FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Vanderwel, MC Slot, M Lichstein, JW Reich, PB Kattge, J Atkin, OK Bloomfield, KJ Tjoelker, MG Kitajima, K AF Vanderwel, Mark C. Slot, Martijn Lichstein, Jeremy W. Reich, Peter B. Kattge, Jens Atkin, Owen K. Bloomfield, Keith J. Tjoelker, Mark G. Kitajima, Kaoru TI Global convergence in leaf respiration from estimates of thermal acclimation across time and space SO NEW PHYTOLOGIST LA English DT Article DE autotrophic respiration; carbon flux; climate change; temperature; terrestrial biosphere modelling; thermal acclimation ID CARBON-CYCLE FEEDBACK; PLANT RESPIRATION; TEMPERATURE-ACCLIMATION; SOUTHERN-POPULATIONS; DARK RESPIRATION; PINUS-BANKSIANA; CLIMATE; MODEL; PHOTOSYNTHESIS; VEGETATION AB Recent compilations of experimental and observational data have documented global temperature-dependent patterns of variation in leaf dark respiration (R), but it remains unclear whether local adjustments in respiration over time (through thermal acclimation) are consistent with the patterns in R found across geographical temperature gradients. We integrated results from two global empirical syntheses into a simple temperature-dependent respiration framework to compare the measured effects of respiration acclimation-over-time and variation-across-space to one another, and to a null model in which acclimation is ignored. Using these models, we projected the influence of thermal acclimation on: seasonal variation in R; spatial variation in mean annual R across a global temperature gradient; and future increases in R under climate change. The measured strength of acclimation-over-time produces differences in annual R across spatial temperature gradients that agree well with global variation-across-space. Our models further project that acclimation effects could potentially halve increases in R (compared with the null model) as the climate warms over the 21st Century. Convergence in global temperature-dependent patterns of R indicates that physiological adjustments arising from thermal acclimation are capable of explaining observed variation in leaf respiration at ambient growth temperatures across the globe. C1 [Vanderwel, Mark C.] Univ Regina, Dept Biol, Regina, SK S4S 0A2, Canada. [Vanderwel, Mark C.; Slot, Martijn; Lichstein, Jeremy W.; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Slot, Martijn] Smithsonian Trop Res Inst, Balboa, Panama. [Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Reich, Peter B.; Tjoelker, Mark G.] Univ Western Sydney, Hawkesbury Inst Environm, Penrith, NSW 2751, Australia. [Kattge, Jens] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Atkin, Owen K.; Bloomfield, Keith J.] Australia Natl Univ, ARC Ctr Excellence Plant Energy Biol, Res Sch Biol, Canberra, ACT 2601, Australia. [Kitajima, Kaoru] Kyoto Univ, Div Forest & Biomat Sci, Kyoto 6068502, Japan. RP Vanderwel, MC (reprint author), Univ Regina, Dept Biol, Regina, SK S4S 0A2, Canada. EM mark.vanderwel@uregina.ca RI Kattge, Jens/J-8283-2016; Tjoelker, Mark/M-2413-2016; Atkin, Owen/C-8415-2009 OI Kattge, Jens/0000-0002-1022-8469; Tjoelker, Mark/0000-0003-4607-5238; Atkin, Owen/0000-0003-1041-5202 FU National Science Foundation (NSF-IOS) [1051789] FX We thank participants in the 8th New Phytologist Workshop on leaf respiration in large-scale vegetation models for valuable discussions that helped improve the final paper. We also thank three anonymous reviewers for their helpful comments. Funding for this project was provided by the National Science Foundation (NSF-IOS grant 1051789). NR 54 TC 9 Z9 9 U1 5 U2 53 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 SEP PY 2015 VL 207 IS 4 BP 1026 EP 1037 DI 10.1111/nph.13417 PG 12 WC Plant Sciences SC Plant Sciences GA CO2DP UT WOS:000358965800013 PM 25898850 ER PT J AU Geng, GN Zhang, Q Martin, RV van Donkelaar, A Huo, H Che, HZ Lin, JT He, KB AF Geng, Guannan Zhang, Qiang Martin, Randall V. van Donkelaar, Aaron Huo, Hong Che, Huizheng Lin, Jintai He, Kebin TI Estimating long-term PM2.5 concentrations in China using satellite-based aerosol optical depth and a chemical transport model SO REMOTE SENSING OF ENVIRONMENT LA English DT Article DE Particulate matter; Aerosol optical depth; Satellite remote sensing ID FINE PARTICULATE MATTER; GROUND-LEVEL PM2.5; CONTIGUOUS UNITED-STATES; AIR-POLLUTION; EASTERN CHINA; NORTH CHINA; MORTALITY; HAZE; MODIS; QUALITY AB Epidemiological and health impact studies of fine particulate matter (PM2.5) have been limited in China because of the lack of spatially and temporally continuous PM2.5 monitoring data. Satellite remote sensing of aerosol optical depth (ADD) is widely used in estimating ground-level PM2.5 concentrations. We improved the method for estimating long-term surface PM2.5 concentrations using satellite remote sensing and a chemical transport model, and derived PM2.5 concentrations over China for 2006-2012. We generated a map of surface PM2.5 concentrations at 0.1 degrees x 0.1 degrees over China using the nested-grid GEOS-Chem model, most recent bottom-up emission inventory, and satellite observations from the MODIS and MISR instruments. Aerosol vertical profiles from the space-based CALIOP lidar were used to adjust the climatological drivers of the bias in the simulated results, and corrections were made for incomplete sampling. We found significant spatial agreement between the satellite-derived PM2.5 concentrations and the ground-level PM2.5 measurements collected from literatures (r = 0.74, slope = 0.77, intercept = 1121 mu g/m(3)). The population-weighted mean of PM2.5 concentrations in China is 71 mu g/m(3) and more than one billion people live in locations where PM2.5 concentrations exceed the World Health Organization Air Quality Interim Target-1 of 35 mu g/m(3). The results from our work are substantially higher than previous work, especially in heavily polluted regions. The overall population-weighted mean uncertainty over China is 17.2 mu g/m(3), as estimated using ground-level AOD measurements and vertical profiles observed from CALIOP. (C) 2015 Elsevier Inc. All rights reserved. C1 [Geng, Guannan; Zhang, Qiang] Tsinghua Univ, Ctr Earth Syst Sci, Minist Educ Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China. [Geng, Guannan; Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Geng, Guannan; He, Kebin] Tsinghua Univ, Sch Environm, State Key Joint Lab Environm Simulat & Pollut Con, Beijing 100084, Peoples R China. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huo, Hong] Tsinghua Univ, Inst Energy Environm & Econ, Beijing 100084, Peoples R China. [Che, Huizheng] Chinese Acad Meteorol Sci, Inst Atmospher Composit, Key Lab Atmospher Chem LAC, Beijing 100081, Peoples R China. [Lin, Jintai] Peking Univ, Sch Phys, Dept Atmospher & Ocean Sci, Lab Climate & Ocean Atmosphere Studies, Beijing 100871, Peoples R China. RP Zhang, Q (reprint author), Tsinghua Univ, Ctr Earth Syst Sci, Minist Educ Key Lab Earth Syst Modeling, Beijing 100084, Peoples R China. EM qiangzhang@tsinghua.edu.cn RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Zhang, Qiang/D-9034-2012; Lin, Jintai/A-8872-2012; che, Huizheng/B-1354-2014 OI Martin, Randall/0000-0003-2632-8402; Lin, Jintai/0000-0002-2362-2940; che, Huizheng/0000-0002-9458-3387 FU National Science Foundation of China [41222036, 41275026, 71322304, 41175127]; Collaborative Innovation Center for Regional Environmental Quality; Natural Sciences and Engineering Research Council of Canada [5265-417449-12] FX This study was supported by the National Science Foundation of China (41222036, 41275026, 71322304, and 41175127). Q. Zhang and K. B. He are supported by the Collaborative Innovation Center for Regional Environmental Quality. The work at Dalhousie was supported by the Natural Sciences and Engineering Research Council of Canada (5265-417449-12). We thank the two anonymous reviewers for their constructive comments. NR 54 TC 22 Z9 22 U1 23 U2 111 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0034-4257 EI 1879-0704 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD SEP 1 PY 2015 VL 166 BP 262 EP 270 DI 10.1016/j.rse.2015.05.016 PG 9 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA CN7RU UT WOS:000358632500021 ER PT J AU Micheletti, T Brown, JL Walker, SL Cubas, ZS Furtado, PV Putman, SB de Moraes, W de Oliveira, MJ de Oliveira, CA Moreira, N AF Micheletti, Tatiane Brown, Janine L. Walker, Susan L. Cubas, Zalmir S. Furtado, Priscila V. Putman, Sarah B. de Moraes, Wanderlei de Oliveira, Marcos J. de Oliveira, Claudio A. Moreira, Nei TI The use of altrenogest to avoid hyperestrogenism after eCG-hCG ovulation induction in southern tigrina (Leopardus guttulus) SO THERIOGENOLOGY LA English DT Article DE Captive reproduction; Gonadotropin; Neotropical felid; Ovulation induction; Progestin ID ARTIFICIAL-INSEMINATION; DOMESTIC CAT; EXOGENOUS GONADOTROPINS; ENZYME-IMMUNOASSAY; OVARIAN ACTIVITY; CLOUDED LEOPARD; GNRH ANTAGONIST; FELIS-CATUS; EMBRYO; PROGESTERONE AB The goal of this study was to optimize an ovulation induction protocol for use with artificial insemination in the southern tigrina (Leopard us guttulus). The specific aims were to report the efficacy of using altrenogest, an oral progestin (Regumate, MSD Animal Health, Merck Animal Health), to suppress ovarian activity and prevent follicular hyperstimulation and hyperestrogenism after the administration of exogenous eCG and hCG. To monitor ovarian responses, fecal estrogen and progestogen metabolites were quantified by enzyme immunoassay in females before and after intramuscular administration of 200-IU eCG and 150-IU hCG in two trials, 4 months apart. During the first trial, there was no use of altrenogest, only the eCG-hCG ovulation induction protocol. In the second trial, the ovulation induction protocol was preceded by the administration of oral altrenogest for 14 days (minimum of 0.192 mg per kg per day). Altrenogest administration resulted in a suppression of follicular activity in three out of six females before eCG-hCG administration on the basis of lower mean estrogen concentrations (P < 0.05). It also resulted in four out of six females presenting lower fecal estrogen metabolite concentrations (P < 0.05) after ovulation induction, and two out of six individuals showed a reduction (P < 0.05) in postovulatory fecal progestogen metabolite concentrations, all when compared to the same female's cycles without the progestin. Fecal estrogen metabolite concentrations were closer to baseline in 50% of these individuals after altrenogest and eCG-hCG treatments when compared to basal concentrations before gonadotropins without the use of altrenogest. This study reported that use of altrenogest in southern tigrina can suppress ovarian, activity and avoid hyperestrogenism after administration of eCG and hCG treatment. However, not all females responded uniformly, so more studies are needed to increase the efficacy of ovulation induction for use with artificial insemination in this species. (C) 2015 Elsevier Inc. All rights reserved. C1 [Micheletti, Tatiane; Moreira, Nei] Univ Fed Parana, Dept Vet Med & Anim Sci, Palotina, Parana, Brazil. [Micheletti, Tatiane] Brazilian Inst Conservat Med TRIADE, Curitiba, Parana, Brazil. [Brown, Janine L.; Putman, Sarah B.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Walker, Susan L.] Chester Zoo, Reprod & Welf Res Unit, Upton By Chester, England. [Cubas, Zalmir S.; de Moraes, Wanderlei; de Oliveira, Marcos J.] Itaipu Binacl, Refugio Biol Bela Vista, Foz Do Iguacu, Parana, Brazil. [Furtado, Priscila V.; de Oliveira, Claudio A.] Univ Sao Paulo, Dept Anim Reprod, Lab Dosagens Hormonais, Sao Paulo, SP, Brazil. RP Micheletti, T (reprint author), Tech Univ Dresden, Inst Forstbot & Forstzool, Pienner Str 7 Cotta Bau, D-01737 Tharandt, Germany. EM micheletti@forst.tu-dresden.de FU Brazilian's National Council for Scientific and Technological Development FX The authors would like to acknowledge everyone that helped with this project, specially all the staff from Refugio Biologico Bela Vista at Itaipu Binacional, Laboratorio de Dosagens Hormonais (LDH-USP) and Smithsonian Conservation Biology Institute, and the colleagues Aline Rafaeli Hoffmann, Alcides Ricieri Rinaldi, Debora Tramujas Ballarotti, Jackson Wolf, Luiz Ernandes Kozicki, Patricia Cubas, Renata Carolina F. Santos, Rosana de Almeida, and Romildo Romualdo Weiss for the essential support during this project's execution. They also would like to acknowledge Brazilian's National Council for Scientific and Technological Development that partially funded the first author with a temporary masters' scholarship and Smithsonian Conservation Biology Institute that provided accommodation during the samples analyses. NR 30 TC 0 Z9 0 U1 1 U2 13 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 SEP 1 PY 2015 VL 84 IS 4 BP 575 EP 582 DI 10.1016/j.theriogenology.2015.04.015 PG 8 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA CO3DK UT WOS:000359036600013 PM 26001599 ER PT J AU Falcon-Lang, HJ Lucas, SG Kerp, H Krainer, K Montanez, IP Vachard, D Chaney, DS Elrick, SD Contreras, DL Kurzawe, F DiMichele, WA Looy, CV AF Falcon-Lang, Howard J. Lucas, Spencer G. Kerp, Hans Krainer, Karl Montanez, Isabel P. Vachard, Daniel Chaney, Dan S. Elrick, Scott D. Contreras, Dori L. Kurzawe, Francine DiMichele, William A. Looy, Cindy V. TI Early Permian (Asselian) vegetation from a seasonally dry coast in western equatorial Pangea: Paleoecology and evolutionary significance SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Permian; Estuary; Volrzian conifers; Callipterids; Mangrove; New Mexico ID PALEOZOIC ICE-AGE; CENTRAL NEW-MEXICO; CENTRAL APPALACHIAN BASIN; NORTH-CENTRAL TEXAS; SOUTHERN NEW-MEXICO; SMALLER FORAMINIFERS; SEQUENCE STRATIGRAPHY; ROBLEDO MOUNTAINS; RATTENDORF GROUP; TROPICAL FLORAS AB The Pennsylvanian-Permian transition has been inferred to be a time of significant glaciation in the Southern Hemisphere, the effects of which were manifested throughout the world. In the equatorial regions of Pangea, the response of terrestrial ecosystems was highly variable geographically, reflecting the interactions of polar ice and geographic patterns on atmospheric circulation. In general, however, there was a drying trend throughout most of the western and central equatorial belt. In western Pangea, the climate proved to be considerably more seasonally dry and with much lower mean annual rainfall than in areas in the more central and easterly portions of the supercontinent. Here we describe lower Permian (upper Asselian) fossil plant assemblages from the Community Pit Formation in Prehistoric Trackways National Monument near Las Cruces, south-central New Mexico, U.S.A. The fossils occur in sediments within a 140-m-wide channel that was incised into indurated marine carbonates. The channel filling can be divided into three phases. A basal channel, limestone conglomerate facies contains allochthonous trunks of walchian conifers. A middle channel fill is composed of mictitic limestone beds containing a brackish-to-marine fauna with carbon, oxygen and strontium isotopic composition that provide independent support for salinity inferences. The middle limestone also contains a (par)autochthonous adpressed megaflora co-dominated by voltzian conifers and the callipterid Lodevia oxydata. The upper portions of the channel are filled with muddy, gypsiferous limestone that lacks plant fossils. This is the geologically oldest occurrence of voltzian conifers. It also is the westernmost occurrence of L. oxydata, a rare callipterid known only from the Pennsylvanian-Permian transition in Poland, the Appalachian Basin and New Mexico. The presence of in situ fine roots within these channel-fill limestone beds and the taphonomic constraints on the incorporation of aerial plant remains into a lime mudstone indicate that the channel sediments were periodically colonized by plants, which suggests that these species were tolerant of salinity, making these plants one of, if not the earliest unambiguous mangroves. (C) 2015 Elsevier B.V. All rights reserved. C1 [Falcon-Lang, Howard J.; Kurzawe, Francine] Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [Falcon-Lang, Howard J.; Kerp, Hans] Univ Munster, Forsch Stelle Palaobot, Geol Palaontol Inst, D-48149 Munster, Germany. [Lucas, Spencer G.] New Mexico Museum Nat Hist & Sci, Albuquerque, NM 87104 USA. [Krainer, Karl] Univ Innsbruck, Inst Geol & Paleontol, A-6020 Innsbruck, Austria. [Montanez, Isabel P.] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Vachard, Daniel] Univ Lille 1, UMR Geosyst 8217, F-59655 Villeneuve Dascq, Ufr, France. [Chaney, Dan S.; DiMichele, William A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Elrick, Scott D.] Illinois State Geol Survey, Champaign, IL 61820 USA. [Contreras, Dori L.; Looy, Cindy V.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Contreras, Dori L.; Looy, Cindy V.] Univ Calif Berkeley, Museum Paleontol, Berkeley, CA 94720 USA. RP Looy, CV (reprint author), Univ Calif Berkeley, Dept Integrat Biol, 3060 Valley Life Sci Bldg, Berkeley, CA 94720 USA. EM looy@berkeley.edu FU Bureau of Land Management (BLM Las Cruces District Office) [BLM L09AC15951]; NERC at Royal Holloway, University of London [NE/F014120/2]; NSF [EAR1024737]; NSF GRF [DGE 1106400]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, Brazil) [202078/2011-6]; National Museum of Natural History Small Grants program; Hellman Fellowship; University of California Museum of Paleontology FX We thank the staff of the Bureau of Land Management (BLM Las Cruces District Office and Patricia Hester, formerly BLM Regional Paleontologist) for permitting access to PTNM, and for generous financial support of this project (BLM L09AC15951). Jerry MacDonald originally discovered the fossil wood locality described here. Thanks to Dave Osleger for comments on carbonate accumulating environments. HFL gratefully acknowledges a NERC Advanced Fellowship (NE/F014120/2) held at Royal Holloway, University of London, and field support from the New Mexico Museum of Natural History and Science. SGL gratefully acknowledges the field assistance of Larry Rinehart and Justin Spielmann. IPM acknowledges support from NSF (EAR1024737). This material is in part based upon work supported by the NSF GRF under Grant No. DGE 1106400 to DLC. FK gratefully acknowledges a Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, Brazil) Postdoctoral Fellowship (202078/2011-6). WAD acknowledges support from the National Museum of Natural History Small Grants program. CVL acknowledges support from the Hellman Fellowship and the University of California Museum of Paleontology. NR 126 TC 2 Z9 2 U1 3 U2 88 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 SEP 1 PY 2015 VL 433 BP 158 EP 173 DI 10.1016/j.palaeo.2015.05.010 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA CN5JU UT WOS:000358466400013 ER PT J AU Evans, LG Peplowski, PN McCubbin, FM Mccoy, TJ Nittler, LR Zolotov, MY Ebel, DS Lawrence, DJ Starr, RD Weider, SZ Solomon, SC AF Evans, Larry G. Peplowski, Patrick N. McCubbin, Francis M. McCoy, Timothy J. Nittler, Larry R. Zolotov, Mikhail Yu. Ebel, Denton S. Lawrence, David J. Starr, Richard D. Weider, Shoshana Z. Solomon, Sean C. TI Chlorine on the surface of Mercury: MESSENGER gamma-ray measurements and implications for the planet's formation and evolution SO ICARUS LA English DT Article DE Mercury, surface; Gamma-ray spectroscopy; Geological processes; Planetary formation ID ENSTATITE CHONDRITES; NEUTRON SPECTROMETER; LUNAR MANTLE; VOLCANISM; ELEMENTS; WATER; POTASSIUM; ABUNDANCE; SODIUM; ORIGIN AB Orbital measurements obtained by the MESSENGER Gamma-Ray Spectrometer have been analyzed to determine the surface abundance of chlorine in Mercury's northern hemisphere. The derived Cl/Si mass ratio is 0.0057 +/- 0.001, which for an assumed Si abundance of 24.6 wt% corresponds to 0.14 +/- 0.03 wt% Cl. The abundance of Cl is a factor of 2.9 +/- 1.3 higher in the north polar region (>80 degrees N) than at latitudes 0-60 degrees N, a latitudinal variation similar to that observed for Na. Our reported Cl abundances are consistent with measured bulk concentrations of neutron-absorbing elements on Mercury, particularly those observed at high northern latitudes. The Cl/K ratio on Mercury is chondritic, indicating a limited impact history akin to that of Mars, which accreted rapidly. Hypotheses for the origin of Mercury's high metal-to-silicate ratio must be able to reproduce Mercury's observed elemental abundances, including Cl. Chlorine is also an important magmatic volatile, and its elevated abundance in the northern polar region of Mercury indicates that it could have played a role in the production, ascent, and eruption of flood volcanic material in this region. We have identified several candidate primary mineralogical hosts for Cl on Mercury, including the halide minerals lawrencite (FeCl2), sylvite (KCl), and halite (NaCl), as well as Cl-bearing alkali sulfides. Amphiboles, micas, apatite, and aqueously deposited halides, in contrast, may be ruled out as mineralogical hosts of Cl on Mercury. (C) 2015 Elsevier Inc. All rights reserved. C1 [Evans, Larry G.] Comp Sci Corp, Lanham, MD 20706 USA. [Peplowski, Patrick N.; Lawrence, David J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [McCubbin, Francis M.] Univ New Mexico, Inst Meteorit, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [McCoy, Timothy J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Nittler, Larry R.; Weider, Shoshana Z.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Zolotov, Mikhail Yu.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Ebel, Denton S.