000387738500005 ER PT J AU Martins, ARP Faynel, C Robbins, RK AF Martins, Ananda Regina P. Faynel, Christophe Robbins, Robert K. TI VARIATION OF MALE SECONDARY SEXUAL STRUCTURES AND THE TAXONOMY OF THERITAS LISUS AND RELATIVES (LEPIDOPTERA, LYCAENIDAE, EUMAEINI) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Atlides Section; DNA barcoding; scent pad; scent pouch; Theritas espiritosanto; Theritas silma; Theritas viresco AB We assess variation of male secondary sexual structures, genitalia, and wing patterns in Theritas lisus (Stoll) and relatives to clarify the species level taxonomy, which is needed for a phylogenetic analysis. Variation in the male ventral hindwing scent pouch was especially useful taxonomically. This pouch may be absent, present without androconia, or present with androconia in T. lisus. Despite this variation, pouch size (when present) distinguishes T. lisus from its closest relatives. As an overview, we propose distinguishing traits for a phenetic T. lisus species group, re-examine and confirm the proposed synonymies of T. hisbon and T. orsina with T. lisus and of T. photeinos with T. viresco, confirm the association of the sexes of T. lisus and T. viresco, and describe Theritas silma Martins, Faynel, & Robbins, new species, from French Guiana. CO1 mitochondrial sequences are consistent with these taxonomic results, but the recently introduced barcode index numbers (BINs) recognized too many species. A nomenclatural list summarizes the taxonomic actions in the T. lisus species group. C1 [Martins, Ananda Regina P.] Univ Sao Paulo, Museu Zool, Ave Nazare 481, BR-04263000 Sao Paulo, SP, Brazil. [Martins, Ananda Regina P.] McGill Univ, Redpath Museum, 859 Sherbrooke St West, Montreal, PQ H3A 2K6, Canada. [Faynel, Christophe] 16 Rue Aspres, F-34160 Montaud, France. [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, POB 37012, Washington, DC 20013 USA. RP Martins, ARP (reprint author), Univ Sao Paulo, Museu Zool, Ave Nazare 481, BR-04263000 Sao Paulo, SP, Brazil.; Martins, ARP (reprint author), McGill Univ, Redpath Museum, 859 Sherbrooke St West, Montreal, PQ H3A 2K6, Canada. EM anandarpmartins@gmail.com; eumaeini@yahoo.fr; robbinsr@si.edu RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Sao Paulo Research Foundation - FAPESP, Brazil [2012/03854-8 e 2013/00952-1, 2002/13898-0, 2010/14682-8, 2011/50225-3]; National Council for Scientific and Technological Development - CNPq/ SISBIOTA, Brazil [563332/2010-7]; European Regional Development Fund (ERDF); Conseil regional de Guyane; Conseil general de Guyane; Direction de l'Environnement, de l'Amenagement et du Logement; Ministere de l'Education nationale, de l'Enseignement superieur et de la Recherche, France FX The senior author thanks the Sao Paulo Research Foundation - FAPESP, Brazil (grants: 2012/03854-8 e 2013/00952-1; 2002/13898-0; 2010/14682-8; 2011/50225-3) and the National Council for Scientific and Technological Development - CNPq/ SISBIOTA, Brazil (grant: 563332/2010-7) for financial support. Paratypes were collected during the "Our Planet Reviewed" Guyane-2015 expedition in the Mitaraka range, in the core area of the French Guiana Amazonian Park, organized by the MNHN and Pro-Natura International. The expedition was funded by the European Regional Development Fund (ERDF), the Conseil regional de Guyane, the Conseil general de Guyane, the Direction de l'Environnement, de l'Amenagement et du Logement and by the Ministere de l'Education nationale, de l'Enseignement superieur et de la Recherche, France. It was realized in collaboration with the Parc amazonien de Guyane and the Societe entomologique Antilles-Guyane (SEAG), France. For expertise with illustration and other technical aspects of this project, we are grateful to Karie Darrow, Brian Harris, and Vichai Malikul at the USNM. For sharing specimens and rearing data, we are indebted to D. Ahrenholz, R. Busby, P. DeVries, W. Hallwachs, and D. Janzen. We acknowledge the Canadian Centre for DNA Barcoding (CCDB), Canada, especially the gracious help of Jeremy DeWaard, Vlad Dinca, and E. V. Zakharov. NR 30 TC 0 Z9 0 U1 2 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2016 VL 118 IS 4 BP 555 EP 573 DI 10.4289/0013-8797.118.4.555 PG 19 WC Entomology SC Entomology GA EB9SX UT WOS:000387738500006 ER PT J AU Smith, DR Dolan, AC AF Smith, David R. Dolan, Amelia C. TI A NEW SPECIES OF HUCKLEBERRY SAWFLY OF THE FORMER TRIBE PRISTOLINI (HYMENOPTERA: TENTHREDINIDAE) FROM MONTANA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Symphyta; Nematinae; Pristolini; Melastola; Pristola; fruit feeders AB Pristiphora fructicola Smith and Dolan, n. sp., is described from Montana. It would belong to the former genus Melastola Wong of the former tribe Pristolini, recently synonymized with Pristiphora Latreille. Adults were numerous around Vaccinium globulare Rydberg (Ericaceae), the presumed host, where larvae feed in the fruits. The species is distinguished from the other two species previously placed in Melastola, P. resinicolor (Marlatt) and P. ferruginosa (Wong) (n. comb.). Several new distribution records and host plant associations are given for the species of "Pristolini." C1 [Smith, David R.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. [Dolan, Amelia C.] Montana State Univ, Montana Entomol Collect, Marsh Labs, Room 50,POB 173145, Bozeman, MT 59717 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com; amelia.clare1229@gmail.com FU Montana Department of Agriculture's Specialty Crop Block Grant Program FX We thank Chris Grinter, Illinois Natural History Survey, Champaign, IL, for loan of the type slide of Melastola ferruginosa and Derek Sikes, UAM, for loan of specimens. Michael Ivie, Montana State University, assisted in the determination of this species and loaned specimens for study. Paloma Amaral assisted with field work. This work was conducted with funding to Michael Ivie from a grant by the Montana Department of Agriculture's Specialty Crop Block Grant Program titled "Huckleberry Challenges: Pollinator Mysteries, Pests and New Invasive Threats." Work in the Custer Gallatin National Forest was conducted with permission of Mary C. Erickson, Forest Supervisor, U. S. National Forest Service, Bozeman. This is a contribution of the Montana Agricultural Experiment Station. Mention of trade names or commercial products in this publication is solely for the purpose of providing specific information and does not imply recommendation or endorsement by the USDA. USDA is an equal opportunity provider and employer. NR 7 TC 0 Z9 0 U1 1 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2016 VL 118 IS 4 BP 594 EP 601 DI 10.4289/0013-8797.118.4.594 PG 8 WC Entomology SC Entomology GA EB9SX UT WOS:000387738500010 ER PT J AU Smith, DR Strazanac, JS AF Smith, David R. Strazanac, John S. TI ANNOTATED LIST OF WEST VIRGINIA SAWFLIES (HYMENOPTERA: SYMPHYTA) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE species list; Xyelidae; Pamphiliidae; Pergidae; Argidae; Cimbicidae; Diprionidae; Tenthredinidae; Siricidae; Xiphydriidae; Orussidae; Cephidae ID EASTERN UNITED-STATES; QUERCUSCOCCINEAE DYAR HYMENOPTERA; NEMATUS PANZER HYMENOPTERA; NORTH-AMERICA; CENTRAL KENTUCKY; HOST PLANTS; TENTHREDINIDAE; GENUS; WASHINGTON; ARGIDAE AB Records for 281 species of sawflies in 11 families are listed for West Virginia. Results are based on extensive Malaise trap collections at several sites in Hardy, Tucker, and Pocohantas counties and data from museum specimens. County records and recorded host plants are given for each species. C1 [Smith, David R.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. [Strazanac, John S.] West Virginia Univ, Div Plant & Soil Sci, Morgantown, WV 26506 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com; fritzstraz@gmail.com NR 73 TC 0 Z9 0 U1 0 U2 0 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2016 VL 118 IS 4 BP 602 EP 616 DI 10.4289/0013-8797.118.4.602 PG 15 WC Entomology SC Entomology GA EB9SX UT WOS:000387738500011 ER PT J AU Adaime, R de Jesus-Barros, CR Uramoto, K Norrbom, AL Zucchi, RA AF Adaime, Ricardo de Jesus-Barros, Cristiane Ramos Uramoto, Keiko Norrbom, Allen L. Zucchi, Roberto Antonio TI First Record of Anastrepha zacharyi Norrbom (Diptera, Tephritidae) in Brazil, and Notes on its Host Plant and Parasitoid SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material ID HYMENOPTERA; STATE C1 [Adaime, Ricardo; de Jesus-Barros, Cristiane Ramos] Embrapa Amapa, BR-68903419 Macapa, Amapa, Brazil. [Uramoto, Keiko; Zucchi, Roberto Antonio] Univ Sao Paulo, Dept Entomol & Acarol, Escola Super Agr Luiz de Queiroz, BR-13418900 Sao Paulo, Brazil. [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. RP Adaime, R (reprint author), Embrapa Amapa, BR-68903419 Macapa, Amapa, Brazil. EM ricardo.adaime@embrapa.br NR 15 TC 0 Z9 0 U1 2 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2016 VL 118 IS 4 BP 636 EP 640 DI 10.4289/0013-8797.118.4.636 PG 5 WC Entomology SC Entomology GA EB9SX UT WOS:000387738500014 ER PT J AU Messmer, T Wiggenhauser, M Ortega, HE Albrecht, L Tschapka, M Wilcke, W AF Messmer, Tobias Wiggenhauser, Matthias Ortega, Hilario Espinosa Albrecht, Larissa Tschapka, Marco Wilcke, Wolfgang TI Base metal fluxes from fig trees to soil on Barro Colorado Island, Panama: potential contribution of the common frugivorous bat Artibeus jamaicensis SO BIOGEOCHEMISTRY LA English DT Article DE Artibeus jamaicensis; Canopy budget; Ficus insipida; Keystone species; Litterfall; Panama; Species-specific nutrient cycling; Tropical lowland forest ID TROPICAL RAIN-FOREST; DRY-SEASON IRRIGATION; NUTRIENT FLUXES; FRUIT CHARACTERISTICS; LITTER DECOMPOSITION; CANOPY HERBIVORES; DECIDUOUS FORESTS; THROUGHFALL; STEMFLOW; NITROGEN AB The contribution of animals to element fluxes in ecosystems is little known. We therefore estimated the contribution of a common frugivorous bat species (Phyllostomidae: Artibeus jamaicensis) to the base metal fluxes (Ca, Mg, and K) from fig trees to soil in a tropical lowland forest on Barro Colorado Island (BCI) because figs provide large parts of the Ca required by these mammals. We chose three individual old-growth fig trees on each of four geological units of BCI varying in soil exchangeable base metal concentrations. To assess element fluxes, we determined internal base metal cycling via canopy exchange and litterfall, external input through bulk and dry deposition, and contributions of bats through pellets and bat faeces as well as element absorption in bats. Assuming a consumption of 20 % of the total fig production by A. jamaicensis, total mean fluxes from fig trees to soil were 24 +/- 7 g m(-2) year(-1) for Ca, 4.6 +/- 1.6 for Mg, and 21 +/- 4 for K, respectively. The largest part of Ca and Mg was cycled as bulk litterfall (79 +/- 9 and 62 +/- 15 %, respectively) and of K as canopy leaching (56 +/- 12 %). A. jamaicensis contributed 1.7 +/- 0.5, 2.3 +/- 0.6, and 6.1 +/- 1.8 % to the total fluxes of Ca, Mg and K under fig trees, respectively. The contribution of A. jamaicensis to the base metal fluxes below the fig canopy was similar to that of bulk deposition. Our results demonstrate that the contribution of a single frugivorous mammal species to internal base metal cycling in a tropical ecosystem may be similarly important as bulk deposition and can have measurable effects on local soil fertility. C1 [Messmer, Tobias] Univ Bern, Inst Geog, Hallerstr 12, CH-3012 Bern, Switzerland. [Wiggenhauser, Matthias] Swiss Fed Inst Technol, Inst Agr Sci, Eschikon 33, CH-8315 Lindau, Switzerland. [Ortega, Hilario Espinosa; Tschapka, Marco] Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Panama. [Albrecht, Larissa; Tschapka, Marco] Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, Albert Einstein Allee 11, D-89069 Ulm, Germany. [Wilcke, Wolfgang] KIT, Inst Geog & Geoecol, Reinhard Baumeister Pl 1, D-76131 Karlsruhe, Germany. RP Wilcke, W (reprint author), KIT, Inst Geog & Geoecol, Reinhard Baumeister Pl 1, D-76131 Karlsruhe, Germany. EM wolfgang.wilcke@kit.edu FU German Research Foundation (DFG) [Wi1601/14-1] FX This study was funded by the German Research Foundation (DFG, Wi1601/14-1). We thank Oris Acevedo and Belkys Jimenez for their organizational and logistical support on BCI, Graciela Valdespino and Karel Flores for field assistance and Inga Geipel for their helpful advices in the field on BCI. We are indebted to the Smithsonian Tropical Research Institute (STRI) for granting access to its research station and the Panamanian authorities (ANAM) for the export permits. NR 77 TC 0 Z9 0 U1 13 U2 13 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-2563 EI 1573-515X J9 BIOGEOCHEMISTRY JI Biogeochemistry PD OCT PY 2016 VL 130 IS 1-2 BP 13 EP 30 DI 10.1007/s10533-016-0236-2 PG 18 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA EB3OH UT WOS:000387274300002 ER PT J AU Lohmann, AC Evangelista, D Waldrop, LD Mah, CL Hedrick, TL AF Lohmann, Amanda C. Evangelista, Dennis Waldrop, Lindsay D. Mah, Christopher L. Hedrick, Tyson L. TI Covering Ground: Movement Patterns and Random Walk Behavior in Aquilonastra anomala Sea Stars SO BIOLOGICAL BULLETIN LA English DT Article ID CORRELATED RANDOM-WALK; LEVY WALK; FORAGING MOVEMENTS; FLIGHTS; ECHINODERMATA; DISTRIBUTIONS; ASTEROIDEA; PREDATOR; PHYTOPLANKTON; SUCCESS AB The paths animals take while moving through their environments affect their likelihood of encountering food and other resources; thus, models of foraging behavior abound. To collect movement data appropriate for comparison with these models, we used time-lapse photography to track movements of a small, hardy, and easy-to-obtain organism, Aquilonastra anomala sea stars. We recorded the sea stars in a tank over many hours, with and without a food cue. With food present, they covered less distance, as predicted by theory; this strategy would allow them to remain near food. We then compared the paths of the sea stars to three common models of animal movement: Brownian motion, Levy walks, and correlated random walks; we found that the sea stars' movements most closely resembled a correlated random walk. Additionally, we compared the search performance of models of Brownian motion, a Levy walk, and a correlated random walk to that of a model based on the sea stars' movements. We found that the behavior of the modeled sea star walk was similar to that of the modeled correlated random walk and the Brownian motion model, but that the sea star walk was slightly more likely than the other walks to find targets at intermediate distances. While organisms are unlikely to follow an idealized random walk in all details, our data suggest that comparing the effectiveness of an organism's paths to those from theory can give insight into the organism's actual movement strategy. Finally, automated optical tracking of invertebrates proved feasible, and A. anomala was revealed to be a tractable, 2D-movement study system. C1 [Lohmann, Amanda C.; Hedrick, Tyson L.] Univ North Carolina Chapel Hill, Dept Biol, Chapel Hill, NC 27599 USA. [Evangelista, Dennis] US Naval Acad, Dept Weap & Syst Engn, Annapolis, MD 21401 USA. [Waldrop, Lindsay D.] Univ Calif Merced, Div Nat Sci, Merced, CA 95343 USA. [Mah, Christopher L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Lohmann, AC (reprint author), Univ North Carolina Chapel Hill, Dept Biol, Chapel Hill, NC 27599 USA. EM alohmann@live.unc.edu FU Office of Naval Research [N0001410109452]; National Science Foundation [IOS 1253276] FX We thank L. Miller, the Miller Lab, and the Integrative Mathematical Physiology group at UNC for their advice and support of this project, and Jonathan Rader for assistance with the statistical analysis. This work was supported by the Office of Naval Research (grant no. N0001410109452 to TH and 8 others) and by the National Science Foundation (no. IOS 1253276 to TH). NR 47 TC 0 Z9 0 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0006-3185 EI 1939-8697 J9 BIOL BULL-US JI Biol. Bull. PD OCT PY 2016 VL 231 IS 2 BP 130 EP 141 PG 12 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA EB3IE UT WOS:000387256600005 PM 27820905 ER PT J AU Lawley, JW Ames, CL Bentlage, B Yanagihara, A Goodwill, R Kayal, E Hurwitz, K Collins, AG AF Lawley, Jonathan W. Ames, Cheryl Lewis Bentlage, Bastian Yanagihara, Angel Goodwill, Roger Kayal, Ehsan Hurwitz, Kikiana Collins, Allen G. TI Box Jellyfish Alatina alata Has a Circumtropical Distribution SO BIOLOGICAL BULLETIN LA English DT Article ID CNIDARIA CUBOZOA; LIFE-CYCLE; MAXIMUM-LIKELIHOOD; LARVAL DISPERSAL; SEQUENCE; PHYLOGENIES; EVOLUTION; SOFTWARE; IRUKANDJI; INSIGHTS AB Species of the box jellyfish (Cubozoa) genus Alatina are notorious for their sting along the beaches of several localities of the Atlantic and Pacific. These species include Alatina alata on the Caribbean Island of Bonaire (the Netherlands), A. moseri in Hawaii, and A. mordens in Australia. Most cubozoans inhabit coastal waters, but Alatina is unusual in that specimens have also been collected in the open ocean at great depths. Alatina is notable in that populations form monthly aggregations for spermcast mating in conjunction with the lunar cycle. Nominal species are difficult to differentiate morphologically, and it has been unclear whether they are distinct or a single species with worldwide distribution. Here we report the results of a population genetic study, using nuclear and mitochondrial sequence data from four geographical localities. Our analyses revealed a general lack of geographic structure among Alatina populations, and slight though significant isolation by distance. These data corroborate morphological and behavioral similarities observed in the geographically disparate localities, and indicate the presence of a single, pantropically distributed species, Alatina alata. While repeated, human-mediated introductions of A. alata could explain the patterns we have observed, it seems more likely that genetic metapopulation cohesion is maintained via dispersal through the swimming medusa stage, and perhaps via dispersal of encysted planulae, which are described here for the first time in Alatina. C1 [Lawley, Jonathan W.] Univ Fed Santa Catarina, Dept Ecol & Zool, BR-88040970 Florianopolis, SC, Brazil. [Lawley, Jonathan W.; Ames, Cheryl Lewis; Bentlage, Bastian; Kayal, Ehsan; Collins, Allen G.] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Ames, Cheryl Lewis] Univ Maryland, Grad Sch Biol Sci, College Pk, MD 20742 USA. [Yanagihara, Angel] Univ Hawaii Manoa, John A Burns Sch Med, Dept Trop Med Med Microbiol & Pharmacol, Honolulu, HI 96822 USA. [Goodwill, Roger; Hurwitz, Kikiana] Brigham Young Univ Hawaii, Dept Biol, Laie, HI 96792 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, NOAA,Fisheries Serv, Washington, DC 20013 USA. RP Lawley, JW (reprint author), Univ Fed Santa Catarina, Dept Ecol & Zool, BR-88040970 Florianopolis, SC, Brazil.; Lawley, JW (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. EM jonathan.lawley@yahoo.com.br RI Lawley, Jonathan/S-5825-2016 OI Lawley, Jonathan/0000-0003-1267-5294 FU Brigham Young University-Hawaii Student Associateship Research Fund; Yamagata Foundation; Biology Department Student Mentored Research Fund FX Geoff Keel and the rest of the collections staff of the Department of Invertebrate Zoology at the Smithsonian NMNH are gratefully acknowledged for assistance in working with specimens. This work would not have been possible without the generous support of Rita Peachey and staff of CIEE Bonaire; citizen scientists Bud Gillan, Johan van Blerk, and Arjen van Dorsten; and the cooperation of the staff of STINAPA Bonaire. We also acknowledge Julia Souza's assistance, from the Marine Biodiversity Lab at UFSC, for phylogeographic analysis. Much of this work was performed using resources of the Laboratories of Analytical Biology at the Smithsonian NMNH. Saipan research was financially supported by the Brigham Young University-Hawaii Student Associateship Research Fund, Yamagata Foundation, and Biology Department Student Mentored Research Fund. Collection support by BYU-Hawaii students include Sheung Ting, Abigail Smith, Haley Sorenson-Pruitt, Tavaiilau Lueli, and Teylon Wilson. NR 112 TC 0 Z9 0 U1 6 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0006-3185 EI 1939-8697 J9 BIOL BULL-US JI Biol. Bull. PD OCT PY 2016 VL 231 IS 2 BP 152 EP 169 PG 18 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA EB3IE UT WOS:000387256600007 PM 27820907 ER PT J AU Abernethy, EF Turner, KL Beasley, JC DeVault, TL Pitt, WC Rhodes, OE AF Abernethy, Erin F. Turner, Kelsey L. Beasley, James C. DeVault, Travis L. Pitt, William C. Rhodes, Olin E., Jr. TI Carcasses of invasive species are predominantly utilized by invasive scavengers in an island ecosystem SO ECOSPHERE LA English DT Article DE cane toads; cannibalism; carrion; ecosystem function; Hawai'i; invasive species; mongoose; scavenging ID UNGULATE CARCASSES; AVIAN SCAVENGERS; CARRION; DECOMPOSITION; IMPACTS; SUCCESSION; PREDATORS; AUSTRALIA; NITROGEN; BIOLOGY AB Invasive species have significantly affected ecosystems, particularly islands, and species invasions continue with increasing globalization. Largely unstudied, the influence of invasive species on island ecosystem functions, especially scavenging and decomposition, could be substantive. Quantifying carcass utilization by different scavengers and shifts in community dynamics in the presence of invasive animals is of particular interest for understanding impacts on nutrient recycling. Invasive species could benefit greatly from carcass resources within highly invaded island ecosystems, through increased invasion success and population growth, subsequently exacerbating their impacts on native species. We quantified how experimentally placed invasive amphibian, reptile, small mammal, and bird carcasses were utilized by vertebrate and invertebrate scavengers on the Big Island of Hawai'i in three island habitats: a barren lava field, a vegetated lava field, and a rainforest. We used camera traps to record vertebrate scavengers removing carcasses and elapsed time until removal. We evaluated differences in scavenging between vertebrates and invertebrates and within the vertebrate community across different habitats and carcass types. Despite the small carcass sizes (<1 kg) used in this study, 55% of carcasses were removed by vertebrate scavengers, all invasive: mongoose, rodents, cats, pigs, and a common myna. Our data indicate that invasive vertebrate scavengers in this island ecosystem are highly efficient at assimilating a range of carrion resources across a variety of habitats. Carcasses of invasive animals could contribute substantially to energy budgets of other invasive vertebrate species. This may be a critical component contributing to successful invasions especially on islands and subsequent impacts on ecosystem function. C1 [Abernethy, Erin F.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Abernethy, Erin F.; Turner, Kelsey L.; Beasley, James C.; Rhodes, Olin E., Jr.] Univ Georgia, Savannah River Ecol Lab, Aiken, SC 29802 USA. [Turner, Kelsey L.; Beasley, James C.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [DeVault, Travis L.] USDA APHIS, Natl Wildlife Res Ctr, Sandusky, OH 44870 USA. [Pitt, William C.] USDA APHIS, Natl Wildlife Res Ctr, Hilo, HI 96720 USA. [Abernethy, Erin F.] Oregon State Univ, Dept Integrat Biol, Corvallis, OR 97331 USA. [Pitt, William C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Abernethy, EF (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA.; Abernethy, EF (reprint author), Univ Georgia, Savannah River Ecol Lab, Aiken, SC 29802 USA.; Abernethy, EF (reprint author), Oregon State Univ, Dept Integrat Biol, Corvallis, OR 97331 USA. EM efabernethy@gmail.com FU University of Georgia Research Foundation; USDA NWRC Hilo Field Station [12-7415-0936-CA]; US Department of Energy [DE-FC09-07SR22506]; agency of the US Government FX We appreciate the field assistance of Shem Unger. We sincerely thank Kelton Kotake, Bob Sugihara, Dean Foster, Tom McAuliffe, and Aaron Shiels at the USDA National Wildlife Research Center Hilo Field Station for making this study possible. We thank Hawai'i Volcanoes National Park and the Natural Area Reserve System of HI DLNR for giving us a location and permit to conduct our study. This work was supported through Cooperative Agreements among the University of Georgia Research Foundation, the USDA NWRC Hilo Field Station (No. 12-7415-0936-CA), and the US Department of Energy (No. DE-FC09-07SR22506). This paper was prepared as an account of work sponsored by an agency of the US Government. Neither the US Government nor any agency thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise does not necessarily constitute or imply its endorsement, recommendation, or favoring by the US Government or any agency thereof. The views and opinions of authors expressed herein do not necessarily state or reflect those of the US Government or any agency thereof. NR 61 TC 0 Z9 0 U1 15 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD OCT PY 2016 VL 7 IS 10 AR e01496 DI 10.1002/ecs2.1496 PG 15 WC Ecology SC Environmental Sciences & Ecology GA EB2TU UT WOS:000387216300034 ER PT J AU Thompson, JR Lambert, KF Foster, DR Broadbent, EN Blumstein, M Zambrano, AMA Fan, YC AF Thompson, Jonathan R. Lambert, Kathleen F. Foster, David R. Broadbent, Eben N. Blumstein, Meghan Zambrano, Angelica M. Almeyda Fan, Yuanchao TI The consequences of four land-use scenarios for forest ecosystems and the services they provide SO ECOSPHERE LA English DT Article DE ecosystem services; land use; scenarios; socio-ecological futures ID CLIMATE-CHANGE; MASSACHUSETTS; CONSERVATION; SIMULATION; BIOMASS; BIODIVERSITY; OWNERSHIPS; MANAGEMENT; MODEL; ROAD AB Anticipating landscape-to regional-scale impacts of land use on ecosystems and the services they provide is a central challenge for scientists, policymakers, and resource managers. Working with a panel of practitioners and regional experts, we developed and analyzed four plausible but divergent land-use scenarios that depict the future of Massachusetts from 2010 to 2060 to address two questions: (1) "How do the magnitude and spatial distribution of ecosystem service provisioning vary under the different land-use regimes?" and (2) "What are the synergies and trade-offs among direct human uses, ecosystem services, and habitat quality?" Each scenario specifies the detailed prescriptions for the major uses of the forests, including conversion to residential and commercial development, clearing new farmland, shifting silvicultural practices, and designating forests protected from development. We simulated the land-use scenarios and their interactions with anticipated climate change by coupling statistical models of land use to the LANDIS-II landscape model and then evaluated the outcomes in terms of the magnitude and spatial distribution of (1) direct human uses of the landscape (residential and commercial development, agricultural, timber harvest), (2) ecosystem services (carbon storage, flood regulation, nutrient retention), and (3) habitat quality (forest tree species composition, interior forest habitat). Across all scenarios, conflicts occurred between dispersed residential development and the supply of ecosystem services and habitat quality. In all but the scenario that envisioned a significant agricultural expansion, forest growth resulted in net increases in aboveground carbon storage, despite the concomitant forest clearing and harvesting. One scenario, called Forests as Infrastructure, showed the potential for synergies between increased forest harvest volume through the sustainable practices that encouraged the maintenance of economically and ecologically important tree species, and carbon storage. This scenario also showed trade-offs between development density and water quantity and quality at the watershed scale. The process of integrated scenario analysis led to important insights for land managers and policymakers in a populated forested region where there are tensions among development, forest harvesting, and land conservation. More broadly, the results emphasize the need to consider the consequences of contrasting land-use regimes that result from the interactions between human decisions and spatially heterogeneous landscape dynamics. C1 [Thompson, Jonathan R.; Lambert, Kathleen F.; Foster, David R.; Blumstein, Meghan] Harvard Univ, Harvard Forest, 324 North Main St, Petersham, MA 01366 USA. [Thompson, Jonathan R.; Broadbent, Eben N.; Blumstein, Meghan; Zambrano, Angelica M. Almeyda; Fan, Yuanchao] Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22360 USA. RP Thompson, JR (reprint author), Harvard Univ, Harvard Forest, 324 North Main St, Petersham, MA 01366 USA.; Thompson, JR (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22360 USA. EM jthomps@fas.harvard.edu FU NSF Long Term Ecological Research Grant [DEB-1237491]; Highstead Foundation FX We thank our expert panel for their commitment and patience: Kathy Baskin, Director of the Office of Water Policy, Mass Executive office of Energy and Environmental Affairs; Stephanie Cooper, Chief of Staff, Department of Conservation and Recreation; Andrew Finton, Massachusetts Director of Conservation Science, The Nature Conservancy; Kurt Gaertner, Smart Growth/Smart Energy, Mass Executive Office of Energy and Environmental Affairs; Jim Levitt, Director of The Program On Conservation Innovation; Robert O'Connor, Director of Land and Forests, Mass Executive Office of Energy and Environmental Affairs; Robert Perschel, Northeast Region Director, Forest Guild; Lisa Vernegaard, Vice President for Sustainability, The Trustees of Reservations. We also thank the Office of Geographic Information (MassGIS) for curating and disseminating the state's valuable environmental data, without which studies such as this would be impossible. We thank Matthew Duveneck and Luca Morreale for technical help and reviews of this manuscript. Thanks to O2 designs for help with Fig. 1. Funding was provided by an NSF Long Term Ecological Research Grant to Harvard Forest (DEB-1237491) and the Highstead Foundation. NR 46 TC 0 Z9 0 U1 27 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD OCT PY 2016 VL 7 IS 10 AR e01469 DI 10.1002/ecs2.1469 PG 22 WC Ecology SC Environmental Sciences & Ecology GA EB2TU UT WOS:000387216300011 ER PT J AU Schmidt, JA Jacob, DJ Horowitz, HM Hu, L Sherwen, T Evans, MJ Liang, Q Suleiman, RM Oram, DE Le Breton, M Percival, CJ Wang, S Dix, B Volkamer, R AF Schmidt, J. A. Jacob, D. J. Horowitz, H. M. Hu, L. Sherwen, T. Evans, M. J. Liang, Q. Suleiman, R. M. Oram, D. E. Le Breton, M. Percival, C. J. Wang, S. Dix, B. Volkamer, R. TI Modeling the observed tropospheric BrO background: Importance of multiphase chemistry and implications for ozone, OH, and mercury SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE halogen; troposphere; ozone; mercury; modeling; GEOS-Chem ID MARINE BOUNDARY-LAYER; SEA-SALT AEROSOLS; BROMINE CHEMISTRY; GLOBAL OBSERVATIONS; HALOGEN CHEMISTRY; IODINE CHEMISTRY; NORTH-ATLANTIC; GEOS-CHEM; IN-SITU; CONSTRAINTS AB Aircraft and satellite observations indicate the presence of ppt (pptpmol/mol) levels of BrO in the free troposphere with important implications for the tropospheric budgets of ozone, OH, and mercury. We can reproduce these observations with the GEOS-Chem global tropospheric chemistry model by including a broader consideration of multiphase halogen (Br-Cl) chemistry than has been done in the past. Important reactions for regenerating BrO from its nonradical reservoirs include HOBr+Br-/Cl- in both aerosols and clouds, and oxidation of Br- by ClNO3 and ozone. Most tropospheric BrO in the model is in the free troposphere, consistent with observations and originates mainly from the photolysis and oxidation of ocean-emitted CHBr3. Stratospheric input is also important in the upper troposphere. Including production of gas phase inorganic bromine from debromination of acidified sea salt aerosol increases free tropospheric Br-y by about 30%. We find HOBr to be the dominant gas-phase reservoir of inorganic bromine. Halogen (Br-Cl) radical chemistry as implemented here in GEOS-Chem drives 14% and 11% decreases in the global burdens of tropospheric ozone and OH, respectively, a 16% increase in the atmospheric lifetime of methane, and an atmospheric lifetime of 6months for elemental mercury. The dominant mechanism for the Br-Cl driven tropospheric ozone decrease is oxidation of NOx by formation and hydrolysis of BrNO3 and ClNO3. C1 [Schmidt, J. A.; Jacob, D. J.; Hu, L.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Schmidt, J. A.] Univ Copenhagen, Dept Chem, Copenhagen, Denmark. [Jacob, D. J.; Horowitz, H. M.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Sherwen, T.; Evans, M. J.] Univ York, Dept Chem, WACL, York, N Yorkshire, England. [Liang, Q.] NASA, Goddard Space Flight Ctr, Lab Atmospher Chem & Dynam, Greenbelt, MD USA. [Suleiman, R. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Oram, D. E.] Univ East Anglia, Ctr Oceanog & Atmospher Sci, Natl Ctr Atmospher Sci, Norwich, Norfolk, England. [Le Breton, M.; Percival, C. J.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Ctr Atmospher Sci, Manchester, Lancs, England. [Wang, S.] Univ Michigan, Dept Chem, Ann Arbor, MI 48109 USA. [Wang, S.; Dix, B.; Volkamer, R.] Univ Colorado Boulder, Dept Chem & Biochem, Boulder, CO USA. [Wang, S.; Volkamer, R.] Univ Colorado Boulder, Cooperat Inst Res Environm Sci, Boulder, CO USA. RP Schmidt, JA (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA.; Schmidt, JA (reprint author), Univ Copenhagen, Dept Chem, Copenhagen, Denmark. EM schmidt@chem.ku.dk RI Volkamer, Rainer/B-8925-2016; Liang, Qing/B-1276-2011; Chem, GEOS/C-5595-2014; OI Volkamer, Rainer/0000-0002-0899-1369; Sherwen, Tomas/0000-0002-3006-3876; Hu, Lu/0000-0002-4892-454X; Evans, Mathew John/0000-0003-4775-032X FU Danish Council for Independent Research/Natural Sciences; NASA Atmospheric Composition Modeling and Analysis Program; National Science Foundation (NSF) [AGS-1104104]; NSF; Fulbright Junior Research Award; NOAA Climate Program Office FX J.A.S. acknowledges support from the Danish Council for Independent Research/Natural Sciences. This work was supported by the NASA Atmospheric Composition Modeling and Analysis Program (grants to D.J.J. and Q.L.). We acknowledge Eric Apel and the TORERO Science Team. The TORERO project is funded by the National Science Foundation (NSF) under award AGS-1104104 (Principal Investigator: R.V.). The involvement of the NSF-sponsored Lower Atmospheric Observing Facilities, managed and operated by the National Center for Atmospheric Research Earth Observing Laboratory, is acknowledged. S.W. is a recipient of the Fulbright Junior Research Award. We acknowledge the CAST Science Team. We acknowledge C. Brenninkmeijer, A. Rauthe-Schoech, and the CARIBIC Science Team. We acknowledge E. Atlas, S. Montzka, and the HIPPO Science Team. NOAA flask measurements onboard the HIPPO missions were provided by S. Montzka, F. Moore, B. Miller, C. Sweeney, and J. Elkins and were supported in part by NOAA Climate Program Office's AC4 program. GEOS-Chem is available to the community through the standard GEOS-Chem repository www.geos-chem.org. Model output from the simulations described above are available upon request (schmidt@chem.ku.dk). Observational data from the TORERO campaign is available to the community through http://www.eol.ucar.edu/node/4527. NR 65 TC 7 Z9 7 U1 9 U2 9 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD OCT PY 2016 VL 121 IS 19 BP 11819 EP 11835 DI 10.1002/2015JD024229 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA EA9PK UT WOS:000386976100017 ER PT J AU Gao, P Plavchan, P Gagne, J Furlan, E Bottom, M Anglada-Escude, G White, R Davison, CL Beichman, C Brinkworth, C Johnson, J Ciardi, D Wallace, K Mennesson, B von Braun, K Vasisht, G Prato, L Kane, SR Tanner, A Crawford, TJ Latham, D Rougeot, R Geneser, CS Catanzarite, J AF Gao, Peter Plavchan, P. Gagne, J. Furlan, E. Bottom, M. Anglada-Escude, G. White, R. Davison, C. L. Beichman, C. Brinkworth, C. Johnson, J. Ciardi, D. Wallace, K. Mennesson, B. von Braun, K. Vasisht, G. Prato, L. Kane, S. R. Tanner, A. Crawford, T. J. Latham, D. Rougeot, R. Geneser, C. S. Catanzarite, J. TI Retrieval of Precise Radial Velocities from Near-infrared High-resolution Spectra of Low-mass Stars SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article DE methods: data analysis; planets and satellites: detection; techniques: radial velocities ID M-DWARFS; GAS CELL; ECHELLE SPECTROGRAPH; DETECTING PLANETS; ABSORPTION CELLS; GIANT PLANET; PHOTON NOISE; BROWN DWARF; M4 DWARF; SEARCH AB Given that low-mass stars have intrinsically low luminosities at optical wavelengths and a propensity for stellar activity, it is advantageous for radial velocity (RV) surveys of these objects to use near-infrared (NIR) wavelengths. In this work, we describe and test a novel RV extraction pipeline dedicated to retrieving RVs from low-mass stars using NIR spectra taken by the CSHELL spectrograph at the NASA Infrared Telescope Facility, where a methane isotopologue gas cell is used for wavelength calibration. The pipeline minimizes the residuals between the observations and a spectral model composed of templates for the target star, the gas cell, and atmospheric telluric absorption; models of the line-spread function, continuum curvature, and sinusoidal fringing; and a parameterization of the wavelength solution. The stellar template is derived iteratively from the science observations themselves without a need for separate observations dedicated to retrieving it. Despite limitations from CSHELL's narrow wavelength range and instrumental systematics, we are able to (1) obtain an RV precision of 35 m s(-1) for the RV standard star GJ 15 A over a time baseline of 817 days, reaching the photon noise limit for our attained signal-to-noise ratio; (2) achieve similar to 3 m s(-1) RV precision for the M giant SV Peg over a baseline of several days and confirm its long-term RV trend due to stellar pulsations, as well as obtain nightly noise floors of similar to 2-6 m s(-1); and (3) show that our data are consistent with the known masses, periods, and orbital eccentricities of the two most massive planets orbiting GJ 876. Future applications of our pipeline to RV surveys using the next generation of NIR spectrographs, such as iSHELL, will enable the potential detection of super-Earths and mini-Neptunes in the habitable zones of M dwarfs. C1 [Gao, Peter] CALTECH, Div Geol & Planetary Sci, MC 150-21,1200 East Calif Blvd, Pasadena, CA 91125 USA. [Plavchan, P.; Geneser, C. S.] Missouri State Univ, Dept Phys, 901 S Natl Ave, Springfield, MO 65897 USA. [Gagne, J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Furlan, E.; Beichman, C.; Brinkworth, C.; Ciardi, D.] CALTECH, NASA Exoplanet Sci Inst, 770 S Wilson Ave, Pasadena, CA 91125 USA. [Bottom, M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Anglada-Escude, G.] Queen Mary Univ London, Sch Phys & Astron, 327 Mile End Rd, London E1 4NS, England. [Anglada-Escude, G.] Univ Hertfordshire, Ctr Astrophys Res, Coll Lane, Hatfield AL10 9AB, Herts, England. [White, R.; Davison, C. L.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Brinkworth, C.] Natl Ctr Atmospher Res, POB 3000, Boulder, CO 80307 USA. [Johnson, J.; Latham, D.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Wallace, K.; Mennesson, B.; Vasisht, G.; Crawford, T. J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91125 USA. [von Braun, K.; Prato, L.] Lowell Observ, West Mars Hill Rd, Flagstaff, AZ 86001 USA. [Kane, S. R.] San Francisco State Univ, Dept Phys & Astron, 1600 Holloway Ave, San Francisco, CA 94132 USA. [Tanner, A.] Mississippi State Univ, Dept Phys & Astron, Hilbun Hall, Starkville, MS 39762 USA. [Rougeot, R.] ESA, European Space Res & Technol Ctr, Noordwijk Binnen, Provincie Zuid, Netherlands. [Catanzarite, J.] NASA Ames Res Ctr, MS 245-3,POB 1, Moffett Field, CA 94035 USA. RP Gao, P (reprint author), CALTECH, Div Geol & Planetary Sci, MC 150-21,1200 East Calif Blvd, Pasadena, CA 91125 USA. EM pgao@caltech.edu OI Gao, Peter/0000-0002-8518-9601; Anglada Escude, Guillem/0000-0002-3645-5977; Ciardi, David/0000-0002-5741-3047 FU JPL Research and Technology Development Grant; JPL Center for Exoplanet Science; Venus Express program via NASA [NNX10AP80G]; University of Washington; California Institute of Technology [NNH12ZDA002C]; [NNA13AA93A] FX We thank K. Sung, S. Crawford, B. Drouin, E. Garcia-Berrios, N.S. Lewis, S. Mills, and S. Lin for their effort in the building and setting up of the methane isotopologue gas cell. We thank B. Walp for his help with data collection at NASA IRTF. We thank J. Rayner, L. Bergknut, B. Bus, and the telescope operators at NASA IRTF for their help throughout this project. This work uses observations obtained at NASA IRTF through program numbers 2010B022, 2011A083, 2011B083, and 2012B021. This work was supported in part by a JPL Research and Technology Development Grant and the JPL Center for Exoplanet Science. Additional support includes the Venus Express program via NASA NNX10AP80G grant to the California Institute of Technology, and an NAI Virtual Planetary Laboratory grant from the University of Washington to the Jet Propulsion Laboratory and California Institute of Technology under solicitation NNH12ZDA002C and cooperative agreement number NNA13AA93A. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 77 TC 2 Z9 2 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD OCT PY 2016 VL 128 IS 968 AR 104501 DI 10.1088/1538-3873/128/968/104501 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EB1LN UT WOS:000387113500005 ER PT J AU Jander, KC Herre, EA AF Jander, K. Charlotte Herre, Edward Allen TI Host sanctions in Panamanian Ficus are likely based on selective resource allocation SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE coevolution; cooperation; Ficus; fig wasp; Moraceae; mutualism; partner choice; pollination; resource allocation; sanctions; species interaction ID FIG-WASP MUTUALISM; PREFERENTIAL ALLOCATION; MYCORRHIZAL MUTUALISM; POLLINATING WASPS; PARTNER CHOICE; COOPERATION; EVOLUTION; STABILITY; SYMBIONTS; RHIZOBIA AB PREMISE OF THE STUDY: Fig trees and their pollinators, fig wasps, present a powerful model system for studying mutualism stability: both partners depend on each other for reproduction, cooperation levels can be manipulated, and the resulting field-based fitness quantified. Previous work has shown that fig trees can severely reduce the fitness of wasps that do not pollinate by aborting unpollinated figs or reducing the number and size of wasp off spring. Here we evaluated four hypotheses regarding the mechanism of sanctions in four Panamanian fig species. METHODS: We examined wasp and fig samples from field experiments with manipulated levels of pollination. KEY RESULTS: In unpollinated figs, the fig wall and the wasp off spring had a lower dry mass. Unpollinated figs had as many initiated wasp galls as pollinated figs but fewer galls that successfully produced live wasp off spring. Across three experimentally increasing levels of pollination, we found nonlinear increases in fig wall mass, the proportion of wasp galls that develop, and wasp mass. CONCLUSIONS: Our data did not support the hypotheses that lack of pollination prevents gall formation or that fertilized endosperm is required for wasp development. While our data are potentially consistent with the hypothesis that trees produce a wasp-specific toxin in response to lack of pollination, we found the hypothesis that sanctions are a consequence of trees allocating more resources to better-pollinated figs more parsimonious with the aggregate data. Our findings are completely analogous to the selective resource allocation to more beneficial tissues documented in other mutualistic systems. C1 [Jander, K. Charlotte] Harvard Univ, Dept Organism & Evolutionary Biol, Level 4 MCZ Labs,26 Oxford St, Cambridge, MA 02138 USA. [Jander, K. Charlotte] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Herre, Edward Allen] Smithsonian Trop Res Inst, Unit 9100 Box 0948, Dpo, AA 34002 USA. RP Jander, KC (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, Level 4 MCZ Labs,26 Oxford St, Cambridge, MA 02138 USA.; Jander, KC (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. EM cjander@oeb.harvard.edu FU Yale University; Wenner-Gren foundations; Smithsonian Tropical Research Institute FX The authors thank Lena Berg, Daniel Castle, Ethan Cheng, Lovisa Duck, Adalberto Gomez, Tiff any Hsu, Bonnie Lau, Maritza Lopez, and Ara Vehian for assistance in the field and laboratory. The authors thank Jim Leebens-Mack and three anonymous reviewers for insightful comments that improved the manuscript. The authors thank Yale University and the Wenner-Gren foundations for funding (K.C.J.), and the Smithsonian Tropical Research Institute for funding (K.C.J., A.E.H.) and for maintaining the research site that made this study possible. NR 50 TC 2 Z9 2 U1 8 U2 8 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 EI 1537-2197 J9 AM J BOT JI Am. J. Bot. PD OCT PY 2016 VL 103 IS 10 BP 1753 EP 1762 DI 10.3732/ajb.1600082 PG 10 WC Plant Sciences SC Plant Sciences GA EA6TJ UT WOS:000386761600006 PM 27562207 ER PT J AU Perez, DM Christy, JH Backwell, PRY AF Perez, Daniela M. Christy, John H. Backwell, Patricia R. Y. TI Choosing a mate in a high predation environment: Female preference in the fiddler crab Uca terpsichores SO ECOLOGY AND EVOLUTION LA English DT Article DE courtship; sensory trap; male location; male quality; wave display; drumming display ID CLAW-WAVING DISPLAY; SEXUAL SELECTION; SENSORY BIAS; SIGNAL EVOLUTION; VISUAL ECOLOGY; COURTSHIP; CHOICE; BEHAVIOR; ANNULIPES; ATTRACTIVENESS AB The interplay between a receiver's sensory system and a sender's courtship signals is fundamental to the operation of sexual selection. Male courtship signals that match a female receiver's preexisting perceptual biases can be favored yet the message they communicate is not always clear. Do they simply beacon the male's location or also indicate his quality? We explored this question in a species of fiddler crab Uca terpsichores that courts under elevated predation risk and that mates and breeds underground in the safety of males' burrows. Sexually receptive females leave their own burrows and are thereby exposed to avian predators as they sequentially approach several courting males before they choose one. Males court by waving their single greatly enlarge claw and sometimes by building a sand hood next to their burrow entrance. Hoods are attractive because they elicit a risk-reducing orientation behavior in females, and it has been suggested that claw waving may also serve primarily to orient the female to the male. If the wave communicates male quality, then females should discriminate mates on the basis of variation in elements of the wave, as has been shown for other fiddler crabs. Alternatively, variation in elements of the claw waving display may have little effect on the display's utility as a beacon of the location of the male and his burrow. We filmed courting males and females under natural conditions as females responded to claw waving and chose mates. Analysis of the fine-scale courtship elements between the males that females rejected and those they chose revealed no differences. When predation risk during courtship is high, males' courtship displays may serve primarily to guide females to safe mating and breeding sites and not as indicators of male quality apart from their roles as beacons. C1 [Perez, Daniela M.; Backwell, Patricia R. Y.] Australian Natl Univ, Res Sch Biol, Canberra, ACT, Australia. [Christy, John H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Perez, DM (reprint author), Australian Natl Univ, Res Sch Biol, Div Evolut Ecol & Genet, Canberra, ACT, Australia. EM daniela.perez@anu.edu.au FU ARC [DP 120101427] FX ARC Discovery Grant, Grant/Award Number: DP 120101427; NR 59 TC 0 Z9 0 U1 18 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD OCT PY 2016 VL 6 IS 20 BP 7443 EP 7450 DI 10.1002/ece3.2510 PG 8 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA EA2NA UT WOS:000386429200026 ER PT J AU Smith, JB Turner, KL Beasley, JC DeVault, TL Pitt, WC Rhodes, OE AF Smith, Joshua B. Turner, Kelsey L. Beasley, James C. DeVault, Travis L. Pitt, William C. Rhodes, Olin E., Jr. TI Brown tree snake (Boiga irregularis) population density and carcass locations following exposure to acetaminophen SO ECOTOXICOLOGY LA English DT Article DE Acetaminophen; Carcass location; Brown tree snake; Indirect toxicant transfer; Scavenging ID RESOURCE PULSES; GUAM; ISLAND; TREESNAKES; CARRION; DECOMPOSITION; SCAVENGERS; REPTILIA; EFFICACY; IMPACTS AB Mass aerial delivery of dead mouse baits treated with acetaminophen has been evaluated as a means to reduce brown tree snake (Boiga irregularis) populations over large areas, increasing the likelihood of wide-scale eradication on Guam. Given the high density of snakes in some areas of their invasive range, eradication efforts could result in a resource pulse that may influence food web dynamics and the indirect transport of acetaminophen among trophic levels. We evaluated abundance, habitat type, and snake size (i.e., age) within two study sites on Guam, a secondary limestone forest (upland) and an abandoned coconut plantation (coastal), to determine how experimentally dosing snakes with acetaminophen is likely to influence carrion availability. We found snakes trapped in 3.24 ha plots occurred in greater abundance (population size = 72.5 snakes; SE = 8.8) and were significantly larger (978.6 mm, SE = 14.9) in the coastal than in the upland site (population size = 26.9, SE = 21.5; length = 903.0 mm, SE = 15.9). Despite these differences, carcasses of snakes that died after consuming acetaminophen-laced mice (80 mg) were recovered in consistent locations between sites, with 92 % located on the ground, 4 % in trees, and 4 % found in rock cavities at both sites. Given that most snakes were found on the ground rather than in the tree canopy, our results suggest that many poisoned snake carcasses will be accessible to a wide range of potential scavengers, possibly influencing food web dynamics and potentially contributing to indirect toxicant transfer within affected ecosystems. C1 [Smith, Joshua B.; Turner, Kelsey L.; Beasley, James C.; Rhodes, Olin E., Jr.] Savannah River Ecol Lab, PO Drawer E, Aiken, SC 29802 USA. [Turner, Kelsey L.; Beasley, James C.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [DeVault, Travis L.] USDA, Natl Wildlife Res Ctr, 6100 Columbus Ave, Sandusky, OH USA. [Pitt, William C.] Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. [Rhodes, Olin E., Jr.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. RP Smith, JB (reprint author), Savannah River Ecol Lab, PO Drawer E, Aiken, SC 29802 USA. EM jsmith77@uga.edu FU University of Georgia Research Foundation; United Stated Department of the Navy via the United States Department of Agriculture National Wildlife Research Center [14-7439-1099-CA]; United States Department of Energy [DE-FC09-07SR22506] FX We thank M. Hall, S. Mosher, D. Lujan, and the staff at the United States Department of Agriculture Wildlife Service Andersen Air Force Base, Guam for logistical support and capture assistance. This work was supported through Cooperative Agreements between the University of Georgia Research Foundation and the United Stated Department of the Navy via the United States Department of Agriculture National Wildlife Research Center (No. 14-7439-1099-CA) and the United States Department of Energy (No. DE-FC09-07SR22506). NR 51 TC 0 Z9 0 U1 10 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0963-9292 EI 1573-3017 J9 ECOTOXICOLOGY JI Ecotoxicology PD OCT PY 2016 VL 25 IS 8 BP 1556 EP 1562 DI 10.1007/s10646-016-1711-1 PG 7 WC Ecology; Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA EA6BU UT WOS:000386710800010 PM 27604786 ER PT J AU Kramina, TE Degtjareva, GV Samigullin, TH Valiejo-Roman, CM Kirkbride, JH Volis, S Deng, T Sokoloff, DD AF Kramina, Tatiana E. Degtjareva, Galina V. Samigullin, Tahir H. Valiejo-Roman, Carmen M. Kirkbride, Joseph H., Jr. Volis, Sergei Deng, Tao Sokoloff, Dmitry D. TI Phylogeny of Lotus (Leguminosae: Loteae): Partial incongruence between nrITS, nrETS and plastid markers and biogeographic implications SO TAXON LA English DT Article DE 5 ' ETS; biogeography; Dorycnium; ITS; Leguminosae; Lotus; molecular phylogeny; psbA-trnH; rps16 Mediterranean ID DISPERSAL-VICARIANCE ANALYSIS; NUCLEAR RIBOSOMAL DNA; CONCERTED EVOLUTION; CHLOROPLAST DNA; RETICULATE EVOLUTION; CORNICULATUS L; FABACEAE; SEQUENCES; ORIGIN; TREES AB Lotus comprises ca. 130 species of herbs, semishrubs and shrubs native to the Old World, including important pasture crops and a model legume, L. japonicus. Earlier nrITS-based phylogenies were incongruent with all taxonomic classifications of the genus. In particular, members of the former genus Dorycnium were unexpectedly placed near species of L. sect. Lotus. The primary goal of the present study is to explore whether the unexpected placement of members of sect. Lotus and the former genus Dorycnium in earlier phylogenetic studies resulted from (1) insufficient taxon sampling and/or (2) the use of only one DNA marker. The rooting of the Lotus phylogeny, its major clades and basic biogeographic patterns are also discussed. This is the first global phylogenetic study of Lotus that uses both plastid and nuclear markers. The nrITS region was analyzed in 155 ingroup specimens representing 98 species of Lotus. Sequences of nrITS, nrETS, psbA-trnH spacer and rps16 intron were analyzed for 70 ingroup specimens representing 54 species. The placement of the segregate genera Dorycnium and Tetragonolobus in the synonymy of Lotus was confirmed. Analyses of plastid data strongly supported a basal split of Lotus into two clades, one comprising species of sect. Lotus plus those traditionally placed in Dorycnium and the other including the rest of the species. The former clade has a centre of species diversity in Europe and N Asia, and the latter in Macaronesia, Africa and S Asia. Only the "Southern" clade is resolved in analyses of nrITS and nrETS data. Trees inferred from plastid, nrITS and nrETS data shared the occurrence of several smaller clades corresponding to traditionally recognized infrageneric taxa or species groups as well as the occurrence of some well-supported clades that differ from traditional taxonomic concepts. Several instances of incongruence were documented between nuclear and plastid markers and between the two nuclear markers, possibly resulting from reticulate evolution. The extant geographic patterns of Lotus are likely biased by at least one round of area fragmentation followed by expansion coupled with extensive speciation associated with the complex history of the Mediterranean biome. C1 [Kramina, Tatiana E.; Sokoloff, Dmitry D.] Lomonosov Moscow State Univ, Fac Biol, Dept Higher Plants, GSP 1, Moscow 119234, Russia. [Degtjareva, Galina V.] Lomonosov Moscow State Univ, Bot Garden, Fac Biol, GSP 1, Moscow 119234, Russia. [Samigullin, Tahir H.; Valiejo-Roman, Carmen M.] Lomonosov Moscow State Univ, AN Belozersky Inst Physicochem Biol, GSP 1, Moscow 119991, Russia. [Kirkbride, Joseph H., Jr.] Smithsonian Inst, Dept Bot, NMNH MRC 166,POB 37012, Washington, DC 20013 USA. [Volis, Sergei; Deng, Tao] Chinese Acad Sci, Kunming Inst Bot, Key Lab Plant Divers & Biogeog East Asia, Kunming 650201, Peoples R China. RP Kramina, TE (reprint author), Lomonosov Moscow State Univ, Fac Biol, Dept Higher Plants, GSP 1, Moscow 119234, Russia. EM tkramina@yandex.ru RI Samigullin, Tahir/K-1347-2013 FU Russian Foundation for Basic Research [14-04-01094, 09-04-01323]; Russian Science Foundation (RNF) [14-50-00029] FX We are indebted to the curators of all herbaria whose material was studied. The research was supported by grants from the Russian Foundation for Basic Research, projects 14-04-01094 (data assembling for section Lotus) and 09-04-01323 (data assembling for other sections). Phylogenetic analyses and analyses of congruence of tree topologies were supported by the Russian Science Foundation (RNF), grant #14-50-00029, "Scientific basis of the national biobank-depository of the living systems" (branch "Plants"). We are grateful to S.R. Majorov and M.S. Nuraliev for the photographs used in Fig. 1, to J. Francisco-Ortega and two anonymous reviewers for their helpful comments and to D.F. Lyskov for discussions on biogeography. NR 101 TC 0 Z9 0 U1 8 U2 8 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD OCT PY 2016 VL 65 IS 5 BP 997 EP 1018 DI 10.12705/655.4 PG 22 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA EA4QE UT WOS:000386597600004 ER PT J AU Pace, MR Zuntini, AR Lohmann, LG Angyalossy, V AF Pace, Marcelo R. Zuntini, Alexandre R. Lohmann, Lucia G. Angyalossy, Veronica TI Phylogenetic relationships of enigmatic Sphingiphila (Bignoniaceae) based on molecular and wood anatomical data SO TAXON LA English DT Article DE Bignonieae; cambial variants; chaco; liana; perforated ray cells; Tabebuia alliance; Tecomeae ID BIGNONIEAE BIGNONIACEAE; NEOTROPICAL LIANAS; MIXED MODELS; EVOLUTION; CLASSIFICATION; GENUS AB Sphingiphila is a monospecific genus, endemic to the Bolivian and Paraguayan Chaco, a semi-arid lowland region. The circumscription of Sphingiphila has been controversial since the genus was first described. Sphingiphila tetramera is perhaps the most enigmatic taxon of Bignoniaceae due to the presence of very unusual morphological features, such as simple leaves, thorn-tipped branches, and tetramerous, actinomorphic flowers, making its tribal placement within the family uncertain. Here we combined molecular and wood anatomical data to determine the placement of Sphingiphila within the family. The analyses of a large ndhF dataset, which included members of all Bignoniaceae tribes, placed Sphingiphila within Bignonieae. A second, smaller ndhF and pepC dataset, which included only members of tribe Bignonieae, placed the genus within Tanaecium. Unlike most macro-morphological traits, Sphingiphila is not unusual within Bignoniaceae from a wood anatomical point of view. Sphingiphila shares the presence of narrow vessels and vasicentric to aliform confluent parenchyma with the rest of the family. In addition, Sphingiphila has several specific wood anatomical traits, such as vessels in a diagonal to tangential arrangement, small intervessel pits, and non-storied heterocellular rays with occasional perforated ray cells. These features suggest that the genus is best placed either in Tecomeae s.str. or Bignonieae, with a better placement in Bignonieae due to its abundant parenchyma, despite lacking the cambial variant synapomorphic for this group. Sphingiphila and Tanaecium form a clade that is strongly supported by molecular characters, including two indels that are molecular synapomorphies of this clade. In addition, careful morphological inspections show that S. tetramera shares with Tanaecium the subulate, bromeliad-like prophylls, the most evident synapomorphy of this genus apart from long, tubular, villose corollas, and a lepidote ovary. Given the molecular phylogenetic placement of S. tetramera and its macro-morphological and wood anatomical similarities with Tanaecium, we propose the new combination Tanaecium tetramerum. C1 [Pace, Marcelo R.; Zuntini, Alexandre R.; Lohmann, Lucia G.; Angyalossy, Veronica] Univ Sao Paulo, Inst Biociencias, Dept Bot, Rua Matao 277, BR-05508090 Sao Paulo, SP, Brazil. [Pace, Marcelo R.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. [Zuntini, Alexandre R.] Univ Estadual Campinas, Inst Biol, Dept Biol Vegetal, Rua Monteiro Lobato 255, BR-13083970 Campinas, SP, Brazil. RP Pace, MR (reprint author), Univ Sao Paulo, Inst Biociencias, Dept Bot, Rua Matao 277, BR-05508090 Sao Paulo, SP, Brazil.; Pace, MR (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. EM marcelorpace@yahoo.com.br RI Zuntini, Alexandre/C-6764-2013 OI Zuntini, Alexandre/0000-0003-0705-8902 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [481034/2007-2, 486971/2012-0]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2011/50859-2, 2012/50260-6, 2012/01099-8, 2013/09160-5, 2013/10679-0]; CNPq [307781/2013-5, 308441/2012-5]; Peter Buck fellowship at the Smithsonian Institution FX We are very grateful to Daniel Villavoel and Luzmilla Arroyo for their support during fieldwork in Bolivia; Alex Wiedenhoeft, Mike Wiemann and Regis Miller from the Forest Products Laboratory in Madison (Wisconsin) for allowing us to study the wood slide collection hosted in that Institute; Richard Olmstead and an anonymous reviewer for valuable suggestions on the manuscript; Dewey Litwiller for English editing; the Missouri Botanical Garden for allowing us to extract DNA from a Herbarium specimen (Antezana Valera 1327) and use images of Tanaecium caudiculatum from TROPICOS; Beatriz Gomes for kindly providing images of Tanaecium jaroba. Funds for this study were provided by the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, grants 481034/2007-2; 486971/2012-0) and Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP, grants 2011/50859-2; 2012/50260-6; 2012/01099-8; 2013/09160-5; 2013/10679-0). LGL and VA are supported by CNPq 307781/2013-5 and 308441/2012-5, respectively and MRP is supported by the Peter Buck fellowship at the Smithsonian Institution. NR 47 TC 0 Z9 0 U1 5 U2 5 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD OCT PY 2016 VL 65 IS 5 BP 1050 EP 1063 DI 10.12705/655.7 PG 14 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA EA4QE UT WOS:000386597600007 ER PT J AU Gostel, M Barker, K AF Gostel, Morgan Barker, Katharine TI GGI-GARDENS: PRESERVING GLOBAL PLANT DIVERSITY SO TAXON LA English DT Editorial Material C1 [Gostel, Morgan] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Barker, Katharine] Smithsonian Inst, Global Genome Initiat & Global Genome Biodivers N, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Gostel, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. EM gostelm@si.edu; barkerk@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD OCT PY 2016 VL 65 IS 5 BP 1217 EP 1218 DI 10.12705/655.44 PG 2 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA EA4QE UT WOS:000386597600043 ER PT J AU Massaro, F Crespo, NA D'Abrusco, R Landoni, M Masetti, N Ricci, F Milisavljevic, D Paggi, A Chavushyan, V Jimenez-Bailon, E Patino-Alvarez, V Strader, J Chomiuk, L La Franca, F Smith, HA Tosti, G AF Massaro, F. Crespo, N. Alvarez D'Abrusco, R. Landoni, M. Masetti, N. Ricci, F. Milisavljevic, D. Paggi, A. Chavushyan, V. Jimenez-Bailon, E. Patino-Alvarez, V. Strader, J. Chomiuk, L. La Franca, F. Smith, Howard A. Tosti, G. TI The gamma-ray blazar quest: new optical spectra, state of art and future perspectives SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE Galaxies: active; Galaxies: BL Lacertae objects; Quasars: general; Surveys; Radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; BL LACERTAE OBJECTS; FERMI UNASSOCIATED SOURCES; 2ND SOURCE CATALOG; X-RAY; SPECTROSCOPIC OBSERVATIONS; UNCERTAIN TYPE; LAT CATALOG; 1ST SURVEY AB We recently developed a procedure to recognize gamma-ray blazar candidates within the positional uncertainty regions of the unidentified/unassociated gamma-ray sources (UGSs). Such procedure was based on the discovery that Fermi blazars show peculiar infrared colors. However, to confirm the real nature of the selected candidates, optical spectroscopic data are necessary. Thus, we performed an extensive archival search for spectra available in the literature in parallel with an optical spectroscopic campaign aimed to reveal and confirm the nature of the selected gamma-ray blazar candidates. Here, we first search for optical spectra of a selected sample of gamma-ray blazar candidates that can be potential counterparts of UGSs using the Sloan Digital Sky Survey (SDSS DR12). This search enables us to update the archival search carried out to date. We also describe the state-of-art and the future perspectives of our campaign to discover previously unknown gamma-ray blazars. C1 [Massaro, F.; Crespo, N. Alvarez] Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy. [Massaro, F.; Crespo, N. Alvarez] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [D'Abrusco, R.] Univ Napoli Federico II, Dept Phys Sci, Via Cinthia 9, I-80126 Naples, Italy. [Landoni, M.; Smith, Howard A.] INAF Osservatorio Astron Brera, Via Emilio Bianchi 46, I-23807 Merate, Italy. [Masetti, N.] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy. [Masetti, N.] Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile. [Ricci, F.; La Franca, F.] Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00146 Rome, Italy. [Milisavljevic, D.; Paggi, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Chavushyan, V.; Patino-Alvarez, V.] Inst Nacl Astrofis Opt & Electr, Apartado Postal 51-216, Puebla 72000, Mexico. [Jimenez-Bailon, E.] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 877, Ensenada 22800, Baja California, Mexico. [Strader, J.; Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. RP Massaro, F (reprint author), Univ Turin, Dipartimento Fis, Via Pietro Giuria 1, I-10125 Turin, Italy.; Massaro, F (reprint author), Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. EM f.massaro@unito.it OI Massaro, Francesco/0000-0002-1704-9850; La Franca, Fabio/0000-0002-1239-2721 FU Programma Giovani Ricercatori - Rita Levi Montalcini - Rientro dei Cervelli; Italian Ministry of Education, Universities and Research (MIUR); NASA [NNX12AO97G, NNX13AP20G]; ASI/INAF [I/005/12/0]; NASA/JPL [NNX14AJ61G]; UNAM; CONACyT (Mexico) [151494]; NASA's Goddard Space Flight Center; National Aeronautics and Space Administration; National Science Foundation; U.S. Department of Energy Office of Science; Astrophysical Research Consortium; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We thank the anonymous referee for useful comments that led to improvements in the paper. F.M. gratefully acknowledges the financial support of the Programma Giovani Ricercatori - Rita Levi Montalcini - Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). This investigation is supported by the NASA grants NNX12AO97G and NNX13AP20G. The work by G. Tosti is supported by the ASI/INAF contract I/005/12/0. H.A. Smith acknowledges partial support from NASA/JPL grant NNX14AJ61G. H. Oti-Floranes is funded by a postdoctoral UNAM grant. V. Chavushyan acknowledges funding by CONACyT research grant 151494 (Mexico). We thank the staff at the Observatorio Astronomico Nacional in San Pedro M~rtir (Mexico) for all their help during the observation runs. We thank the staff of the Astronomical Observatory of Bologna in Loiano for their assistance during the observations. Part of this work is based on archival data, software or on-line services provided by the ASI Science Data Center. This research has made use of data obtained from the high-energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasbourg, France; the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This research has made use of the USNOFS Image and Catalogue Archive operated by the United States Naval Observatory, Flagstaff Station (http://www. nofs.navy.mil/data/fchpix/). TOPCAT2 (Taylor 2005) for the preparation and manipulation of the tabular data and the images.; The Aladin Java applet3 was used to create the finding charts reported in this paper (Bonnarel et al. 2000). It can be started from the CDS (Strasbourg - France), from the CFA (Harvard - USA), from the ADAC (Tokyo - Japan), from the IUCAA (Pune - India), from the UKADC (Cambridge - UK), or from the CADC (Victoria - Canada). NR 86 TC 1 Z9 1 U1 1 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X EI 1572-946X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD OCT PY 2016 VL 361 IS 10 AR 337 DI 10.1007/s10509-016-2926-6 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA EA1NW UT WOS:000386360000016 ER PT J AU Zabin, CJ Wasson, K Fork, S AF Zabin, Chela J. Wasson, Kerstin Fork, Susanne TI Restoration of native oysters in a highly invaded estuary SO BIOLOGICAL CONSERVATION LA English DT Article DE Invasive species; Ostrea lurida; Restoration design; Stress gradient; Tidal elevation ID LURIDA CARPENTER 1864; BIOLOGICAL INVASIONS; OLYMPIA OYSTER; ENVIRONMENTAL-STRESS; HABITAT RESTORATION; EVALUATING PERFORMANCE; PRAIRIE RESTORATION; COMPETITIVE CONTROL; TOPSOIL REMOVAL; CALIFORNIA AB Restoration of native species may be hampered by competition with non-native species. The outcomes of competition are often context-dependent, with one species dominating under some conditions but not others. Where non-natives differ from natives in their ability to tolerate stressful environmental conditions, restoration practitioners may be able to manipulate conditions or strategically locate restoration projects along naturally occurring stress gradients to favor native species. We tested the responses of native oysters and a suite of non-native sessile invertebrate species (mostly soft-bodied organisms) to varying tidal elevations, shoreline types, and distances from source populations. Cover of non-natives was lower at higher tidal elevation and far from adult populations. Native oyster recruitment was also reduced at the high tidal elevation. At this elevation oyster dominance was increased, but abundance was reduced. To test an adaptive management approach, we moved substrates from the low to high tidal elevations. Cover of non-natives had decreased dramatically one year later, while oyster metrics were unaffected or improved compared to those on substrates remaining at the low elevation. Our study indicates that reduction of non-native species abundance, often an explicit goal of restoration, may be achieved by strategic location of restoration units, although abundance of target species may also be reduced, at least over the short term. However, restoration practitioners may be able to increase abundance of target species and reduce non-natives by applying stress differentially over time, with benign conditions during sensitive early life stages, and increasing stress after target organisms become more tolerant. Published by Elsevier Ltd. C1 [Zabin, Chela J.] Smithsonian Environm Res Ctr, 3152 Paradise Dr, Tiburon, CA 94920 USA. [Zabin, Chela J.] Univ Calif Davis, Environm Sci & Policy Dept, 1 Shields Ave, Davis, CA 95616 USA. [Wasson, Kerstin; Fork, Susanne] Elkhorn Slough Natl Estuarine Res Reserve, 1700 Elkhorn Rd, Watsonville, CA 95076 USA. [Wasson, Kerstin] Univ Calif Santa Cruz, Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. RP Zabin, CJ (reprint author), Smithsonian Environm Res Ctr, 3152 Paradise Dr, Tiburon, CA 94920 USA.; Zabin, CJ (reprint author), Univ Calif Davis, Environm Sci & Policy Dept, 1 Shields Ave, Davis, CA 95616 USA. EM zabinc@si.edu; kerstin.wasson@gmail.com; skfork@gmail.com FU California Department of Fish and Wildlife's Environmental Enhancement Fund; NOAA's Office for Coastal Management FX We gratefully acknowledge primary funding from California Department of Fish and Wildlife's Environmental Enhancement Fund and a grant from NOAA's Office for Coastal Management to the Elkhorn Slough Foundation on behalf of the Elkhorn Slough National Estuarine Research Reserve. We thank Joel Fodrie and three anonymous reviewers for helpful suggestions on this manuscript. We also thank the numerous staff and volunteers who helped collect shells, made and deployed shell necklaces and assisted us with monitoring, including: Miguel Rodriguez, Shirley Murphy, Ron Eby, Gabi Estill, John Haskins, Zachary Kaufman, Lorena Paras, Laura Gray, Dean Robbins, Carrie Stevenson, Darah Wallsten, Alger Omongos, Kristy Whiteson, Inger Marie Laursen, Daniel Vee Lewis, Margie Kay, Amanda Peters, Laura Mehner, Beth Gillespie. We thank Blu Forman and Charlie Endris for preparation of figures. NR 65 TC 0 Z9 0 U1 7 U2 7 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD OCT PY 2016 VL 202 BP 78 EP 87 DI 10.1016/j.biocon.2016.08.026 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA EA0ZP UT WOS:000386318400009 ER PT J AU Wright, SJ Calderon, O Hernandez, A Detto, M Jansen, PA AF Wright, S. Joseph Calderon, Osvaldo Hernandez, Andres Detto, Matteo Jansen, Patrick A. TI Interspecific associations in seed arrival and seedling recruitment in a Neotropical forest SO ECOLOGY LA English DT Article DE anemochory; Barro Colorado Island; contagious seed dispersal; fruiting phenology; seed production; seed rain; seedling recruitment; zoochory ID TROPICAL FOREST; FRUITING PHENOLOGIES; DISPERSAL PATTERNS; VIROLA-CALOPHYLLA; TREES; CONSEQUENCES; BIRDS; LIMITATION; DIVERSITY; WIND AB Contagious seed dispersal refers to the tendency for some sites to receive many dispersed seeds while other sites receive few dispersed seeds. Contagious dispersal can lead to interspecific associations in seed arrival, and this in turn might lead to interspecific associations in seedling recruitment. We evaluate the extent of spatially contagious seed arrival, the frequency of positive interspecific associations in seed arrival, and their consequences for seedling recruitment at the community level in a tropical moist forest. We quantified seed arrival to 200 passive seed traps for 28yr of weekly censuses and seedling recruitment to 600 1-m(2) quadrats for 21yr of annual censuses on Barro Colorado Island, Panama. We assessed whether spatially contagious seed dispersal was more important among zoochorous species than among anemochorous species, increased in importance with similarity in fruiting times, and led to interspecific associations in seed arrival and seedling recruitment. We controlled adult seed source associations statistically to evaluate predicted relationships. We found that spatially contagious seed arrival was widespread among zoochorous species, but also occurred among anemochorous species when the strong, consistent trade winds were present. Significant interspecific associations in seed arrival were more likely for pairs of species with zoochorous seeds and similar fruiting times and persisted through seedling recruitment. Thus, interspecifically contagious seed dispersal affects local species composition and alters the mixture of interspecific interactions through the seed, germination, and early seedling stages in this forest. Future investigations should consider the implications of interspecific association at the regeneration stages documented here for later life stages and species coexistence. C1 [Wright, S. Joseph; Calderon, Osvaldo; Hernandez, Andres; Detto, Matteo; Jansen, Patrick A.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, Wageningen, Netherlands. RP Wright, SJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. EM wrightsj@si.edu FU Environmental Sciences Program of the Smithsonian Institution; STRI; U.S. National Science Foundation FX Seed and seedling censuses were funded by the Environmental Sciences Program of the Smithsonian Institution. The forest dynamics plot was founded by S. P. Hubbell and R. B. Foster and is now managed by R. Condit, S. Lao, and R. Perez for the Center for Tropical Forest Science and the Smithsonian Tropical Research Institute (STRI). Numerous organizations provided funding, principally STRI and the U.S. National Science Foundation, and hundreds of field workers have contributed. NR 51 TC 0 Z9 0 U1 17 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD OCT PY 2016 VL 97 IS 10 BP 2780 EP 2790 DI 10.1002/ecy.1519 PG 11 WC Ecology SC Environmental Sciences & Ecology GA DZ7ZQ UT WOS:000386088000024 PM 27859106 ER PT J AU Reeder-Myers, L Rick, T Lowery, D Wah, J Henkes, G AF Reeder-Myers, Leslie Rick, Torben Lowery, Darrin Wah, John Henkes, Gregory TI HUMAN ECOLOGY AND COASTAL FORAGING AT FISHING BAY, MARYLAND, USA SO JOURNAL OF ETHNOBIOLOGY LA English DT Article DE Chesapeake Bay; historical ecology; coastal archaeology; shell midden analysis; eastern oyster ID CHESAPEAKE BAY; ATLANTIC COAST; HOLOCENE CLIMATE; MIDDLE ATLANTIC; SHELL MIDDENS; ICE-AGE; EUTROPHICATION; VARIABILITY; HISTORY; CHRONOLOGIES AB Chesapeake Bay is the largest estuary in the United States and is famous for its once extensive and now severely degraded eastern oyster (Crassostrea virginica) populations, along with a number of other important fisheries including crabs, rockfish, and menhaden. Here we explore the historical ecology of Native American subsistence and land use strategies in the Fishing Bay area of Maryland's Eastern Shore, building on our broader bay-wide analyses of oyster fisheries and human-environmental interactions. Archaeological analysis of faunal remains from shell middens dated between AD 500 to 1500, along with analysis of locally collected modern oysters, help reconstruct Fishing Bay's evolution during the late Holocene, and document shellfish harvest strategies and predation pressure. These data suggest a stable and sustainable prehistoric oyster fishery in Fishing Bay, likely due to: 1) seasonal harvest and local consumption; 2) intertidal harvest that allowed replenishment from subtidal populations; and 3) relatively low human population densities. When placed in the context of our broader bay-wide analysis, these data provide implications for managing the present day oyster fishery, lending support to increasing no-take zones and expanding oyster sanctuaries that can be rotated with areas actively being fished. C1 [Reeder-Myers, Leslie; Rick, Torben] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, Washington, DC 20013 USA. [Lowery, Darrin] Chesapeake Watershed Archaeol Res Fdn, Tempe, AZ USA. [Wah, John] Matapeake Soil & Environm Consultants, Shippensburg, PA USA. [Henkes, Gregory] Harvard Univ, Hoffman Lab G9, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Reeder-Myers, L (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Dept Anthropol, Washington, DC 20013 USA. EM reeder-myersL@si.edu FU Restricted Endowment Grant from the Smithsonian Institution FX Our work at Fishing Bay was supported by a Restricted Endowment Grant from the Smithsonian Institution awarded to Torben Rick. We thank Charlie Hall and the Maryland Historical Trust, as well as the Fishing Bay Wildlife Management Area for facilitating our permits and access to the Fishing Bay archaeological sites. Thanks to Chris Wolff, Edgar Alarcon, Courtney Hofman, Frances Seay, and Kelin Flanagan for help in the field, and Sheel Jagani, Daniel Weller, Jennifer Eliot, Elaine Hall, and Carina Reich for help in the laboratory. Finally, we thank Lisa Nagaoka and Steve Wolverton for inviting us to contribute to this special issue of the Journal of Ethnobiology, and four anonymous reviewers for their valuable comments on the manuscript. NR 66 TC 0 Z9 0 U1 2 U2 2 PU SOC ETHNOBIOLOGY PI DENTON PA UNIV NORTH TEXAS, DEPT GEOGRAPHY, 1155 UNION CIRCLE 305279, DENTON, TX 76203-5017 USA SN 0278-0771 EI 2162-4496 J9 J ETHNOBIOL JI J. Ethnobiol. PD OCT PY 2016 VL 36 IS 3 BP 595 EP 616 PG 22 WC Anthropology; Biology SC Anthropology; Life Sciences & Biomedicine - Other Topics GA DZ8RL UT WOS:000386138600008 ER PT J AU Leasi, F Gaynus, C Mahardini, A Moore, TN Norenburg, JL Barber, PH AF Leasi, Francesca Gaynus, Camille Mahardini, Angka Moore, Tiara N. Norenburg, Jon L. Barber, Paul H. TI Spatial and ecologic distribution of neglected microinvertebrate communities across endangered ecosystems: meiofauna in Bali (Indonesia) SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE LA English DT Article DE Biodiversity; coral reef; Coral Triangle; microscopic organisms; sand flat; seagrass ID SOUTHEAST-ASIAN BIODIVERSITY; MALDIVES INDIAN-OCEAN; 6TH MASS EXTINCTION; MARINE BIODIVERSITY; CONSERVATION PRIORITIES; TROPHIC RELATIONSHIPS; CLIMATE-CHANGE; DIVERSITY; SEA; SEDIMENTS AB Biodiversity estimations, particularly in vulnerable tropical regions, are essential to understanding ecosystem structure, function and conservation. While threats to marine and terrestrial ecosystems have fueled increased interest in biodiversity research, information on meiofauna, a key trophic and ecologic community of microscopic organisms that lives within sediments, is still lacking. Here we report the results of a faunistic investigation conducted in Bali, Indonesia. The results reveal that the biodiversity of marine meiofauna in Bali is very high. Meiofauna from coral reefs, sand flats and seagrass beds differed significantly in abundance and diversity. Nonetheless, overall community compositions show that meiofauna communities are affected by environmental variables. The high meiofaunal diversity observed in Bali, a low diversity region of the Coral Triangle, indicates the importance of further meiofaunal research across this region and across a broader diversity of habitats. The data presented provide an important baseline for future studies on biodiversity conservation in the face of environmental changes due to anthropogenic impacts and/or natural events. C1 [Leasi, Francesca; Norenburg, Jon L.] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, 1000 Constitut Ave NW, Washington, DC 20560 USA. [Gaynus, Camille; Barber, Paul H.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90024 USA. [Mahardini, Angka] Indonesian Biodivers Res Ctr, Denpasar, Bali, Indonesia. [Moore, Tiara N.] Old Dominion Univ, Dept Ocean Earth & Atmospher Sci, Norfolk, VA USA. RP Leasi, F (reprint author), Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, 1000 Constitut Ave NW, Washington, DC 20560 USA. EM leasif@si.edu RI LEASI, FRANCESCA/E-4361-2017 FU National Science Foundation - Partnerships for International Research and Education (Office of International Science and Engineering) [1243541]; United States Agency for International Development [497-A-00-10-00008-00]; University of California - Historically Black Colleges and Universities Program FX This work was conducted as part of international education programs funded by National Science Foundation - Partnerships for International Research and Education (Office of International Science and Engineering - 1243541), United States Agency for International Development (to Cooperative Agreement No. 497-A-00-10-00008-00) and the University of California - Historically Black Colleges and Universities Program. We thank the Indonesian Biodiversity Research Center, Bali Dive Academy and T. Sari for logistical support, and State Ministry of Research and Technology and the government of Indonesia for research permits (185/SIP/RFP/SM/VI/2013). Thanks to W. Meyers in the Department of Ocean, Earth and Atmospheric Sciences at Old Dominion University for help with the grain-size analysis, and to A. G. Collins (Smithsonian Institution) and M. A. Todaro (Modena and Reggio Emila University, Italy) for their helpful comments on an early version of the manuscript. We are exceedingly grateful to G. Hunt (Smithsonian Institution) for his invaluable suggestions on the statistical analyses, and M. V. SOrensen (Natural History Museum of Denmark) for identifying the taxonomy of kinorhynchs. M. V. SOrensen and an anonymous reviewer greatly improved an advanced version of the manuscript. The author contributions were as follows: F.L. led the meiofauna educational program in Bali, carried out sorting and identification of organisms, designed the experiment, performed the data and statistical analyses and wrote the manuscript. C.G., A.M. and T.M.N. designed the project along with F.L., and collected and sorted samples. T.M.N. undertook the granulometric sorting. J.L.N. provided funding support for F.L. and provided the equipment used in the field. P.H.B. wrote the grants and directed the educational programs that supported this work, assisted with field logistics, obtained research permits and contributed to the writing of the manuscript. NR 85 TC 0 Z9 0 U1 6 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0173-9565 EI 1439-0485 J9 MAR ECOL-EVOL PERSP JI Mar. Ecol.-Evol. Persp. PD OCT PY 2016 VL 37 IS 5 BP 970 EP 987 DI 10.1111/maec.12305 PG 18 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DZ4MC UT WOS:000385831800004 ER PT J AU Alvarado, JJ Cortes, J Guzman, H Reyes-Bonilla, H AF Jose Alvarado, Juan Cortes, Jorge Guzman, Hector Reyes-Bonilla, Hector TI Bioerosion by the sea urchin Diadema mexicanum along Eastern Tropical Pacific coral reefs SO MARINE ECOLOGY-AN EVOLUTIONARY PERSPECTIVE LA English DT Article DE Bioaccretion; bioerosion; coral cover; coral framework; rugosity; sea urchin size ID CALCIUM-CARBONATE BUDGETS; LAGOONS FRENCH-POLYNESIA; 1982-1983 EL-NINO; COSTA-RICA; ECHINOID BIOEROSION; COMMUNITY STRUCTURE; CAULERPA-SERTULARIOIDES; DISTRIBUTION PATTERNS; SCLERACTINIAN CORALS; POPULATION-DENSITY AB Bioerosion is a natural process in coral reefs. It is fundamental to the health of these ecosystems. In the Eastern Tropical Pacific (ETP) coral reefs, the most important bioeroders are sponges, bivalves, sea urchins and the fish Arothron meleagris. In the 1980s, El Nino caused high coral mortality and an increase in macroalgal growth. As a result, greater sea urchin bioerosion occurred. This weakened the reef framework. Considering the high vulnerability of the ETP coral reefs, the goal of this study was to determine the current bioerosion impact of the sea urchin Diadema mexicanum along the western coasts of Mexico, El Salvador, Costa Rica and Panama. The balance between coral bioaccretion and sea urchin bioerosion was also calculated. Between 2009 and 2010, in 12 coral reefs localities, D.mexicanum density, bottom cover and rugosity were quantified along band transects. The daily bioerosion rate was obtained from the amount of carbonates evacuated by sea urchins per unit time. The rate of coral accretion was calculated by multiplying the coral growth rate of the dominant genus by the density of their skeleton and by their specific coral cover. The localities were dissimilar (R=0.765, P<0.001) in terms of live coral cover, crustose calcareous algae, turf cover, rugosity index, and density and size of D.mexicanum. At all sites, with the exception of Bahia Culebra (Costa Rica), coral bioerosion was less than coral bioaccretion. Diadema mexicanum plays a dominant role in the balance of carbonates in the ETP, but this depends on reef condition (protection, overfishing, eutrophication) and so the impacts can be either positive or negative. C1 [Jose Alvarado, Juan; Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, Ciudad Invest, San Jose 115012060, Costa Rica. [Jose Alvarado, Juan; Cortes, Jorge] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. [Guzman, Hector] Smithsonian Trop Res Inst, Balboa, Panama. [Reyes-Bonilla, Hector] Univ Autonoma Baja California Sur, Dept Biol Marina, La Paz, Mexico. RP Alvarado, JJ (reprint author), Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, Ciudad Invest, San Jose 115012060, Costa Rica. EM juan.alvarado@ucr.ac.cr FU Vicerrectoria de Investigacion of the Universidad de Costa Rica; Ministerio de Ciencia y Tecnologia de Costa Rica; Consejo Nacional para Investigaciones Cientificas y Tecnologicas de Costa Rica; Consejo Nacional de Ciencia y Tecnologia de Mexico; Fonds Francais pour l'Environnement Mondial; Ecodesarrollo Papagayo and Grupo Adelante FX We acknowledge the following persons and institutions that collaborated during the development of this work: C. Fernandez, O. Breedy, C. Sanchez, S. Martinez, E. Gomez, A. Planas, V. Flores, O. Norzagaray, L. E. Calderon-Aguilera, A. Ayala, J. Carrion, L. Hernandez, G. Ramirez, V. Vargas, J. Ramirez, the Bezy, Sanchez-Camacho and Garcia-Zuniga families, Centro de Investigacion en Ciencias del Mar y Limnologia (Universidad de Costa Rica), Universidad Autonoma de Baja California Sur, the personnel of the 'Laboratorio de Sistemas Arrecifales', Centro de Investigaciones en Ciencias Marinas, Universidad de Guadalajara, Centro de Investigacion Cientifica y Educacion Superior de Ensenada, Universidad del Mar, Ministerios del Ambiente y Recursos Naturales from El Salvador, Universidad de El Salvador, Smithsonian Tropical Research Institute, Liquid Jungle Lab, Charles Darwin Foundation, Hotel Pacifica, Mero Divers, Vallartec, Fundarrecife, the park rangers of Reserva Biologica Isla del Cano, Parque Nacional Isla del Coco and Parque Nacional Los Cobanos, MY Adventure crew, Instituto Costarricense de Turismo, Sistema Nacional de Areas de Conservacion from Costa Rica, Autoridad Nacional del Ambiente from Panama, Hotel Punta Marenco Lodge and aguila de Osa Inn. Special acknowledgements for their economic support are due to Vicerrectoria de Investigacion of the Universidad de Costa Rica, Ministerio de Ciencia y Tecnologia de Costa Rica, Consejo Nacional para Investigaciones Cientificas y Tecnologicas de Costa Rica, Consejo Nacional de Ciencia y Tecnologia de Mexico, Fonds Francais pour l'Environnement Mondial, Ecodesarrollo Papagayo and Grupo Adelante. Finally, we are grateful to M. Chavez for help with the graphs and to J. Lawrence for the English review and comments. We appreciate the comments of two anonymous reviewers who greatly improved this paper. NR 110 TC 0 Z9 0 U1 8 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0173-9565 EI 1439-0485 J9 MAR ECOL-EVOL PERSP JI Mar. Ecol.-Evol. Persp. PD OCT PY 2016 VL 37 IS 5 BP 1088 EP 1102 DI 10.1111/maec.12372 PG 15 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA DZ4MC UT WOS:000385831800015 ER PT J AU deVries, MS Stock, BC Christy, JH Goldsmith, GR Dawson, TE AF deVries, Maya S. Stock, Brian C. Christy, John H. Goldsmith, Gregory R. Dawson, Todd E. TI Specialized morphology corresponds to a generalist diet: linking form and function in smashing mantis shrimp crustaceans SO OECOLOGIA LA English DT Article DE Stomatopoda; Stable isotopes; Bayesian mixing model; Raptorial appendage; Feeding ecology ID ISOTOPE MIXING MODELS; STABLE-ISOTOPES; INDIVIDUAL SPECIALIZATION; ECOLOGICAL SPECIALIZATION; AGONISTIC BEHAVIOR; ADAPTIVE RADIATION; PRIOR INFORMATION; FRUGIVOROUS BATS; CLAW MORPHOLOGY; CICHLID FISH AB Many animals are considered to be specialists because they have feeding structures that are fine-tuned for consuming specific prey. For example, "smasher" mantis shrimp have highly specialized predatory appendages that generate forceful strikes to break apart hard-shelled prey. Anecdotal observations suggest, however, that the diet of smashers may include soft-bodied prey as well. Our goal was to examine the diet breadth of the smasher mantis shrimp, Neogonodactylus bredini, to determine whether it has a narrow diet of hard-shelled prey. We combined studies of prey abundance, feeding behavior, and stable isotope analyses of diet in both seagrass and coral rubble to determine if N. bredini's diet was consistent across different habitat types. The abundances of hard-shelled and soft-bodied prey varied between habitats. In feeding experiments, N. bredini consumed both prey types. N. bredini consumed a range of different prey in the field as well and, unexpectedly, the stable isotope analysis demonstrated that soft-bodied prey comprised a large proportion (29-53 %) of the diet in both habitats. Using a Bayesian mixing model framework (MixSIAR), we found that this result held even when we used uninformative, or generalist, priors and informative priors reflecting a specialist diet on hard-shelled prey and prey abundances in the field. Thus, contrary to expectation, the specialized feeding morphology of N. bredini corresponds to a broad diet of both hard-shelled and soft-bodied prey. Using multiple lines of study to describe the natural diets of other presumed specialists may demonstrate that specialized morphology often broadens rather than narrows diet breadth. C1 [deVries, Maya S.; Goldsmith, Gregory R.; Dawson, Todd E.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [deVries, Maya S.; Stock, Brian C.] Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr 0202, San Diego, CA 92093 USA. [Christy, John H.] Smithsonian Trop Res Inst, Naos Marine Labs, Panama City, Panama. [Goldsmith, Gregory R.] Paul Scherrer Inst, Ecosyst Fluxes Grp, Lab Atmospher Chem, CH-5232 Villigen, Switzerland. RP deVries, MS (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA.; deVries, MS (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr 0202, San Diego, CA 92093 USA. EM mdevries@ucsd.edu FU American Museum of Natural History Lerner-Gray Fund; Berkeley and National Sigma Xi Scientific Honors Society Grants-In-Aid-of-Research; Fulbright Student Research Grant; Society of Integrative and Comparative Biology Grants-In-Aid-of-Research; Smithsonian Tropical Research Institute's Short-Term Fellowship Award; UC Berkeley Department of Integrative Biology Endowment; UC Museum of Paleontology Graduate Student Research Award; National Science Foundation Integrative Organismal Systems Grant [1014573]; National Science Foundation Graduate Research Fellowship [DGE-1144086]; Phi Beta Kappa Graduate Fellowship FX We thank E. Gonzalez-Ulloa, F. Guerra, J. Morales, E. Staaterman, G. Thomas, T. Claverie, S. N. Patek, J. R. A. Taylor, R. L. Caldwell, D. Desmet, J. Hassen, A. Pickard, M. Limm, and M. E. Power and for assistance with study design, field work, and sample analysis. Fieldwork would not have been possible without I. Grenald and the staff at the Smithsonian Tropical Research Institute's Galeta Point Marine Laboratory. We also thank S. Beissinger, R. L. Caldwell, J. Harris, S. Mambelli, A. Roddy, B. X. Semmens, M. I. Shuldman, T. S. Tunstall, P. C. Wainwright, and especially S. N. Patek for insightful discussion about data analysis and for comments on this manuscript. We thank J. Wortham and two anonymous reviewers for thoughtful comments on the manuscript. We are grateful for the use of the photograph in Fig. 1 from R. L. Caldwell. We thank the Autoridad Nacional del Ambiente in Panama for granting permits for this research (spring SEX/A-88-08, fall SEX/A-133-08). Research was funded by the American Museum of Natural History Lerner-Gray Fund, the Berkeley and National Sigma Xi Scientific Honors Society Grants-In-Aid-of-Research, the Fulbright Student Research Grant, the Society of Integrative and Comparative Biology Grants-In-Aid-of-Research, the Smithsonian Tropical Research Institute's Short-Term Fellowship Award, the UC Berkeley Department of Integrative Biology Endowment, and the UC Museum of Paleontology Graduate Student Research Award (all awards to M. S. deVries), and a National Science Foundation Integrative Organismal Systems Grant (#1014573 to S. N. Patek). B. C. Stock was supported by the National Science Foundation Graduate Research Fellowship (DGE-1144086). Manuscript preparation was funded by the Phi Beta Kappa Graduate Fellowship (to M. S. deVries). NR 93 TC 2 Z9 2 U1 13 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD OCT PY 2016 VL 182 IS 2 BP 429 EP 442 DI 10.1007/s00442-016-3667-5 PG 14 WC Ecology SC Environmental Sciences & Ecology GA DW5FS UT WOS:000383669300010 PM 27312263 ER PT J AU Baldeck, CA Kembel, SW Harms, KE Yavitt, JB John, R Turner, BL Madawala, S Gunatilleke, N Gunatilleke, S Bunyavejchewin, S Kiratiprayoon, S Yaacob, A Supardi, MNN Valencia, R Navarrete, H Davies, SJ Chuyong, GB Kenfack, D Thomas, DW Dalling, JW AF Baldeck, C. A. Kembel, S. W. Harms, K. E. Yavitt, J. B. John, R. Turner, B. L. Madawala, S. Gunatilleke, N. Gunatilleke, S. Bunyavejchewin, S. Kiratiprayoon, S. Yaacob, A. Supardi, M. N. N. Valencia, R. Navarrete, H. Davies, S. J. Chuyong, G. B. Kenfack, D. Thomas, D. W. Dalling, J. W. TI Phylogenetic turnover along local environmental gradients in tropical forest communities SO OECOLOGIA LA English DT Article DE Center for tropical forest science; Distance-based redundancy analysis; Phylogenetic beta diversity; Phylogenetic community structure; Phylomatic ID BETA DIVERSITY; COMPREHENSIVE FRAMEWORK; HABITAT ASSOCIATIONS; NICHE CONSERVATISM; PLANT-COMMUNITIES; NEIGHBOR MATRICES; SPECIES-RICHNESS; TREE; EVOLUTION; TRAIT AB While the importance of local-scale habitat niches in shaping tree species turnover along environmental gradients in tropical forests is well appreciated, relatively little is known about the influence of phylogenetic signal in species' habitat niches in shaping local community structure. We used detailed maps of the soil resource and topographic variation within eight 24-50 ha tropical forest plots combined with species phylogenies created from the APG III phylogeny to examine how phylogenetic beta diversity (indicating the degree of phylogenetic similarity of two communities) was related to environmental gradients within tropical tree communities. Using distance-based redundancy analysis we found that phylogenetic beta diversity, expressed as either nearest neighbor distance or mean pairwise distance, was significantly related to both soil and topographic variation in all study sites. In general, more phylogenetic beta diversity within a forest plot was explained by environmental variables this was expressed as nearest neighbor distance versus mean pairwise distance (3.0-10.3 % and 0.4-8.8 % of variation explained among plots, respectively), and more variation was explained by soil resource variables than topographic variables using either phylogenetic beta diversity metric. We also found that patterns of phylogenetic beta diversity expressed as nearest neighbor distance were consistent with previously observed patterns of niche similarity among congeneric species pairs in these plots. These results indicate the importance of phylogenetic signal in local habitat niches in shaping the phylogenetic structure of tropical tree communities, especially at the level of close phylogenetic neighbors, where similarity in habitat niches is most strongly preserved. C1 [Baldeck, C. A.] Univ Illinois, Program Ecol Evolut & Conservat Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. [Baldeck, C. A.; Dalling, J. W.] Univ Illinois, Dept Plant Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. [Kembel, S. W.] Univ Quebec, Dept Sci Biol, CP 8888,Succ Ctr Ville, Montreal, PQ H3C 3P8, Canada. [Harms, K. E.] Louisiana State Univ, Dept Biol Sci, 202 Life Sci Bldg, Baton Rouge, LA 70803 USA. [Yavitt, J. B.] Cornell Univ, Dept Nat Resources, 16 Fernow Hall, Ithaca, NY 14853 USA. [John, R.] Indian Inst Sci Educ & Res, PO BCKV Campus Main Off, Nadia 741252, W Bengal, India. [Turner, B. L.; Davies, S. J.; Dalling, J. W.] Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. [Madawala, S.; Gunatilleke, N.; Gunatilleke, S.] Univ Peradeniya, Dept Bot, Fac Sci, Peradeniya 20400, Sri Lanka. [Bunyavejchewin, S.] Natl Parks Wildlife & Plant Conservat Dept, Bangkok 10900, Thailand. [Kiratiprayoon, S.] Thammasat Univ Rangsit, Fac Sci & Technol, Klongluang 12121, Patumtani, Thailand. [Yaacob, A.] Univ Teknol MARA, Fac Plantat & Agrotechnol, Shah Alam 40450, Selangor, Malaysia. [Supardi, M. N. N.] Forest Res Inst Malaysia, Div Forest Environm, Kepong 52109, Selangor Darul, Malaysia. [Valencia, R.; Navarrete, H.] Pontificia Univ Catolica Ecuador, Lab Ecol Plantas & Herbario QCA, Escuela Ciencias Biol, Apartado 17-01-2184, Quito, Ecuador. [Davies, S. J.; Kenfack, D.] Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum Asia Program, Cambridge, MA 02138 USA. [Chuyong, G. B.] Univ Buea, Dept Plant & Anim Sci, POB 63, Buea, Cameroon. [Thomas, D. W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Baldeck, CA (reprint author), Univ Illinois, Program Ecol Evolut & Conservat Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA.; Baldeck, CA (reprint author), Univ Illinois, Dept Plant Biol, 505 S Goodwin Ave, Urbana, IL 61801 USA. EM cabaldeck@gmail.com; kembel.steven_w@uqam.ca; kharms@lsu.edu; jby1@cornell.edu; robert.chandran@gmail.com; turnerbl@si.edu; sumdilki@yahoo.com; nimalgun@pdn.ac.lk; savnim@slt.lk; sarayudh_b@yahoo.com; sxk49@yahoo.com; adzmiy@salam.uitm.edu.my; supardi@frim.gov.my; lrvalencia@puce.edu.ec; hnavarrete@puce.edu.ec; sdavies@oeb.harvard.edu; chuyong99@yahoo.com; KenfackD@si.edu; duncanwt@gmail.com; dallingj@life.illinois.edu RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Kembel, Steven/0000-0001-5224-0952 FU National Science Foundation [DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197]; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund; US National Science Foundation [DEB 0211004, DEB 0211115, DEB 0212284, DEB 0212818, OISE 0314581]; soils initiative of the Smithsonian Tropical Research Institute; CTFS grant FX We thank the Center for Tropical Forest Science for their collection and organization of the tree census data used in this study. The BCI forest dynamics research project was made possible by National Science Foundation Grants to Stephen P. Hubbell: DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Small World Institute Fund. Funding for soils work was provided by the US National Science Foundation Grants DEB 0211004, DEB 0211115, DEB 0212284, DEB 0212818, and OISE 0314581, the soils initiative of the Smithsonian Tropical Research Institute, and a CTFS grant to cover collection and extraction of soils from Korup. We also thank editor Walter Carson and two anonymous reviewers for their thoughtful comments on the manuscript. NR 49 TC 1 Z9 1 U1 16 U2 16 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD OCT PY 2016 VL 182 IS 2 BP 547 EP 557 DI 10.1007/s00442-016-3686-2 PG 11 WC Ecology SC Environmental Sciences & Ecology GA DW5FS UT WOS:000383669300021 PM 27337965 ER PT J AU Zapico, SC Menendez, ST AF Zapico, Sara C. Menendez, Sofia T. TI Human mitochondrial DNA and nuclear DNA isolation from food bite marks SO ARCHIVES OF ORAL BIOLOGY LA English DT Article DE Food bite marks; Human nuclear DNA isolation; mtDNA; PCR efficiency; Haplogroup; Sequencing ID SALIVA STAINS; HUMAN SKIN; EXTRACTION; STAMPS; SEX AB Objective: Bite mark analysis is used for comparison between bite marks on a bitten object and the suspects' teeth. However, if it is not possible to obtain a correct match, it is important to recover salivary DNA. Previous studies have tried to isolate human nuclear DNA from bitten foods but were not completely successful. In the present work, we studied the efficiency of human nuclear and mitochondria] DNA isolation from bite marks in cheese, a donut and an apple. Design: Using a double swab technique and silica-based DNA extraction kit, nuclear and mitochondrial DNA were isolated. Human housekeeping genes were amplified to analyse the efficiency of nuclear DNA profiling. mtDNA was sequencing and haplogroup assign. Results: Although cheese and apple samples showed the highest concentration of DNA, the purity of DNA on the apple was low. Moreover, apple samples failed to amplify the two human housekeeping genes, GAPDH and RPL22. In contrast, cheese samples have high purity and amplification efficiency. Donut samples showed an intermediate value and low amplification efficiency. In spite of these results, isolation and characterization/sequencing of human mitochondria] DNA was completely successful in the three samples, which pointed out the possibility of identification through this type of DNA. Conclusions: This research indicated that it is possible to recover and isolate human nuclear and mitochondrial DNA from bitten foods, although the quantity and purity of nuclear DNA depends on the type of food. That is of significance important in forensic sciences for the correct identification of a suspect. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Zapico, Sara C.] Smithsonian Inst, Dept Anthropol, NMNH MRC 112, Washington, DC 20013 USA. [Menendez, Sofia T.] HUCA, IUOPA, Oviedo 33006, Asturias, Spain. [Menendez, Sofia T.] Univ Oviedo, E-33006 Oviedo, Asturias, Spain. RP Zapico, SC (reprint author), Smithsonian Inst, Dept Anthropol, NMNH MRC 112, Washington, DC 20013 USA. EM Casado-Zapicos@si.edu; sofiatirados@googlemail.com NR 23 TC 0 Z9 0 U1 9 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0003-9969 EI 1879-1506 J9 ARCH ORAL BIOL JI Arch. Oral Biol. PD OCT PY 2016 VL 70 BP 67 EP 72 DI 10.1016/j.archoralbio.2016.06.004 PG 6 WC Dentistry, Oral Surgery & Medicine SC Dentistry, Oral Surgery & Medicine GA DY7RX UT WOS:000385328100010 ER PT J AU Han, C Udalski, A Gould, A Bozza, V Jung, YK Albrow, MD Kim, SL Lee, CU Cha, SM Kim, DJ Lee, Y Park, BG Shin, IG Szymanski, MK Soszynski, I Skowron, J Mroz, P Poleski, R Pietrukowicz, P Kozlowski, S Ulaczyk, K Wyrzykowski, L Pawlak, M AF Han, C. Udalski, A. Gould, A. Bozza, V. Jung, Y. K. Albrow, M. D. Kim, S. -L. Lee, C. -U. Cha, S. -M. Kim, D. -J. Lee, Y. Park, B. -G. Shin, I. -G. Szymanski, M. K. Soszynski, I. Skowron, J. Mroz, P. Poleski, R. Pietrukowicz, P. Kozlowski, S. Ulaczyk, K. Wyrzykowski, L. Pawlak, M. CA KMTNET Collaboration OGLE Collaboration TI OGLE-2015-BLG-0051/KMT-2015-BLG-0048LB: A GIANT PLANET ORBITING A LOW-MASS BULGE STAR DISCOVERED BY HIGH-CADENCE MICROLENSING SURVEYS SO ASTRONOMICAL JOURNAL LA English DT Article DE gravitational lensing: micro; planetary systems ID GALACTIC BULGE; OPTICAL DEPTH; PHOTOMETRY; SYSTEMS; DWARF; EVENTS; SEARCH; BINARY; LINE AB We report the discovery of an extrasolar planet detected from the combined data of a microlensing event OGLE-2015-BLG-0051/KMT-2015-BLG-0048 acquired by two microlensing surveys. Despite the fact that the short planetary signal occurred in the very early Bulge season during which the lensing event could be seen for just about an hour, the signal was continuously and densely covered. From the Bayesian analysis using models of the mass function, and matter and velocity distributions, combined with information on the angular Einstein radius, it is found that the host of the planet is located in the Galactic bulge. The planet has a mass 0.72(0.07)(+0.65) M-J and it is orbiting a low-mass M-dwarf host with a projected separation d(1) = 0.73 +/- 0.08 au. The discovery of the planet demonstrates the capability of the current high-cadence microlensing lensing surveys in detecting and characterizing planets. C1 [Han, C.; Jung, Y. K.; Shin, I. -G.] Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea. [Udalski, A.; Szymanski, M. K.; Soszynski, I.; Skowron, J.; Mroz, P.; Poleski, R.; Pietrukowicz, P.; Kozlowski, S.; Ulaczyk, K.; Wyrzykowski, L.; Pawlak, M.] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland. [Gould, A.; Poleski, R.] Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. [Gould, A.; Kim, S. -L.; Lee, C. -U.; Cha, S. -M.; Kim, D. -J.; Lee, Y.; Park, B. -G.] Korea Astron & Space Sci Inst, Daejon 305348, South Korea. [Bozza, V.] Univ Salerno, Dipartimento Fis ER Caianiello, Via Giovanni Paolo 2, I-84084 Fisciano, SA, Italy. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, Via Cintia, I-80126 Naples, Italy. [Jung, Y. K.; Shin, I. -G.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Albrow, M. D.] Univ Canterbury, Dept Phys & Astron, Private Bag 4800, Christchurch 8020, New Zealand. [Cha, S. -M.; Lee, Y.] Kyung Hee Univ, Sch Space Res, Yongin 446701, South Korea. RP Han, C (reprint author), Chungbuk Natl Univ, Dept Phys, Cheongju 361763, South Korea. FU Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; JPL [1500811] FX Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. The OGLE Team thanks Professors M. Kubiak and G. Pietrzynski, former members of the OGLE team, for their contribution to the collection of the OGLE photometric data over the past years. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to AU. Work by A.G. was supported by JPL grant 1500811. We acknowledge the high-speed internet service (KREONET) provided by Korea Institute of Science and Technology Information (KISTI). The KMTNet telescopes are operated by the Korea Astronomy and Space Science Institute (KASI). NR 39 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2016 VL 152 IS 4 AR 95 DI 10.3847/0004-6256/152/4/95 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ2QO UT WOS:000385686500006 ER PT J AU Holman, MJ Payne, MJ AF Holman, Matthew J. Payne, Matthew J. TI OBSERVATIONAL CONSTRAINTS ON PLANET NINE: CASSINI RANGE OBSERVATIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE celestial mechanics; ephemerides; methods: data analysis; planets and satellites: individual (Saturn); space vehicles ID KUIPER-BELT OBJECTS; ASTEROID MASSES; SCATTERED DISK; SOLAR-SYSTEM; UNCERTAINTIES; DISCOVERY; LIMIT AB We examine the tidal perturbations induced by a possible additional, distant planet in the solar system on the distance between the Earth and the Cassini. spacecraft. We find that measured range residuals alone can significantly constrain the sky position, distance, and mass of the perturbing planet to sections of the sky essentially orthogonal to the orbit of Saturn. When we combine these constraints from tidal perturbations with the dynamical constraints from Batygin & Brown and Brown & Batygin, we further constrain the allowed location of the perturbing planet to a region of the sky approximately centered on (R.A., decl.) = (40 degrees, - 15 degrees) and extending similar to 20 degrees in all directions. C1 [Holman, Matthew J.; Payne, Matthew J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. RP Holman, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM mholman@cfa.harvard.edu; mpayne@cfa.harvard.edu FU NASA [NNX13A124G, NNX10AH40G, 1312645088477, NNX16AD69G]; BSF [2012384]; Smithsonian CGPS/Pell Grant program FX M.J.H. and M.J.P. gratefully acknowledge NASA Origins of Solar Systems Program grant NNX13A124G, NASA Origins of Solar Systems Program grant NNX10AH40G via sub-award agreement 1312645088477, BSF Grant Number 2012384, NASA Solar System Observations grant NNX16AD69G, as well as support from the Smithsonian 2015 CGPS/Pell Grant program. NR 41 TC 3 Z9 3 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2016 VL 152 IS 4 AR 94 DI 10.3847/0004-6256/152/4/94 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DZ2QO UT WOS:000385686500005 ER PT J AU Abdelhamid, HM Lingam, M Mahajan, SM AF Abdelhamid, Hamdi M. Lingam, Manasvi Mahajan, Swadesh M. TI EXTENDED MHD TURBULENCE AND ITS APPLICATIONS TO THE SOLAR WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic fields; magnetohydrodynamics (MHD); methods: analytical; plasmas; solar wind; turbulence ID ELECTRON MAGNETOHYDRODYNAMIC TURBULENCE; INCOMPRESSIBLE HALL MAGNETOHYDRODYNAMICS; WEAKLY COLLISIONAL PLASMAS; REVERSE DYNAMO MECHANISM; DISSIPATION RANGE; WAVE TURBULENCE; MAGNETIC-FIELD; SPECTRAL BREAKS; ENERGY CASCADE; POWER SPECTRA AB Extended MHD is a one-fluid model that incorporates two-fluid effects such as electron inertia and the Hall drift. This model is used to construct fully nonlinear Alfvenic wave solutions, and thereby derive the kinetic and magnetic spectra by resorting to a Kolmogorov-like hypothesis based on the constant cascading rates of the energy and generalized helicities of this model. The magnetic and kinetic spectra are derived in the ideal (k < 1/lambda(i)), Hall (1/lambda(i) < k < 1/lambda(e)), and electron inertia (k > 1/lambda(e)) regimes; k is the wavenumber and lambda(s) = c/omega(ps) is the skin depth of species "s." In the Hall regime, it is shown that the emergent results are fully consistent with previous numerical and analytical studies, especially in the context of the solar wind. The focus is primarily on the electron inertia regime, where magnetic energy spectra with power-law indexes of -11/3 and -13/3 are always recovered. The latter, in particular, is quite close to recent observational evidence from the solar wind with a potential slope of approximately -4 in this regime. It is thus plausible that these spectra may constitute a part of the (extended) inertial range, as opposed to the standard "dissipation" range paradigm. C1 [Abdelhamid, Hamdi M.] Univ Tokyo, Grad Sch Frontier Sci, Kashiwa, Chiba 2778561, Japan. [Abdelhamid, Hamdi M.] Mansoura Univ, Dept Phys, Fac Sci, Mansoura 35516, Egypt. [Lingam, Manasvi] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Lingam, Manasvi] Harvard Univ, Harvard John A Paulson Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Lingam, Manasvi] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Mahajan, Swadesh M.] Univ Texas Austin, Dept Phys, Austin, TX 78712 USA. [Mahajan, Swadesh M.] Univ Texas Austin, Inst Fus Studies, Austin, TX 78712 USA. [Mahajan, Swadesh M.] Shiv Nadar Univ, Dept Phys, Sch Nat Sci, Lucknow 201314, Uttar Pradesh, India. RP Abdelhamid, HM (reprint author), Univ Tokyo, Grad Sch Frontier Sci, Kashiwa, Chiba 2778561, Japan.; Abdelhamid, HM (reprint author), Mansoura Univ, Dept Phys, Fac Sci, Mansoura 35516, Egypt. EM hamdi@ppl.k.u-tokyo.ac.jp; mlingam@princeton.edu OI Abdelhamid, Hamdi/0000-0002-0641-1543 FU Egyptian Ministry of Higher Education; DOE [DE-AC02-09CH-11466, DE-FG03-96ER-54366]; NSF [AGS-1338944] FX HMA would like to thank the Egyptian Ministry of Higher Education for supporting his research activities, and gratefully acknowledges the hospitality of the Princeton Plasma Physics Laboratory where this work was initiated. ML was supported by the DOE (Grant No. DE-AC02-09CH-11466) and the NSF (Grant No. AGS-1338944) while pursuing this work. SMM's work was supported by the DOE (Contract No.DE-FG03-96ER-54366). The authors wish to thank the referee for the helpful comments and suggestions, which helped improve the quality of the paper. NR 101 TC 4 Z9 4 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 87 DI 10.3847/0004-637X/829/2/87 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200029 ER PT J AU Bergner, JB Oberg, KI Rajappan, M Fayolle, EC AF Bergner, Jennifer B. Oberg, Karin I. Rajappan, Mahesh Fayolle, Edith C. TI KINETICS AND MECHANISMS OF THE ACID-BASE REACTION BETWEEN NH3 AND HCOOH IN INTERSTELLAR ICE ANALOGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; methods: laboratory: solid state; molecular processes ID COMPLEX ORGANIC-MOLECULES; SPITZER SPECTROSCOPIC SURVEY; YOUNG STELLAR OBJECTS; GRAIN MANTLES; EMBEDDED PROTOSTARS; ABSORPTION FEATURES; OCN-FORMATION; LINE SURVEY; W 33A; MU-M AB Interstellar complex organic molecules are commonly observed during star formation, and are proposed to form through radical chemistry in icy grain mantles. Reactions between ions and neutral molecules in ices may provide an alternative cold channel to complexity, as ion-neutral reactions are thought to have low or even no-energy barriers. Here we present a study of the kinetics and mechanisms of a potential ion-generating, acid-base reaction between NH3 and HCOOH to form the salt NH4+HCOO-. We observe salt growth at temperatures as low as 15 K, indicating that this reaction is feasible in cold environments. The kinetics of salt growth are best fit by a two-step model involving a slow "pre-reaction" step followed by a fast reaction step. The reaction energy barrier is determined to be 70 +/- 30 K with a pre-exponential factor 1.4 +/- 0.4 x 10(-3) s(-1). The pre-reaction rate varies under different experimental conditions and likely represents a combination of diffusion and orientation of reactant molecules. For a diffusion-limited case, the pre-reaction barrier is 770 +/- 110 K with a pre-exponential factor of similar to 7.6 x 10(-3) s(-1). Acid-base chemistry of common ice constituents is thus a potential cold pathway to generating ions in interstellar ices. C1 [Bergner, Jennifer B.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Oberg, Karin I.; Rajappan, Mahesh; Fayolle, Edith C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bergner, JB (reprint author), Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. EM jennifer.bergner@cfa.harvard.edu FU National Science Foundation [DGE1144152]; Simons Collaboration on the Origins of Life (SCOL) investigator award FX J.B.B. acknowledges funding from the National Science Foundation Graduate Research Fellowship under Grant DGE1144152. K.I.O. acknowledges funding from the Simons Collaboration on the Origins of Life (SCOL) investigator award. NR 40 TC 0 Z9 0 U1 3 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 85 DI 10.3847/0004-637X/829/2/85 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200027 ER PT J AU Eftekhari, T Stovall, K Dowell, J Schinzel, FK Taylor, GB AF Eftekhari, T. Stovall, K. Dowell, J. Schinzel, F. K. Taylor, G. B. TI A LOW FREQUENCY SURVEY OF GIANT PULSES FROM THE CRAB PULSAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general ID RADIO-CONTINUUM EMISSION; FLUX DENSITIES; WIDEFIELD ARRAY; SPECTRAL INDEX; NP 0532; SCATTERING; NEBULA; MHZ; DISPERSION; TELESCOPE AB We present a large survey of giant pulses from the Crab Pulsar as observed with the first station of the Long Wavelength Array. Automated methods for detecting giant pulses at low frequencies where scattering becomes prevalent are also explored. More than 1400 pulses were detected across four frequency bands between 20 and 84 MHz over a seven-month period beginning in 2013, with additional followup observations in late 2014 and early 2015. A handful of these pulses were detected simultaneously across all four frequency bands. We examine pulse characteristics, including pulse broadening and power law indices for amplitude distributions. We find that the flux density increases toward shorter wavelengths, consistent with a spectral turnover at 100 MHz. Our observations uniquely span multiple scattering epochs, manifesting as a notable trend in the number of detections per observation. These results are characteristic of the variable interface between the synchrotron nebula and the surrounding interstellar medium. C1 [Eftekhari, T.; Stovall, K.; Dowell, J.; Schinzel, F. K.; Taylor, G. B.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87106 USA. [Eftekhari, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Eftekhari, T (reprint author), Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87106 USA.; Eftekhari, T (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. OI Schinzel, Frank/0000-0001-6672-128X; Eftekhari, Tarraneh/0000-0003-0307-9984 FU Office of Naval Research [N00014-07-C-0147]; Air Force Office of Scientific Research DURIP program; National Science Foundation of University Radio Observatory program [AST-1139963, AST-1139974] FX Construction of the LWA has been supported by the Office of Naval Research under Contract N00014-07-C-0147 and by the Air Force Office of Scientific Research DURIP program. Support for operations and continuing development of the LWA1 is provided by the National Science Foundation under grants AST-1139963 and AST-1139974 of the University Radio Observatory program. NR 38 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 62 DI 10.3847/0004-637X/829/2/62 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200004 ER PT J AU Hornbeck, JB Swearingen, JR Grady, CA Williger, GM Brown, A Sitko, ML Wisniewski, JP Perrin, MD Lauroesch, JT Schneider, G Apai, D Brittain, S Brown, JM Champney, EH Hamaguchi, K Henning, T Lynch, DK Petre, R Russell, RW Walter, FM Woodgate, B AF Hornbeck, J. B. Swearingen, J. R. Grady, C. A. Williger, G. M. Brown, A. Sitko, M. L. Wisniewski, J. P. Perrin, M. D. Lauroesch, J. T. Schneider, G. Apai, D. Brittain, S. Brown, J. M. Champney, E. H. Hamaguchi, K. Henning, Th. Lynch, D. K. Petre, R. Russell, R. W. Walter, F. M. Woodgate, B. TI PANCHROMATIC IMAGING OF A TRANSITIONAL DISK: THE DISK OF GM AUR IN OPTICAL AND FUV SCATTERED LIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (GM Aur); stars: protostars; stars: variables: T Tauri, Herbig Ae/Be; ultraviolet: planetary systems ID T-TAURI STARS; YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTIONS; FLUORESCENT H-2 EMISSION; MOLECULAR-HYDROGEN EMISSION; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISK; SIZE DISTRIBUTION; EMBEDDED PLANETS; DUST FILTRATION AB We have imaged GM Aurigae with the Hubble Space Telescope, detected its disk in scattered light at 1400 and 1650 angstrom, and compared these with observations at 3300 angstrom, 5550 angstrom, 1.1 mu m, and 1.6 mu m. The scattered light increases at shorter wavelengths. The radial surface brightness profile at 3300 angstrom shows no evidence of the 24 au radius cavity that has been previously observed in submillimeter observations. Comparison with dust grain opacity models indicates that. the surface of the entire disk is populated with submicron grains. We have compiled a. spectral energy distribution from 0.1 mu m to 1 mm. and used it to constrain a model of the star + disk system that includes the submillimeter cavity using the Monte Carlo radiative transfer code by Barbara Whitney. The best-fit model image indicates that the cavity should be detectable in the F330W bandpass if the cavity has been cleared of both large and small dust grains, but we do not detect it. The lack of an observed cavity can be explained by the presence of submicron grains interior to the submillimeter cavity wall. We suggest one explanation for this that. could be due to a planet of mass <9 M-J interior to 24 au. A unique cylindrical structure is detected in the far-UV data from the Advanced Camera for Surveys/ Solar Blind Channel. It is aligned along the system semiminor axis, but does not resemble an accretion-driven jet. The structure is limb. brightened and extends 190 +/- 35 au above the disk midplane. The inner radius of the limb. brightening is 40 +/- 10 au, just beyond the submillimeter cavity wall. C1 [Hornbeck, J. B.; Williger, G. M.; Lauroesch, J. T.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Swearingen, J. R.; Sitko, M. L.; Champney, E. H.] Univ Cincinnati, Dept Phys, 400 Geol Phys Bldg,POB 210011, Cincinnati, OH 45221 USA. [Grady, C. A.] Eureka Sci, 2452 Delmer St,Suite 100, Oakland, CA 96402 USA. [Grady, C. A.] Goddard Space Flight Ctr, Exoplanets & Stellar Astrophys Lab, Code 667, Greenbelt, MD 20771 USA. [Williger, G. M.] Univ Nice, Lab Lagrange, UMR 7293, F-06108 Nice 2, France. [Williger, G. M.] Catholic Univ Amer, Dept Phys, IACS, Washington, DC 20064 USA. [Williger, G. M.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Brown, A.] Univ Colorado, CASA, Boulder, CO 80309 USA. [Sitko, M. L.] Space Sci Inst, Ctr Extrasolar Planetary Syst, Boulder, CO 80301 USA. [Wisniewski, J. P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. [Perrin, M. D.; Schneider, G.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Apai, D.] Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Apai, D.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. [Apai, D.] Univ Arizona, Dept Planetary Sci, 1629 E Univ Blvd, Tucson, AZ 85721 USA. [Apai, D.] Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. [Brittain, S.] Clemson Univ, Dept Phys & Astron, 118 Kinard Lab, Clemson, SC 29634 USA. [Brown, J. M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hamaguchi, K.] UMBC, Dept Phys, Baltimore, MD 21250 USA. [Hamaguchi, K.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Hamaguchi, K.] NASA GSFC, X Ray Astrophys Lab, Greenbelt, MD 20771 USA. [Henning, Th.] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Lynch, D. K.; Russell, R. W.] Aerosp Corp, Los Angeles, CA 90009 USA. [Petre, R.; Woodgate, B.