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. RP Evans, LG (reprint author), Comp Sci Corp, Lanham, MD 20706 USA. EM Larry.G.Evans@nasa.gov RI Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015 OI Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667 FU NASA [NAS5-97271, NASW-0002, NNX14AK43G, NNX10AI42G]; MESSENGER Participating Scientist Program FX This work was supported by the NASA Discovery Program under contracts NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-0002 to the Carnegie Institution of Washington. All of the data used in the present study are available in the Planetary Data System (PDS). Support was also provided to LGE, DJL, LRN, and RDS by the MESSENGER Participating Scientist Program. FMM and DSE acknowledge support from the NASA Cosmochemistry Program during this study (through grants NNX14AK43G and NNX10AI42G, respectively). We especially thank the dedicated MESSENGER operations team for their continued support of this mission. NR 73 TC 8 Z9 8 U1 2 U2 20 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 SEP 1 PY 2015 VL 257 BP 417 EP 427 DI 10.1016/j.icarus.2015.04.039 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN0KA UT WOS:000358101300033 ER PT J AU de Queiroz, LP Pastore, JFB Cardoso, D Snak, C Lima, ALD Gagnon, E Vatanparast, M Holland, AE Egan, AN AF de Queiroz, Luciano Paganucci Pastore, Jose Floriano B. Cardoso, Domingos Snak, Cristiane Lima, Ana Luisa de C. Gagnon, Edeline Vatanparast, Mohammad Holland, Ailsa E. Egan, Ashley N. TI A multilocus phylogenetic analysis reveals the monophyly of a recircumscribed papilionoid legume tribe Diocleae with well-supported generic relationships SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Leguminosae; Papilionoideae; Phaseoleae; Phylogeny; Diocleinae ID INTERNAL TRANSCRIBED SPACERS; NUCLEAR RIBOSOMAL DNA; CHLOROPLAST DNA; SUBTRIBE DIOCLEINAE; FIELD PRESERVATION; LEGUMINOSAE; FABACEAE; SEQUENCES; PHASEOLEAE; POLLINATION AB Deciphering the phylogenetic relationships within the species-rich Millettioid clade has persisted as one of the major challenges in the systematics and evolutionary history of papilionoid legumes (Leguminosae, Papilionoideae). Historically, the predominantly neotropical lianas of subtribe Diocleinae in the Millettioid legumes have been taxonomically tangled together with the largely heterogeneous tribe Phaseoleae. This work presents a comprehensive molecular phylogenetic analysis based on nuclear and chloroplast markers and includes all genera ever referred to Diocleae except for the monospecific Philippine Luzonia, resolving several key generic relationships within the Millettioid legumes. The first of two separate analyses includes 310 matK accessions and strongly supports the reestablishment of tribe Diocleae as a branch of the Millettioid clade. This work sheds greater light on the higher-level phylogeny of Diocleae and allows the recognition of three major lineages: the Canavalia, Dioclea, and Galactia clades. The second set of phylogenetic analyses utilized nuclear (ITS/5.8S and ETS) and plastid (matK and tmT-Y) DNA sequences to reveal (i) the monophyly of Canavalia and Cleobulia; (ii) the monophyly of Bionia with the exclusion of Bionia belle; (iii) the paraphyly of Dioclea with respect to Cleobulia, Cymbosema, and Macropsychanthus; (iv) the paraphyly of Cratylia with respect to the broadly polyphyletic Camptosema; and (v) the polyphyly of Galactia with species scattered widely across the tree. (C) 2015 Elsevier Inc. All rights reserved. C1 [de Queiroz, Luciano Paganucci; Pastore, Jose Floriano B.; Cardoso, Domingos; Snak, Cristiane; Lima, Ana Luisa de C.] Univ Estadual Feira de Santana, Dept Ciencias Biol, BR-44036900 Feira De Santana, BA, Brazil. [Cardoso, Domingos] Univ Fed Bahia, Inst Biol, Dept Bot, BR-40170115 Salvador, BA, Brazil. [Gagnon, Edeline] Univ Montreal, Inst Rech Biol Vegetale, Dept Sci Biol, Montreal, PQ H1X 2B2, Canada. [Vatanparast, Mohammad; Egan, Ashley N.] Smithsonian Inst, Washington, DC 20013 USA. [Vatanparast, Mohammad] Chiba Univ, Grad Sch Sci, Dept Biol, Inage Ku, Chiba, Japan. [Holland, Ailsa E.] Queensland Herbarium, Brisbane Bot Gardens, Toowong, Qld 4066, Australia. RP de Queiroz, LP (reprint author), Univ Estadual Feira de Santana, Dept Ciencias Biol, Ave Transnordestina S-N, BR-44036900 Feira De Santana, BA, Brazil. EM luciano.paganucci@gmail.com RI de Queiroz, Luciano Paganucci/I-1378-2012; Cardoso, Domingos/D-1304-2014 OI de Queiroz, Luciano Paganucci/0000-0001-7436-0939; Cardoso, Domingos/0000-0001-7072-2656 FU Programa de Pesquisa em Biodiversidade do Semi-arido (PPBIO); Sistema Nacional de Pesquisa em Biodiversidade [SISBIOTA CNPq 563084/2010-3/FAPESB PES0053/2011]; PRONEX [FAPESB PNX0014/2009]; REFLORA [CNPq 563546/2010-7/FAPESB PES0054/2011]; CNPq Edital Universal [Process 473526/2011-5]; FAPESB [Process PET0039/2012]; Pq/CNPq; PDJ/CNPq FX We thank to John Gwaltney and Charles Bryson for providing leaf material of Lackeya multiflora from USA; Roger Graveson for the leaf material of Galactia longiflora from Saint Lucia; Roberto Salas for leaf material of Dioclea burkartii and D. paraguariensis from Argentina; Abel Conceicao for leaf material of Rhodopis planisiliqua from Dominican Republic; Elvia Souza, Patricia Jesus, M. Torres, Laura Lima, Haroldo Lima, Cassio van den Berg, Jomar Jardim, and Rafaela Forzza for the leaf material of several species from Brazil. Jefferson G. Carvalho-Sobrinho, Petala Ribeiro, Francisco Haroldo Nascimento, Ricardo Machado, Raymond Harley, Ana Maria Giulietti-Harley (UEFS), Charles Zartman (INPA), Elsa Cabral, Roberto Salas, and Andrea Cabanas (IBONE, Argentina) provided help and support during fieldwork. Seeds of species of Dioclea and Galactia from the forage germplasm collection were provided by the Centro Internacional de Agricultura Tropical (CAT, Cali, Colombia) and the transference of seeds to Brazil was kindly arranged by Luis Guillermo Santos Melendez (CAT, Programa de Recursos Geneticos), Marcelo Fragomeni Simon, and Manuela Oliveira (Embrapa, Centro Nacional de Recursos Geneticos e Biotecnologia, Brazil). DNA extraction from herbarium material of Macropsychanthus and some North-American species of Galactia was kindly allowed by Gwil Lewis (K) and Matt Lavin (MONT). Fieldwork and DNA sequencing were sponsored by Programa de Pesquisa em Biodiversidade do Semi-arido (PPBIO), Sistema Nacional de Pesquisa em Biodiversidade (SISBIOTA CNPq 563084/2010-3/FAPESB PES0053/2011), PRONEX (FAPESB PNX0014/2009), REFLORA (CNPq 563546/2010-7/FAPESB PES0054/2011), and CNPq Edital Universal (Process 473526/2011-5). DC also acknowledges FAPESB (Process PET0039/2012) for providing financial support to his research on phylogenetics. LPQ is continuously supported by a Pq/CNPq fellowship and DC and JFBP were supported by PDJ/CNPq fellowships while postdocs at Universidade Estadual de Feira de Santana. NR 104 TC 2 Z9 2 U1 3 U2 20 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 SEP PY 2015 VL 90 BP 1 EP 19 DI 10.1016/j.ympev.2015.04.016 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CM8PW UT WOS:000357965100001 PM 25934529 ER PT J AU Glowska, E Laniecka, I Milensky, CM AF Glowska, Eliza Laniecka, Izabella Milensky, Christopher M. TI Two new picobiin mite species (Acari: Cheyletoidea: Syringophilidae) parasitizing passerine birds in Guyana SO ACTA PARASITOLOGICA LA English DT Article DE Quill mites; Syringophilidae; Neopicobia; Rafapicobia; ectoparasites; systematics AB Two new picobiin mite species (Cheyletoidea: Syringophilidae) are described from passeriform birds in Guyana, Rafapicobia automoli sp. nov. parasitizing two furnariid species Automolus ochrolaemus (Tschudi) (type host) and Automolus rufipileatus (Pelzeln) (Passeriformes: Furnariidae) and Neopicobia herbicolae sp. nov. from Emberizoides herbicola (Vieillot) (Thraupidae). Additionally, Picumnus exilis (Lichtenstein) (Piciformes: Picidae) is recorded as a new host species for Neopicobia hepburni Glowska et Laniecka, 2014. C1 [Glowska, Eliza; Laniecka, Izabella] Adam Mickiewicz Univ, Dept Anim Morphol, Fac Biol, PL-61614 Poznan, Poland. [Milensky, Christopher M.] Smithsonian Inst, Div Birds, Washington, DC 20013 USA. RP Glowska, E (reprint author), Adam Mickiewicz Univ, Dept Anim Morphol, Fac Biol, Umultowska 89, PL-61614 Poznan, Poland. EM glowska@amu.edu.pl NR 13 TC 0 Z9 0 U1 1 U2 3 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 1230-2821 EI 1896-1851 J9 ACTA PARASITOL JI Acta Parasitolog. PD SEP PY 2015 VL 60 IS 3 BP 488 EP 493 DI 10.1515/ap-2015-0069 PG 6 WC Parasitology SC Parasitology GA CK6MC UT WOS:000356341200019 PM 26204188 ER PT J AU Foster, BL Ao, M Willoughby, C Soenjaya, Y Holm, E Lukashova, L Tran, AB Wimer, HF Zerfas, PM Nociti, FH Kantovitz, KR Quan, BD Sone, ED Goldberg, HA Somerman, MJ AF Foster, B. L. Ao, M. Willoughby, C. Soenjaya, Y. Holm, E. Lukashova, L. Tran, A. B. Wimer, H. F. Zerfas, P. M. Nociti, F. H., Jr. Kantovitz, K. R. Quan, B. D. Sone, E. D. Goldberg, H. A. Somerman, M. J. TI Mineralization defects in cementum and craniofacial bone from loss of bone sialoprotein SO BONE LA English DT Article DE Extracellular matrix; Mineralization; Bone; Cementum; Dentin; Cartilage ID DENTIN MATRIX PROTEIN-1; EXTRINSIC FIBER CEMENTUM; IN-VITRO; HYDROXYAPATITE FORMATION; MOUSE MODEL; SKELETAL MINERALIZATION; PERIODONTAL ATTACHMENT; EXTRACELLULAR-MATRIX; ACELLULAR CEMENTUM; SIBLING PROTEINS AB Bone sialoprotein (BSP) is a multifunctional extracellular matrix protein found in mineralized tissues, including bone, cartilage, tooth root cementum (both acellular and cellular types), and dentin. In order to define the role BSP plays in the process of biomineralization of these tissues, we analyzed cementogenesis, dentinogenesis, and osteogenesis (intramembranous and endochondral) in craniofacial bone in Bsp null mice and wild-type (WT) controls over a developmental period (1-60 days post natal; dpn) by histology, immunohistochemistry, undecalcified histochemistry, microcomputed tomography (microCT), scanning electron microscopy (SEM), transmission electron microscopy (TEM), and quantitative PCR (qPCR). Regions of intramembranous ossification in the alveolus, mandible, and calvaria presented delayed mineralization and osteoid accumulation, assessed by von Kossa and Goldner's trichrome stains at 1 and 14 dpn. Moreover, Bsp(-/-) mice featured increased cranial suture size at the early time point, 1 dpn. Immunostaining and PCR demonstrated that osteoblast markers, osterix, alkaline phosphatase, and osteopontin were unchanged in Bsp null mandibles compared to WT. Bsp(-/-) mouse molars featured a lack of functional acellular cementum formation by histology, SEM, and TEM, and subsequent loss of Sharpey's collagen fiber insertion into the tooth root structure. Bsp(-/-) mouse alveolar and mandibular bone featured equivalent or fewer osteoclasts at early ages (1 and 14 dpn), however, increased RANKL immunostaining and mRNA, and significantly increased number of osteodast-like cells (2-5 fold) were found at later ages (26 and 60 dpn), corresponding to periodontal breakdown and severe alveolar bone resorption observed following molar teeth entering occlusion. Dentin formation was unperturbed in Bsp(-/-) mouse molars, with no delay in mineralization, no alteration in dentin dimensions, and no differences in odontoblast markers analyzed. No defects were identified in endochondral ossification in the cranial base, and craniofacial morphology was unaffected in Bsp(-/-) mice. These analyses confirm a critical role for BSP in processes of cementogenesis and intramembranous ossification of craniofacial bone, whereas endochondral ossification in the cranial base was minimally affected and dentinogenesis was normal in Bsp(-/-) molar teeth. Dissimilar effects of loss of BSP on mineralization of dental and craniofacial tissues suggest local differences in the role of BSP and/or yet to be defined interactions with site-specific factors. Published by Elsevier Inc. C1 [Foster, B. L.; Ao, M.; Willoughby, C.; Tran, A. B.; Nociti, F. H., Jr.; Kantovitz, K. R.; Somerman, M. J.] Natl Inst Arthrit & Musculoskeletal & Skin Dis NI, NIH, Bethesda, MD 20892 USA. [Willoughby, C.; Goldberg, H. A.] Univ Western Ontario, Biomed Engn Program, Schulich Sch Med & Dent, London, ON N6A 5C1, Canada. [Holm, E.; Goldberg, H. A.] Univ Western Ontario, Dept Biochem, Schulich Sch Med & Dent, London, ON N6A 5C1, Canada. [Lukashova, L.] Hosp Special Surg, New York, NY 10021 USA. [Wimer, H. F.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. [Zerfas, P. M.] Off Res Serv, NIH, Div Vet Resources, Bethesda, MD 20892 USA. [Nociti, F. H., Jr.] Univ Estadual Campinas, Sch Dent, Div Periodont, Dept Prosthodont & Periodont, BR-13414903 Piracicaba, SP, Brazil. [Kantovitz, K. R.] Univ Estadual Campinas, Dept Pediat Dent, Sch Dent, BR-13414903 Piracicaba, SP, Brazil. [Quan, B. D.; Sone, E. D.] Univ Toronto, Inst Biomat & Biomed Engn, Toronto, ON M5S 3G9, Canada. [Sone, E. D.] Univ Toronto, Dept Mat Sci & Engn, Toronto, ON M5S 3G9, Canada. [Sone, E. D.] Univ Toronto, Fac Dent, Toronto, ON M5S 3G9, Canada. [Goldberg, H. A.] Univ Western Ontario, Sch Dent, Schulich Sch Med & Dent, London, ON N6A 5C1, Canada. RP Foster, BL (reprint author), Natl Inst Arthrit & Musculoskeletal & Skin Dis NI, NIH, Bldg 50 Room 4120, Bethesda, MD 20892 USA. EM brian.foster@nih.gov; fnu.aomin@nih.gov; chelseawilloughby15@gmail.com; yosoenjay@uwo.ca; eholm@uwa.ca; lukashoval@hss.edu; anne.tran2@nih.gov; helen.wimer@nih.gov; patricia.zerfas@nih.gov; nociti@unicamp.br; kamilark@yahoo.com.br; bryan.quan@utoronto.ca; eli.sone@utotonto.ca; hagoldbe@uwo.ca; Martha.somerman@nih.gov RI Foster, Brian/H-8375-2015; Kantovitz, Kamila/J-4567-2013 OI Foster, Brian/0000-0003-3444-0576; Kantovitz, Kamila/0000-0003-2045-7924 FU National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS)/NIH [AR 066110]; Intramural Research Program of NIAMS; Canadian Institutes of Health Research [130572]; CIHR Institute of Musculoskeletal Health and Arthritis [134216] FX This research was supported by sources including grant AR 066110 to BLF from the National Institute of Arthritis and Musculoskeletal and Skin Diseases (NIAMS)/NIH, the Intramural Research Program of NIAMS (MJS), the Canadian Institutes of Health Research (#130572; HAG), and the CIHR Institute of Musculoskeletal Health and Arthritis (#134216; EDS). We thank Kenn Holmbeck of the National Institute of Dental and Craniofacial Research (NIDCR) for assistance with microCT analysis and Nasrin Kalantari Pour (NIAMS) for assistance with histology. NR 88 TC 5 Z9 5 U1 6 U2 29 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 8756-3282 EI 1873-2763 J9 BONE JI Bone PD SEP PY 2015 VL 78 BP 150 EP 164 DI 10.1016/j.bone.2015.05.007 PG 15 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA CK9LQ UT WOS:000356562000019 PM 25963390 ER PT J AU Hara, H Smith, DR AF Hara, Hideho Smith, David R. TI Japanese species of the sawfly genus Nesodiprion (Hymenoptera, Diprionidae) SO ZOOTAXA LA English DT Article DE Symphyta; new host record; new distribution record ID SYMPHYTA; NOV.; KEY AB Nesodiprion flavipes sp. nov. associated with Tsuga diversifolia (Maxim.) Mast. and N. kojimai sp. nov. associated with Abies veitchii Lindl. are described from Honshu, Japan. Additional taxonomic and biological information is given for other Japanese congeners, N. japonicus (Marlatt, 1898), N. albiventris Togashi, 1998, N. shinoharai Togashi, 1998, N. nigerrimus Togashi, 1998, N. kagaensis Togashi, 1998, N. niger Togashi, 2001 and N. tsugae Togashi, 2001. The males of N. shinoharai, N. kagaensis and N. tsugae are described for the first time. The host plants of N. shinoharai are Pinus spp. Nesodiprion kagaensis is newly recorded from Hokkaido, Japan, and its host plants are Pinus spp. and Larix kaempferi (Lamb.) Carriere. Larvae of N. japonicus and N. kagaensis are briefly described. A division of Nesodiprion into the following five species groups is proposed: N. tsugae group, N. niger group, N. flavipes group, N. japonicus group and N. shinoharai group. Additions to the key to Nesodiprion species by Hara & Smith (2012) are given. C1 [Hara, Hideho] Hokkaido Res Org, Forestry Res Inst, Bibai, Hokkaido 0790198, Japan. [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Natl Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Hara, H (reprint author), Hokkaido Res Org, Forestry Res Inst, Bibai, Hokkaido 0790198, Japan. EM hara-hideho@hro.or.jp; sawfly2@aol.com FU JSPS KAKENHI [20580165, 25440223] FX We deeply appreciate H. Kojima (Nagano) for offering valuable material and information and A. Shinohara (NSMT) for his kind help in various ways. Our thanks are also due N. Hirai and S. Kobayashi (OPU), T. Hirowatari (Kyushu University), K. Maeto (KU), H. Nagase (Kamakura), M. Ohara (HU), K. Ozaki (FFPRIH) and I. Togashi (Hakusan) for gifts or loans of the material for this study. We appreciate the comments and suggestions of two anonymous reviewers for improvement of the manuscript. This study was partly supported by JSPS KAKENHI Grant No. 20580165 and No. 25440223. NR 24 TC 1 Z9 1 U1 0 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 AUG 31 PY 2015 VL 4007 IS 4 BP 481 EP 508 PG 28 WC Zoology SC Zoology GA CQ1LL UT WOS:000360359100002 PM 26623828 ER PT J AU Strandburg-Peshkin, A Farine, DR Couzin, ID Crofoot, MC AF Strandburg-Peshkin, Ariana Farine, Damien R. Couzin, Iain D. Crofoot, Margaret C. TI The wisdom of baboon decisions Response SO SCIENCE LA English DT Letter ID CONSENSUS DECISION; ANIMAL GROUPS C1 [Strandburg-Peshkin, Ariana; Couzin, Iain D.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Farine, Damien R.; Crofoot, Margaret C.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.; Crofoot, Margaret C.] Smithsonian Trop Res Inst, Panama City, Panama. [Farine, Damien R.] Univ Oxford, Edward Grey Inst Field Ornithol, Dept Zool, Oxford OX1 3PS, England. [Couzin, Iain D.] Max Planck Inst Ornithol, Dept Collect Behav, D-78457 Constance, Germany. [Couzin, Iain D.] Univ Konstanz, Dept Biol, Chair Biodivers & Collect Behav, D-78457 Constance, Germany. RP Strandburg-Peshkin, A (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. EM astrandb@princeton.edu; damien.farine@zoo.ox.ac.uk; mccrofoot@ucdavis.edu NR 6 TC 0 Z9 0 U1 3 U2 25 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 AUG 28 PY 2015 VL 349 IS 6251 BP 935 EP 936 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CQ5LW UT WOS:000360646800028 PM 26315425 ER PT J AU Lea, AM Ryan, MJ AF Lea, Amanda M. Ryan, Michael J. TI SEXUAL SELECTION Irrationality in mate choice revealed by tungara frogs SO SCIENCE LA English DT Article ID MATING SIGNALS; PREFERENCE; DOMINANCE; ECONOMICS; ABSOLUTE; DECISION; UTILITY; SPACE AB Mate choice models derive from traditional microeconomic decision theory and assume that individuals maximize their Darwinian fitness by making economically rational decisions. Rational choices exhibit regularity, whereby the relative strength of preferences between options remains stable when additional options are presented. We tested female frogs with three simulated males who differed in relative call attractiveness and call rate. In binary choice tests, females' preferences favored stimulus caller B over caller A; however, with the addition of an inferior "decoy" C, females reversed their preferences and chose A over B. These results show that the relative valuation of mates is not independent of inferior alternatives in the choice set and therefore cannot be explained with the rational choice models currently used in sexual selection theory. C1 [Lea, Amanda M.; Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Lea, AM (reprint author), Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. EM alea@utexas.edu FU NSF [1120031] FX We thank the Autoridad Nacional del Ambiente for permission to do field work in Panama; the Smithsonian Tropical Research Institute for logistical support; M. Still, S. Beckett, and A. Smejdir for assistance; and M. Jennions and an anonymous reviewer for helpful suggestions on the manuscript. M.J.R. thanks M. Bateson for early conversations on decoys. This study was supported by NSF Integrative Organismal Systems grant 1120031 to M.J.R., R. Taylor, and R. Page and an NSF Predoctoral Fellowship to A.M.L. Procedures were approved by the Institutional Animal Care and Use Committees at The University of Texas at Austin and the Smithsonian Tropical Research Institute (AUP 2011-0825-2014-02). Experimental data are provided in the supplementary materials. NR 24 TC 10 Z9 11 U1 11 U2 54 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 AUG 28 PY 2015 VL 349 IS 6251 BP 964 EP 966 DI 10.1126/science.aab2012 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CQ5LW UT WOS:000360646800050 PM 26315434 ER PT J AU Bahia, RG Amado, GM Maneveldt, GW Adey, WH Johnson, G Jesionek, MB Longo, LL AF Bahia, Ricardo G. Amado-Filho, Gilberto M. Maneveldt, Gavin W. Adey, Walter H. Johnson, Gabriel Jesionek, Michel B. Longo, Leila L. TI Sporolithon yoneshigueae sp nov (Sporolithales, Corallinophycidae, Rhodophyta), a new rhodolith-forming coralline alga from the southwest Atlantic SO PHYTOTAXA LA English DT Article DE genetic marker; molecular phylogeny; Sporolithaceae; taxonomy ID PTYCHOIDES HEYDRICH; RED ALGAE; SPERMONDE ARCHIPELAGO; PHYLOGENY; SEQUENCES; AFRICA; GENUS; PSBA; CERAMIACEAE; MORPHOLOGY AB The aim of this study was to describe the new rhodolith-forming coralline alga species, Sporolithon yoneshigueae sp. nov., based on both morpho-anatomical and molecular data. Specimens were collected in rhodolith beds between 28 and 66 m depths in northeastern and southeastern Brazil. The new species can be distinguished from all other species of the genus Sporolithon by its wide tetrasporangial compartment pore diameter (35-43 mu m) and the correspondingly large number (19-24) of rosette cells surrounding the tetrasporangial compartment pore. Phylogenies inferred from psbA and SSU markers support it as a new species within Sporolithon with interspecific genetic divergence varying from 8.86-10.94 %, and 3.67-4.63%, respectively. Observations from recent gathering and from herbarium collections show that specimens previously designated as Sporolithon mediterraneum in Brazil correspond to Sporolithon yoneshigueae. C1 [Bahia, Ricardo G.; Amado-Filho, Gilberto M.; Longo, Leila L.] Diretoria Pesquisa Cient, Inst Pesquisas Jardim Bot Rio de Janeiro, BR-22460030 Rio De Janeiro, RJ, Brazil. [Maneveldt, Gavin W.] Univ Western Cape, Dept Biodivers & Conservat Biol, ZA-7535 Bellville, South Africa. [Adey, Walter H.; Johnson, Gabriel] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Jesionek, Michel B.] Univ Fed Rio de Janeiro, Ctr Ciencias Saude, Inst Biol, BR-21941900 Rio De Janeiro, RJ, Brazil. RP Amado, GM (reprint author), Diretoria Pesquisa Cient, Inst Pesquisas Jardim Bot Rio de Janeiro, Rua Pacheco Leao 915, BR-22460030 Rio De Janeiro, RJ, Brazil. EM gilbertoamadofilho@gmail.com FU CNPq; CAPES; FAPERJ; South African National Research Foundation; CNPq (National Research Council-Brazil); FAPES (Fundacao de Amparo a Pesquisa do Espirito Santo); Brasoil/ANP FX We are thankful to Dr. Mariana Cabral Oliveira (Universidade de Sao Paulo) for their important suggestions to improve the manuscript quality. RGB, GMAF, LL and RGB acknowledge the Brazilian Scientific Agencies CNPq, CAPES and FAPERJ for grants, postdocs and postgraduate scholarships. GWM acknowledges research support from the South African National Research Foundation. This work is a contribution of the Rede Abrolhos/SISBIOTA and PELD Abrolhos surveys. Financial support was obtained from CNPq (National Research Council-Brazil), FAPES (Fundacao de Amparo a Pesquisa do Espirito Santo) and Brasoil/ANP. NR 55 TC 2 Z9 2 U1 0 U2 5 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 AUG 28 PY 2015 VL 224 IS 2 BP 140 EP 158 DI 10.11646/phytotaxa.224.2.2 PG 19 WC Plant Sciences SC Plant Sciences GA CP8JM UT WOS:000360139800002 ER PT J AU Babb, JF AF Babb, James F. TI Empirically constructed dynamic electric dipole polarizability function of magnesium and its applications SO PHYSICAL REVIEW A LA English DT Article ID PHOTOIONIZATION CROSS-SECTIONS; MG ISOELECTRONIC SEQUENCE; LONG-RANGE INTERACTIONS; GROUND-STATE MAGNESIUM; DER-WAALS COEFFICIENTS; RADIATIVE ATOMIC DATA; L2 CI CALCULATION; OSCILLATOR-STRENGTHS; TRANSITION-PROBABILITIES; NEUTRAL MAGNESIUM AB The dynamic electric dipole polarizability function for the magnesium atom is formed by assembling the atomic electric dipole oscillator strength distribution from combinations of theoretical and experimental data for resonance oscillator strengths and for photoionization cross sections of valence and inner shell electrons. Consistency with the oscillator strength (Thomas-Reiche-Kuhn) sum rule requires the adopted principal resonance line oscillator strength to be several percent lower than the values given in two critical tabulations, though the value adopted is consistent with a number of theoretical determinations. The static polarizability is evaluated. Comparing the resulting dynamic polarizability as a function of the photon energy with more elaborate calculations reveals the contributions of inner shell electron excitations. The present results are applied to calculate the long-range interactions between two and three magnesium atoms and the interaction between a magnesium atom and a perfectly conducting metallic plate. Extensive comparisons of prior results for the principal resonance line oscillator strength, for the static polarizability, and for the van der Waals coefficient are given in the Appendix. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Babb, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 14, Cambridge, MA 02138 USA. OI Babb, James/0000-0002-3883-9501 FU National Science Foundation FX Discussions with C. Ballance, T. G. Lee, T. Gorczyca, C. F. Fischer, S. Manson, and M. Bromley are gratefully acknowledged. This work was supported in part by grants for ITAMP from the National Science Foundation to the Smithsonian Institution and to Harvard University. I thank Dr. Y. Singh for communicating his recent result. NR 123 TC 1 Z9 1 U1 3 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD AUG 27 PY 2015 VL 92 IS 2 AR 022712 DI 10.1103/PhysRevA.92.022712 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CP8DJ UT WOS:000360121600006 ER PT J AU Miyamoto, K Nonaka, A Oka, SI AF Miyamoto, Kei Nonaka, Ai Oka, Shin-Ichiro TI Northernmost record of a poorly known tuskfish, Choerodon margaritiferus (Perciformes: Labridae), from southern Japan, and first description of a female SO ZOOTAXA LA English DT Article DE Pisces; labrid; distribution; Okinawa; Japan AB We describe 5 specimens of Choerodon margaritiferus Fowler and Bean, 1928 (94.5-107.0 mm standard length, 1 male and 4 females) collected near Okinawa Island, southern Japan. This is the northernmost record of this species and the first record of it in Japanese waters; until now, C. margaritiferus was recorded only from the western central Pacific. This species was originally described on the basis of 1 male specimen, and all additional specimens described in the literature were also male. Morphological characters of both sexes are described, and new diagnostic characters of the female are presented. C1 [Miyamoto, Kei; Oka, Shin-Ichiro] Okinawa Churashima Fdn, Motobu, Okinawa 9050206, Japan. [Nonaka, Ai] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Miyamoto, K (reprint author), Okinawa Churashima Fdn, Ishikawa 888, Motobu, Okinawa 9050206, Japan. EM k-miyamoto@okichura.jp NR 18 TC 0 Z9 0 U1 1 U2 4 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 AUG 26 PY 2015 VL 4007 IS 1 BP 82 EP 90 PG 9 WC Zoology SC Zoology GA CP6OS UT WOS:000360007600005 PM 26623789 ER PT J AU Basset, Y Barrios, H Segar, S Srygley, RB Aiello, A Warren, AD Delgado, F Coronado, J Lezcano, J Arizala, S Rivera, M Perez, F Bobadilla, R Lopez, Y Ramirez, JA AF Basset, Yves Barrios, Hector Segar, Simon Srygley, Robert B. Aiello, Annette Warren, Andrew D. Delgado, Francisco Coronado, James Lezcano, Jorge Arizala, Stephany Rivera, Marleny Perez, Filonila Bobadilla, Ricardo Lopez, Yacksecari Alejandro Ramirez, Jose TI The Butterflies of Barro Colorado Island, Panama: Local Extinction since the 1930s SO PLOS ONE LA English DT Article ID TROPICAL RAIN-FORESTS; NEOTROPICAL BUTTERFLIES; HELICONIUS BUTTERFLIES; BRITISH BUTTERFLIES; DNA BARCODES; EL-NINO; LEPIDOPTERA; ECOLOGY; CONSERVATION; ASSEMBLAGES AB Few data are available about the regional or local extinction of tropical butterfly species. When confirmed, local extinction was often due to the loss of host-plant species. We used published lists and recent monitoring programs to evaluate changes in butterfly composition on Barro Colorado Island (BCI, Panama) between an old (1923-1943) and a recent (19932013) period. Although 601 butterfly species have been recorded from BCI during the 1923-2013 period, we estimate that 390 species are currently breeding on the island, including 34 cryptic species, currently only known by their DNA Barcode Index Number. Twenty-three butterfly species that were considered abundant during the old period could not be collected during the recent period, despite a much higher sampling effort in recent times. We consider these species locally extinct from BCI and they conservatively represent 6% of the estimated local pool of resident species. Extinct species represent distant phylogenetic branches and several families. The butterfly traits most likely to influence the probability of extinction were host growth form, wing size and host specificity, independently of the phylogenetic relationships among butterfly species. On BCI, most likely candidates for extinction were small hesperiids feeding on herbs (35% of extinct species). However, contrary to our working hypothesis, extinction of these species on BCI cannot be attributed to loss of host plants. In most cases these host plants remain extant, but they probably subsist at lower or more fragmented densities. Coupled with low dispersal power, this reduced availability of host plants has probably caused the local extinction of some butterfly species. Many more bird than butterfly species have been lost from BCI recently, confirming that small preserves may be far more effective at conserving invertebrates than vertebrates and, therefore, should not necessarily be neglected from a conservation viewpoint. C1 [Basset, Yves; Srygley, Robert B.; Aiello, Annette; Coronado, James; Lezcano, Jorge; Arizala, Stephany; Perez, Filonila; Bobadilla, Ricardo; Lopez, Yacksecari; Alejandro Ramirez, Jose] Smithsonian Trop Res Inst, Panama City, Panama. [Basset, Yves; Segar, Simon] Univ South Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Basset, Yves; Segar, Simon] Acad Sci Czech Republic, Inst Entomol, Ctr Biol, CR-37005 Ceske Budejovice, Czech Republic. [Basset, Yves; Barrios, Hector; Rivera, Marleny] Univ Panama, Maestria Entomol, Panama City 080814, Panama. [Srygley, Robert B.] ARS, Northern Plains Agr Lab, USDA, Sidney, MT 59270 USA. [Warren, Andrew D.] Univ Florida, Florida Museum Nat Hist, McGuire Ctr Lepidoptera & Biodivers, Gainesville, FL 32611 USA. [Delgado, Francisco] Univ Panama, Ctr Reg Univ Veraguas, Santiago, Panama. RP Basset, Y (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM bassety@si.edu RI Segar, Simon/K-6783-2015; Basset, Yves/B-6642-2014 FU Smithsonian Institution Barcoding Opportunity [FY012, FY013]; Czech Science foundation GACR [41-14-36068G]; USB Postdoc project - EU Education for Competitiveness Operational Programme [CZ.1.07/2.3.00/30.0006]; European Social Fund; Czech State Budget; STRI; NSF Graduate Research Fellowship; OTS-Mellon award; NSF [DEB 9419543, DEB 9119619] FX 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 the sequencing of many of the butterfly specimens collected recently on BCI. YB was supported by Czech Science foundation GACR grant 41-14-36068G and is a member of the Sistema Nacional de Investigacion, SENACYT, Panama. SS was funded by a USB Postdoc project (reg. no. CZ.1.07/2.3.00/30.0006), funded by the EU Education for Competitiveness Operational Programme, the European Social Fund and the Czech State Budget. RBS's sampling was supported by a short-term Fellowship from STRI, an NSF Graduate Research Fellowship, and an OTS-Mellon award. Tom Kursar kindly made available the BCI butterfly data of P.D. Coley and T.A. Kursar, which were supported by NSF grants DEB 9419543 and DEB 9119619. NR 95 TC 6 Z9 7 U1 2 U2 15 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 AUG 25 PY 2015 VL 10 IS 8 AR e0136623 DI 10.1371/journal.pone.0136623 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CP6KK UT WOS:000359995500100 PM 26305111 ER PT J AU Farfurnik, D Jarmola, A Pham, LM Wang, ZH Dobrovitski, VV Walsworth, RL Budker, D Bar-Gill, N AF Farfurnik, D. Jarmola, A. Pham, L. M. Wang, Z. H. Dobrovitski, V. V. Walsworth, R. L. Budker, D. Bar-Gill, N. TI Optimizing a dynamical decoupling protocol for solid-state electronic spin ensembles in diamond SO PHYSICAL REVIEW B LA English DT Article ID COHERENCE TIME; RESOLUTION; SEQUENCES; CENTERS; BATH; NMR AB We demonstrate significant improvements of the spin coherence time of a dense ensemble of nitrogen-vacancy (NV) centers in diamond through optimized dynamical decoupling (DD). Cooling the sample down to 77 K suppresses longitudinal spin relaxation T-1 effects and DD microwave pulses are used to increase the transverse coherence time T-2 from similar to 0.7 ms up to similar to 30 ms. We extend previous work of single-axis (Carr-Purcell-Meiboom-Gill) DD towards the preservation of arbitrary spin states. Following a theoretical and experimental characterization of pulse and detuning errors, we compare the performance of various DD protocols. We identify that the optimal control scheme for preserving an arbitrary spin state is a recursive protocol, the concatenated version of the XY8 pulse sequence. The improved spin coherence might have an immediate impact on improvements of the sensitivities of ac magnetometry. Moreover, the protocol can be used on denser diamond samples to increase coherence times up to NV-NV interaction time scales, a major step towards the creation of quantum collective NV spin states. C1 [Farfurnik, D.; Bar-Gill, N.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-9190401 Jerusalem, Israel. [Farfurnik, D.; Bar-Gill, N.] Hebrew Univ Jerusalem, Ctr Nanosci & Nanotechnol, IL-9190401 Jerusalem, Israel. [Jarmola, A.; Budker, D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Pham, L. M.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Z. H.] Univ So Calif, Dept Chem, Los Angeles, CA 90089 USA. [Dobrovitski, V. V.] Iowa State Univ, Ames Lab, Ames, IA 50011 USA. [Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Budker, D.] Johannes Gutenberg Univ Mainz, Helmholtz Inst, D-55099 Mainz, Germany. [Bar-Gill, N.] Hebrew Univ Jerusalem, Dept Appl Phys, Rachel & Selim Sch Engn, IL-9190401 Jerusalem, Israel. RP Farfurnik, D (reprint author), Hebrew Univ Jerusalem, Racah Inst Phys, IL-9190401 Jerusalem, Israel. RI Budker, Dmitry/F-7580-2016 OI Budker, Dmitry/0000-0002-7356-4814 FU EU CIG; Minerva ARCHES award; Israel Science Foundation [750/14]; Ministry of Science and Technology, Israel; German-Israeli Project Cooperation (DIP) program; NSF [ECCS-1202258]; AFOSR/DARPA QuASAR program; U.S. Department of Energy-Basic Energy Sciences [DE-AC02-07CH11358]; CAMBR fellowship for Nanoscience and Nanotechnology; Binational Science Foundation Rahamimoff travel grant FX We thank Gonzalo A. Alvarez for fruitful discussions. This work has been supported in part by the EU CIG, the Minerva ARCHES award, the Israel Science Foundation (Grant No. 750/14), and the Ministry of Science and Technology, Israel. Additional support was provided by the German-Israeli Project Cooperation (DIP) program, the NSF through Grant No. ECCS-1202258, and the AFOSR/DARPA QuASAR program. Work at Ames Laboratory was supported by the U.S. Department of Energy-Basic Energy Sciences under Contract No. DE-AC02-07CH11358. D.F. was partially supported by the CAMBR fellowship for Nanoscience and Nanotechnology, and the Binational Science Foundation Rahamimoff travel grant. NR 39 TC 12 Z9 12 U1 3 U2 23 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD AUG 24 PY 2015 VL 92 IS 6 AR 060301 DI 10.1103/PhysRevB.92.060301 PG 5 WC Physics, Condensed Matter SC Physics GA CS6SO UT WOS:000362212200002 ER PT J AU Holzmeyer, L Duretto, M Crayn, D Horandl, E Heslewood, M Jayanthan, J Appelhans, MS AF Holzmeyer, Laura Duretto, Marco Crayn, Darren Hoerandl, Elvira Heslewood, Margaret Jayanthan, Janani Appelhans, Marc S. TI Phylogeny of Acronychia (Rutaceae) and First Insights into Its Historical Biogeography and the Evolution of Fruit Characters SO PLOS ONE LA English DT Article ID MOLECULAR PHYLOGENY; CLADISTIC-ANALYSIS; NONCODING REGIONS; GEOGRAPHIC RANGE; CHLOROPLAST DNA; REVISION; SUBFAMILIES; DISPERSAL; INFERENCE; MELICOPE AB Background The genus Acronychia (Citrus family, Rutaceae) contains 49 species of trees and shrubs that are found mainly in rain forest. The genus has a large distributional range from mainland southern Asia to Australia and New Caledonia, but most species are endemic to either New Guinea or Australia. This study aimed to provide the first detailed molecular phylogeny of Acronychia and use it to test the taxonomic value of fruit morphological characters, and infer the historical biogeography of the genus. Methodology Phylogenetic analyses (Bayesian Inference, Maximum Likelihood) were undertaken on nucleotide sequence data from two plastid (psbA-trnH, trnL-trnF) and three nuclear markers (ETS, ITS, NIAi3) from 29 Acronychia species (59% of the genus) and representatives of related genera. Results and Conclusions The results indicate that the South-East Asian genus Maclurodendron is nested phylogenetically within Acronychia and must be synonymized to render Acronychia monophyletic. Fruit morphological characters have been used previously to infer relationships within Acronychia and our analyses show that these characters are informative for some subclades but are homoplasious for the group as a whole. Apocarpous fruits are the ancestral state in Acronychia and subapocarpous and fully syncarpous fruits are derived. The unisexual flowers of Maclurodendron are derived from bisexual flowers, which are found in all species of Acronychia as well as its relatives. Acronychia probably first evolved on Australia with range expansion to New Guinea via stepping-stone dispersal or direct land connections within the Sahul Shelf, followed by two independent dispersals to areas west of New Guinea. Most species of Acronychia occur in either Australia or New Guinea, but no species occurs in both regions. This is surprising given the close proximity of the landmasses, but might be explained by ecological factors. C1 [Holzmeyer, Laura; Hoerandl, Elvira; Appelhans, Marc S.] Univ Gottingen, Dept Systemat Biodivers & Evolut Plants, D-37073 Gottingen, Germany. [Duretto, Marco; Heslewood, Margaret] Royal Bot Gardens & Domain Trust, Natl Herbarium New South Wales, Sydney, NSW, Australia. [Crayn, Darren; Jayanthan, Janani] James Cook Univ, Australian Trop Herbarium, Cairns, Australia. [Appelhans, Marc S.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Appelhans, MS (reprint author), Univ Gottingen, Dept Systemat Biodivers & Evolut Plants, Untere Karspule 2, D-37073 Gottingen, Germany. EM marc.appelhans@biologie.uni-goettingen.de RI Research ID, CTBCC /O-3564-2014; James Cook University, TESS/B-8171-2012; Crayn, Darren/A-7386-2011 OI Crayn, Darren/0000-0001-6614-4216 FU Open Access Publication Funds of Gottingen University FX The authors acknowledge support by the Open Access Publication Funds of Gottingen University. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 72 TC 0 Z9 0 U1 1 U2 12 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 AUG 24 PY 2015 VL 10 IS 8 AR e0136296 DI 10.1371/journal.pone.0136296 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CP5VA UT WOS:000359951900055 PM 26301574 ER PT J AU Ruffle, PME Kemper, F Jones, OC Sloan, GC Kraemer, KE Woods, PM Boyer, ML Srinivasan, S Antoniou, V Lagadec, E Matsuura, M McDonald, I Oliveira, JM Sargent, BA Sewilo, M Szczerba, R van Loon, JT Volk, K Zijlstra, AA AF Ruffle, Paul M. E. Kemper, F. Jones, O. C. Sloan, G. C. Kraemer, K. E. Woods, Paul M. Boyer, M. L. Srinivasan, S. Antoniou, V. Lagadec, E. Matsuura, M. McDonald, I. Oliveira, J. M. Sargent, B. A. Sewilo, M. Szczerba, R. van Loon, J. Th. Volk, K. Zijlstra, A. A. TI Spitzer infrared spectrograph point source classification in the Small Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; surveys; dust, extinction; H ii regions; Magellanic Clouds; infrared: stars ID GIANT BRANCH STARS; LONG-PERIOD VARIABLES; YOUNG STELLAR OBJECTS; WOLF-RAYET STARS; SPACE-TELESCOPE OBSERVATIONS; BINARY HD 5980; VLT-FLAMES SURVEY; ULTRAVIOLET INTERSTELLAR ABSORPTION; SPECTROSCOPIC-EXPLORER OBSERVATIONS; EMISSION-LINE STARS AB The Magellanic Clouds are uniquely placed to study the stellar contribution to dust emission. Individual stars can be resolved in these systems even in the mid-infrared, and they are close enough to allow detection of infrared excess caused by dust. We have searched the Spitzer Space Telescope data archive for all Infrared Spectrograph (IRS) staring-mode observations of the Small Magellanic Cloud (SMC) and found that 209 Infrared Array Camera (IRAC) point sources within the footprint of the Surveying the Agents of Galaxy Evolution in the Small Magellanic Cloud (SAGE-SMC) Spitzer Legacy programme were targeted, within a total of 311 staring-mode observations. We classify these point sources using a decision tree method of object classification, based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information. We find 58 asymptotic giant branch (AGB) stars, 51 young stellar objects, 4 post-AGB objects, 22 red supergiants, 27 stars (of which 23 are dusty OB stars), 24 planetary nebulae (PNe), 10 Wolf-Rayet stars, 3 H ii regions, 3 R Coronae Borealis stars, 1 Blue Supergiant and 6 other objects, including 2 foreground AGB stars. We use these classifications to evaluate the success of photometric classification methods reported in the literature. C1 [Ruffle, Paul M. E.; Jones, O. C.; McDonald, I.; Zijlstra, A. A.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Ruffle, Paul M. E.; Kemper, F.; Srinivasan, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Jones, O. C.; Volk, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Kraemer, K. E.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Woods, Paul M.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Boyer, M. L.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Antoniou, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lagadec, E.] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, Observ Cote Azur, F-06304 Nice, France. [Matsuura, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Matsuura, M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Oliveira, J. M.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Sargent, B. A.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Sewilo, M.] Space Sci Inst, Boulder, CO 80301 USA. [Sewilo, M.] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr 366, Baltimore, MD 21218 USA. [Szczerba, R.] N Copernicus Astron Ctr, PL-87100 Torun, Poland. EM ciska@asiaa.sinica.edu.tw RI Woods, Paul/E-6926-2011; Kemper, Francisca/D-8688-2011; Antoniou, Vallia/E-3837-2013; OI Woods, Paul/0000-0003-4340-3590; Kemper, Francisca/0000-0003-2743-8240; Antoniou, Vallia/0000-0001-7539-1593; Jones, Olivia/0000-0003-4870-5547; Kraemer, Kathleen/0000-0002-2626-7155 FU STFC; National Science Council; Ministry of Science and Technology [NSC100-2112-M-001-023-MY3, MOST103-2112-M-001-0330]; NASA ADP [NNX11AB06G]; Polish NCN grant [2011/01/B/ST9/02031, DEC-2013/08/M/ST9/00664]; National Aeronautics and Space Administration; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G] FX The authors wish to thank Paul Ruffle's partner Rose Wheeler, Rose provided access to Paul's notes and files, which allowed us to finish this work. PMER thanks Academia Sinica Institute of Astronomy and Astrophysics (ASIAA) for their financial support and hospitality during the preparation of this work. The authors thank David Whelan for making available Spitzer spectra of point sources described in his 2013 paper. Astrophysics at JBCA is supported by STFC. FK acknowledges support from the former National Science Council and the Ministry of Science and Technology in the form of grants NSC100-2112-M-001-023-MY3 and MOST103-2112-M-001-0330. BAS acknowledges support from NASA ADP NNX11AB06G. RSz acknowledges support from the Polish NCN grant 2011/01/B/ST9/02031. The research presented here was conducted within the scope of the HECOLS International Associated Laboratory, supported in part by the Polish NCN grant DEC-2013/08/M/ST9/00664 (E.L.; R.Sz). This work is based (in part) on observations made with the Spitzer Space Telescope, obtained from the NASA/IPAC Infrared Science Archive, both of which are operated by the Jet Propulsion Laboratory, California Institute of Technology under a 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. 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 Hobble Space Telescope (HST) data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This research has also made use of the SAGE CASJobs data base, which made possible by the Sloan Digital Sky Survey Collaboration; SAOImage DS9, developed by Smithsonian Astrophysical Observatory; the VizieR catalogue access tool. CDS, Strasbourg, France; the SIMBAD data base, operated at CDS, Strasbourg, France; and NASA's Astrophysics Data System Bibliographic Services. NR 286 TC 4 Z9 4 U1 1 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 AUG 21 PY 2015 VL 451 IS 4 BP 3504 EP 3536 DI 10.1093/mnras/stv1106 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8HA UT WOS:000360846400013 ER PT J AU Tremblay, GR O'Dea, CP Baum, SA Mittal, R McDonald, MA Combes, F Li, Y McNamara, BR Bremer, MN Clarke, TE Donahue, M Edge, AC Fabian, AC Hamer, SL Hogan, MT Oonk, JBR Quillen, AC Sanders, JS Salome, P Voit, GM AF Tremblay, G. R. O'Dea, C. P. Baum, S. A. Mittal, R. McDonald, M. A. Combes, F. Li, Y. McNamara, B. R. Bremer, M. N. Clarke, T. E. Donahue, M. Edge, A. C. Fabian, A. C. Hamer, S. L. Hogan, M. T. Oonk, J. B. R. Quillen, A. C. Sanders, J. S. Salome, P. Voit, G. M. TI Far-ultraviolet morphology of star-forming filaments in cool core brightest cluster galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: star formation ID GALACTIC NUCLEUS FEEDBACK; RAY-LUMINOUS CLUSTERS; CENTRAL-DOMINANT-GALAXIES; X-RAY; FLOW CLUSTERS; MOLECULAR GAS; EMISSION-LINE; HYDRA-A; PERSEUS CLUSTER; ABELL 2597 AB We present a multiwavelength morphological analysis of star-forming clouds and filaments in the central (a parts per thousand(2)50 kpc) regions of 16 low-redshift (z < 0.3) cool core brightest cluster galaxies. New Hubble Space Telescope imaging of far-ultraviolet continuum emission from young (a parts per thousand(2)10 Myr), massive (a parts per thousand(3)5 M-aS (TM)) stars reveals filamentary and clumpy morphologies, which we quantify by means of structural indices. The FUV data are compared with X-ray, Ly alpha, narrow-band H alpha, broad-band optical/IR, and radio maps, providing a high spatial resolution atlas of star formation locales relative to the ambient hot (similar to 10(7-8) K) and warm ionized (similar to 10(4) K) gas phases, as well as the old stellar population and radio-bright active galactic nucleus (AGN) outflows. Nearly half of the sample possesses kpc-scale filaments that, in projection, extend towards and around radio lobes and/or X-ray cavities. These filaments may have been uplifted by the propagating jet or buoyant X-ray bubble, or may have formed in situ by cloud collapse at the interface of a radio lobe or rapid cooling in a cavity's compressed shell. The morphological diversity of nearly the entire FUV sample is reproduced by recent hydrodynamical simulations in which the AGN powers a self-regulating rain of thermally unstable star-forming clouds that precipitate from the hot atmosphere. In this model, precipitation triggers where the cooling-to-free-fall time ratio is t(cool)/t(ff) similar to 10. This condition is roughly met at the maximal projected FUV radius for more than half of our sample, and clustering about this ratio is stronger for sources with higher star formation rates. C1 [Tremblay, G. R.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Tremblay, G. R.] Yale Univ, Ctr Astron & Astrophys, New Haven, CT 06511 USA. [Tremblay, G. R.] European So Observ, D-85748 Garching, Germany. [O'Dea, C. P.; Baum, S. A.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [O'Dea, C. P.; Baum, S. A.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Baum, S. A.] Univ Manitoba, Fac Sci, Winnipeg, MB R3T 2N2, Canada. [Baum, S. A.; Mittal, R.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Mittal, R.] Albert Einstein Inst, Max Planck Inst Gravitationsphys, D-30167 Hannover, Germany. [McDonald, M. A.] MIT, Kavil Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Combes, F.; Hamer, S. L.; Salome, P.] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Li, Y.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [McNamara, B. R.; Hogan, M. T.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Clarke, T. E.] US Navy, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Edge, A. C.] Inst Astron, Cambridge CB3 0HA, England. [Oonk, J. B. R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Quillen, A. C.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Tremblay, GR (reprint author), Yale Univ, Dept Phys, 217 Prospect St, New Haven, CT 06511 USA. EM grant.tremblay@yale.edu OI Edge, Alastair/0000-0002-3398-6916; Tremblay, Grant/0000-0002-5445-5401; Li, Yuan/0000-0001-5262-6150; Sanders, Jeremy/0000-0003-2189-4501; Combes, Francoise/0000-0003-2658-7893; Voit, Gerard/0000-0002-3514-0383 FU NASA [PF-150128, NAS8-03060, NNX12AH41G, NNX12AC98G, ATP12-ATP12-0017, NAS8-39073, 5-26555]; European Southern Observatory (ESO) Fellowship - European Community [229517]; National Aeronautics and Space Administration through Einstein Postdoctoral Fellowship Award [PF-150128]; NSF [AST-0908390, AST-1008134, AST-1210890, AST-1008454]; NASA through Chandra award [G06-7115B]; 6.1 Base funds FX The authors thank Drs. Richard Bower, Tim Davis, Bill Forman, Nina Hatch, Claudia Lagos, Robert Laing, Jason Spyromilio, and Aurora Simionescu for thoughtful discussions. GRT acknowledges support from a NASA Einstein Fellowship under award number PF-150128, as well as a European Southern Observatory (ESO) Fellowship partially funded by the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement number 229517. Support for this work was provided by the National Aeronautics and Space Administration through Einstein Postdoctoral Fellowship Award Number PF-150128 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. YE acknowledges financial support from NSF grants AST-0908390, AST-1008134, AST-1210890, AST-1008454, NASA grants NNX12AH41G, NNX12AC98G, and ATP12-ATP12-0017, as well as computational resources from NASA, NSF XSEDE and Columbia University. TEC was partially supported by NASA through Chandra award G06-7115B issued by the Chandra X-ray Observatory Center for and on behalf of NASA under contract NAS8-39073. Basic research into radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funds. This paper is based on observations made with the NASA/ESA Hobble 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 5-26555. This research made use of Astropy, a community-developed core grams package for Astronomy (Astropy Collaboration et al. 2013). We have also made extensive use of the NASA Astrophysics Data System bibliographic services and the NASA/IPAC Extragalactic Database, operated by the Jet Propulsion Laboratory, California Institute of Technology. under contract with NASA. NR 168 TC 19 Z9 19 U1 0 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 AUG 21 PY 2015 VL 451 IS 4 BP 3768 EP 3800 DI 10.1093/mnras/stv1151 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8HA UT WOS:000360846400030 ER PT J AU George, LT Dwarakanath, KS Johnston-Hollitt, M Hurley-Walker, N Hindson, L Kapinska, AD Tingay, SJ Bell, M Callingham, JR For, BQ Hancock, PJ Lenc, E McKinley, B Morgan, J Offringa, A Procopio, P Staveley-Smith, L Wayth, RB Wu, C Zheng, Q Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF George, L. T. Dwarakanath, K. S. Johnston-Hollitt, M. Hurley-Walker, N. Hindson, L. Kapinska, A. D. Tingay, S. J. Bell, M. Callingham, J. R. For, Bi-Qing Hancock, P. J. Lenc, E. McKinley, B. Morgan, J. Offringa, A. Procopio, P. Staveley-Smith, L. Wayth, R. B. Wu, Chen Zheng, Q. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI An analysis of the halo and relic radio emission from Abell 3376 from Murchison Widefield Array observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: Abell 3376; galaxies: clusters: intracluster medium ID X-RAY-EMISSION; GALAXY CLUSTERS; COSMIC-RAYS; NONTHERMAL EMISSION; SHOCK ACCELERATION; MAGNETIC-FIELDS; MASS FUNCTION; SKY SURVEY; GAMMA-RAY; REACCELERATION AB We have carried out multiwavelength observations of the nearby (z = 0.046) rich, merging galaxy cluster Abell 3376 with the Murchison Widefield Array (MWA). As a part of the GaLactic and Extragalactic All-sky MWA Survey, this cluster was observed at 88, 118, 154, 188, and 215 MHz. The known radio relics, towards the eastern and western peripheries of the cluster, were detected at all the frequencies. The relics, with a linear extent of similar to 1 Mpc each, are separated by similar to 2 Mpc. Combining the current observations with those in the literature, we have obtained the spectra of these relics over the frequency range 80-1400 MHz. The spectra follow power laws, with alpha = -1.17 +/- A 0.06 and -1.37 +/- A 0.08 for the west and east relics, respectively (S infinity nu(infinity)). Assuming the break frequency to be near the lower end of the spectrum we estimate the age of the relics to be similar to 0.4 Gyr. No diffuse radio emission from the central regions of the cluster (halo) was detected. The upper limit on the radio power of any possible halo that might be present in the cluster is a factor of 35 lower than that expected from the radio power and X-ray luminosity correlation for cluster haloes. From this we conclude that the cluster halo is very extended (> 500 kpc) and/or most of the radio emission from the halo has decayed. The current limit on the halo radio power is a factor of 10 lower than the existing upper limits with possible implications for models of halo formation. C1 [George, L. T.; Dwarakanath, K. S.; Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Johnston-Hollitt, M.; Hindson, L.; Zheng, Q.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Hurley-Walker, N.; Tingay, S. J.; Hancock, P. J.; Morgan, J.; Wayth, R. B.; Emrich, D.; Lynch, M. J.; Ord, S. M.; Waterson, M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Kapinska, A. D.; Tingay, S. J.; Callingham, J. R.; Hancock, P. J.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Kapinska, A. D.; For, Bi-Qing; Staveley-Smith, L.; Wu, Chen] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Bell, M.; Callingham, J. R.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Epping, NSW 1710, Australia. [Callingham, J. R.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [McKinley, B.; Procopio, P.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Offringa, A.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Bernardi, G.] Square Kilometre Array South Africa SKASA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, 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. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Roshi, A.] NRAO, Charlottesville, VA USA. [Roshi, A.] NRAO, Green Bank, WV USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Morgan, E.; Williams, C. L.] MIT, Kavil Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP George, LT (reprint author), Raman Res Inst, Bangalore 560080, Karnataka, India. EM lijo@rri.res.in; dwaraka@rri.res.in RI Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Dwarakanath, K /D-4876-2012; Wayth, Randall/B-2444-2013; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Kapinska, Anna/B-3999-2014; Staveley-Smith, Lister/A-1683-2011; OI Lenc, Emil/0000-0002-9994-1593; Wayth, Randall/0000-0002-6995-4131; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Kapinska, Anna/0000-0002-5289-5729; Staveley-Smith, Lister/0000-0002-8057-0294; Callingham, Joseph/0000-0002-7167-1819; Hancock, Paul/0000-0002-4203-2946 FU US National Science Foundation [AST-0457585, PHY-0835713, 0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University); CSIRO; National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia by Western Australian State government FX This scientific work makes use of the Murchison Radio-astronomy Observatory, operated by the Commonwealth Scientific and Industrial Research Organisation (CSIRO), We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site Support for the MWA comes from the US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER 0847753 and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 73 TC 0 Z9 0 U1 0 U2 6 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 AUG 21 PY 2015 VL 451 IS 4 BP 4207 EP 4214 DI 10.1093/mnras/stv1152 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8HA UT WOS:000360846400065 ER PT J AU Callingham, JR Gaensler, BM Ekers, RD Tingay, SJ Wayth, RB Morgan, J Bernardi, G Bell, ME Bhat, R Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Ewall-Wice, A Feng, L Greenhill, LJ Hazelton, BJ Hindson, L Hurley-Walker, N Jacobs, DC Johnston-Hollitt, M Kaplan, DL Kudrayvtseva, N Lenc, E Lonsdale, CJ McKinley, B McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Offringa, AR Ord, SM Pindor, B Prabu, T Procopio, P Riding, J Srivani, KS Subrahmanyan, R Shankar, NU Webster, RL Williams, A Williams, CL AF Callingham, J. R. Gaensler, B. M. Ekers, R. D. Tingay, S. J. Wayth, R. B. Morgan, J. Bernardi, G. Bell, M. E. Bhat, R. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Ewall-Wice, A. Feng, L. Greenhill, L. J. Hazelton, B. J. Hindson, L. Hurley-Walker, N. Jacobs, D. C. Johnston-Hollitt, M. Kaplan, D. L. Kudrayvtseva, N. Lenc, E. Lonsdale, C. J. McKinley, B. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Offringa, A. R. Ord, S. M. Pindor, B. Prabu, T. Procopio, P. Riding, J. Srivani, K. S. Subrahmanyan, R. Shankar, N. Udaya Webster, R. L. Williams, A. Williams, C. L. TI BROADBAND SPECTRAL MODELING OF THE EXTREME GIGAHERTZ-PEAKED SPECTRUM RADIO SOURCE PKS B0008-421 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (PKS B0008-421); radiation mechanisms: general; radio continuum: general ID COMPACT STEEP-SPECTRUM; FREE-FREE ABSORPTION; HIGH-FREQUENCY PEAKERS; SYNCHROTRON SELF-ABSORPTION; SYMMETRIC OBJECTS; SOURCE CATALOG; SOUTHERN SKY; LOUD AGN; REIONIZATION OBSERVATORIES; SOURCE EVOLUTION AB We present broadband observations and spectral modeling of PKS B0008-421. and identify it as an extreme gigahertz-peaked spectrum (GPS) source. PKS B0008-421 is characterized by the steepest known spectral slope below the turnover, close to the theoretical limit of synchrotron self-absorption, and the smallest known spectral width of any GPS source. Spectral coverage of the source spans from 0.118 to 22 GHz, which includes data from the Murchison Widefield Array and the wide bandpass receivers on the Australia Telescope Compact Array. We have implemented a Bayesian inference model fitting routine to fit the data with internal free-free absorption (FFA), single-and double-component FFA in an external homogeneous medium, FFA in an external inhomogeneous medium, or single-and double-component synchrotron self-absorption models, all with and without a high-frequency exponential break. We find that without the inclusion of a high-frequency break these models cannot accurately fit the data, with significant deviations above and below the peak in the radio spectrum. The addition of a high-frequency break provides acceptable spectral fits for the inhomogeneous FFA and double-component synchrotron self-absorption models, with the inhomogeneous FFA model statistically favored. The requirement of a high-frequency spectral break implies that the source has ceased injecting fresh particles. Additional support for the inhomogeneous FFA model as being responsible for the turnover in the spectrum is given by the consistency between the physical parameters derived from the model fit and the implications of the exponential spectral break, such as the necessity of the source being surrounded by a dense ambient medium to maintain the peak frequency near the gigahertz region. This implies that PKS B0008-421 should display an internal H I column density greater than 10(20) cm(-2). The discovery of PKS B0008-421 suggests that the next generation of low radio frequency surveys could reveal a large population of GPS sources that have ceased activity, and that a portion of the ultra-steep-spectrum source population could be composed of these GPS sources in a relic phase. C1 [Callingham, J. R.; Gaensler, B. M.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Callingham, J. R.; Ekers, R. D.; Bell, M. E.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Marsfield, NSW 2122, Australia. [Callingham, J. R.; Gaensler, B. M.; Tingay, S. J.; Wayth, R. B.; Bell, M. E.; Bhat, R.; Briggs, F.; Lenc, E.; Mitchell, D. A.; Offringa, A. R.; Ord, S. M.; Pindor, B.; Procopio, P.; Riding, J.; Subrahmanyan, R.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Tingay, S. J.; Wayth, R. B.; Morgan, J.; Bhat, R.; Hurley-Walker, N.; Kudrayvtseva, N.; Ord, S. M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res ICRAR, Bentley, WA 6102, Australia. [Bernardi, G.] Sq Kilometre Array South Africa SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.; Jacobs, D. C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Srivani, K. S.; Subrahmanyan, R.; Shankar, N. Udaya] Raman Res Inst, Bangalore 560080, Karnataka, India. [Ewall-Wice, A.; Feng, L.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Hindson, L.; Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Offringa, A. R.] Netherlands Inst Radio Astron ASTRON, Dwingeloo, Netherlands. RP Callingham, JR (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. EM j.callingham@physics.usyd.edu.au RI Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Wayth, Randall/B-2444-2013; Hurley-Walker, Natasha/B-9520-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; OI Callingham, Joseph/0000-0002-7167-1819; Wayth, Randall/0000-0002-6995-4131; Hurley-Walker, Natasha/0000-0002-5119-4808; M, Manjunath/0000-0001-8710-0730; /0000-0002-0086-7363; Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593; Ekers, Ron/0000-0002-3532-9928 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (via grant from the New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research Grant); CSIRO; National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Commonwealth of Australia FX The authors thank Geoffrey Bicknell, David Jauncey, and Edward King for stimulating discussions about the theoretical aspects of the absorption models and the VLBI measurements of PKS B0008-421. This scientific work makes use of the Murchison Radioastronomy Observatory, operated by CSIRO. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian federal government provides additional support via the CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing. and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and the University of Western Australia, funded by the Western Australian State government. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This paper includes archived data obtained through the Australia Telescope Online Archive (http://atoa.atnf.csiro.au). 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. NR 96 TC 13 Z9 13 U1 0 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 AUG 20 PY 2015 VL 809 IS 2 AR 168 DI 10.1088/0004-637X/809/2/168 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100061 ER PT J AU Corcoran, MF Nichols, JS Pablo, H Shenar, T Pollock, AMT Waldron, WL Moffat, AFJ Richardson, ND Russell, CMP Hamaguchi, K Huenemoerder, DP Oskinova, L Hamann, WR Naze, Y Ignace, R Evans, NR Lomax, JR Hoffman, JL Gayley, K Owocki, SP Leutenegger, M Gull, TR Hole, KT Lauer, J Iping, RC AF Corcoran, M. F. Nichols, J. S. Pablo, H. Shenar, T. Pollock, A. M. T. Waldron, W. L. Moffat, A. F. J. Richardson, N. D. Russell, C. M. P. Hamaguchi, K. Huenemoerder, D. P. Oskinova, L. Hamann, W. -R. Naze, Y. Ignace, R. Evans, N. R. Lomax, J. R. Hoffman, J. L. Gayley, K. Owocki, S. P. Leutenegger, M. Gull, T. R. Hole, K. T. Lauer, J. Iping, R. C. TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. I. OVERVIEW OF THE X-RAY SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: early-type; stars: individual (Delta Ori); stars: mass-loss; X-rays: stars ID HOT-STAR WINDS; O-TYPE STARS; RADIATION-DRIVEN WINDS; COLLIDING WINDS; EMISSION; CHANDRA; SPECTROSCOPY; SIMULATIONS; SYSTEMS; MODELS AB We present an overview of four deep phase-constrained Chandra HETGS X-ray observations of delta Ori A. Delta Ori A is actually a triple system that includes the nearest massive eclipsing spectroscopic binary, delta Ori Aa, the only such object that can be observed with little phase-smearing with the Chandra gratings. Since the fainter star, delta Ori Aa2, has a much lower X-ray luminosity than the brighter primary (delta Ori Aa1), delta Ori Aa provides a unique system with which to test the spatial distribution of the X-ray emitting gas around delta Ori Aa1 via occultation by the photosphere of, and wind cavity around, the X-ray dark secondary. Here we discuss the X-ray spectrum and X-ray line profiles for the combined observation, having an exposure time of nearly 500 ks and covering nearly the entire binary orbit. The companion papers discuss the X-ray variability seen in the Chandra spectra, present new space-based photometry and ground-based radial velocities obtained simultaneously with the X-ray data to better constrain the system parameters, and model the effects of X-rays on the optical and UV spectra. We find that the X-ray emission is dominated by embedded wind shock emission from star Aa1, with little contribution from the tertiary star Ab or the shocked gas produced by the collision of the wind of Aa1 against the surface of Aa2. We find a similar temperature distribution to previous X-ray spectrum analyses. We also show that the line half-widths are about 0.3-0.5 times the terminal velocity of the wind of star Aa1. We find a strong anti-correlation between line widths and the line excitation energy, which suggests that longer-wavelength, lower-temperature lines form farther out in the wind. Our analysis also indicates that the ratio of the intensities of the strong and weak lines of Fe XVII and Ne X are inconsistent with model predictions, which may be an effect of resonance scattering. C1 [Corcoran, M. F.; Hamaguchi, K.; Leutenegger, M.; Iping, R. C.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.; Leutenegger, M.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Nichols, J. S.; Lauer, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pablo, H.; Moffat, A. F. J.; Richardson, N. D.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Pablo, H.; Moffat, A. F. J.; Richardson, N. D.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada. [Shenar, T.; Oskinova, L.; Hamann, W. -R.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Pollock, A. M. T.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain. [Waldron, W. L.] Eureka Sci Inc, Oakland, CA 94602 USA. [Russell, C. M. P.] NASA GSFC, Greenbelt, MD 20771 USA. [Hamaguchi, K.; Leutenegger, M.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Huenemoerder, D. P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Naze, Y.] Univ Liege, Grp Astrophys Hautes Energies, Inst Astrophys & Geophys, B-4000 Sart Tilman Par Liege, Belgium. [Ignace, R.] E Tennessee State Univ, Phys & Astron, Johnson City, TN 37614 USA. [Evans, N. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lomax, J. R.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Hoffman, J. L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Gayley, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Owocki, S. P.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Gull, T. R.] NASA Goddard Space Flight Ctr, Lab Extraterr Planets & Stellar Astrophys, Greenbelt, MD 20771 USA. [Hole, K. T.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA. [Iping, R. C.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Iping, R. C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Corcoran, MF (reprint author), NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. EM michael.f.corcoran@nasa.gov FU National Aeronautics and Space Administration [GO3-14015A, GO3-14015E]; National Aeronautics Space Administration [NAS8-03060]; NASA [NNG06EO90A, NNX13AF40G]; Chandra X-ray Center NASA [NAS8-03060]; NASA Postdoctoral Program at the Goddard Space Flight Center; Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics; Leibniz Institute for Astrophysics Potsdam (AIP); institute of Physics and Astronomy of the University of Potsdam; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMM and Integral contracts; "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe); CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship; NSERC (Canada); FRQNT (Quebec); NSF [AST-0807477] FX We thank the MOST team for the award of observing time for delta Ori A. We also thank our anonymous referee, whose comments significantly improved this paper. M.F.C. thanks John Houck and Michael Nowak for many helpful discussions concerning data analysis with ISIS. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14015A and GO3-14015E 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. M.F.C., J.S.N., W.L.W., C.M.P.R., and K.H. gratefully acknowledge this support. M.F.C. acknowledges support from NASA under cooperative agreement number NNG06EO90A. N.R.E. is grateful for support from the Chandra X-ray Center NASA Contract NAS8-03060. C.M.P.R. is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. T.S. is grateful for financial support from the Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics, a joint project of the Leibniz Institute for Astrophysics Potsdam (AIP) and the institute of Physics and Astronomy of the University of Potsdam. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe). N.D.R. gratefully acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. A.F.J.M. is grateful for financial support from NSERC (Canada) and FRQNT (Quebec). J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. This research has made use of NASA's Astrophysics Data System. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research also made use of the Chandra Transmission Grating Catalog and archive (http://tgcat.mit.edu). The SPH simulations presented in this paper made use of the resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 68 TC 4 Z9 4 U1 0 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 AUG 20 PY 2015 VL 809 IS 2 AR 132 DI 10.1088/0004-637X/809/2/132 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100025 ER PT J AU Guillochon, J Ramirez-Ruiz, E AF Guillochon, James Ramirez-Ruiz, Enrico TI A DARK YEAR FOR TIDAL DISRUPTION EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; gravitation ID MASSIVE BLACK-HOLE; OBLIQUE SHOCK BREAKOUT; GALACTIC NUCLEI; STELLAR DISRUPTION; WHITE-DWARFS; SWIFT J1644+57; DISK ACCRETION; STARS; DYNAMICS; FLARES AB Main-sequence disruptions of stars by supermassive black holes result in the production of an extended, geometrically thin debris stream winding repeatedly around the black hole. In the absence of black hole spin, inplane relativistic precession causes this stream to intersect with itself after a single winding. In this paper we show that relativistic precessions arising from black hole spin can induce deflections out of the original orbital plane that prevent the stream from self-intersecting even after many windings. This naturally leads to a " dark period" in which the flare is not observable for some time, persisting for up to a dozen orbital periods of the most bound material, which translates to years for disruptions around black holes with masses similar to 10(7)M(circle dot). When the stream eventually self-intersects, the distance from the black hole and the angle at which this collision occurs determine the rate of energy dissipation. We find that more-massive black holes (M-h greater than or similar to 10(7)M(circle dot)) tend to have more violent stream self-intersections, resulting in prompt accretion. For these tidal disruption events (TDEs), the accretion rate onto the black hole should still closely follow the original fallback rate after a fixed delay time t(delay), (M) over dot(acc) (t + t(delay) ) = (M) over dot (fb) (t). For lower black hole masses (M-h less than or similar to 10(6)), we find that flares are typically slowed down by about an order of magnitude, resulting in the majority of TDEs being sub-Eddington at peak. This also implies that current searches for TDEs are biased toward prompt flares, with slowed flares likely having been unidentified. C1 [Guillochon, James] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Guillochon, J (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM jguillochon@cfa.harvard.edu OI Guillochon, James/0000-0002-9809-8215 FU Aspen Center for Physics (NSF) [1066293]; Einstein grant [PF3-140108]; Packard grant; NASA ATP grant [NNX14AH37G] FX We thank J. Dexter, G. Farrar, A. Gruzinov, Y. Jiang, D. Kasen, J. Krolik, A. Loeb, M. MacLeod, M. McCourt, M. Rees, E. Rossi, N. Roth, J. Steiner, N. Stone, and E. Tejeda for useful discussions, and the Aspen Center for Physics (NSF grant 1066293) for their hospitality. We also would like to thank the anonymous referee for their helpful suggestions. This work was supported by Einstein grant PF3-140108 (J. G.), the Packard grant (E. R.), and NASA ATP grant NNX14AH37G (E. R.). NR 66 TC 21 Z9 21 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 AUG 20 PY 2015 VL 809 IS 2 AR 166 DI 10.1088/0004-637X/809/2/166 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100059 ER PT J AU Guo, XY Esin, A Di Stefano, R Taylor, J AF Guo, Xinyi Esin, Ann Di Stefano, Rosanne Taylor, Jeffrey TI PERIODIC SIGNALS IN BINARY MICROLENSING EVENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; Galaxy: general; gravitational lensing: micro; methods: data analysis; planets and satellites: general ID TIME-SERIES; DIFFERENTIAL ROTATION; PLANET PHOTOMETRY; GALACTIC HALO; LIGHT CURVES; LENSES; DISCOVERY; DATABASE; SYSTEMS; STARS AB Gravitational microlensing events are powerful tools for the study of stellar populations. In particular, they can be used to discover and study a variety of binary systems. A large number of binary lenses have already been found through microlensing surveys and a few of these systems show strong evidence of orbital motion on the timescale of the lensing event. We expect that more binary lenses of this kind will be detected in the future. For binaries whose orbital period is comparable to the event duration, the orbital motion can cause the lensing signal to deviate drastically from that of a static binary lens. The most striking property of such light curves is the presence of quasi-periodic features, which are produced as the source traverses the same regions in the rotating lens plane. These repeating features contain information about the orbital period of the lens. If this period can be extracted, then much can be learned about the lensing system even without performing time-consuming, detailed light-curve modeling. However, the relative transverse motion between the source and the lens significantly complicates the problem of period extraction. To resolve this difficulty, we present a modification of the standard Lomb-Scargle periodogram analysis. We test our method for four representative binary lens systems and demonstrate its efficiency in correctly extracting binary orbital periods. C1 [Guo, Xinyi; Di Stefano, Rosanne] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guo, Xinyi] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA. [Esin, Ann; Taylor, Jeffrey] Harvey Mudd Coll, Dept Phys, Claremont, CA 91711 USA. RP Guo, XY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST-1211843, AST-0708924, AST-0908878]; NASA [NNX12AE39GAR-13243.01-A] FX We thank Christopher Night for significant contributions to an earlier version of this work and the anonymous referee for constructive comments. This work was supported in part by support from NSF AST-1211843, AST-0708924, and AST-0908878 and NASA NNX12AE39GAR-13243.01-A. NR 35 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 AUG 20 PY 2015 VL 809 IS 2 AR 182 DI 10.1088/0004-637X/809/2/182 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100075 ER PT J AU Lansbury, GB Gandhi, P Alexander, DM Assef, RJ Aird, J Annuar, A Ballantyne, DR Balokovic, M Bauer, FE Boggs, SE Brandt, WN Brightman, M Christensen, FE Civano, F Comastri, A Craig, WW Del Moro, A Grefenstette, BW Hailey, CJ Harrison, FA Hickox, RC Koss, M LaMassa, SM Luo, B Puccetti, S Stern, D Treister, E Vignali, C Zappacosta, L Zhang, WW AF Lansbury, G. B. Gandhi, P. Alexander, D. M. Assef, R. J. Aird, J. Annuar, A. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Boggs, S. E. Brandt, W. N. Brightman, M. Christensen, F. E. Civano, F. Comastri, A. Craig, W. W. Del Moro, A. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Hickox, R. C. Koss, M. LaMassa, S. M. Luo, B. Puccetti, S. Stern, D. Treister, E. Vignali, C. Zappacosta, L. Zhang, W. W. TI NuSTAR REVEALS EXTREME ABSORPTION IN z < 0.5 TYPE 2 QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; HARD X-RAY; DIGITAL-SKY-SURVEY; SEYFERT 2 GALAXIES; COMPTON-THICK AGN; XMM-NEWTON OBSERVATIONS; ULTRALUMINOUS INFRARED GALAXIES; RESOLUTION SPECTRAL TEMPLATES; LUMINOUS OBSCURED QUASARS; APPROXIMATE-TO 2 AB The intrinsic column density (N-H) distribution of quasars is poorly known. At the high obscuration end of the quasar population and for redshifts z < 1, the X-ray spectra can only be reliably characterized using broad-band measurements that extend to energies above 10 keV. Using the hard X-ray observatory NuSTAR, along with archival Chandra and XMM-Newton data, we study the broad-band X-ray spectra of nine optically selected (from the SDSS), candidate Compton-thick (N-H > 1.5 x 10(24) cm(-2)) type 2 quasars (CTQSO2s); five new NuSTAR observations are reported herein, and four have been previously published. The candidate CTQSO2s lie at z < 0.5, have observed [O III] luminosities in the range 8.4< log(L-[O III]/L circle dot)< 9.6, and show evidence for extreme, Compton-thick absorption when indirect absorption diagnostics are considered. Among the nine candidate CTQSO2s, five are detected by NuSTAR in the high-energy (8-24 keV) band: two are weakly detected at the approximate to 3 sigma confidence level and three are strongly detected with sufficient counts for spectral modeling (greater than or similar to 90 net source counts at 8-24 keV). For these NuSTAR-detected sources direct (i.e., X-ray spectral) constraints on the intrinsic active galactic nucleus properties are feasible, and we measure column densities approximate to 2.5-1600 times higher and intrinsic (unabsorbed) X-ray luminosities approximate to 10-70 times higher than pre-NuSTAR constraints from Chandra and XMM-Newton. Assuming the NuSTAR-detected type 2 quasars are representative of other Compton-thick candidates, we make a correction to the N-H distribution for optically selected type 2 quasars as measured by Chandra and XMM-Newton for 39 objects. With this approach, we predict a Compton-thick fraction of f(CT) = 36(-12)(+14)%, although higher fractions (up to 76%) are possible if indirect absorption diagnostics are assumed to be reliable. C1 [Lansbury, G. B.; Gandhi, P.; Alexander, D. M.; Annuar, A.; Del Moro, A.] Univ Durham, Ctr Extragalact Astron, Dept Phys, Durham DH1 3LE, England. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17, Hants, England. [Assef, R. J.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Santiago, Chile. [Aird, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Brightman, M.; Grefenstette, B. W.; Harrison, F. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Civano, F.; LaMassa, S. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, F.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, M.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.; Zappacosta, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Vignali, C.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lansbury, GB (reprint author), Univ Durham, Ctr Extragalact Astron, Dept Phys, South Rd, Durham DH1 3LE, England. EM g.b.lansbury@durham.ac.uk RI Comastri, Andrea/O-9543-2015; Vignali, Cristian/J-4974-2012; Brandt, William/N-2844-2015; Boggs, Steven/E-4170-2015; OI Comastri, Andrea/0000-0003-3451-9970; Lansbury, George/0000-0002-5328-9827; Vignali, Cristian/0000-0002-8853-9611; Puccetti, Simonetta/0000-0002-2734-7835; Brandt, William/0000-0002-0167-2453; Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Ballantyne, David/0000-0001-8128-6976 FU Science and Technology Facilities Council (STFC) [ST/K501979/1, ST/J003697/1, ST/I001573/1]; Leverhulme Trust; Gemini-CONICYT [32120009]; ERC Advanced Grant FEEDBACK at the University of Cambridge; NSF AST award [1008067]; NASA Earth and Space Science Fellowship Program [NNX14AQ07H]; CONICYT-Chile [PFB-06/2007, FONDECYT 1141218, ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Caltech NuSTAR subcontract [44A-1092750]; NASA ADP grant [NNX10AC99G]; Caltech Kingsley visitor program; ASI/INAF [I/037/12/0011/13]; NASA ADAP award [NNX12AE38G]; National Science Foundation [1211096]; Swiss National Science Foundation [PP00P2_138979/1]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank the referee for a careful review, which has improved this work. We acknowledge financial support from: the Science and Technology Facilities Council (STFC) grants ST/K501979/1 (G.B.L.), ST/J003697/1 (P.G.), ST/I001573/1 (D.M.A. and A.D.M.); the Leverhulme Trust (D.M.A.); Gemini-CONICYT grant 32120009 (R.J.A.); the ERC Advanced Grant FEEDBACK at the University of Cambridge (J.A.); NSF AST award 1008067 (D.R.B.); the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H (M.B.); CONICYT-Chile grants Basal-CATA PFB-06/2007 (F.E.B.), FONDECYT 1141218 (F.E.B.), and "EMBIGGEN" Anillo ACT1101 (F.E.B.); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.); Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.); NASA ADP grant NNX10AC99G (W.N.B. and B.L.); the Caltech Kingsley visitor program (A.C.); ASI/INAF grant I/037/12/0011/13 (A.C., S.P., C.V.); NASA ADAP award NNX12AE38G (R.C.H.); National Science Foundation grant 1211096 (R.C.H.); and Swiss National Science Foundation grant PP00P2_138979/1 (M.K.). We thank Andrew Ptak and Jianjun Jia for the useful correspondence. 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). NR 112 TC 21 Z9 21 U1 1 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 AUG 20 PY 2015 VL 809 IS 2 AR 115 DI 10.1088/0004-637X/809/2/115 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100008 ER PT J AU Nichols, J Huenemoerder, DP Corcoran, MF Waldron, W Naze, Y Pollock, AMT Moffat, AFJ Lauer, J Shenar, T Russell, CMP Richardson, ND Pablo, H Evans, NR Hamaguchi, K Gull, T Hamann, WR Oskinova, L Ignace, R Hoffman, JL Hole, KT Lomax, JR AF Nichols, J. Huenemoerder, D. P. Corcoran, M. F. Waldron, W. Naze, Y. Pollock, A. M. T. Moffat, A. F. J. Lauer, J. Shenar, T. Russell, C. M. P. Richardson, N. D. Pablo, H. Evans, N. R. Hamaguchi, K. Gull, T. Hamann, W. -R. Oskinova, L. Ignace, R. Hoffman, Jennifer L. Hole, K. T. Lomax, J. R. TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. II. X-RAY VARIABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: individual ([HD 36486]delta Ori A) ID EARLY-TYPE STARS; SHORT-TERM VARIABILITY; HELIUM-LIKE IONS; O-TYPE STARS; ABSORPTION COMPONENTS; LINE INTENSITIES; COLLIDING WINDS; MAIN-SEQUENCE; ZETA-OPHIUCHI; TIME-SERIES AB We present time-resolved and phase-resolved variability studies of an extensive X-ray high-resolution spectral data set of the delta Ori Aa binary system. The four observations, obtained with Chandra ACIS HETGS, have a total exposure time of approximate to 479 ks and provide nearly complete binary phase coverage. Variability of the total X-ray flux in the range of 5-25 is is confirmed, with a maximum amplitude of about +/- 15% within a single approximate to 125 ks observation. Periods of 4.76 and 2.04 days are found in the total X-ray flux, as well as an apparent overall increase in the flux level throughout the nine-day observational campaign. Using 40 ks contiguous spectra derived from the original observations, we investigate the variability of emission line parameters and ratios. Several emission lines are shown to be variable, including S XV, Si XIII, and Ne IX. For the first time, variations of the X-ray emission line widths as a function of the binary phase are found in a binary system, with the smallest widths at phi = 0.0 when the secondary delta Ori Aa2 is at the inferior conjunction. Using 3D hydrodynamic modeling of the interacting winds, we relate the emission line width variability to the presence of a wind cavity created by a wind-wind collision, which is effectively void of embedded wind shocks and is carved out of the X-ray-producing primary wind, thus producing phase-locked X-ray variability. C1 [Nichols, J.; Lauer, J.; Evans, N. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huenemoerder, D. P.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.; Hamaguchi, K.] NASA GSFC, XRay Astrophys Lab, Greenbelt, MD 20771 USA. [Waldron, W.] Univ Space Res Assoc, Columbia, MD 21046 USA. [Naze, Y.] Eureka Sci Inc, Oakland, CA 94602 USA. [Pollock, A. M. T.] Univ Liege, FNRS Dept AGO, B-4000 Liege, Belgium. [Moffat, A. F. J.; Richardson, N. D.; Pablo, H.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain. [Shenar, T.; Hamann, W. -R.; Oskinova, L.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Hamaguchi, K.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Gull, T.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Ignace, R.] NASA GSFC, Greenbelt, MD 20771 USA. [Hoffman, Jennifer L.] E Tennessee State Univ, Phys & Astron, Johnson City, TN 37614 USA. [Hole, K. T.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Lomax, J. R.] Weber State Univ, Dept Phys, Ogden, UT 84408 USA. [Russell, C. M. P.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Russell, C. M. P.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. RP Nichols, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU National Aeronautics and Space Administration through Chandra Award [GO3-14015A, G03-14015E, GO3-14015G]; National Aeronautics Space Administration [NAS8-03060]; NASA through the Smithsonian Astrophysical Observatory [SV3-73016]; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMM and Integral contracts; Action de Recherche Concertee (CFWB-Academie Wallonie Europe); NSRC (Canada); FRQNT (Quebec); CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship; DLR [50 OR 1302]; Chandra X-ray Center NASA [NAS8-03060]; NASA [NNX13AF40G]; NSF [AST-0807477] FX The authors acknowledge the constructive comments of the anomymous referee. M.F.C., J.S.N., W.L.W., C.M.P.R., and K.H. are grateful for support provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14015A, G03-14015E, and GO3-14015G 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. D.P.H. was supported by NASA through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for the Chandra X-ray Center and Science Instruments. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the Action de Recherche Concertee (CFWB-Academie Wallonie Europe). A.F.J.M. is grateful for financial aid from NSRC (Canada) and FRQNT (Quebec). N.D.R. gratefully acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. L.M.O. acknowledges support from DLR grant 50 OR 1302. N.R.E. is grateful for support from the Chandra X-ray Center NASA Contract NAS8-03060. J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. M.F.C., J.S.N., and K.H. also acknowledge helpful discussions with John Houck and Michael Nowak on data analysis with ISIS, and Craig Anderson for technical support. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research made use of the Chandra Transmission Grating Catalog and archive (http://tgcat.mit.edu). This research also has made use of NASA's Astrophysics Data System. NR 80 TC 5 Z9 5 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 AUG 20 PY 2015 VL 809 IS 2 AR 133 DI 10.1088/0004-637X/809/2/133 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100026 ER PT J AU Nunez, A Agueros, MA Covey, KR Hartman, JD Kraus, AL Bowsher, EC Douglas, ST Lopez-Morales, M Pooley, DA Posselt, B Saar, SH West, AA AF Nunez, Alejandro Agueeros, Marcel A. Covey, Kevin R. Hartman, Joel D. Kraus, Adam L. Bowsher, Emily C. Douglas, Stephanie T. Lopez-Morales, Mercedes Pooley, David A. Posselt, Bettina Saar, Steven H. West, Andrew A. TI LINKING STELLAR CORONAL ACTIVITY AND ROTATION AT 500 MYR: A DEEP CHANDRA OBSERVATION OF M37 SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (M37); stars: activity; stars: coronae; stars: rotation X-rays: individual (M37) ID X-RAY-EMISSION; SOLAR-TYPE STARS; LOW-MASS STARS; PERSEI OPEN CLUSTER; DIGITAL SKY SURVEY; MMT1 TRANSIT SURVEY; FIELD-NORTH SURVEY; ALPHA-PERSEI; MAGNETIC ACTIVITY; RADIAL-VELOCITIES AB Empirical calibrations of the stellar age-rotation-activity relation (ARAR) rely on observations of the co-eval populations of stars in open clusters. We used the Chandra X-ray Observatory to study M37, a 500-Myr-old open cluster that has been extensively surveyed for rotation periods (P-rot). M37 was observed almost continuously for five days, for a total of 440.5 ks, to measure stellar X-ray luminosities (L-X), a proxy for coronal activity, across a wide range of masses. The cluster's membership catalog was revisited to calculate updated membership probabilities from photometric data and each star's distance to the cluster center. The result is a comprehensive sample of 1699 M37 members: 426 with Prot, 278 with X-ray detections, and 76 with both. We calculate Rossby numbers, R-o = P-rot/T, where T is the convective turnover time, and ratios of the X-ray-to-bolometric luminosity, L-X/L-bol, to minimize mass dependencies in our characterization of the rotation-coronal activity relation at 500 Myr. We find that fast rotators, for which R-o< 0.09 +/- 0.01, show saturated levels of activity, with log(L-X/L-bol) = -3.06 +/- 0.04. For R-o. 0.09 +/- 0.01, activity is unsaturated and follows a power law of the form Ro b, where beta = -2.03(-0.14)(+0.17). This is the largest sample available for analyzing the dependence of coronal emission on rotation for a single-aged population, covering stellar masses in the range 0.4-1.3 M-circle dot, P-rot in the range 0.4-12.8 days, and L-X in the range 10(28.4-30.5) erg s(-1). Our results make M37 a new benchmark open cluster for calibrating the ARAR at ages of approximate to 500 Myr. C1 [Nunez, Alejandro; Agueeros, Marcel A.; Bowsher, Emily C.; Douglas, Stephanie T.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Covey, Kevin R.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Hartman, Joel D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kraus, Adam L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Lopez-Morales, Mercedes; Saar, Steven H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02183 USA. [Pooley, David A.] Sam Houston State Univ, Dept Phys, Huntsville, TX 77341 USA. [Pooley, David A.] Eureka Sci Inc, Oakland, CA 94602 USA. [Posselt, Bettina] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [West, Andrew A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Nunez, A (reprint author), Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA. OI Nunez, Alejandro/0000-0002-8047-1982; Douglas, Stephanie/0000-0001-7371-2832; Posselt, Bettina/0000-0003-2317-9747; Covey, Kevin/0000-0001-6914-7797; Hartman, Joel/0000-0001-8732-6166; Agueros, Marcel/0000-0001-7077-3664 FU NASA through Chandra Award [G02-13025A]; NASA [NAS8-03060]; NSF [AST-1255419] FX We thank the referee for a careful reading of the paper. We thank Patrick Broos for his help with the AE package and Maureen van den Berg for her help with obtaining unabsorbed X-ray fluxes. Support for this work was provided by NASA through Chandra Award Number G02-13025A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. M.A.A. acknowledges support provided by the NSF through grant AST-1255419. NR 81 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 AUG 20 PY 2015 VL 809 IS 2 AR 161 DI 10.1088/0004-637X/809/2/161 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100054 ER PT J AU Pablo, H Richardson, ND Moffat, AFJ Corcoran, M Shenar, T Benvenuto, O Fuller, J Naze, Y Hoffman, JL Miroshnichenko, A Apellaniz, JM Evans, N Eversberg, T Gayley, K Gull, T Hamaguchi, K Hamann, WR Henrichs, H Hole, T Ignace, R Iping, R Lauer, J Leutenegger, M Lomax, J Nichols, J Oskinova, L Owocki, S Pollock, A Russell, CMP Waldron, W Buil, C Garrel, T Graham, K Heathcote, B Lemoult, T Li, D Mauclaire, B Potter, M Ribeiro, J Matthews, J Cameron, C Guenther, D Kuschnig, R Rowe, J Rucinski, S Sasselov, D Weiss, W AF Pablo, Herbert Richardson, Noel D. Moffat, Anthony F. J. Corcoran, Michael Shenar, Tomer Benvenuto, Omar Fuller, Jim Naze, Yael Hoffman, Jennifer L. Miroshnichenko, Anatoly Apellaniz, Jesus Maiz Evans, Nancy Eversberg, Thomas Gayley, Ken Gull, Ted Hamaguchi, Kenji Hamann, Wolf-Rainer Henrichs, Huib Hole, Tabetha Ignace, Richard Iping, Rosina Lauer, Jennifer Leutenegger, Maurice Lomax, Jamie Nichols, Joy Oskinova, Lida Owocki, Stan Pollock, Andy Russell, Christopher M. P. Waldron, Wayne Buil, Christian Garrel, Thierry Graham, Keith Heathcote, Bernard Lemoult, Thierry Li, Dong Mauclaire, Benjamin Potter, Mike Ribeiro, Jose Matthews, Jaymie Cameron, Chris Guenther, David Kuschnig, Rainer Rowe, Jason Rucinski, Slavek Sasselov, Dimitar Weiss, Werner TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. III. ANALYSIS OF OPTICAL PHOTOMETRIC (MOST) AND SPECTROSCOPIC (GROUND BASED) VARIATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: early-type; stars: individual (delta Ori A); stars: mass-loss; stars: variables: general ID APSIDAL MOTION; STARS; SYSTEM; PULSATIONS; KOI-54; SPECTRA; ORBITS; SPOTS; ORI AB We report on both high-precision photometry from the Microvariability and Oscillations of Stars (MOST) space telescope and ground-based spectroscopy of the triple system delta Ori A, consisting of a binary O9.5II+early-B (Aa1 and Aa2) with P = 5.7 days, and a more distant tertiary (O9 IV P > 400 years). This data was collected in concert with X-ray spectroscopy from the Chandra X-ray Observatory. Thanks to continuous coverage for three weeks, the MOST light curve reveals clear eclipses between Aa1 and Aa2 for the first time in non-phased data. From the spectroscopy, we have a well-constrained radial velocity (RV) curve of Aa1. While we are unable to recover RV variations of the secondary star, we are able to constrain several fundamental parameters of this system and determine an approximate mass of the primary using apsidal motion. We also detected second order modulations at 12 separate frequencies with spacings indicative of tidally influenced oscillations. These spacings have never been seen in a massive binary, making this system one of only a handful of such binaries that show evidence for tidally induced pulsations. C1 [Pablo, Herbert; Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Pablo, Herbert; Richardson, Noel D.; Moffat, Anthony F. J.