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Walter, F. M.] SUNY Stony Brook, Dept Phys & Astron, Z 3800, Stony Brook, NY 11794 USA. RP Hornbeck, JB (reprint author), Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. EM jeremy.hornbeck@louisville.edu; carol.a.grady@nasa.gov; gmwill06@louisville.edu FU NASA [NAS 5-26555, NNH06CC28C, NNX09AC73G]; NASA Kentucky Space Grant Consortium [3049024102-11-175]; [HST-GO-10864]; [HST-GO-11336]; [HST-GO-12016]; [HST-GO-11336.01-A] FX This work is, in part, based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. J.B.H. was supported in part by funding from the NASA Kentucky Space Grant Consortium, Award # 3049024102-11-175. Data used in this study were obtained under programs HST-GO-10864, HST-GO-11336, and HST-GO-12016. We thank A.. M. Hughes and S. Andrews for the SMA and Plateau de Bure data. A.B. was supported by the grant HST-GO-11336.01-A, for which observing time was granted by the Chandra X-ray Observatory peer review. The authors thank the support staff members of the IRTF telescope for assistance in obtaining the SED data, and the IR&D program at The Aerospace Corporation. We also acknowledge support from NASA NNH06CC28C (M.L.S.) and NNX09AC73G (C.A.G. and M.L.S.). We would like to thank Kenneth Wood and Michael J. Wolff for their quick response to our questions about their dust grain models during private communications. Finally, we thank two anonymous referees for many suggestions that. significantly improved this paper. We dedicate this paper to the memory of Bruce Woodgate, a colleague, mentor, and friend who died during the preparation of this paper. NR 97 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 65 DI 10.3847/0004-637X/829/2/65 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200007 ER PT J AU Imara, N Burkhart, B AF Imara, Nia Burkhart, Blakesley TI THE H I PROBABILITY DISTRIBUTION FUNCTION AND THE ATOMIC-TO-MOLECULAR TRANSITION IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: clouds; ISM: individual objects (Orion A, Rosette); ISM: structure; photon-dominated region (PDR) ID SMALL-MAGELLANIC-CLOUD; TURBULENT MAGNETIZED CLOUDS; FIELD EXTINCTION MAPS; YOUNG STELLAR OBJECTS; INITIAL MASS FUNCTION; MACH NUMBER RELATION; WARM NEUTRAL MEDIUM; STAR-FORMATION RATE; COLUMN DENSITY; INTERSTELLAR CLOUDS AB We characterize the column-density probability distribution. functions (PDFs) of the atomic hydrogen gas, H I, associated with seven Galactic molecular clouds (MCs). We use 21 cm observations from the Leiden/Argentine/Bonn Galactic H I. Survey to derive column-density maps and PDFs. We find that the peaks of the H I. PDFs occur at column densities in the range. similar to 1-2 x 10(21) cm(-2) (equivalently, similar to 0.5-1 mag). The PDFs are uniformly narrow,. with a mean dispersion of sigma(Pi) (I) approximate to 10(20) cm(-2) (similar to 0.1 mag). We also investigate the H I-to-H-2. transition toward the cloud complexes and estimate H I. surface densities ranging from 7 to 16 M-circle dot pc(-2). at the transition. We propose that the H I. PDF is a fitting tool for identifying the H I-to-H-2. transition column in Galactic MCs. C1 [Imara, Nia; Burkhart, Blakesley] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Imara, N (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nimara@cfa.harvard.edu FU NASA Einstein Postdoctoral Fellowship; Harvard-MIT FFL Fellowship FX We thank Tom Dame, Bruce Draine, and Charlie Lada for their helpful comments on earlier drafts of this paper,. and we thank Marco Lombardi for providing the NICEST data used in this study. We thank the anonymous referee whose insights and thorough attention to an earlier draft helped to improve this paper. N. Imara is supported by the Harvard-MIT FFL Fellowship, and B. Burkhart is supported by the NASA Einstein Postdoctoral Fellowship. NR 100 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 102 DI 10.3847/0004-637X/829/2/102 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200044 ER PT J AU Liu, T Kim, KT Yoo, H Liu, SY Tatematsu, K Qin, SL Zhang, QZ Wu, YF Wang, K Goldsmith, PF Juvela, M Lee, JE Toth, LV Mardones, D Garay, G Bronfman, L Cunningham, MR Li, D Lo, N Ristorcelli, I Schnee, S AF Liu, Tie Kim, Kee-Tae Yoo, Hyunju Liu, Sheng-Yuan Tatematsu, Ken'ichi Qin, Sheng-Li Zhang, Qizhou Wu, Yuefang Wang, Ke Goldsmith, Paul F. Juvela, Mika Lee, Jeong-Eun Toth, L. Viktor Mardones, Diego Garay, Guido Bronfman, Leonardo Cunningham, Maria R. Li, Di Lo, Nadia Ristorcelli, Isabelle Schnee, Scott TI STAR FORMATION LAWS IN BOTH GALACTIC MASSIVE CLUMPS AND EXTERNAL GALAXIES: EXTENSIVE STUDY WITH DUST CONINUUM, HCN (4-3), AND CS (7-6) SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: ISM; ISM: kinematics and dynamics; stars: formation ID ULTRALUMINOUS INFRARED GALAXIES; DENSE GAS TRACERS; HIGH-J CO; MOLECULAR CLOUDS; FORMING REGIONS; COMPLETE SAMPLE; FORMATION RATES; MILKY-WAY; LUMINOSITY; CONTINUUM AB We observed 146 Galactic clumps in HCN (4-3) and CS (7-6) with the Atacama Submillimeter Telescope Experiment 10 m telescope. A tight linear relationship between star formation rate and gas mass traced by dust continuum emission was found for both Galactic clumps and the high redshift (z > 1) star forming galaxies (SFGs), indicating a constant gas depletion time of similar to 100 Myr for molecular gas in both Galactic clumps and high z SFGs. However, low z galaxies do not follow this relation and seem to have a longer global gas depletion time. The correlations between total infrared luminosities (L-TIR) and molecular line luminosities (L-mol') of HCN (4-3) and CS (7-6) are tight and sublinear extending down to clumps with L-TIR similar to 10(3) L-circle dot. These correlations become linear when extended to external galaxies. A bimodal behavior in the L-TIR-L-mol' correlations was found for clumps with different dust temperature, luminosity-to-mass ratio, and sigma(line)/sigma(vir). Such bimodal behavior may be due to evolutionary effects. The slopes of L-TIR-L-mol' correlations become more shallow as clumps evolve. We compared our results with lower J transition lines in Wu et al. (2010). The correlations between clump masses and line luminosities are close to linear for low effective excitation density tracers but become sublinear for high effective excitation density tracers for clumps with L-TIR larger than L-TIR similar to 10(4.5) L-circle dot. High effective excitation density tracers cannot linearly trace the total clump masses, leading to a sublinear correlations for both M-clump-L-mol' and L-TIR-L-mol' relations. C1 [Liu, Tie; Kim, Kee-Tae; Yoo, Hyunju] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea. [Yoo, Hyunju] Chungnam Natl Univ, Dept Astron & Space Sci, Daejeon, South Korea. [Liu, Sheng-Yuan] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. [Tatematsu, Ken'ichi] Natl Astron Observ Japan, Natl Inst Nat Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Qin, Sheng-Li] Yunnan Univ, Dept Astron, Kunming 650091, Peoples R China. [Qin, Sheng-Li] Key Lab Astroparticle Phys Yunnan Prov, Kunming 650091, Peoples R China. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wu, Yuefang] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Wang, Ke] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Goldsmith, Paul F.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Juvela, Mika] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland. [Lee, Jeong-Eun] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. [Toth, L. Viktor] Eotvos Lorand Univ, Dept Astron, Pazmany Peter Setany 1, H-1117 Budapest, Hungary. [Mardones, Diego; Garay, Guido; Bronfman, Leonardo; Lo, Nadia] Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. [Cunningham, Maria R.] Univ New South Wales, Sch Phys, Sydney, NSW 2052, Australia. [Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Li, Di] Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Jiangsu, Peoples R China. [Ristorcelli, Isabelle] Univ Toulouse 3, IRAP, CNRS, UMR5277, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France. [Schnee, Scott] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. RP Liu, T (reprint author), Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea. EM liutiepku@gmail.com RI Toth, L. Viktor/C-8667-2017; OI Toth, L. Viktor/0000-0002-5310-4212; Wang, Ke/0000-0002-7237-3856; Cunningham, Maria/0000-0001-7020-6176; Zhang, Qizhou/0000-0003-2384-6589 FU KASI fellowship; China Ministry of Science and Technology under State Key Development Program for Basic Research [2012CB821800]; NSFC [11373009, 11433008, 11373026]; ESO fellowship; DFG Priority Program ("Physics of the Interstellar Medium") [1573, WA3628-1/1]; Top Talents Program of Yunnan Province [2015HA030]; Academy of Finland [1285769]; CONICYT [PFB-06]; Basic Science Research Program through the National Research Foundation of Korea (NRF) [NRF-2015R1A2A2A01004769]; Korea Astronomy and Space Science Institute under the RD program [20151-32018]; OTKA [K101393, NN-111016] FX We are grateful to the ASTE staff. The ASTE telescope is operated by National Astronomical Observatory of Japan (NAOJ). Tie Liu is supported by KASI fellowship. Y. Wu is partly supported by the China Ministry of Science and Technology under State Key Development Program for Basic Research (No.2012CB821800), the grants of NSFC No.11373009 and No.11433008. Ke Wang acknowledges the support from ESO fellowship and DFG Priority Program 1573 ("Physics of the Interstellar Medium") grant WA3628-1/1. This work was carried out in part at the Jet Propulsion Laboratory, operated for NASA by the California Institute of Technology. S. L. Qin is supported by NSFC under grant No. 11373026, and Top Talents Program of Yunnan Province (2015HA030). MJ acknowledges the support of the Academy of Finland Grant No.1285769. LB acknowledges support from CONICYT grant PFB-06. JEL was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) (grant No. NRF-2015R1A2A2A01004769) and the Korea Astronomy and Space Science Institute under the R&D program (Project No.20151-32018) supervised by the Ministry of Science, ICT, and Future Planning. LVT acknowledges the support by the OTKA grants K101393 and NN-111016. The anonymous referee provided very insightful comments. NR 43 TC 1 Z9 1 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 59 DI 10.3847/0004-637X/829/2/59 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200001 ER PT J AU Sakari, CM Shetrone, MD Schiavon, RP Bizyaev, D Prieto, CA Beers, TC Caldwell, N Garcia-Hernandez, DA Lucatello, S Majewski, S O'Connell, RW Pan, KK Strader, J AF Sakari, Charli M. Shetrone, Matthew D. Schiavon, Ricardo P. Bizyaev, Dmitry Prieto, Carlos Allende Beers, Timothy C. Caldwell, Nelson Anibal Garcia-Hernandez, Domingo Lucatello, Sara Majewski, Steven O'Connell, Robert W. Pan, Kaike Strader, Jay TI INFRARED HIGH-RESOLUTION INTEGRATED LIGHT SPECTRAL ANALYSES OF M31 GLOBULAR CLUSTERS FROM APOGEE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: individual (M31); galaxies: star clusters: general; globular clusters: general ID HOBBY-EBERLY TELESCOPE; METAL-POOR STARS; STELLAR EVOLUTION DATABASE; GIANT BRANCH STARS; POPULATION SYNTHESIS; CHEMICAL ABUNDANCES; FEATURE INDEXES; DWARF GALAXIES; RED GIANTS; OUTER HALO AB Chemical abundances are presented for 25 M31 globular clusters (GCs), based on moderately high resolution (R = 22,500) H-band integrated light (IL) spectra from the Apache Point Observatory Galactic Evolution Experiment (APOGEE). Infrared (IR) spectra offer lines from new elements, lines of different strengths, and lines at higher excitation potentials compared to the optical. Integrated abundances of C, N, and O are derived from CO, CN, and OH molecular features, while Fe, Na, Mg, Al, Si, K, Ca, and Ti abundances are derived from atomic features. These abundances are compared to previous results from the optical, demonstrating the validity and value of IR IL analyses. The CNO abundances are consistent with typical tip of the red giant branch stellar abundances. but are systematically offset from optical. Lick index abundances. With a few exceptions, the other abundances agree between the optical and the IR within the 1 sigma uncertainties. The first integrated K abundances are also presented. and demonstrate that K tracks the a. elements. The combination of IR and optical abundances allows better determinations of GC properties. and enables probes of the multiple populations in extragalactic GCs. In particular, the integrated effects of the Na/O anticorrelation can be directly examined for the first time. C1 [Sakari, Charli M.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Shetrone, Matthew D.] Univ Texas Austin, McDonald Observ, HC75 Box 1337 MCD, Ft Davis, TX 79734 USA. [Schiavon, Ricardo P.] Gemini Observ, 670 N AOhoku Pl, Hilo, HI 96720 USA. [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. [Bizyaev, Dmitry; Pan, Kaike] Apache Point Observ, POB 59, Sunspot, NM 88349 USA. [Bizyaev, Dmitry; Pan, Kaike] New Mexico State Univ, POB 59, Sunspot, NM 88349 USA. [Bizyaev, Dmitry] Russian AS, Special Astrophys Observ, Nizhnii Arkhyz, Russia. [Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prosp 13, Moscow, Russia. [Prieto, Carlos Allende; Anibal Garcia-Hernandez, Domingo] IAC, Va Lactea S-N, E-38205 Tenerife, Spain. [Prieto, Carlos Allende; Anibal Garcia-Hernandez, Domingo] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Beers, Timothy C.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Beers, Timothy C.] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 USA. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lucatello, Sara] INAF Osservatorio Astronomico Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy. [Majewski, Steven; O'Connell, Robert W.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Sakari, CM (reprint author), Univ Washington, Dept Astron, Seattle, WA 98195 USA. EM sakaricm@u.washington.edu OI Bizyaev, Dmitry/0000-0002-3601-133X FU Kenilworth Foundation; RSF [14-50-00043]; Spanish MINECO [AYA2014-56359-P]; Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA) [PHY08-22648]; Physics Frontier Center/JINA Center [PHY 14-30152]; US National Science Foundation; Ramon y Cajal fellowship [RYC-2013-14182]; Spanish Ministry of Economy and Competitiveness (MINECO) [AYA-2014-58082-P]; NSF [AST-1514763]; Packard Foundation FX The authors thank the anonymous referee for suggestions that improved the manuscript. The authors also thank Chris Sneden for developing the synpop version of MOOG and maintaining the code, Andrew McWilliam for discussions regarding integrated light analyses, and Masen Lamb for discussions regarding IR syntheses. CMS acknowledges funding from the Kenilworth Foundation. DB acknowledges support from grant RSF 14-50-00043. CAP is thankful to the Spanish MINECO for funding through grant AYA2014-56359-P. TCB acknowledges partial support for this work from grants PHY08-22648, Physics Frontier Center/Joint Institute or Nuclear Astrophysics (JINA); and PHY 14-30152, Physics Frontier Center/JINA Center for the Evolution of the Elements (JINA-CEE), awarded by the US National Science Foundation. DAGH was funded by the Ramon y Cajal fellowship number RYC-2013-14182 and he acknowledges support provided by the Spanish Ministry of Economy and Competitiveness (MINECO) under grant AYA-2014-58082-P. JS acknowledges partial support from NSF grant AST-1514763 and the Packard Foundation. NR 69 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 116 DI 10.3847/0004-637X/829/2/116 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200058 ER PT J AU Schaefer, L Wordsworth, RD Berta-Thompson, Z Sasselov, D AF Schaefer, Laura Wordsworth, Robin D. Berta-Thompson, Zachory Sasselov, Dimitar TI PREDICTIONS OF THE ATMOSPHERIC COMPOSITION OF GJ 1132b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planet-star interactions; planets and satellites: atmospheres; planets and satellites: composition planets and satellites: individual (GJ 1132b) ID ACTIVITY-ROTATION RELATIONSHIP; LOCKED TERRESTRIAL PLANETS; THERMAL PHASE CURVES; PRE-MAIN-SEQUENCE; M DWARFS; MAGMA OCEAN; HABITABLE ZONES; SUPER-EARTHS; M-STARS; HYDRODYNAMIC ESCAPE AB GJ 1132b is a nearby Earth-sized exoplanet transiting an M dwarf, and is among the most highly characterizable small exoplanets currently known. In this paper, we study the interaction of a magma ocean with a water-rich atmosphere on GJ 1132b and determine that it must have begun with more than 5 wt% initial water in order to still retain a water-based atmosphere. We also determine the amount of O-2 that can build up in the atmosphere as a result of hydrogen dissociation and loss. We find that the magma ocean absorbs at most similar to 10% of the O-2 produced, whereas more than 90% is lost to space through hydrodynamic drag. The most common outcome for GJ 1132b from our simulations is a tenuous atmosphere dominated by O-2, though, for very large initial water abundances,. atmospheres with several thousands of bars of O-2 are possible. A substantial steam envelope would indicate either the existence of an earlier H-2 envelope or low XUV flux over the system's lifetime. A steam atmosphere would also imply the continued existence of a magma ocean on GJ 1132b. Further modeling is needed to study the evolution of CO2 or N-2-rich atmospheres on GJ 1132b. C1 [Schaefer, Laura; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wordsworth, Robin D.] Harvard Paulson Sch Engn & Appl Sci, 29 Oxford St, Cambridge, MA 02138 USA. [Wordsworth, Robin D.] Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. [Berta-Thompson, Zachory] MIT, Kavli Inst Astrophys & Space Res, 77 Massachussetts Ave Bldg 37, Cambridge, MA 02139 USA. RP Schaefer, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lschaefer@cfa.harvard.edu OI Schaefer, Laura/0000-0003-2915-5025 FU FAS Division of Science, Research Computing Group at Harvard University; Simons Foundation; MIT Torres Fellowship FX The authors thank Colin Goldblatt for providing the runaway greenhouse OLR data used to perform the intercomparison shown in Figure 3, and an anonymous referee for a positive and helpful review. The line-by-line opacity computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. L.S. and D.S. acknowledge support from the Simons Foundation. Z.K.B.T. gratefully acknowledges support from the MIT Torres Fellowship for Exoplanet Research. NR 97 TC 4 Z9 4 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2016 VL 829 IS 2 AR 63 DI 10.3847/0004-637X/829/2/63 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8JX UT WOS:000385377200005 ER PT J AU Steiner, JF Remillard, RA Garcia, JA McClintock, JE AF Steiner, James F. Remillard, Ronald A. Garcia, Javier A. McClintock, Jeffrey E. TI STRONGER REFLECTION FROM BLACK HOLE ACCRETION DISKS IN SOFT X-RAY STATES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID XTE J1550-564; GRS 1915+105; INNER-DISK; BINARIES; SPECTRA; SPIN; MASS; TRANSIENT; PHOTOIONIZATION; APPEARANCE AB We analyze 15,000 spectra of 29 stellar-mass black hole (BH) candidates collected over the 16 year mission lifetime of Rossi X-ray Timing Explorer using a simple phenomenological model. As these BHs vary widely in luminosity and progress through a sequence of spectral states, which we broadly refer to as hard and soft, we focus on two spectral components: the Compton power law and the reflection spectrum it generates by illuminating the accretion disk. Our proxy for the strength of reflection is the equivalent width of the Fe-K line as measured with respect to the power law. A key distinction of our work is that for all states we estimate the continuum under the line by excluding the thermal disk component and using only the component that is responsible for fluorescing the Fe-K line, namely, the Compton power law. We find that reflection is several times more pronounced (similar to 3) in soft compared to hard spectral states. This is most readily caused by the dilution of the Fe line amplitude from Compton scattering in the corona, which has a higher optical depth in hard states. Alternatively, this could be explained by a more compact corona in soft (compared to hard) states, which would result in a higher reflection fraction. C1 [Steiner, James F.; Remillard, Ronald A.] MIT, MIT Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. [Garcia, Javier A.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Steiner, JF (reprint author), MIT, MIT Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. EM jsteiner@mit.edu OI Garcia, Javier/0000-0003-3828-2448; Remillard, Ronald/0000-0003-4815-0481 FU NASA Einstein Fellowship grant [PF5-160144] FX J.F.S. has been supported by the NASA Einstein Fellowship grant PF5-160144. NR 45 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2016 VL 829 IS 2 AR L22 DI 10.3847/2041-8205/829/2/L22 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8WJ UT WOS:000385412300001 ER PT J AU Koehn, LE Hard, JJ Akst, EP Boersma, PD AF Koehn, Laura E. Hard, Jeffrey J. Akst, Elaine P. Boersma, P. Dee TI Natural selection on morphology varies among years and by sex in Magellanic Penguins (Spheniscus magellanicus) SO AUK LA English DT Article DE animal model; heritability; Magellanic Penguins; morphology; natural selection; reproductive success ID REPRODUCTIVE SUCCESS; DARWINS FINCHES; BODY-SIZE; SEVERE WEATHER; TARSUS LENGTH; ANIMAL-MODEL; EGG-SIZE; HERITABILITY; TRAITS; DIMORPHISM AB The evolution of morphology in a population reflects several factors, including the influence of environmental variability on natural selection. We estimated natural selection on, and heritability of, 4 individual morphological traits (bill length, bill depth, flipper length, and foot length) and 2 multivariate morphological traits in adult Magellanic Penguins (Spheniscus magellanicus) at Punta Tombo, Argentina, from 1983 to 2010. We estimated heritability of morphology with parent-offspring regression and animal models, conditioning on sex because the species is sexually dimorphic. For the analysis of selection on each trait, we estimated both linear and quadratic selection gradients, based on the number of fledglings produced, for breeding males and females in each year. Estimates from animal models indicated that all 6 traits were heritable; in parent-offspring regressions, corresponding heritabilities were significantly higher in sons than in daughters in 100% of tests. Over 28 yr, we detected no selection in 21 yr for males and in 21 yr for females. For the years in which we did detect selection, the direction and intensity of selection on traits varied, being especially variable for females. We detected selection on primarily multivariate body size but also on male bill sizes and female bill and foot lengths. Selection on male flipper and foot lengths and on female bill depth was detectable only in relation to selection on body size. When there was selection in males, selection on body and bill sizes was mainly toward larger sizes and occurred in 4 of 6 yr with high chick starvation. The absence of detectable selection on morphology in most years suggests that it is not tightly linked to fitness and that the dynamic environment where Magellanic Penguins live helps maintain morphological variation. The temporal variability in selection likely fosters stability of morphology through time, a pattern that might not be evident in short-term studies. C1 [Koehn, Laura E.] Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA. [Koehn, Laura E.; Boersma, P. Dee] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Hard, Jeffrey J.] NOAA, Conservat Biol Div, Northwest Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA USA. [Akst, Elaine P.; Boersma, P. Dee] Wildlife Conservat Soc, Bronx, NY USA. [Akst, Elaine P.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Mol Genet Lab, Washington, DC USA. RP Koehn, LE (reprint author), Univ Washington, Sch Aquat & Fishery Sci, Seattle, WA 98195 USA.; Koehn, LE (reprint author), Univ Washington, Dept Biol, Seattle, WA 98195 USA. EM laura.koehn216@gmail.com FU WCS; Pew Fellows Program in Marine Conservation; ExxonMobil Foundation; Disney Worldwide Conservation Fund; National Geographic Society; Chase foundation; Cunningham foundation; CGMK foundation; Offield foundation; Peach foundation; Thorne foundation; Tortuga foundation; Kellogg foundation; Wadsworth Endowed Chair in Conservation Science at the University of Washington; Friends of the Penguins; National Science Foundation (NSF) Graduate Fellowship; Smithsonian Institution; NSF Research Training Grant FX Data were collected under a joint agreement between the Wildlife Conservation Society (WCS) and the Office of Tourism, Province of Chubut, Argentina, since 1982. We thank the Province of Chubut and the La Regina family for logistical support and access to the penguin colony, and the many students and field volunteers who collected data over the years. P. Garcia Borboroglu, W. Conway, G. Harris, and P. Harris facilitated the research and helped with permits. Research funding for our dataset includes WCS; Pew Fellows Program in Marine Conservation; ExxonMobil Foundation; Disney Worldwide Conservation Fund; National Geographic Society; the Chase, Cunningham, CGMK, Offield, Peach, Thorne, Tortuga, and Kellogg foundations; the Wadsworth Endowed Chair in Conservation Science at the University of Washington; and Friends of the Penguins. We thank Trimble for donating 6 tablet computers and Canon for contributing 2 pairs of binoculars for our research. E. P. Akst did the penguin chick sexing at the Center for Conservation and Evolutionary Genetics Lab, facilitated by R. Fleischer and supported by a National Science Foundation (NSF) Graduate Fellowship, the Smithsonian Institution, and an NSF Research Training Grant to the University of Maryland and the Smithsonian Institution and WCS. Toby Bradshaw, Tim Essington, Olivia Kane, Ginger Rebstock, Gordon Orians, Wayne Arendt, and anonymous reviewers improved the manuscript. NR 76 TC 0 Z9 0 U1 11 U2 11 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD OCT PY 2016 VL 133 IS 4 BP 783 EP 805 DI 10.1642/AUK-16-50.1 PG 23 WC Ornithology SC Zoology GA DY9CP UT WOS:000385430800017 ER PT J AU Moser, WE Richardson, DJ Lazo-Wasem, EA AF Moser, William E. Richardson, Dennis J. Lazo-Wasem, Eric A. TI Distribution of Placobdella ornata (Verrill, 1872) (Hirudinida: Glossiphoniidae) SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Placobdella ornata; Placobdella phalera; Hirudinida; Glossiphoniidae; New England ID REDESCRIPTION AB The distribution of Placobdella ornata (Verrill, 1872) is unclear as there has been much taxonomic confusion regarding this species. New collections and redetermination of museum specimens revealed 24 new locality records for Placobdella ornata, including the first reports of the species in New York and Rhode Island. Placobdella ornata is now known to occur in Massachusetts, Rhode Island, Connecticut, and eastern New York, USA, as well as Belgium (presumably introduced). A specimen from the syntype series of Placobdella ornata (Verrill, 1872) is designated as the lecto-type of the species. C1 [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Richardson, Dennis J.] Quinnipiac Univ, Dept Biol Sci, Hamden, CT 06518 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. EM moserw@si.edu NR 15 TC 1 Z9 1 U1 0 U2 0 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2016 VL 57 IS 2 BP 175 EP 179 PG 5 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DZ5MS UT WOS:000385906800005 ER PT J AU Schnell, NK Konstantinidis, P Johnson, GD AF Schnell, Nalani K. Konstantinidis, Peter Johnson, G. David TI High-proof Ethanol Fixation of Larval and Juvenile Fishes for Clearing and Double Staining SO COPEIA LA English DT Article ID FORMALIN CONCENTRATION; PRESERVATION; LENGTH; SHRINKAGE; SALINITY AB The fixation of larval and juvenile fishes in 95% ethanol can be substituted for formalin and bears several advantages for morphological and molecular studies: 1) specimens clear and double stain rapidly and brilliantly; 2) otoliths are preserved; and 3) high-quality DNA is available from the tissues. We present merits and limitations of 70% ethanol and 95% ethanol as alternative fixatives to 4% buffered formalin. In particular, we compare our results of clearing and double staining teleost larvae and juveniles from these three fixatives and those that have been frozen at -20 degrees C prior to the initial fixation. With our results, we can refute the long-standing notion that ethanol-fixed specimens disintegrate during clearing and staining. C1 [Schnell, Nalani K.] Sorbonne Univ, Univ Paris 06, CNRS,EPHE, Inst Systemat,Evolut,Biodivers,ISYEB,UMR 7205,MNH, 57 Rue Cuvier,CP 30, F-75005 Paris, France. [Konstantinidis, Peter] Coll William & Mary, Virginia Inst Marine Sci, Dept Fisheries Sci, POB 1346,Rt 1208 Greate Rd, Gloucester Point, VA 23062 USA. [Johnson, G. David] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, POB 37012,MRC 0159, Washington, DC 20013 USA. RP Schnell, NK (reprint author), Sorbonne Univ, Univ Paris 06, CNRS,EPHE, Inst Systemat,Evolut,Biodivers,ISYEB,UMR 7205,MNH, 57 Rue Cuvier,CP 30, F-75005 Paris, France. EM nschnell@mnhn.fr; peterk@vims.edu; johnsond@si.edu NR 26 TC 0 Z9 0 U1 9 U2 9 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD OCT PY 2016 VL 104 IS 3 BP 617 EP 622 DI 10.1643/CI-15-382 PG 6 WC Zoology SC Zoology GA DY9CH UT WOS:000385429700001 ER PT J AU Smith, DG Schwarzhans, WW Pogonoski, JJ AF Smith, David G. Schwarzhans, Werner W. Pogonoski, John J. TI The Identity of Conger japonicus Bleeker, 1879 (Anguilliformes: Congridae) SO COPEIA LA English DT Article AB The number of species of the congrid eel genus Conger in Japan has been unsettled for more than half a century. The principal authors have disagreed over how many species are present and what their correct names are. The main question involves the identity of Conger japonicus Bleeker, 1879. It has variously been treated as a valid species or a synonym of Conger myriaster (Brevoort, 1856). We examined the holotype and determined that Conger japonicus is a synonym of Conger myriaster. The four valid species of Conger in Japan are Conger cinereus, Conger myriaster, Conger erebennus, and Conger jordani. C1 [Smith, David G.] Smithsonian Inst, Museum Support Ctr, MSC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. [Schwarzhans, Werner W.] Nat Hist Museum Denmark, Zool Museum, Univ Pk 15, DK-2100 Copenhagen, Denmark. [Pogonoski, John J.] CSIRO Natl Res Collect Australia, Australian Natl Fish Collect, GPO Box 1538, Hobart, Tas 7001, Australia. RP Smith, DG (reprint author), Smithsonian Inst, Museum Support Ctr, MSC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM smithd@si.edu; wwschwarz@aol.com; john.pogonoski@csiro.au RI Pogonoski, John /E-1710-2017 NR 9 TC 0 Z9 0 U1 5 U2 5 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD OCT PY 2016 VL 104 IS 3 BP 734 EP 737 DI 10.1643/CI-16-408 PG 4 WC Zoology SC Zoology GA DY9CH UT WOS:000385429700017 ER PT J AU Rifai, SW Munoz, JDU Negron-Juarez, RI Arevalo, FRR Tello-Espinoza, R Vanderwel, MC Lichstein, JW Chambers, JQ Bohlman, SA AF Rifai, Sami W. Urquiza Munoz, Jose D. Negron-Juarez, Robinson I. Ramirez Arevalo, Fredy R. Tello-Espinoza, Rodil Vanderwel, Mark C. Lichstein, Jeremy W. Chambers, Jeffrey Q. Bohlman, Stephanie A. TI Landscape-scale consequences of differential tree mortality from catastrophic wind disturbance in the Amazon SO ECOLOGICAL APPLICATIONS LA English DT Article DE Amazon; blowdown; canopy gap; downburst; INLA; Iquitos; Loreto; necromass; selective mortality; spectral mixture analysis; tree mortality; wind disturbance; windthrow; wood density ID TROPICAL RAIN-FOREST; WOOD DENSITY; LARGE BLOWDOWNS; MODELS; GROWTH; DAMAGE; WINDTHROW; DROUGHT; MOUNTAINS; WORLDWIDE AB Wind disturbance can create large forest blowdowns, which greatly reduces live biomass and adds uncertainty to the strength of the Amazon carbon sink. Observational studies from within the central Amazon have quantified blowdown size and estimated total mortality but have not determined which trees are most likely to die from a catastrophic wind disturbance. Also, the impact of spatial dependence upon tree mortality from wind disturbance has seldom been quantified, which is important because wind disturbance often kills clusters of trees due to large treefalls killing surrounding neighbors. We examine (1) the causes of differential mortality between adult trees from a 300-ha blowdown event in the Peruvian region of the northwestern Amazon, (2) how accounting for spatial dependence affects mortality predictions, and (3) how incorporating both differential mortality and spatial dependence affect the landscape level estimation of necromass produced from the blowdown. Standard regression and spatial regression models were used to estimate how stem diameter, wood density, elevation, and a satellite-derived disturbance metric influenced the probability of tree death from the blowdown event. The model parameters regarding tree characteristics, topography, and spatial autocorrelation of the field data were then used to determine the consequences of non-random mortality for landscape production of necromass through a simulation model. Tree mortality was highly non-random within the blowdown, where tree mortality rates were highest for trees that were large, had low wood density, and were located at high elevation. Of the differential mortality models, the non-spatial models overpredicted necromass, whereas the spatial model slightly underpredicted necromass. When parameterized from the same field data, the spatial regression model with differential mortality estimated only 7.5% more dead trees across the entire blowdown than the random mortality model, yet it estimated 51% greater necromass. We suggest that predictions of forest carbon loss from wind disturbance are sensitive to not only the underlying spatial dependence of observations, but also the biological differences between individuals that promote differential levels of mortality. C1 [Rifai, Sami W.; Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Urquiza Munoz, Jose D.; Ramirez Arevalo, Fredy R.; Tello-Espinoza, Rodil] Univ Nacl Amazonia Peruana, Fac Ciencias Forestales, Iquitos, Peru. [Negron-Juarez, Robinson I.; Chambers, Jeffrey Q.] Lawrence Berkeley Natl Lab, Climate Sci Dept, Div Earth Sci, Berkeley, CA 94720 USA. [Vanderwel, Mark C.] Univ Regina, Dept Biol, 3737 Wascana Pkwy, Regina, SK S4S 0A2, Canada. [Lichstein, Jeremy W.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Chambers, Jeffrey Q.] Univ Calif Berkeley, Dept Geog, Berkeley, CA 94720 USA. [Chambers, Jeffrey Q.] Inst Nacl de Pesquisas da Amazonia, Coordenacao Pesquisas Silvicultura Trop, BR-69060001 Manaus, Amazonas, Brazil. [Bohlman, Stephanie A.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. RP Rifai, SW (reprint author), Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. EM srifai@gmail.com FU NASA Biodiversity Program [NNX09AK21G]; NASA Earth and Space Science Graduate Fellowship; Next-Generation Ecosystems Experiments-Tropics (NGEE Tropics); Regional and Global Climate Modeling (RGCM) program - U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research FX Conducted research was funded by the NASA Biodiversity Program (Project NNX09AK21G). S. W. Rifai was supported by a NASA Earth and Space Science Graduate Fellowship. R. Negron-Juarez was supported by Next-Generation Ecosystems Experiments-Tropics (NGEE Tropics) and the Regional and Global Climate Modeling (RGCM) program funded by the U.S. Department of Energy, Office of Science, Office of Biological and Environmental Research. We greatly acknowledge the field assistance of Jarli Isuiza, Pablo Marin Ruiz, and Randal Regnifo. We also thank two anonymous reviewers for comments that improved the manuscript. NR 53 TC 0 Z9 0 U1 10 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD OCT PY 2016 VL 26 IS 7 BP 2225 EP 2237 DI 10.1002/eap.1368 PG 13 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA DZ1TR UT WOS:000385623900020 PM 27755720 ER PT J AU Williams, MR Wessel, BM Filoso, S AF Williams, Michael R. Wessel, Barret M. Filoso, Solange TI Sources of iron (Fe) and factors regulating the development of flocculate from Fe-oxidizing bacteria in regenerative streamwater conveyance structures SO ECOLOGICAL ENGINEERING LA English DT Article DE Best management practice (BMP); Coastal plain; Flocculate; Iron-oxidizing bacteria (FeOB); Piedmont; Regenerative streamwater conveyance (RSC); Stream restoration ID ECOSYSTEM SERVICES; RESTORATION; SCIENCE; EXPORT AB Regenerative streamwater conveyances (RSCs) are a relatively new stream restoration best management practice (BMP) being extensively implemented in degraded perennial streams and stormwater drainages throughout the mid-Atlantic. Although there is currently a great deal of interest in this type of BMP as a means of reducing nutrient and sediment export from disturbed catchments, little is known of its pollutant reduction capabilities and whether there are unintended ecological consequences associated with these structures. For example, dense accumulations of flocculate from iron-oxidizing bacteria (FeOB) have been observed at numerous RSC sites, yet it is unknown whether this flocculate is predominately natural, a consequence of leached iron (Fe) from the materials used in the RSC construction, or because of mobilized Fe from catchment soils influenced by higher groundwater levels that may occur after construction. We analyzed Fe and other solute concentrations in groundwater and perennial streams at RSC and control sites located in the Coastal Plain and Piedmont physiographic provinces of MD and DC, and conducted leaching experiments using RSC soils and construction materials. Iron flocculate from FeOB in RSCs is commonly localized and depends on several factors including a source of reduced Fe, the availability of dissolved organic carbon (DOC), and specific hydrological (i.e., low flow) and physical (i.e., warmer temperatures) conditions. Sources of reduced Fe are derived from both construction materials and catchment soils, which leach Fe in the presence of DOC originating from natural organic matter (OM) deposits and OM incorporated into the RSCs (i.e., wood chips, leaves, logs). Using construction materials that have relatively low Fe content in areas strongly influenced by OM will likely decrease the spatial and temporal presence of dense mats of Fe flocculate thereby improving stream habitat. (C) 2016 Elsevier B.V. All rights reserved. C1 [Williams, Michael R.; Filoso, Solange] Univ Maryland, Chesapeake Biol Lab, Ctr Environm Sci, Solomons, MD 20688 USA. [Wessel, Barret M.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20742 USA. RP Williams, MR (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM williamsmi@si.edu FU District Department of Energy and the Environment (DOEE) [12G-12-NFWF-UMCES/WPD-2]; Maryland Sea Grant (REU program); NOAA [NA10OAR4310221]; National Science Foundation (REU) FX Support for this project was provided by the District Department of Energy and the Environment (DOEE) (grant # 12G-12-NFWF-UMCES/WPD-2), Maryland Sea Grant (REU program), NOAA (grant # NA10OAR4310221), and the National Science Foundation (REU student/mentor travel award). We thank Steve Saari and Joe Berg for assistance with site selection, as well as Peter May and Delvin Fanning for constructive input on the REU project. Rosemary Ury and Jake Kames provided lab and field assistance. This manuscript benefited from the constructive comments of DOEE staff and two anonymous reviewers. NR 51 TC 0 Z9 0 U1 4 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0925-8574 EI 1872-6992 J9 ECOL ENG JI Ecol. Eng. PD OCT PY 2016 VL 95 BP 723 EP 737 DI 10.1016/j.ecoleng.2016.06.120 PG 15 WC Ecology; Engineering, Environmental; Environmental Sciences SC Environmental Sciences & Ecology; Engineering GA DY8HX UT WOS:000385371400084 ER PT J AU Stockey, RA Rothwell, GW Johnson, KR AF Stockey, Ruth A. Rothwell, Gar W. Johnson, Kirk R. TI EVALUATING RELATIONSHIPS AMONG FLOATING AQUATIC MONOCOTS: A NEW SPECIES OF COBBANIA (ARACEAE) FROM THE UPPER MAASTRICHTIAN OF SOUTH DAKOTA SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Alismatales; aquatic angiosperms; Araceae; Cobbania; Cretaceous; fossil ID CRETACEOUS-TERTIARY BOUNDARY; SP-NOV NYMPHAEACEAE; PHYLOGENETIC-RELATIONSHIPS; NORTH-DAKOTA; FAMILY ARACEAE; MIDDLE EOCENE; HELL CREEK; SEED COAT; HYDROCHARITACEAE; FOSSIL AB Premise of research. A large number of floating aquatic aroid fossils have been recovered from pond sediments in the Hell Creek Formation (Upper Cretaceous) of South Dakota, providing valuable new data about aquatic vegetation of the uppermost Cretaceous, that are used to describe a new species of the genus Cobbania, and to evaluate associated reproductive structures and phylogenetic relationships among floating aquatic monocots. Methodology. Fossils were uncovered as needed with fine needles to reveal surface features of the specimens. Images were captured with a digital scanning camera, and phylogenetic analyses were conducted with TNT implemented through WinClada. Pivotal results. The new species, Cobbania hickeyi Stockey, Rothwell & Johnson, extends the range of the genus to the uppermost Cretaceous, supports the taxonomic integrity of the genus Cobbania, and increases our understanding of structural variation and species richness within the genus. Associated reproductive structures include an aroid spadix, strengthening the assignment of Cobbania to the Araceae. Phylogenetic analyses using "total-evidence" data help resolve conflicting results from either morphological or nucleotide sequence analyses of relationships among floating aquatic aroids, and the fossil taxon Aquaephyllum does not nest among the other floating aquatic species in any of our results. Conclusions. Species of the genus Cobbania were an important component of aquatic vegetation across the Northern Hemisphere during the Late Cretaceous. In tests of competing hypotheses for relationships among Pistia stratiotes, Cobbania spp., and species of Araceae subfamily Lemnoideae, the results from a "total-evidence" analysis suggest that specializations for the floating aquatic life form may be overwhelming other characters in the results of morphological analyses alone. C1 [Stockey, Ruth A.; Rothwell, Gar W.] Oregon State Univ, Dept Bot & Plant Pathol, 2082 Cordley Hall, Corvallis, OR 97331 USA. [Rothwell, Gar W.] Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. [Johnson, Kirk R.] Smithsonian Inst, Natl Museum Nat Hist, MRC 106,POB 37012, Washington, DC 20013 USA. RP Stockey, RA (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, 2082 Cordley Hall, Corvallis, OR 97331 USA. EM stockeyr@science.oregonstate.edu NR 50 TC 0 Z9 0 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 EI 1537-5315 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD OCT PY 2016 VL 177 IS 8 BP 706 EP 725 DI 10.1086/688285 PG 20 WC Plant Sciences SC Plant Sciences GA DZ0ZM UT WOS:000385568200006 ER PT J AU Uribe, MC Grier, HJ Garcia-Alarcon, A Parenti, LR AF Carmen Uribe, Mari Grier, Harry J. Garcia-Alarcon, Adriana Parenti, Lynne R. TI Oogenesis: From Oogonia to Ovulation in the Flagfish, Jordanella floridae Goode and Bean, 1879 (Teleostei:Cyprinodontidae) SO JOURNAL OF MORPHOLOGY LA English DT Article DE asynchronous spawning; germinal epithelium; fluid yolk; ovarian cycle; micropyle ID OVARIAN GERMINAL EPITHELIUM; FUNDULUS-HETEROCLITUS; OOCYTE DEVELOPMENT; FOLLICULAR ATRESIA; TELEOST FISH; ONCORHYNCHUS-MYKISS; CORTICAL ALVEOLI; GERMLINE CYSTS; RAINBOW-TROUT; COMMON SNOOK AB We provide histological details of the development of oocytes in the cyprinodontid flagfish, Jordanella floridae. There are six stages of oogenesis: Oogonial proliferation, chromatin nucleolus, primary growth (previtellogenesis [PG]), secondary growth (vitellogenesis), oocyte maturation and ovulation. The ovarian lamellae are lined by a germinal epithelium composed of epithelial cells and scattered oogonia. During primary growth, the development of cortical alveoli and oil droplets, are initiated simultaneously. During secondary growth, yolk globules coalesce into a fluid mass. The full-grown oocyte contains a large globule of fluid yolk. The germinal vesicle is at the animal pole, and the cortical alveoli and oil droplets are located at the periphery. The disposition of oil droplets at the vegetal pole of the germinal vesicle during late secondary growth stage is a unique characteristic. The follicular cell layer is composed initially of a single layer of squamous cells during early PG which become columnar during early vitellogenesis. During primary and secondary growth stages, filaments develop among the follicular cells and also around the micropyle. The filaments are seen extending from the zona pellucida after ovulation. During ovulation, a space is evident between the oocyte and the zona pellucida. Asynchronous spawning activity is confirmed by the observation that, after ovulation, the ovarian lamellae contain follicles in both primary and secondary growth stages; in contrast, when the seasonal activity of oogenesis and spawning ends, after ovulation, the ovarian lamellae contain only follicles in the primary growth stage. J. Morphol. 277:1339-1354, 2016. (c) 2016 Wiley Periodicals, Inc. C1 [Carmen Uribe, Mari; Garcia-Alarcon, Adriana] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Biol Comparada, Mexico City 04510, DF, Mexico. [Grier, Harry J.] Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. [Grier, Harry J.; Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Uribe, MC (reprint author), Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Biol Comparada, Mexico City 04510, DF, Mexico. EM mari3uribe3@gmail.com NR 69 TC 0 Z9 0 U1 4 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD OCT PY 2016 VL 277 IS 10 BP 1339 EP 1354 DI 10.1002/jmor.20580 PG 16 WC Anatomy & Morphology SC Anatomy & Morphology GA DW4CK UT WOS:000383589500007 PM 27418385 ER PT J AU Watters, TR Daud, K Banks, ME Selvans, MM Chapman, CR Ernst, CM AF Watters, Thomas R. Daud, Katie Banks, Maria E. Selvans, Michelle M. Chapman, Clark R. Ernst, Carolyn M. TI Recent tectonic activity on Mercury revealed by small thrust fault scarps SO NATURE GEOSCIENCE LA English DT Article ID RECONNAISSANCE ORBITER CAMERA; INNER SOLAR-SYSTEM; IMPACT CRATERS; LUNAR; MOON; MESSENGER; VOLCANISM; REGOLITH; STRESSES; RATES AB Large tectonic landforms on the surface of Mercury, consistent with significant contraction of the planet, were revealed by the flybys of Mariner 10 in the mid-1970s(1). The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission confirmed that the planet's past 4 billion years of tectonic history have been dominated by contraction expressed by lobate fault scarps that are hundreds of kilometres long2-5. Here we report the discovery of small thrust fault scarps in images from the low-altitude campaign at the end of the MESSENGER mission that are orders of magnitude smaller than the large-scale lobate scarps. These small scarps have tens of metres of relief, are only kilometres in length and are comparable in scale to small young scarps on the Moon6-8. Their small-scale, pristine appearance, crosscutting of impact craters and association with small graben all indicate an age of less than 50Myr. We propose that these scarps are the smallest members of a continuum in scale of thrust fault scarps on Mercury. The young age of the small scarps, along with evidence for recent activity on large-scale scarps, suggests that Mercury is tectonically active today and implies a prolonged slow cooling of the planet's interior. C1 [Watters, Thomas R.; Daud, Katie; Banks, Maria E.; Selvans, Michelle M.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Banks, Maria E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Chapman, Clark R.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO 80302 USA. [Ernst, Carolyn M.] Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. RP Watters, TR (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. EM watterst@si.edu FU NASA [NNX07AR60G] FX We thank P. D. Spudis and A. Nahm for helpful comments and suggestions that greatly improved the manuscript. We also thank C. Johnson for valuable discussions. We are grateful to S. C. Solomon, the MDIS team, and the MESSENGER engineers, and technical support personnel at Johns Hopkins University Applied Physics Laboratory. This work is also supported by NASA grant NNX07AR60G. NR 32 TC 0 Z9 0 U1 4 U2 4 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD OCT PY 2016 VL 9 IS 10 BP 743 EP 747 DI 10.1038/NGEO2814 PG 5 WC Geosciences, Multidisciplinary SC Geology GA DY8IL UT WOS:000385373000007 ER PT J AU Demars, BOL Gislason, GM Olafsson, JS Manson, JR Friberg, N Hood, JM Thompson, JJD Freitag, TE AF Demars, Benoit O. L. Gislason, Gisli M. Olafsson, Jon S. Manson, J. Russell Friberg, Nikolai Hood, James M. Thompson, Joshua J. D. Freitag, Thomas E. TI Impact of warming on CO2 emissions from streams countered by aquatic photosynthesis SO NATURE GEOSCIENCE LA English DT Article ID TEMPERATURE-DEPENDENCE; METABOLIC BALANCE; LAND-USE; CONCENTRATING MECHANISMS; PRIMARY PRODUCTIVITY; DISSOLVED-OXYGEN; ALGAL GROWTH; RESPIRATION; ECOSYSTEM; RUBISCO AB Streams and rivers are an important source of CO2 emissions(1). One important control of these emissions is the metabolic balance between photosynthesis, which converts CO2 to organic carbon, and respiration, which converts organic carbon into CO2 (refs2,3). Carbon emissions from rivers could increase with warming, independently of organic carbon inputs, because the apparent activation energy is predicted to be higher for respiration than photosynthesis(4,5). However, physiological CO2-concentrating mechanisms may prevent the increase in photorespiration, limiting photosynthesis with warming(6). Here we report the thermal response of aquatic photosynthesis from streams located in geothermal areas of North America, Iceland and Kamchatka with water temperatures ranging between 4 and 70 degrees C. Based on a thermodynamic theory of enzyme kinetics, we show that the apparent activation energy of aquatic ecosystem photosynthesis is approximately 0.57 electron volts (eV) for temperatures ranging from 4 to 45 degrees C, which is similar to that of respiration(4,5,7-9). This result and a global synthesis of 222 streams suggest that warming will not create increased stream and river CO2 emissions from a warming-induced imbalance between photosynthesis and respiration. However, temperature could affect annual CO2 emissions from streams if ecosystem respiration is independent of gross primary production, and may be amplified by increasing organic carbon supply. C1 [Demars, Benoit O. L.; Freitag, Thomas E.] James Hutton Inst, Aberdeen AB15 8QH, Scotland. [Gislason, Gisli M.] Univ Iceland, Inst Life & Environm Sci, Sturlugata 7, IS-101 Reykjavik, Iceland. [Olafsson, Jon S.] Marine & Freshwater Res Inst, Arleyni 22, IS-112 Reykjavik, Iceland. [Manson, J. Russell] Stockton Univ, Appl Phys, Galloway, NJ 08205 USA. [Friberg, Nikolai] Norwegian Inst Water Res, Gaustaallen 21, N-0349 Oslo, Norway. [Friberg, Nikolai] Univ Leeds, Sch Geog, Water Leeds, Leeds LS2 9JT, W Yorkshire, England. [Hood, James M.] Montana State Univ, Dept Ecol, Bozeman, MT 59717 USA. [Thompson, Joshua J. D.] Bangor Univ, Sch Environm Nat Resources & Geog, Deiniol Rd, Bangor LL57 2UW, Gwynedd, Wales. [Hood, James M.] Ohio State Univ, Aquat Ecol Lab, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43212 USA. [Thompson, Joshua J. D.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. RP Demars, BOL (reprint author), James Hutton Inst, Aberdeen AB15 8QH, Scotland. EM benoit.demars@hutton.ac.uk RI Gislason, Gisli /B-2109-2008 OI Gislason, Gisli /0000-0001-8507-1796 FU Scottish Government Rural and Environmental Science and Analytical Services (RESAS); Icelandic National Power Company's Energy and Environmental Fund; Stockton University; AU IDEAS; Icelandic Research Fund (i. Rannsoknasjoour) [141840-051]; NERC [NE/J011967/1] FX We wish to thank the park rangers for permission to work in Iceland and Kamchatka; B. Marteau, R. Magnusdottir, D. Arnadottir, Yu. Bespalaya, O. Usacheva, A. Kondakov and I. Bolotov for help with fieldwork; and Y. Cook, H. Watson, L. Johnson, S. McIntyre for processing water chemical analyses. B.O.L.D. and T.E.F. were funded by the Scottish Government Rural and Environmental Science and Analytical Services (RESAS). J.S.O., G.M.G. and B.O.L.D. were funded by the Icelandic National Power Company's Energy and Environmental Fund. J.R.M. was funded by Stockton University. N.F. and the travel to Kamchatka were partly funded by AU IDEAS. J.M.H. was supported by the Icelandic Research Fund (i. Rannsoknasjoour) 141840-051 during manuscript preparation. J.J.D.T. was funded by NERC grant NE/J011967/1. Comments by S. Maberly and J. Kemp improved the manuscript. NR 63 TC 0 Z9 0 U1 23 U2 23 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD OCT PY 2016 VL 9 IS 10 BP 758 EP + DI 10.1038/NGEO2807 PG 6 WC Geosciences, Multidisciplinary SC Geology GA DY8IL UT WOS:000385373000010 ER PT J AU Zalamea, PC Turner, BL Winter, K Jones, FA Sarmiento, C Dalling, JW AF Zalamea, Paul-Camilo Turner, Benjamin L. Winter, Klaus Jones, F. Andrew Sarmiento, Carolina Dalling, James W. TI Seedling growth responses to phosphorus reflect adult distribution patterns of tropical trees SO NEW PHYTOLOGIST LA English DT Article DE phosphatase activity; phosphorus limitation; pioneer trees; plant communities; plant growth; species distributions; tropical soil resources ID HABITAT SPECIALIZATION; RAIN-FORESTS; NUTRIENT AVAILABILITY; DECIDUOUS FOREST; SOIL NUTRIENTS; PIONEER TREE; NITROGEN; PHYLOGENETICS; DIVERSITY; BORNEO AB Soils influence tropical forest composition at regional scales. In Panama, data on tree communities and underlying soils indicate that species frequently show distributional associations to soil phosphorus. To understand how these associations arise, we combined a pot experiment to measure seedling responses of 15 pioneer species to phosphorus addition with an analysis of the phylogenetic structure of phosphorus associations of the entire tree community. Growth responses of pioneers to phosphorus addition revealed a clear tradeoff: species from high-phosphorus sites grew fastest in the phosphorus-addition treatment, while species from low-phosphorus sites grew fastest in the low-phosphorus treatment. Traits associated with growth performance remain unclear: biomass allocation, phosphatase activity and phosphorus-use efficiency did not correlate with phosphorus associations; however, phosphatase activity was most strongly down-regulated in response to phosphorus addition in species from high-phosphorus sites. Phylogenetic analysis indicated that pioneers occur more frequently in clades where phosphorus associations are overdispersed as compared with the overall tree community, suggesting that selection on phosphorus acquisition and use may be strongest for pioneer species with high phosphorus demand. Our results show that phosphorus-dependent growth rates provide an additional explanation for the regional distribution of tree species in Panama, and possibly elsewhere. C1 [Zalamea, Paul-Camilo; Turner, Benjamin L.; Winter, Klaus; Jones, F. Andrew; Sarmiento, Carolina; Dalling, James W.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. [Jones, F. Andrew] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. RP Zalamea, PC (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM camilozalamea@gmail.com RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Sarmiento, Carolina/0000-0002-8575-7170 FU University of Illinois; Oregon State University; National Science Foundation [DEB 1257976] FX J.W.D. acknowledges support from the University of Illinois, F.A.J. acknowledges support from Oregon State University and the National Science Foundation (DEB 1257976). N. Swenson provided R code for phylogenetic analyses. We thank P. Escobar, A. Bielnicka, C. Delevich, J. Perez and D. Agudo for laboratory assistance and J. Aranda, D. Rincon and J. Salas for assistance in the pot experiment. This manuscript was improved by valuable comments from J. O'Dwyer, R. Condit, M. Slot, M. Sheldrake, K. Heineman, and three anonymous reviewers. NR 49 TC 1 Z9 1 U1 5 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD OCT PY 2016 VL 212 IS 2 BP 400 EP 408 DI 10.1111/nph.14045 PG 9 WC Plant Sciences SC Plant Sciences GA DW4EQ UT WOS:000383595700015 PM 27282142 ER PT J AU Olson, SL Lund, JN AF Olson, Storrs L. Lund, Judith N. TI Additional references to "woggin" as a name for penguins SO ARCHIVES OF NATURAL HISTORY LA English DT Article C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Dept Vertebrate Zool, NHB MRC 116,POB 37012, Washington, DC 20013 USA. [Lund, Judith N.] 7 Middle St, Dartmouth, MA 02748 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Dept Vertebrate Zool, NHB MRC 116,POB 37012, Washington, DC 20013 USA. EM olsons@si.edu; jnlund@comcast.net NR 5 TC 0 Z9 0 U1 1 U2 1 PU EDINBURGH UNIV PRESS PI EDINBURGH PA THE TUN-HOLYROOD RD, 12 2F JACKSONS ENTRY, EDINBURGH EH8 8PJ, SCOTLAND SN 0260-9541 EI 1755-6260 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2016 VL 43 IS 2 BP 360 EP 362 DI 10.3366/anh.2016.0392 PG 3 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA DX8IN UT WOS:000384631400015 ER PT J AU Waters, LE Andrews, BJ AF Waters, Laura E. Andrews, Benjamin J. TI The role of superheating in the formation of Glass Mountain obsidians (Long Valley, CA) inferred through crystallization of sanidine SO CONTRIBUTIONS TO MINERALOGY AND PETROLOGY LA English DT Article DE Obsidian; Rhyolite; Sanidine; Crystallization; Superheating; Long Valley ID DECOMPRESSION-INDUCED CRYSTALLIZATION; DEGASSING-INDUCED CRYSTALLIZATION; SILICIC MAGMA SYSTEM; BISHOP TUFF; EXPERIMENTAL CONSTRAINTS; RESIDENCE TIMES; RHYOLITIC MAGMA; PRECALDERA LAVAS; ISOTOPIC RECORD; PHASE-RELATIONS AB The Glass Mountain obsidians (Long Valley, CA) are crystal poor (<8 vol%) and highly evolved (high SiO2, low Sr), and therefore, their formation required extremely efficient separation of melts from a crystal-rich source. A petrologic and experimental investigation of the mineral phases in Glass Mountain lavas identifies conditions under which phenocrysts grew and the driving mechanism for crystallization, which places constraints on the possible processes that generated the obsidians. The obsidian in this study (GM-11) is saturated in nine phases (sanidine + quartz + plagioclase + titanomagnetite + ilmenite + zircon + apatite + allanite + biotite), and results of high-resolution SEM compositional mapping and electron microprobe analysis reveal that individual sanidine crystals are normally zoned and span a range of compositions (Or40-78). Sanidines have a "granophyric" texture, characterized by intergrowths of quartz and sanidine. Mineral phases in the natural sample are compared to H2O-saturated phase equilibrium experiments conducted in cold-seal pressure vessels, over a range of conditions (700-850 degrees C; 75-225 MPa), and all are found to be plausible phenocrysts. Comparison of sanidine compositions from the natural sample with those grown in phase equilibrium experiments demonstrates that sanidine in the natural sample occurs in a reduced abundance. Further comparison with phase equilibrium experiments suggests that sanidine compositions track progressive loss of dissolved melt water (+/- cooling), suggesting that crystallization in the natural obsidian was driven predominantly by degassing resulting from decompression. It is paradoxical that an effusively (slowly) erupted lava should contain multiple phenocryst phases, including sanidine crystals that span a range of compositions with granophyric textures, and yet remain so crystal poor. To resolve this paradox, it is necessary that the solidification mechanism (degassing or cooling) that produced the sanidine crystals (and other mineral phases) must have an associated kinetic effect(s) that efficiently hinders crystal nucleation and growth. Decompression experiments conducted in this study and from the literature collectively demonstrate that the simplest way to inhibit nucleation during degassing-induced crystallization is to initiate degassing +/- cooling from superliquidus conditions, and therefore, the Glass Mountain obsidians were superheated prior to crystallization. C1 [Waters, Laura E.; Andrews, Benjamin J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th St & Constitut Ave NW, Washington, DC 20560 USA. RP Waters, LE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th St & Constitut Ave NW, Washington, DC 20560 USA. EM watersl@si.edu FU Smithsonian Institution National Museum of Natural History Peter S. Buck Postdoctoral Scholarship Program FX Stephanie Grocke is thanked for extensive discussion and feedback on this manuscript. Gail Mahood is thanked for lively discussion and feedback following presentation of this paper at AGU 2015. Silvio Mollo, Matteo Masotta and an anonymous third and fourth reviewers are sincerely thanked for extensive, constructive feedback, which significantly improved this manuscript. Becky Lange, James Jolles and John Naliboff are additionally thanked for assistance with field work. Funding for this work was provided by the Smithsonian Institution National Museum of Natural History Peter S. Buck Postdoctoral Scholarship Program. NR 55 TC 0 Z9 0 U1 4 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0010-7999 EI 1432-0967 J9 CONTRIB MINERAL PETR JI Contrib. Mineral. Petrol. PD OCT PY 2016 VL 171 IS 10 AR 79 DI 10.1007/s00410-016-1291-3 PG 19 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA DY5RB UT WOS:000385158300002 ER PT J AU Choo, SW Rayko, M Tan, TK Hari, R Komissarov, A Wee, WY Yurchenko, AA Kliver, S Tamazian, G Antunes, A Wilson, RK Warren, WC Koepfli, KP Minx, P Krasheninnikova, K Kotze, A Dalton, DL Vermaak, E Paterson, IC Dobrynin, P Sitam, FT Rovie-Ryan, JJ Johnson, WE Yusoff, AM Luo, SJ Karuppannan, KV Fang, G Zheng, D Gerstein, MB Lipovich, L O'Brien, SJ Wong, GJ AF Choo, Slew Woh Rayko, Mike Tan, Tze King Hari, Ranjeev Komissarov, Aleksey Wee, Wei Yee Yurchenko, Andrey A. Kliver, Sergey Tamazian, Gaik Antunes, Agostinho Wilson, Richard K. Warren, Wesley C. Koepfli, Klaus-Peter Minx, Patrick Krasheninnikova, Ksenia Kotze, Antoinette Dalton, Desire L. Vermaak, Elaine Paterson, Ian C. Dobrynin, Pavel Sitam, Frankie Thomas Rovie-Ryan, Jeffrine J. Johnson, Warren E. Yusoff, Aini Mohamed Luo, Shu-Jin Karuppannan, Kayal Vizi Fang, Gang Zheng, Deyou Gerstein, Mark B. Lipovich, Leonard O'Brien, Stephen J. Wong, Guat Jah TI Pangolin genomes and the evolution of mammalian scales and immunity SO GENOME RESEARCH LA English DT Article ID FIBER CELL CYTOSKELETON; INTERFERON-EPSILON; BURKHOLDERIA-PSEUDOMALLEI; INFECTION; LENS; SEQUENCE; MUTATION; MUCOSAL; CP49; TOOL AB Pangolins, unique mammals with scales over most of their body, no teeth, poor vision, and an acute olfactory system, comprise the only placental order (Pholidota) without a whole-genome map. To investigate pangolin biology and evolution, we developed genome assemblies of the Malayan (Manis javanica) and Chinese (M. pentadactyla) pangolins. Strikingly, we found that interferon epsilon (IFNE), exclusively expressed in epithelial cells and important in skin and mucosal immunity, is pseudogenized in all African and Asian pangolin species that we examined, perhaps impacting resistance to infection. We propose that scale development was an innovation that provided protection against injuries or stress and reduced pangolin vulnerability to infection. Further evidence of specialized adaptations was evident from positively selected genes involving immunity-related pathways, inflammation, energy storage and metabolism, muscular and nervous systems, and scale/hair development. Olfactory receptor gene families are significantly expanded in pangolins, reflecting their well-developed olfaction system. This study provides insights into mammalian adaptation and functional diversification, new research tools and questions, and perhaps a new natural IFNE-deficient animal model for studying mammalian immunity. C1 [Choo, Slew Woh; Tan, Tze King; Hari, Ranjeev; Wee, Wei Yee; Yusoff, Aini Mohamed; Wong, Guat Jah] Univ Malaya, Ctr Res Biotechnol Agr CEBAR, Genome Informat Res Lab, Kuala Lumpur 50603, Malaysia. [Choo, Slew Woh; Tan, Tze King; Hari, Ranjeev; Wee, Wei Yee; Paterson, Ian C.; Yusoff, Aini Mohamed] Univ Malaya, Fac Dent, Dept Oral & Craniofacial Sci, Kuala Lumpur 50603, Malaysia. [Choo, Slew Woh] Univ Malaya, Genome Solut Sdn Bhd, Res Management & Innovat Complex, Kuala Lumpur 50603, Malaysia. [Rayko, Mike; Komissarov, Aleksey; Yurchenko, Andrey A.; Kliver, Sergey; Tamazian, Gaik; Krasheninnikova, Ksenia; Dobrynin, Pavel; O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199004, Russia. [Antunes, Agostinho] Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, P-4050123 Oporto, Portugal. [Antunes, Agostinho] Univ Porto, Fac Sci, Dept Biol, P-4169007 Oporto, Portugal. [Wilson, Richard K.; Warren, Wesley C.; Minx, Patrick] Washington Univ, McDonnell Genome Inst, St Louis, MO 63108 USA. [Koepfli, Klaus-Peter; Johnson, Warren E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [Kotze, Antoinette; Dalton, Desire L.; Vermaak, Elaine] Natl Zool Gardens South Africa, ZA-0001 Pretoria, South Africa. [Kotze, Antoinette; Dalton, Desire L.] Univ Free State, Dept Genet, ZA-9300 Bloemfontein, South Africa. [Paterson, Ian C.] Univ Malaya, Fac Dent, Oral Canc Res & Coordinating Ctr, Kuala Lumpur 50603, Malaysia. [Sitam, Frankie Thomas; Rovie-Ryan, Jeffrine J.; Karuppannan, Kayal Vizi] Dept Wildlife & Natl Pk, Ex Situ Conservat Div, Kuala Lumpur 56100, Malaysia. [Luo, Shu-Jin] Peking Univ, Coll Life Sci, Peking Tsinghua Ctr Life Sci, Beijing 100871, Peoples R China. [Fang, Gang] NYU Shanghai, Shanghai 200122, Peoples R China. [Zheng, Deyou] Albert Einstein Coll Med, Dept Neurol, Bronx, NY 10461 USA. [Gerstein, Mark B.] Yale Univ, Program Computat Biol & Bioinformat, New Haven, CT 06520 USA. [Gerstein, Mark B.] Yale Univ, Dept Mol Biophys & Biochem, POB 6666, New Haven, CT 06520 USA. [Gerstein, Mark B.] Yale Univ, Dept Comp Sci, POB 2158, New Haven, CT 06520 USA. [Lipovich, Leonard] Wayne State Univ, Ctr Mol Med & Genet, Detroit, MI 48201 USA. [Lipovich, Leonard] Wayne State Univ, Sch Med, Dept Neurol, Detroit, MI 48201 USA. [O'Brien, Stephen J.] Nova Southeastern Univ, Oceanog Ctr, Ft Lauderdale, FL 33004 USA. RP Choo, SW (reprint author), Univ Malaya, Ctr Res Biotechnol Agr CEBAR, Genome Informat Res Lab, Kuala Lumpur 50603, Malaysia.; Choo, SW (reprint author), Univ Malaya, Fac Dent, Dept Oral & Craniofacial Sci, Kuala Lumpur 50603, Malaysia.; Choo, SW (reprint author), Univ Malaya, Genome Solut Sdn Bhd, Res Management & Innovat Complex, Kuala Lumpur 50603, Malaysia. EM l.choo@genomesolutions.com RI Paterson, Ian/G-8688-2011; Management Center, Dental Research/C-2478-2013; Tamazian, Gaik/P-4723-2015 OI Tamazian, Gaik/0000-0002-2931-1123 FU University of Malaya and Ministry of Education, Malaysia [UM.C/HIR/MOHE/08]; UMRG grant from the University of Malaya and Ministry of Education, Malaysia [RG541-13HTM]; Russian Ministry of Science [11.G34.31.0068]; NIH-NHGRI grant [5U54HG00307907] FX We thank Kerstin Lindblad-Toh and Jessica Alfoldi for generously providing guidance and sharing their advice. We also thank all members of the Genome Informatics Research Laboratory, University of Malaya in contributing to this research. Special thanks to Tan Shi Yang for providing IT and bioinformatics support in this project. This project was mainly supported by the University of Malaya and Ministry of Education, Malaysia, under the High Impact Research (HIR) grant UM.C/HIR/MOHE/08 and UMRG grant (grant number: RG541-13HTM) from the University of Malaya and Ministry of Education, Malaysia. This research was also supported in part by the Russian Ministry of Science (Mega grant no.11.G34.31.0068; S.J.O., Principal Investigator), and the funding to R.K.W. was provided by NIH-NHGRI grant 5U54HG00307907. NR 59 TC 0 Z9 0 U1 35 U2 35 PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT PI COLD SPRING HARBOR PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA SN 1088-9051 EI 1549-5469 J9 GENOME RES JI Genome Res. PD OCT PY 2016 VL 26 IS 10 BP 1312 EP 1322 DI 10.1101/gr.203521.115 PG 11 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity GA DY3BK UT WOS:000384965600002 PM 27510566 ER PT J AU Kral, K Shue, J Vrska, T Gonzalez-Akre, EB Parker, GG McShea, WJ McMahon, SM AF Kral, Kamil Shue, Jessica Vrska, Tomas Gonzalez-Akre, Erika B. Parker, Geoffrey G. McShea, William J. McMahon, Sean M. TI Fine-scale patch mosaic of developmental stages in Northeast American secondary temperate forests: the European perspective SO EUROPEAN JOURNAL OF FOREST RESEARCH LA English DT Article DE Forest cycle; Patch structure; Fine-scale mosaic; Developmental phases; Mean patch size; Successional dynamics ID CENTRAL NEW-ENGLAND; VEGETATION DYNAMICS; DECIDUOUS FORESTS; FAGUS-SYLVATICA; BEECH FORESTS; ABIES-ALBA; LAND-USE; COMPLEMENTARITY; BIODIVERSITY; CARPATHIANS AB Conceptual models that describe temperate forest dynamics differ substantially between Europe and America. In Europe, the concept of the forest cycle describes a sequentially shifting fine-scale mosaic of patches in different phases of forest development. In North America, the descriptive concept is largely based on severe coarse-scale disturbances that repeat in a cyclic fashion and restart the succession of the whole forest stand from initiation through to 'old-growth,' neglecting the within-stand dynamics on the patch level. Here, we investigate fine-scale stand structures across European and North American forests by applying the European concept of forest developmental phases to all stands. The patches of four major forest developmental stages were recognized and delineated by the spatially explicit rule-based classification system implemented in GIS, which employs stem position maps of live and dead trees for analysis. The basic quantitative characteristics of identified patch structures in the N. American stands, as the Mean Patch Size of the mosaic (between 760 and 890 m(2)), were comparable with European old-growth stands, although mosaic complexity was higher in the latter. We demonstrated that in addition to the large-scale forest cycle assumed by N. American conceptual models there simultaneously exist finer-scale patch dynamics described by the European conceptual model. We also demonstrated that the occurrence of the Steady State stage was promoted by higher local tree species richness, which may explain the abundant occurrence of this stage in N. American secondary stands. The Steady State stage of the European model might represent an important commonality across both paradigms. C1 [Kral, Kamil; Vrska, Tomas] Silva Tarouca Res Inst Landscape & Ornamental Gar, Dept Forest Ecol, Lidicka 25-27, Brno 60200, Czech Republic. [Shue, Jessica; Parker, Geoffrey G.; McMahon, Sean M.] Smithsonian Inst Forest Global Earth Observ, Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD USA. [Gonzalez-Akre, Erika B.; McShea, William J.] Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, 1500 Remount Rd, Front Royal, VA USA. RP Kral, K (reprint author), Silva Tarouca Res Inst Landscape & Ornamental Gar, Dept Forest Ecol, Lidicka 25-27, Brno 60200, Czech Republic. EM kamil.kral@vukoz.cz OI Parker, Geoffrey/0000-0001-7055-6491 FU Czech Ministry of Education, Youth and Sports [KONTAKT II-No. LH12038] FX We are grateful to all the people who participated in the forest plots censuses. Thanks to Petruska Dolezelova and Dusan Adam for technical support. The research was funded by the Czech Ministry of Education, Youth and Sports (Project KONTAKT II-No. LH12038). NR 69 TC 0 Z9 0 U1 4 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1612-4669 EI 1612-4677 J9 EUR J FOREST RES JI Eur. J. For. Res. PD OCT PY 2016 VL 135 IS 5 BP 981 EP 996 DI 10.1007/s10342-016-0988-1 PG 16 WC Forestry SC Forestry GA DX7MM UT WOS:000384571700015 ER PT J AU Marra, PR SanteIla, C AF Marra, Peter R. SanteIla, Chris TI Belling the Cat SO NATURAL HISTORY LA English DT Article C1 [Marra, Peter R.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Marra, PR (reprint author), Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. NR 0 TC 0 Z9 0 U1 2 U2 2 PU NATURAL HISTORY MAGAZINE PI NEW YORK PA 36 WEST 25TH STREET, FIFTH FLOOR, NEW YORK, NY 10010 USA SN 0028-0712 J9 NAT HIST JI Nat. Hist. PD OCT PY 2016 VL 124 IS 9 BP 22 EP 27 PG 6 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DX8JS UT WOS:000384634500011 ER PT J AU Christensen, GA Wymore, AM King, AJ Podar, M Hurt, RA Santillan, EU Soren, A Brandt, CC Brown, SD Palumbo, AV Wall, JD Gilmour, CC Elias, DA AF Christensen, Geoff A. Wymore, Ann M. King, Andrew J. Podar, Mircea Hurt, Richard A., Jr. Santillan, Eugenio U. Soren, Ally Brandt, Craig C. Brown, Steven D. Palumbo, Anthony V. Wall, Judy D. Gilmour, Cynthia C. Elias, Dwayne A. TI Development and Validation of Broad-Range Qualitative and Clade-Specific Quantitative Molecular Probes for Assessing Mercury Methylation in the Environment SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID METHYLMERCURY PRODUCTION; RELATIVE QUANTIFICATION; REDUCING BACTERIUM; GENE HGCA; SULFATE; TIME; SEQUENCE; MODEL; PCR; MICROORGANISMS AB Two genes, hgcA and hgcB, are essential for microbial mercury (Hg) methylation. Detection and estimation of their abundance, in conjunction with Hg concentration, bioavailability, and biogeochemistry, are critical in determining potential hot spots of methylmercury (MeHg) generation in at-risk environments. We developed broad-range degenerate PCR primers spanning known hgcAB genes to determine the presence of both genes in diverse environments. These primers were tested against an extensive set of pure cultures with published genomes, including 13 Deltaproteobacteria, nine Firmicutes, and nine methanogenic Archaea genomes. A distinct PCR product at the expected size was confirmed for all hgcAB(+) strains tested via Sanger sequencing. Additionally, we developed clade-specific degenerate quantitative PCR (qPCR) primers that targeted hgcA for each of the three dominant Hg-methylating clades. The clade-specific qPCR primers amplified hgcA from 64%, 88%, and 86% of tested pure cultures of Deltaproteobacteria, Firmicutes, and Archaea, respectively, and were highly specific for each clade. Amplification efficiencies and detection limits were quantified for each organism. Primer sensitivity varied among species based on sequence conservation. Finally, to begin to evaluate the utility of our primer sets in nature, we tested hgcA and hgcAB recovery from pure cultures spiked into sand and soil. These novel quantitative molecular tools designed in this study will allow for more accurate identification and quantification of the individual Hg-methylating groups of microorganisms in the environment. The resulting data will be essential in developing accurate and robust predictive models of Hg methylation potential, ideally integrating the geochemistry of Hg methylation to the microbiology and genetics of hgcAB. C1 [Christensen, Geoff A.; Wymore, Ann M.; King, Andrew J.; Podar, Mircea; Hurt, Richard A., Jr.; Brandt, Craig C.; Brown, Steven D.; Palumbo, Anthony V.; Elias, Dwayne A.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Santillan, Eugenio U.; Soren, Ally; Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. [Wall, Judy D.] Univ Missouri, Columbia, MO USA. RP Elias, DA (reprint author), Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. EM eliasda@ornl.gov OI Christensen, Geoffrey/0000-0003-1360-0729 FU U.S. Department of Energy (DOE) Office of Science Biological and Environmental Research Subsurface Biogeochemical Research (SBR) Program; subsurface biogeochemical research program of the U.S. Department of Energy [DE-AC05-00OR22725]; Smithsonian Burch Fellowship FX This research is sponsored by the U.S. Department of Energy (DOE) Office of Science Biological and Environmental Research Subsurface Biogeochemical Research (SBR) Program. Oak Ridge National Laboratory (ORNL) is managed by UT-Battelle for the U.S. Department of Energy.; The Hg Science Focus Area at ORNL is funded by the subsurface biogeochemical research program of the U.S. Department of Energy under contract DE-AC05-00OR22725. E.U.S. was supported by a Smithsonian Burch Fellowship. NR 34 TC 0 Z9 0 U1 16 U2 17 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0099-2240 EI 1098-5336 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD OCT PY 2016 VL 82 IS 19 BP 6068 EP 6078 DI 10.1128/AEM.01271-16 PG 11 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA DX0JX UT WOS:000384048700034 PM 27422835 ER PT J AU Mouttham, L Comizzoli, P AF Mouttham, Lara Comizzoli, Pierre TI The preservation of vital functions in cat ovarian tissues during vitrification depends more on the temperature of the cryoprotectant exposure than on the sucrose supplementation SO CRYOBIOLOGY LA English DT Article DE Ovary; Cryopreservation; Morphology; Viability; RNA transcription; Follicle; Cat ID IN-VITRO CULTURE; SOLID-SURFACE VITRIFICATION; BOVINE PREANTRAL FOLLICLES; FERTILITY PRESERVATION; PRIMORDIAL FOLLICLES; SECONDARY FOLLICLES; ANTRAL FOLLICLES; CRYOPRESERVATION; VIABILITY; MORPHOLOGY AB The objective of this study was to better characterize the impact of cryoprotectant exposure (temperature and sucrose supplementation) on the health and function of preantral follicles in ovarian tissues during vitrification using the domestic cat model. Ovarian cortical pieces from peri-pubertal individuals were exposed to cryoprotectants at 4 degrees C or room temperature and supplemented with 0 or 0.5 M of sucrose, followed by vitrification. After rapid warming, cortical pieces were cultured in vitro and assessed for normal follicular morphology, viability and resumption of transcriptional activities for up to 7 days. Throughout the culture period, follicular morphology (up to 67.5% normal follicles) and global RNA transcription (up to 50.9% follicles with transcriptional activity) in warmed tissues were improved by cryoprotectant exposure at 4 degrees C compared to room temperature, but viability (up to 84.6% viable follicles) did not seem to be affected by exposure temperature. Sucrose supplementation did not have a consistent effect as it increased RNA transcription but decreased normal follicular morphology. For the first time, the study demonstrated that the preservation of critical tissue functions, such as the transcriptional activities, highly depends on the temperature of the cryoprotectant exposure and not necessarily on the presence of sucrose. Published by Elsevier Inc. C1 [Mouttham, Lara; Comizzoli, Pierre] Natl Zool Pk, Smithsonian Conservat Biol Inst, POB 37012,MRC 5502, Washington, DC 20008 USA. [Mouttham, Lara] Cornell Univ, Dept Biomed Sci, Ithaca, NY 14853 USA. RP Comizzoli, P (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, POB 37012,MRC 5502, Washington, DC 20008 USA. EM comizzolip@si.edu NR 59 TC 0 Z9 0 U1 4 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 EI 1090-2392 J9 CRYOBIOLOGY JI Cryobiology PD OCT PY 2016 VL 73 IS 2 BP 187 EP 195 DI 10.1016/j.cryobiol.2016.07.013 PG 9 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA DX4ZC UT WOS:000384388600013 PM 27475292 ER PT J AU Panyaboriban, S Pukazhenthi, B Brown, ME Crowe, C Lynch, W Singh, RP Techakumphu, M Songsasen, N AF Panyaboriban, Saritvich Pukazhenthi, Budhan Brown, Megan E. Crowe, Chris Lynch, Warren Singh, Ram P. Techakumphu, Mongkol Songsasen, Nucharin TI Influence of cooling and thawing conditions and cryoprotectant concentration on frozen-thawed survival of white-naped crane (Antigone vipio) spermatozoa SO CRYOBIOLOGY LA English DT Article DE White naped crane; Sperm; Motility; Cooling condition; Cryopreservation; Me2SO; Thawing rate ID FOWL SEMINAL PLASMA; ARTIFICIAL-INSEMINATION; SEMEN CHARACTERISTICS; CRYOGENIC PRESERVATION; SATELLITE TRACKING; AVIAN SPERMATOZOA; SANDHILL CRANE; SPERM QUALITY; CRYOPRESERVATION; COLLECTION AB To assist in genetic resource management and recovery efforts of the white-naped crane (Antigone vipio), we conducted two experiments to evaluate the effect of cooling condition, thawing rate, and cryoprotectant concentration on sperm survival post-thaw. Semen was collected from four mature males during breeding season (March and April) and evaluated for volume, sperm concentration, motility, and membrane integrity. In Experiment 1, ejaculates (n = 8) were diluted with Beltsville Poultry Semen Extender (BPSE) containing 10% dimethylsulfoxide (Me2SO) and frozen using either one (average cooling rate = 2.5 degrees C/min) or two step (average cooling rate = 7 and 9 degrees C/min, respectively) cooling method. The frozen samples were thawed using one of two thawing rates: 37 degrees C 30 s vs. 4 degrees C 1 min. In Experiment 2, samples were diluted with crane semen extender containing either 6% or 10% Me2SO, frozen using two-step method and then thawed at 37 degrees C for 30 s. Both cooling condition (two-step > one-step) and thawing rate (37 degrees C 30 s > 4 degrees C 1 min) impacted sperm motility, progression and kinetic characteristics (P < 0.05), but did not (P > 0.05) affect plasma membrane or acrosomal integrity. Concentration of Me2SO did not impact frozen-thaw survival. We conclude that white-naped crane sperm cryopreserved using a combination of two-step cooling and thawing at 37 degrees C 30 s was superior to other cooling and thawing combinations regarding to sustaining sperm motility with good motility kinetics. Findings represent the first steps towards the development of effective cryopreservation protocols and establishment of a genome resource bank for this threatened species. (C) 2016 Published by Elsevier Inc. C1 [Panyaboriban, Saritvich; Pukazhenthi, Budhan; Brown, Megan E.; Crowe, Chris; Lynch, Warren; Singh, Ram P.; Songsasen, Nucharin] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. [Panyaboriban, Saritvich; Techakumphu, Mongkol] Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok 10330, Thailand. [Brown, Megan E.] Univ Maryland, Dept Anim & Avian Sci, Anim Sci Ctr 1413, College Pk, MD 20742 USA. [Singh, Ram P.] Salim Ali Ctr Ornithol & Nat Hist, Coimbatore 641108, Tamil Nadu, India. RP Songsasen, N (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, 1500 Remount Rd, Front Royal, VA 22630 USA. EM songsasenn@si.edu FU Royal Golden Jubilee-PhD-industrial link program, Thailand Research Fund [PHD/0365/2551]; Fulbright-Nehru Fellowship [1942/FNPDR/2014] FX Panyaboriban was supported by Royal Golden Jubilee-PhD-industrial link program, Thailand Research Fund (PHD/0365/2551). Ram Pratap Singh was supported by the Fulbright-Nehru Fellowship (1942/FNPDR/2014). NR 61 TC 0 Z9 0 U1 9 U2 9 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 EI 1090-2392 J9 CRYOBIOLOGY JI Cryobiology PD OCT PY 2016 VL 73 IS 2 BP 209 EP 215 DI 10.1016/j.cryobiol.2016.07.009 PG 7 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA DX4ZC UT WOS:000384388600016 PM 27426074 ER PT J AU McLean, KA Trainor, AM Asner, GP Crofoot, MC Hopkins, ME Campbell, CJ Martin, RE Knapp, DE Jansen, PA AF McLean, Kevin A. Trainor, Anne M. Asner, Gregory P. Crofoot, Margaret C. Hopkins, Mariah E. Campbell, Christina J. Martin, Roberta E. Knapp, David E. Jansen, Patrick A. TI Movement patterns of three arboreal primates in a Neotropical moist forest explained by LiDAR-estimated canopy structure SO LANDSCAPE ECOLOGY LA English DT Article DE Alouatta palliata; Ateles geoffroyi; Arboreal habitat; Canopy structure; Cebus capucinus; LiDAR; Movement ecology; Primate; Step selection function ID CAPUCHINS CEBUS-CAPUCINUS; SEED DISPERSAL; RESOURCE SELECTION; PREDATION RISK; ECOLOGY; MONKEYS; MODELS; VERTEBRATES; BEHAVIOR; FUSION AB Many arboreal mammals in Neotropical forests are important seed dispersers that influence the spatial patterns of tree regeneration via their movement patterns, which in turn are determined by the canopy structure of the forest itself. However, the relationship between arboreal mammal movement and canopy structure is poorly understood, due in large part to the complexity of quantifying arboreal habitat structure. We relate detailed movement trajectories of three sympatric primate species to attributes of canopy structure derived from airborne light detection and ranging (LiDAR) in order to understand the role of structure in arboreal movement in the tropical moist forest of Barro Colorado Island, Panama. We used high-resolution LiDAR to quantify three-dimensional attributes of the forest canopy of the entire island, high-resolution GPS tracking to map the movement patterns of the monkey species, and step selection functions to relate movement decisions to canopy attributes. We found that movement decisions were correlated with canopy height and distance to gaps, which indicate forest maturity and lateral connectivity, in all three species. In the two faster-moving species, step selection was also correlated with the thickness of the crown layer and the density of vegetation within the crown. The correlations detected are fully in line with known differences in the locomotor adaptations and movement strategies of the study species, and directly reflect maximization of energetic efficiency and ability to escape from predators. Quantification of step selection in relation to structure thus provides insight into the ways in which arboreal animals use their environment. C1 [McLean, Kevin A.] Yale Sch Forestry & Environm Studies, Greeley Mem Lab, 370 Prospect St, New Haven, CT 06511 USA. [McLean, Kevin A.; Crofoot, Margaret C.; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Panama. [Trainor, Anne M.] Nature Conservancy, 4245 Fairfax Dr, Arlington, VA 22203 USA. [Asner, Gregory P.; Martin, Roberta E.; Knapp, David E.] Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. [Crofoot, Margaret C.] Univ Calif Davis, Dept Anthropol, 1 Shields Ave, Davis, CA 95616 USA. [Hopkins, Mariah E.] Univ Texas Austin, Dept Anthropol, SAC 4-102,2201 Speedway Stop C3200, Austin, TX 78712 USA. [Campbell, Christina J.] Calif State Univ Northridge, Dept Anthropol, 18111 Nordhoff St, Northridge, CA 91330 USA. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, POB 47, NL-6700 AA Wageningen, Netherlands. RP McLean, KA (reprint author), Yale Sch Forestry & Environm Studies, Greeley Mem Lab, 370 Prospect St, New Haven, CT 06511 USA.; McLean, KA (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM kevin.mclean@yale.edu FU NASA Earth and Space Science Graduate Fellowship [NNX13AO29H]; Yale Institute for Biospheric Studies; Max Planck Institute for Ornithology; Smithsonian Tropical Research Institute; National Science Foundation [BCS-1440755, 0622611]; Nature Conservancy's NatureNet Science Fellows program; College of Social and Behavioral Sciences at CSU-Northridge; Wenner-Gren Foundation; American Association of University Women; Leakey Foundation; University of California at Berkeley; CTFS; STRI; MacArthur Foundation; Mellon Foundation; Celera Foundation FX This work was supported by the NASA Earth and Space Science Graduate Fellowship (NNX13AO29H) and Yale Institute for Biospheric Studies. We are grateful to Oswald Schmitz, Katherine Mertes, Jennifer Miller, and Colin Donihue for editorial reviews and Roland Kays for providing conceptual support in the early stages of this study. We also benefitted greatly from the comments of two anonymous reviewers. MCC acknowledges support from the Max Planck Institute for Ornithology, the Smithsonian Tropical Research Institute and National Science Foundation grant BCS-1440755. AMT acknowledges support from The Nature Conservancy's NatureNet Science Fellows program. CJC thanks the College of Social and Behavioral Sciences at CSU-Northridge and Stephanie Ramirez for funding and field data collection, respectively. MEH acknowledges support from the National Science Foundation (#0622611), The Wenner-Gren Foundation, the American Association of University Women, The Leakey Foundation, the Smithsonian Tropical Research Institute, and the University of California at Berkeley. The Center for Tropical Forest Science also provided MEH with georeferenced tree locations on the 50-ha forest dynamics plot, data which were made possible by NSF grants to S. Hubbell, support from CTFS, STRI, the MacArthur Foundation, the Mellon Foundation, the Celera Foundation, and numerous private individuals, and through the hard work of over 100 people. The Carnegie Airborne Observatory is made possible by the Avatar Alliance Foundation, Margaret A. Cargill Foundation, John D. and Catherine T. MacArthur Foundation, Gordon and Betty Moore Foundation, Grantham Foundation for the Protection of the Environment, W.M. Keck Foundation, Mary Anne Nyburg Baker and G. Leonard Baker Jr., and William R. Hearst III. NR 42 TC 1 Z9 1 U1 20 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 EI 1572-9761 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD OCT PY 2016 VL 31 IS 8 BP 1849 EP 1862 DI 10.1007/s10980-016-0367-9 PG 14 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA DV4PD UT WOS:000382906600014 ER PT J AU Templeton, TJ Martinsen, E Kaewthamasorn, M Kaneko, O AF Templeton, Thomas J. Martinsen, Ellen Kaewthamasorn, Morakot Kaneko, Osamu TI The rediscovery of malaria parasites of ungulates SO PARASITOLOGY LA English DT Review DE malaria; ungulates; ruminants; Haemosporidia; Apicomplexa; malaria parasites ID DUIKER SYLVICAPRA GRIMMIA; CYTOCHROME-B; PLASMODIUM; PHYLOGENY; GENOME; BLOOD; INFECTIONS; CEPHALOPHI; EVOLUTION AB Over a hundred years since their first description in 1913, the sparsely described malaria parasites (genus Plasmodium) of ungulates have been rediscovered using molecular typing techniques. In the span of weeks, three studies have appeared describing the genetic characterization and phylogenetic analyses of malaria parasites from African antelope (Cephalophus spp.) and goat (Capra aegagrus hircus), Asian water buffalo (Bubalus bubalis), and North American white-tailed deer (Odocoileus virginianus). Here we unify the contributions from those studies with the literature on pre-molecular characterizations of ungulate malaria parasites, which are largely based on surveys of Giemsa-reagent stained blood smears. We present a phylogenetic tree generated from all available ungulate malaria parasite sequence data, and show that parasites from African duiker antelope and goat, Asian water buffalo and New World white-tailed deer group together in a clade, which branches early in Plasmodium evolution. Anopheline mosquitoes appear to be the dominant, if not sole vectors for parasite transmission. We pose questions for future phylogenetic studies, and discuss topics that we hope will spur further molecular and cellular studies of ungulate malaria parasites. C1 [Templeton, Thomas J.; Kaneko, Osamu] Nagasaki Univ, Inst Trop Med NEKKEN, Dept Protozool, 1-12-4 Sakamoto, Nagasaki 8528523, Japan. [Templeton, Thomas J.] Weill Cornell Med Sch, Dept Microbiol & Immunol, New York, NY 10021 USA. [Martinsen, Ellen] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC 20013 USA. [Kaewthamasorn, Morakot] Chulalongkorn Univ, Dept Pathol, Vet Parasitol Unit, Fac Vet Sci, Bangkok 10330, Thailand. RP Kaneko, O (reprint author), Nagasaki Univ, Inst Trop Med NEKKEN, Dept Protozool, 1-12-4 Sakamoto, Nagasaki 8528523, Japan. EM okaneko@nagasaki-u.ac.jp OI Kaewthamasorn, Morakot/0000-0003-3072-8708 FU visiting professorship at the Institute of Tropical Medicine, Nagasaki University, Japan; MEXT, Japan [JP16H05807, JP23117008]; grants for development of new faculty staff, Chulalongkorn University [GDNS 56-020-31-001]; Chulalongkorn University-Veterinary Science Research Fund [RG 15/2559]; Morris Animal Foundation [D10ZO-043]; National Science Foundation [DEB-1241041] FX T. J. T. was supported by a visiting professorship at the Institute of Tropical Medicine, Nagasaki University, Japan. This work was conducted at the Joint Usage/Research Center on Tropical Disease, Institute of Tropical Medicine, Nagasaki University and supported in part by Grants-in-Aids for Scientific Research JP16H05807 and Scientific Research on Innovative Areas JP23117008, MEXT, Japan (O.K.). M. K. is a recipient of grants for development of new faculty staff, Chulalongkorn University (GDNS 56-020-31-001) and Chulalongkorn University-Veterinary Science Research Fund (RG 15/2559). The white-tailed deer work was carried out at the Smithsonian Conservation Biology Institute's Center for Conservation and Evolutionary Genetics and funded by a grant from the Morris Animal Foundation (D10ZO-043) and the National Science Foundation (DEB-1241041). We thank Robert C. Fleischer for providing resources and input into the white-tailed deer malaria parasite portion of the work. NR 39 TC 0 Z9 0 U1 6 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0031-1820 EI 1469-8161 J9 PARASITOLOGY JI Parasitology PD OCT PY 2016 VL 143 IS 12 BP 1501 EP 1508 DI 10.1017/S0031182016001141 PG 8 WC Parasitology SC Parasitology GA DX5IW UT WOS:000384415700002 PM 27444556 ER PT J AU Holman, MJ Payne, MJ AF Holman, Matthew J. Payne, Matthew J. TI OBSERVATIONAL CONSTRAINTS ON PLANET NINE: ASTROMETRY OF PLUTO AND OTHER TRANS-NEPTUNIAN OBJECTS SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; ephemerides; Kuiper Belt: general; Kuiper Belt objects: individual (Pluto) ID OUTER SOLAR-SYSTEM; KUIPER-BELT OBJECTS; SIZE DISTRIBUTION; MASSIVE BODY; ORIGIN; DISCOVERY; ORBIT; GIANT; ARCHITECTURE; COMPANION AB We use astrometry of Pluto and other trans-neptunian objects to constrain the sky location, distance, and mass of the possible additional planet (Planet Nine) hypothesized by Batygin & Brown. We find that over broad regions of the sky, the inclusion of a massive, distant planet degrades the fits to the observations. However, in other regions, the fits are significantly improved by the addition of such a planet. Our best fits suggest a planet that is either more massive or closer than argued for by Batygin & Brown based on the orbital distribution of distant trans-neptunian objects (or by Fienga et al. based on range measured to the Cassini spacecraft). The trend to favor larger and closer perturbing planets is driven by the residuals to the astrometry of Pluto, remeasured from photographic plates using modern stellar catalogs, which show a clear trend in decl. over the course of two decades, that drive a preference for large perturbations. Although this trend may be the result of systematic errors of unknown origin in the observations, a possible resolution is that the decl. trend may be due to perturbations from a body, in addition to Planet Nine, that is closer to Pluto but less massive than Planet Nine. C1 [Holman, Matthew J.; Payne, Matthew J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. RP Holman, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM mholman@cfa.harvard.edu; mpayne@cfa.harvard.edu FU NASA [NNX10AH40G, NNX13A124G, 1312645088477, NNX16AD69G]; BSF grant [2012384]; Smithsonian CGPS/Pell grant program FX We thank Norman Murray, Gareth Williams, Cesar Fuentes, Michael Lackner, Pedro Lacerda, Gongjie Li, Joshua Winn, Scott Tremaine, Doug Finkbeiner, Avi Loeb, Tsevi Mazeh, William Folkner, and Scott Gaudi for helpful discussions. We thank Paul Edmon for his help with our computations on the Harvard Odyssey HPC. M.J.H. and M.J.P. gratefully acknowledge NASA Origins of Solar Systems Program grant NNX13A124G, NASA Origins of Solar Systems Program grant NNX10AH40G via sub-award agreement 1312645088477, BSF grant Number 2012384, NASA Solar System Observations grant NNX16AD69G, as well as support from the Smithsonian 2015 CGPS/Pell grant program. NR 72 TC 3 Z9 3 U1 7 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2016 VL 152 IS 4 AR 80 DI 10.3847/0004-6256/152/4/80 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW7BB UT WOS:000383805000002 ER PT J AU Rabus, M Jordan, A Hartman, JD Bakos, GA Espinoza, N Brahm, R Penev, K Ciceri, S Zhou, G Bayliss, D Mancini, L Bhatti, W de Val-Borro, M Csbury, Z Sato, B Tan, TG Henning, T Schmidt, B Bento, J Suc, V Noyes, R Lazar, J Papp, I Sari, P AF Rabus, M. Jordan, A. Hartman, J. D. Bakos, G. A. Espinoza, N. Brahm, R. Penev, K. Ciceri, S. Zhou, G. Bayliss, D. Mancini, L. Bhatti, W. de Val-Borro, M. Csbury, Z. Sato, B. Tan, T. -G. Henning, T. Schmidt, B. Bento, J. Suc, V. Noyes, R. Lazar, J. Papp, I. Sari, P. TI HATS-11B AND HATS-12B: TWO TRANSITING HOT JUPITERS ORBITING SUBSOLAR METALLICITY STARS SELECTED FOR THE K2 CAMPAIGN 7 SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HATS-11-HATS-12); techniques: photometric; techniques: spectroscopic ID CANDIDATE HOST STARS; PLANET CONSUMPTION; HATSOUTH SURVEY; KEPLER FIELD; METAL-RICH; STELLAR; ALGORITHM; DWARF; MASS; ISOCHRONES AB We report the discovery of two transiting extrasolar planets from the HATSouth survey. HATS-11, a V = 14.1 G0-star shows a periodic 12.9 mmag dip in its light curve every 3.6192 days and a radial velocity variation consistent with a Keplerian orbit. HATS-11 has a mass of 1.000 +/- 0.060 M-circle dot, a radius of 1.444 +/- 0.057 R-circle dot and an effective temperature of 6060 +/- 150 K, while its companion is a 0.85 +/- 0.12 M-J, 1.510 +/- 0.078 R-J planet in a circular orbit. HATS-12 shows a periodic 5.1 mmag flux decrease every 3.1428 days and Keplerian RV variations around a V = 12.8 F-star. HATS-12 has a mass of 1.489 +/- 0.071 M-circle dot, a radius of 2.21 +/- 0.21 R-circle dot, and an effective temperature of 6408 +/- 75 K. For HATS-12b, our measurements indicate that this is a 2.38 +/- 0.11 M-J, 1.35 +/- 0.17 R-J planet in a circular orbit. Both host stars show subsolar metallicities of -0.390 +/- 0.060 dex and -0.100 +/- 0.040 dex, respectively, and are (slightly) evolved stars. In fact, HATS-11 is among the most metal-poor and, HATS-12, with a log g(*) of 3.923 +/- 0.065, is among the most evolved stars hosting a hot-Jupiter planet. Importantly, HATS-11 and HATS-12 have been observed in long cadence by Kepler as part of K2 campaign 7 (EPIC216414930 and EPIC218131080 respectively). C1 [Rabus, M.; Jordan, A.; Espinoza, N.; Brahm, R.; Suc, V.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile. [Rabus, M.; Ciceri, S.; Mancini, L.; Henning, T.] Max Planck Inst Astron, Heidelberg, Germany. [Hartman, J. D.; Bakos, G. A.; Penev, K.; Bhatti, W.; de Val-Borro, M.; Csbury, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Zhou, G.; Bayliss, D.; Schmidt, B.; Bento, J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Bayliss, D.] Univ Geneva, Observ Astron, 51ch Maillettes, CH-1290 Versoix, Switzerland. [Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan. [Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Noyes, R.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Rabus, M (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile.; Rabus, M (reprint author), Max Planck Inst Astron, Heidelberg, Germany. EM mrabus@astro.puc.cl OI Schmidt, Brian/0000-0001-6589-1287; Bakos, Gaspar/0000-0001-7204-6727; Espinoza Perez, Nestor/0000-0001-9513-1449; Tan, Thiam-Guan/0000-0001-5603-6895; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX09AB29G, NNX12AH91H, NNX13AQ62G]; FONDECYT [1130857]; "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy [IC120009]; BASAL CATA [PFB-06]; CONICYT-PCHA/Doctorado Nacional; ARC Laureate Fellowship Grant [FL0992131]; Robert Martin Ayers Sciences Fund; SIMBAD database, operated at CDS, Strasbourg, France; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations have been supported by NASA grants NNX09AB29G and NNX12AH91H, and follow-up observations receive partial support from grant NSF/AST-1108686. A.J. acknowledges support from FONDECYT project 1130857, BASAL CATA PFB-06, and project IC120009 "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. are supported by CONICYT-PCHA/Doctorado Nacional. R.B. and N.E. acknowledge additional support from project IC120009 " Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. K.P. acknowledges support from NASA grant NNX13AQ62G. This work is based on observations made with ESO Telescopes at the La Silla Observatory. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope. Observing times were obtained through CNTAC proposals CN2013B-55, CN2014A-104, CN2014B-57, and CN2015A-51. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD database, operated at CDS, Strasbourg, France. Operations at the MPG 2.2 m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. The imaging system GROND has been built by the high-energy group of MPE in collaboration with the LSW Tautenburg and ESO. We thank the MPG 2.2 m Telescope support team for their technical assistance during observations. We are grateful to P. Sackett for her help in the early phase of the HATSouth project. NR 54 TC 0 Z9 0 U1 4 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2016 VL 152 IS 4 AR 88 DI 10.3847/0004-6256/152/4/88 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW7BB UT WOS:000383805000010 ER PT J AU Tilley, A Lopez-Angarita, J AF Tilley, Alexander Lopez-Angarita, Juliana TI Predicting vulnerability to management changes in data-limited, small-scale fisheries SO MARINE POLICY LA English DT Article DE Adaptive capacity; Gill nets; Livelihoods; Poverty; Colombia; Pacific ID CORAL-REEF; FISHING COMMUNITIES; RESOURCE-MANAGEMENT; ADAPTIVE CAPACITY; SUSTAINABILITY; POVERTY; SYSTEMS; POOR AB It is estimated that more than 200 million people worldwide depend on small-scale fisheries for their livelihood, driving the need for fisheries reform to develop effective, local-level governance systems to protect food security and lessen reliance on common resources. However, our ability to impose new management relies on the assessment of vulnerability and adaptive capacity, and the lack of social ecological data often stifles decision making. Here we test the use of simple fisheries attributes from 33 fishing communities in an understudied, and chronically poor region of the Colombian Pacific, to generate indicators of relative fisheries adaptive capacity, as a proxy for vulnerability to planned management changes. We demonstrate the strengths of this approach using four variables (species assemblage, spatial dependence, gear dependence and compliance), and illustrate how potential threats to livelihoods can be identified early, and with limited data, allowing for management to adapt decision-making accordingly. We show that in the absence of detailed socio-economic information, relatively basic fisheries data recorded by community observers can be applied to decrease uncertainty by providing a rapid characterisation of community vulnerability to management decision-making, in a range of management intervention options. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Tilley, Alexander; Lopez-Angarita, Juliana] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Tilley, Alexander; Lopez-Angarita, Juliana] Fdn Talking Oceans, Carrera 16,127-81, Bogota 110121, Colombia. [Lopez-Angarita, Juliana] Univ York, Dept Environm, York YO10 5DD, N Yorkshire, England. RP Tilley, A (reprint author), WorldFish Ctr, Ave Presidente Nicolau Lobato, Dili, Timor Leste. EM alextilley@gmail.com NR 55 TC 0 Z9 0 U1 12 U2 12 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0308-597X EI 1872-9460 J9 MAR POLICY JI Mar. Pol. PD OCT PY 2016 VL 72 BP 211 EP 218 DI 10.1016/j.marpol.2016.05.034 PG 8 WC Environmental Studies; International Relations SC Environmental Sciences & Ecology; International Relations GA DW7HJ UT WOS:000383821500022 ER PT J AU Kim, S Lee, S McCormick, M Kim, JG Kang, H AF Kim, Sunghyun Lee, Seunghoon McCormick, Melissa Kim, Jae Geun Kang, Hojeong TI Microbial Community and Greenhouse Gas Fluxes from Abandoned Rice Paddies with Different Vegetation SO MICROBIAL ECOLOGY LA English DT Article DE Microbial community; Microbial abundance; Abandoned rice paddy; Greenhouse gas; Organic carbon ID NITROUS-OXIDE FLUXES; SOIL RESPIRATION; CARBON-DIOXIDE; NORTHERN PEATLANDS; METHANE OXIDATION; QUANTITATIVE PCR; PLANT COMMUNITY; N2O EMISSIONS; WATER-TABLE; CLIMATE AB The area of rice paddy fields has declined continuously in East Asian countries due to abandonment of agriculture and concurrent socioeconomic changes. When they are abandoned, rice paddy fields generally transform into wetlands by natural succession. While previous studies have mainly focused on vegetation shifts in abandoned rice paddies, little information is available about how these changes may affect their contribution to wetland functions. As newly abandoned fields proceed through succession, their hydrology and plant communities often change. Moreover, the relationships between these changes, soil microbial characteristics, and emissions of greenhouse gasses are poorly understood. In this study, we examined changes over the course of secondary succession of abandoned rice paddies to wetlands and investigated their ecological functions through changes in greenhouse gas fluxes and microbial characteristics. We collected gas and soil samples in summer and winter from areas dominated by Cyperaceae, Phragmites, and Sphagnum in each site. We found that CO2 emissions in summer were significantly higher than those in winter, but CH4 and N2O emission fluxes were consistently at very low levels and were similar among seasons and locations, due to their low nutrient conditions. These results suggest that microbial activity and abundance increased in summer. Greenhouse gas flux, soil properties, and microbial abundance were not affected by plant species, although the microbial community composition was changed by plant species. This information adds to our basic understanding of the contribution of wetlands that are transformed from abandoned rice paddy systems. C1 [Kim, Sunghyun; McCormick, Melissa] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Kim, Sunghyun; Lee, Seunghoon; Kang, Hojeong] Yonsei Univ, Sch Civil & Environm Engn, Seoul, South Korea. [Kim, Jae Geun] Seoul Natl Univ, Dept Biol Educ, Seoul, South Korea. RP Kang, H (reprint author), Yonsei Univ, Sch Civil & Environm Engn, Seoul, South Korea. EM hj_kang@yonsei.ac.kr FU ERC [2011-0030040]; National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology [86457858] FX This study was supported by ERC (No. 2011-0030040). S. Kim was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (86457858). NR 64 TC 0 Z9 0 U1 31 U2 31 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0095-3628 EI 1432-184X J9 MICROB ECOL JI Microb. Ecol. PD OCT PY 2016 VL 72 IS 3 BP 692 EP 703 DI 10.1007/s00248-016-0801-1 PG 12 WC Ecology; Marine & Freshwater Biology; Microbiology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA DW2KH UT WOS:000383470800019 PM 27352281 ER PT J AU Favole, G Comparat, J Prada, F Yepes, G Jullo, E Niemiec, A Kneib, JP Rodriguez-Torres, SA Klypin, A Skibba, RA McBride, CK Eisenstein, DJ Schlegel, DJ Nuza, SE Chuang, CH Delubac, T Yeche, C Schneider, DP AF Favole, Ginevra Comparat, Johan Prada, Francisco Yepes, Gustavo Jullo, Eric Niemiec, Anna Kneib, Jean-Paul Rodriguez-Torres, Sergio A. Klypin, Anatoly Skibba, Ramin A. McBride, Cameron K. Eisenstein, Daniel J. Schlegel, David J. Nuza, Sebastian E. Chuang, Chia-Hsun Delubac, Timothee Yeche, Christophe Schneider, Donald P. TI Clustering properties of g-selected galaxies at z similar to 0.8 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: distances and redshifts; galaxies: haloes; galaxies: statistics; cosmology: observations; cosmology: theory; large-scale structure of Universe ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; HALO OCCUPATION DISTRIBUTION; TELESCOPE LENSING SURVEY; REDSHIFT SURVEY VIPERS; LARGE-SCALE STRUCTURE; LESS-THAN 1.2; SDSS-III; DARK-MATTER; DATA RELEASE AB Current and future large redshift surveys, as the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey (SDSS-IV/eBOSS) or the Dark Energy Spectroscopic Instrument (DESI), will use emission-line galaxies (ELGs) to probe cosmological models by mapping the large-scale structure of the Universe in the redshift range 0.6 < z < 1.7. With current data, we explore the halo-galaxy connection by measuring three clustering properties of g-selected ELGs as matter tracers in the redshift range 0.6 < z < 1: (i) the redshift-space two-point correlation function using spectroscopic redshifts from the BOSS ELG sample and VIPERS; (ii) the angular two-point correlation function on the footprint of the CFHT-LS; (iii) the galaxy-galaxy lensing signal around the ELGs using the CFHTLenS. We interpret these observations by mapping them on to the latest high-resolution MultiDark Planck N-body simulation, using a novel (Sub) Halo-Abundance Matching technique that accounts for the ELG incompleteness. ELGs at z similar to 0.8 live in haloes of (1 +/- 0.5) x 10(12) h(-1)M(circle dot) and 22.5 +/- 2.5 per cent of them are satellites belonging to a larger halo. The halo occupation distribution of ELGs indicates that we are sampling the galaxies in which stars form in the most efficient way, according to their stellar-to-halo mass ratio. C1 [Favole, Ginevra; Comparat, Johan; Prada, Francisco; Rodriguez-Torres, Sergio A.; Chuang, Chia-Hsun] Univ Autonoma Madrid, Inst Fis Teor IFT UAM CSIC, E-28049 Madrid, Spain. [Favole, Ginevra; Comparat, Johan; Prada, Francisco; Rodriguez-Torres, Sergio A.; Chuang, Chia-Hsun] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Comparat, Johan; Yepes, Gustavo; Rodriguez-Torres, Sergio A.] Univ Autonoma Madrid, Dept Fis Teor M8, E-28049 Madrid, Spain. [Prada, Francisco; Schlegel, David J.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Prada, Francisco] Inst Astrofis Andalucia CSIC, E-18008 Granada, Spain. [Jullo, Eric; Niemiec, Anna; Kneib, Jean-Paul] Univ Aix Marseille, Lab Astrophys Marseille LAM, F-13388 Marseille, France. [Jullo, Eric; Niemiec, Anna; Kneib, Jean-Paul] CNRS, UMR7326, F-13388 Marseille, France. [Kneib, Jean-Paul; Delubac, Timothee] Ecole Polytech Fed Lausanne, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland. [Klypin, Anatoly] New Mexico State Univ, Astron Dept, MSC 4500,POB 30001, Las Cruces, NM USA. [Skibba, Ramin A.] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, San Diego, CA 92093 USA. [McBride, Cameron K.; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Nuza, Sebastian E.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. [Yeche, Christophe] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. RP Favole, G; Comparat, J (reprint author), Univ Autonoma Madrid, Inst Fis Teor IFT UAM CSIC, E-28049 Madrid, Spain.; Favole, G; Comparat, J (reprint author), Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain.; Comparat, J (reprint author), Univ Autonoma Madrid, Dept Fis Teor M8, E-28049 Madrid, Spain. EM g.favole@csic.es; johan.comparat@uam.es FU Ministerio de Educacion y Ciencia of the Spanish Government through FPI grant [AYA2010-2131-C02-01]; MINECO (Spain) [AYA2012-31101, FPA2012-34694]; CNRS; Labex OCEVU; Deutsche Forschungsgemeinschaft [NU 332/21]; Spanish MICINN Consolider-Ingenio Programme [CSD2009-00064]; MINECO Centro de Excelencia Severo Ochoa Programme [SEV-2012-0249]; MINECO [AYA2014-60641-C2-1-P]; spanish MEC 'Salvador de Madariaga' program [PRX14/00444]; PRACE [2012060963]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX GF is supported by the Ministerio de Educacion y Ciencia of the Spanish Government through FPI grant AYA2010-2131-C02-01. JC acknowledges financial support from MINECO (Spain) under project number AYA2012-31101. GY acknowledges financial support from MINECO (Spain) under project number AYA2012-31101 and grant FPA2012-34694. EJ acknowledges the support of CNRS, and the Labex OCEVU. SEN acknowledges support by the Deutsche Forschungsgemeinschaft under the grant NU 332/21. GF, FP, SART, AK, SN and CC acknowledge financial support from the Spanish MICINN Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, MINECO Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249, and MINECO grant AYA2014-60641-C2-1-P. GF, JC and FP wish to thank the Lawrence Berkeley National Laboratory for the hospitality during the creation of this work. FP acknowledges the spanish MEC 'Salvador de Madariaga' program, Ref. PRX14/00444.; The MultiDark Planck simulation has been performed in the Supermuc supercomputer at the Libniz Supercomputing Center (LRZ, Munich) thanks to the cpu time awarded by PRACE (proposal number 2012060963).; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 83 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 3421 EP 3431 DI 10.1093/mnras/stw1483 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900003 ER PT J AU Taylor, C Boylan-Kolchin, M Torrey, P Vogelsberger, M Hernquist, L AF Taylor, Corbin Boylan-Kolchin, Michael Torrey, Paul Vogelsberger, Mark Hernquist, Lars TI The mass profile of the Milky Way to the virial radius from the Illustris simulation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: fundamental parameters; Galaxy: halo; Galaxy: structure; dark matter ID DARK-MATTER HALOES; VELOCITY DISPERSION PROFILE; GALAXY FORMATION PHYSICS; TELESCOPE PROPER MOTION; LARGE-MAGELLANIC-CLOUD; LOCAL GROUP; DENSITY PROFILE; STAR-FORMATION; COSMOLOGICAL SIMULATIONS; SATELLITE GALAXIES AB We use particle data from the Illustris simulation, combined with individual kinematic constraints on the mass of the Milky Way (MW) at specific distances from the Galactic Centre, to infer the radial distribution of the MW's dark matter halo mass. Our method allows us to convert any constraint on the mass of the MW within a fixed distance to a full circular velocity profile to the MW's virial radius. As primary examples, we take two recent (and discrepant) measurements of the total mass within 50 kpc of the Galaxy and find that they imply very different mass profiles and stellar masses for the Galaxy. The dark-matter-only version of the Illustris simulation enables us to compute the effects of galaxy formation on such constraints on a halo-by-halo basis; on small scales, galaxy formation enhances the density relative to dark-matter-only runs, while the total mass density is approximately 20 per cent lower at large Galactocentric distances. We are also able to quantify how current and future constraints on the mass of the MW within specific radii will be reflected in uncertainties on its virial mass: even a measurement of M(<50 kpc) with essentially perfect precision still results in a 20 per cent uncertainty on the virial mass of the Galaxy, while a future measurement of M(<100 kpc) with 10 per cent errors would result in the same level of uncertainty. We expect that our technique will become even more useful as (1) better kinematic constraints become available at larger distances and (2) cosmological simulations provide even more faithful representations of the observable Universe. C1 [Taylor, Corbin] Univ Maryland, Dept Astron, 1113 Phys Sci Complex Bldg 415, College Pk, MD 20742 USA. [Boylan-Kolchin, Michael] Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. [Torrey, Paul; Vogelsberger, Mark] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Torrey, Paul] CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Taylor, C (reprint author), Univ Maryland, Dept Astron, 1113 Phys Sci Complex Bldg 415, College Pk, MD 20742 USA. EM cjtaylor@astro.umd.edu FU NASA through a Hubble Space Telescope theory grant from Space Telescope Science Institute (STScI) [AR-12836]; Association of Universities for Research in Astronomy (AURA), Inc., under NASA [NAS5-26555]; NASA ATP Grant [NNX14AH35G]; NASA [NNX12AC67G]; NSF [AST-1312095] FX We thank Joss Bland-Hawthorn, Nitya Kallivayalil, Julio Navarro, and Annalisa Pillepich for helpful conversations. The analysis of the Illustris data sets for this paper was done using the Odyssey cluster, which is supported by the FAS Division of Science, Research Computing Group at Harvard University. MB-K acknowledges support provided by NASA through a Hubble Space Telescope theory grant (programme AR-12836) from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555. PT acknowledges support from NASA ATP Grant NNX14AH35G. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. NR 67 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 3483 EP 3493 DI 10.1093/mnras/stw1522 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900007 ER PT J AU Hayasaki, K Stone, N Loeb, A AF Hayasaki, Kimitake Stone, Nicholas Loeb, Abraham TI Circularization of tidally disrupted stars around spinning supermassive black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; gravitational waves; hydrodynamics ID X-RAY OUTBURSTS; ACCRETION DISKS; GALACTIC NUCLEI; MAGNETOHYDRODYNAMIC SIMULATION; HYDRODYNAMIC SIMULATIONS; RELATIVISTIC JETS; COMPACT BINARIES; EXTRACTION; RADIATION; GALAXIES AB We study the circularization of tidally disrupted stars on bound orbits around spinning supermassive black holes by performing 3D smoothed particle hydrodynamic simulations with post-Newtonian corrections. Our simulations reveal that debris circularization depends sensitively on the efficiency of radiative cooling. There are two stages in debris circularization if radiative cooling is inefficient: first, the stellar debris streams self-intersect due to relativistic apsidal precession; shocks at the intersection points thermalize orbital energy and the debris forms a geometrically thick, ring-like structure around the black hole. The ring rapidly spreads via viscous diffusion, leading to the formation of a geometrically thick accretion disc. In contrast, if radiative cooling is efficient, the stellar debris circularizes due to self-intersection shocks and forms a geometrically thin ring-like structure. In this case, the dissipated energy can be emitted during debris circularization as a precursor to the subsequent tidal disruption flare. The circularization time-scale is remarkably long in the radiatively efficient cooling case, and is also sensitive to black hole spin. Specifically, Lense-Thirring torques cause dynamically important nodal precession, which significantly delays debris circularization. On the other hand, nodal precession is too slow to produce observable signatures in the radiatively inefficient case. Since the stellar debris is optically thick and its photon diffusion time is likely longer than the time-scale of shock heating, our inefficient cooling scenario is more generally applicable in eccentric tidal disruption events (TDEs). However, in parabolic TDEs for M-BH greater than or similar to 2 x 10(6) M-circle dot, the spin-sensitive behaviour associated with efficient cooling may be realized. C1 [Hayasaki, Kimitake] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 361763, South Korea. [Hayasaki, Kimitake] Korea Astron & Space Sci Inst, Daedeokdaero 776, Daejeon 305348, South Korea. [Hayasaki, Kimitake; Stone, Nicholas; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, 60 GardenSt, Cambridge, MA 02138 USA. [Stone, Nicholas] Columbia Univ, Dept Astron, 550 W 120th St, York, NY 10027 USA. RP Hayasaki, K (reprint author), Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 361763, South Korea.; Hayasaki, K (reprint author), Korea Astron & Space Sci Inst, Daedeokdaero 776, Daejeon 305348, South Korea.; Hayasaki, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 GardenSt, Cambridge, MA 02138 USA. EM kimi@cbnu.ac.kr FU Kavli Institute for Theoretical Physics (KITP); Chungbuk National University; Korea Astronomy and Space Science Institute; Alfred P. Sloan Foundation; NSF [AST-1312034] FX The authors thank to the anonymous referee for fruitful comments and suggestions. KH is grateful to Atsuo. T Okazaki and Jongsoo Kim for their helpful discussions and continuous encouragement. KH would also like to thank the Kavli Institute for Theoretical Physics (KITP) for their hospitality and support during the program on A Universe of Black Holes. During the completion of this paper, we became aware of complementary numerical simulations by Amaro-Seoane et al. (in preparation), but both efforts have proceeded independently. Numerical simulations and data reductions reported here were performed by using a high-performance computing cluster (Polaris) at the Korea Astronomy and Space Science Institute and by using computer facilities at Department of Astronomy, Kyoto University, and Harvard-Smithsonian Center for Astrophysics, Harvard University. This work was supported in part by the research grants of the Chungbuk National University in 2015 and Korea Astronomy and Space Science Institute in 2016 [KH], the Alfred P. Sloan Foundation through a grant to Brian Metzger [NS], and NSF grant AST-1312034 [AL]. NR 68 TC 6 Z9 6 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 3760 EP 3780 DI 10.1093/mnras/stw1387 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900030 ER PT J AU Chuang, CH Prada, F Pellejero-Ibanez, M Beutler, F Cuesta, AJ Eisenstein, DJ Escoffier, S Ho, S Kitaura, FS Kneib, JP Manera, M Nuza, SE Rodriguez-Torres, S Ross, A Rubino-Martin, JA Samushia, L Schlegel, DJ Schneider, DP Wang, YT Weaver, BA Zhao, GB Brownstein, JR Dawson, KS Maraston, C Olmstead, MD Thomas, D AF Chuang, Chia-Hsun Prada, Francisco Pellejero-Ibanez, Marcos Beutler, Florian Cuesta, Antonio J. Eisenstein, Daniel J. Escoffier, Stephanie Ho, Shirley Kitaura, Francisco-Shu Kneib, Jean-Paul Manera, Marc Nuza, Sebastian E. Rodriguez-Torres, Sergio Ross, Ashley Rubino-Martin, J. A. Samushia, Lado Schlegel, David J. Schneider, Donald P. Wang, Yuting Weaver, Benjamin A. Zhao, Gongbo Brownstein, Joel R. Dawson, Kyle S. Maraston, Claudia Olmstead, Matthew D. Thomas, Daniel TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; cosmology: observations; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; REDSHIFT-SPACE DISTORTIONS; DATA RELEASE 9; FINAL DATA RELEASE; MEASURING D-A; ACOUSTIC-OSCILLATIONS; POWER-SPECTRUM; DARK ENERGY; GROWTH-RATE AB With the largest spectroscopic galaxy survey volume drawn from the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS), we can extract cosmological constraints from the measurements of redshift and geometric distortions at quasi-linear scales (e.g. above 50 h(-1) Mpc). We analyse the broad-range shape of the monopole and quadrupole correlation functions of the BOSS Data Release 12 (DR12) CMASS galaxy sample, at the effective redshift z = 0.59, to obtain constraints on the Hubble expansion rate H(z), the angular-diameter distance D-A(z), the normalized growth rate f(z)sigma(8)(z), and the physical matter density Omega(m)h(2). We obtain robust measurements by including a polynomial as the model for the systematic errors, and find it works very well against the systematic effects, e.g. ones induced by stars and seeing. We provide accurate measurements {D-A(0.59)r(s,fid)/r(s), H(0.59)r(s)/r(s, fid), f(0.59)sigma(8)(0.59), Omega(m)h(2)} = {1427 +/- 26 Mpc, 97.3 +/- 3.3 km s(-1) Mpc(-1), 0.488 +/- 0.060, 0.135 +/- 0.016}, where r(s) is the comoving sound horizon at the drag epoch and r(s, fid) = 147.66 Mpc is the sound scale of the fiducial cosmology used in this study. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets, e.g. cosmic microwave background (CMB), are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i. e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. The uncertainty on the dark energy equation of state parameter, w, from CMB+CMASS is about 8 per cent. The uncertainty on the curvature fraction, Omega(k), is 0.3 per cent. We do not find deviation from flat Lambda CDM. C1 [Chuang, Chia-Hsun; Prada, Francisco; Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain. [Chuang, Chia-Hsun; Kitaura, Francisco-Shu; Nuza, Sebastian E.] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. [Prada, Francisco; Rodriguez-Torres, Sergio] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] Inst Astrofis Andalucia CSIC, Glorieta Astron, E-18080 Granada, Spain. [Pellejero-Ibanez, Marcos; Rubino-Martin, J. A.] Inst Astrofis Canarias, C Via Lactea S-N, E-38200 Tenerife, Spain. [Pellejero-Ibanez, Marcos; Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Beutler, Florian; Kitaura, Francisco-Shu; Schlegel, David J.] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. [Beutler, Florian; Manera, Marc; Samushia, Lado; Wang, Yuting; Zhao, Gongbo; Maraston, Claudia; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. [Cuesta, Antonio J.] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-08028 Barcelona, Spain. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Escoffier, Stephanie] Aix Marseille Univ, CNRS, IN2P3, CPPM, F-13288 Marseille, France. [Ho, Shirley] Carnegie Mellon Univ, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA. [Kitaura, Francisco-Shu] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Kitaura, Francisco-Shu] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kneib, Jean-Paul] Ecole Polytech Fed Lausanne, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland. [Kneib, Jean-Paul] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille, UMR 7326, F-13388 Marseille, France. [Manera, Marc] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Dept Fis Teor M8, E-28049 Madrid, Spain. [Ross, Ashley] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Samushia, Lado] Kansas State Univ, Manhattan, KS 66506 USA. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, 2A Kazbegi Ave, GE-1060 Tbilisi, Rep of Georgia. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Wang, Yuting; Zhao, Gongbo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, 550 1St Ave, New York, NY 10003 USA. [Brownstein, Joel R.; Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, 115 S 1400 E, Salt Lake City, UT 84112 USA. [Olmstead, Matthew D.] Kings Coll, Dept Chem & Phys, 133 North River St, Wilkes Barre, PA 18711 USA. RP Chuang, CH (reprint author), Univ Autonoma Madrid, Inst Fis Teor UAM CSIC, E-28049 Madrid, Spain.; Chuang, CH (reprint author), Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany. EM achuang@aip.de RI Gil Marin, Hector/B-2013-2017; OI Gil Marin, Hector/0000-0003-0265-6217; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470 FU Spanish MICINN's Consolider-Ingenio Programme [CSD2009-00064, AYA2010-21231-C02-01]; Comunidad de Madrid [HEPHACOS S2009/ESP-1473]; MINECO [AYA2012-39702-C02-01]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX CC would like to thank Savvas Nesseris for useful discussions. CC and FP acknowledge support from the Spanish MICINN's Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064 and AYA2010-21231-C02-01 grant. CC was also supported by the Comunidad de Madrid under grant HEPHACOS S2009/ESP-1473. MPI acknowledges support from MINECO under the grant AYA2012-39702-C02-01.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 104 TC 8 Z9 8 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 3781 EP 3793 DI 10.1093/mnras/stw1535 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900031 ER PT J AU Baxter, E Clampitt, J Giannantonio, T Dodelson, S Jain, B Huterer, D Bleem, L Crawford, T Efstathiou, G Fosalba, P Kirk, D Kwan, J Sanchez, C Story, K Troxel, MA Abbott, TMC Abdalla, FB Armstrong, R Benoit-Levy, A Benson, B Bernstein, GM Bernstein, RA Bertin, E Brooks, D Carlstrom, J Rosell, AC Kind, MC Carretero, J Chown, R Crocce, M Cunha, CE da Costa, LN Desai, S Diehl, HT Dietrich, JP Doel, P Evrard, AE Neto, AF Flaugher, B Frieman, J Gruen, D Gruendl, RA Gutierrez, G de Haan, T Holder, G Honscheid, K Hou, Z James, DJ Kuehn, K Kuropatkin, N Lima, M March, M Marshall, JL Martini, P Melchior, P Miller, CJ Miquel, R Mohr, JJ Nord, B Omori, Y Plazas, AA Reichardt, C Romer, AK Rykoff, ES Sanchez, E Sevilla-Noarbe, I Sheldon, E Smith, RC Soares-Santos, M Sobreira, F Suchyta, E Stark, A Swanson, MEC Tarle, G Thomas, D Walker, AR Wechsler, RH AF Baxter, E. Clampitt, J. Giannantonio, T. Dodelson, S. Jain, B. Huterer, D. Bleem, L. Crawford, T. Efstathiou, G. Fosalba, P. Kirk, D. Kwan, J. Sanchez, C. Story, K. Troxel, M. A. Abbott, T. M. C. Abdalla, F. B. Armstrong, R. Benoit-Levy, A. Benson, B. Bernstein, G. M. Bernstein, R. A. Bertin, E. Brooks, D. Carlstrom, J. Carnero Rosell, A. Kind, M. Carrasco Carretero, J. Chown, R. Crocce, M. Cunha, C. E. da Costa, L. N. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Evrard, A. E. Fausti Neto, A. Flaugher, B. Frieman, J. Gruen, D. Gruendl, R. A. Gutierrez, G. de Haan, T. Holder, G. Honscheid, K. Hou, Z. James, D. J. Kuehn, K. Kuropatkin, N. Lima, M. March, M. Marshall, J. L. Martini, P. Melchior, P. Miller, C. J. Miquel, R. Mohr, J. J. Nord, B. Omori, Y. Plazas, A. A. Reichardt, C. Romer, A. K. Rykoff, E. S. Sanchez, E. Sevilla-Noarbe, I. Sheldon, E. Smith, R. C. Soares-Santos, M. Sobreira, F. Suchyta, E. Stark, A. Swanson, M. E. C. Tarle, G. Thomas, D. Walker, A. R. Wechsler, R. H. TI Joint measurement of lensing-galaxy correlations using SPT and DES SV data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: weak; cosmic background radiation; large-scale structure of the Universe ID SCIENCE VERIFICATION DATA; SOUTH-POLE TELESCOPE; PHOTOMETRIC REDSHIFT PDFS; BACKGROUND DAMPING TAIL; MATTER POWER SPECTRUM; DARK ENERGY SURVEY; SHEAR MEASUREMENT; DISTANT GALAXIES; MODEL; EVOLUTION AB We measure the correlation of galaxy lensing and cosmic microwave background lensing with a set of galaxies expected to trace the matter density field. The measurements are performed using pre-survey Dark Energy Survey (DES) Science Verification optical imaging data and millimetre-wave data from the 2500 sq. deg. South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey. The two lensing-galaxy correlations are jointly fit to extract constraints on cosmological parameters, constraints on the redshift distribution of the lens galaxies, and constraints on the absolute shear calibration of DES galaxy-lensing measurements. We show that an attractive feature of these fits is that they are fairly insensitive to the clustering bias of the galaxies used as matter tracers. The measurement presented in this work confirms that DES and SPT data are consistent with each other and with the currently favoured Lambda cold dark matter cosmological model. It also demonstrates that joint lensing-galaxy correlation measurement considered here contains a wealth of information that can be extracted using current and future surveys. C1 [Baxter, E.; Clampitt, J.; Jain, B.; Kwan, J.; Bernstein, G. M.; March, M.; Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Giannantonio, T.; Efstathiou, G.