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada. [Corcoran, Michael; Hamaguchi, Kenji] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Corcoran, Michael; Hamaguchi, Kenji] NASA GSFC, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, Michael; Iping, Rosina] Univ Space Res Assoc, Columbia, MD 21046 USA. [Shenar, Tomer; Hamann, Wolf-Rainer; Oskinova, Lida] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Benvenuto, Omar] Univ Nacl La Plata, Fac Ciencias Astron & Geofis, RA-1900 Buenos Aires, DF, Argentina. [Benvenuto, Omar] UNLP, CONICET, CCT, IALP, La Plata, Buenos Aires, Argentina. [Fuller, Jim] CALTECH, Walter Burke Inst Theoret Phys, TAPIR, Pasadena, CA 91125 USA. [Fuller, Jim; Leutenegger, Maurice] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Naze, Yael] Univ Liege, FNRS Dept AGO, B-4000 Liege, Belgium. [Hoffman, Jennifer L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Miroshnichenko, Anatoly] Univ N Carolina, Dept Phys & Astron, Greensboro, NC 27402 USA. [Apellaniz, Jesus Maiz] Ctr Astrobiol CSIC INTA, E-28691 Villanueva De La Caada, Spain. [Evans, Nancy; Lauer, Jennifer; Nichols, Joy] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Eversberg, Thomas] Schnorringen Telescope Sci Inst, Waldbrol, Germany. [Gayley, Ken] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Gull, Ted] NASA Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Henrichs, Huib] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Hole, Tabetha; Ignace, Richard] E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA. [Lomax, Jamie] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Owocki, Stan] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Pollock, Andy] European Space Agcy, E-28691 Madrid, Spain. [Russell, Christopher M. P.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Russell, Christopher M. P.] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. [Waldron, Wayne] Eureka Sci Inc, Oakland, CA 94602 USA. [Buil, Christian] Castanet Tolosan Observ, F-31320 Castanet Tolosan, France. [Garrel, Thierry] Observ Juvignac, F-34990 Juvignac, France. [Heathcote, Bernard] Barfold Observ, Glenhope, Vic 3444, Australia. [Lemoult, Thierry] Chelles Observ, F-77500 Chelles, France. [Li, Dong] Jade Observ, Tianjin 300251, Peoples R China. [Mauclaire, Benjamin] Observ Val Arc, F-13530 Trets, France. [Ribeiro, Jose] Observ Inst Geog Exercito, Lisbon, Portugal. [Matthews, Jaymie; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Canada. [Guenther, David] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Kuschnig, Rainer] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Rowe, Jason] NASA Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, Slavek] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pablo, H (reprint author), Univ Montreal, Dept Phys, CP 6128,Succ Ctr Ville, Montreal, PQ H3C 3J7, Canada. EM hpablo@astro.umontreal.ca; richardson@astro.umontreal.ca FU Chandra grant [GO3-14015A, GO3-14015E]; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMMAction de Recherche Concertee (CFWB-Academie Wallonie Europe); CRAQ (Centre de Recherche en Astrophysique du Quebec); Spanish Government Ministerio de Economia y Competitividad (MINECO) [AYA2010-15 081, AYA2010-17 631, AYA2013-40 611-P]; Consejeria de Educacion of the Junta de Andalucia [P08-TIC-4075]; Austrian Science Fund (FWF); Chandra X-ray Center NASA [NAS8-03060]; NASA [NNX13AF40G]; NSF [AST-0807477] FX M.F.C., J.S.N., W.L.W., and K.H. are grateful for support via Chandra grant GO3-14015A and GO3-14015E. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the Action de Recherche Concertee (CFWB-Academie Wallonie Europe). N.D.R. gratefully acknowledges his CRAQ (Centre de Recherche en Astrophysique du Quebec) fellowship. A.F.J.M., D.B.G., J.M.M., and S.M.R. are grateful for financial aid to NSERC (Canada). A.F.J.M. and H.P. also thank FRQNT (Quebec) and the Canadian Space Agency. J.M.A. acknowledges support from (a) the Spanish Government Ministerio de Economia y Competitividad (MINECO) through grants AYA2010-15 081, AYA2010-17 631, and AYA2013-40 611-P and (b) the Consejeria de Educacion of the Junta de Andalucia through grant P08-TIC-4075. R.K. and W.W. acknowledge support by the Austrian Science Fund (FWF). N.R.E. is grateful for support from the Chandra X-ray Center NASA Contract NAS8-03060. J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. NR 61 TC 4 Z9 4 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 AUG 20 PY 2015 VL 809 IS 2 AR 134 DI 10.1088/0004-637X/809/2/134 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100027 ER PT J AU Roettenbacher, RM Monnier, JD Fekel, FC Henry, GW Korhonen, H Latham, DW Muterspaugh, MW Williamson, MH Baron, F ten Brummelaar, TA Che, X Harmon, RO Schaefer, GH Scott, NJ Sturmann, J Sturmann, L Turner, NH AF Roettenbacher, Rachael M. Monnier, John D. Fekel, Francis C. Henry, Gregory W. Korhonen, Heidi Latham, David W. Muterspaugh, Matthew W. Williamson, Michael H. Baron, Fabien ten Brummelaar, Theo A. Che, Xiao Harmon, Robert O. Schaefer, Gail H. Scott, Nicholas J. Sturmann, Judit Sturmann, Laszlo Turner, Nils H. TI DETECTING THE COMPANIONS AND ELLIPSOIDAL VARIATIONS OF RS CVN PRIMARIES. II. o DRACONIS, A CANDIDATE FOR RECENT LOW-MASS COMPANION INGESTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: activity; stars: imaging; stars: individual (o Draconis); stars: variables: general ID CLOSE BINARY-SYSTEMS; CHROMOSPHERICALLY ACTIVE STARS; CHARA ARRAY; SPECTROSCOPIC BINARIES; MODEL ATMOSPHERES; PRECISION ORBITS; SIGMA-GEMINORUM; TIDAL EVOLUTION; MAIN-SEQUENCE; ROTATION AB To measure the stellar and orbital properties of the metal-poor RS CVn binary o Draconis (o Dra), we directly detect the companion using interferometric observations obtained with the Michigan InfraRed Combiner at Georgia State University's Center for High Angular Resolution Astronomy (CHARA) Array. The H-band flux ratio between the primary and secondary stars is the highest confirmed flux ratio (370 +/- 40) observed with long-baseline optical interferometry. These detections are combined with radial velocity data of both the primary and secondary stars, including new data obtained with the Tillinghast Reflector Echelle Spectrograph on the Tillinghast Reflector at the Fred Lawrence Whipple Observatory and the 2 m Tennessee State University Automated Spectroscopic Telescope at Fairborn Observatory. We determine an orbit from which we find model-independent masses and ages of the components (M-A=1.35 +/- 0.05M., MB=0.99 +/- 0.02M(circle dot), system age = 3.0. -/+ 0.5 Gyr). An average of a 23-year light curve of o Dra from the Tennessee State University Automated Photometric Telescope folded over the orbital period newly reveals eclipses and the quasi-sinusoidal signature of ellipsoidal variations. The modeled light curve for our system's stellar and orbital parameters confirm these ellipsoidal variations due to the primary star partially filling its Roche lobe potential, suggesting most of the photometric variations are not due to stellar activity (starspots). Measuring gravity darkening from the average light curve gives a best-fit of beta=0.07 +/- 0.03, a value consistent with conventional theory for convective envelope stars. The primary star also exhibits an anomalously short rotation period, which, when taken with other system parameters, suggests the star likely engulfed a low-mass companion that had recently spun-up the star. C1 [Roettenbacher, Rachael M.; Monnier, John D.; Baron, Fabien; Che, Xiao] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Fekel, Francis C.; Henry, Gregory W.; Muterspaugh, Matthew W.; Williamson, Michael H.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Korhonen, Heidi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [ten Brummelaar, Theo A.; Schaefer, Gail H.; Scott, Nicholas J.; Sturmann, Judit; Sturmann, Laszlo; Turner, Nils H.] Georgia State Univ, Ctr High Angular Resolut Astron, Mt Wilson, CA 91023 USA. [Harmon, Robert O.] Ohio Wesleyan Univ, Dept Phys & Astron, Delaware, OH 43015 USA. RP Roettenbacher, RM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM rmroett@umich.edu RI Korhonen, Heidi/E-3065-2016; OI Korhonen, Heidi/0000-0003-0529-1161; Fekel, Francis/0000-0002-9413-3896; Latham, David/0000-0001-9911-7388 FU National Science Foundation through NSF [AST-0908253, AST-1211129]; Georgia State University through the College of Arts and Sciences; University of Michigan; NSF from the Major Research Instrumentation Program [1039522]; NASA; NSF [AST-1108963]; Tennessee State University; Centers of Excellence Program; NASA Harriet G. Jenkins Pre-Doctoral Fellowship; Sigma Xi FX We thank F. C. Adams, J. A. Orosz, D. Pourbaix, and M. Rieutord for their help and comments, as well as L. Boyd of Fairborn Observatory for his support of the photometric observations. The interferometric data in this paper were obtained at the CHARA Array, funded by the National Science Foundation through NSF grants AST-0908253 and AST-1211129, and by Georgia State University through the College of Arts and Sciences. The MIRC instrument at the CHARA Array was funded by the University of Michigan. NSF grant 1039522 from the Major Research Instrumentation Program, awarded to Tennessee State University, made extracting the secondary velocities possible. Astronomy at Tennessee State University is supported by the state of Tennessee through its Centers of Excellence program. The APT program was supported by NASA, NSF, Tennessee State University, and the Centers of Excellence Program. The Nordic Optical Telescope is 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. R.M.R. would like to acknowledge support from the NASA Harriet G. Jenkins Pre-Doctoral Fellowship and a Sigma Xi Grant-in-Aid of Research. J.D.M. and R.M.R. acknowledge support of NSF grant AST-1108963. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and the Jean-Marie Mariotti Center SearchCal service8 co-developed by FIZEAU and LAOG/IPAG, and of CDS Astronomical Databases SIMBAD and VIZIER.9 NR 66 TC 4 Z9 4 U1 0 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 AUG 20 PY 2015 VL 809 IS 2 AR 159 DI 10.1088/0004-637X/809/2/159 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100052 ER PT J AU Shenar, T Oskinova, L Hamann, WR Corcoran, MF Moffat, AFJ Pablo, H Richardson, ND Waldron, WL Huenemoerder, DP Apellaniz, JM Nichols, JS Todt, H Naze, Y Hoffman, JL Pollock, AMT Negueruela, I AF Shenar, T. Oskinova, L. Hamann, W. -R. Corcoran, M. F. Moffat, A. F. J. Pablo, H. Richardson, N. D. Waldron, W. L. Huenemoerder, D. P. Maiz Apellaniz, J. Nichols, J. S. Todt, H. Naze, Y. Hoffman, J. L. Pollock, A. M. T. Negueruela, I. TI A COORDINATED X-RAY AND OPTICAL CAMPAIGN OF THE NEAREST MASSIVE ECLIPSING BINARY, delta ORIONIS Aa. IV. A MULTIWAVELENGTH, NON-LTE SPECTROSCOPIC ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; stars: early-type; stars: individual ([HD 36486]delta Ori A); X-rays: stars ID O-TYPE STARS; RADIATION-DRIVEN WINDS; BLANKETED MODEL ATMOSPHERES; EMISSION-LINE-PROFILES; B-TYPE SUPERGIANTS; HELIUM-LIKE IONS; STELLAR WINDS; GALACTIC O; LOSS RATES; COMPOSITE SPECTRA AB Eclipsing systems of massive stars allow one to explore the properties of their components in great detail. We perform a multi-wavelength, non-LTE analysis of the three components of the massive multiple system delta Ori A, focusing on the fundamental stellar properties, stellar winds, and X-ray characteristics of the system. The primary's distance-independent parameters turn out to be characteristic for its spectral type (O9.5 II), but usage of the Hipparcos parallax yields surprisingly low values for the mass, radius, and luminosity. Consistent values follow only if delta Ori lies at about twice the Hipparcos distance, in the vicinity of the sigma-Orionis cluster. The primary and tertiary dominate the spectrum and leave the secondary only marginally detectable. We estimate the V-band magnitude difference between primary and secondary to be Delta V approximate to 2.(m)8. The inferred parameters suggest that the secondary is an early B-type dwarf (approximate to B1 V), while the tertiary is an early B-type subgiant (approximate to B0 IV). We find evidence for rapid turbulent velocities (similar to 200 km s(-1)) and wind inhomogeneities, partially optically thick, in the primary's wind. The bulk of the X-ray emission likely emerges from the primary's stellar wind (logL(X)/L-Bol approximate to -6.85), initiating close to the stellar surface at R-0 similar to 1.1 R-*. Accounting for clumping, the mass-loss rate of the primary is found to be log (M) over dot approximate to -6.4 (M-circle dot yr(-1))., which agrees with hydrodynamic predictions, and provides a consistent picture along the X-ray, UV, optical, and radio spectral domains. C1 [Shenar, T.; Oskinova, L.; Hamann, W. -R.; Todt, H.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Corcoran, M. F.] NASA Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Corcoran, M. F.] NASA Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Corcoran, M. F.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Moffat, A. F. J.; Pablo, H.; Richardson, N. D.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Moffat, A. F. J.; Pablo, H.; Richardson, N. D.] Univ Montreal, CRAQ, Montreal, PQ H3C 3J7, Canada. [Waldron, W. L.] Eureka Sci Inc, Oakland, CA 94602 USA. [Huenemoerder, D. P.] MIT, Kalvi Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Maiz Apellaniz, J.] INTA CSIC, Ctr Astrobiol, E-28691 Madrid, Spain. [Nichols, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Naze, Y.] Univ Liege, Inst Astrophys & Geophys, Grp Astrophys Hautes Energies, B-4000 Sart Tilman Par Liege, Belgium. [Hoffman, J. L.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Pollock, A. M. T.] European Space Agcy, XMM Newton Sci Operat Ctr, European Space Astron Ctr, E-28691 Villanueva De La Canada, Spain. [Negueruela, I.] Univ Alicante, Escuela Politecn Super, Dept Fis Ingn Sistemas & Teoria Senal, E-03080 Alicante, Spain. RP Shenar, T (reprint author), Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany. FU Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics; Leibniz Institute for Astrophysics Potsdam (AIP); institute of Physics and Astronomy of the University of Potsdam; DLR [50 OR 1302]; Chandra grants [GO3-14015A, GO3-14015E]; NSERC (Canada); FRQNT (Quebec); Spanish Government Ministerio de Economia y Competitividad (MINECO) [AYA2010-15 081, AYA2010-17 631]; Consejeria de Educacion of the Junta de Andaluc ia [P08-TIC-4075]; Centre du Recherche en Astrophysique du Quebec (CRAQ) fellowship; Fonds National de la Recherche Scientifique (Belgium); Communaute Francaise de Belgique; PRODEX XMM and Integral contracts; "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe); NASA [NNX13AF40G]; NSF [AST-0807477]; Spanish Mineco [AYA2012-39364-C02-01/02]; European Union FX We thank the anonymous referee for constructive comments which helped to improve our paper. T.S. is grateful for financial support from the Leibniz Graduate School for Quantitative Spectroscopy in Astrophysics, a joint project of the Leibniz Institute for Astrophysics Potsdam (AIP) and the institute of Physics and Astronomy of the University of Potsdam. L.M.O. acknowledges support from DLR grant 50 OR 1302. We thank A. Valeev and S. Fabrika for kindly providing us with an optical spectrum of the system. We thank T. J. Henry and J. A. Caballero for fruitful discussions regarding system's distance. M.F.C., J.S.N., and W.L.W. are grateful for support via Chandra grants GO3-14015A and GO3-14015E. A.F.J.M. acknowledges financial aid from NSERC (Canada) and FRQNT (Quebec). J.M.A. acknowledges support from (a) the Spanish Government Ministerio de Economia y Competitividad (MINECO) through grants AYA2010-15 081 and AYA2010-17 631 and (b) the Consejeria de Educacion of the Junta de Andaluc ia through grant P08-TIC-4075. Caballero N.D.R. gratefully acknowledges his Centre du Recherche en Astrophysique du Quebec (CRAQ) fellowship. Y.N. acknowledges support from the Fonds National de la Recherche Scientifique (Belgium), the Communaute Francaise de Belgique, the PRODEX XMM and Integral contracts, and the "Action de Recherche Concertee" (CFWB-Academie Wallonie Europe). J.L.H. acknowledges support from NASA award NNX13AF40G and NSF award AST-0807477. I.N. is supported by the Spanish Mineco under grant AYA2012-39364-C02-01/02, and the European Union. NR 146 TC 13 Z9 13 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 AUG 20 PY 2015 VL 809 IS 2 AR 135 DI 10.1088/0004-637X/809/2/135 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100028 ER PT J AU Webb, T Noble, A DeGroot, A Wilson, G Muzzin, A Bonaventura, N Cooper, M Delahaye, A Foltz, R Lidman, C Surace, J Yee, HKC Chapman, S Dunne, L Geach, J Hayden, B Hildebrandt, H Huang, JS Pope, A Smith, MWL Perlmutter, S Tudorica, A AF Webb, Tracy Noble, Allison DeGroot, Andrew Wilson, Gillian Muzzin, Adam Bonaventura, Nina Cooper, Mike Delahaye, Anna Foltz, Ryan Lidman, Chris Surace, Jason Yee, H. K. C. Chapman, Scott Dunne, Loretta Geach, James Hayden, Brian Hildebrandt, Hendrik Huang, Jiasheng Pope, Alexandra Smith, Matthew W. L. Perlmutter, Saul Tudorica, Alex TI AN EXTREME STARBURST IN THE CORE OF A RICH GALAXY CLUSTER AT z=1.7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: evolution; galaxies: interactions; galaxies: starburst ID ACTIVE GALACTIC NUCLEI; NEAR-INFRARED PROPERTIES; STAR-FORMATION ACTIVITY; WIDE-FIELD CAMERA; SPECTROSCOPIC CONFIRMATION; COOLING FLOWS; STELLAR MASS; X-RAY; EXTRAGALACTIC SURVEY; PHOTOMETRIC SYSTEM AB We have discovered an optically rich galaxy cluster at z = 1.7089 with star formation occurring in close proximity to the central galaxy. The system, SpARCS104922.6+ 564032.5, was detected within the Spitzer Adaptation of the red-sequence Cluster Survey, and confirmed through Keck-MOSFIRE spectroscopy. The rest-frame optical richness of N-gal (500 kpc) = 30 +/- 8 implies a total halo mass, within 500 kpc, of similar to 3.8 +/- 1.2 x 10(14) M-circle dot, comparable to other clusters at or above this redshift. There is a wealth of ancillary data available, including Canada-France-Hawaii Telescope optical, UKIRT-K, Spitzer-IRAC/MIPS, and Herschel-SPIRE. This work adds submillimeter imaging with the SCUBA2 camera on the James Clerk Maxwell Telescope and near-infrared imaging with the Hubble Space Telescope. The mid/far-infrared (M/FIR) data detect an Ultra-luminous Infrared Galaxy spatially coincident with the central galaxy, with L-IR = 6.2 +/- 0.9 x 10(12) L-circle dot. The detection of polycyclic aromatic hydrocarbons at z = 1.7 in a Spitzer-IRS spectrum of the source implies the FIR luminosity is dominated by star formation (an Active Galactic Nucleus contribution of 20%) with a rate of similar to 860 +/- 130 M-circle dot yr(-1). The optical source corresponding to the IR emission is likely a chain of > 10 individual clumps arranged as " beads on a string" over a linear scale of 66 kpc. Its morphology and proximity to the Brightest Cluster Galaxy (BCG) imply a gas-rich interaction at the center of the cluster triggered the star formation. This system indicates that wet mergers may be an important process in forming the stellar mass of BCGs at early times. C1 [Webb, Tracy; Bonaventura, Nina; Delahaye, Anna] McGill Univ, Dept Phys, Montreal, PQ H3P 1T3, Canada. [Noble, Allison; Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [DeGroot, Andrew; Wilson, Gillian; Foltz, Ryan] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Muzzin, Adam; Chapman, Scott] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cooper, Mike] Univ Calif Irvine, Ctr Galaxy Evolut, Dept Phys & Astron, Irvine, CA 92697 USA. [Lidman, Chris] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Surace, Jason] CALTECH, Spitzer Space Sci Ctr, Pasadena, CA 91125 USA. [Chapman, Scott] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 2R4, Canada. [Dunne, Loretta] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Dunne, Loretta] Univ Edinburgh, Insitute Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Geach, James] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Hayden, Brian; Perlmutter, Saul] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Hildebrandt, Hendrik; Tudorica, Alex] Argelander Inst Astron, D-53121 Bonn, Germany. [Huang, Jiasheng] Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China. [Huang, Jiasheng] Chinese Acad Sci, China Chile Joint Ctr Astron, Santiago 1515, Chile. [Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pope, Alexandra] Univ Massachusetts, Dept Astron, Amherst, MA 01100 USA. [Smith, Matthew W. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Perlmutter, Saul] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Webb, T (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3P 1T3, Canada. FU W. M. Keck Foundation; NASA [NAS 5-26555]; US Department of Energy, Office of Science, Office of High Energy Physics [AC02-05CH11231]; European Research Council; NSERC; NASA from the Space Telescope Science Institute [GO-13306, GO-13677, GO-13747, GO-13845, GO-14327] FX 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. Financial support for this work was provided by NASA through program GO-13677 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. This material is based upon work supported in part by the US Department of Energy, Office of Science, Office of High Energy Physics, under contract No. AC02-05CH11231. 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. L.D. acknowledges support from European Research Council Advanced Grant: cosmicism. T.M.A.W. acknowledges the support of an NSERC Discovery Grant. Financial support for this work was provided by NASA through programs GO-13306, GO-13677, GO-13747, GO-13845, and GO-14327 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. NR 84 TC 11 Z9 11 U1 0 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 AUG 20 PY 2015 VL 809 IS 2 AR 173 DI 10.1088/0004-637X/809/2/173 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9EC UT WOS:000361655100066 ER PT J AU Huang, J Ouml;berg, KI AF Huang, Jane Oeberg, Karin I. TI DETECTION OF N2D+ IN A PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks ID DEUTERIUM FRACTIONATION; MOLECULAR-SPECTROSCOPY; DEUTERATED MOLECULES; INTERSTELLAR CLOUDS; COLOGNE DATABASE; DM TAURI; CHEMISTRY; CORES; LINE; ICE AB Observations of deuterium fractionation in the solar system, and in interstellar and circumstellar material, are commonly used to constrain the formation environment of volatiles. Toward protoplanetary disks, this approach has been limited by the small number of detected deuterated molecules, i.e., DCO+ and DCN. Based on ALMA Cycle 2 observations toward the disk around the T Tauri star AS 209, we report the first detection of N2D+ (J = 3-2) in a protoplanetary disk. These data are used together with previous Submillimeter Array observations of N2H+ (J = 3-2) to estimate a disk-averaged D/H ratio of 0.3-0.5, an order of magnitude higher than disk-averaged ratios previously derived for DCN/HCN and DCO+/HCO+ around other young stars. The high fractionation in N2H+ is consistent with model predictions. The presence of abundant N2D+ toward AS 209 also suggests that N2D+ and the N2D+/N2H+ ratio can be developed into effective probes of deuterium chemistry, kinematics, and ionization processes outside the CO snow line of disks. C1 [Huang, Jane; Oeberg, Karin I.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Huang, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Simons Collaboration on the Origins of Life (SCOL); Alfred P. Sloan Foundation; David and Lucile Packard Foundation FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00226. 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 thank Adam Leroy and the NAASC for assistance with calibration and imaging, Ryan Loomis and Viviana Guzman for helpful discussions on the data, and the referee for useful comments on the paper. K.I.O. also acknowledges funding from the Simons Collaboration on the Origins of Life (SCOL), the Alfred P. Sloan Foundation, and the David and Lucile Packard Foundation. NR 39 TC 1 Z9 1 U1 2 U2 3 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 AUG 20 PY 2015 VL 809 IS 2 AR L26 DI 10.1088/2041-8205/809/2/L26 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ6LI UT WOS:000360715500009 ER PT J AU Loomis, RA Cleeves, LI Oberg, KI Guzman, VV Andrews, SM AF Loomis, Ryan A. Cleeves, L. Ilsedore Oeberg, Karin I. Guzman, Viviana V. Andrews, Sean M. TI THE DISTRIBUTION AND CHEMISTRY OF H2CO IN THE DM TAU PROTOPLANETARY DISK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; circumstellar matter; ISM: molecules; protoplanetary disks; radio Lines: ISM ID CO SNOW LINE; ORGANIC-MOLECULES; H-2 FLUORESCENCE; CHEMICAL-MODEL; IMAGING SURVEY; COSMIC-RAYS; TW-HYDRAE; HD 163296; LY-ALPHA; X-RAY AB H2CO ice on dust grains is an important precursor of complex organic molecules (COMs). H2CO gas can be readily observed in protoplanetary disks and may be used to trace COM chemistry. However, its utility as a COM probe is currently limited by a lack of constraints on the relative contributions of two different formation pathways: on icy grain surfaces and in the gas phase. We use archival Atacama Large (sub-) Millimeter Array observations of the resolved distribution of H2CO emission in the disk around the young low-mass star DM Tau to assess the relative importance of these formation routes. The observed H2CO emission has a centrally peaked and radially broad brightness profile (extending out to 500 AU). We compare these observations with disk chemistry models with and without grain-surface formation reactions and find that both gas and grain-surface chemistry are necessary to explain the spatial distribution of the emission. Gas-phase H2CO production is responsible for the observed central peak, while grain-surface chemistry is required to reproduce the emission exterior to the CO snow line (where H2CO mainly forms through the hydrogenation of CO ice before being non-thermally desorbed). These observations demonstrate that both gas and grain-surface pathways contribute to the observed H2CO in disks and that their relative contributions depend strongly on distance from the host star. C1 [Loomis, Ryan A.; Oeberg, Karin I.; Guzman, Viviana V.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Cleeves, L. Ilsedore] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Loomis, RA (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM rloomis@cfa.harvard.edu OI Cleeves, L. Ilsedore/0000-0003-2076-8001 FU National Science Foundation Graduate Research Fellowship; NSF grant [AST-1008800]; Rackham Predoctoral Fellowship; Simons Collaboration on the Origins of Life (SCOL); Alfred P. Sloan Foundation; David and Lucile Packard Foundation FX We thank the anonymous referee for useful comments. We thank David Wilner and Charlie Qi for productive and insightful conversations. R.A.L. gratefully acknowledges funding from an National Science Foundation Graduate Research Fellowship. L.I.C. acknowledges support by NSF grant AST-1008800 and the Rackham Predoctoral Fellowship. K.I.O. also acknowledges funding from the Simons Collaboration on the Origins of Life (SCOL), the Alfred P. Sloan Foundation, and the David and Lucile Packard Foundation. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO. ALMA# 2011.0.00629.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. NR 52 TC 3 Z9 3 U1 1 U2 3 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 AUG 20 PY 2015 VL 809 IS 2 AR L25 DI 10.1088/2041-8205/809/2/L25 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ6LI UT WOS:000360715500008 ER PT J AU Laporta, GZ Linton, YM Wilkerson, RC Bergo, ES Nagaki, SS Sant'Ana, DC Sallum, MAM AF Laporta, Gabriel Zorello Linton, Yvonne-Marie Wilkerson, Richard C. Bergo, Eduardo Sterlino Nagaki, Sandra Sayuri Sant'Ana, Denise Cristina Mureb Sallum, Maria Anice TI Malaria vectors in South America: current and future scenarios SO PARASITES & VECTORS LA English DT Article DE Anopheles darlingi; Albitarsis Complex; Climate change; Ecological niche model; Plasmodium falciparum ID NYSSORHYNCHUS ALBITARSIS DIPTERA; POLYMERASE CHAIN-REACTION; CLIMATE-CHANGE; ANOPHELES-NYSSORHYNCHUS; POTENTIAL DISTRIBUTION; PLASMODIUM-FALCIPARUM; CULICIDAE; COMPLEX; BRAZIL; TRANSMISSION AB Background: Malaria remains a significant public health issue in South America. Future climate change may influence the distribution of the disease, which is dependent on the distribution of those Anopheles mosquitoes competent to transmit Plasmodium falciparum. Herein, predictive niche models of the habitat suitability for P. falciparum, the current primary vector Anopheles darlingi and nine other known and/or potential vector species of the Neotropical Albitarsis Complex, were used to document the current situation and project future scenarios under climate changes in South America in 2070. Methods: To build each ecological niche model, we employed topography, climate and biome, and the currently defined distribution of P. falciparum, An. darlingi and nine species comprising the Albitarsis Complex in South America. Current and future (i.e., 2070) distributions were forecast by projecting the fitted ecological niche model onto the current environmental situation and two scenarios of simulated climate change. Statistical analyses were performed between the parasite and each vector in both the present and future scenarios to address potential vector roles in the dynamics of malaria transmission. Results: Current distributions of malaria vector species were associated with that of P. falciparum, confirming their role in transmission, especially An. darlingi, An. marajoara and An. deaneorum. Projected climate changes included higher temperatures, lower water availability and biome modifications. Regardless of future scenarios considered, the geographic distribution of P. falciparum was exacerbated in 2070 South America, with the distribution of the pathogen covering 35-46 % of the continent. As the current primary vector An. darlingi showed low tolerance for drier environments, the projected climate change would significantly reduce suitable habitat, impacting both its distribution and abundance. Conversely, climate generalist members of the Albitarsis Complex showed significant spatial and temporal expansion potential in 2070, and we conclude these species will become more important in the dynamics of malaria transmission in South America. Conclusions: Our data suggest that climate and landscape effects will elevate the importance of members of the Albitarsis Complex in malaria transmission in South America in 2070, highlighting the need for further studies addressing the bionomics, ecology and behaviours of the species comprising the Albitarsis Complex. C1 [Laporta, Gabriel Zorello; Nagaki, Sandra Sayuri; Sant'Ana, Denise Cristina; Mureb Sallum, Maria Anice] Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-01255 Sao Paulo, SP, Brazil. [Laporta, Gabriel Zorello] Univ Sao Paulo, Fac Med, Lab Informat Med, Sao Paulo, SP, Brazil. [Laporta, Gabriel Zorello] Fac Med ABC, Setor Posgrad Pesquisa & Inovacao, Santo Andre, SP, Brazil. [Linton, Yvonne-Marie; Wilkerson, Richard C.] Walter Reed Army Inst Res, Div Entomol, Silver Spring, MD USA. [Linton, Yvonne-Marie; Wilkerson, Richard C.] Smithsonian Inst, Walter Reed Biosystemat Unit, Museum Support Ctr, Suitland, MD USA. [Linton, Yvonne-Marie; Wilkerson, Richard C.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Linton, Yvonne-Marie] Uniformed Serv Univ Hlth Sci, Dept Preventat Med & Biostat, Bethesda, MD 20814 USA. [Bergo, Eduardo Sterlino] Secretaria Estado Saude Sao Paulo, Superintendencia Controle Endemias SUCEN, Araraquara, SP, Brazil. RP Laporta, GZ (reprint author), Univ Sao Paulo, Fac Saude Publ, Dept Epidemiol, BR-01255 Sao Paulo, SP, Brazil. EM gabrielzorelo@usp.br RI Laporta, Gabriel/B-8662-2012; Nagaki, Sandra/G-7069-2016; OI Laporta, Gabriel/0000-0001-7412-9390 FU Sao Paulo Research Foundation (FAPESP) [2014/26229-7]; Brazilian National Council for Scientific and Technological Development (CNPq) [301666/2011-3]; National Institute of Health, USA [R01 AI50139-02]; FAPESP [2014/09774-1, 2015/09669-6] FX We gratefully acknowledge financial support from the Sao Paulo Research Foundation (FAPESP, Grant no. 2014/26229-7), the Brazilian National Council for Scientific and Technological Development (CNPq, Grant no. 301666/2011-3) to MAMS; RCW was partially supported by an award from the National Institute of Health, USA (grant R01 AI50139-02 to Jan Conn). GZL is currently financially supported by FAPESP Grant no. 2014/09774-1 and FAPESP Grant no. 2015/09669-6. Funders of this study had no role in the design, collection, analysis or interpretation of the results, nor in the writing of this report or the decision to publish it. Part of this research was performed 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 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. This manuscript was prepared whilst YML held a National Research Council (NRC) Senior Research Associateship Award at the Walter Reed Army Institute of Research. NR 55 TC 6 Z9 6 U1 2 U2 37 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1756-3305 J9 PARASITE VECTOR JI Parasites Vectors PD AUG 19 PY 2015 VL 8 AR 426 DI 10.1186/s13071-015-1038-4 PG 13 WC Parasitology SC Parasitology GA CP3DE UT WOS:000359756200003 PM 26283539 ER PT J AU McCarthy, MC Tamassia, F Thorwirth, S AF McCarthy, M. C. Tamassia, F. Thorwirth, S. TI High-resolution rotational spectroscopy of iminosilylene, HNSi SO MOLECULAR PHYSICS LA English DT Article DE vibrational excitation; quantum chemical calculations; rotational spectroscopy; molecular structure ID CORRELATED MOLECULAR CALCULATIONS; SILICON-NITROGEN CHEMISTRY; GAUSSIAN-BASIS SETS; EQUILIBRIUM STRUCTURE; HYPERFINE-STRUCTURE; 2ND DERIVATIVES; CARBON CHAINS; ATOMS; HSIN; PERTURBATION AB By means of Fourier transform microwave spectroscopy of a supersonic beam, the fundamental rotational transition of isotopic and vibrationally excited iminosilylene, HNSi, has been detected. In addition to seven isotopic species, vibrational satellite transitions from more than 30 vibrationally excited states, including the three fundamental modes, have been detected. Those from nu(2) are particularly intense, enabling detection of transitions from as high as (0,22(0),0) (i.e. similar to 10,000 cm(-1) above ground). At high spectral resolution, well-resolved nitrogen quadrupole structure has been observed in nearly every transition. Excitation of nu(1) or nu(3) changes eQq(N) little, but eQq(N) systematically decreases with increasing excitation of the nu(2) bend, from a value of 0.376(5) MHz for (0,0(0),0) to -2.257(5) MHz for (0,20(0),0). With the large amount of new data in hand, it has also been possible to determine the leading vibration-rotation constants (alpha(i) and gamma(i)) for nu(2) or nu(3) to high precision, and derive a revised semi-empirical equilibrium structure for this fundamental triatomic molecule. Various electronic and molecular properties of iminosilylene have been calculated at the coupled cluster level of theory, and these generally agree well with experiment and previous calculations. An unsuccessful search for HSiN, a highly polar isomer calculated to lie nearly 3 eV above HNSi, is also reported. C1 [McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Tamassia, F.] Univ Bologna, Dipartimento Chim Ind Toso Montanari, Bologna, Italy. [Thorwirth, S.] Univ Cologne, Inst Phys 1, Cologne, Germany. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011 OI Thorwirth, Sven/0000-0001-8200-6710 FU NSF [CHE-1058063]; Universita di Bologna; MIUR [20129ZFHFE]; Deutsche Forschungsgemeinschaft [TH 1301/3-1, TH 1301/3-2] FX The work in Cambridge is supported by NSF [grant number CHE-1058063]; F. Tamassia acknowledges the Universita di Bologna and MIUR [grant number 20129ZFHFE] (PRIN 2012 funds under the project 'STAR: Spectroscopic and computational Techniques for Astrophysical and Atmospheric Research') for financial support; S. Thorwirth gratefully acknowledges support from the Deutsche Forschungsgemeinschaft [grant number TH 1301/3-1], [grant number TH 1301/3-2]. NR 58 TC 1 Z9 1 U1 1 U2 3 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD AUG 18 PY 2015 VL 113 IS 15-16 SI SI BP 2204 EP 2216 DI 10.1080/00268976.2015.1019583 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CQ9BN UT WOS:000360906000018 ER PT J AU Koepfli, KP Pollinger, J Godinho, R Robinson, J Lea, A Hendricks, S Schweizer, RM Thalmann, O Silva, P Fan, ZX Yurchenko, AA Dobrynin, P Makunin, A Cahill, JA Shapiro, B Alvares, F Brito, JC Geffen, E Leonard, JA Helgen, KM Johnson, WE O'Brien, SJ Van Valkenburgh, B Wayne, RK AF Koepfli, Klaus-Peter Pollinger, John Godinho, Raquel Robinson, Jacqueline Lea, Amanda Hendricks, Sarah Schweizer, Rena M. Thalmann, Olaf Silva, Pedro Fan, Zhenxin Yurchenko, Andrey A. Dobrynin, Pavel Makunin, Alexey Cahill, James A. Shapiro, Beth Alvares, Francisco Brito, Jose C. Geffen, Eli Leonard, Jennifer A. Helgen, Kristofer M. Johnson, Warren E. O'Brien, Stephen J. Van Valkenburgh, Blaire Wayne, Robert K. TI Genome-wide Evidence Reveals that African and Eurasian Golden Jackals Are Distinct Species SO CURRENT BIOLOGY LA English DT Article ID NEOFELIS-NEBULOSA; CLOUDED LEOPARD; CLIMATE-CHANGE; EVOLUTION; CARNIVORA; CANIDS; DIVERGENCE; DELIMITATION; SEQUENCE; MAMMALIA AB The golden jackal of Africa (Canis aureus) has long been considered a conspecific of jackals distributed throughout Eurasia, with the nearest source populations in the Middle East. However, two recent reports found that mitochondrial haplotypes of some African golden jackals aligned more closely to gray wolves (Canis lupus) [1,2], which is surprising given the absence of gray wolves in Africa and the phenotypic divergence between the two species. Moreover, these results imply the existence of a previously unrecognized phylogenetically distinct species despite a long history of taxonomic work on African canids. To test the distinct-species hypothesis and understand the evolutionary history that would account for this puzzling result, we analyzed extensive genomic data including mitochondrial genome sequences, sequences from 20 autosomal loci (17 introns and 3 exon segments), microsatellite loci, X- and Y-linked zinc-finger protein gene (ZFX and ZFY) sequences, and whole-genome nuclear sequences in African and Eurasian golden jackals and gray wolves. Our results provide consistent and robust evidence that populations of golden jackals from Africa and Eurasia represent distinct monophyletic lineages separated for more than one million years, sufficient to merit formal recognition as different species: C. anthus (African golden wolf) and C. aureus (Eurasian golden jackal). Using morphologic data, we demonstrate a striking morphologic similarity between East African and Eurasian golden jackals, suggesting parallelism, which may have misled taxonomists and likely reflects uniquely intense interspecific competition in the East African carnivore guild. Our study shows how ecology can confound taxonomy if interspecific competition constrains size diversification. C1 [Koepfli, Klaus-Peter] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [Koepfli, Klaus-Peter; Yurchenko, Andrey A.; Dobrynin, Pavel; Makunin, Alexey; O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. [Pollinger, John; Robinson, Jacqueline; Schweizer, Rena M.; Van Valkenburgh, Blaire; Wayne, Robert K.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Godinho, Raquel; Silva, Pedro; Alvares, Francisco; Brito, Jose C.] Univ Porto, CIBIO InBIO Ctr Invest Biodiversidade & Recursos, P-4485661 Vairao, Portugal. [Godinho, Raquel; Silva, Pedro; Alvares, Francisco; Brito, Jose C.] Univ Porto, Fac Ciencias, Dept Biol, P-4169007 Oporto, Portugal. [Godinho, Raquel] Univ Johannesburg, Dept Zool, ZA-2006 Auckland Pk, South Africa. [Lea, Amanda] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Hendricks, Sarah] Univ Idaho, Dept Biol Sci, Inst Bioinformat & Evolutionary Studies, Moscow, ID 83844 USA. [Thalmann, Olaf] Univ Turku, Div Genet & Physiol, Dept Biol Sci, Turku 20014, Finland. [Thalmann, Olaf] Univ Oulu, Dept Biol, Oulu 90014, Finland. [Fan, Zhenxin] Sichuan Univ, Coll Life Sci, Sichuan Key Lab Conservat Biol Endangered Wildlif, Chengdu 610064, Peoples R China. [Cahill, James A.; Shapiro, Beth] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Geffen, Eli] Tel Aviv Univ, Dept Zool, IL-69978 Tel Aviv, Israel. [Leonard, Jennifer A.] Conservat & Evolutionary Genet Grp EBD CSIC, Estn Biol Donana, Seville 41092, Spain. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Amer Hist, Div Mammals, Washington, DC 20013 USA. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Dania, FL 33004 USA. RP Koepfli, KP (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM koepflik@si.edu; rwayne@ucla.edu RI Makunin, Alexey/N-2055-2015; Yurchenko, Andrey/N-2698-2015; Brito, Jose/A-7831-2010; CSIC, EBD Donana/C-4157-2011; Leonard, Jennifer/A-7894-2010; OI Makunin, Alexey/0000-0002-9555-5097; Yurchenko, Andrey/0000-0002-2239-6902; Brito, Jose/0000-0001-5444-8132; CSIC, EBD Donana/0000-0003-4318-6602; Leonard, Jennifer/0000-0003-0291-7819; Alvares, Francisco/0000-0002-4033-6989; Shapiro, Beth/0000-0002-2733-7776 FU Russian Ministry of Science Mega-grant [11.G34.31.0068]; FCT [IF/00564/2012, IF/00459/2013]; National Geographic Society [CRE 7629-04, CRE 8412-08]; CIBIO; Project "Genomics Applied to Genetic Resources"; North Portugal Regional Operational Programme (ON.2 - O Novo Norte), under the National Strategic Reference Framework, through the European Regional Development Fund; National Science Foundation Graduate Research Fellowship; Marie Curie Intra-European Fellowship within the 7th European Community Framework Program FX K.-P.K., A.A.Y., P.D., A.M., and S.J.O. were supported by Russian Ministry of Science Mega-grant 11.G34.31.0068. R.G. and J.C.B. were supported by FCT contracts (IF/00564/2012 and IF/00459/2013, respectively). Fieldwork of J.C.B. and F.A. in North Africa was supported by the National Geographic Society (CRE 7629-04 and CRE 8412-08) and CIBIO, respectively. Microsatellite lab work was partially funded by Project "Genomics Applied to Genetic Resources" cofinanced by North Portugal Regional Operational Programme 2007/2013 (ON.2 - O Novo Norte), under the National Strategic Reference Framework, through the European Regional Development Fund. R.M.S. was supported by a National Science Foundation Graduate Research Fellowship. O.T. is financed by a Marie Curie Intra-European Fellowship within the 7th European Community Framework Program and is grateful to M. Webster. We thank the Tel Aviv University Zoological Museum for providing samples of golden jackals and gray wolves used in this study. We gratefully acknowledge Frank Zachos (Naturhistorisches Museum Wien) for providing samples of golden jackals from Serbia and for constructive comments on the manuscript. We also thank N. Ferrand for helpful comments on the manuscript. We thank Michael Campana (Smithsonian Conservation Biology Institute) for conducting additional phylogenetic analyses on the mitochondrial genome dataset. We are grateful to Pauline Charruau-Dau and rev.com for providing translations of Frederic Cuvier's description of Canis anthus. We also thank D. Gordon E. Robertson for permission to use the photograph of a golden jackal from Serengeti National Park, Tanzania, for the graphical abstract. Finally, we thank four anonymous reviewers for providing excellent comments that improved the manuscript. NR 29 TC 15 Z9 15 U1 3 U2 36 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 AUG 17 PY 2015 VL 25 IS 16 BP 2158 EP 2165 DI 10.1016/j.cub.2015.06.060 PG 8 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA CP4WB UT WOS:000359882200028 PM 26234211 ER PT J AU Farine, DR Spencer, KA Boogert, NJ AF Farine, Damien R. Spencer, Karen A. Boogert, Neeltje J. TI Early-Life Stress Triggers Juvenile Zebra Finches to Switch Social Learning Strategies SO CURRENT BIOLOGY LA English DT Article ID DIFFUSION ANALYSIS; NETWORK STRUCTURE; SELECTION; INNOVATIONS; PERSPECTIVE; PERFORMANCE; CONFORMITY; PLASTICITY; STARLINGS; DYNAMICS AB Stress during early life can cause disease and cognitive impairment in humans and non-humans alike [1]. However, stress and other environmental factors can also program developmental pathways [2, 3]. We investigate whether differential exposure to developmental stress can drive divergent social learning strategies [4, 5] between siblings. In many species, juveniles acquire essential foraging skills by copying others: they can copy peers (horizontal social learning), learn from their parents (vertical social learning), or learn from other adults (oblique social learning) [6]. However, whether juveniles' learning strategies are condition dependent largely remains a mystery. We found that juvenile zebra finches living in flocks socially learned novel foraging skills exclusively from adults. By experimentally manipulating developmental stress, we further show that social learning targets are phenotypically plastic. While control juveniles learned foraging skills from their parents, their siblings, exposed as nestlings to experimentally elevated stress hormone levels, learned exclusively from unrelated adults. Thus, early-life conditions triggered individuals to switch strategies from vertical to oblique social learning. This switch could arise from stress-induced differences in developmental rate, cognitive and physical state, or the use of stress as an environmental cue. Acquisition of alternative social learning strategies may impact juveniles' fit to their environment and ultimately change their developmental trajectories. C1 [Farine, Damien R.] Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, Oxford OX1 3PS, England. [Farine, Damien R.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Spencer, Karen A.; Boogert, Neeltje J.] Univ St Andrews, Sch Psychol & Neurosci, St Andrews KY16 9JP, Fife, Scotland. [Boogert, Neeltje J.