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Giannantonio, T.; Efstathiou, G.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Giannantonio, T.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. [Dodelson, S.; Benson, B.; Diehl, H. T.; Flaugher, B.; Frieman, J.; Gutierrez, G.; Kuropatkin, N.; Nord, B.; Soares-Santos, M.; Sobreira, F.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Dodelson, S.; Bleem, L.; Crawford, T.; Benson, B.; Carlstrom, J.; Frieman, J.; Hou, Z.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Huterer, D.; Evrard, A. E.; Miller, C. J.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Bleem, L.; Carlstrom, J.; Hou, Z.] Univ Chicago, Dept Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA. [Bleem, L.] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. [Crawford, T.; Benson, B.; Carlstrom, J.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Fosalba, P.; Carretero, J.; Crocce, M.] IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [Kirk, D.; Abdalla, F. B.; Benoit-Levy, A.; Brooks, D.; Doel, P.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Sanchez, C.; Carretero, J.; Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain. [Story, K.; Wechsler, R. H.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Story, K.; Cunha, C. E.; Gruen, D.; Rykoff, E. S.; Wechsler, R. H.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Troxel, M. A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Abbott, T. M. C.; James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Armstrong, R.; Melchior, P.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Benoit-Levy, A.; Bertin, E.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.; Bertin, E.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Bernstein, R. A.] Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA. [Carnero Rosell, A.; da Costa, L. N.; Fausti Neto, A.; Lima, M.; Sobreira, F.] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Chown, R.; de Haan, T.; Holder, G.; Omori, Y.] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Desai, S.; Dietrich, J. P.; Mohr, J. J.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Gruen, D.; Rykoff, E. S.; Wechsler, R. H.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [de Haan, T.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Honscheid, K.; Martini, P.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Martini, P.] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mohr, J. J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Reichardt, C.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, E-28040 Madrid, Spain. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Stark, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 12, Cambridge, MA 02138 USA. [Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. RP Baxter, E (reprint author), Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. EM ebax@sas.upenn.edu RI Lima, Marcos/E-8378-2010; OI Abdalla, Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658; Stark, Antony/0000-0002-2718-9996 FU US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago, University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; OzDES Membership Consortium; National Science Foundation [AST-1138766, PLR-1248097]; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union [240672, 291329, 306478]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation [947]; US Department of Energy [DE-AC02-06CH11357] FX This paper has gone through internal review by the DES collaboration. Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES.; The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium.; The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478.; The SPT programme is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago. Argonne National Laboratory's work was supported under the US Department of Energy contract DE-AC02-06CH11357. NR 65 TC 3 Z9 3 U1 5 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 4099 EP 4114 DI 10.1093/mnras/stw1584 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900057 ER PT J AU Garrison, LH Eisenstein, DJ Ferrer, D Metchnik, MV Pinto, PA AF Garrison, Lehman H. Eisenstein, Daniel J. Ferrer, Douglas Metchnik, Marc V. Pinto, Philip A. TI Improving initial conditions for cosmological N-body simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: haloes; large-scale structure of Universe ID PRECISION COSMOLOGY; 2-BODY RELAXATION; MASS FUNCTION; TRANSIENTS; HALOES; SPACE AB In cosmological N-body simulations, the representation of dark matter as discrete 'macroparticles' suppresses the growth of structure, such that simulations no longer reproduce linear theory on small scales near k(Nyquist). Marcos et al. demonstrate that this is due to sparse sampling of modes near k(Nyquist) and that the often-assumed continuum growing modes are not proper growing modes of the particle system. We develop initial conditions (ICs) that respect the particle linear theory growing modes and then rescale the mode amplitudes to account for growth suppression. These ICs also allow us to take advantage of our very accurate N-body code ABACUS to implement second-order Lagrangian perturbation theory (2LPT) in configuration space. The combination of 2LPT and rescaling improves the accuracy of the late-time power spectra, halo mass functions, and halo clustering. In particular, we achieve 1 per cent accuracy in the power spectrum down to k(Nyquist), versus k(Nyquist)/4 without rescaling or k(Nyquist)/13 without 2LPT, relative to an oversampled reference simulation. We anticipate that our 2LPT will be useful for large simulations where fast Fourier transforms are expensive and that rescaling will be useful for suites of medium-resolution simulations used in cosmic emulators and galaxy survey mock catalogues. Code to generate ICs is available at https://github.com/lgarrison/zeldovich-PLT. C1 [Garrison, Lehman H.; Eisenstein, Daniel J.; Ferrer, Douglas] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Metchnik, Marc V.; Pinto, Philip A.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85121 USA. RP Garrison, LH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lgarrison@cfa.harvard.edu OI Garrison, Lehman/0000-0002-9853-5673 FU National Science Foundation [AST-1313285, 1228509]; US Department of Energy [DE-SC0013718]; FAS Division of Science, Research Computing Group at Harvard University FX We thank Svetlin Tassev for helpful discussions and the referee for comments that helped improve the quality of this paper. We acknowledge use of the University of Washington N-body Shop friends-of friends code. Some computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. This work has been supported by grant AST-1313285 from the National Science Foundation and by grant DE-SC0013718 from the US Department of Energy. Some of the computations used in this study were performed on the El Gato supercomputer at the University of Arizona, supported by grant 1228509 from the National Science Foundation. NR 32 TC 1 Z9 1 U1 2 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 4125 EP 4145 DI 10.1093/mnras/stw1594 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900059 ER PT J AU Carroll, PA Line, J Morales, MF Barry, N Beardsley, AP Hazelton, BJ Jacobs, DC Pober, JC Sullivan, IS Webster, RL Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE de Oliveira-Costa, A Dillon, JS Emrich, D Ewall-Wice, A Feng, L Gaensler, BM Goeke, R Greenhill, LJ Hewitt, JN Hurley-Walker, N Johnston-Hollitt, M Kaplan, DL Kasper, JC Kim, HS Kratzenberg, E Lenc, E Loeb, A Lonsdale, CJ Lynch, MJ McKinley, B McWhirter, SR Mitchell, DA Morgan, E Neben, AR Oberoi, D Offringa, AR Ord, SM Paul, S Pindor, B Prabu, T Procopio, P Riding, J Rogers, AEE Roshi, A Shankar, NU Sethi, SK Srivani, KS Subrahmanyan, R Tegmark, M Thyagarajan, N Tingay, SJ Trott, CM Waterson, M Wayth, RB Whitney, AR Williams, A Williams, CL Wu, C Wyithe, JSB AF Carroll, P. A. Line, J. Morales, M. F. Barry, N. Beardsley, A. P. Hazelton, B. J. Jacobs, D. C. Pober, J. C. Sullivan, I. S. Webster, R. L. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. de Oliveira-Costa, A. Dillon, J. S. Emrich, D. Ewall-Wice, A. Feng, L. Gaensler, B. M. Goeke, R. Greenhill, L. J. Hewitt, J. N. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. L. Kasper, J. C. Kim, H. S. Kratzenberg, E. Lenc, E. Loeb, A. Lonsdale, C. J. Lynch, M. J. McKinley, B. McWhirter, S. R. Mitchell, D. A. Morgan, E. Neben, A. R. Oberoi, D. Offringa, A. R. Ord, S. M. Paul, S. Pindor, B. Prabu, T. Procopio, P. Riding, J. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Sethi, S. K. Srivani, K. S. Subrahmanyan, R. Tegmark, M. Thyagarajan, Nithyanandan Tingay, S. J. Trott, C. M. Waterson, M. Wayth, R. B. Whitney, A. R. Williams, A. Williams, C. L. Wu, C. Wyithe, J. S. B. TI A high reliability survey of discrete Epoch of Reionization foreground sources in the MWA EoR0 field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues ID MURCHISON WIDEFIELD ARRAY; CM POWER SPECTRA; SKY SURVEY; RADIO-SOURCES; DECONVOLUTION; CATALOG AB Detection of the epoch of reionization HI signal requires a precise understanding of the intervening galaxies and AGN, both for instrumental calibration and foreground removal. We present a catalogue of 7394 extragalactic sources at 182 MHz detected in the RA = 0 field of the Murchison Widefield Array Epoch of Reionization observation programme. Motivated by unprecedented requirements for precision and reliability we develop new methods for source finding and selection. We apply machine learning methods to self-consistently classify the relative reliability of 9490 source candidates. A subset of 7466 are selected based on reliability class and signal-to-noise ratio criteria. These are statistically cross-matched to four other radio surveys using both position and flux density information. We find 7369 sources to have confident matches, including 90 partially resolved sources that split into a total of 192 sub-components. An additional 25 unmatched sources are included as new radio detections. The catalogue sources have a median spectral index of -0.85. Spectral flattening is seen towards lower frequencies with a median of -0.71 predicted at 182 MHz. The astrometric error is 7 arcsec compared to a 2.3 arcmin beam FWHM. The resulting catalogue covers similar to 1400 deg(2) and is complete to approximately 80 mJy within half beam power. This provides the most reliable discrete source sky model available to date in the MWA EoR0 field for precision foreground subtraction. C1 [Carroll, P. A.; Morales, M. F.; Barry, N.; Beardsley, A. P.; Hazelton, B. J.; Pober, J. C.; Sullivan, I. S.] Univ Washington, Seattle, WA 98195 USA. [Line, J.; Webster, R. L.; Kim, H. S.; McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Wyithe, J. S. B.] Univ Melbourne, Parkville, Vic 3010, Australia. [Line, J.; Webster, R. L.; Briggs, F.; Gaensler, B. M.; Kim, H. S.; Lenc, E.; McKinley, B.; Mitchell, D. A.; Offringa, A. R.; Ord, S. M.; Pindor, B.; Procopio, P.; Riding, J.; Subrahmanyan, R.; Tingay, S. J.; Trott, C. M.; Wayth, R. B.; Wyithe, J. S. B.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Beardsley, A. P.; Jacobs, D. C.; Bowman, J. D.; Thyagarajan, Nithyanandan] Univ Washington, ESci Inst, Seattle, WA 98195 USA. [Hazelton, B. J.] Arizona State Univ, Tempe, AZ 85287 USA. [Pober, J. C.] Brown Univ, Providence, RI 02912 USA. [Bernardi, G.] SKA SA, ZA-7405 Cape Town, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6139 Grahamstown, South Africa. [Briggs, F.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [de Oliveira-Costa, A.; Dillon, J. S.; Ewall-Wice, A.; Feng, L.; Goeke, R.; Hewitt, J. N.; Morgan, E.; Neben, A. R.; Tegmark, M.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Dillon, J. S.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Emrich, D.; Hurley-Walker, N.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Trott, C. M.; Wayth, R. B.; Williams, A.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Gaensler, B. M.] Univ Sydney, Sydney, NSW 2006, Australia. [Gaensler, B. M.; Lenc, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Greenhill, L. J.; Kasper, J. C.; Loeb, A.] Victoria Univ Wellington, Sch Chem & Phys Sci, POB 600, Wellington 6140, New Zealand. [Johnston-Hollitt, M.] Univ Wisconsin, Milwaukee, WI 53211 USA. [Kaplan, D. L.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Kasper, J. C.] CSIRO Astron & Space Sci CASS, Marsfield, NSW 2122, Australia. [Mitchell, D. A.] Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Oberoi, D.] Netherlands Inst Radio Astron ASTRON, NL-7991 PD Dwingeloo, Netherlands. [Offringa, A. R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Paul, S.; Prabu, T.; Shankar, N. Udaya; Sethi, S. K.; Srivani, K. S.; Subrahmanyan, R.] Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. [Roshi, A.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia. [Waterson, M.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Waterson, M.; Wu, C.] Jodrell Bank, SKA Org Headquarters, Macclesfield SK11 9DL, Cheshire, England. RP Carroll, PA (reprint author), Univ Washington, Seattle, WA 98195 USA. EM pcarroll@uw.edu; jline@student.unimelb.au.edu; mmorales@phys.washington.edu RI Wayth, Randall/B-2444-2013; Udayashankar , N/D-4901-2012; Subrahmanyan, Ravi/D-4889-2012; OI Wayth, Randall/0000-0002-6995-4131; /0000-0002-0086-7363; Lenc, Emil/0000-0002-9994-1593 FU NVIDIA at Harvard University; American Australian Association Sir Keith Murdoch fellowship; University of Washington Graduate Opportunities and Minority Achievement Program dissertation fellowship; National Science Foundation [AST-0847753, AST-1410484, AST-1506024] FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the operation of the MWA is provided by the Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS), under a contract to Curtin University administered by Astronomy Australia Limited. We acknowledge the iVEC Petabyte Data Store and the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University.; PC would like to acknowledge the support of the American Australian Association Sir Keith Murdoch fellowship and the University of Washington Graduate Opportunities and Minority Achievement Program dissertation fellowship. This work was supported by National Science Foundation grants AST-0847753, AST-1410484, and AST-1506024. NR 34 TC 3 Z9 3 U1 5 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 4151 EP 4175 DI 10.1093/mnras/stw1599 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900061 ER PT J AU Maughan, BJ Giles, PA Rines, KJ Diaferio, A Geller, MJ Van Der Pyl, N Bonamente, M AF Maughan, Ben J. Giles, Paul A. Rines, Kenneth J. Diaferio, Antonaldo Geller, Margaret J. Van Der Pyl, Nina Bonamente, Massimiliano TI Hydrostatic and caustic mass profiles of galaxy clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: kinematics and dynamics; cosmology: observations; X-rays: galaxies: clusters ID WEAK-LENSING MASSES; X-RAY LUMINOSITY; TEMPERATURE RELATION; CROSS-CALIBRATION; SCALING RELATION; VIRIAL RADIUS; XMM-NEWTON; CHANDRA; SAMPLE; HECTOSPEC AB We compare X-ray and caustic mass profiles for a sample of 16 massive galaxy clusters. We assume hydrostatic equilibrium in interpreting the X-ray data, and use large samples of cluster members with redshifts as a basis for applying the caustic technique. The hydrostatic and caustic masses agree to better than approximate to 20 per cent on average across the radial range covered by both techniques (similar to[0.2-1.25] R-500). The mass profiles were measured independently and do not assume a common functional form. Previous studies suggest that, at R-500, the hydrostatic and caustic masses are biased low and high, respectively. We find that the ratio of hydrostatic to caustic mass at R-500 is 1.20(-0.11)(+0.13); thus it is larger than 0.9 at approximate to 3 sigma and the combination of under-and overestimation of the mass by these two techniques is approximate to 10 per cent at most. There is no indication of any dependence of the mass ratio on the X-ray morphology of the clusters, indicating that the hydrostatic masses are not strongly systematically affected by the dynamical state of the clusters. Overall, our results favour a small value of the so-called hydrostatic bias due to non-thermal pressure sources. C1 [Maughan, Ben J.; Giles, Paul A.; Van Der Pyl, Nina] Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. [Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Rines, Kenneth J.; Geller, Margaret J.] Smithsonian Astrophys Observ, 60 Garden St,MS 20, Cambridge, MA 02138 USA. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis, Via P Giuria 1, I-10125 Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, Via P Giuria 1, I-10125 Turin, Italy. [Bonamente, Massimiliano] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Bonamente, Massimiliano] NASA, Natl Space Sci & Technol Ctr, Huntsville, AL 35812 USA. RP Maughan, BJ (reprint author), Univ Bristol, HH Wills Phys Lab, Tyndall Ave, Bristol BS8 1TL, Avon, England. EM ben.maughan@bristol.ac.uk FU STFC [ST/J001414/1, ST/M000907/1]; University of Torino [Progetti di Ateneo/CSP_TO_Call2_2012_0011 'Marco Polo']; INFN grant InDark; grant PRIN 'Fisica Astroparticellare Teorica' of the Italian Ministry of University and Research FX BJM and PAG acknowledge support from STFC grants ST/J001414/1 and ST/M000907/1. AD acknowledges support from the grant Progetti di Ateneo/CSP_TO_Call2_2012_0011 'Marco Polo' of the University of Torino, the INFN grant InDark, and the grant PRIN 2012 'Fisica Astroparticellare Teorica' of the Italian Ministry of University and Research. NR 56 TC 2 Z9 2 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 4182 EP 4191 DI 10.1093/mnras/stw1610 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900063 ER PT J AU Schaal, K Springel, V Pakmor, R Pfrommer, C Nelson, D Vogelsberger, M Genel, S Pillepich, A Sijacki, D Hernquist, L AF Schaal, Kevin Springel, Volker Pakmor, Ruediger Pfrommer, Christoph Nelson, Dylan Vogelsberger, Mark Genel, Shy Pillepich, Annalisa Sijacki, Debora Hernquist, Lars TI Shock finding on a moving-mesh - II. Hydrodynamic shocks in the Illustris universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; shock waves; methods: numerical; galaxies: clusters: general; galaxies: kinematics and dynamics; large-scale structure of Universe ID LARGE-SCALE STRUCTURE; GAMMA-RAY EMISSION; SIMULATING COSMIC-RAYS; COSMOLOGICAL GAS ACCRETION; GALAXY FORMATION PHYSICS; EXTENDED RADIO-EMISSION; X-RAY; STAR-FORMATION; BLACK-HOLES; BOW SHOCK AB Hydrodynamical shocks are a manifestation of the non-linearity of the Euler equations and play a fundamental role in cosmological gas dynamics. In this work, we identify and analyse shocks in the Illustris simulation, and contrast the results with those of non-radiative runs. We show that simulations with more comprehensive physical models of galaxy formation pose new challenges for shock finding algorithms due to radiative cooling and star-forming processes, prompting us to develop a number of methodology improvements. We find in Illustris a total shock surface area which is about 1.4 times larger at the present epoch compared to non-radiative runs, and an energy dissipation rate at shocks which is higher by a factor of around 7. Remarkably, shocks with Mach numbers above and below M approximate to 10 contribute about equally to the total dissipation across cosmic time. This is in sharp contrast to non-radiative simulations, and we demonstrate that a large part of the difference arises due to strong black hole radiomode feedback in Illustris. We also provide an overview of the large diversity of shock morphologies, which includes complex networks of halo-internal shocks, shocks on to cosmic sheets, feedback shocks due to black holes and galactic winds, as well as ubiquitous accretion shocks. In high-redshift systems more massive than 10(12) M-circle dot, we discover the existence of a double accretion shock pattern in haloes. They are created when gas streams along filaments without being shocked at the outer accretion shock, but then forms a second, roughly spherical accretion shock further inside. C1 [Schaal, Kevin; Springel, Volker; Pakmor, Ruediger; Pfrommer, Christoph] Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. [Schaal, Kevin; Springel, Volker] Heidelberg Univ, Zentrum Astron, Astron Recheninst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. [Nelson, Dylan] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. [Vogelsberger, Mark] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. [Genel, Shy] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. [Pillepich, Annalisa; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Sijacki, Debora] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. RP Schaal, K (reprint author), Heidelberg Inst Theoret Studies, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany.; Schaal, K (reprint author), Heidelberg Univ, Zentrum Astron, Astron Recheninst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. EM kevin.schaal@h-its.org; volker.springel@h-its.org FU subproject EXAMAG of the Priority Programme of the German Science Foundation [1648 SPPEXA]; European Research Council through ERC-StG grant [EXAGAL-308037]; ERC-CoG grant [CRAGSMAN-646955]; NASA through Hubble Fellowship - STScI [HST-HF2-51341.001-A]; NASA [NAS5-26555, NNX12AC67G]; STFC; ERC [638707]; NSF [AST-1312095]; IMPRS for Astronomy and Cosmic Physics at the University of Heidelberg FX It is a pleasure to thank Andreas Bauer, Rainer Weinberger, Christian Arnold, Christine Simpson, Robert Grand, Martin Sparre, Federico Marinacci, Rahul Kannan, Lorenzo Sironi, and Blakesley Burkhart for useful comments and insightful discussions. Moreover, the authors would like to thank the referee for a constructive report which helped improving this paper. KS and VS acknowledge support through subproject EXAMAG of the Priority Programme 1648 SPPEXA of the German Science Foundation, and the European Research Council through ERC-StG grant EXAGAL-308037. CP acknowledges support through the ERC-CoG grant CRAGSMAN-646955. SG acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51341.001-A awarded by the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. DS acknowledges support by the STFC and the ERC Starting Grant 638707 'BHs and their host galaxies: co-evolution across cosmic time'. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. KS, VS, RP, and CP like to thank the Klaus Tschira Foundation, and KS acknowledges support by the IMPRS for Astronomy and Cosmic Physics at the University of Heidelberg. NR 120 TC 2 Z9 2 U1 3 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2016 VL 461 IS 4 BP 4441 EP 4465 DI 10.1093/mnras/stw1587 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW3AS UT WOS:000383514900086 ER PT J AU Oster, JL Kelley, NP AF Oster, Jessica L. Kelley, Neil P. TI Tracking regional and global teleconnections recorded by western North American speleothem records SO QUATERNARY SCIENCE REVIEWS LA English DT Review DE Speleothem; Western North America; Oxygen isotopes; Paleoclimate ID SOUTHWESTERN UNITED-STATES; LAST GLACIAL MAXIMUM; ATLANTIC THERMOHALINE CIRCULATION; INTERTROPICAL CONVERGENCE ZONE; STABLE-ISOTOPE VARIATIONS; EAST-ASIAN MONSOON; GULF-OF-MEXICO; CLIMATE-CHANGE; MILLENNIAL-SCALE; HIGH-RESOLUTION AB Speleothem proxy records are useful for interrogating past climates in the low and mid-latitudes given their ability to provide continuous, high-resolution, and long-lived records that can be dated with high precision. Several speleothem oxygen isotope records from western North America have recently been developed that highlight the importance of this archive in documenting past changes in atmospheric circulation. Taken individually, these records hint at teleconnections between western North American hydroclimate and climate changes in the high northern latitudes and tropics. However, there has been no systematic investigation of global climate teleconnections to this region that draws upon the body of North American speleothem records as a whole. Here we review the dominant controls on precipitation oxygen isotopes across the region, and conduct statistical comparisons and network visualizations of high-resolution speleothem oxygen isotope records from western North America to investigate the regional response to pronounced climate changes of the last deglaciation and to determine the pattern of global teleconnections to this region. We find that most western North American speleothem oxygen isotope records demonstrate a robust and consistent response to the events of the last deglaciation, despite differing controls on the oxygen isotope ratio of precipitation across the region. One record that receives a strong influence from the Gulf of Mexico exhibits a contrasting pattern in oxygen isotopes relative to most of the other records, which are dominated by westerly storms generated in the Pacific. During the studied interval, major shifts in Western North American speleothem records appear broadly synchronous at least within the uncertainty of age models. We also find strong statistical linkages between western North American speleothem records and speleothem records of Asian monsoon variability and other records from regions directly influenced by movement of the Intertropical Convergence Zone, demonstrating that nearly synchronous changes in atmospheric circulation measurably altered precipitation dynamics in these regions during the last deglaciation. Further multi-proxy investigations are needed to determine how such changes in atmospheric circulation recorded by speleothem oxygen isotope ratios influenced precipitation amounts in drought-prone western North America. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Oster, Jessica L.; Kelley, Neil P.] Vanderbilt Univ, Dept Earth & Environm Sci, Nashville, TN 37235 USA. [Kelley, Neil P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Oster, JL (reprint author), Vanderbilt Univ, Dept Earth & Environm Sci, Nashville, TN 37235 USA. EM jessica.l.oster@vanderbilt.edu OI Oster, Jessica/0000-0002-1780-2435 FU NSF [AGS-1203701]; Peter S. Buck postdoctoral fellowship FX This work was supported by NSF grant AGS-1203701 to JLO and a Peter S. Buck postdoctoral fellowship to NPK. NR 133 TC 1 Z9 1 U1 9 U2 9 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD OCT 1 PY 2016 VL 149 BP 18 EP 33 DI 10.1016/j.quascirev.2016.07.009 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA DW7IW UT WOS:000383825400002 ER PT J AU Ghafouri, B Amiri, BJ Shabani, AA Songer, M AF Ghafouri, Bahareh Amiri, Bahman Jabbarian Shabani, Afshin Alizadeh Songer, Melissa TI Examining Relationships Between Socioeconomic Factors and Landscape Metrics in the Southern Basin of the Caspian Sea SO ENVIRONMENTAL MODELING & ASSESSMENT LA English DT Article DE Landscape pattern; Human-related factors; Landscape ecological metrics; Mazandaran; Guilan; Multiple linear regression ID LAND-COVER; URBAN-GROWTH; POPULATION-DENSITY; PATTERN AB Socioeconomic forces are not only among the main drivers of landscape dynamics; they are also influenced by landscape patterns. Landscape structure and functions are closely related to natural and social factors. The objective of this study was to investigate the relationships among some human-related factors and landscape ecological metrics as landscape pattern indicators and to identify suitable metrics for modeling these relationships. To this goal, landscape ecological metrics were calculated for each of the 32 counties of Mazandaran and Guilan provinces located in the southern basin of the Caspian Sea using land use/cover maps in class level. Stream network metrics were calculated using a digital elevation model, road density metrics were calculated using map of main roads separately, and significant metrics were selected according to results of correlation tests and factor analysis. The correlations between these metrics and socioeconomic factors were tested, and their relationships were modeled with multiple linear regressions. Significant relationships were found among socioeconomic factors and landscape ecological metrics, and land use/cover data are applicable for modeling socioeconomic factors, especially demographic and employment structure factors. Among the landscape metrics applied in this study, road density, mean patch size, mean nearest neighbor distance, and percentage of a land use/cover class in landscape were important metrics for predicting socioeconomic factors. Our findings indicated that road density metric and percentages of urban class are useful for predicting urban socioeconomic factors and percentage of agriculture and forest classes in the landscape are suitable metrics for predicting rural socioeconomic factors. C1 [Ghafouri, Bahareh; Amiri, Bahman Jabbarian; Shabani, Afshin Alizadeh] Univ Tehran, Fac Nat Resources, Dept Environm Sci, Karaj 3158777878, Iran. [Songer, Melissa] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. RP Amiri, BJ (reprint author), Univ Tehran, Fac Nat Resources, Dept Environm Sci, Karaj 3158777878, Iran. EM Bahareh.ghafoori@ut.ac.ir; jabbarian@ut.ac.ir; Ashabani@ut.ac.ir; Songerm@si.edu OI Jabbarian Amiri, Bahman/0000-0003-1382-786X NR 34 TC 0 Z9 0 U1 7 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1420-2026 EI 1573-2967 J9 ENVIRON MODEL ASSESS JI Environ. Model. Assess. PD OCT PY 2016 VL 21 IS 5 BP 669 EP 680 DI 10.1007/s10666-016-9503-9 PG 12 WC Environmental Sciences SC Environmental Sciences & Ecology GA DU1TY UT WOS:000381993700009 ER PT J AU Sonsthagen, SA Wilson, RE Chesser, RT Pons, JM Crochet, PA Driskell, A Dove, C AF Sonsthagen, Sarah A. Wilson, Robert E. Chesser, R. Terry Pons, Jean-Marc Crochet, Pierre-Andre Driskell, Amy Dove, Carla TI Recurrent hybridization and recent origin obscure phylogenetic relationships within the 'white-headed' gull (Larus sp.) complex SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Hybridization; Laridae; Multilocus phylogeny; Speciation; White-headed gulls ID RECENT SECONDARY CONTACT; HYBRID ZONES; GENE FLOW; HELICONIUS BUTTERFLIES; REPRODUCTIVE ISOLATION; POPULATION-STRUCTURE; MOLECULAR PHYLOGENY; GENOMIC LANDSCAPE; LOCAL ADAPTATION; SEXUAL SELECTION AB Species complexes that have undergone recent radiations are often characterized by extensive allele sharing due to recent ancestry and (or) introgressive hybridization. This can result in discordant evolutionary histories of genes and heterogeneous genomes, making delineating species limits difficult. Here we examine the phylogenetic relationships among a complex group of birds, the white-headed gulls (Ayes: Laridae), which offer a unique window into the speciation process due to their recent evolutionary history and propensity to hybridize. Relationships were examined among 17 species (61 populations) using a multilocus approach, including mitochondria] and nuclear intron DNA sequences and microsatellite genotype information. Analyses of microsatellite and intron data resulted in some species-based groupings, although most species were not represented by a single cluster. Considerable allele and haplotype sharing among white-headed gull species was observed; no locus contained a species-specific Glade. Despite this, our multilocus approach provided better resolution among some species than previous studies. Interestingly, most clades appear to correspond to geographic locality: our BEAST analysis recovered strong support for a northern European/Icelandic Glade, a southern European/Russian Glade, and a western North American/cams Glade, with weak evidence for a high latitude Glade spanning North America and northwestern Europe. This geographical structuring is concordant with behavioral observations of pervasive hybridization in areas of secondary contact. The extent of allele and haplotype sharing indicates that ecological and sexual selection are likely not strong enough to complete reproductive isolation within several species in the white-headed gull complex. This suggests that just a few genes are driving the speciation process. Published by Elsevier Inc. C1 [Sonsthagen, Sarah A.; Dove, Carla] Smithsonian Inst, Dept Vertebrate Zool, Div Birds, Natl Museum Nat Hist, Washington, DC 20013 USA. [Sonsthagen, Sarah A.; Driskell, Amy] Smithsonian Inst, Labs Analyt Biol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Sonsthagen, Sarah A.; Wilson, Robert E.] US Geol Survey, Alaska Sci Ctr, 4210 Univ Dr, Anchorage, AK 99508 USA. [Wilson, Robert E.] Univ Alaska Fairbanks, Inst Arctic Biol, Fairbanks, AK 99775 USA. [Chesser, R. Terry] US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Pons, Jean-Marc] Univ Paris 04, Inst Systemat Evolut Biodivers, Dept Systemat & Evolut, CNRS,MNHN,UPMC,EPHE,UMR 7205, CP 51,55 Rue Buffon, F-75231 Paris 05, France. [Pons, Jean-Marc] MNHN, CNRS, UMS Outils & Methodes Systemat Integrat OMSI 2700, 57 Rue Cuvier, F-75231 Paris 05, France. [Crochet, Pierre-Andre] Univ Paul Valery Montpellier, Univ Montpellier, CNRS, EPHE,CEFE UMR 5175, 1919 Route Mende, F-34293 Montpellier 5, France. RP Sonsthagen, SA (reprint author), US Geol Survey, Alaska Sci Ctr, 4210 Univ Dr, Anchorage, AK 99508 USA. EM ssonsthagen@usgs.gov FU Federal Aviation Administration (FM); Laboratories of Analytical Biology and Division of Birds, National Museum of Natural History, Smithsonian Institution FX Funding was provided by the Federal Aviation Administration (FM) and the Laboratories of Analytical Biology and Division of Birds, National Museum of Natural History, Smithsonian Institution. We thank the following museums and Dr. David Boertmann for their significant contributions of tissues for this work; Academy of Natural Sciences of Philadelphia, American Museum of Natural History, Bell Museum of Natural History, Burke Museum of Natural History and Culture, California Academy of Sciences, Cornell University Museum of Vertebrates, Field Museum of Natural History, Louisiana State University Museum of Natural Science, Museo Argentino de Ciencias Naturales, Natural History Museum of Los Angeles County, U.S. National Museum of Natural History, New York State Museum, Royal Alberta Museum, Royal Ontario Museum, University of Alaska Anchorage Museum, University of Alaska Museum, University of California Berkeley Museum of Vertebrate Zoology, University of Kansas Biodiversity Institute, and University of Michigan Museum of Zoology. We would also like to thank the numerous individuals that helped facilitate field work for the various museums; Jeffrey Hunt, Smithsonian Institution, who provided technical laboratory support; Christopher Milensky and Faridah Dahlan, Smithsonian Institution, for assistance with sample collection and preparation; and Marcy Heacker and Lee Weigt, Smithsonian Institution, and Kevin Omland, University of Maryland Baltimore County, for their guidance and advice throughout this project. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 89 TC 0 Z9 0 U1 18 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2016 VL 103 BP 41 EP 54 DI 10.1016/j.ympev.2016.06.008 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA DT9PS UT WOS:000381835400005 PM 27369453 ER PT J AU Larabee, FJ Fisher, BK Schmidt, CA Matos-Maravi, P Janda, M Suarez, AV AF Larabee, Fredrick J. Fisher, Brian K. Schmidt, Chris A. Matos-Maravi, Pavel Janda, Milan Suarez, Andrew V. TI Molecular phylogenetics and diversification of trap jaw ants in the genera Anochetus and Odontomachus (Hymenoptera: Formicidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Odontomachus; Anochetus; Trap-jaw ants; Ants; Phylogenetics ID GEOGRAPHIC RANGE; MANDIBLE STRIKE; MODEL SELECTION; EVOLUTION; PONERINAE; INFERENCE; TREES; BIOGEOGRAPHY; MORPHOLOGY; BEHAVIOR AB Ants in the genera Anochetus and Odontomachus belong to one of the largest clades in the subfamily Ponerinae, and are one of four lineages of ants possessing spring-loaded "trap -jaws." Here we present results from the first global species-level molecular phylogenetic analysis of these trap jaw ants, reconstructed from one mitochondria], one ribosomal RNA, and three nuclear protein-coding genes. Bayesian and likelihood analyses strongly support reciprocal monophyly for the genera Anochetus and Odontomachus. Additionally, we found strong support for seven trap-jaw ant clades (four in Anochetus and three in Odontomachus) mostly concordant with geographic distribution. Ambiguity remains concerning the closest living non-trap-jaw ant relative of the Anochetus + Odontomachus Glade, but Bayes factor hypothesis testing strongly suggests that trap jaw ants evolved from a short mandible ancestor. Ponerine trap jaw ants originated in the early Eocene (52.5 Mya) in either South America or Southeast Asia, where they have radiated rapidly in the last 30 million years, and subsequently dispersed multiple times to Africa and Australia. These results will guide future taxonomic work on the group and act as a phylogenetic framework to study the macroevolution of extreme ant mouthpart specialization. (C) 2016 Elsevier Inc. All rights reserved. C1 [Larabee, Fredrick J.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 169, Washington, DC 20560 USA. [Larabee, Fredrick J.; Suarez, Andrew V.] Univ Illinois, Dept Entomol, 320 Morrill Hall, Urbana, IL 61801 USA. [Fisher, Brian K.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. [Schmidt, Chris A.] Univ Arizona, Mel & Enid Zuckerman Coll Publ Hlth, Tucson, AZ USA. [Schmidt, Chris A.] Univ Arizona, Dept Entomol, Tucson, AZ USA. [Matos-Maravi, Pavel; Janda, Milan] Acad Sci Czech Republic, Ctr Biol, Inst Entomol, Ceske Budejovice, Czech Republic. [Matos-Maravi, Pavel] Univ South Bohemia, Fac Sci, Dept Zool, Ceske Budejovice, Czech Republic. [Janda, Milan] Univ Guanajuato, Dept Biol, Guanajuato, Mexico. [Suarez, Andrew V.] Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. RP Larabee, FJ (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 169, Washington, DC 20560 USA. EM larabeef@si.edu FU University of Illinois School of Integrative Biology; Peter Buck Foundation; National Science Foundation [DDIG DEB 1407279]; Czech Science Foundation [P505/12/2467]; Marie Curie Fellowship [PIOFGA2009-25448]; GAJU grant [156/2013/P] FX Ant samples used in this study comply to the regulations for export and exchange of research samples outlined in the Convention of Biology Diversity and the Convention on International Trade in Endangered Species of Wild Fauna and Flora. For samples collected in Australia, Madagascar, Malaysia, Peru, Uganda, Venezuela, permits to research, collect and export ants were obtained by BLF as part of Ant Course organized by BLF. We are grateful to the staff of the New Guinea Binatang Research Center for indispensable field assistance, to V. Novotny and S.E. Miller for advice and support of this research, and to the Papua New Guinea Department of Environment and Conservation for assistance with research permits. Many individuals donated or loaned specimens and their generosity is appreciated: L.E. Alonso, E.P. Economo, J.A. Holley, D. General, A. Jesovnik, J. Lapolla, J.T. Longino, A. Lucky, C. S. Moreau, E.M. Sarnat, T.R. Schultz, P.S. Ward, J. Wetterer, A. Wild, and B.D. Wills. We thank T.R. Schultz and two anonymous reviewers for their comments for improving early drafts of the manuscript. Assistance in the SI Laboratories of Analytical Biology was provided by M.W. Lloyd. FJL was supported from funds from the University of Illinois School of Integrative Biology, the Peter Buck Foundation, and the National Science Foundation (DDIG DEB 1407279). PMM and MJ were supported by Czech Science Foundation (P505/12/2467), Marie Curie Fellowship (PIOFGA2009-25448) and the GAJU grant (156/2013/P). NR 67 TC 0 Z9 0 U1 19 U2 19 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2016 VL 103 BP 143 EP 154 DI 10.1016/j.ympev.2016.07.024 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA DT9PS UT WOS:000381835400014 PM 27450781 ER PT J AU Darroch, SAF Boag, TH Racicot, RA Tweedt, S Mason, SJ Erwin, DH Laflamme, M AF Darroch, Simon A. F. Boag, Thomas H. Racicot, Rachel A. Tweedt, Sarah Mason, Sara J. Erwin, Douglas H. Laflamme, Marc TI A mixed Ediacaran-metazoan assemblage from the Zaris Sub-basin, Namibia SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Ediacaran; Cambrian; Metazoans; Trace fossil; Ecosystem engineering; Conichnus; Shaanxilithes; Aspidella ID PRECAMBRIAN-CAMBRIAN BOUNDARY; MISTAKEN POINT; TRACE FOSSILS; NAMA GROUP; SOUTHERN NAMIBIA; MACROSCOPIC COMMUNITIES; ESCAPE STRUCTURES; UNITED-STATES; 1ST FINDS; NEWFOUNDLAND AB It has been proposed that the terminal Neoproterozoic Ediacara biota were driven to extinction by the evolution of metazoan groups capable of engineering their environments (the 'biotic replacement' model). However, evidence for an overlapping ecological association between metazoans and soft-bodied Ediacaran organisms is limited. Here, we describe new fossil localities from southern Namibia that preserve soft-bodied Ediacara biota, enigmatic tubular organisms thought to represent metazoans, and vertically-oriented metazoan trace fossils. Although the precise identity of the tracemakers remains elusive, the structures bear several striking similarities with the Cambrian-Recent ichnogenus Conichnus. These new data support inference of stratigraphic and ecological overlap between two very different eukaryotic clades, and indicate the existence of unusual ecosystems comprising both Ediacara biota and metazoans immediately prior to the Cambrian explosion. (C) 2016 Elsevier B.V. All rights reserved. C1 [Darroch, Simon A. F.] Vanderbilt Univ, Dept Earth & Environm Sci, 2301 Vanderbilt Pl, Nashville, TN 37235 USA. [Darroch, Simon A. F.; Racicot, Rachel A.; Tweedt, Sarah; Erwin, Douglas H.] Smithsonian Inst, POB 37012,MRC 121, Washington, DC 20013 USA. [Boag, Thomas H.] Stanford Univ, Dept Geol Sci, 450 Serra Mall,Bldg 320,Room 118, Stanford, CA 94305 USA. [Racicot, Rachel A.] Nat Hist Museum Los Angeles Cty, Dinosaur Inst, 900 Exposit Blv, Los Angeles, CA 90007 USA. [Mason, Sara J.; Laflamme, Marc] Univ Toronto Mississauga, Dept Chem & Phys Sci, 3356 Mississauga Rd North, Mississauga, ON L5L 1C6, Canada. RP Darroch, SAF (reprint author), Vanderbilt Univ, Dept Earth & Environm Sci, 2301 Vanderbilt Pl, Nashville, TN 37235 USA. EM simon.a.darroch@vanderbilt.edu; tomboag@stanford.edu; rracicot@nhm.org; tweedts@si.edu; s.mason@mail.utoronto.ca; Erwind@si.edu; marc.laflamme@utoronto.ca FU Yale Peabody Museum of Natural History; NSF [DEB 1331980, PLR 134175]; NASA National Astrobiology Institute [NNA13AA90A]; Connaught Foundation; National Science and Engineering Research Council of Canada (NSERC) [RGPIN 435402]; National Geographic Society [9241-13]; Mary H. Beatty Fellowship FX We extend thanks to the Geological Survey of Namibia, and in particular Helke Mocke, Charlie Hoffmann, Roger Swart, and Gabi Schneider for logistical help in conducting fieldwork. S.A.F.D. and R.A.R. thank the Yale Peabody Museum of Natural History for generous financial support. R.A.R. is currently funded by NSF grants DEB 1331980 and PLR 134175 to N. Smith. M.L., S.T., and D.H.E. thank the NASA National Astrobiology Institute (Grant # NNA13AA90A); M.L. and T.H.B. thank the Connaught Foundation, National Science and Engineering Research Council of Canada (NSERC 2013 Discovery Grant RGPIN 435402 to M.L., and an NSERC Graduate MSc Scholarship to T.H.B.), and National Geographic Society (GRANT #9241-13 to M.L.) for generous funding. This work was supported by a Mary H. Beatty Fellowship to T.H.B. We also thank Luis Buatois, Gabriela Mangano, and Lidya Tarhan for constructive criticism, and Rachel Jongsma for assistance in the field. NR 85 TC 2 Z9 2 U1 10 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD OCT 1 PY 2016 VL 459 BP 198 EP 208 DI 10.1016/j.palaeo.2016.07.003 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA DV0EU UT WOS:000382591600015 ER PT J AU Baumgardner, RW DiMichele, WA Vieira, ND AF Baumgardner, Robert W., Jr. DiMichele, William A. Vieira, Nathalia de Siqueira TI An early Permian coastal flora dominated by Germaropteris martinsii from basinal sediments in the Midland Basin, West Texas SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Peltasperm; Sphenopteris; Supaia; Wolfcamp ID NEW-MEXICO; RED BEDS; PALEOBOTANY; PALYNOLOGY; MOUNTAINS; PANGEA AB Fossils found in cores from wells in the Midland Basin of West Texas include several kinds of terrestrial plants and a variety of marine animal remains. Depositional settings ranged from basin slope to deep-water basin floor, hence the presence of land plants was unexpected. The fossil plant assemblage is depauperate, dominated by Germaropteris martinsii, a Permian-age peltasperm. Other specimens include the peltasperm Supaia, Sphenopteris germanica, axes of uncertain affinity, and incertae sedis remains presumed to be terrestrial plants. Fossil plants are found predominantly in fine-grained, siliceous mudrocks between coarser-grained calcareous floatstones and wackestones/packstones interpreted as debrites and turbidites, suggesting that the plants were carried from land by surface currents before sinking to the basin floor and being buried by slowly accumulating hemipelagic sediment. Specimens were examined from drillcores in 14 wells spanning an interval from the lower Wolfcamp through the lower Leonard. This record of G. martinsii in lower Permian Wolfcamp rocks is among the earliest occurrences of these plants, which have been found most abundantly in upper Permian strata of Western Europe. (C) 2016 Elsevier B.V. All rights reserved. C1 [Baumgardner, Robert W., Jr.] Univ Texas Austin, Bur Econ Geol, Jackson Sch Geosci, Austin, TX 78713 USA. [DiMichele, William A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Vieira, Nathalia de Siqueira] Univ Fed Ouro Preto, Engn Geol, BR-35400000 Ouro Preto, MG, Brazil. RP Baumgardner, RW (reprint author), Univ Texas Austin, Bur Econ Geol, Jackson Sch Geosci, Austin, TX 78713 USA. EM robert.baumgardner@beg.utexas.edu FU Mudrock Systems Research Lab consortium at the Bureau of Economic Geology, Jackson School of Geosciences, The University of Texas at Austin [OSP 200803001] FX This work was supported by funding from the Mudrock Systems Research Lab consortium at the Bureau of Economic Geology, Jackson School of Geosciences, The University of Texas at Austin (OSP 200803001). Members included Anadarko, Apache, BHP, BP, Cenovus, Centrica, Chesapeake, Chevron, Cima, Cimarex, Concho, ConocoPhillips, Cypress, Devon, Encana, ENI, EOG, EXCO, ExxonMobil, FEI, Hess, Husky, IMP, Kerogen, Marathon, Murphy, Newfield, Oxy, Penn Virginia, Penn West, Pioneer, QEP, Samson, Shell, StatOil, Talisman, Texas American Resources, The Unconventionals, US Enercorp, Valence, and YPF. Cores were donated to the CRC by Shell and BP Amoco/Altura. CT scan of the R. Ricker 1 core was provided by Ingrain, Inc., Houston, TX. Core access and sampling were provided by CRC personnel: James Donnelly, Andrew Faigle, Nathan Ivicic, Randy McDonald, Bill Molthen, and Brandon Williamson. The authors thank Robert Hook for his assistance with this project, including identification and selection of fossil specimens, and we thank Greg Wahlman for his guidance in sorting out the chronostratigraphy of the study interval. Ann Molineux, Director, and Angella Thompson of the Non-Vertebrate Paleontology Laboratory at The University of Texas at Austin were instrumental in archiving samples collected during this study. Megan Carter of the Interdisciplinary Earth Data Alliance (IEDA) facilitated registration of the sample metadata in the SESAR database. Text was edited by Stephanie Jones. Core photographs were prepared for publication by David Stephens. Illustrations were edited by Cathy Brown. Reviews by Thomas Algeo and two anonymous reviewers materially improved the manuscript. Publication authorized by the Director, Bureau of Economic Geology. NR 70 TC 0 Z9 0 U1 3 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD OCT 1 PY 2016 VL 459 BP 409 EP 422 DI 10.1016/j.palaeo.2016.07.024 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA DV0EU UT WOS:000382591600028 ER PT J AU Chen, XG Namjoo, MH Wang, Y AF Chen, Xingang Namjoo, Mohammad Hossein Wang, Yi TI A direct probe of the evolutionary history of the primordial universe SO SCIENCE CHINA-PHYSICS MECHANICS & ASTRONOMY LA English DT Letter ID INFLATIONARY UNIVERSE; DENSITY PERTURBATIONS; GRAVITY-WAVES; POLARIZATION; SUPERNOVAE; FLATNESS; HORIZON; VACUUM C1 [Chen, Xingang; Namjoo, Mohammad Hossein] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. [Wang, Yi] Hong Kong Univ Sci & Technol, Dept Phys, Kowloon, Hong Kong, Peoples R China. RP Chen, XG; Namjoo, MH (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA.; Wang, Y (reprint author), Hong Kong Univ Sci & Technol, Dept Phys, Kowloon, Hong Kong, Peoples R China. EM xingang.chen@cfa.harvard.edu; mohammad.namjoo@cfa.harvard.edu; phyw@ust.hk NR 36 TC 2 Z9 2 U1 1 U2 1 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 1674-7348 EI 1869-1927 J9 SCI CHINA PHYS MECH JI Sci. China-Phys. Mech. Astron. PD OCT PY 2016 VL 59 IS 10 AR 101021 DI 10.1007/s11433-016-0278-8 PG 4 WC Physics, Multidisciplinary SC Physics GA DU6ZL UT WOS:000382363000008 ER PT J AU Latham, DW AF Latham, David W. TI Celebrating Paper 250 SO OBSERVATORY LA English DT Letter C1 [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Solar Stellar & Planetary Sci Div, 60 Garden St, Cambridge, MA 02138 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, Solar Stellar & Planetary Sci Div, 60 Garden St, Cambridge, MA 02138 USA. EM dlatham@cfa.harvard.edu NR 2 TC 0 Z9 0 U1 0 U2 0 PU OBSERVATORY PI OXFORD PA RUTHERFORD APPLETON LAB, CHILTON DIDCOT,, OXFORD OX11 OQX, ENGLAND SN 0029-7704 J9 OBSERVATORY JI Observatory PD OCT PY 2016 VL 136 IS 1254 BP 233 EP 235 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DU6VO UT WOS:000382352900004 ER PT J AU Toon, GC Blavier, JF Sung, K Rothman, LS Gordon, IE AF Toon, Geoffrey C. Blavier, Jean-Francois Sung, Keeyoon Rothman, Laurence S. Gordon, Iouli E. TI HITRAN spectroscopy evaluation using solar occultation FTIR spectra SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Spectroscopy; Infrared; Atmosphere; Remote Sensing; HITRAN ID DATABASE; (CH4)-C-12; PARAMETERS; REGION; SYSTEM; OXYGEN; BAND AB High resolution FTIR solar occultation spectra, acquired by the JPL MkIV Fourier transform spectrometer from balloon, covering 650-5650 cm(-1) at 0.01 cm(-1) resolution, are systematically analyzed using the last four versions of the HITRAN linelist (2000, 2004, 2008, 2012). The rms spectral fitting residuals are used to assess the quality and adequacy of the linelists as a function of wavenumber and altitude. Although there have been substantial overall improvements with each successive version of HITRAN, there are nevertheless a few spectral regions where the latest HITRAN version (2012) has regressed, or produces residuals that far exceed the noise level. A few of these instances are investigated further and their causes identified. We emphasize that fitting atmospheric spectra, in addition to laboratory spectra, should be part of the quality assurance for any new linelist before public release. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Toon, Geoffrey C.; Blavier, Jean-Francois; Sung, Keeyoon] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Rothman, Laurence S.; Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Toon, GC (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM Geoffrey.C.Toon@jpl.nasa.gov RI Sung, Keeyoon/I-6533-2015 FU NASA's Upper Atmosphere Research Program [NNH12ZDA001N-UACO]; NASA AURA program Grant [NNX14AI55G] FX We thank NASA's Upper Atmosphere Research Program who funded the JPL MkIV instrument through Grant NNH12ZDA001N-UACO. The Columbia Scientific Balloon Facility (CSBF) who launched the balloon and recovered the MkIV payload. The HITRAN team gratefully acknowledges support from the NASA AURA program Grant NNX14AI55G. We also thank the Worldwide spectroscopy community whose work is encapsulated in the HITRAN linelists. Part of this research was performed at the Jet Propulsion Laboratory, California of Technology, under contract with NASA. NR 27 TC 1 Z9 1 U1 3 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2016 VL 182 BP 324 EP 336 DI 10.1016/j.jqsrt.2016.05.021 PG 13 WC Optics; Spectroscopy SC Optics; Spectroscopy GA DT2OZ UT WOS:000381321600028 ER PT J AU Prissel, TC Whitten, JL Parman, SW Head, JW AF Prissel, Tabb C. Whitten, Jennifer L. Parman, Stephen W. Head, James W. TI On the potential for lunar highlands Mg-suite extrusive volcanism and implications concerning crustal evolution SO ICARUS LA English DT Article DE Moon; Volcanism; Geological processes; Spectroscopy ID PROCELLARUM KREEP TERRANE; MAGMATIC SILICATE LIQUIDS; FLOOR-FRACTURED CRATERS; MOONS INTERIOR; MARE VOLCANISM; GRAIL GRAVITY; REFLECTANCE SPECTROSCOPY; IGNEOUS ACTIVITY; MAGNESIAN SUITE; BASALT AB The lunar magnesian-suite (Mg-suite) was produced during the earliest periods of magmatic activity on the Moon. Based on the cumulate textures of the samples and a lack of evidence for Mg-suite extrusives in both the sample and remote sensing databases, several petrogenetic models deduce a predominantly intrusive magmatic history for Mg-suite lithologies. Considering that similar to 18% of the lunar surface is covered by mare basalt flows, which are substantially higher in density than estimated Mg-suite magmas (similar to 2900 versus similar to 2700 kg/m(3)), the apparent absence of low-density Mg-suite volcanics is surprising. Were Mg-suite magmas predominantly intrusive, or have their extrusive equivalents been covered by subsequent impact ejecta and/or later stage volcanism? If Mg-suite magmas were predominantly intrusive, what prevented these melts from erupting? Or, if they are present as extrusives, what regions of the Moon are most likely to contain Mg-suite volcanic deposits? This study investigates buoyancy-driven ascent of Mg-suite parental melts and is motivated by recent measurements of crustal density from GRAIL. Mg-suite dunite, troctolite, and spinel anorthosite parental melts (2742, 2699, and 2648 kg/m(3), respectively) are considered, all of which have much lower melt densities relative to mare basalts and picritic glasses. Mg-suite parental melts are more dense than most of the crust and would not be expected to buoyantly erupt. However, about 10% of the lunar crust is greater in density than Mg-suite melts. These areas are primarily within the nearside southern highlands and South Pole-Aitken (SP-A) basin. Mg-suite extrusions and/or shallow intrusions were possible within these regions, assuming crustal density structure at >4.1 Ga was similar to the present day crust. We review evidence for Mg-suite activity within both the southern highlands and SP-A and discuss the implications concerning crustal evolution as well as Mg-suite petrogenesis. Lower crustal densities measured by GRAIL are consistent with the lack of observed Mg-suite extrusives. If Mg-suite extrusive volcanism was prevented by the low density of the crust, it would suggest the lunar crust was fractured shortly after solidification (>4.3 Ga). The thermal-and stress-state of the lunar crust may have also inhibited Mg-suite extrusion. (C) 2016 Elsevier Inc. All rights reserved. C1 [Prissel, Tabb C.; Parman, Stephen W.; Head, James W.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Whitten, Jennifer L.] Smithsonian Inst, MRC 315,POB 37012, Washington, DC 20013 USA. RP Prissel, TC (reprint author), Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. EM tcprissel@gmail.com FU NASA SSERVI Grant [NNA14AB01A] FX We would like to thank and greatly appreciate Mark Wieczorek and the GRAIL team for the gravity data used in this study. We also extend a special thank you to both Brad Jolliff for fruitful conversations and Oded Aharonson for serving as our editor. This manuscript benefited from the insightful reviews of Larry Taylor, Satoru Yamamoto, and one unnamed reviewer. This research was supported through the NASA SSERVI Grant NNA14AB01A. NR 107 TC 0 Z9 0 U1 8 U2 8 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD OCT PY 2016 VL 277 BP 319 EP 329 DI 10.1016/j.icarus.2016.05.018 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DS1UB UT WOS:000380385100022 ER PT J AU Brusatte, SL Carr, TD Williamson, TE Holtz, TR Hone, DWE Williams, SA AF Brusatte, Stephen L. Carr, Thomas D. Williamson, Thomas E. Holtz, Thomas R., Jr. Hone, David W. E. Williams, Scott A. TI Dentary groove morphology does not distinguish 'Nanotyrannus' as a valid taxon of tyrannosauroid dinosaur. Comment on: "Distribution of the dentary groove of theropod dinosaurs: Implications for theropod phylogeny and the validity of the genus Nanotyrannus Bakker et al., 1988" SO CRETACEOUS RESEARCH LA English DT Editorial Material DE Nanotyrannus; Tyrannosaurus; Tyrannosauroid; Dinosaur; Theropod; Ontogeny ID OSTEOLOGY; EVOLUTION; MONGOLIA; HISTORY; SIZE AB There has been considerable debate about whether the controversial tyrannosauroid dinosaur 'Nanotyrannus lancensis' from the uppermost Cretaceous of North America is a valid taxon or a juvenile of the contemporaneous Tyrannosaurus rex. In a recent Cretaceous Research article, Schmerge and Rothschild (2016) brought a new piece of evidence to this discussion: the morphology of the dentary groove, a depression on the lateral surface of the dentary that houses neurovascular foramina. They argued that an alleged 'Nanotyrannus' specimen, which possesses a groove, cannot be referable to Tyrannosaurus rex, which they considered as lacking the groove, and they hypothesized that 'Nanotyrannus' is closely related to albertosaurine tyrannosauroids, which also are said to possess the groove. However, we show that the groove is a widespread feature of tyrannosauroids that is present in T. rex and many other specimens, and that it is an ontogenetically variable feature that changes from a sharp, deeply-impressed groove to a shallower sulcus as an individual matures. As a result, the presence or absence of a dentary groove does not clarify the validity of 'Nanotyrannus' or its phylogenetic position among tyrannosauroids. We consider it most parsimonious that 'Nanotyrannus' specimens belong to juvenile T. rex. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Brusatte, Stephen L.] Univ Edinburgh, Grant Inst, Sch Geosci, James Hutton Rd, Edinburgh EH9 3FE, Midlothian, Scotland. [Carr, Thomas D.] Carthage Coll, Dept Biol, 2001 Alford Pk Dr, Kenosha, WI 53140 USA. [Williamson, Thomas E.] New Mexico Museum Nat Hist & Sci, 1801 Mt Rd NW, Albuquerque, NM 87104 USA. [Holtz, Thomas R., Jr.] Univ Maryland, Dept Geol, 8000 Regents Dr, College Pk, MD 20742 USA. [Holtz, Thomas R., Jr.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Hone, David W. E.] Queen Mary Univ London, Sch Biol & Chem Sci, Mile End Rd, London E1 4NS, England. [Williams, Scott A.] Burpee Museum Nat Hist, 737 North Main St, Rockford, IL 60115 USA. RP Brusatte, SL (reprint author), Univ Edinburgh, Grant Inst, Sch Geosci, James Hutton Rd, Edinburgh EH9 3FE, Midlothian, Scotland. EM Stephen.Brusatte@ed.ac.uk NR 29 TC 1 Z9 1 U1 11 U2 11 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD OCT PY 2016 VL 65 BP 232 EP 237 DI 10.1016/j.cretres.2016.02.007 PG 6 WC Geology; Paleontology SC Geology; Paleontology GA DP0LY UT WOS:000378182500019 ER PT J AU Perez, LM Carpenter, JM Andrews, SM Ricci, L Isella, A Linz, H Sargent, AI Wilner, DJ Henning, T Deller, AT Chandler, CJ Dullemond, CP Lazio, J Menten, KM Corder, SA Storm, S Testi, L Tazzari, M Kwon, W Calvet, N Greaves, JS Harris, RJ Mundy, LG AF Perez, Laura M. Carpenter, John M. Andrews, Sean M. Ricci, Luca Isella, Andrea Linz, Hendrik Sargent, Anneila I. Wilner, David J. Henning, Thomas Deller, Adam T. Chandler, Claire J. Dullemond, Cornelis P. Lazio, Joseph Menten, Karl M. Corder, Stuartt A. Storm, Shaye Testi, Leonardo Tazzari, Marco Kwon, Woojin Calvet, Nuria Greaves, Jane S. Harris, Robert J. Mundy, Lee G. TI Spiral density waves in a young protoplanetary disk SO SCIENCE LA English DT Article ID GRAVITATING CIRCUMSTELLAR DISCS; STAR-FORMATION; AB AURIGAE; MWC 758; ARMS; ACCRETION; OPHIUCHUS; IMAGES; PLANET; ALMA AB Gravitational forces are expected to excite spiral density waves in protoplanetary disks, disks of gas and dust orbiting young stars. However, previous observations that showed spiral structure were not able to probe disk midplanes, where most of the mass is concentrated and where planet formation takes place. Using the Atacama Large Millimeter/submillimeter Array, we detected a pair of trailing symmetric spiral arms in the protoplanetary disk surrounding the young star Elias 2-27. The arms extend to the disk outer regions and can be traced down to the midplane. These millimeter-wave observations also reveal an emission gap closer to the star than the spiral arms. We argue that the observed spirals trace shocks of spiral density waves in the midplane of this young disk. C1 [Perez, Laura M.; Menten, Karl M.] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. [Carpenter, John M.; Corder, Stuartt A.] Joint Atacama Large Millimeter Submillimeter Arra, Ave Alonso Cordova 3107, Santiago, Chile. [Andrews, Sean M.; Ricci, Luca; Wilner, David J.; Storm, Shaye] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Isella, Andrea] Rice Univ, 6100 Main St, Houston, TX 77005 USA. [Linz, Hendrik; Henning, Thomas] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Sargent, Anneila I.] CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. [Deller, Adam T.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Chandler, Claire J.] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA. [Dullemond, Cornelis P.] Heidelberg Univ, Ctr Astron, Albert Ueberle Str 2, Heidelberg, Germany. [Lazio, Joseph] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91106 USA. [Testi, Leonardo; Tazzari, Marco] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Testi, Leonardo] Ist Nazl Astrofis INAF Osservatorio Astrofis Arce, Largo E Fermi 5, I-50125 Florence, Italy. [Kwon, Woojin] Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea. [Kwon, Woojin] Korea Univ Sci & Technol, 217 Gajeong Ro, Daejeon 34113, South Korea. [Calvet, Nuria] Univ Michigan, 830 Dennison Bldg,500 Church St, Ann Arbor, MI 48109 USA. [Greaves, Jane S.] Cardiff Univ, Sch Phys & Astron, 4 Parade, Cardiff CF24 3AA, S Glam, Wales. [Harris, Robert J.] Univ Illinois, 1002 West Green St, Urbana, IL 61801 USA. [Mundy, Lee G.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Perez, LM (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM lperez@mpifr-bonn.mpg.de OI Tazzari, Marco/0000-0003-3590-5814; Deller, Adam/0000-0001-9434-3837 FU Alexander von Humboldt Foundation; NSF [AST-1109334/1535809, AST 1140063]; NASA Origins of Solar Systems program [NNX14AD26G] FX We thank L. Loinard for useful discussions. L.M.P. acknowledges support from the Alexander von Humboldt Foundation. A.I. acknowledges support from NSF award AST-1109334/1535809 and from the NASA Origins of Solar Systems program through award NNX14AD26G. A.I.S. is partially supported by NSF grant AST 1140063. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation (NSF) operated under cooperative agreement by Associated Universities Inc. (AUI). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00498.S, which can be obtained from the ALMA Science Data Archive, https://almascience.nrao.edu/alma-data (raw format) and from https://safe.nrao.edu/evla/disks/elias2-27 in the calibrated fits format used for analysis here. ALMA is a partnership of the European Southern Observatory (ESO) (representing its member states), NSF (USA) and the National Institute of Natural Sciences (Japan), together with the National Research Council (Canada), National Science Council and Academia Sinica's Institute of Astronomy and Astrophysics (Taiwan), and the Korea Astronomy and Space Science Institute (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and the National Astronomical Observatory of Japan. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. NR 30 TC 7 Z9 7 U1 2 U2 2 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 30 PY 2016 VL 353 IS 6307 BP 1519 EP 1521 DI 10.1126/science.aaf8296 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA EB8YU UT WOS:000387678700040 PM 27708098 ER PT J AU Cowie, RH Heros, V Yeung, NW Hayes, KA AF Cowie, Robert H. Heros, Virginie Yeung, Norine W. Hayes, Kenneth A. TI Annotated catalogue of types of Hawaiian land and freshwater snails (Mollusca: Gastropoda) in the Museum national d'Histoire naturelle, Paris, with lectotype designations. Addendum: lectotype designation for Lymnaea affinis Souleyet, 1852 SO ZOOSYSTEMA LA English DT Article DE Lymnaeidae; types; MNHN; Hawaii; lectotypification AB A catalogue of types of Hawaiian land and freshwater snails (Mollusca: Gastropoda) deposited in the Museum national d'Histoire naturelle (MNHN), Paris, was recently published in Zoosystema. Type material of an additional species, Lymnaea affinis Souleyet, 1852, has since been found and is here documented and a lectotype designated. C1 [Cowie, Robert H.; Yeung, Norine W.] Univ Hawaii, Pacific Biosci Res Ctr, 3050 Maile Way,Gilmore 408, Honolulu, HI 96822 USA. [Heros, Virginie] Univ Paris 04, Museum Natl Hist Nat, Inst Systemat Evolut Biodiversite, UMR 7205,CNRS,MNHN,UPMC,EPHE, Case Postale 50,57 Rue Cuvier, F-75231 Paris 05, France. [Yeung, Norine W.] Bernice P Bishop Museum, 1525 Bernice St, Honolulu, HI 96817 USA. [Yeung, Norine W.; Hayes, Kenneth A.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hayes, Kenneth A.] Howard Univ, Dept Biol, 415 Coll St NW,EE 332, Washington, DC 20059 USA. RP Cowie, RH (reprint author), Univ Hawaii, Pacific Biosci Res Ctr, 3050 Maile Way,Gilmore 408, Honolulu, HI 96822 USA. EM cowie@hawaii.edu; malaco@mnhn.fr; nyeung@hawaii.edu; kenneth.hayes@howard.edu FU US National Science Foundation [DEB-1120906]; MNHN Visiting Curatorship; Manuel Caballer of the MNHN project E-RECOLNAT [ANR-11-INBS-0004] FX We thank Carl Christensen for alerting us to the presence of type material of Lymnaea affinis in the MNHN and Manuel Caballer of the MNHN project E-RECOLNAT ANR-11-INBS-0004 for photographing the lectotype and preparing Figure 1. This work is part of a US National Science Foundation funded project (DEB-1120906) and was partially supported by an MNHN Visiting Curatorship to Robert Cowie, initiated by Philippe Bouchet, whom we thank for his support. This paper constitutes Contributions no. 2016-006 to the Hawaii Biological Survey and 9707 of the University of Hawaii School of Ocean and Earth Science and Technology. NR 13 TC 0 Z9 0 U1 2 U2 2 PU PUBLICATIONS SCIENTIFIQUES DU MUSEUM, PARIS PI PARIS CEDEX 05 PA CP 39-57, RUE CUVIER, F-75231 PARIS CEDEX 05, FRANCE SN 1280-9551 EI 1638-9387 J9 ZOOSYSTEMA JI Zoosystema PD SEP 30 PY 2016 VL 38 IS 3 BP 389 EP 391 DI 10.5252/z2016n3a6 PG 3 WC Zoology SC Zoology GA DY9BO UT WOS:000385427500006 ER PT J AU Cleary, DFR Polonia, ARM Renema, W Hoeksema, BW Rachello-Dolmen, PG Moolenbeek, RG Budiyanto, A Yahmantoro Tuti, Y Giyanto Draisma, SGA van Reine, WFP Hariyanto, R Gittenberger, A Rikoh, MS de Voogd, NJ AF Cleary, D. F. R. Polonia, A. R. M. Renema, W. Hoeksema, B. W. Rachello-Dolmen, P. G. Moolenbeek, R. G. Budiyanto, A. Yahmantoro Tuti, Y. Giyanto Draisma, S. G. A. van Reine, W. F. Prud'homme Hariyanto, R. Gittenberger, A. Rikoh, M. S. de Voogd, N. J. TI Variation in the composition of corals, fishes, sponges, echinoderms, ascidians, molluscs, foraminifera and macroalgae across a pronounced in-to-offshore environmental gradient in the Jakarta Bay-Thousand Islands coral reef complex SO MARINE POLLUTION BULLETIN LA English DT Article DE Composition; Redundancy analysis; Multi-taxon; Urbanisation ID GREAT-BARRIER-REEF; LONG-TERM CHANGES; SPERMONDE ARCHIPELAGO; WATER-QUALITY; BENTHIC FORAMINIFERA; SW SULAWESI; SCLERACTINIA FUNGIIDAE; DISTRIBUTION PATTERNS; COMMUNITY COMPOSITION; OULASTREA-CRISPATA AB Substrate cover, water quality parameters and assemblages of corals, fishes, sponges, echinoderms, ascidians, molluscs, benthic foraminifera and macroalgae were sampled across a pronounced environmental gradient in the Jakarta Bay-Thousand Islands reef complex. Inshore sites mainly consisted of sand, rubble and turf algae with elevated temperature, dissolved oxygen, pH and chlorophyll concentrations and depauperate assemblages of all taxa. Live coral cover was very low inshore and mainly consisted of sparse massive coral heads and a few encrusting species. Faunal assemblages were more speciose and compositionally distinct mid- and offshore compared to inshore. There were, however, small-scale differences among taxa. Certain midshore sites, for example, housed assemblages resembling those typical of the inshore environment but this differed depending on the taxon. Substrate, water quality and spatial variables together explained from 31% (molluscs) to 72% (foraminifera) of the variation in composition. In general, satellite-derived parameters outperformed locally measured parameters. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Cleary, D. F. R.; Polonia, A. R. M.] Univ Aveiro, Dept Biol, CESAM, Campus Univ Santiago, P-3810193 Aveiro, Portugal. [Renema, W.; Hoeksema, B. W.; Moolenbeek, R. G.; van Reine, W. F. Prud'homme; Gittenberger, A.; de Voogd, N. J.] Nat Biodivers Ctr, Darwinweg 2, NL-2333 CR Leiden, Netherlands. [Hoeksema, B. W.; Gittenberger, A.] Leiden Univ, Inst Biol IBL, POB 9516, NL-2300 RA Leiden, Netherlands. [Rachello-Dolmen, P. G.] Smithsonian Trop Res Inst, Naos Isl Marine Lab, Panama City 205219100, Panama. [Rachello-Dolmen, P. G.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA. [Budiyanto, A.; Yahmantoro; Tuti, Y.; Giyanto; Hariyanto, R.; Rikoh, M. S.] Indonesian Inst Sci, Res Ctr Oceanog, Pasir Putih 1, Ancol Timur 11048, Jakarta Utara, Indonesia. [Draisma, S. G. A.] Prince Songkla Univ, Fac Sci, Ctr Excellence Biodivers Peninsular Thailand, Hat Yai 90112, Songkhla, Thailand. [Gittenberger, A.] GiMaRIS, JH Oortweg 21, NL-2333 CH Leiden, Netherlands. RP de Voogd, NJ (reprint author), Nat Biodivers Ctr, Darwinweg 2, NL-2333 CR Leiden, Netherlands. EM nicole.devoogd@naturalis.nl RI Renema, Willem/E-2851-2016; Hoeksema, Bert/B-2973-2010; CESAM, UA/M-3762-2015; OI Renema, Willem/0000-0002-1627-5995; Hoeksema, Bert/0000-0001-8259-3783; Draisma, Stefano/0000-0002-0446-908X FU Council for Earth and Life Sciences of the Netherlands Organisation for Scientific Research (ALW-NWO) [852.000.50]; Portuguese Foundation for Science and Technology (FCT) [PTDC/AAC-AMB/115304/2009]; NWO-WOTRO [R 85-381] FX This publication is a result of the Thousand Islands Expedition, September 2005, organized by the Research Centre for Oceanography (PPO-LIPI, Jakarta, Indonesia) and Naturalis Biodiversity Center (Leiden, the Netherlands). The research by Naturalis was part of the project 'Climate change and Indonesian coral reef biotas' within the theme 'Biodiversity in Relation to Global Change' of the Council for Earth and Life Sciences of the Netherlands Organisation for Scientific Research (ALW-NWO grant 852.000.50). DFRC was supported by the Portuguese Foundation for Science and Technology (FCT) under grant PTDC/AAC-AMB/115304/2009 (LESS CORAL). WFP'hvR and SGAD were supported by NWO-WOTRO grant R 85-381. We are grateful to LIPI for granting research permits. We thank staff of PPO-LIPI for logistical support. NR 111 TC 3 Z9 3 U1 15 U2 15 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD SEP 30 PY 2016 VL 110 IS 2 BP 701 EP 717 DI 10.1016/j.marpolbu1.2016.04.042 PG 17 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA DX4XJ UT WOS:000384384100010 PM 27179997 ER PT J AU Gonzalez-Terrazas, TP Koblitz, JC Fleming, TH Medellin, RA Kalko, EKV Schnitzler, HU Tschapka, M AF Gonzalez-Terrazas, Tania P. Koblitz, Jens C. Fleming, Theodore H. Medellin, Rodrigo A. Kalko, Elisabeth K. V. Schnitzler, Hans-Ulrich Tschapka, Marco TI How Nectar-Feeding Bats Localize their Food: Echolocation Behavior of Leptonycteris yerbabuenae Approaching Cactus Flowers SO PLOS ONE LA English DT Article ID FRUIT-EATING BATS; DESERT COLUMNAR CACTI; MACROPHYLLUM-MACROPHYLLUM; CAROLLIA-PERSPICILLATA; POLLINATION BIOLOGY; EPTESICUS-FUSCUS; MEXICO; PHYLLOSTOMIDAE; OLFACTION; NIVALIS AB Nectar-feeding bats show morphological, physiological, and behavioral adaptations for feeding on nectar. How they find and localize flowers is still poorly understood. While scent cues alone allow no precise localization of a floral target, the spatial properties of flower echoes are very precise and could play a major role, particularly at close range. The aim of this study is to understand the role of echolocation for classification and localization of flowers. We compared the approach behavior of Leptonycteris yerbabuenae to flowers of a columnar cactus, Pachycereus pringlei, to that to an acrylic hollow hemisphere that is acoustically conspicuous to bats, but has different acoustic properties and, contrary to the cactus flower, present no scent. For recording the flight and echolocation behaviour we used two infrared video cameras under stroboscopic illumination synchronized with ultrasound recordings. During search flights all individuals identified both targets as a possible food source and initiated an approach flight; however, they visited only the cactus flower. In experiments with the acrylic hemisphere bats aborted the approach at ca. 40-50 cm. In the last instant before the flower visit the bats emitted a long terminal group of 10-20 calls. This is the first report of this behaviour for a nectar-feeding bat. Our findings suggest that L. yerbabuenae use echolocation for classification and localization of cactus flowers and that the echo-acoustic characteristics of the flower guide the bats directly to the flower opening. C1 [Gonzalez-Terrazas, Tania P.; Kalko, Elisabeth K. V.; Tschapka, Marco] Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, Ulm, Germany. [Koblitz, Jens C.] BioAcoust Network, Neuss, Germany. [Fleming, Theodore H.] Univ Miami, Dept Biol, Miami, FL USA. [Medellin, Rodrigo A.] Univ Nacl Autonoma Mexico, Inst Ecol, Mexico City, DF, Mexico. [Kalko, Elisabeth K. V.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. [Schnitzler, Hans-Ulrich] Univ Tubingen, Inst Neurobiol, Anim Physiol, Tubingen, Germany. RP Gonzalez-Terrazas, TP (reprint author), Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, Ulm, Germany. EM tania.gonzalez@uni-ulm.de FU University of Ulm; CONACYT-DAAD FX This study was supported by the University of Ulm (to EKVK and MT) and a grant from CONACYT-DAAD (to TPG-T). NR 54 TC 0 Z9 0 U1 21 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 29 PY 2016 VL 11 IS 9 AR e0163492 DI 10.1371/journal.pone.0163492 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DX4CV UT WOS:000384328500062 PM 27684373 ER PT J AU Pabst, S Sytcheva, A Geffert, O Santra, R AF Pabst, Stefan Sytcheva, Arina Geffert, Otfried Santra, Robin TI Stability of the time-dependent configuration-interaction-singles method in the attosecond and strong-field regimes: A study of basis sets and absorption methods SO PHYSICAL REVIEW A LA English DT Article ID HIGH HARMONIC-GENERATION; GENERALIZED PSEUDOSPECTRAL METHOD; MULTIELECTRON DYNAMICS; MULTIPHOTON DETACHMENT; THRESHOLD-IONIZATION; LASER CONTROL; RESONANCES; SPECTROSCOPY; POTENTIALS; MOLECULES AB We investigate the behavior of several spatial grid methods and complex absorbers for strong-field and attosecond scenarios when using the time-dependent configuration-interaction singles method to solve the multi-electron time-dependent Schrodinger equation for atoms. We compare the pseudospectral grid, finite-element, and finite-element-discrete-variable-representation (DVR) methods with each other and discuss their advantages and disadvantages. Additionally, we study the performances of complex absorbing potential (CAP) and smooth exterior complex scaling (SES) to absorb the outgoing electron. We find that SES performs generally better than CAP for calculating high-harmonic generation spectra and XUV photoelectron spectra. In both of these cases, the DVR and even more the FEM grid representations show more reliable results-especially when using SES. Both absorbers show drawbacks when calculating photoelectron spectra in the strong-field regime. C1 [Pabst, Stefan] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Pabst, Stefan; Sytcheva, Arina; Geffert, Otfried; Santra, Robin] DESY, Ctr Free Electron Laser Sci, Notkestr 85, D-22607 Hamburg, Germany. [Santra, Robin] Univ Hamburg, Dept Phys, Jungiusstr 9, D-20355 Hamburg, Germany. RP Pabst, S (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA.; Pabst, S; Santra, R (reprint author), DESY, Ctr Free Electron Laser Sci, Notkestr 85, D-22607 Hamburg, Germany.; Santra, R (reprint author), Univ Hamburg, Dept Phys, Jungiusstr 9, D-20355 Hamburg, Germany. EM stefan.pabst@cfa.harvard.edu; robin.santra@cfel.de RI Santra, Robin/E-8332-2014; Pabst, Stefan/J-6541-2013 OI Santra, Robin/0000-0002-1442-9815; Pabst, Stefan/0000-0003-1134-4629 FU Alexander von Humboldt Foundation; NSF; Deutsche Forschungs-Gemeinschaft (DFG) [SFB 925/A5] FX S.P. is funded by the Alexander von Humboldt Foundation and by the NSF through a grant to ITAMP. This work has been supported by the Deutsche Forschungs-Gemeinschaft (DFG) under Grant No. SFB 925/A5. NR 66 TC 0 Z9 0 U1 4 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD SEP 29 PY 2016 VL 94 IS 3 AR 033421 DI 10.1103/PhysRevA.94.033421 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DX4SY UT WOS:000384372600012 ER PT J AU Forrey, RC Babb, JF Stancil, PC McLaughlin, BM AF Forrey, Robert C. Babb, James F. Stancil, Phillip C. McLaughlin, Brendan M. TI Formation of silicon monoxide by radiative association: the impact of resonances SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article DE radiative association; resonances; silicon monoxide ID ELECTRONIC STATES; SIO MOLECULE; BASIS-SETS; ATOMS; COLLISIONS; C+ AB Detailed quantum chemistry calculations within the multireference configuration interaction approximation with the Davidson correction are presented using an aug-cc-pV6Z basis set, for the potential energy curves and transition dipole moments between low lying molecular states of singlet spin symmetry for the SiO molecule. The high quality molecular data are used to obtain radiative association cross sections and rate coefficients for collisions between ground state Si and O atoms. Quantal calculations are compared with semiclassical results. Using a quantum kinetic theory of radiative association in which quasibound levels are assumed to be in local thermodynamic equilibrium, we find that resonances play an important role in enhancing the rate coefficients at low temperatures by several orders of magnitude from that predicted by standard quantum scattering formulations. These new molecular formation rates may have important implications for applications in astrophysics. C1 [Forrey, Robert C.] Penn State Univ, Dept Phys, Berks Campus, Reading, PA 19610 USA. [Babb, James F.; McLaughlin, Brendan M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, MS-14, Cambridge, MA 02138 USA. [Stancil, Phillip C.] Univ Georgia, Dept Phys & Astron, Athens, GA 30602 USA. [Stancil, Phillip C.] Univ Georgia, Ctr Simulat Phys, Athens, GA 30602 USA. [McLaughlin, Brendan M.] Queens Univ Belfast, Ctr Theoret Atom Mol & Opt Phys CTAMOP, Sch Math & Phys, David Bates Bldg,7 Coll Pk, Belfast BT7 1NN, Antrim, North Ireland. RP Forrey, RC (reprint author), Penn State Univ, Dept Phys, Berks Campus, Reading, PA 19610 USA. EM rcf6@psu.edu; bmclaughlin899@btinternet.com OI Babb, James/0000-0002-3883-9501 FU NSF [PHY-1203228, PHY-1503615]; NASA [NNX15AI61G]; Queen's University Belfast FX RCF acknowledges support from NSF Grant Nos. PHY-1203228 and PHY-1503615. PCS acknowledges support from NASA grant NNX15AI61G. BMMcL acknowledges support from NSF through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics under the visitors program, and Queen's University Belfast for the award of a visiting research fellowship (VRF). The electronic structure work was carried out at the National Energy Research Scientific Computing Center in Oakland, CA, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart, Stuttgart, Germany. NR 44 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-4075 EI 1361-6455 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 28 PY 2016 VL 48 IS 18 AR 184002 DI 10.1088/0953-4075/49/18/184002 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DX2QA UT WOS:000384214400001 ER PT J AU Gao, TP Shih, CK Labandeira, CC Santiago-Blay, JA Yao, YZ Ren, D AF Gao, Taiping Shih, Chungkun Labandeira, Conrad C. Santiago-Blay, Jorge A. Yao, Yunzhi Ren, Dong TI Convergent evolution of ramified antennae in insect lineages from the Early Cretaceous of Northeastern China SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE trichoptera; mecoptera; hymenoptera; sensilla; pectinate antennae; key innovation ID DUPLICATED GENES; COLEOPTERA; SENSILLA; ORIGIN; HYMENOPTERA; TRICHOPTERA; ROBUSTNESS; DIVERGENCE; MORPHOLOGY; MECOPTERA AB Antennae are important, insect sensory organs that are used principally for communication with other insects and the detection of environmental cues. Some insects independently evolved ramified (branched) antennae, which house several types of sensilla for motion detection, sensing olfactory and chemical cues, and determining humidity and temperature levels. Though ramified antennae are common in living insects, occasionally they are present in the Mesozoic fossil record. Here, we present the first caddisflies with ramified antennae, the earliest known fossil sawfly, and a scorpionfly also with ramified antennae from the mid-Lower Cretaceous Yixian Formation of Northeastern China, dated at 125 million years ago (Ma). These three insect taxa with ramified antennae consist of three unrelated lineages and provide evidence for broad structural convergence that historically has been best demonstrated by features such as convergent mouthparts. In addition, ramified antennae in these Mid-Mesozoic lineages likely do not constitute a key innovation, as they are not associated with significantly increased diversification compared with closely related lineages lacking this trait, and nor are they ecologically isolated from numerous, co-occurring insect species with unmodified antennae. C1 [Gao, Taiping; Shih, Chungkun; Labandeira, Conrad C.; Yao, Yunzhi; Ren, Dong] Capital Normal Univ, Coll Life Sci, 105 Xisanhuanbeilu, Beijing 100048, Peoples R China. [Shih, Chungkun; Labandeira, Conrad C.; Santiago-Blay, Jorge A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. [Santiago-Blay, Jorge A.] Univ Puerto Rico, Dept Crop & Agroenvironm Sci, Mayaguez, PR 00681 USA. RP Gao, TP; Ren, D (reprint author), Capital Normal Univ, Coll Life Sci, 105 Xisanhuanbeilu, Beijing 100048, Peoples R China. EM tpgao@cnu.edu.cn; rendong@mail.cnu.edu.cn FU National Natural Science Foundation of China [31230065, 31672323, 31401993]; Program for Changjiang Scholars and Innovative Research Team at University [IRT13081] FX D.R. was supported by grants from the National Natural Science Foundation of China (grant nos. 31230065 and 31672323), Program for Changjiang Scholars and Innovative Research Team at University (IRT13081); T.P.G. was supported by the National Natural Science Foundation of China (31401993). This is contribution 310 of the Evolution of Terrestrial Ecosystems consortium of the National Museum of Natural History, in Washington, D.C. NR 56 TC 0 Z9 0 U1 3 U2 3 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD SEP 28 PY 2016 VL 283 IS 1839 AR 20161448 DI 10.1098/rspb.2016.1448 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA EA3GG UT WOS:000386489200012 ER PT J AU Stuurman, CM Osinski, GR Holt, JW Levy, JS Brothers, TC Kerrigan, M Campbell, BA AF Stuurman, C. M. Osinski, G. R. Holt, J. W. Levy, J. S. Brothers, T. C. Kerrigan, M. Campbell, B. A. TI SHARAD detection and characterization of subsurface water ice deposits in Utopia Planitia, Mars SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ARCADIA PLANITIA; CLIMATE-CHANGE; GROUND ICE; EXCESS ICE; MIDLATITUDES; EVOLUTION; ORIGIN; ANTARCTICA; TOPOGRAPHY; OBLIQUITY AB Morphological analyses of Utopia Planitia, Mars, have led to the hypothesis that the region contains a substantial amount of near-surface ice. This paper tests this hypothesis using ground-penetrating radar techniques. We have identified an expansive radar reflective region spanning approximately 375,000 km(2) in SHAllow RADar (SHARAD) data over western Utopia Planitia. The SHARAD reflective regions coincides with high densities of scalloped depressions and polygonal terrain. The reflectors are associated with layered mesas similar to 80-170 m thick. We find a value of 2.8 +/- 0.8 for the dielectric constant of the material overlying the reflectors. This work finds that the dielectric constant is consistent with a mixture of ice, air, and dust, containing a water ice volume up to 14,300 km(3) in this unit. C1 [Stuurman, C. M.; Holt, J. W.; Levy, J. S.; Brothers, T. C.; Campbell, B. A.] Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA. [Stuurman, C. M.; Osinski, G. R.; Kerrigan, M.] Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, London, ON, Canada. [Osinski, G. R.] Univ Western Ontario, Dept Phys & Astron, London, ON, Canada. [Brothers, T. C.] Malin Space Sci Syst, San Diego, CA USA. [Campbell, B. A.] Smithsonian Inst, Washington, DC 20560 USA. RP Stuurman, CM (reprint author), Univ Texas Austin, Inst Geophys, Austin, TX 78712 USA.; Stuurman, CM (reprint author), Univ Western Ontario, Dept Earth Sci, Ctr Planetary Sci & Explorat, London, ON, Canada. EM cassiestuurman@gmail.com OI Brothers, Thomas/0000-0002-8043-7987 FU NSERC; NSERC/CSA/MDA Industrial Research Chair in Planetary Geology FX SHARAD, MOLA, and CTX data are publicly available on NASA's Planetary Data System (PDS). C.M. Stuurman acknowledges funding from NSERC (USRA and CREATE fellowships). G.R. Osinski acknowledges funding from the NSERC/CSA/MDA Industrial Research Chair in Planetary Geology. We thank the entire SHARAD team for making this analysis possible. We also thank Jeffrey Plaut and Ali Bramson for the constructive feedback and helpful suggestions. Finally, we are grateful to Tanya Harrison for the insightful discussions and enthusiastic support. NR 39 TC 0 Z9 0 U1 10 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD SEP 28 PY 2016 VL 43 IS 18 BP 9484 EP 9491 DI 10.1002/2016GL070138 PG 8 WC Geosciences, Multidisciplinary SC Geology GA DY8PS UT WOS:000385392900017 ER PT J AU Troia, A Pereira, JB Kim, C Taylor, WC AF Troia, Angelo Pereira, Jovani B. Kim, Changkyun Taylor, W. Carl TI The genus Isoetes (Isoetaceae): a provisional checklist of the accepted and unresolved taxa SO PHYTOTAXA LA English DT Article ID QUILLWORT; PTERIDOPHYTES; CONSERVATION; CONSPECTUS; NUCLEAR; COMPLEX; KEY AB Isoetes is a widely distributed lycophyte genus of at least 200 species occurring in diverse habitats. The species can be difficult to identify because Isoetes, with its apparent simplicity of form and conserved morphology, provides few diagnostic features to reliably distinguish its species. The last worldwide monograph, published nearly a century ago, listed 77 taxa. The first step in producing a flora or monograph of all known species of a genus is to compile a list of the acceptable species names. The list presented here is a compilation of 192 accepted names representing taxa from regions around the world: chromosome numbers were assigned to 101 of them, with polyploidy settled on 46.7%. Distribution mapping of the accepted species indicates that South America is the center of diversity for Isoetes and species diversity is the highest in temperate regions. Many of the species on this list are rare and have limited ranges. The list of taxa can be used to initiate floristic studies and conservation efforts in keeping with the target goals of the Global Strategy for Plant Conservation. C1 [Troia, Angelo] Univ Palermo, Dipartimento Sci & Tecnol Biol Chim & Farmaceut S, Sez Bot Ecol Vegetale, Via Archirafi 38, I-90123 Palermo, Italy. [Pereira, Jovani B.] Ruhr Univ Bochum, Dept Evolut & Biodivers Plants, D-44780 Bochum, Germany. [Kim, Changkyun] Gachon Univ, Dept Life Sci, Seongnam 13120, South Korea. [Taylor, W. Carl] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Troia, A (reprint author), Univ Palermo, Dipartimento Sci & Tecnol Biol Chim & Farmaceut S, Sez Bot Ecol Vegetale, Via Archirafi 38, I-90123 Palermo, Italy. EM angelo.troia@unipa.it OI TROIA, Angelo/0000-0001-5193-8865 NR 51 TC 1 Z9 1 U1 3 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD SEP 27 PY 2016 VL 277 IS 2 BP 101 EP 145 DI 10.11646/phytotaxa.277.2.1 PG 45 WC Plant Sciences SC Plant Sciences GA ED5WZ UT WOS:000388925000001 ER PT J AU Kuznetsova, E Rittenhouse, ST Sadeghpour, HR Yelin, SF AF Kuznetsova, Elena Rittenhouse, Seth T. Sadeghpour, H. R. Yelin, Susanne F. TI Rydberg-atom- mediated nondestructive readout of collective rotational states in polar-molecule arrays SO PHYSICAL REVIEW A LA English DT Article ID NUCLEAR-SPIN; ULTRACOLD ATOMS; QUANTUM LOGIC; SPECTROSCOPY; GATES; PHOTOASSOCIATION; ELECTRON; QUBITS; IONS AB We analyze the possibility to exploit charge-dipole interaction between a single polar molecule or a one-dimensional (1D) molecular array and a single Rydberg atom to read out molecular rotational populations. We calculate the energy shift of a single Rb(60s) atom interacting with a single KRb or RbYb molecule in their lowest two rotational states. At atom-molecule distances, relevant to trapping of molecules in optical lattices, the Rydberg electron energy shifts conditioned on the rotational states, are of the order of several MHz. Atom excitation to a Rydberg state and detection of atomic fluorescence conditioned on a rotational state preserves the molecule, making our scheme a nondestructive measurement of the rotational state. Similarly, a 1D array of polar molecules can shift the electron energy of a blockaded Rydberg superatom. We consider a scheme to read out the molecular array collective rotational states using the conditioned Rydberg energy shifts, and numerically analyze a system with three and five KRb or RbYb molecules interacting with Rb(60s) superatom. C1 [Kuznetsova, Elena] Rzhanov Inst Semicond Phys, Novosibirsk 630090, Russia. [Kuznetsova, Elena] Russian Quantum Ctr, 100 Novaya St, Skolkovo 143025, Moscow Region, Russia. [Kuznetsova, Elena] Inst Appl Phys, 46 Ulyanov St, Nizhnii Novgorod 603950, Russia. [Rittenhouse, Seth T.] US Naval Acad, Dept Phys, Annapolis, MD 21402 USA. [Sadeghpour, H. R.; Yelin, Susanne F.] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Yelin, Susanne F.] Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA. [Yelin, Susanne F.] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. RP Kuznetsova, E (reprint author), Rzhanov Inst Semicond Phys, Novosibirsk 630090, Russia.; Kuznetsova, E (reprint author), Russian Quantum Ctr, 100 Novaya St, Skolkovo 143025, Moscow Region, Russia.; Kuznetsova, E (reprint author), Inst Appl Phys, 46 Ulyanov St, Nizhnii Novgorod 603950, Russia. FU Russian Science Foundation [16-12-00028]; Russian Fund for Basic Research [RFBR 14-02-00174]; Institute for Theoretical Atomic and Molecular Physics; NSF [PHY-1516337, PHY-1516421]; Cottrell College Science Award through the Research Corporation for Scientific Advancement FX E.K. was supported by the Russian Science Foundation (Grant No. 16-12-00028) in the part of analysis of rotational states readout via atom-molecule entanglement, and the Russian Fund for Basic Research (Grant No. RFBR 14-02-00174), and would like to thank the Institute for Theoretical Atomic and Molecular Physics for hospitality and financial support during her visit. S.F.Y. would like to thank the NSF for funding. S.T.R. acknowledges support from NSF Grants No. PHY-1516337 and No. PHY-1516421 and from a Cottrell College Science Award through the Research Corporation for Scientific Advancement. NR 69 TC 0 Z9 0 U1 4 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD SEP 27 PY 2016 VL 94 IS 3 AR 032325 DI 10.1103/PhysRevA.94.032325 PG 21 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DX0NP UT WOS:000384060100004 ER PT J AU Ortega-Jimenez, VM Badger, M Wang, H Dudley, R AF Ortega-Jimenez, V. M. Badger, M. Wang, H. Dudley, R. TI Into rude air: hummingbird flight performance in variable aerial environments SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Review DE flight; hummingbird; manoeuvrability; perturbation; rain; unsteady flow ID HOVERING PERFORMANCE; ANNAS HUMMINGBIRDS; BAT FLIGHT; HEAVY RAIN; KINEMATICS; ORIENTATION; MORPHOLOGY; PHYSIOLOGY; ENERGETICS; HELIOX AB Hummingbirds are well known for their ability to sustain hovering flight, but many other remarkable features of manoeuvrability characterize the more than 330 species of trochilid. Most research on hummingbird flight has been focused on either forward flight or hovering in otherwise non perturbed air. In nature, however, hummingbirds fly through and must compensate for substantial environmental perturbation, including heavy rain, unpredictable updraughts and turbulent eddies. Here, we review recent studies on hummingbirds flying within challenging aerial environments, and discuss both the direct and indirect effects of unsteady environmental flows such as rain and von Karman vortex streets. Both perturbation intensity and the spatio-temporal scale of disturbance (expressed with respect to characteristic body size) will influence mechanical responses of volant taxa. Most features of hummingbird manoeuvrability remain undescribed, as do evolutionary patterns of flight-related adaptation within the lineage. Trochilid flight performance under natural conditions far exceeds that of microair vehicles at similar scales, and the group as a whole presents many research opportunities for understanding aerial manoeuvrability. This article is part of the themed issue 'Moving in a moving medium: new perspectives on flight'. C1 [Ortega-Jimenez, V. M.; Badger, M.; Dudley, R.] Univ Calif Berkeley, Integrat Biol, Berkeley, CA 94720 USA. [Wang, H.] Nanjing Univ Aeronaut & Astronaut, Coll Astronaut, Nanjing, Jiangsu, Peoples R China. [Dudley, R.] Smithsonian Trop Res Inst, Balboa, Panama. RP Dudley, R (reprint author), Univ Calif Berkeley, Integrat Biol, Berkeley, CA 94720 USA.; Dudley, R (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM wings@berkeley.edu OI Ortega-Jimenez, Victor Manuel/0000-0003-0024-5086 FU AFOSR Flow Interactions and Control grant [13RSA030] FX Much of the experimental work described here was supported by AFOSR Flow Interactions and Control grant no. 13RSA030 to R.D. NR 54 TC 2 Z9 2 U1 14 U2 14 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 EI 1471-2970 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD SEP 26 PY 2016 VL 371 IS 1704 AR 20150387 DI 10.1098/rstb.2015.0387 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA DV7JJ UT WOS:000383111900006 ER PT J AU Banda-R, K Delgado-Salinas, A Dexter, KG Linares-Palomino, R Oliveira, A Prado, D Pullan, M Quintana, C Riina, R Rodriguez, GM Weintritt, J Acevedo-Rodriguez, P Adarve, J Alvarez, E Aranguren, A Arteaga, JC Aymard, G Castano, A Ceballos-Mago, N Cogollo, A Cuadros, H Delgado, F Devia, W Duenas, H Fajardo, L Fernandez, A Fernandez, MA Franklin, J Freid, EH Galetti, LA Gonto, R Gonzalez-M, R Graveson, R Helmer, EH Idarraga, A Lopez, R Marcano-Vega, H Martinez, OG Maturo, HM McDonald, M McLaren, K Melo, O Mijares, F Mogni, V Molina, D Moreno, ND Nassar, JM Neves, DM Oakley, LJ Oatham, M Olvera-Luna, AR Pezzini, FF Dominguez, OJR Rios, ME Rivera, O Rodriguez, N Rojas, A Sarkinen, T Sanchez, R Smith, M Vargas, C Villanueva, B Pennington, RT AF Banda-R, Karina Delgado-Salinas, Alfonso Dexter, Kyle G. Linares-Palomino, Reynaldo Oliveira-Filho, Ary Prado, Darien Pullan, Martin Quintana, Catalina Riina, Ricarda Rodriguez M, Gina M. Weintritt, Julia Acevedo-Rodriguez, Pedro Adarve, Juan Alvarez, Esteban Aranguren B, Anairamiz Camilo Arteaga, Julian Aymard, Gerardo Castano, Alejandro Ceballos-Mago, Natalia Cogollo, Alvaro Cuadros, Hermes Delgado, Freddy Devia, Wilson Duenas, Hilda Fajardo, Laurie Fernandez, Angel Angel Fernandez, Miller Franklin, Janet Freid, Ethan H. Galetti, Luciano A. Gonto, Reina Gonzalez-M, Roy Graveson, Roger Helmer, Eileen H. Idarraga, Alvaro Lopez, Rene Marcano-Vega, Humfredo Martinez, Olga G. Maturo, Hernan M. McDonald, Morag McLaren, Kurt Melo, Omar Mijares, Francisco Mogni, Virginia Molina, Diego del Pilar Moreno, Natalia Nassar, Jafet M. Neves, Danilo M. Oakley, Luis J. Oatham, Michael Rosa Olvera-Luna, Alma Pezzini, Flavia F. Reyes Dominguez, Orlando Joel Elvira Rios, Maria Rivera, Orlando Rodriguez, Nelly Rojas, Alicia Sarkinen, Tiina Sanchez, Roberto Smith, Melvin Vargas, Carlos Villanueva, Boris Pennington, R. Toby TI Plant diversity patterns in neotropical dry forests and their conservation implications SO SCIENCE LA English DT Article ID SPECIES DISTRIBUTIONS; FLORISTIC DIVERSITY; TROPICAL FORESTS; SOUTH-AMERICA; VEGETATION; DOMINANCE; REGIONS AB Seasonally dry tropical forests are distributed across Latin America and the Caribbean and are highly threatened, with less than 10% of their original extent remaining in many countries. Using 835 inventories covering 4660 species of woody plants, we show marked floristic turnover among inventories and regions, which may be higher than in other neotropical biomes, such as savanna. Such high floristic turnover indicates that numerous conservation areas across many countries will be needed to protect the full diversity of tropical dry forests. Our results provide a scientific framework within which national decision-makers can contextualize the floristic significance of their dry forest at a regional and continental scale. C1 [Banda-R, Karina; Delgado-Salinas, Alfonso; Dexter, Kyle G.; Pullan, Martin; Weintritt, Julia; Neves, Danilo M.; Pezzini, Flavia F.; Sarkinen, Tiina; Pennington, R. Toby] Royal Bot Garden Edinburgh, 20a Inverleith Row, Edinburgh EH3 5LR, Midlothian, Scotland. [Delgado-Salinas, Alfonso; Rosa Olvera-Luna, Alma] Univ Nacl Autonoma Mexico, Dept Bot, Mexico City, DF, Mexico. [Dexter, Kyle G.] Univ Edinburgh, Sch GeoSci, Edinburgh, Midlothian, Scotland. [Linares-Palomino, Reynaldo] Univ Nacl Agr La Molina, Ave La Molina, Lima, Peru. [Oliveira-Filho, Ary] Univ Fed Minas Gerais, ICB, Dept Bot, Ave Antonio Carlos,6627 Pampulha, Belo Horizonte, MG, Brazil. [Prado, Darien; Galetti, Luciano A.; Maturo, Hernan M.; Mogni, Virginia; Oakley, Luis J.] Univ Nacl Rosario, Catedra Bot, IICAR, CONICET,Fac Ciencias Agr, CC 14,S2125ZAA, Zavalla, Argentina. [Quintana, Catalina] Pontificia Univ Catolica Ecuador, Fac Ciencias Exactas, Escuela Biol, Ave 12 Octubre 1076 & Roca, Quito, Ecuador. [Riina, Ricarda] CSIC, RJB, Plaza Murillo 2, E-28014 Madrid, Spain. [Banda-R, Karina; Rodriguez M, Gina M.] Fdn Ecosistemas Secos Colombia, Calle 5 A 70 C-31, Bogota, Colombia. [Linares-Palomino, Reynaldo] Smithsonian Conservat Biol Inst, Los Libertadores 215, Lima, Peru. [Acevedo-Rodriguez, Pedro] Smithsonian Natl Museum Nat Hist, West Loading Dock, 10th & Constitut Ave NW, Washington, DC 20560 USA. [Adarve, Juan] Parque Reg El Vinculo INCIVA, El Vinculo Kilometro 3 Buga Carretera Panamer, Valle Del Cauca, Colombia. [Alvarez, Esteban; Cogollo, Alvaro] Jardin Bot Medellin Joaquin Antonio Uribe, Calle 73 51D-14, Medellin, Colombia. [Aranguren B, Anairamiz] Univ Los Andes, Inst Ciencias Ambient & Ecol, Fac Ciencias, Nucleo Pedro Rincon, 3Er Piso, Merida, Venezuela. [Camilo Arteaga, Julian; Duenas, Hilda] Univ Surcolombiana, Herbario SURCO, Neiva, Colombia. [Aymard, Gerardo] Herbario Univ PORT, UNELLEZ Guanare, Programa Ciencias Agro & Mar, Mesa De Cavacas 3350, Estado Portugue, Venezuela. [Castano, Alejandro] Jardin Bot Juan Maria Cespedes INCIVA, Tulua, Valle Del Cauca, Colombia. [Ceballos-Mago, Natalia] Proyecto Mono Margarita, Isla De Margarita, Estado Nueva Es, Venezuela. [Ceballos-Mago, Natalia] Fdn Vuelta Larga, Isla De Margarita, Estado Nueva Es, Venezuela. [Cuadros, Hermes] Univ Atlantico Kilometro, 7 Via Puerto, Barranquilla, Atlantico, Colombia. [Delgado, Freddy] Ctr Invest Serv Ambientales ECOVIDA, Delegac Terr Minist Ciencia Tecnol & Medio Ambien, Pinar Del Rio, Cuba. [Devia, Wilson] Unidad Cent Valle Cauca UCEVA, Carrera 25 B 44-28, Tulua, Valle Del Cauca, Colombia. [Fajardo, Laurie; Nassar, Jafet M.] Inst Venezolano Invest Cient, Ctr Ecol, Apartado 20632, Caracas 1020A, Venezuela. [Fernandez, Angel; Gonto, Reina] Inst Venezolano Invest Cient, Ctr Biofis & Bioquim Herbarium, Apartado 20632, Caracas 1020A, Venezuela. [Franklin, Janet] Arizona State Univ, Sch Geog Sci & Urban Planning, POB 875302, Tempe, AZ 85287 USA. [Freid, Ethan H.] Bahamas Natl Trust, Leon Levy Nat Plant Preserve, Eleuthera, Bahamas. [Gonzalez-M, Roy] Inst Invest Recursos Biol Alexander von Humboldt, Ave Paseo Bolivar 16-20, Bogota, DC, Colombia. [Helmer, Eileen H.; Marcano-Vega, Humfredo] Jardin Bot Sur, Int Inst Trop Forestry, Southern Res Stn, Forest Serv, 1201 Calle Ceiba, San Juan, PR 00926 USA. [Idarraga, Alvaro; Molina, Diego] Univ Antioquia, Grp Estudios Bot, Medellin 1226, Colombia. [Lopez, Rene] Univ Distrital Francisco Jose de Caldas, Carrera 5 Este 15-82, Bogota, Colombia. [Martinez, Olga G.] Univ Nacl Salta, Fac Ciencias Nat, Ave Bolivia 5150, RA-4400 Salta, Argentina. [McDonald, Morag] Bangor Univ, Sch Environm Nat Resources & Geog, Thoday Bldg,Room G21, Bangor LL57 2DG, Gwynedd, Wales. [McLaren, Kurt] Univ West Indies, Dept Life Sci, Mona, Jamaica. [Melo, Omar; Villanueva, Boris] Univ Tolima, Codigo Postal 730006299, Ibague, Tolima, Colombia. [Mijares, Francisco; Oatham, Michael] Fdn Orinoquia Biodiversa, Calle 15 12-15, Tame, Arauca, Colombia. [del Pilar Moreno, Natalia; Rivera, Orlando] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. Univ West Indies St Augustine, Dept Life Sci, Nat Sci Bldg,Old Wing,Room 222, Augustine, Trinid & Tobago. [Elvira Rios, Maria; Sanchez, Roberto] Univ Pamplona, Pamplona, Norte De Santan, Colombia. [Rodriguez, Nelly] Univ Nacl Colombia, Dept Biol, Codigo Postal 111321,Ave Carrera 30 45-03, Bogota, Colombia. [Rojas, Alicia] Jardin Bot Eloy Valenzuela, Ave Bucarica, Santander, Colombia. [Vargas, Carlos] Jardin BOt Eggota Jose Celestino Mutis, Ave Calle 63, Bogota, Colombia. [Gonzalez-M, Roy; Vargas, Carlos] Univ Rosario, Fac Ciencias Nat & Matemat, Carrera 26 63B-48, Bogota, Colombia. [Neves, Danilo M.] Kew, Royal Bot Gardens, Richmond, Surrey, England. RP Pennington, RT (reprint author), Royal Bot Garden Edinburgh, 20a Inverleith Row, Edinburgh EH3 5LR, Midlothian, Scotland. EM t.pennington@rbge.ac.uk OI Riina, Ricarda/0000-0002-7423-899X; Rodriguez Eraso, Nelly/0000-0001-7616-2493; Linares-Palomino, Reynaldo/0000-0002-7631-5549; Smith, M Alex/0000-0002-8650-2575 FU Royal Botanic Garden Edinburgh by a Leverhulme Trust International Network Grant [IN-074]; U.K. Natural Environment Research Council [NE/I028122/1]; Colciencias Ph.D. scholarship [529]; Synthesys Programme [GBTAF-2824]; NSF [NSF 1118340, 1118369]; Instituto Humboldt (IAvH)-Red colombiana de investigacion y monitoreo en bosque seco; Inter-American Institute for Global Change Research (IAI) [CRN2-021]; NSF GEO [0452325]; Universidad Nacional de Rosario (UNR); Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) FX This paper is the result of the Latin American and Caribbean Seasonally Dry Tropical Forest Floristic Network (DRYFLOR), which has been supported at the Royal Botanic Garden Edinburgh by a Leverhulme Trust International Network Grant (IN-074). This work was also supported by the U.K. Natural Environment Research Council grant NE/I028122/1; Colciencias Ph.D. scholarship 529; Synthesys Programme GBTAF-2824; the NSF (NSF 1118340 and 1118369); the Instituto Humboldt (IAvH)-Red colombiana de investigacion y monitoreo en bosque seco; the Inter-American Institute for Global Change Research (IAI; Tropi-Dry, CRN2-021, funded by NSF GEO 0452325); Universidad Nacional de Rosario (UNR); and Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET). The data reported in this paper are available at www.dryflor.info. R.T.P. conceived the study. M.P., A.O.-F., K.B.-R., R.T.P., and J.W. designed the DRYFLOR database system. K.B.-R. and K.G.D. carried out most analyses. K.B.-R. R.T.P., and K.G.D. wrote the manuscript with substantial input from A.D.-S., R.L.-P., A.O.-F., D.P., C.Q., and R.R. All the authors contributed data, discussed further analyses, and commented on various versions of the manuscript. K.B.-R. thanks G. Galeano who introduced her to dry forest research. We thank J.L. Marcelo, I. Huamantupa, C. Reynel, S. Palacios, and A. Daza for help with fieldwork and data entry in Peru. NR 34 TC 2 Z9 2 U1 52 U2 52 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 23 PY 2016 VL 353 IS 6306 BP 1383 EP 1387 DI 10.1126/science.aaf5080 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DW5TB UT WOS:000383708700032 ER PT J AU Hudson, CM McCurry, MR Lundgren, P McHenry, CR Shine, R AF Hudson, C. M. McCurry, M. R. Lundgren, P. McHenry, C. R. Shine, R. TI Constructing an Invasion Machine: The Rapid Evolution of a Dispersal-Enhancing Phenotype During the Cane Toad Invasion of Australia SO PLOS ONE LA English DT Article ID CHAUNUS BUFO MARINUS; TROPICAL AUSTRALIA; ANURAN LOCOMOTION; RHINELLA-MARINA; FRONT; FROGS; HISTORY; PERFORMANCE; PHYLOGENY; BUFONIDAE AB Biological invasions can induce rapid evolutionary change. As cane toads (Rhinella marina) have spread across tropical Australia over an 80-year period, their rate of invasion has increased from around 15 to 60 km per annum. Toads at the invasion front disperse much faster and further than conspecifics from range-core areas, and their offspring inherit that rapid dispersal rate. We investigated morphological changes that have accompanied this dramatic acceleration, by conducting three-dimensional morphometric analyses of toads from both range-core and invasion-front populations. Morphology of heads, limbs, pectoral girdles and pelvic girdles differed significantly between toads from the two areas, ranging from 0.5% to 16.5% difference in mean bone dimensions between populations, with invasion-front toads exhibiting wider forelimbs, narrower hindlimbs and more compact skulls. Those changes plausibly reflect an increased reliance on bounding (multiple short hops in quick succession) rather than separate large leaps. Within an 80-year period, invasive cane toads have converted the basic anuran body plan - which evolved for occasional large leaps to evade predators - into a morphotype better-suited to sustained long-distance travel. C1 [Hudson, C. M.; Shine, R.] Univ Sydney, Sch Life & Environm Sci A08, Sydney, NSW 2006, Australia. [McCurry, M. R.; Lundgren, P.; McHenry, C. R.] Monash Univ, Anat & Dev Biol, Clayton, Vic 3800, Australia. [McCurry, M. R.] Museum Victoria, Geosci, Carlton, Vic 3001, Australia. [McCurry, M. R.] Smithsonian Inst, Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Hudson, CM (reprint author), Univ Sydney, Sch Life & Environm Sci A08, Sydney, NSW 2006, Australia. EM cameron.hudson@sydney.edu.au FU Australian Research Council [FF0561365] FX This research was funded by the Australian Research Council (Grant #FF0561365). NR 49 TC 1 Z9 1 U1 21 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 22 PY 2016 VL 11 IS 9 AR e0156950 DI 10.1371/journal.pone.0156950 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DW8GO UT WOS:000383893200001 PM 27658247 ER PT J AU Patton, DR Qamar, FD Ellison, SL Bluck, AFL Simard, L Mendel, JT Moreno, J Torrey, P AF Patton, David R. Qamar, Farid D. Ellison, Sara L. Bluck, Asa F. L. Simard, Luc Mendel, J. Trevor Moreno, Jorge Torrey, Paul TI Galaxy pairs in the Sloan Digital Sky Survey - XI. A new method for measuring the influence of the closest companion out to wide separations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: statistics; galaxies: structure ID MASS-METALLICITY RELATION; TRIGGERED STAR-FORMATION; ACTIVE GALACTIC NUCLEI; DWARF-DWARF INTERACTIONS; CNOC2 REDSHIFT SURVEY; MERGER RATE EVOLUTION; STELLAR MASS; INTERACTING GALAXIES; FORMING GALAXIES; FIELD GALAXIES AB We describe a statistical approach for measuring the influence that a galaxy's closest companion has on the galaxy's properties out to arbitrarily wide separations. We begin by identifying the closest companion for every galaxy in a large spectroscopic sample of Sloan Digital Sky Survey galaxies. We then characterize the local environment of each galaxy by using the number of galaxies within 2 Mpc and by determining the isolation of the galaxy pair from other neighbouring galaxies. We introduce a sophisticated algorithm for creating a statistical control sample for each galaxy, matching on stellar mass, redshift, local density and isolation. Unlike traditional studies of close galaxy pairs, this approach is effective in a wide range of environments, regardless of how faraway the closest companion is (although a very distant closest companion is unlikely to have a measurable influence on the galaxy in question). We apply this methodology to measurements of galaxy asymmetry, and find that the presence of nearby companions drives a clear enhancement in galaxy asymmetries. The asymmetry excess peaks at the smallest projected separations (<10 kpc), where the mean asymmetry is enhanced by a factor of 2.0 +/- 0.2. Enhancements in mean asymmetry decline as pair separation increases, but remain statistically significant (1 sigma-2 sigma) out to projected separations of at least 50 kpc. C1 [Patton, David R.; Qamar, Farid D.] Trent Univ, Dept Phys & Astron, 1600 West Bank Dr, Peterborough, ON K9L 0G2, Canada. [Qamar, Farid D.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Ellison, Sara L.; Bluck, Asa F. L.; Mendel, J. Trevor] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Bluck, Asa F. L.] Swiss Fed Inst Technol, Inst Astron, 27 Wolfgang Pauli Str, CH-8093 Zurich, Switzerland. [Simard, Luc] Natl Res Council Canada, 5071 West Saanich Rd, Victoria, BC V9E 2E7, Canada. [Mendel, J. Trevor] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Moreno, Jorge] Calif State Polytech Univ Pomona, Dept Phys & Astron, Pomona, CA 91768 USA. [Moreno, Jorge] CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA. [Moreno, Jorge; Torrey, Paul] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RP Patton, DR (reprint author), Trent Univ, Dept Phys & Astron, 1600 West Bank Dr, Peterborough, ON K9L 0G2, Canada. EM dpatton@trentu.ca FU NSERC; NASA ATP [NNX14AH35G]; NSF [AST-1516364] FX DRP and SLE gratefully acknowledge the receipt of NSERC Discovery Grants which helped to fund this research. PT acknowledges support from NASA ATP Grant NNX14AH35G. JM is supported by NSF grant AST-1516364. NR 101 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2016 VL 461 IS 3 BP 2589 EP 2604 DI 10.1093/mnras/stw1494 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW2OG UT WOS:000383481100024 ER PT J AU Morabito, LK Deller, AT Rottgering, H Miley, G Varenius, E Shimwell, TW Moldon, J Jackson, N Morganti, R van Weeren, RJ Oonk, JBR AF Morabito, Leah K. Deller, Adam T. Rottgering, Huub Miley, George Varenius, Eskil Shimwell, Timothy W. Moldon, Javier Jackson, Neal Morganti, Raffaella van Weeren, Reinout J. Oonk, J. B. R. TI LOFAR VLBI studies at 55 MHz of 4C 43.15, a z=2.4 radio galaxy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: 4C 43.15; galaxies: jets; radio continuum: galaxies ID FLUX DENSITIES; SPECTRAL INDEX; GHZ SOURCES; SKY SURVEY; REDSHIFT; CALIBRATION; CATALOG; SCINTILLATION; EVOLUTION; QUASARS AB The correlation between radio spectral index and redshift has been exploited to discover high-redshift radio galaxies, but its underlying cause is unclear. It is crucial to characterize the particle acceleration and loss mechanisms in high-redshift radio galaxies to understand why their radio spectral indices are steeper than their local counterparts. Low-frequency information on scales of similar to 1 arcsec are necessary to determine the internal spectral index variation. In this paper we present the first spatially resolved studies at frequencies below 100 MHz of the z = 2.4 radio galaxy 4C 43.15 which was selected based on its ultrasteep spectral index (alpha < -1; S-v similar to v(alpha)) between 365 MHz and 1.4 GHz. Using the International Low Frequency Array Low Band Antenna we achieve subarcsecond imaging resolution at 55MHz with very long baseline interferometry techniques. Our study reveals low-frequency radio emission extended along the jet axis, which connects the two lobes. The integrated spectral index for frequencies <500 MHz is -0.83. The lobes have integrated spectral indices of -1.31 +/- 0.03 and -1.75 +/- 0.01 for frequencies = 1.4 GHz, implying a break frequency between 500 MHz and 1.4 GHz. These spectral properties are similar to those of local radio galaxies. We conclude that the initially measured ultrasteep spectral index is due to a combination of the steepening spectrum at high frequencies with a break at intermediate frequencies. C1 [Morabito, Leah K.; Rottgering, Huub; Miley, George; Shimwell, Timothy W.; Oonk, J. B. R.] Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. [Deller, Adam T.; Morganti, Raffaella; Oonk, J. B. R.] Netherlands Inst Radio Astron ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands. [Varenius, Eskil; Jackson, Neal] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Moldon, Javier] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England. [Morganti, Raffaella] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [van Weeren, Reinout J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Morabito, LK (reprint author), Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM morabito@strw.leidenuniv.nl OI Varenius, Eskil/0000-0002-3248-9467; Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660 FU NWO Top LOFAR project [614.001.006]; ERC Advanced Investigator programme NewClusters [321271]; European Research Council under the European Union's Seventh Framework Programme (FP)/ERC Advanced Grant [RADIOLIFE-320745]; National Science Foundation [ACI-1440620]; National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project [NCC5-626] FX LKM acknowledges financial support from NWO Top LOFAR project, project no. 614.001.006. LKM and HR acknowledge support from the ERC Advanced Investigator programme NewClusters 321271. The authors would like to thank J. Harwood and H. Intema for many useful discussions. RM gratefully acknowledge support from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant RADIOLIFE-320745. This paper is based (in part) on data obtained with the International LOFAR Telescope (ILT). LOFAR (van Haarlem et al. 2013) is the Low Frequency Array designed and constructed by ASTRON. It has facilities in several countries, that are owned by various parties (each with their own funding sources), and that are collectively operated by the ILT foundation under a joint scientific policy. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research made use of Montage. It is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. NR 57 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2016 VL 461 IS 3 BP 2676 EP 2687 DI 10.1093/mnras/stw1501 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW2OG UT WOS:000383481100030 ER PT J AU Bernardi, G Zwart, JTL Price, D Greenhill, LJ Mesinger, A Dowell, J Eftekhari, T Ellingson, SW Kocz, J Schinzel, F AF Bernardi, G. Zwart, J. T. L. Price, D. Greenhill, L. J. Mesinger, A. Dowell, J. Eftekhari, T. Ellingson, S. W. Kocz, J. Schinzel, F. TI Bayesian constraints on the global 21-cm signal from the Cosmic Dawn SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: statistical; cosmology: observations; dark ages, reionization, first stars; diffuse radiation ID CM POWER SPECTRUM; SIMILAR-TO 20; MURCHISON-WIDEFIELD-ARRAY; INTERGALACTIC MEDIUM; MODEL SELECTION; DARK-MATTER; PAPER-64 CONSTRAINTS; PARAMETER-ESTIMATION; RADIATIVE FEEDBACK; GALAXY FORMATION AB The birth of the first luminous sources and the ensuing epoch of reionization are best studied via the redshifted 21-cm emission line, the signature of the first two imprinting the last. In this work, we present a fully Bayesian method, HIBAYES, for extracting the faint, global (sky-averaged) 21-cm signal from the much brighter foreground emission. We show that a simplified (but plausible) Gaussian model of the 21-cm emission from the Cosmic Dawn epoch (15 less than or similar to z less than or similar to 30), parametrized by an amplitude A(HI), a frequency peak nu(HI) and a width sigma(HI), can be extracted even in the presence of a structured foreground frequency spectrum (parametrized as a seventh-order polynomial), provided sufficient signal-to-noise (400 h of observation with a single dipole). We apply our method to an early, 19-min-long observation from the Large aperture Experiment to detect the Dark Ages, constraining the 21-cm signal amplitude and width to be -890 < A(HI) < 0 mK and sigma(HI) > 6.5 MHz (corresponding to Delta z > 1.9 at redshift z similar or equal to 20) respectively at the 95-per cent confidence level in the range 13.2 < z < 27.4 (100 > nu > 50 MHz). C1 [Bernardi, G.] SKA South Africa, 3rd Floor,Pk Rd, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Price, D.; Greenhill, L. J.; Eftekhari, T.] Harvard Smithsonian Ctr Astrophys, Garden St 60, Cambridge, MA 02138 USA. [Zwart, J. T. L.] Univ Western Cape, Dept Phys & Astron, Private Bag X17, ZA-7535 Bellville, Cape Town, South Africa. [Zwart, J. T. L.] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr, Private Bag X3, ZA-7701 Rondebosch, South Africa. [Mesinger, A.] Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy. [Dowell, J.; Schinzel, F.] Univ New Mexico, Dept Phys & Astron, Albuquerque, NM 87131 USA. [Ellingson, S. W.] Virginia Tech, Bradley Dept Elect & Comp Engn, Blacksburg, VA 24061 USA. [Kocz, J.] Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91104 USA. RP Bernardi, G (reprint author), SKA South Africa, 3rd Floor,Pk Rd, ZA-7405 Pinelands, South Africa.; Bernardi, G (reprint author), Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa.; Bernardi, G (reprint author), Harvard Smithsonian Ctr Astrophys, Garden St 60, Cambridge, MA 02138 USA. EM giannibernardi75@gmail.com OI Zwart, Jonathan/0000-0002-4967-946X; Eftekhari, Tarraneh/0000-0003-0307-9984 FU NSF [AST/1106059, PHY/0835713]; South Africa National Research Foundation; Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence 'Origin and Structure of the Universe'; Ministry of Foreign Affairs and International Cooperation, Directorate General for the Country Promotion [ZA14GR02] FX We thank an anonymous referee for helpful comments that considerably improved the manuscript. GB thanks Judd Bowman, Andrea Ferrara, Adrian Liu and Aaron Ewall-Wice for useful inputs and comments on this work and Jordan Mirocha for help with ARES. The LEDA experiment is supported by NSF grants AST/1106059 and PHY/0835713. JZ gratefully acknowledges a South Africa National Research Foundation Square Kilometre Array Research Fellowship. This research was supported by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence 'Origin and Structure of the Universe'. With the support of the Ministry of Foreign Affairs and International Cooperation, Directorate General for the Country Promotion (Bilateral Grant Agreement ZA14GR02 - Mapping the Universe on the Pathway to SKA). NR 73 TC 4 Z9 4 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2016 VL 461 IS 3 BP 2847 EP 2855 DI 10.1093/mnras/stw1499 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW2OG UT WOS:000383481100041 ER PT J AU Soergel, B Flender, S Story, KT Bleem, L Giannantonio, T Efstathiou, G Rykoff, E Benson, BA Crawford, T Dodelson, S Habib, S Heitmann, K Holder, G Jain, B Rozo, E Saro, A Weller, J Abdalla, FB Allam, S Annis, J Armstrong, R Benoit-Levy, A Bernstein, GM Carlstrom, JE Rosell, AC Kind, MC Castander, FJ Chiu, I Chown, R Crocce, M Cunha, CE D'Andrea, CB da Costa, LN de Haan, T Desai, S Diehl, HT Dietrich, JP Doel, P Estrada, J Evrard, AE Flaugher, B Fosalba, P Frieman, J Gaztanaga, E Gruen, D Gruendl, RA Holzapfel, WL Honscheid, K James, DJ Keisler, R Kuehn, K Kuropatkin, N Lahav, O Lima, M Marshall, JL McDonald, M Melchior, P Miller, CJ Miquel, R Nord, B Ogando, R Omori, Y Plazas, AA Rapetti, D Reichardt, CL Romer, AK Roodman, A Saliwanchik, BR Sanchez, E Schubnell, M Sevilla-Noarbe, I Sheldon, E Smith, RC Soares-Santos, M Sobreira, F Stark, A Suchyta, E Swanson, MEC Tarle, G Thomas, D Vieira, JD Walker, AR Whitehorn, N AF Soergel, B. Flender, S. Story, K. T. Bleem, L. Giannantonio, T. Efstathiou, G. Rykoff, E. Benson, B. A. Crawford, T. Dodelson, S. Habib, S. Heitmann, K. Holder, G. Jain, B. Rozo, E. Saro, A. Weller, J. Abdalla, F. B. Allam, S. Annis, J. Armstrong, R. Benoit-Levy, A. Bernstein, G. M. Carlstrom, J. E. Carnero Rosell, A. Kind, M. Carrasco Castander, F. J. Chiu, I. Chown, R. Crocce, M. Cunha, C. E. D'Andrea, C. B. da Costa, L. N. de Haan, T. Desai, S. Diehl, H. T. Dietrich, J. P. Doel, P. Estrada, J. Evrard, A. E. Flaugher, B. Fosalba, P. Frieman, J. Gaztanaga, E. Gruen, D. Gruendl, R. A. Holzapfel, W. L. Honscheid, K. James, D. J. Keisler, R. Kuehn, K. Kuropatkin, N. Lahav, O. Lima, M. Marshall, J. L. McDonald, M. Melchior, P. Miller, C. J. Miquel, R. Nord, B. Ogando, R. Omori, Y. Plazas, A. A. Rapetti, D. Reichardt, C. L. Romer, A. K. Roodman, A. Saliwanchik, B. R. Sanchez, E. Schubnell, M. Sevilla-Noarbe, I. Sheldon, E. Smith, R. C. Soares-Santos, M. Sobreira, F. Stark, A. Suchyta, E. Swanson, M. E. C. Tarle, G. Thomas, D. Vieira, J. D. Walker, A. R. Whitehorn, N. CA DES Collaboration SPT Collaboration TI Detection of the kinematic Sunyaev-Zel'dovich effect with DES Year 1 and SPT SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; cosmic background radiation; large-scale structure of Universe ID SOUTH-POLE TELESCOPE; MICROWAVE BACKGROUND ANISOTROPIES; RELAXED GALAXY CLUSTERS; LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; DARK-MATTER HALOS; SZ SURVEY; X-RAY; PECULIAR VELOCITIES; COSMOLOGICAL CONSTRAINTS AB We detect the kinematic Sunyaev-Zel'dovich (kSZ) effect with a statistical significance of 4.2 sigma by combining a cluster catalogue derived from the first year data of the Dark Energy Survey with cosmic microwave background temperature maps from the South Pole Telescope Sunyaev-Zel'dovich Survey. This measurement is performed with a differential statistic that isolates the pairwise kSZ signal, providing the first detection of the large-scale, pairwise motion of clusters using redshifts derived from photometric data. By fitting the pairwise kSZ signal to a theoretical template, we measure the average central optical depth of the cluster sample, (tau) over bar (e) = (3.75 +/- 0.89) x 10(-3). We compare the extracted signal to realistic simulations and find good agreement with respect to the signal to noise, the constraint on (tau) over bar (e), and the corresponding gas fraction. High-precision measurements of the pairwise kSZ signal with future data will be able to place constraints on the baryonic physics of galaxy clusters, and could be used to probe gravity on scales greater than or similar to 100 Mpc. C1 [Soergel, B.; Giannantonio, T.; Efstathiou, G.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Soergel, B.; Giannantonio, T.; Efstathiou, G.] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. [Flender, S.; Bleem, L.; Habib, S.; Heitmann, K.; Carlstrom, J. E.] Argonne Natl Lab, HEP Div, 9700 S Cass Ave, Lemont, IL 60439 USA. [Flender, S.; Bleem, L.; Benson, B. A.; Crawford, T.; Dodelson, S.; Habib, S.; Heitmann, K.; Carlstrom, J. E.; Frieman, J.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Story, K. T.; Rykoff, E.; Cunha, C. E.; Gruen, D.; Roodman, A.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA. [Story, K. T.; Keisler, R.] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. [Giannantonio, T.] Univ Cambridge, Ctr Theoret Cosmol, DAMTP, Wilberforce Rd, Cambridge CB3 0WA, England. [Rykoff, E.; Gruen, D.; Roodman, A.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Benson, B. A.; Dodelson, S.; Allam, S.; Annis, J.; Diehl, H. T.; Estrada, J.; Flaugher, B.; Frieman, J.; Kuropatkin, N.; Nord, B.; Soares-Santos, M.] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA. [Benson, B. A.; Crawford, T.; Dodelson, S.; Carlstrom, J. E.] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Habib, S.; Heitmann, K.] Argonne Natl Lab, MCS Div, 9700 S Cass Ave, Lemont, IL 60439 USA. [Holder, G.; Chown, R.; Omori, Y.] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. [Jain, B.; Bernstein, G. M.; Suchyta, E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Rozo, E.] Univ Arizona, Dept Phys, 1118 E 4th St, Tucson, AZ 85721 USA. [Saro, A.; Chiu, I.; Desai, S.; Dietrich, J. P.; Rapetti, D.] Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany. [Saro, A.; Weller, J.; Chiu, I.; Desai, S.; Dietrich, J. P.; Rapetti, D.] Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. [Weller, J.] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. [Weller, J.] Univ Munich, Fak Phys, Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany. [Abdalla, F. B.; Benoit-Levy, A.; Doel, P.; Lahav, O.] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. [Abdalla, F. B.] Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa. [Armstrong, R.; Melchior, P.] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA. [Benoit-Levy, A.] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France. [Benoit-Levy, A.] Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Carlstrom, J. E.] Univ Chicago, Dept Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. [Carnero Rosell, A.; da Costa, L. N.; Lima, M.; Ogando, R.; Sobreira, F.] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Carnero Rosell, A.; da Costa, L. N.; Ogando, R.] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil. [Kind, M. Carrasco; Gruendl, R. A.; Sevilla-Noarbe, I.; Vieira, J. D.] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Kind, M. Carrasco; Gruendl, R. A.; Swanson, M. E. C.] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA. [Castander, F. J.; Crocce, M.; Fosalba, P.; Gaztanaga, E.] CSIC, IEEC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain. [D'Andrea, C. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [D'Andrea, C. B.; Thomas, D.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [de Haan, T.; Holzapfel, W. L.; Whitehorn, N.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Evrard, A. E.; Miller, C. J.; Schubnell, M.; Tarle, G.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Evrard, A. E.; Miller, C. J.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA. [Honscheid, K.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [James, D. J.; Smith, R. C.; Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile. [Kuehn, K.] Australian Astron Observ, N Ryde, NSW 2113, Australia. [Lima, M.] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil. [Marshall, J. L.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Marshall, J. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. [Miquel, R.] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Miquel, R.] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Barcelona, Spain. [Plazas, A. A.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Romer, A. K.] Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England. [Saliwanchik, B. R.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Private Bag X54001, ZA-4000 Durban, South Africa. [Sanchez, E.; Sevilla-Noarbe, I.] Ctr Invest Energet Medioambientales & Tecnol CIEM, Complutense 40, Madrid 28040, Spain. [Sheldon, E.] Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA. [Stark, A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. RP Soergel, B (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England.; Soergel, B (reprint author), Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England. EM bsoergel@ast.cam.ac.uk RI Lima, Marcos/E-8378-2010; Ogando, Ricardo/A-1747-2010; Gaztanaga, Enrique/L-4894-2014; OI Ogando, Ricardo/0000-0003-2120-1154; Gaztanaga, Enrique/0000-0001-9632-0815; Weller, Jochen/0000-0002-8282-2010; Abdalla, Filipe/0000-0003-2063-4345; Sobreira, Flavia/0000-0002-7822-0658; Stark, Antony/0000-0002-2718-9996 FU Isaac Newton Studentship at the University of Cambridge; Science and Technologies Facilities Council (STFC); Kavli Foundation; STFC [ST/L000636/1]; Australian Research Council [DP150103208]; US Department of Energy; US National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministerio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; National Science Foundation [AST-1138766, PLR-1248097]; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zurich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen; associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Pennsylvania; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; MINECO [AYA2012-39559, ESP2013-48274, FPA2013-47986]; Centro de Excelencia Severo Ochoa [SEV-2012-0234]; European Research Council under the European Union including ERC [240672, 291329, 306478]; NSF Physics Frontier Center [PHY-0114422]; Gordon and Betty Moore Foundation [947]; US Department of Energy [DE-AC02-06CH11357]; DOE/SC [DE-AC02-06CH11357] FX BS thanks Anthony Challinor, Jens Chluba, Suet-Ying Mak, Emmanuel Schaan, and Fabian Schmidt for helpful discussions. BS further acknowledges support from an Isaac Newton Studentship at the University of Cambridge and from the Science and Technologies Facilities Council (STFC). KTS acknowledges support from the Kavli Foundation. TG further thanks David Bacon for useful discussion, and acknowledges support from the Kavli Foundation and STFC grant ST/L000636/1. CR acknowledges support from the Australian Research Council's Discovery Projects scheme (DP150103208).; Funding for the DES Projects has been provided by the US Department of Energy, the US National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under Grant Number AST-1138766.; The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC), the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, and Texas A&M University.; The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2012-39559, ESP2013-48274, FPA2013-47986, and Centro de Excelencia Severo Ochoa SEV-2012-0234. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478.; The South Pole Telescope programme is supported by the National Science Foundation through grant PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant GBMF#947 to the University of Chicago.; Argonne National Laboratory's work was supported under the US Department of Energy contract DE-AC02-06CH11357. This research used resources of the ALCF, which is supported by DOE/SC under contract DE-AC02-06CH11357. NR 102 TC 6 Z9 6 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2016 VL 461 IS 3 BP 3172 EP 3193 DI 10.1093/mnras/stw1455 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DW2OG UT WOS:000383481100065 ER PT J AU Chael, AA Johnson, MD Narayan, R Doeleman, SS Wardle, JFC Bouman, KL AF Chael, Andrew A. Johnson, Michael D. Narayan, Ramesh Doeleman, Sheperd S. Wardle, John F. C. Bouman, Katherine L. TI HIGH-RESOLUTION LINEAR POLARIMETRIC IMAGING FOR THE EVENT HORIZON TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; Galaxy: center; techniques: high angular resolution; techniques: image processing; techniques: interferometric ID MAXIMUM-ENTROPY METHOD; SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEI; BOUND-CONSTRAINED OPTIMIZATION; MAGNETIC-FIELDS; 86 GHZ; VLBI OBSERVATIONS; ACCRETION DISKS; A-ASTERISK; JET BASE AB Images of the linear polarizations of synchrotron radiation around active galactic nuclei (AGNs) highlight their projected magnetic field lines and provide key data for understanding the physics of accretion and outflow from supermassive black holes. The highest-resolution polarimetric images of AGNs are produced with Very Long Baseline Interferometry (VLBI). Because VLBI incompletely samples the Fourier transform of the source image, any image reconstruction that fills in unmeasured spatial frequencies will not be unique and reconstruction algorithms are required. In this paper, we explore some extensions of the Maximum Entropy Method (MEM) to linear polarimetric VLBI imaging. In contrast to previous work, our polarimetric MEM algorithm combines a Stokes I imager that only uses bispectrum measurements that are immune to atmospheric phase corruption, with a joint Stokes Q and U imager that operates on robust polarimetric ratios. We demonstrate the effectiveness of our technique on 7 and 3 mm wavelength quasar observations from the VLBA and simulated 1.3 mm Event Horizon Telescope observations of Sgr A* and M87. Consistent with past studies, we find that polarimetric MEM can produce superior resolution compared to the standard CLEAN algorithm, when imaging smooth and compact source distributions. As an imaging framework, MEM is highly adaptable, allowing a range of constraints on polarization structure. Polarimetric MEM is thus an attractive choice for image reconstruction with the EHT. C1 [Chael, Andrew A.; Johnson, Michael D.; Narayan, Ramesh; Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Doeleman, Sheperd S.] MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. [Wardle, John F. C.] Brandeis Univ, Dept Phys, Waltham, MA 02454 USA. [Bouman, Katherine L.] MIT, Comp Sci & Artificial Intelligence Lab, 32 Vassar St, Cambridge, MA 02139 USA. RP Chael, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM achael@cfa.harvard.edu FU National Science Foundation [AST-1310896, AST-1312034, AST-1211539, AST-1440254]; Gordon and Betty Moore Foundation [GBMF-3561]; NSF [AST1312651, CGV-1111415]; NASA [TCAN NNX14AB47G]; NSF Graduate Fellowship; NASA through the Fermi Guest Investigator Program FX We thank the National Science Foundation (AST-1310896, AST-1312034, AST-1211539, and AST-1440254) and the Gordon and Betty Moore Foundation (#GBMF-3561) for financial support of this work. R.N.'s research was supported in part by NSF grant AST1312651 and NASA grant TCAN NNX14AB47G. K.B. was supported by NSF CGV-1111415 and a NSF Graduate Fellowship. We thank Svetlana Jorstad, Alan Marscher, and Kazuhiro Hada for providing the data imaged in Section 5.2 and for their helpful comments. We thank Avery Broderick, Jason Dexter, and Roman Gold for generously providing model images. We also thank Lindy Blackburn for his help on simulating gain and phase errors and Kazunori Akiyama for his suggestion of applying total variation as a polarimetric regularizer. We thank the anonymous referee, whose thorough suggestions significantly improved this paper. This study makes use of 43 GHz VLBA data from the VLBA-BU Blazar Monitoring Program (VLBABU-BLAZAR; http://www.bu.edu/blazars/VLBAproject. html), funded by NASA through the Fermi Guest Investigator Program. The VLBA is an instrument of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation that is operated by Associated Universities, Inc. NR 54 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2016 VL 829 IS 1 AR 11 DI 10.3847/0004-637X/829/1/11 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8IY UT WOS:000385374500011 ER PT J AU Maksym, WP Fabbiano, G Elvis, M Karovska, M Paggi, A Raymond, J Wang, JF Storchi-Bergmann, T AF Maksym, W. Peter Fabbiano, Giuseppina Elvis, Martin Karovska, Margarita Paggi, Alessandro Raymond, John Wang, Junfeng Storchi-Bergmann, Thaisa TI MAPPING SEYFERT AND LINER EXCITATION MODES IN THE INNER KPC OF NGC 3393 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 3393); galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; DEEP CHANDRA ACIS; X-RAY; HOST GALAXIES; REGION; KINEMATICS; EMISSION; FEEDBACK; CLASSIFICATION; UNIVERSE AB We mapped the extended narrowline region (ENLR) of NGC 3393 on scales of r less than or similar to 4 '' (similar to 1 kpc) from the nucleus using emission line images of H alpha lambda 6563, [O III] lambda 5007, and [S II] lambda lambda 6717, 6731, taken with the Hubble Space Telescope as part of the CHandra survey of Extended Emission line Regions in nearby Seyfert galaxies (CHEERS). By mapping these lines onto a spatially resolved Baldwin-Phillips-Terlevich diagram, we investigate the impact of feedback from a Compton-thick active galactic nucleus on its circumnuclear ISM. We find that the expected Seyfert-like emission within the ionization bicone (less than or similar to 3 ''; 770 pc). We also find a new, figure-8-shaped low ionization emission line region (LINER) cocoon enveloping the bicone and defining a sharp (less than or similar to 100 pc) transition between higher and lower-ionization zones. These data illustrate the morphological dependence of ionization states of the ENLR relative to bicone and host gas geometries. C1 [Maksym, W. Peter; Fabbiano, Giuseppina; Elvis, Martin; Karovska, Margarita; Paggi, Alessandro; Raymond, John] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Wang, Junfeng] Xiamen Univ, Dept Astron, Phys Bldg, Xiamen 361005, Fujian, Peoples R China. [Storchi-Bergmann, Thaisa] Univ Fed Rio Grande do Sul, Dept Astron, IF, CP 15051, BR-91501970 Porto Alegre, RS, Brazil. RP Maksym, WP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM walter.maksym@cfa.harvard.edu RI Paggi, Alessandro/C-1219-2017; OI Paggi, Alessandro/0000-0002-5646-2410; Fabbiano, Giuseppina/0000-0002-3554-3318; Elvis, Martin/0000-0001-5060-1398 FU NSFC [11473021, 11522323]; Fundamental Research Funds for the Central Universities [20720160023]; NASA [NAS8-03060]; NSF [1066293]; Chandra grant [GO-415107X, GO5-16099X, GO2-13127X]; Hubble grant [GO-13741.002-A] FX W.P.M. acknowledges support from Chandra grants GO-415107X, GO5-16099X, and GO2-13127X, and Hubble grant GO-13741.002-A, and also thanks Henrique Schmitt for helpful discussions. J.W. acknowledges support from the NSFC grants 11473021 and 11522323, and the Fundamental Research Funds for the Central Universities under grant 20720160023. We acknowledge partial support by NASA contract NAS8-03060 (CXC). STSDAS and PyRAF are products of the Space Telescope Science Institute, which is operated by AURA for NASA. We thank the anonymous referee for comments that improved the quality of the paper. M.E. and G.F. thank the Aspen Center for Physics, funded by NSF grant #1066293 and for their hospitality while this paper was completed. NR 37 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2016 VL 829 IS 1 AR 46 DI 10.3847/0004-637X/829/1/46 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8IY UT WOS:000385374500046 ER PT J AU Morris, PW Gupta, H Nagy, Z Pearson, JC Ossenkopf-Okada, V Falgarone, E Lis, DC Gerin, M Melnick, G Neufeld, DA Bergin, EA AF Morris, Patrick W. Gupta, Harshal Nagy, Zsofia Pearson, John C. Ossenkopf-Okada, Volker Falgarone, Edith Lis, Dariusz C. Gerin, Maryvonne Melnick, Gary Neufeld, David A. Bergin, Edwin A. TI HERSCHEL/HIFI SPECTRAL MAPPING OF C+, CH+, AND CH IN ORION BN/KL: THE PREVAILING ROLE OF ULTRAVIOLET IRRADIATION IN CH+ FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: lines and bands; ISM: molecules; molecular processes ID PHOTON-DOMINATED REGIONS; STAR-FORMING REGIONS; DIFFUSE INTERSTELLAR-MEDIUM; VIBRATIONALLY EXCITED H-2; MOLECULAR LINE EMISSION; C-12/C-13 ISOTOPE RATIO; MEUDON PDR CODE; KL HOT CORE; PHYSICAL CONDITIONS; ROTATIONAL-EXCITATION AB The CH+ ion is a key species in the initial steps of interstellar carbon chemistry. Its formation in diverse environments where it is observed is not well understood, however, because the main production pathway is so endothermic (4280 K) that it is unlikely to proceed at the typical temperatures of molecular clouds. We investigate the formation of this highly reactive molecule with the first velocity-resolved spectral mapping of the CH+ J. = 1-0, 2-1 rotational transitions, three sets of CH Lambda-doubled triplet lines, C-12(+) and C-13(+) P-2(3/2)-P-2(1/2),andCH(3)OH 835 GHz E-symmetry Q-branch transitions, obtained with Herschel/HIFI over a region of approximate to 12 arcmin(2) centered on the Orion BN/KL source. We present the spatial morphologies and kinematics, cloud boundary conditions, excitation temperatures, column densities, and C-12(+) optical depths. Emission from all of C+, CH+, and CH is indicated to arise in the diluted gas, outside the explosive, dense BN/KL outflow. Our models show that UV irradiation provides favorable conditions for steady-state production of CH+ in this environment. Surprisingly, no spatial or kinematic correspondences of the observed species are found with H-2 S(1) emission tracing shocked gas in the outflow. We propose that C+ is being consumed by rapid production of CO to explain the lack of both C+ and CH+ in the outflow. Hence, in star-forming environments containing sources of shocks and strong UV radiation, a description of the conditions leading to CH+ formation and excitation is incomplete without including the important-possibly dominant-role of UV irradiation. C1 [Morris, Patrick W.; Gupta, Harshal] CALTECH, NASA, Herschel Sci Ctr, IPAC M-C 100-22, Pasadena, CA 91125 USA. [Gupta, Harshal] Natl Sci Fdn, Div Astron Sci, 4201 Wilson Blvd,Suite 1045, Arlington, VA 22230 USA. [Nagy, Zsofia; Ossenkopf-Okada, Volker] Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. [Nagy, Zsofia] Univ Toledo, Dept Phys & Astron, 2801 West Bancroft St, Toledo, OH 43606 USA. [Pearson, John C.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Falgarone, Edith; Gerin, Maryvonne] Univ Paris 06, Sorbonne Univ, PSL Res Univ, LERMA,Observ Paris,CNRS,Ecole Normale Super, F-75005 Paris, France. [Lis, Dariusz C.] Univ Paris 06, Sorbonne Univ, PSL Res Univ, LERMA,Observ Paris,CNRS, F-75014 Paris, France. [Lis, Dariusz C.] CALTECH, Cahill Ctr Astron & Astrophys MC 301 17, Pasadena, CA 91125 USA. [Melnick, Gary] Harvard Smithsonian Ctr Astrophys, 60 Garden St,Mail Stop 66, Cambridge, MA 02138 USA. [Neufeld, David A.] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. RP Morris, PW (reprint author), CALTECH, NASA, Herschel Sci Ctr, IPAC M-C 100-22, Pasadena, CA 91125 USA. EM pmorris@ipac.caltech.edu FU NASA (Herschel GT funding); JPL/Caltech; Deutsche Forschungsgemeinschaft (DFG) [SFB 956, C1]; CNES; INSU program PCMI; National Science Foundation (NSF) FX This work is based on observations made with the HIFI instrument on the Herschel Space Observatory, which was designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States (the National Aeronautics and Space Administration, NASA) under the leadership of the Netherlands Institute for Space Research (SRON), Groningen, The Netherlands, and with major contributions from Germany, France, and the US. We express our gratitude to Nathan Crockett for helpful discussions and providing the Orion BN/KL continuum data, and to John Bally and Nathan Cunningham for providing the H2 observations of the BN/KL outflow. We also thank Octavio Roncero and Alexandre Zanchet for providing their CH+ state-to-state formation rates, and we especially appreciate support with the Meudon PDR code from Frank Le Petit. We are grateful to the HIFI Instrument Control Center team for its many years of dedicated work and support. We also thank an anonymous referee for thorough review of the manuscript and thoughtful comments to improve its quality. Support for this work was provided by NASA (Herschel GT funding) through an award issued by JPL/Caltech. V.O. acknowledges support by the Deutsche Forschungsgemeinschaft (DFG) via the collaborative research grant SFB 956, project C1. E.F. and M.G. thank the CNES and the INSU program PCMI for funding. A part of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. H.G. acknowledges support from the National Science Foundation (NSF). Any opinions, findings, and conclusions in this article are those of the authors, and do not necessarily reflect the views of the NSF. NR 139 TC 1 Z9 1 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2016 VL 829 IS 1 AR 15 DI 10.3847/0004-637X/829/1/15 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8IY UT WOS:000385374500015 ER PT J AU Timmons, N Cooray, A Riechers, DA Nayyeri, H Fu, H Jullo, E Gladders, MD Baes, M Bussmann, RS Calanog, J Clements, DL da Cunha, E Dye, S Eales, SA Furlanetto, C Gonzalez-Nuevo, J Greenslade, J Gurwell, M Messias, H Michalowski, MJ Oteo, I Perez-Fournon, I Scott, D Valiante, E AF Timmons, Nicholas Cooray, Asantha Riechers, Dominik A. Nayyeri, Hooshang Fu, Hai Jullo, Eric Gladders, Michael D. Baes, Maarten Bussmann, R. Shane Calanog, Jae Clements, David L. da Cunha, Elisabete Dye, Simon Eales, Stephen A. Furlanetto, Cristina Gonzalez-Nuevo, Joaquin Greenslade, Joshua Gurwell, Mark Messias, Hugo Michalowski, Michal J. Oteo, Ivan Perez-Fournon, Ismael Scott, Douglas Valiante, Elisabetta TI MULTI-WAVELENGTH LENS RECONSTRUCTION OF A PLANCK AND HERSCHEL- DETECTED STAR-BURSTING GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; infrared: galaxies; submillimeter: galaxies ID DEEP-FIELD-SOUTH; LUMINOUS SUBMILLIMETER GALAXIES; SEQUENCE CLUSTER SURVEY; MOLECULAR GAS; FORMING GALAXIES; HIGH-REDSHIFT; INFRARED-EMISSION; MASSIVE GALAXIES; FORMATION RATES; STELLAR MASSES AB We present a source-plane reconstruction of a Herschel and Planck-detected gravitationally lensed dusty star-forming galaxy (DSFG) at z = 1.68 using Hubble, Submillimeter Array (SMA), and Keck observations. The background submillimeter galaxy (SMG) is strongly lensed by a foreground galaxy cluster at z = 0.997 and appears as an arc with a. length of similar to 15 ''. in the optical images. The continuum dust emission, as seen by SMA, is limited to a single knot within this arc. We present a lens model with source-plane reconstructions at several wavelengths to show the difference in magnification between the stars and dust, and highlight the importance of. multi-wavelength lens models for studies involving lensed DSFGs. We estimate the physical properties of the galaxy by fitting the flux densities to model spectral energy distributions leading to a magnification-corrected star-formation rate (SFR) of 390 +/- 60 M-circle dot yr(-1) and a stellar mass of 1.1 +/- 0.4 x 10(11) M-circle dot. These values are consistent with high-redshift massive galaxies that have formed most of their stars already. The estimated gas-to-baryon fraction, molecular gas surface density, and SFR surface density have values of 0.43 +/- 0.13, 350 +/- 200 M-circle dot pc(-2), and similar to 12 +/- 7 M-circle dot yr(-1) kpc(-2), respectively. The ratio of SFR surface density to molecular gas surface density puts this among the most star-forming systems, similar to other measured SMGs and local ULIRGs. C1 [Timmons, Nicholas; Cooray, Asantha; Nayyeri, Hooshang] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Riechers, Dominik A.; Bussmann, R. Shane] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Jullo, Eric] Aix Marseille Univ, CNRS, LAM, UMR 7326, 38 Rue Joliot Curie, F-13388 Marseille, France. [Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA. [Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA. [Baes, Maarten] Univ Ghent, Sterrenkundig Observ, Krijgslaan 281S9, B-9000 Ghent, Belgium. [Calanog, Jae] San Diego Miramar Coll, Dept Phys Sci, San Diego, CA 92126 USA. [Clements, David L.; Greenslade, Joshua] Imperial Coll, Dept Phys, Blackett Lab, Prince Consort Rd, London SW7 2AZ, England. [da Cunha, Elisabete] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Dye, Simon; Furlanetto, Cristina] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England. [Eales, Stephen A.; Valiante, Elisabetta] Cardiff Univ, Sch Phys & Astron, Queens Bldg, Cardiff CF24 3AA, S Glam, Wales. [Furlanetto, Cristina] Minist Educ Brazil, CAPES Fdn, BR-70040020 Brasilia, DF, Brazil. [Gonzalez-Nuevo, Joaquin] Univ Oviedo, Dept Fis, C Calvo Sotelo S-N, E-33007 Oviedo, Spain. [Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Messias, Hugo] Univ Lisbon, OAL, Inst Astrofis & Ciencias Espaco, PT-1349018 Lisbon, Portugal. [Michalowski, Michal J.; Oteo, Ivan] Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Oteo, Ivan] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Perez-Fournon, Ismael] IAC, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Perez-Fournon, Ismael] Univ La Laguna, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain. [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. RP Timmons, N (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RI Gonzalez-Nuevo, Joaquin/I-3562-2014; OI Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; da Cunha, Elisabete/0000-0001-9759-4797 FU NASA through Space Telescope Science Institute [HST-GO-13399]; NASA [NAS 5-26555]; NSF [AST-1313319]; W.M. Keck Foundation; Smithsonian Institution; Academia Sinica; CAPES [12203-1]; Spanish MINECO; Fundacao para a Ciencia e a Tecnologia (FCT) [SFRH/BPD/97986/2013]; European Research Council [321302]; National Science Foundation [AST-1614213] FX We wish to thank the anonymous referee whose comments helped improve the paper. Financial support for this work was provided by NASA through grant HST-GO-13399 from the Space Telescope Science Institute, which is operated by Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Additional support for N.T., A.C., and H.N. was from NSF through AST-1313319. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. C.F. acknowledges funding from CAPES (proc. 12203-1). J.G.N. acknowledges financial support from the Spanish MINECO for a Ramon y Cajal fellowship. H.M. acknowledges support from the Fundacao para a Ciencia e a Tecnologia (FCT) through the Fellowship SFRH/BPD/97986/2013. I.O. acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. D.A.R. acknowledges support from the National Science Foundation under grant number AST-1614213 to Cornell University. NR 72 TC 0 Z9 0 U1 5 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2016 VL 829 IS 1 AR 21 DI 10.3847/0004-637X/829/1/21 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8IY UT WOS:000385374500021 ER PT J AU White, JA Boley, AC Hughes, AM Flaherty, KM Ford, E Wilner, D Corder, S Payne, M AF White, J. A. Boley, A. C. Hughes, A. M. Flaherty, K. M. Ford, E. Wilner, D. Corder, S. Payne, M. TI ALMA OBSERVATIONS OF HD 141569's CIRCUMSTELLAR DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; stars: individual (HD 141569); submillimeter: planetary systems ID DEBRIS DISKS; MOLECULAR GAS; PROTOPLANETARY DISKS; BETA-PICTORIS; PLANET FORMATION; UPPER LIMITS; CO EMISSION; STARS; HD-141569; NEARBY AB We present ALMA band 7 (345 GHz) continuum and (CO)-C-12(J = 3-2) observations of the circumstellar disk surrounding HD 141569. At an age of about 5 Myr, the disk has a complex morphology that may be best interpreted as a nascent debris system with gas. Our 870 mu m ALMA continuum observations resolve a dust disk out to approximately 56 au from the star (assuming a distance of 116 pc) with 0 ''.38 resolution and 0.07 mJy beam(-1) sensitivity. We measure a continuum flux density for this inner material of 3.8 +/- 0.4 mJy (including calibration uncertainties). The (CO)-C-12(3-2) gas is resolved kinematically and spatially from about 30 to 210 au. The integrated (CO)-C-12(3-2) line flux density is 15.7 +/- 1.6 Jy kms(-1). We estimate the mass of the millimeter debris and (CO)-C-12(3-2) gas to be greater than or similar to 0.04 M-circle plus and similar to 2 x 10(-3) M-circle plus respectively. If the millimeter grains are part of a collisional cascade, then we infer that the inner disk (<50 au) has similar to 160 M-circle plus contained within objects less than 50 km in radius, depending on the planetesimal size distribution and density assumptions. Markov Chain Monte Carlo modeling of the system reveals a disk morphology with an inclination of 53 degrees.4 centered around an M = 2.39M(circle dot) Me host star (Msin(i) = 1.92. M-circle dot). We discuss whether the gas in HD 141569's disk may be second generation. If it is, the system can be used to study the clearing stages of planet formation. C1 [White, J. A.; Boley, A. C.] Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. [Hughes, A. M.; Flaherty, K. M.] Wesleyan Univ, Dept Astron, Van Vleck Observ, 96 Foss Hill Dr, Middletown, CT 06459 USA. [Ford, E.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, 525 Davey Lab, University Pk, PA 16802 USA. [Ford, E.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. [Ford, E.] Penn State Univ, Ctr Astrostat, 417C Thomas Bldg, University Pk, PA 16802 USA. [Wilner, D.; Payne, M.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Corder, S.] Natl Radio Astron Observ, North Amer ALMA Sci Ctr, 520 Edgemont Rd, Charlottesville, VA 22903 USA. RP White, JA (reprint author), Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada. EM jawhite@astro.ubc.ca OI /0000-0001-6545-639X FU NSERC; Canadian Foundation for Innovation; University of British Columbia; European Research Council [320620]; NSF [AST-1412647]; Center for Exoplanets and Habitable Worlds; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NASA [NNX13A124G, NNX10AH40G, 1312645088477, NNX16AD69G]; BSF Grant [2012384]; Smithsonian CGPS/Pell Grant Program FX J.A.W. and A.C.B. acknowledge support from an NSERC Discovery Grant, the Canadian Foundation for Innovation, The University of British Columbia, and the European Research Council (agreement number 320620). A.M.H. and K.M.F. are supported by NSF grant AST-1412647. E.B.F.'s contribution was supported in part by funding from the Center for Exoplanets and Habitable Worlds. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. A.C.B. and E.B.F. also acknowledge The University of Florida and the NASA Sagan Fellowship program. M.J.P. also acknowledges NASA Origins of Solar Systems Program grant NNX13A124G, NASA Origins of Solar System Program grant NNX10AH40G via award agreement 1312645088477, NASA Solar System Observations grant NNX16AD69G, BSF Grant Number 2012384, as well as support from the Smithsonian 2015 CGPS/Pell Grant Program. NR 66 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2016 VL 829 IS 1 AR 6 DI 10.3847/0004-637X/829/1/6 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8IY UT WOS:000385374500006 ER PT J AU Howell, SB Everett, ME Horch, EP Winters, JG Hirsch, L Nusdeo, D Scott, NJ AF Howell, Steve B. Everett, Mark E. Horch, Elliott P. Winters, Jennifer G. Hirsch, Lea Nusdeo, Dan Scott, Nicholas J. TI SPECKLE IMAGING EXCLUDES LOW-MASS COMPANIONS ORBITING THE EXOPLANET HOST STAR TRAPPIST-1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: imaging; stars: individual (TRAPPIST-1, 2MASS J23062928-0502285) ID KEPLER; TELESCOPE; PROGRAM; PLANETS; SYSTEMS; DWARFS; K2 AB We have obtained the highest-resolution images available of TRAPPIST-1 using the Gemini-South telescope and our speckle imaging camera. Observing at 692 and 883 nm, we reached the diffraction limit of the telescope providing a best resolution of 27 mas or, at the distance of TRAPPIST-1, a spatial resolution of 0.32 au. Our imaging of the star extends from 0.32 to 14.5 au. We show that to a high confidence level, we can exclude all possible stellar and brown dwarf companions, indicating that TRAPPIST-1 is a single star. C1 [Howell, Steve B.; Scott, Nicholas J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Everett, Mark E.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Horch, Elliott P.] Southern Connecticut State Univ, Dept Phys, 501 Crescent St, New Haven, CT 06515 USA. [Winters, Jennifer G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hirsch, Lea] Univ Calif Berkeley, Dept Astron, 510 Campbell Hall, Berkeley, CA 94720 USA. [Nusdeo, Dan] Georgia State Univ, Dept Phys & Astron, POB 5060, Atlanta, GA 30302 USA. RP Howell, SB (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. FU John Templeton Foundation; Gemini Observatory [GS-2016A-Q-80] FX We wish to thank the staff of the Gemini-South Observatory for their kind assistance with our visiting instrument and during our observation run. The referee made a number of suggestions that led to a better presentation. Elisa Quintana provided helpful discussions on the topic of planet stability under the influence of a disturbing companion star. J.W. is supported through a grant from the John Templeton Foundation. The opinions expressed here do not necessarily reflect the views of the John Templeton Foundation. These results are based on observations obtained as part of the program GS-2016A-Q-80 at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina), and Ministerio da Ciencia, Tecnologia e Inovacao (Brazil). NR 19 TC 0 Z9 0 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2016 VL 829 IS 1 AR L2 DI 10.3847/2041-8205/829/1/L2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8WG UT WOS:000385412000002 ER PT J AU Iono, D Yun, MS Aretxaga, I Hatsukade, B Hughes, D Ikarashi, S Izumi, T Kawabe, R Kohno, K Lee, M Matsuda, Y Nakanishi, K Saito, T Tamura, Y Ueda, J Umehata, H Wilson, G Michiyama, T Ando, M AF Iono, Daisuke Yun, Min S. Aretxaga, Itziar Hatsukade, Bunyo Hughes, David Ikarashi, Soh Izumi, Takuma Kawabe, Ryohei Kohno, Kotaro Lee, Minju Matsuda, Yuichi Nakanishi, Kouichiro Saito, Toshiki Tamura, Yoichi Ueda, Junko Umehata, Hideki Wilson, Grant Michiyama, Tomonari Ando, Misaki TI CLUMPY AND EXTENDED STARBURSTS IN THE BRIGHTEST UNLENSED SUBMILLIMETER GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst ID FAR-INFRARED EMISSION; STAR-FORMING GALAXIES; ARP 220; PHYSICAL SCALE; HIGH-REDSHIFT; COSMOS FIELD; C II; ALMA; DISKS; ARP-220 AB The central structure in three of the brightest unlensed z = 3-4 submillimeter galaxies is investigated through 0".015-0".05 (120-360 pc) 860 mu m continuum images obtained using the Atacama Large Millimeter/submillimeter Array ( ALMA). The distribution in the central kiloparsec in AzTEC1 and AzTEC8 is extremely complex, and they are composed of multiple similar to 200 pc clumps. AzTEC4 consists of two sources that are separated by similar to 1.5 kpc, indicating a mid-stage merger. The peak star formation rate densities in the central clumps are similar to 300-3000Me yr(-1) kpc(-2), suggesting regions with extreme star formation near the Eddington limit. By comparing the flux obtained by ALMA and Submillimeter Array, we find that 68%-90% of the emission is extended (greater than or similar to 1 kpc) in AzTEC4 and 8. For AzTEC1, we identify at least 11 additional compact (similar to 200 pc) clumps in the extended 3-4 kpc region. Overall, the data presented here suggest that the luminosity surface densities observed at less than or similar to 150 pc scales are roughly similar to that observed in local ULIRGs, as in the eastern nucleus of Arp 220. Between 10% and 30% of the 860 mu m continuum is concentrated in clumpy structures in the central kiloparsec, while the remaining flux is distributed over greater than or similar to 1 kpc regions, some of which could also be clumpy. These sources can be explained by a rapid inflow of gas such as a merger of gas-rich galaxies, surrounded by extended and clumpy starbursts. However, the cold mode accretion model is not ruled out. C1 [Iono, Daisuke; Hatsukade, Bunyo; Kawabe, Ryohei; Matsuda, Yuichi; Nakanishi, Kouichiro] Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Iono, Daisuke; Matsuda, Yuichi; Nakanishi, Kouichiro; Michiyama, Tomonari; Ando, Misaki] SOKENDAI Grad Univ Adv Studies, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. [Yun, Min S.; Wilson, Grant] Univ Massachusetts, Dept Astron, 710 North Pleasant St, Amherst, MA 01003 USA. [Aretxaga, Itziar; Hughes, David] INAOE, Luis Enrique Erro 1, Puebla, Mexico. [Ikarashi, Soh] Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. [Izumi, Takuma; Kohno, Kotaro; Tamura, Yoichi; Umehata, Hideki] Univ Tokyo, Inst Astron, 2-21-1 Osawa, Mitaka, Tokyo 1810015, Japan. [Kohno, Kotaro] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Lee, Minju] Univ Tokyo, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. [Ueda, Junko] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Iono, D (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.; Iono, D (reprint author), SOKENDAI Grad Univ Adv Studies, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM d.iono@nao.ac.jp OI Hatsukade, Bunyo/0000-0001-6469-8725; Lee, Minju/0000-0002-2419-3068; Yun, Min/0000-0001-7095-7543 FU Japan Society for Promotion of Science (JSPS) KAKENHI [15H02074]; Inamori Research Grants Program; National Science Foundation [PHY-1066293]; Netherlands Organization for Scientific Research (NWO) [614.001.403] FX We thank our referee for valuable comments that improved the contents of this Letter significantly. We thank P. Cox, S. Iguchi, T. Kodama, D. Narayanan, and J. Simpson for useful discussion. D. I. is supported by Japan Society for Promotion of Science (JSPS) KAKENHI (No. 15H02074) and by the 2015 Inamori Research Grants Program. This work was performed in part at the Aspen Center for Physics, which is supported by National Science Foundation grant PHY-1066293. S. I. acknowledges the support of the Netherlands Organization for Scientific Research (NWO) through the Top Grant Project 614.001.403. This Letter makes use of the following ALMA data: ADS/JAO. ALMA#2012.1.00978.S and #2015.1.01345.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. NR 46 TC 2 Z9 2 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2016 VL 829 IS 1 AR L10 DI 10.3847/2041-8205/829/1/L10 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8WG UT WOS:000385412000010 ER PT J AU Vanderburg, A Bieryla, A Duev, DA Jensen-Clem, R Latham, DW Mayo, AW Baranec, C Berlind, P Kulkarni, S Law, NM Nieberding, MN Riddle, R Salama, M AF Vanderburg, Andrew Bieryla, Allyson Duev, Dmitry A. Jensen-Clem, Rebecca Latham, David W. Mayo, Andrew W. Baranec, Christoph Berlind, Perry Kulkarni, Shrinivas Law, Nicholas M. Nieberding, Megan N. Riddle, Reed Salama, Maissa TI TWO SMALL PLANETS TRANSITING HD 3167 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; planets and satellites: detection; stars: individual (HD 3167) ID EXTRASOLAR GIANT PLANETS; SUPER-EARTH; TRANSMISSION SPECTRUM; CANDIDATES; STAR; SEARCH; SYSTEM; K2; ATMOSPHERE; EFFICIENT AB We report the discovery of two super-Earth-sized planets transiting the bright (V = 8.94, K = 7.07) nearby late G-dwarf HD 3167, using data collected by the K2 mission. The inner planet, HD 3167 b, has a radius of 1.6 R-circle plus and an ultra-short orbital period of only 0.96 days. The outer planet, HD 3167 c, has a radius of 2.9 R-circle plus and orbits its host star every 29.85 days. At a distance of just 45.8 +/- 2.2 pc, HD 3167 is one of the closest and brightest stars hosting multiple transiting planets, making HD 3167 b and c well suited for follow-up observations. The star is chromospherically inactive with low rotational line-broadening, ideal for radial velocity observations to measure the planets' masses. The outer planet is large enough that it likely has a thick gaseous envelope that could be studied via transmission spectroscopy. Planets transiting bright, nearby stars like HD 3167 are valuable objects to study leading up to the launch of the James Webb Space Telescope. C1 [Vanderburg, Andrew; Bieryla, Allyson; Latham, David W.; Mayo, Andrew W.; Berlind, Perry] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Duev, Dmitry A.; Jensen-Clem, Rebecca; Kulkarni, Shrinivas; Riddle, Reed] CALTECH, Pasadena, CA 91125 USA. [Baranec, Christoph] Univ Hawaii Manoa, Hilo, HI 96720 USA. [Law, Nicholas M.] Univ North Carolina Chapel Hill, Chapel Hill, NC 27599 USA. [Nieberding, Megan N.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Salama, Maissa] Univ Hawaii Manoa, Honolulu, HI 96822 USA. RP Vanderburg, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avanderburg@cfa.harvard.edu OI Vanderburg, Andrew/0000-0001-7246-5438; Latham, David/0000-0001-9911-7388 FU NSF [DGE 1144152]; Kepler mission under NASA [NNX13AB58A]; Smithsonian Astrophysical Observatory; Alfred P. Sloan Foundation; National Geographic Society; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mt. Cuba Astronomical Foundation FX We thank Hannah Diamond- Lowe, Christophe Lovis, and Phil Muirhead for valuable conversations, and we thank the anonymous referee for helpful comments. A.V. is supported by the NSF Graduate Research Fellowship, grant No. DGE 1144152. D.W.L. acknowledges partial support from the Kepler mission under NASA Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. C.B. acknowledges support from the Alfred P. Sloan Foundation.; This research has made use of NASA's Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. The National Geographic Society-Palomar Observatory Sky Atlas was made by the California Institute of Technology with grants from the National Geographic Society. The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory.; This Letter includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-Hubble Space Telescope data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts.; Robo-AO KP is a partnership between the California Institute of Technology, University of Hawai'i Manoa, University of North Carolina, Chapel Hill, the Inter-University Centre for Astronomy and Astrophysics, and the National Central University, Taiwan. Robo-AO KP was supported by a grant from Sudha Murty, Narayan Murthy, and Rohan Murty. The Robo-AO instrument was developed with support from the National Science Foundation under grants AST-0906060, AST-0960343, and AST-1207891, the Mt. Cuba Astronomical Foundation, and by a gift from Samuel Oschin. Based in part on observations at Kitt Peak National Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: 15B-3001), which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 39 TC 0 Z9 0 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2016 VL 829 IS 1 AR L9 DI 10.3847/2041-8205/829/1/L9 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8WG UT WOS:000385412000009 ER PT J AU Guimond, PO Pichler, H Rauschenbeutel, A Zoller, P AF Guimond, Pierre-Olivier Pichler, Hannes Rauschenbeutel, Arno Zoller, Peter TI Chiral quantum optics with V-level atoms and coherent quantum feedback SO PHYSICAL REVIEW A LA English DT Article ID ARTIFICIAL ATOM; SINGLE PHOTONS; CAVITY; DRIVEN; CIRCUITS; PHONONS; SYSTEMS AB We study the dissipative dynamics of an atom in a V-level configuration driven by lasers and coupled to a semi-infinite waveguide. The coupling to the waveguide is chiral, in that each transition interacts only with the modes propagating in a given direction, and this direction is opposite for the two transitions. The waveguide is terminated by a mirror which coherently feeds the photon stream emitted by one transition back to the atom. First, we are interested in the dynamics of the atom in the Markovian limit where the time delay in the feedback is negligible. Specifically, we study the conditions under which the atom evolves towards a pure "dark" stationary state, where the photons emitted by both transitions interfere destructively thanks to the coherent feedback, and the overall emission vanishes. This is a single-atom analog of the quantum dimer, where a pair of laser-driven two-level atoms is coupled to a unidirectional waveguide and dissipates towards a pure entangled dark state. Our setup should be feasible with current state-of-the-art experiments. Second, we extend our study to non-Markovian regimes and investigate the effect of the feedback retardation on the steady state. C1 [Guimond, Pierre-Olivier; Pichler, Hannes; Zoller, Peter] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. [Guimond, Pierre-Olivier; Zoller, Peter] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Pichler, Hannes] Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. [Pichler, Hannes] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. [Rauschenbeutel, Arno] Vienna Univ Technol, Vienna Ctr Quantum Sci & Technol, Atominst, A-1020 Vienna, Austria. RP Guimond, PO (reprint author), Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria.; Guimond, PO (reprint author), Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. RI Zoller, Peter/O-1639-2014; Pichler, Hannes/M-5150-2015; Rauschenbeutel, Arno/C-1472-2013 OI Zoller, Peter/0000-0003-4014-1505; Pichler, Hannes/0000-0003-2144-536X; Rauschenbeutel, Arno/0000-0003-2467-4029 FU ERC Synergy Grant UQUAM; Austrian Science Fund through SFB FO-QUS; EU FET Proactive Initiative SIQS; Army Research Laboratory Center for Distributed Quantum Information via the project SciNet; NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University; Smithsonian Astrophysical Observatory; EU FET Proactive Initiative RYQS FX The work at Innsbruck is supported by the ERC Synergy Grant UQUAM, the Austrian Science Fund through SFB FO-QUS, the EU FET Proactive Initiative SIQS and RYQS, and the Army Research Laboratory Center for Distributed Quantum Information via the project SciNet. H.P. was supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory. NR 50 TC 1 Z9 1 U1 10 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD SEP 16 PY 2016 VL 94 IS 3 AR 033829 DI 10.1103/PhysRevA.94.033829 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA DW0NI UT WOS:000383336700008 ER PT J AU Gomes, DGE Page, RA Geipel, I Taylor, RC Ryan, MJ Halfwerk, W AF Gomes, D. G. E. Page, R. A. Geipel, I. Taylor, R. C. Ryan, M. J. Halfwerk, W. TI Bats perceptually weight prey cues across sensory systems when hunting in noise SO SCIENCE LA English DT Article ID FROG; COMPLEXITY AB Anthropogenic noise can interfere with environmental information processing and thereby reduce survival and reproduction. Receivers of signals and cues in particular depend on perceptual strategies to adjust to noisy conditions. We found that predators that hunt using prey sounds can reduce the negative impact of noise by making use of prey cues conveyed through additional sensory systems. In the presence of masking noise, but not in its absence, frog-eating bats preferred and were faster in attacking a robotic frog emitting multiple sensory cues. The behavioral changes induced by masking noise were accompanied by an increase in active localization through echolocation. Our findings help to reveal how animals can adapt to anthropogenic noise and have implications for the role of sensory ecology in driving species interactions. C1 [Gomes, D. G. E.; Page, R. A.; Geipel, I.; Taylor, R. C.; Ryan, M. J.; Halfwerk, W.] Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama. [Gomes, D. G. E.] Max Planck Inst Ornithol, D-82319 Seewiesen, Germany. [Taylor, R. C.] Salisbury Univ, Dept Biol, Salisbury, MD 21801 USA. [Ryan, M. J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Halfwerk, W.] Vrije Univ Amsterdam, Dept Ecol Sci, NL-1081 HV Amsterdam, Netherlands. RP Halfwerk, W (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Panama.; Halfwerk, W (reprint author), Vrije Univ Amsterdam, Dept Ecol Sci, NL-1081 HV Amsterdam, Netherlands. EM w.h.halfwerk@vu.nl FU Smithsonian fellowship; NSF [IOS 1120031]; Smithsonian Tropical Research Institute FX For support in the field, we thank the Gamboa Bat Lab, specifically L. F. Gomez-Feuillet. We thank B. Klein, P. Clements, and Moey Inc. for fabricating the pneumatic robotic frog system, and J. Ellers and H. Goerlitz for comments that substantially improved the manuscript. Supported by a Smithsonian fellowship (W.H.), NSF grant IOS 1120031 (R.C.T., M.J.R., and R.A.P.), and the Smithsonian Tropical Research Institute (R.A.P.). All research reported here complied with STRI IACUC protocols (2015-0209-2018; 2014-0101-2017). We obtained all required permits from the Government of Panama (SE/A-86-14). The authors report no conflict of interest. Raw data are available at the Dryad Data Repository (dx.doi:10.5061/dryad.5gk8j). NR 20 TC 1 Z9 1 U1 57 U2 57 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 16 PY 2016 VL 353 IS 6305 BP 1277 EP 1280 DI 10.1126/science.aaf7934 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DW2AD UT WOS:000383444400044 PM 27634533 ER PT J AU Sohn, JC Stanescu, M AF Sohn, Jae-Cheon Stanescu, Mihai TI Revised status of Oridryas Meyrick, 1938: new synonyms of Ypsolopha Latreille, 1796, and Ypsolopha parenthesella (Linnaeus, 1761) (Yponomeutoidea: Ypsolophidae) SO ZOOTAXA LA English DT Letter C1 [Sohn, Jae-Cheon] Mokpo Natl Univ, Inst Littoral Environm, Muan 58554, Jeonnam, South Korea. [Sohn, Jae-Cheon] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, 10th & Constitut NW, Washington, DC 20560 USA. [Stanescu, Mihai] Grigore Antipa Natl Museum Nat Hist, Kiseleff 1, Bucharest, Romania. RP Sohn, JC (reprint author), Mokpo Natl Univ, Inst Littoral Environm, Muan 58554, Jeonnam, South Korea.; Sohn, JC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, 10th & Constitut NW, Washington, DC 20560 USA. EM jay.c.sohn@gmail.com; mihaist@antipa.ro NR 12 TC 0 Z9 0 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 16 PY 2016 VL 4168 IS 3 BP 589 EP 593 DI 10.11646/zootaxa.4168.3.12 PG 5 WC Zoology SC Zoology GA DV8MZ UT WOS:000383192400012 PM 27701332 ER PT J AU Hong, T AF Hong, Terry TI Vaseline Buddha SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 15 PY 2016 VL 141 IS 15 BP 79 EP 79 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA DV8XR UT WOS:000383220500096 ER PT J AU Fioletov, VE McLinden, CA Krotkov, N Li, C Joiner, J Theys, N Carn, S Moran, MD AF Fioletov, Vitali E. McLinden, Chris A. Krotkov, Nickolay Li, Can Joiner, Joanna Theys, Nicolas Carn, Simon Moran, Mike D. TI A global catalogue of large SO2 sources and emissions derived from the Ozone Monitoring Instrument SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID SULFUR-DIOXIDE EMISSIONS; GROUND-BASED MEASUREMENTS; FIRED POWER-PLANTS; SATELLITE RETRIEVALS; EL-CHICHON; MAPPING SPECTROMETER; SURFACE MEASUREMENTS; BOUNDARY-LAYER; AIR-POLLUTION; VOLCANO AB Sulfur dioxide (SO2) measurements from the Ozone Monitoring Instrument (OMI) satellite sensor processed with the new principal component analysis (PCA) algorithm were used to detect large point emission sources or clusters of sources. The total of 491 continuously emitting point sources releasing from about 30 kt yr(-1) to more than 4000 kt yr(-1) of SO2 per year have been identified and grouped by country and by primary source origin: volcanoes (76 sources); power plants (297); smelters (53); and sources related to the oil and gas industry (65). The sources were identified using different methods, including through OMI measurements themselves applied to a new emission detection algorithm, and their evolution during the 2005-2014 period was traced by estimating annual emissions from each source. For volcanic sources, the study focused on continuous degassing, and emissions from explosive eruptions were excluded. Emissions from degassing volcanic sources were measured, many for the first time, and collectively they account for about 30% of total SO2 emissions estimated from OMI measurements, but that fraction has increased in recent years given that cumulative global emissions from power plants and smelters are declining while emissions from oil and gas industry remained nearly constant. Anthropogenic emissions from the USA declined by 80% over the 2005-2014 period as did emissions from western and central Europe, whereas emissions from India nearly doubled, and emissions from other large SO2-emitting regions (South Africa, Russia, Mexico, and the Middle East) remained fairly constant. In total, OMI-based estimates account for about a half of total reported anthropogenic SO2 emissions; the remaining half is likely related to sources emitting less than 30 kt yr(-1) and not detected by OMI. C1 [Fioletov, Vitali E.; McLinden, Chris A.; Joiner, Joanna; Moran, Mike D.] Environm Canada, Air Qual Res Div, Toronto, ON, Canada. [Krotkov, Nickolay; Li, Can] NASA, Atmospher Chem & Dynam Lab, Goddard Space Flight Ctr, Green Belt, MD USA. [Li, Can] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Theys, Nicolas] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Carn, Simon] Michigan Technol Univ, Dept Geol & Min Engn & Sci, Houghton, MI 49931 USA. [Carn, Simon] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Fioletov, VE (reprint author), Environm Canada, Air Qual Res Div, Toronto, ON, Canada. EM vitali.fioletov@outlook.com FU NASA Earth Science Division FX We acknowledge the NASA Earth Science Division, specifically the Aura science team program, for funding OMI SO2 product development and analysis. The Dutch/Finnish-built OMI instrument is part of the NASA EOS Aura satellite payload. The OMI project is managed by KNMI and the Netherlands Space Agency (NSO). We would like to thank Arlin Krueger and an anonymous reviewer for their comments that helped us improve the manuscript. NR 91 TC 5 Z9 5 U1 22 U2 22 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD SEP 15 PY 2016 VL 16 IS 18 BP 11497 EP 11519 DI 10.5194/acp-16-11497-2016 PG 23 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DX3CW UT WOS:000384251700002 ER PT J AU Uramoto, K Norrbom, AL Zucchi, RA AF Uramoto, Keiko Norrbom, Allen L. Zucchi, Roberto A. TI Redescription, lectotype designation and new records of Anastrepha luederwaldti Lima (Diptera, Tephritidae) SO ZOOTAXA LA English DT Article DE Diptera; Tephritidae AB The previously poorly known species Anastrepha luederwaldti Lima, 1934 is redescribed based on a reexamination of the syntypes from Sao Paulo and additional specimens from Santa Catarina and Rio Grande do Sul, Brazil. A lectotype is designated. C1 [Uramoto, Keiko; Zucchi, Roberto A.] Univ Sao Paulo, ESALQ, Dept Entomol & Acarol, Caixa Postal 9, BR-13418900 Piracicaba, SP, Brazil. [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. RP Uramoto, K (reprint author), Univ Sao Paulo, ESALQ, Dept Entomol & Acarol, Caixa Postal 9, BR-13418900 Piracicaba, SP, Brazil. EM uramoto@usp.br; allen.norrbom@ars.usda.gov; razucchi@usp.br RI Zucchi, Roberto/D-7738-2012; Gesseff, Ednilson/A-3019-2017 OI Zucchi, Roberto/0000-0001-9861-7460; NR 18 TC 0 Z9 0 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 15 PY 2016 VL 4168 IS 2 BP 341 EP 346 DI 10.11646/zootaxa.4168.2.7 PG 6 WC Zoology SC Zoology GA DV8MN UT WOS:000383191200007 PM 27701340 ER PT J AU Hong, T AF Hong, Terry TI Kurosawa's Rashomon: A Vanished City, a Lost Brother, and the Voice Inside His Most Iconic Films SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20024 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20024 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 15 PY 2016 VL 141 IS 15 BP 84 EP 86 PG 3 WC Information Science & Library Science SC Information Science & Library Science GA DV8XR UT WOS:000383220500118 ER PT J AU MacDonald, GM Moser, KA Bloom, AM Potito, AP Porinchu, DF Holmquist, JR Hughes, J Kremenetski, KV AF MacDonald, Glen M. Moser, Katrina A. Bloom, Amy M. Potito, Aaron P. Porinchu, David F. Holmquist, James R. Hughes, Julia Kremenetski, Konstantine V. TI Prolonged California aridity linked to climate warming and Pacific sea surface temperature SO SCIENTIFIC REPORTS LA English DT Article ID ORGANIC-MATTER SOURCES; TROPICAL PACIFIC; SIERRA-NEVADA; LATE-HOLOCENE; EL-NINO; SOUTHERN CALIFORNIA; DECADAL OSCILLATION; NORTH-AMERICA; DROUGHT; OCEAN AB California has experienced a dry 21st century capped by severe drought from 2012 through 2015 prompting questions about hydroclimatic sensitivity to anthropogenic climate change and implications for the future. We address these questions using a Holocene lake sediment record of hydrologic change from the Sierra Nevada Mountains coupled with marine sediment records from the Pacific. These data provide evidence of a persistent relationship between past climate warming, Pacific sea surface temperature (SST) shifts and centennial to millennial episodes of California aridity. The link is most evident during the thermal-maximum of the mid-Holocene (similar to 8 to 3 ka; ka = 1,000 calendar years before present) and during the Medieval Climate Anomaly (MCA) (similar to 1 ka to 0.7 ka). In both cases, climate warming corresponded with cooling of the eastern tropical Pacific despite differences in the factors producing increased radiative forcing. The magnitude of prolonged eastern Pacific cooling was modest, similar to observed La Nina excursions of 1 degrees to 2 degrees C. Given differences with current radiative forcing it remains uncertain if the Pacific will react in a similar manner in the 21st century, but should it follow apparent past behavior more intense and prolonged aridity in California would result. C1 [MacDonald, Glen M.; Kremenetski, Konstantine V.] Univ Calif Los Angeles, Dept Geog, 1255 Bunche Hall, Los Angeles, CA 90095 USA. [Moser, Katrina A.] Univ Western Ontario, Dept Geog, 1151 Richmond St North, London, ON N6A 5C2, Canada. [Moser, Katrina A.] Univ Western Ontario, Ctr Environm & Sustainabil, 1151 Richmond St North, London, ON N6A 5C2, Canada. [Bloom, Amy M.] Illinois State Univ, Dept Geog & Geol, Campus Box 4400, Normal, IL 61790 USA. [Potito, Aaron P.] Natl Univ Ireland, Sch Geog & Archaeol, Galway, Ireland. [Porinchu, David F.] Univ Georgia, Dept Geog, 210 Field St, Athens, GA 30602 USA. [Holmquist, James R.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Hughes, Julia] Westminster Sch, Geog, London SW1P 3PF, England. RP MacDonald, GM (reprint author), Univ Calif Los Angeles, Dept Geog, 1255 Bunche Hall, Los Angeles, CA 90095 USA. EM macdonal@geog.ucla.edu FU NSF Regional Sciences [BSC-9905350, BSC-0135748, BSC-0101268]; NSERC Discovery grant; NSF Doctoral Dissertation Improvement grant [BCS-0101268]; Geological Society of America (GSA) graduate student research grant; University Research Grant Program New Faculty Initiative Grant (NFIG) from the College of Arts and Sciences at Illinois State University FX Funds for this research were provided by a NSF Regional Sciences grants to G.M.M. and K.A.M. (BSC-9905350, BSC-0135748, BSC-0101268), a NSERC Discovery grant to K.A.M., a NSF Doctoral Dissertation Improvement grant to A.P.P. (BCS-0101268), a Geological Society of America (GSA) graduate student research grant to A.P.P., and a University Research Grant Program New Faculty Initiative Grant (NFIG) from the College of Arts and Sciences at Illinois State University to A.M.B. This is a Southwest Climate Science Center contribution. NR 47 TC 0 Z9 0 U1 39 U2 39 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD SEP 15 PY 2016 VL 6 AR 33325 DI 10.1038/srep33325 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DV8LI UT WOS:000383188100001 PM 27629520 ER PT J AU Ballent, A Corcoran, PL Madden, O Helm, PA Longstaffe, FJ AF Ballent, Anika Corcoran, Patricia L. Madden, Odile Helm, Paul A. Longstaffe, Fred J. TI Sources and sinks of microplastics in Canadian Lake Ontario nearshore, tributary and beach sediments SO MARINE POLLUTION BULLETIN LA English DT Article DE Microplastics; Lake Ontario; Sediments; Raman spectroscopy; Nearshore; Watershed ID LAURENTIAN GREAT-LAKES; PLASTIC DEBRIS; MARINE-ENVIRONMENT; SURFACE WATERS; RIVER; IDENTIFICATION; POLLUTION; LITTER; ACCUMULATION; DEGRADATION AB Microplastics contamination of Lake Ontario sediments is investigated with the aim of identifying distribution patterns and hotspots in nearshore, tributary and beach depositional environments. Microplastics are concentrated in nearshore sediments in the vicinity of urban and industrial regions. In Humber Bay and Toronto Harbour microplastic concentrations were consistently >500 particles per kg dry sediment. Maximum concentrations of similar to 28,000 particles per kg dry sediment were determined in Etobicoke Creek. The microplastic particles were primarily fibres and fragments <2 mm in size. Both low- and high-density plastics were identified using Raman spectroscopy. We provide a baseline for future monitoring and discuss potential sources of microplastics in terms of how and where to implement preventative measures to reduce the contaminant influx. Although the impacts of microplastics contamination on ecosystem health and functioning is uncertain, understanding, monitoring and preventing further microplastics contamination in Lake Ontario and the other Great Lakes is crucial. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Ballent, Anika; Corcoran, Patricia L.; Longstaffe, Fred J.] Univ Western Ontario, Dept Earth Sci, 1151 Richmond St N, London, ON N6A 5B7, Canada. [Madden, Odile] Smithsonian Inst, Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. [Helm, Paul A.] Ontario Minist Environm & Climate Change, Environm Monitoring & Reporting Branch, 125 Resources Rd, Toronto, ON M9P 3V6, Canada. RP Ballent, A (reprint author), Univ Western Ontario, Dept Earth Sci, 1151 Richmond St N, London, ON N6A 5B7, Canada. EM 4anikab@gmail.com FU Great Lakes Strategy / Canada-Ontario Agreement [2206] FX This work was funded under the Great Lakes Strategy / Canada-Ontario Agreement with Respect to the Great Lakes program (Project ID #2206). We would like to thank Danielle Cocchetto and Tim Howe for assisting with field work, as well as our editor, Charles Sheppard, at the Marine Pollution Bulletin and reviewers for their constructive feedback and assistance in improving this manuscript. NR 70 TC 5 Z9 5 U1 86 U2 89 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD SEP 15 PY 2016 VL 110 IS 1 BP 383 EP 395 DI 10.1016/j.marpolbul.2016.06.037 PG 13 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA DU6QO UT WOS:000382339900053 PM 27342902 ER PT J AU Lunning, NG Corrigan, CM McSween, HY Tenner, TJ Kita, NT Bodnar, RJ AF Lunning, Nicole G. Corrigan, Catherine M. McSween, Harry Y., Jr. Tenner, Travis J. Kita, Noriko T. Bodnar, Robert J. TI CV and CM chondrite impact melts SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Impact melt; Carbonaceous chondrite; CV chondrite; Howardite; CM chondrite; Vesta; Regolith; Oxygen isotopes; Relict olivine; Melt spherule; Melt pocket; Melt clast ID ASTEROID 4 VESTA; 162173 1999 JU3; OXYGEN-ISOTOPE SYSTEMATICS; CARBONACEOUS CHONDRITES; SHOCK METAMORPHISM; DARK MATERIAL; PARENT BODY; MAIN-BELT; COMPOSITIONAL CLASSIFICATION; METEORITIC CHONDRULES AB Volatile-rich and typically oxidized carbonaceous chondrites, such as CV and CM chondrites, potentially respond to impacts differently than do other chondritic materials. Understanding impact melting of carbonaceous chondrites has been hampered by the dearth of recognized impact melt samples. In this study we identify five carbonaceous chondrite impact melt clasts in three host meteorites: a CV3(red) chondrite, a CV3(oxA) chondrite, and a regolithic howardite. The impact melt clasts in these meteorites respectively formed from CV3(red) chondrite, CV3(oxA) chondrite, and CM chondrite protoliths. We identified these impact melt clasts and interpreted their precursors based on their texture, mineral chemistry, silicate bulk elemental composition, and in the case of the CM chondrite impact melt clast, in situ measurement of oxygen three-isotope signatures in olivine. These impact melts typically contain euhedral-subhedral olivine microphenocrysts, sometimes with relict cores, in glassy groundmasses. Based on petrography and Raman spectroscopy, four of the impact melt clasts exhibit evidence for volatile loss: these melt clasts either contain vesicles or are depleted in H2O relative to their precursors. Volatile loss (i.e., H2O) may have reduced the redox state of the CM chondrite impact melt clast. The clasts that formed from the more oxidized precursors (CV3(oxA) and CM chondrites) exhibit phase and bulk silicate elemental compositions consistent with higher intrinsic oxygen fugacities relative to the clast that formed from a more reduced precursor (CV3(red) chondrite). The mineral chemistries and assemblages of the CV and CM chondrite impact melt clasts identified here provide a template for recognizing carbonaceous chondrite impact melts on the surfaces of asteroids. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Lunning, Nicole G.; McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Lunning, Nicole G.; McSween, Harry Y., Jr.] Univ Tennessee, Planetary Geosci Inst, Knoxville, TN 37996 USA. [Lunning, Nicole G.; Corrigan, Catherine M.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Tenner, Travis J.; Kita, Noriko T.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Tenner, Travis J.] Los Alamos Natl Lab, Div Chem, Nucl & Radiochem, MSJ514, Los Alamos, NM 87545 USA. [Bodnar, Robert J.] Virginia Tech, Dept Geosci, Blacksburg, VA 24061 USA. RP Lunning, NG (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012,MRC 119, Washington, DC 20013 USA. EM lunningn@si.edu; corriganc@si.edu; mcsween@utk.edu; tenner@lanl.gov; noriko@geology.wisc.edu; rjb@vt.edu OI Lunning, Nicole/0000-0002-9845-5104 NR 121 TC 1 Z9 1 U1 6 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD SEP 15 PY 2016 VL 189 BP 338 EP 358 DI 10.1016/j.gca.2016.05.038 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DS4LR UT WOS:000380753100020 ER PT J AU Schrader, DL Davidson, J Mccoy, TJ AF Schrader, Devin L. Davidson, Jemma Mccoy, Timothy J. TI Widespread evidence for high-temperature formation of pentlandite in chondrites SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article DE Pentlandite; Pyrrhotite; Exsolution; High-temperature; Annealing; Aqueous alteration; Meteorite; Chondrite ID PARENT BODY METAMORPHISM; CK CARBONACEOUS CHONDRITES; MONOSULFIDE SOLID-SOLUTION; COBALT-IRON-SULFUR; COMET WILD 2; NI-S SYSTEM; THERMAL HISTORY; MICRORAMAN SPECTROSCOPY; CHEMICAL-COMPOSITIONS; AQUEOUS ALTERATION AB By investigating the compositional and textural evolution of sulfides within a wide range of relatively pristine, aqueously altered, and thermally metamorphosed chondrites we constrain the equilibration temperatures of sulfide minerals and compare them to the metamorphic history of their host meteorite. Sulfides in Mighei-like carbonaceous chondrites are complex as they equilibrated mostly between 100 and 135 degrees C, but some may have equilibrated at temperatures up to 600 degrees C. This is consistent with some CM chondrite sulfides forming at high temperature during chondrule cooling and others during low-temperature aqueous alteration and/or annealing. Karoonda-like carbonaceous chondrite sulfides equilibrated between 500 and 230 degrees C, which is consistent with formation during cooling and annealing after thermal metamorphism. Sulfides in the LL chondrites equilibrated between 600 and 230 degrees C, and are consistent with formation during chondrule cooling for Semarkona (LL3.00) and during cooling after thermal metamorphism for the equilibrated samples (types 4-6). Sulfides in the Rumuruti-like (R) chondrites equilibrated between 600 and 500 degrees C, and are consistent with formation after thermal metamorphism. The sulfides within the brachinite equilibrated between 600 and 400 degrees C, consistent with formation during cooling after thermal metamorphism. Contrary to the assertion that pentlandite is solely the product of low-temperature aqueous alteration in many chondrite groups, this study suggests that most sulfides in chondrites are formed at or upon cooling from high-temperature. The evaluation of a single mineral system within samples that retain petrographic context is vital to the interpretation of formation and alteration processes recorded by small extraterrestrial samples, such as those that have been returned by the spacecraft missions Stardust and Hayabusa and will be returned by OSIRIS-REx and Hayabusa2. (C) 2016 Elsevier Ltd. All rights reserved. C1 [Schrader, Devin L.; Mccoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th & Constitut Ave NW, Washington, DC 20560 USA. [Davidson, Jemma] Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. RP Schrader, DL (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Ctr Meteorite Studies, POB 871404, Tempe, AZ 85287 USA. EM schraderd@asu.edu NR 96 TC 1 Z9 1 U1 6 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 EI 1872-9533 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD SEP 15 PY 2016 VL 189 BP 359 EP 376 DI 10.1016/j.gca.2016.06.012 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA DS4LR UT WOS:000380753100021 ER PT J AU Nava, M Martin-Drumel, MA Lopez, CA Crabtree, KN Womack, CC Nguyen, TL Thorwirth, S Cummins, CC Stanton, JF McCarthy, MC AF Nava, Matthew Martin-Drumel, Marie-Aline Lopez, Christopher A. Crabtree, Kyle N. Womack, Caroline C. Nguyen, Thanh L. Thorwirth, Sven Cummins, Christopher C. Stanton, John F. McCarthy, Michael C. TI Spontaneous and Selective Formation of HSNO, a Crucial Intermediate Linking H2S and Nitroso Chemistries SO JOURNAL OF THE AMERICAN CHEMICAL SOCIETY LA English DT Article ID NITRIC-OXIDE SOLUTIONS; S-NITROSOTHIOLS; HYDROGEN-SULFIDE; DISSOCIATION-ENERGIES; VENTILATORY RESPONSE; HNO; ISOMERIZATION; DECOMPOSITION; SPECTROSCOPY; GENERATION AB Thionitrous acid (HSNO), a potential key intermediate in biological signaling pathways, has been proposed to link NO and H2S biochemistries, but its existence and stability in vivo remain controversial. We establish that HSNO is spontaneously formed in high concentration when NO and H2S gases are mixed at room temperature in the presence of metallic surfaces. Our measurements reveal that HSNO is formed by the reaction H2S + N2O3 -> HSNO + HNO2, where N2O3 is a product of NO disproportionation. These studies also suggest that further reaction of HSNO with H2S may form HNO and HSSH. The length of the S-N bond has been derived to high precision and is found to be unusually long: 1.84 angstrom, the longest S-N bond reported to date for an R-SNO compound. The present structural and, particularly, reactivity investigations of this elusive molecule provide a firm foundation to better understand its potential physiological chemistry and propensity to undergo S-N bond cleavage in vivo. C1 [Nava, Matthew; Womack, Caroline C.; Cummins, Christopher C.] MIT, Dept Chem, Cambridge, MA 02139 USA. [Martin-Drumel, Marie-Aline; Crabtree, Kyle N.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Martin-Drumel, Marie-Aline; Crabtree, Kyle N.; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Lopez, Christopher A.; Nguyen, Thanh L.; Stanton, John F.] Univ Texas Austin, Dept Chem, Inst Theoret Chem, Austin, TX 78712 USA. [Thorwirth, Sven] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Crabtree, Kyle N.] Univ Calif Davis, Dept Chem, Davis, CA 95616 USA. [Womack, Caroline C.] NOAA ESRL, Chem Sci Div, Boulder, CO 80305 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA.; McCarthy, MC (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. EM mmccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; Cummins, Christopher/0000-0003-2568-3269; Martin-Drumel, Marie-Aline/0000-0002-5460-4294 FU NASA [NNX13AE59G]; National Science Foundation [CHE-1362118]; CfA Postdoctoral Fellowship from Smithsonian Astrophysical Observatory; Camille and Henry Dreyfus Foundation Postdoctoral Program in Environmental Chemistry; Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-2]; U.S. Department of Energy, Office of Science, Basic Energy Science [DE-FG02-07ER1588] FX We thank Dr. Ivana Ivanovic-Burmazovic for an insightful and helpful discussion of HSNO biochemistry. The experimental work is supported by NASA grant NNX13AE59G. This material is based upon work supported by the National Science Foundation under CHE-1362118. M.A.M.-D. and K.N.C. were supported by a CfA Postdoctoral Fellowship from the Smithsonian Astrophysical Observatory and C.C.W. by the Camille and Henry Dreyfus Foundation Postdoctoral Program in Environmental Chemistry. S.T. gratefully acknowledges support by the Deutsche Forschungsgemeinschaft (DFG) through Grant TH 1301/3-2. J.F.S. and T.L.N. were supported by the U.S. Department of Energy, Office of Science, Basic Energy Science (award no. DE-FG02-07ER1588). NR 35 TC 5 Z9 5 U1 23 U2 23 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0002-7863 J9 J AM CHEM SOC JI J. Am. Chem. Soc. PD SEP 14 PY 2016 VL 138 IS 36 BP 11441 EP 11444 DI 10.1021/jacs.6b05886 PG 4 WC Chemistry, Multidisciplinary SC Chemistry GA DW1NU UT WOS:000383410700005 PM 27540860 ER PT J AU Oberg, KI AF Oberg, Karin I. TI Photochemistry and Astrochemistry: Photochemical Pathways to Interstellar Complex Organic Molecules SO CHEMICAL REVIEWS LA English DT Review ID YOUNG STELLAR OBJECTS; POLYCYCLIC AROMATIC-HYDROCARBONS; CIRCULARLY-POLARIZED LIGHT; ASTROPHYSICAL ICE ANALOGS; VACUUM-ULTRAVIOLET LIGHT; AMORPHOUS SOLID WATER; GAS-GRAIN CHEMISTRY; MASS PROTOSTAR IRAS-16293-2422; ABSORPTION CROSS-SECTIONS; STAR-FORMATION REGIONS AB The interstellar medium is characterized by a rich and diverse chemistry. Many of its complex organic molecules are proposed to form through radical chemistry in icy grain mantles. Radicals form readily when interstellar ices (composed of water and other volatiles) are exposed to UV photons and other sources of dissociative radiation, and if sufficiently mobile the radicals can react to form larger, more complex molecules. The resulting complex organic molecules (COMs) accompany star and planet formation and may eventually seed the origins of life on nascent planets. Experiments of increasing sophistication have demonstrated that known interstellar COMs as well as the prebiotically interesting amino acids can form through ice photochemistry. We review these experiments and discuss the qualitative and quantitative kinetic and mechanistic constraints they have provided. We finally compare the effects of UV radiation with those of three other potential sources of radical production and chemistry in interstellar ices: electrons, ions, and X-rays. C1 [Oberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM koberg@cfa.harvard.edu FU Simons Collaboration on the Origins of Life (SCOL) [321183]; Alfred P. Sloan fellowship; Packard fellowship FX The author thanks Edith Fayolle, Jennifer Bergner, and four anonymous referees for valuable feedback on the manuscript. The author also acknowledges funding from the Simons Collaboration on the Origins of Life (SCOL), award number 321183, an Alfred P. Sloan fellowship, and a Packard fellowship. NR 223 TC 3 Z9 3 U1 45 U2 45 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0009-2665 EI 1520-6890 J9 CHEM REV JI Chem. Rev. PD SEP 14 PY 2016 VL 116 IS 17 BP 9631 EP 9663 DI 10.1021/acs.chemrev.5b00694 PG 33 WC Chemistry, Multidisciplinary SC Chemistry GA DW1NO UT WOS:000383410100002 PM 27099922 ER PT J AU Bak, J Liu, X Kim, JH Deland, MT Chance, K AF Bak, Juseon Liu, Xiong Kim, Jae H. Deland, Matthew T. Chance, Kelly TI Improvement of OMI ozone profile retrievals by simultaneously fitting polar mesospheric clouds SO ATMOSPHERIC MEASUREMENT TECHNIQUES LA English DT Article ID MONITORING INSTRUMENT; SATELLITE; ICE; ULTRAVIOLET; MICROWAVE; VALIDATION; SCIAMACHY; ALGORITHM; EXPLORER; MISSION AB The presence of polar mesospheric clouds (PMCs) at summer high latitudes could affect the retrieval of ozone profiles using backscattered ultraviolet (UV) measurements. PMC-induced errors in ozone profile retrievals from Ozone Monitoring Instrument (OMI) backscattered UV measurements are investigated through comparisons with Microwave Limb Sounder (MLS) ozone measurements. This comparison demonstrates that the presence of PMCs leads to systematic biases for pressures smaller than 6 hPa; the biases increase from similar to -2% at 2 hPa to similar to -20% at 0.5 hPa on average and are significantly correlated with brightness of PMCs. Sensitivity studies show that the radiance sensitivity to PMCs strongly depends on wavelength, increasing by a factor of similar to 4 from 300 to 265 nm. It also strongly depends on the PMC scattering, thus depending on viewing geometry. The optimal estimation-based retrieval sensitivity analysis shows that PMCs located at 80-85 km have the greatest effect on ozone retrievals at similar to 0.2 hPa (similar to 60 km), where the retrieval errors range from -2.5% with PMC vertical optical depth (POD) of 10(-4) to -20% with 10(-3) POD at backscattering angles. The impacts increase by a factor of similar to 5 at forward-scattering angles due to stronger PMC sensitivities. To reduce the interference of PMCs on ozone retrievals, we perform simultaneous retrievals of POD and ozone with a loose constraint of 10(-3) for POD, which results in retrieval errors of 1-4 x 10(-4). It is demonstrated that the negative bias of OMI ozone retrievals relative to MLS can be improved by including the PMC in the forward-model calculation and retrieval. C1 [Bak, Juseon; Kim, Jae H.] Pusan Natl Univ, Dept Atmospher Sci, Busan, South Korea. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Deland, Matthew T.] Syst & Applicat Inc SSAI, 10210 Greenbelt Rd,Suite 600, Lanham, MD 20706 USA. RP Kim, JH (reprint author), Pusan Natl Univ, Dept Atmospher Sci, Busan, South Korea. EM jaekim@pusan.ac.kr RI Liu, Xiong/P-7186-2014 OI Liu, Xiong/0000-0003-2939-574X FU Pusan National University; NASA Aura science team program [NNX11AE95G, NNX14AF16G]; Smithsonian Institution FX The authors thank the OMI and MLS science teams for providing the satellite data. Research at Pusan National University by J. Bak and J. H. Kim was financially supported by "2016 Post-Doc. Development Program" of Pusan National University. Research at the Smithsonian Astrophysical Observatory by X. Liu and K. Chance, as well as J. Bak during her 3-month visit to the Harvard-Smithsonian Center for Astrophysics, was funded by the NASA Aura science team program (NNX11AE95G and NNX14AF16G) and the Smithsonian Institution. NR 44 TC 0 Z9 0 U1 3 U2 3 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1867-1381 EI 1867-8548 J9 ATMOS MEAS TECH JI Atmos. Meas. Tech. PD SEP 13 PY 2016 VL 9 IS 9 DI 10.5194/amt-9-4521-2016 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA DX3CY UT WOS:000384251900001 ER PT J AU Yusoff, AM Tan, TK Hari, R Koepfli, KP Wee, WY Antunes, A Sitam, FT Rovie-Ryan, JJ Karuppannan, KV Wong, GJ Lipovich, L Warren, WC O'Brien, SJ Choo, SW AF Yusoff, Aini Mohamed Tan, Tze King Hari, Ranjeev Koepfli, Klaus-Peter Wee, Wei Yee Antunes, Agostinho Sitam, Frankie Thomas Rovie-Ryan, Jeffrine Japning Karuppannan, Kayal Vizi Wong, Guat Jah Lipovich, Leonard Warren, Wesley C. O'Brien, Stephen J. Choo, Siew Woh TI De novo sequencing, assembly and analysis of eight different transcriptomes from the Malayan pangolin SO SCIENTIFIC REPORTS LA English DT Article ID RNA-SEQ READS; EVOLUTION; MAMMALS; PROTEIN; GENOME; LENGTH; ANNOTATION; GENERATION; REPEATS; GENES AB Pangolins are scale-covered mammals, containing eight endangered species. Maintaining pangolins in captivity is a significant challenge, in part because little is known about their genetics. Here we provide the first large-scale sequencing of the critically endangered Manis javanica transcriptomes from eight different organs using Illumina HiSeq technology, yielding similar to 75 Giga bases and 89,754 unigenes. We found some unigenes involved in the insect hormone biosynthesis pathway and also 747 lipids metabolism-related unigenes that may be insightful to understand the lipid metabolism system in pangolins. Comparative analysis between M. javanica and other mammals revealed many pangolin-specific genes significantly over-represented in stress-related processes, cell proliferation and external stimulus, probably reflecting the traits and adaptations of the analyzed pregnant female M. javanica. Our study provides an invaluable resource for future functional works that may be highly relevant for the conservation of pangolins. C1 [Yusoff, Aini Mohamed; Tan, Tze King; Hari, Ranjeev; Wee, Wei Yee; Wong, Guat Jah; Choo, Siew Woh] Univ Malaya, Genome Informat Res Lab, HIR Bldg, Kuala Lumpur 50603, Malaysia. [Yusoff, Aini Mohamed; Tan, Tze King; Hari, Ranjeev; Wee, Wei Yee; Choo, Siew Woh] Univ Malaya, Fac Dent, DeptrtmentOral & Craniofacial Sci, Kuala Lumpur 50603, Malaysia. [Koepfli, Klaus-Peter] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [Antunes, Agostinho] Univ Porto, Interdisciplinary Ctr Marine & Environm Res, CIIMAR CIMAR, Rua Bragas 177, P-4050123 Oporto, Portugal. [Antunes, Agostinho] Univ Porto, Fac Sci, Dept Biol, Rua Campo Alegre, P-4169007 Oporto, Portugal. [Sitam, Frankie Thomas; Rovie-Ryan, Jeffrine Japning; Karuppannan, Kayal Vizi] DWNP Peninsular Malaysia, Ex Situ Conservat Div, KM 10, Kuala Lumpur 56100, Malaysia. [Lipovich, Leonard] Wayne State Univ, Ctr Mol Med & Genet, Detroit, MI 48201 USA. [Lipovich, Leonard] Wayne State Univ, Sch Med, Dept Neurol, Detroit, MI 48201 USA. [Warren, Wesley C.] Washington Univ, McDonnell Genome Inst, St Louis, MO 63108 USA. [O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199004, Russia. [O'Brien, Stephen J.] Nova Southeastern Univ, Oceanog Ctr, 8000 N Ocean Dr, Ft Lauderdale, FL 33004 USA. [Choo, Siew Woh] Univ Malaya, Innovat Incubator UM, Genome Solut Sdn Bhd, Suite 8,Level 5,Res Management & Innovat Complex, Kuala Lumpur 50603, Malaysia. RP Choo, SW (reprint author), Univ Malaya, Genome Informat Res Lab, HIR Bldg, Kuala Lumpur 50603, Malaysia.; Choo, SW (reprint author), Univ Malaya, Fac Dent, DeptrtmentOral & Craniofacial Sci, Kuala Lumpur 50603, Malaysia.; Choo, SW (reprint author), Univ Malaya, Innovat Incubator UM, Genome Solut Sdn Bhd, Suite 8,Level 5,Res Management & Innovat Complex, Kuala Lumpur 50603, Malaysia. EM l.choo@genomesolutions.com.my RI Management Center, Dental Research/C-2478-2013 FU Russian Ministry of Science Mega-grant [11.G34.31.0068]; University of Malaya; Ministry of Education, Malaysia [UM.C/625/HIR/MOHE/CHAN-08] FX We would like to thank the members of Genome Informatics Research Laboratory and the International Pangolin Research Consortium (IPaRC), University of Malaya for their IT and bioinformatics assistance and inputs in this study. Furthermore, we would like to appreciate SJO supported as PI by Russian Ministry of Science Mega-grant no. 11.G34.31.0068. This project was supported by University of Malaya and Ministry of Education, Malaysia under the High Impact Research (HIR) grant UM.C/625/HIR/MOHE/CHAN-08. NR 49 TC 0 Z9 0 U1 15 U2 17 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD SEP 13 PY 2016 VL 6 AR 28199 DI 10.1038/srep28199 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA DV4UW UT WOS:000382921800001 ER PT J AU Guisande, C Vari, RP Heine, J Garcia-Rosello, E Gonzalez-Dacosta, J Perez-Schofield, BJG Gonzalez-Vilas, L Pelayo-Villami, P AF Guisande, Castor Vari, Richard P. Heine, Jurgen Garcia-Rosello, Emilio Gonzalez-Dacosta, Jacinto Garcia Perez-Schofield, Baltasar J. Gonzalez-Vilas, Luis Pelayo-Villami, Patricia TI VARSEDIG: an algorithm for morphometric characters selection and statistical validation in morphological taxonomy SO ZOOTAXA LA English DT Article DE Statistical method; Fishes; Morphological discrimination ID PACKAGE AB We present and discuss VARSEDIG, an algorithm which identifies the morphometric features that significantly discriminate two taxa and validates the morphological distinctness between them via a Monte-Carlo test. VARSEDIG is freely available as a function of the RWizard application PlotsR (http://www.ipez.es/RWizard) and as R package on CRAN. The variables selected by VARSEDIG with the overlap method were very similar to those selected by logistic regression and discriminant analysis, but overcomes some shortcomings of these methods. VARSEDIG is, therefore, a good alternative by comparison to current classical classification methods for identifying morphometric features that significantly discriminate a taxon and for validating its morphological distinctness from other taxa. As a demonstration of the potential of VARSEDIG for this purpose, we analyze morphological discrimination among some species of the Neotropical freshwater family Characidae. C1 [Guisande, Castor; Gonzalez-Vilas, Luis] Univ Vigo, Fac Ciencias, Vigo 36310, Spain. [Vari, Richard P.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. [Heine, Jurgen; Garcia-Rosello, Emilio; Gonzalez-Dacosta, Jacinto] Univ Vigo, Dept Informat, Edificio Fdn, Vigo 26310, Spain. [Garcia Perez-Schofield, Baltasar J.] Univ Vigo, Escuela Super Ingn Informat, Edificio Politecn S-N,Campus Lagoas, Orense 32004, Spain. [Pelayo-Villami, Patricia] Univ Antioquia, Grp Ictiol, Medellin, Colombia. RP Guisande, C (reprint author), Univ Vigo, Fac Ciencias, Vigo 36310, Spain. EM castor@uvigo.es NR 27 TC 0 Z9 0 U1 3 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 12 PY 2016 VL 4162 IS 3 BP 571 EP 580 DI 10.11646/zootaxa.4162.3.10 PG 10 WC Zoology SC Zoology GA DV8KA UT WOS:000383184700010 PM 27615992 ER PT J AU Tan, TK Tan, KY Hari, R Yusoff, AM Wong, GJ Siow, CC Mutha, NVR Rayko, M Komissarov, A Dobrynin, P Krasheninnikova, K Tamazian, G Paterson, IC Warren, WC Johnson, WE O'Brien, SJ Choo, SW AF Tan, Tze King Tan, Ka Yun Hari, Ranjeev Yusoff, Aini Mohamed Wong, Guat Jah Siow, Cheuk Chuen Mutha, Naresh V. R. Rayko, Mike Komissarov, Aleksey Dobrynin, Pavel Krasheninnikova, Ksenia Tamazian, Gaik Paterson, Ian C. Warren, Wesley C. Johnson, Warren E. O'Brien, Stephen J. Choo, Siew Woh TI PGD: a pangolin genome hub for the research community SO DATABASE-THE JOURNAL OF BIOLOGICAL DATABASES AND CURATION LA English DT Article ID MANIS-PENTADACTYLA-PENTADACTYLA; TOOL; DATABASE; ANNOTATION; BROWSER; UCSC; RNA; IDENTIFICATION; VISUALIZATION; PIPELINE AB Pangolins (order Pholidota) are the only mammals covered by scales. We have recently sequenced and analyzed the genomes of two critically endangered Asian pangolin species, namely the Malayan pangolin (Manis javanica) and the Chinese pangolin (Manis pentadactyla). These complete genome sequences will serve as reference sequences for future research to address issues of species conservation and to advance knowledge in mammalian biology and evolution. To further facilitate the global research effort in pangolin biology, we developed the Pangolin Genome Database (PGD), as a future hub for hosting pangolin genomic and transcriptomic data and annotations, and with useful analysis tools for the research community. Currently, the PGD provides the reference pangolin genome and transcriptome data, gene sequences and functional information, expressed transcripts, pseudogenes, genomic variations, organ-specific expression data and other useful annotations. We anticipate that the PGD will be an invaluable platform for researchers who are interested in pangolin and mammalian research. We will continue updating this hub by including more data, annotation and analysis tools particularly from our research consortium. C1 [Tan, Tze King; Tan, Ka Yun; Hari, Ranjeev; Yusoff, Aini Mohamed; Wong, Guat Jah; Siow, Cheuk Chuen; Mutha, Naresh V. R.; Choo, Siew Woh] Univ Malaya, Ctr Res Biotechnol Agr CEBAR, Genome Informat Res Lab, High Impact Res Bldg, Kuala Lumpur 50603, Malaysia. [Tan, Tze King; Hari, Ranjeev; Yusoff, Aini Mohamed; Paterson, Ian C.; Choo, Siew Woh] Univ Malaya, Fac Dent, Dept Oral & Craniofacial Sci, Kuala Lumpur 50603, Malaysia. [Tan, Ka Yun] Univ Malaya, Fac Sci, Inst Biol Sci, Kuala Lumpur 50603, Malaysia. [Rayko, Mike; Komissarov, Aleksey; Dobrynin, Pavel; Krasheninnikova, Ksenia; Tamazian, Gaik; O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199004, Russia. [Paterson, Ian C.] Univ Malaya, Fac Dent, Oral Canc Res & Coordinating Ctr, Kuala Lumpur 50603, Malaysia. [Warren, Wesley C.] Washington Univ, McDonnell Genome Inst, St Louis, MO 63108 USA. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [O'Brien, Stephen J.] Nova Southeastern Univ, Oceanog Ctr, Ft Lauderdale, FL 33004 USA. [Choo, Siew Woh] Univ Malaya, Genome Solut Sdn Bhd, Innovat Incubator UM, Suite 8,Level 5,Res Management & Innovat Complex, Kuala Lumpur 50603, Malaysia. RP Choo, SW (reprint author), Univ Malaya, Ctr Res Biotechnol Agr CEBAR, Genome Informat Res Lab, High Impact Res Bldg, Kuala Lumpur 50603, Malaysia.; Choo, SW (reprint author), Univ Malaya, Fac Dent, Dept Oral & Craniofacial Sci, Kuala Lumpur 50603, Malaysia.; Choo, SW (reprint author), Univ Malaya, Genome Solut Sdn Bhd, Innovat Incubator UM, Suite 8,Level 5,Res Management & Innovat Complex, Kuala Lumpur 50603, Malaysia. EM l.choo@genomesolutions.com.my RI Paterson, Ian/G-8688-2011; Management Center, Dental Research/C-2478-2013 FU University of Malaya; Ministry of Education, Malaysia under High Impact Research (HIR) grant [UM.C/625/HIR/MOHE/CHAN-08] FX This project was supported by University of Malaya and Ministry of Education, Malaysia under the High Impact Research (HIR) grant UM.C/625/HIR/MOHE/CHAN-08. NR 41 TC 0 Z9 0 U1 10 U2 10 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1758-0463 J9 DATABASE-OXFORD JI Database PD SEP 11 PY 2016 AR baw063 DI 10.1093/database/baw063 PG 10 WC Mathematical & Computational Biology SC Mathematical & Computational Biology GA DW7MN UT WOS:000383835100001 ER PT J AU Montero-Dorta, AD Bolton, AS Brownstein, JR Swanson, M Dawson, K Prada, F Eisenstein, D Maraston, C Thomas, D Comparat, J Chuang, CH McBride, CK Favole, G Guo, H Rodriguez-Torres, S Schneider, DP AF Montero-Dorta, Antonio D. Bolton, Adam S. Brownstein, Joel R. Swanson, Molly Dawson, Kyle Prada, Francisco Eisenstein, Daniel Maraston, Claudia Thomas, Daniel Comparat, Johan Chuang, Chia-Hsun McBride, Cameron K. Favole, Ginevra Guo, Hong Rodriguez-Torres, Sergio Schneider, Donald P. TI The high-mass end of the red sequence at z similar to 0.55 from SDSS-III/BOSS: completeness, bimodality and luminosity function SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; methods: statistical; surveys; galaxies: evolution; galaxies: luminosity function, mass function; galaxies: statistics ID DIGITAL SKY SURVEY; EARLY-TYPE GALAXIES; OSCILLATION SPECTROSCOPIC SURVEY; COLOR-MAGNITUDE RELATION; BARYON ACOUSTIC-OSCILLATIONS; BRIGHTEST CLUSTER GALAXIES; DATA RELEASE; QUIESCENT GALAXIES; STAR-FORMATION; STELLAR POPULATIONS AB We have developed an analytical method based on forward-modelling techniques to characterize the high-mass end of the red sequence (RS) galaxy population at redshift z similar to 0.55, from the DR10 BOSS (Baryon Oscillation Spectroscopic Survey) CMASS spectroscopic sample, which comprises similar to 600 000 galaxies. The method, which follows an unbinned maximum likelihood approach, allows the deconvolution of the intrinsic CMASS colour-colour-magnitude distributions from photometric errors and selection effects. This procedure requires modelling the covariance matrix for the i-band magnitude, g - r colour and r - i colour using Stripe 82 multi-epoch data. Our results indicate that the error-deconvolved intrinsic RS distribution is consistent, within the photometric uncertainties, with a single point (< 0.05 mag) in the colour-colour plane at fixed magnitude, for a narrow redshift slice. We have computed the high-mass end (M-0.55(i) less than or similar to -22) of the (0.55)i-band RS luminosity function (RS LF) in several redshift slices within the redshift range 0.52 < z < 0.63. In this narrow redshift range, the evolution of the RS LF is consistent, within the uncertainties in the modelling, with a passively evolving model with Phi(*) = (7.248 +/- 0.204) x 10(-4) Mpc(-3) mag(-1), fading at a rate of 1.5 +/- 0.4 mag per unit redshift. We report RS completeness as a function of magnitude and redshift in the CMASS sample, which will facilitate a variety of galaxy-evolution and clustering studies using BOSS. Our forward-modelling method lays the foundations for future studies using other dark-energy surveys like the Extended Baryon Oscillation Spectroscopic Survey or the Dark Energy Spectroscopic Instrument, which are affected by the same type of photometric blurring/selection effects. C1 [Montero-Dorta, Antonio D.; Bolton, Adam S.; Brownstein, Joel R.; Dawson, Kyle] Univ Utah, Dept Phys & Astron, 115 South 1400 East, Salt Lake City, UT 84112 USA. [Bolton, Adam S.] Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. [Swanson, Molly; Eisenstein, Daniel; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Prada, Francisco; Comparat, Johan; Chuang, Chia-Hsun; Favole, Ginevra; Rodriguez-Torres, Sergio] Univ Autonoma Madrid, CSIC, Campus Int Excellence, E-28049 Madrid, Spain. [Prada, Francisco; Comparat, Johan; Chuang, Chia-Hsun; Favole, Ginevra; Rodriguez-Torres, Sergio] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain. [Maraston, Claudia; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg, Portsmouth PO1 3FX, Hants, England. [Guo, Hong] Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. RP Montero-Dorta, AD (reprint author), Univ Utah, Dept Phys & Astron, 115 South 1400 East, Salt Lake City, UT 84112 USA. EM amontero@astro.utah.edu FU US Department of Energy, Office of Science, Office of High Energy Physics [DE-SC0010331]; Center for High Performance Computing at the University of Utah; Spanish MICINNs Consolider-Ingenio Programme [MultiDark CSD2009-00064, AYA2010-21231-C02-01]; MINECO Centro de Excelencia Severo Ochoa Programme [SEV-2012-0249]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; University of Florida; French Participation Group; German Participation Group; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX This material is based upon work supported by the US Department of Energy, Office of Science, Office of High Energy Physics, under Award Number DE-SC0010331.; The support and resources from the Center for High Performance Computing at the University of Utah are gratefully acknowledged.; AMD, FP, JC, CC, GF and SR thank the support from the Spanish MICINNs Consolider-Ingenio 2010 Programme under grant MultiDark CSD2009-00064, AYA2010-21231-C02-01 and MINECO Centro de Excelencia Severo Ochoa Programme under grant SEV-2012-0249.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, the University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 82 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 11 PY 2016 VL 461 IS 2 BP 1131 EP 1153 DI 10.1093/mnras/stw1352 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PP UT WOS:000383273600001 ER PT J AU Foley, RJ Pan, YC Brown, P Filippenko, AV Fox, OD Hillebrandt, W Kirshner, RP Marion, GH Milne, PA Parrent, JT Pignata, G Stritzinger, MD AF Foley, Ryan J. Pan, Yen-Chen Brown, P. Filippenko, A. V. Fox, O. D. Hillebrandt, W. Kirshner, R. P. Marion, G. H. Milne, P. A. Parrent, J. T. Pignata, G. Stritzinger, M. D. TI Ultraviolet diversity of Type Ia Supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN1992A, SN2009ig, SN2011by, SN 2011fe, SN 2011iv, SN 2012cg, SN 2013dy, SN 2014J, ASASSN-14lp, SN 2015F; ultraviolet: stars ID HUBBLE-SPACE-TELESCOPE; MAXIMUM-LIGHT ULTRAVIOLET; SN 2011FE; COSMOLOGICAL CONSTRAINTS; HOST GALAXIES; LINE-PROFILES; LOW-REDSHIFT; DECLINE RATE; SDSS-II; SPECTRA AB Ultraviolet (UV) observations of Type Ia supernovae (SNe Ia) probe the outermost layers of the explosion, and UV spectra of SNe Ia are expected to be extremely sensitive to differences in progenitor composition and the details of the explosion. Here, we present the first study of a sample of high signal-to-noise ratio SN Ia spectra that extend blueward of 2900 angstrom. We focus on spectra taken within 5 d of maximum brightness. Our sample of 10 SNe Ia spans, the majority of the parameter space of SN Ia optical diversity. We find that SNe Ia have significantly more diversity in the UV than in the optical, with the spectral variance continuing to increase with decreasing wavelengths until at least 1800 angstrom (the limit of our data). The majority of the UV variance correlates with optical light-curve shape, while there are no obvious and unique correlations between spectral shape and either ejecta velocity or host-galaxy morphology. Using light-curve shape as the primary variable, we create a UV spectral model for SNe Ia at peak brightness. With the model, we can examine how individual SNe vary relative to expectations based on only their light-curve shape. Doing this, we confirm an excess of flux for SN 2011fe at short wavelengths, consistent with its progenitor having a subsolar metallicity. While most other SNe Ia do not show large deviations from the model, ASASSN-14lp has a deficit of flux at short wavelengths, suggesting that its progenitor was relatively metal rich. C1 [Foley, Ryan J.; Pan, Yen-Chen] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. [Brown, P.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA. [Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. [Fox, O. D.] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. [Hillebrandt, W.] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Kirshner, R. P.; Parrent, J. T.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kirshner, R. P.] Gordon & Betty Moore Fdn, 1661 Page Mill Rd, Palo Alto, CA 94304 USA. [Marion, G. H.] Univ Texas Austin, 1 Univ Stn C1400, Austin, TX 78712 USA. [Milne, P. A.] Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85719 USA. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile. [Pignata, G.] Millennium Inst Astrophys, Avda Republ 252, Santiago, Chile. [Stritzinger, M. D.] Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. RP Foley, RJ (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA.; Foley, RJ (reprint author), Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA. EM rfoley@illinois.edu OI stritzinger, maximilian/0000-0002-5571-1833 FU NASA [NAS 5-26555, 14-WPS14-0048]; NSF [AST-1518052, AST-1211916]; Alfred P. Sloan Foundation; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC12009]; TABASGO Foundation; Christopher R. Redlich Fund; Danish Agency for Science and Technology; Innovation realized through a Sapere Aude Level 2 grant FX Based on observations made with the NASA/ESA HST, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programmes GO-4016, GO-12298, GO-12582, GO-12592, GO-13286, and GO-13646. We thank the STScI staff for accommodating our target-of-opportunity programmes. A. Armstrong, R. Bohlin, S. Holland, S. Meyett, D. Sahnow, P. Sonnentrucker, and D. Taylor were critical for the execution of these programmes.; RJF gratefully acknowledges support from NASA grant 14-WPS14-0048, NSF grant AST-1518052, and the Alfred P. Sloan Foundation. GP is supported by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. AVF is grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. MS acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant.; We thank the many amateur and professional astronomers who continue to discover nearby, incredibly scientifically useful SNe and publicly announce their discovery. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 74 TC 1 Z9 1 U1 5 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 11 PY 2016 VL 461 IS 2 BP 1308 EP 1316 DI 10.1093/mnras/stw1440 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PP UT WOS:000383273600011 ER PT J AU Katkov, IY Sil'chenko, OK Chilingarian, IV Uklein, RI Egorov, OV AF Katkov, Ivan Yu. Sil'chenko, Olga K. Chilingarian, Igor V. Uklein, Roman I. Egorov, Oleg V. TI Stellar counter-rotation in lenticular galaxy NGC 448 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: individual: NGC 448; galaxies: ISM; galaxies: kinematics and dynamics ID STAR-FORMATION HISTORIES; ATLAS(3D) PROJECT; SPIRAL GALAXIES; ELLIPTIC GALAXIES; MOLECULAR GAS; POPULATIONS; DISKS; IDENTIFICATION; II.; AGE AB The counter-rotation phenomenon in disc galaxies directly indicates a complex galaxy assembly history which is crucial for our understanding of galaxy physics. Here, we present the complex data analysis for a lenticular galaxy NGC 448, which has been recently suspected to host a counter-rotating stellar component. We collected deep long-slit spectroscopic observations using the Russian 6-m telescope and performed the photometric decomposition of Sloan Digital Sky Survey archival images. We exploited (i) a non-parametric approach in order to recover stellar line-of-sight velocity distributions and (ii) a parametric spectral decomposition technique in order to disentangle stellar population properties of both main and counter-rotating stellar discs. Our spectral decomposition stays in perfect agreement with the photometric analysis. The counter-rotating component contributes approximate to 30 per cent to the total galaxy light. We estimated its stellar mass to be 9.0(-1.8)(+2.7) x 10(9) M-circle dot. The radial scalelength of counter-rotating disc is approximate to 3 times smaller than that of the main disc. Both discs harbour old stars but the counter-rotating components reveal a detectable negative age gradient that might suggest an extended inside-out formation during 3... 4 Gyr. The counter-rotating disc hosts more metal-rich stars and possesses a shallower metallicity gradient with respect to the main disc. Our findings rule out cosmological filaments as a source of external accretion which is considered as a potential mechanism of the counter-rotating component formation in NGC 448, and favour the satellite merger event with the consequent slow gas accretion. C1 [Katkov, Ivan Yu.; Sil'chenko, Olga K.; Chilingarian, Igor V.; Egorov, Oleg V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Skiy Pr 13, Moscow 119992, Russia. [Sil'chenko, Olga K.] Isaac Newton Inst Chile, Moscow Branch, Moscow, Russia. [Chilingarian, Igor V.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St MS09, Cambridge, MA 02138 USA. [Uklein, Roman I.] Special Astrophys Observ, Nizhniy Arkhyz 369167, Karachai Cherke, Russia. RP Katkov, IY (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Skiy Pr 13, Moscow 119992, Russia. EM katkov@sai.msu.ru; sil@sai.msu.ru; igor.chilingarian@cfa.harvard.edu RI Egorov, Oleg/E-7293-2015; Chilingarian, Igor/N-5117-2016; OI Chilingarian, Igor/0000-0002-7924-3253; Katkov, Ivan/0000-0002-6425-6879 FU Russian Science Foundation [14-22-00041]; M.V. Lomonosov Moscow State University programme of Development; Russian Federation Ministry of Education and Science [14.619.21.0004, RFMEFI61914X0004]; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; [MD-7355.2015.2]; [RFBR 15-32-21062]; [RFBR-CNRS 15-52-15050] FX IK thanks Lodovico Coccato and Sergey Khoperskov for useful discussions. The work was supported by the Russian Science Foundation project 14-22-00041 'VOLGA - A View On the Life of GAlaxies'. The final interpretation of the data and paper writing was performed during visits to Chamonix workshop and The Research Institute in Astrophysics and Planetology in Toulouse which were supported by MD-7355.2015.2, RFBR 15-32-21062, and RFBR-CNRS 15-52-15050 grants. The project used computational resources funded by the M.V. Lomonosov Moscow State University programme of Development. The Russian 6-m telescope is exploited under the financial support by the Russian Federation Ministry of Education and Science (agreement No14.619.21.0004, project ID RFMEFI61914X0004). This research has made use of the NED which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and of the Lyon Extragalactic Database (LEDA). In this study, we used the SDSS DR12 data. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS web site is http://www.sdss.org/. NR 56 TC 1 Z9 1 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 11 PY 2016 VL 461 IS 2 BP 2068 EP 2076 DI 10.1093/mnras/stw1452 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PP UT WOS:000383273600069 ER PT J AU de Souza, RS Dantas, MLL Krone-Martins, A Cameron, E Coelho, P Hattab, MW de Val-Borro, M Hilbe, JM Elliott, J Hagen, A AF de Souza, R. S. Dantas, M. L. L. Krone-Martins, A. Cameron, E. Coelho, P. Hattab, M. W. de Val-Borro, M. Hilbe, J. M. Elliott, J. Hagen, A. CA COIN Collaboration TI Is the cluster environment quenching the Seyfert activity in elliptical and spiral galaxies? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; methods: statistical; galaxies: active; galaxies: clusters: general; galaxies: Seyfert ID DIGITAL-SKY-SURVEY; GENERALIZED LINEAR-MODELS; SUPERMASSIVE BLACK-HOLES; STAR-FORMATION RATES; GALACTIC NUCLEI; DISK GALAXIES; HOST GALAXIES; SECULAR EVOLUTION; STELLAR MASS; LOW-REDSHIFT AB We developed a hierarchical Bayesian model (HBM) to investigate how the presence of Seyfert activity relates to their environment, herein represented by the galaxy cluster mass, M-200, and the normalized cluster centric distance, r/r(200). We achieved this by constructing an unbiased sample of galaxies from the Sloan Digital Sky Survey, with morphological classifications provided by the Galaxy Zoo Project. A propensity score matching approach is introduced to control the effects of confounding variables: stellar mass, galaxy colour, and star formation rate. The connection between Seyfert-activity and environmental properties in the de-biased sample is modelled within an HBM framework using the so-called logistic regression technique, suitable for the analysis of binary data (e.g. whether or not a galaxy hosts an AGN). Unlike standard ordinary least square fitting methods, our methodology naturally allows modelling the probability of Seyfert-AGN activity in galaxies on their natural scale, i.e. as a binary variable. Furthermore, we demonstrate how an HBM can incorporate information of each particular galaxy morphological type in an unified framework. In elliptical galaxies our analysis indicates a strong correlation of Seyfert-AGN activity with r/r(200), and a weaker correlation with the mass of the host cluster. In spiral galaxies these trends do not appear, suggesting that the link between Seyfert activity and the properties of spiral galaxies are independent of the environment. C1 [de Souza, R. S.] MTA Eotvos Univ, EIRSA Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary. [Dantas, M. L. L.; Coelho, P.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, R Matao 1226, BR-05508090 Sao Paulo, Brazil. [Krone-Martins, A.] Univ Lisbon, Fac Ciencias, CENTRA SIM, Ed C8, P-1749016 Lisbon, Portugal. [Cameron, E.] Univ Oxford, Dept Zool, Tinbergen Bldg,S Parks Rd, Oxford OX1 3PS, England. [Hattab, M. W.] Virginia Commonwealth Univ, Ctr Biomarker Res & Personalized Med, Richmond, VA USA. [de Val-Borro, M.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Hilbe, J. M.] Arizona State Univ, Dept Stat, Sch SFD, Tempe, AZ USA. [Elliott, J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Hagen, A.] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RP de Souza, RS (reprint author), MTA Eotvos Univ, EIRSA Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary. EM rafael@caesar.elte.hu; maria.luiza.dantas@usp.br OI Coelho, Paula/0000-0003-1846-4826; Hagen, Alex/0000-0003-2031-7737; Krone-Martins, Alberto/0000-0002-2308-6623 FU Imperial Centre for Inference and Cosmology (ICIC), Imperial College of London, UK; Mullard Space Science Laboratory (MSSL) at the University College of London, UK FX This work is a product of the 2nd COIN Residence Program. We thank Alan Heavens and Jason McEwen for encouraging the realization of this edition. We thank E. E. O. Ishida, L. Dobos, R. Beck, B. Kocsis, and B. Villarroel for the fruitful discussions and suggestions. A particular thank goes for M. Trevisan for kindly providing the data set used in this work and for participating in several discussions. We thank the anonymous referee for the constructive suggestions and comments. The program was held in the Isle of Wight, UK in October/2015 and supported by the Imperial Centre for Inference and Cosmology (ICIC), Imperial College of London, UK, and by the Mullard Space Science Laboratory (MSSL) at the University College of London, UK. The IAA Cosmostatistics Initiative9 (COIN) is a non-profit organization whose aim is to nourish the synergy between astrophysics, cosmology, statistics, and machine learning communities. This work was written on the collaborative OVERLEAF platform,10 made use of GITHUB11 a web-based hosting service and git version control software, DATAJOY12 an on-line collaborative programming platform for PYTHON and R users, and SLACK13 a team collaboration platform. NR 112 TC 2 Z9 2 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 11 PY 2016 VL 461 IS 2 BP 2115 EP 2125 DI 10.1093/mnras/stw1459 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DV9PP UT WOS:000383273600073 ER PT J AU MacGregor, MA Lawler, SM Wilner, DJ Matthews, BC Kennedy, GM Booth, M Di Francesco, J AF MacGregor, Meredith A. Lawler, Samantha M. Wilner, David J. Matthews, Brenda C. Kennedy, Grant M. Booth, Mark Di Francesco, James TI ALMA OBSERVATIONS OF THE DEBRIS DISK OF SOLAR ANALOG tau CETI SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (tau Ceti); submillimeter: planetary systems ID MAIN-SEQUENCE STARS; EPSILON-ERIDANI; ALPHA CENTAURI; 1ST DETECTION; KUIPER-BELT; SYSTEM; DUST; MILLIMETER; INTERFEROMETRY; SIMULATIONS AB We present 1.3 mm observations of the Sun-like star tau Ceti with the Atacama Large Millimeter/submillimeter Array that probe angular scales of similar to 1 '' (4 au). This first interferometric image of the tau Ceti system, which hosts both a debris disk and a. possible multiplanet system, shows emission from a nearly face-on belt of cold dust with a position angle of 90 degrees surrounding an unresolved central source at the stellar position. To characterize this emission structure, we fit parametric models to the millimeter visibilities. The resulting best-fit model yields an inner belt edge of 6.2(-4.6)(+9.8) au, consistent with inferences from lower resolution, far-infrared Herschel observations. While the limited data at sufficiently short baselines preclude us from placing stronger constraints on the belt properties and its relation to the proposed five planet system, the observations do provide a strong lower limit on the fractional width of the belt, Delta R/R > 0.75 with 99% confidence. This fractional width is more similar to broad disks such as HD 107146 than narrow belts such as the Kuiper Belt and Fomalhaut. The unresolved central source has a higher flux density than the predicted flux of the stellar photosphere at 1.3 mm. Given previous measurements of an excess by a factor of similar to 2 at 8.7 mm, this emission is likely due to a hot stellar chromosphere. C1 [MacGregor, Meredith A.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Lawler, Samantha M.; Matthews, Brenda C.; Di Francesco, James] Natl Res Council Canada, Herzberg Astron & Astrophys Program, Victoria, BC V9E 2E7, Canada. [Matthews, Brenda C.; Di Francesco, James] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 2Y2, Canada. [Kennedy, Grant M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Booth, Mark] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. RP MacGregor, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI MacGregor, Meredith/0000-0001-7891-8143 FU National Science Foundation Graduate Research Fellowship [DGE1144152]; NRC Canada Plaskett Fellowship; Natural Science and Engineering Research Council (NSERC) Discovery Accelerator Supplement grant; Royal Society; FONDECYT Postdoctral Fellowship [3140479]; Millennium Science Initiative (Chilean Ministry of Economy) [RC130007] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00588.S. ALMA is a partnership of ESO (representing its member states), NSF (USA),. and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M.A.M. acknowledges support from a National Science Foundation Graduate Research Fellowship (DGE1144152). S.M.L. gratefully acknowledges support from the NRC Canada Plaskett Fellowship. B.C.M. acknowledges support from a Natural Science and Engineering Research Council (NSERC) Discovery Accelerator Supplement grant. G.M.K. is supported by the Royal Society as a Royal Society University Research Fellow. M.B. acknowledges support from a FONDECYT Postdoctral Fellowship, project no. 3140479 and the Millennium Science Initiative (Chilean Ministry of Economy), through grant RC130007. NR 35 TC 1 Z9 1 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2016 VL 828 IS 2 AR 113 DI 10.3847/0004-637X/828/2/113 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DY8HU UT WOS:000385371000004 ER PT J AU Feng, SY Beuther, H Zhang, QZ Liu, HB Zhang, ZY Wang, K Qiu, KP AF Feng, Siyi Beuther, Henrik Zhang, Qizhou Liu, Hauyu Baobab Zhang, Zhiyu Wang, Ke Qiu, Keping TI OUTFLOW DETECTION IN A 70 mu m DARK HIGH-MASS CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: lines and bands; stars: formation; stars: massive; submillimeter: ISM ID STAR-FORMATION; SIO EMISSION; SUBMILLIMETER ARRAY; HIERARCHICAL FRAGMENTATION; PHYSICAL-PROPERTIES; EVOLUTIONARY STAGES; MOLECULAR OUTFLOWS; CLOUD G28.34+0.06; NH3 OBSERVATIONS; EARLIEST PHASES AB We present observations toward a high-mass (>40 M-circle dot), low-luminosity (<10 L-circle dot) 70 mu m dark molecular core G28.34 S-A at 3.4 mm, using the IRAM 30 m telescope and the NOEMA interferometer. We report the detection of SiO J = 2 -> 1 line emission, which is spatially resolved in this source at a linear resolution of similar to 0.1 pc, while the 3.4 mm continuum image does not resolve any internal sub-structures. The SiO emission exhibits two W-E oriented lobes centering on the continuum peak. Corresponding to the redshifted and blueshifted gas with velocities up to 40 km s(-1) relative to the quiescent cloud, these lobes clearly indicate the presence of a strong bipolar outflow from this 70 mu m dark core, a source previously considered as one of the best candidates of "starless" core. Our SiO detection is consistent with ALMA archival data of SiO J = 5 -> 4, whose high-velocity blueshifted gas reveals a more compact lobe spatially closer to the dust center. This outflow indicates that the central source may be in an early evolutionary stage of forming a high-mass protostar. We also find that the low-velocity components (in the range of Vlsr(-5)(+3) km s(-1)) have an extended, NW-SE oriented distribution. Discussing the possible accretion scenarios of the outflow-powering young stellar object, we argue that molecular line emission and the molecular outflows may provide a better indication of the accretion history of the forming young stellar object, than snapshot observations of the present bolometric luminosity. This is particularly significant for cases of episodic accretion, which may occur during the collapse of the parent molecular core. C1 [Feng, Siyi] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Feng, Siyi; Beuther, Henrik] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Liu, Hauyu Baobab; Zhang, Zhiyu; Wang, Ke] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Zhang, Zhiyu] Univ Edinburgh, Inst Astron, Royal Observ, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. [Qiu, Keping] Nanjing Univ, Sch Astron & Space Sci, 22 Hankou Rd, Nanjing 210093, Jiangsu, Peoples R China. [Qiu, Keping] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. RP Feng, SY (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany.; Feng, SY (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM syfeng@mpe.mpg.de FU European Research Council (ERC) in the form of Advanced Grant, COSMICISM; German Research Foundation (DFG) through the priority program ("Physics of the Interstellar Medium") [1573, WA3628-1/1] FX Z.Y.Z. acknowledges support from the European Research Council (ERC) in the form of Advanced Grant, COSMICISM. K.W. acknowledges support from grant WA3628-1/1 of the German Research Foundation (DFG) through the priority program 1573 ("Physics of the Interstellar Medium"). NR 83 TC 0 Z9 0 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2016 VL 828 IS 2 AR 100 DI 10.3847/0004-637X/828/2/100 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX2XU UT WOS:000384237800006 ER PT J AU Kite, ES Fegley, B Schaefer, L Gaidos, E AF Kite, Edwin S. Fegley, Bruce, Jr. Schaefer, Laura Gaidos, Eric TI ATMOSPHERE-INTERIOR EXCHANGE ON HOT, ROCKY EXOPLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: individual (Kepler-10 b, CoRoT-7 b, KIC 12557548 b, 55 Cnc e, HD 219134 b) ID MASS-RADIUS RELATIONSHIPS; IN SUPER-EARTHS; RAYLEIGH-TAYLOR INSTABILITY; KIC 12557548 B; TERRESTRIAL PLANETS; SILICATE MELTS; CORE FORMATION; SOLAR-SYSTEM; ISOTOPIC FRACTIONATION; MANTLE CONVECTION AB We provide estimates of atmospheric pressure and surface composition on short-period, rocky exoplanets with dayside magma pools and silicate-vapor atmospheres. Atmospheric pressure tends toward vapor-pressure equilibrium with surface magma, and magma-surface composition is set by the competing effects of fractional vaporization and surface-interior exchange. We use basic models to show how surface-interior exchange is controlled by the planet's temperature, mass, and initial composition. We assume that mantle rock undergoes bulk melting to form the magma pool, and that winds flow radially away from the substellar point. With these assumptions, we find that: (1) atmosphere-interior exchange is fast when the planet's bulk-silicate FeO concentration is low, and slow when the planet's bulk-silicate FeO concentration is high; (2) magma pools are compositionally well mixed for substellar temperatures less than or similar to 2400 K, but compositionally variegated and rapidly variable for substellar temperatures less than or similar to 2400 K; (3) currents within the magma pool tend to cool the top of the solid mantle ("tectonic refrigeration"); (4) contrary to earlier work, many magma planets have time-variable surface compositions. C1 [Kite, Edwin S.] Univ Chicago, Chicago, IL 60637 USA. [Fegley, Bruce, Jr.] Washington Univ, Planetary Chem Lab, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. [Fegley, Bruce, Jr.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Schaefer, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaidos, Eric] Univ Hawaii Manoa, Honolulu, HI 96822 USA. RP Kite, ES (reprint author), Univ Chicago, Chicago, IL 60637 USA. EM kite@uchicago.edu OI Schaefer, Laura/0000-0003-2915-5025 FU NSF [AST-1412175]; Astrophysics and Geosciences Departments at Princeton University FX We thank Bruce Buffett, Michael Manga, Ruth Murray-Clay, Paul Asimow, Larry Grossman, Diana Dragomir, Valeri Makarov, Dorian Abbot, Michael Efroimsky, Ray Pierrehumbert, Eric Ford, Bethany Ehlmann, Brice-Olivier Demory, and especially Jacob Bean and Malte Jansen for discussions. We thank the anonymous reviewer and the editor, Steinn Sigurdsson. B.F. was supported by NSF grant AST-1412175. E.S.K. thanks the Astrophysics and Geosciences Departments at Princeton University for providing financial support and a convivial home while the ideas in this paper were marinating. NR 243 TC 1 Z9 1 U1 16 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2016 VL 828 IS 2 AR 80 DI 10.3847/0004-637X/828/2/80 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX0XE UT WOS:000384089000007 ER PT J AU Nicholl, M Berger, E Margutti, R Chornock, R Blanchard, PK Jerkstrand, A Smartt, SJ Arcavi, I Challis, P Chambers, KC Chen, TW Cowperthwaite, PS Gal-Yam, A Hosseinzadeh, G Howell, DA Inserra, C Kankare, E Magnier, EA Maguire, K Mazzali, PA McCully, C Milisavljevic, D Smith, KW Taubenberger, S Valenti, S Wainscoat, RJ Yaron, O Young, DR AF Nicholl, M. Berger, E. Margutti, R. Chornock, R. Blanchard, P. K. Jerkstrand, A. Smartt, S. J. Arcavi, I. Challis, P. Chambers, K. C. Chen, T. -W. Cowperthwaite, P. S. Gal-Yam, A. Hosseinzadeh, G. Howell, D. A. Inserra, C. Kankare, E. Magnier, E. A. Maguire, K. Mazzali, P. A. McCully, C. Milisavljevic, D. Smith, K. W. Taubenberger, S. Valenti, S. Wainscoat, R. J. Yaron, O. Young, D. R. TI SUPERLUMINOUS SUPERNOVA SN 2015bn IN THE NEBULAR PHASE: EVIDENCE FOR THE ENGINE-POWERED EXPLOSION OF A STRIPPED MASSIVE STAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual (2015bn) ID GAMMA-RAY BURSTS; CORE COLLAPSE SUPERNOVAE; 25 APRIL 1998; LIGHT CURVES; LUMINOUS SUPERNOVAE; MAGNETAR BIRTH; IC SUPERNOVAE; HOST GALAXIES; SPECTRA; SPECTROSCOPY AB We present nebular-phase imaging and spectroscopy for the hydrogen-poor superluminous supernova (SLSN) SN 2015bn, at redshift z = 0.1136, spanning +250-400 days after maximum light. The light curve exhibits a steepening in the decline rate from 1.4 mag (100 days)(-1) to 1.7 mag (100 days)(-1), suggestive of a significant decrease in the opacity. This change is accompanied by a transition from a blue continuum superposed with photospheric absorption lines to a nebular spectrum dominated by emission lines of oxygen, calcium, and magnesium. There are no obvious signatures of circumstellar interaction or large Ni-56 mass. We show that the spectrum at +400 days is virtually identical to a number of energetic SNe Ic such as SN 1997dq, SN 2012au, and SN 1998bw, indicating similar core conditions and strengthening the link between "hypernovae"/long gamma-ray bursts and SLSNe. A single explosion mechanism may unify these events that span absolute magnitudes of -22 < M-B < -17. Both the light curve and spectrum of SN 2015bn are consistent with an engine-driven explosion ejecting 7-30 M-circle dot of oxygen-dominated ejecta (for reasonable choices in temperature and opacity). A strong and relatively narrow O I lambda 7774 line, seen in a number of these energetic events but not in normal supernovae, may point to an inner shell that is the signature of a central engine. C1 [Nicholl, M.; Berger, E.; Blanchard, P. K.; Challis, P.; Cowperthwaite, P. S.; Milisavljevic, D.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Margutti, R.] NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. [Chornock, R.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, 251B Clippinger Lab, Athens, OH 45701 USA. [Jerkstrand, A.; Smartt, S. J.; Inserra, C.; Kankare, E.; Maguire, K.; Smith, K. W.; Young, D. R.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Arcavi, I.; Hosseinzadeh, G.; Howell, D. A.; McCully, C.] Las Cumbres Observ Global Telescope, 6740 Cortona Dr,Suite 102, Goleta, CA 93111 USA. [Chambers, K. C.; Magnier, E. A.; Wainscoat, R. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Chen, T. -W.] Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. [Gal-Yam, A.; Yaron, O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Mazzali, P. A.] Liverpool John Moores Univ, Astrophys Res Inst, IC2,Liverpool Sci Pk,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England. [Mazzali, P. A.; Taubenberger, S.] Max Planck Inst Astron, Karl Schwarzschild Str 1, D-85748 Garching, Germany. [Taubenberger, S.] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. [Valenti, S.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. RP Nicholl, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM matt.nicholl@cfa.harvard.edu OI Chen, Ting-Wan/0000-0002-1066-6098; Chambers, Kenneth /0000-0001-6965-7789; Margutti, Raffaella/0000-0003-4768-7586 FU NASA from NEO Observation Program [NNX12AR65G, NNX14AM74G]; ERC [291222, 307260]; STFC [ST/I001123/1, ST/L000709/1]; Alexander von Humboldt Foundation of Germany; German Research Foundation [TRR33]; Ernest Rutherford Fellowship through STFC FX M.N. thanks the organizers and participants of STScI workshop "The Mysterious Connection Between SLSNe and GRBs" for stimulating discussions and Carlos Contreras for providing magnitudes to check GMOS flux calibration. Based on data from ESO as part of PESSTO (188.D-3003, 191.D-0935). PS1 is supported by NASA grants NNX12AR65G and NNX14AM74G from NEO Observation Program. S.J.S. acknowledges ERC grant 291222 and STFC grants ST/I001123/1 and ST/L000709/1. A.G.Y. acknowledges ERC grant 307260. K.M. acknowledges an Ernest Rutherford Fellowship through STFC. T.W.C. acknowledges the Sofia Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation of Germany. S.T. acknowledges support from TRR33 "The Dark universe" of the German Research Foundation. NR 50 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2016 VL 828 IS 2 AR L18 DI 10.3847/2041-8205/828/2/L18 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DX1BC UT WOS:000384099500002 ER PT J AU Moore, AFP Duffy, JE AF Moore, Althea F. P. Duffy, J. Emmett TI Foundation species identity and trophic complexity affect experimental seagrass communities SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article DE Chesapeake Bay; Ecosystem engineer; Foundation species; Functional redundancy; Ruppia maritima; Seagrass; Species redundancy; Zostera marina ID EELGRASS-ZOSTERA-MARINA; LOWER CHESAPEAKE BAY; SUBMERSED AQUATIC VEGETATION; COLUMN NITRATE ENRICHMENT; RECENT CLIMATE-CHANGE; RUPPIA-MARITIMA; TOP-DOWN; ECOSYSTEM CONSEQUENCES; STRUCTURAL COMPONENTS; ENVIRONMENTAL-FACTORS AB The abundance and species composition of marine foundation species is changing due to range expansion or contraction, with potentially important ecosystem-level consequences. In Chesapeake Bay, USA, warming is likely to favor the more heat and stress-tolerant Ruppia maritima (widgeongrass) over Zostera marina (eelgrass). Because of the key role of seagrasses in providing habitat and trophic support, it is important to determine whether the more stress-tolerant seagrass provides similar ecological functions to the species it may replace. We addressed how trophic control differs between communities associated with the 2 seagrass species in a mesocosm experiment. Grazing of epiphytic algae can benefit seagrasses over competing algae, and crustacean mesograzers are an important link for higher trophic levels. We manipulated seagrass density, species identity, and presence of grazers and predators, and examined the resulting communities of recruiting algae and invertebrates. Overall, predation was higher in Ruppia than in Zostera, although mesograzer species individually differed in their susceptibility to predation and response to seagrass species. The presence of grazers and predators had a greater overall effect on multivariate metrics of fouling community development than did seagrass species identity. Initial densities of seagrass and grazer species had interactive effects on some recruiting microalgae and tunicates. Differences in grazer composition and predation between seagrass species could have consequences for higher trophic levels that rely on fauna in seagrass beds. However, given the considerable effects of manipulated seagrass and mesograzer density on trophic interactions and the fouling community, it may be most important to consider the overall density and distribution of seagrass present, rather than seagrass species identity. Our results highlight the importance of testing redundancy in ecological functions among habitat-forming species. C1 [Moore, Althea F. P.; Duffy, J. Emmett] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Pt, VA 23062 USA. [Moore, Althea F. P.] Northeastern Univ, Ctr Marine Sci, 430 Nahant Rd, Nahant, MA 01908 USA. [Duffy, J. Emmett] Smithsonian Inst, Tennenbaum Marine Observ Network, POB 37012,NHB MRC 106, Washington, DC 20013 USA. RP Moore, AFP (reprint author), Coll William & Mary, Virginia Inst Marine Sci, Gloucester Pt, VA 23062 USA.; Moore, AFP (reprint author), Northeastern Univ, Ctr Marine Sci, 430 Nahant Rd, Nahant, MA 01908 USA. EM moore.alt@husky.neu.edu FU Virginia Institute of Marine Science of The College of William and Mary FX We thank J. Auslander, R. E. Blake, I. Clark, J. P. Richardson, R. Rivera, K. Sobocinski, and M. Whalen for assistance in the lab and field. We thank several anonymous reviewers for comments that significantly improved the manuscript. The Virginia Institute of Marine Science of The College of William and Mary provided funding for this project. NR 96 TC 0 Z9 0 U1 26 U2 26 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD SEP 8 PY 2016 VL 556 BP 105 EP 121 DI 10.3354/meps11785 PG 17 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA DX3AF UT WOS:000384244300008 ER EF