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. RP Farine, DR (reprint author), Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, S Parks Rd, Oxford OX1 3PS, England. EM damien.farine@zoo.ox.ac.uk FU NSF [NSF-IOS1250895]; BBSRC [BB/L006081/1]; BBSRC David Phillips Research Fellowship; Netherlands Organization for Scientific Research (NWO) FX We thank Ben Sheldon, Kevin Laland, Will Hoppitt, Lucy Aplin, Bram Kuijper, and Willem Frankenhuis for their constructive feedback, James Sturdy for his help scoring the videos, and Roland Stump for his help setting up the PIT/RFID system. D.R.F. was funded by grants from the NSF (NSF-IOS1250895) to Margaret Crofoot and BBSRC (BB/L006081/1) to Ben Sheldon, K.A.S. was funded by a BBSRC David Phillips Research Fellowship, and N.J.B. was funded by a Netherlands Organization for Scientific Research (NWO) Rubicon grant. NR 40 TC 10 Z9 10 U1 8 U2 43 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 AUG 17 PY 2015 VL 25 IS 16 BP 2184 EP 2188 DI 10.1016/j.cub.2015.06.071 PG 5 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA CP4WB UT WOS:000359882200032 PM 26212879 ER PT J AU Bastin, JF Barbier, N Rejou-Mechain, M Fayolle, A Gourlet-Fleury, S Maniatis, D de Haulleville, T Baya, F Beeckman, H Beina, D Couteron, P Chuyong, G Dauby, G Doucet, JL Droissart, V Dufrene, M Ewango, C Gillet, JF Gonmadje, CH Hart, T Kavali, T Kenfack, D Libalah, M Malhi, Y Makana, JR Pelissier, R Ploton, P Serckx, A Sonke, B Stevart, T Thomas, DW De Canniere, C Bogaert, J AF Bastin, J. -F. Barbier, N. Rejou-Mechain, M. Fayolle, A. Gourlet-Fleury, S. Maniatis, D. de Haulleville, T. Baya, F. Beeckman, H. Beina, D. Couteron, P. Chuyong, G. Dauby, G. Doucet, J. -L. Droissart, V. Dufrene, M. Ewango, C. Gillet, J. F. Gonmadje, C. H. Hart, T. Kavali, T. Kenfack, D. Libalah, M. Malhi, Y. Makana, J. -R. Pelissier, R. Ploton, P. Serckx, A. Sonke, B. Stevart, T. Thomas, D. W. De Canniere, C. Bogaert, J. TI Seeing Central African forests through their largest trees SO SCIENTIFIC REPORTS LA English DT Article ID TROPICAL FOREST; BIOMASS; SIZE; DISTRIBUTIONS; DIVERSITY AB Large tropical trees and a few dominant species were recently identified as the main structuring elements of tropical forests. However, such result did not translate yet into quantitative approaches which are essential to understand, predict and monitor forest functions and composition over large, often poorly accessible territories. Here we show that the above-ground biomass (AGB) of the whole forest can be predicted from a few large trees and that the relationship is proved strikingly stable in 175 1-ha plots investigated across 8 sites spanning Central Africa. We designed a generic model predicting AGB with an error of 14% when based on only 5% of the stems, which points to universality in forest structural properties. For the first time in Africa, we identified some dominant species that disproportionally contribute to forest AGB with 1.5% of recorded species accounting for over 50% of the stock of AGB. Consequently, focusing on large trees and dominant species provides precise information on the whole forest stand. This offers new perspectives for understanding the functioning of tropical forests and opens new doors for the development of innovative monitoring strategies. C1 [Bastin, J. -F.; De Canniere, C.] Univ Libre Bruxelles, Landscape Ecol & Plant Prod Syst Unit, B-1050 Brussels, Belgium. [Bastin, J. -F.; Fayolle, A.; de Haulleville, T.; Doucet, J. -L.; Dufrene, M.; Gillet, J. F.; Bogaert, J.] Univ Liege, Gembloux Agrobio Tech, BIOSE Dept, B-5030 Gembloux, Belgium. [Bastin, J. -F.; Serckx, A.] Ecole Reg Post Univ Amenagement & Gest Integres, Forets & Terr Tropicaux, Kinshasa, Zaire. [Barbier, N.; Rejou-Mechain, M.; Couteron, P.; Droissart, V.; Libalah, M.; Pelissier, R.; Ploton, P.] IRD, UMR AMAP, F-34000 Montpellier, France. [Rejou-Mechain, M.; Gourlet-Fleury, S.; Gonmadje, C. H.] Campus Int Baillarguet, CIRAD, UPR BSEF, F-34398 Montpellier, France. [Maniatis, D.; Malhi, Y.] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford, England. [de Haulleville, T.; Beeckman, H.] Royal Museum Cent Africa, Lab Wood Biol & Xylarium, Tervuren, Belgium. [Baya, F.] Minist Eaux Forets Chasse & Peche, Bangui, Cent Afr Republ. [Beina, D.] Univ Bangui Cerphameta, Bangui, Cent Afr Republ. [Chuyong, G.] Univ Buea, Dept Anim & Plant Sci, Buea, Cameroon. [Dauby, G.] Univ Libre Bruxelles, Fac Sci, Lab Evolut Biol & Ecol, Brussels, Belgium. [Ewango, C.; Makana, J. -R.] Wildlife Conservat Soc, CEFRECOF, Kinshasa, Zaire. [Gonmadje, C. H.] Natl Herbarium, Yaounde, Cameroon. [Gonmadje, C. H.] CIFOR, Cent African Reg Off, Yaounde 2008, Cameroon. [Hart, T.] Lukuru Wildlife Res Fdn, Kinshasa, Gombe, Zaire. [Kavali, T.] Wildlife Conservat Soc, DRC Program, Kinshasa, Zaire. [Kenfack, D.] Smithsonian Inst, Dept Bot, MRC 166, CTFS ForestGEO, Washington, DC 20013 USA. [Serckx, A.] Univ Liege, Behav Biol Unit, Liege, Belgium. [Serckx, A.] Royal Belgian Inst Nat Sci, Conservat Biol Unit, Brussels, Belgium. [Serckx, A.] Max Planck Inst Evolutionary Anthropol, Dept Primatol, Leipzig, Germany. [Libalah, M.; Sonke, B.] Univ Yaounde, Dept Biol, Plant Systemat & Ecol Lab, Yaounde 1, Cameroon. [Stevart, T.] Africa & Madagascar Dept, Missouri Bot Garden, St Louis, MO USA. [Thomas, D. W.] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Bastin, JF (reprint author), Univ Libre Bruxelles, Landscape Ecol & Plant Prod Syst Unit, CP264-2, B-1050 Brussels, Belgium. EM bastin.jf@gmail.com RI Barbier, Nicolas/A-5489-2010; Pelissier, Raphael/C-1224-2008 OI Barbier, Nicolas/0000-0002-5323-3866; Pelissier, Raphael/0000-0003-4845-5090 FU FRIA (FNRS); ERAIFT (WBI); WWF; CoForTips project [ANR-12-EBID-0002]; COBIMFO project (Congo Basin integrated monitoring for forest carbon mitigation and biodiversity) - Belgian Science Policy Office (Belspo); French Foreign Affairs; CIRAD; SCAC FX J.-F.B. and A. S. were supported by the FRIA (FNRS), ERAIFT (WBI) and WWF; M. R.-M. was supported by the CoForTips project (ANR-12-EBID-0002); T. d. H. was supported by the COBIMFO project (Congo Basin integrated monitoring for forest carbon mitigation and biodiversity) funded by the Belgian Science Policy Office (Belspo); C. H. G was supported by the "Sud Expert Plantes" project of French Foreign Affairs, CIRAD and SCAC. We thank the ARF Project (Appui a la Recherche Forestiere) in CAR for providing access to the M'Baiki site and to the database. We also would like to thank Dr. Valery Gond, for providing and sharing the map used in Fig. 1. NR 30 TC 21 Z9 21 U1 3 U2 18 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 AUG 17 PY 2015 VL 5 AR 13156 DI 10.1038/srep13156 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9YA UT WOS:000359531500002 PM 26279193 ER PT J AU van den Doel, PB Prieto, VR van Rossum-Fikkert, SE Schaftenaar, W Latimer, E Howard, L Chapman, S Masters, N Osterhaus, ADME Ling, PD Dastjerdi, A Martina, B AF van den Doel, Petra B. Rodriguez Prieto, Victor van Rossum-Fikkert, Sarah E. Schaftenaar, Willem Latimer, Erin Howard, Lauren Chapman, Sarah Masters, Nic Osterhaus, Albert D. M. E. Ling, Paul D. Dastjerdi, Akbar Martina, Byron TI A novel antigen capture ELISA for the specific detection of IgG antibodies to elephant endotheliotropic herpes virus SO BMC VETERINARY RESEARCH LA English DT Article DE EEHV; Asian elephant; Glycoprotein B; ELISA; Seroprevalence ID ASIAN ELEPHANTS; SEROLOGICAL EVIDENCE; AFRICAN ELEPHANTS; GLYCOPROTEIN-B; SIMPLEX-VIRUS; MAXIMUS; INFECTION AB Background: Elephants are classified as critically endangered animals by the International Union for Conservation of Species (IUCN). Elephant endotheliotropic herpesvirus (EEHV) poses a large threat to breeding programs of captive Asian elephants by causing fatal haemorrhagic disease. EEHV infection is detected by PCR in samples from both clinically ill and asymptomatic elephants with an active infection, whereas latent carriers can be distinguished exclusively via serological assays. To date, identification of latent carriers has been challenging, since there are no serological assays capable of detecting seropositive elephants. Results: Here we describe a novel ELISA that specifically detects EEHV antibodies circulating in Asian elephant plasma/serum. Approximately 80 % of PCR positive elephants display EEHV-specific antibodies. Monitoring three Asian elephant herds from European zoos revealed that the serostatus of elephants within a herd varied from non-detectable to high titers. The antibody titers showed typical herpes-like rise-and-fall patterns in time which occur in all seropositive animals in the herd more or less simultaneously. Conclusions: This study shows that the developed ELISA is suitable to detect antibodies specific to EEHV. It allows study of EEHV seroprevalence in Asian elephants. Results confirm that EEHV prevalence among Asian elephants (whether captive-born or wild-caught) is high. C1 [van den Doel, Petra B.; Osterhaus, Albert D. M. E.; Martina, Byron] Erasmus MC, Erasmus Med Ctr, ViroSci Lab, NL-3015 GE Rotterdam, Netherlands. [Osterhaus, Albert D. M. E.; Martina, Byron] Artemis One Hlth Res Inst, Utrecht, Netherlands. [Rodriguez Prieto, Victor] Univ Complutense Madrid, Dept Anim Hlth, VISAVET Ctr, Madrid, Spain. [van Rossum-Fikkert, Sarah E.] Erasmus MC, Dept Genet, Rotterdam, Netherlands. [Schaftenaar, Willem] Rotterdam Zoo, Vet Serv, Rotterdam, Netherlands. [Latimer, Erin] Smithsonians Natl Zoo, Smithsonian Conservat Biol Inst, Washington, DC USA. [Howard, Lauren] Houston Zoo Inc, Dept Anim Hlth, Houston, TX USA. [Chapman, Sarah] Twycross Zoo, East Midland Zool Soc, Atherstone, Warwick, England. [Masters, Nic] Zool Soc London, Vet Serv, London, England. [Ling, Paul D.] Baylors Coll Med, Dept Mol Virol & Microbiol, Houston, TX USA. [Dastjerdi, Akbar] Anim & Plant Hlth Agcy, Addlestone, Surrey, England. RP Martina, B (reprint author), Erasmus MC, Erasmus Med Ctr, ViroSci Lab, Room Ee1714,Dr Molewaterpl 50, NL-3015 GE Rotterdam, Netherlands. EM b.martina@erasmusmc.nl RI APHA, Staff publications/E-6082-2010; Dastjerdi, Akbar/E-1803-2011; Account for bibliometric studies, IT VISAVET/C-3115-2014 OI Account for bibliometric studies, IT VISAVET/0000-0003-3319-0050 FU Zoological Society of London FX Zoological Society of London NR 29 TC 1 Z9 1 U1 2 U2 16 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1746-6148 J9 BMC VET RES JI BMC Vet. Res. PD AUG 14 PY 2015 VL 11 AR 203 DI 10.1186/s12917-015-0522-6 PG 10 WC Veterinary Sciences SC Veterinary Sciences GA CO9BH UT WOS:000359466500001 PM 26268467 ER PT J AU Caldwell, RL Ross, R Rodaniche, A Huffard, CL AF Caldwell, Roy L. Ross, Richard Rodaniche, Arcadio Huffard, Christine L. TI Behavior and Body Patterns of the Larger Pacific Striped Octopus SO PLOS ONE LA English DT Article ID ABDOPUS-ACULEATUS DORBIGNY; WUNDERPUS-PHOTOGENICUS; VULCANOCTOPUS-HYDROTHERMALIS; CEPHALOPODA OCTOPODIDAE; MATING-BEHAVIOR; CYANEA GRAY; N.-GEN.; VULGARIS; WILD; CUTTLEFISH AB Over thirty years ago anecdotal accounts of the undescribed Larger Pacific Striped Octopus suggested behaviors previously unknown for octopuses. Beak-to-beak mating, dens shared by mating pairs, inking during mating and extended spawning were mentioned in publications, and enticed generations of cephalopod biologists. In 2012-2014 we were able to obtain several live specimens of this species, which remains without a formal description. All of the unique behaviors listed above were observed for animals in aquaria and are discussed here. We describe the behavior, body color patterns, and postures of 24 adults maintained in captivity. Chromatophore patterns of hatchlings are also shown. C1 [Caldwell, Roy L.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Caldwell, Roy L.; Ross, Richard; Huffard, Christine L.] Calif Acad Sci, San Francisco, CA 94118 USA. [Rodaniche, Arcadio] Smithsonian Trop Res Inst, Panama City, Panama. [Huffard, Christine L.] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA. RP Caldwell, RL (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM rlcaldwell@berkeley.edu FU University of California Museum of Paleontology FX Funding was provided to RLC by the University of California Museum of Paleontology. This funding group had no influence on the authors' study design, interpretation, or communication. NR 60 TC 6 Z9 6 U1 20 U2 66 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 AUG 12 PY 2015 VL 10 IS 8 AR e0134152 DI 10.1371/journal.pone.0134152 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9JT UT WOS:000359492300033 PM 26266543 ER PT J AU Kelehear, C Jones, HI Wood, BA Shine, R AF Kelehear, Crystal Jones, Hugh I. Wood, Benjamin A. Shine, Richard TI Wild Cane Toads (Rhinella marina) Expel Foreign Matter from the Coelom via the Urinary Bladder in Response to Internal Injury, Endoparasites and Disease SO PLOS ONE LA English DT Article ID IMPLANTED DUMMY TRANSMITTERS; BUFO-MARINUS; RHABDIAS-PSEUDOSPHAEROCEPHALA; TRANSINTESTINAL EXPULSION; TROPICAL AUSTRALIA; FROGS; BUFONIDAE; DYNAMICS; ANURA; ACANTHOCEPHALA AB Dissections of > 1,200 wild-caught cane toads (Rhinella marina) in tropical Australia confirm a laboratory report that anurans can expel foreign objects from the coelom by incorporating them into the urinary bladder. The foreign objects that we found inside bladders included a diverse array of items (e.g., grass seeds, twigs, insect prey, parasites), many of which may have entered the coelom via rupture of the gut wall. In some cases, the urinary bladder was fused to other organs including liver, fat bodies, ovaries, Bidder's organs, lungs, mesentery, stomach wall, gall bladder, and the abdominal wall. Acanthocephalan parasites (of a range of developmental stages) were identified from the walls of the urinary bladders of three cane toads. This organ may play a significant role in destroying or excreting metazoan parasites, as well as inanimate objects. C1 [Kelehear, Crystal; Shine, Richard] Univ Sydney, Sch Biol Sci, Camperdown, NSW, Australia. [Jones, Hugh I.] Univ Western Australia, Sch Pathol & Lab Med, Crawley, WA, Australia. [Wood, Benjamin A.] Queen Elizabeth Med Ctr, PathWest Lab Med, Nedlands, WA, Australia. RP Kelehear, C (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM crystal.kelehear@hotmail.com FU Australian Research Council [FL120100074] FX This work was supported by Australian Research Council (http://www.arc.gov.au) Grant FL120100074 to RS. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 29 TC 0 Z9 0 U1 3 U2 9 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 AUG 12 PY 2015 VL 10 IS 8 AR e0134036 DI 10.1371/journal.pone.0134036 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9JT UT WOS:000359492300031 PM 26267862 ER PT J AU Wappler, T Guilbert, E Labandeira, CC Hornschemeyer, T Wedmann, S AF Wappler, Torsten Guilbert, Eric Labandeira, Conrad C. Hoernschemeyer, Thomas Wedmann, Sonja TI Morphological and Behavioral Convergence in Extinct and Extant Bugs: The Systematics and Biology of a New Unusual Fossil Lace Bug from the Eocene SO PLOS ONE LA English DT Article ID GREEN RIVER FORMATION; HEMIPTERA HETEROPTERA; AMBER HEMIPTERA; SP N.; TINGIDAE; CANTACADERINAE; GENUS; COLORADO; USA; RECONSTRUCTION AB The bug Gyaclavator kohlsi Wappler, Guilbert, Wedmann et Labandeira, gen. et sp. nov., represents a new extinct genus of lace bugs (Insecta: Heteroptera: Tingidae) occurring in latest early Eocene deposits of the Green River Formation, from the southern Piceance Basin of Northwestern Colorado, in North America. Gyaclavator can be placed within the Tingidae with certainty, perhaps it is sistergroup to Cantacaderinae. If it belongs to Cantacaderinae, it is the first fossil record of this group for North America. Gyaclavator has unique, conspicuous antennae bearing a specialized, highly dilated distiflagellomere, likely important for intra-or intersex reproductive competition and attraction. This character parallels similar antennae in leaf-footed bugs (Coreidae), and probably is associated with a behavioral convergence as well. C1 [Wappler, Torsten; Wedmann, Sonja] Forschungsstn Grube Messel, Senckenberg Forschungsinst, Messel, Germany. [Wappler, Torsten; Wedmann, Sonja] Forschungsstn Grube Messel, Nat Museum Frankfurt, Messel, Germany. [Wappler, Torsten; Wedmann, Sonja] Senckenberg Biodiversitat & Klima Forschungszentr, Frankfurt, Germany. [Wappler, Torsten] Univ Bonn, Steinmann Inst Geol, Mineral, Palaontol, Bonn, Germany. [Guilbert, Eric] Museum Natl Hist Nat, CNRS, UMR 7205, Dept Systemat & Evolut, Paris, France. [Labandeira, Conrad C.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol & Behav, Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Capital Normal Univ, Coll Life Sci, Beijing, Peoples R China. [Hoernschemeyer, Thomas] Univ Gottingen, Johann Friedrich Blumenbach Inst Zool & Anthropol, Abt Morphol & Systemat, Zool Museum, D-37073 Gottingen, Germany. RP Wappler, T (reprint author), Forschungsstn Grube Messel, Senckenberg Forschungsinst, Messel, Germany. EM twappler@uni-bonn.de; sonja.wedmann@senckenberg.de RI Wappler, Torsten/D-4287-2011; OI Wappler, Torsten/0000-0003-1592-0988; Wedmann, Sonja/0000-0002-9778-4125; Hornschemeyer, Thomas/0000-0002-4924-5389 FU Deutsche Forschungsgemeinschaft (DFG) [WE 2942/6-1, WE 2942/6-2, HO 2306/6-1, HO 2306/6-2]; Hesse's Ministry of Higher Education, Research, and the Arts FX This research was possible thanks to grants of the Deutsche Forschungsgemeinschaft (DFG, grant no WE 2942/6-1 to S. W., grant no WE 2942/6-2 to S. W. and T. W., and grant no HO 2306/6-1 6-2 to T. H.) (www.dfg.de) and by the research funding programme "LOEWE-Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz" of Hesse's Ministry of Higher Education, Research, and the Arts. (https://wissenschaft.hessen.de/). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 76 TC 3 Z9 4 U1 2 U2 12 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 AUG 12 PY 2015 VL 10 IS 8 AR e0133330 DI 10.1371/journal.pone.0133330 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO9JT UT WOS:000359492300014 PM 26267108 ER PT J AU Zhou, G Bayliss, D Hartman, JD Rabus, M Bakos, GA Jordan, A Brahm, R Penev, K Csubry, Z Mancini, L Espinoza, N de Val-Borro, M Bhatti, W Ciceri, S Henning, T Schmidt, B Murphy, SJ Butler, RP Arriagada, P Shectman, S Crane, J Thompson, I Suc, V Noyes, RW AF Zhou, G. Bayliss, D. Hartman, J. D. Rabus, M. Bakos, G. A. Jordan, A. Brahm, R. Penev, K. Csubry, Z. Mancini, L. Espinoza, N. de Val-Borro, M. Bhatti, W. Ciceri, S. Henning, T. Schmidt, B. Murphy, S. J. Butler, R. P. Arriagada, P. Shectman, S. Crane, J. Thompson, I. Suc, V. Noyes, R. W. TI A 0.24+0.18 M-circle dot double-lined eclipsing binary from the HATSouth survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: eclipsing; stars: individual: HATS551-027 ID LOW-MASS STARS; MAIN-SEQUENCE STARS; CM-DRACONIS; M-DWARFS; HOT JUPITER; FUNDAMENTAL PROPERTIES; ABSOLUTE DIMENSIONS; EVOLUTIONARY MODELS; CIRCUMBINARY PLANET; RADIUS RELATION AB We report the discovery and characterization of a new M-dwarf binary, with component masses and radii of M-1 = 0.244(-0.003)(+0.003) M-circle dot, R-1 = 0.261(-0.009)(+0.006) R-circle dot, M-2 = 0.179(-0.001)(+0.002) M-circle dot, R-2 = 0.218(-0.011)(+0.007) R-circle dot, and orbital period of similar to 4.1 d. The M-dwarf binary HATS551-027 (LP 837-20) was identified as an eclipsing binary by the HATSouth survey, and characterized by a series of high-precision photometric observations of the eclipse events, and spectroscopic determinations of the atmospheric parameters and radial velocity orbits. HATS551-027 is one of few systems with both stellar components lying in the fully convective regime of very low mass stars, and can serve as a test for stellar interior models. The radius of HATS551-027A is consistent with models to 1 sigma, whilst HATS551-027B is inflated by 9 per cent at 2s significance. We measure the effective temperatures for the two stellar components to be T-eff,T- (1) = 3190 +/- 100 K and T-eff, (2) = 2990 +/- 110 K; both are slightly cooler than theoretical models predict, but consistent with other M-dwarfs of similar masses that have previously been studied. We also measure significant Ha emission from both components of the binary system, and discuss this in the context of the correlation between stellar activity and the discrepancies between the observed and model temperatures. C1 [Zhou, G.; Bayliss, D.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Hartman, J. D.; Bakos, G. A.; Penev, K.; Csubry, Z.; de Val-Borro, M.; Bhatti, W.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Rabus, M.; Jordan, A.; Brahm, R.; Espinoza, N.; Suc, V.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Mancini, L.; Ciceri, S.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Murphy, S. J.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Butler, R. P.; Arriagada, P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Shectman, S.; Crane, J.; Thompson, I.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhou, G (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. EM george.zhou@anu.edu.au OI Jordan, Andres/0000-0002-5389-3944 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX12AH91H, NNX13AQ62G]; ARC Laureate Fellowship [FL0992131]; Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; FONDECYT [1130857]; BASAL CATA [PFB-06]; CONICYT-PCHA/Doctorado Nacional; La Silla Observatory [P087.A-9014(A), P088.A-9008(A), P089.A9008(A), P087.C-0508(A), 089.A-9006(A).]; Robert Martin Ayers Sciences Fund; [NSF/AST-1108686] FX Development of the HATSouth project was funded by NSF MRI grant NSF/AST-0723074, operations are supported by NASA grant NNX12AH91H, and follow-up observations receive partial support from grant NSF/AST-1108686. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. Follow-up observations with the MPG 2.2 m/FEROS instrument were performed under MPIA guaranteed time (P087.A-9014(A), P088.A-9008(A), P089.A-9008(A)) and Chilean time (P087.C-0508(A)). AJ acknowledges support from project IC120009 'Millennium Institute of Astrophysics (MAS)' of the Millennium Science Initiative, Chilean Ministry of Economy, FONDECYT project 1130857, and BASAL CATA PFB-06. VS acknowledges support form BASAL CATA PFB-06. RB and NE acknowledge support from CONICYT-PCHA/Doctorado Nacional and Fondecyt project 1130857. KP acknowledges support from NASA grant: NNX13AQ62G. This work is based on observations made with ESO Telescopes at the La Silla Observatory under programme IDs P087.A-9014(A), P088.A-9008(A), P089.A9008(A), P087.C-0508(A), and 089.A-9006(A). We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD data base, operated at CDS, Strasbourg, France. Operations at the MPG/ESO 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 Regis Lachaume for his technical assistance during the observations at the MPG 2.2 m Telescope. Australian access to the Magellan Telescopes was supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. We thank Albert Jahnke, Toni Hanke (HESS), Peter Conroy (MSO) for their contributions to the HATSouth project. The HATSouth network is operated by a collaboration consisting of Princeton University (PU), the Max Planck Institut fur Astronomie (MPIA), the Australian National University (ANU), and the Pontificia Universidad Catolica de Chile (PUC). The station at Las Campanas Observatory (LCO) of the Carnegie Institution is operated by PU in conjunction with PUC, the station at the High Energy Spectroscopic Survey (HESS) site is operated in conjunction with MPIA, and the station at Siding Spring Observatory (SSO) is operated jointly with ANU. This paper includes data gathered with the 6.5 metre Magellan Telescopes located at Las Campanas Observatory, Chile. NR 75 TC 4 Z9 4 U1 1 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 AUG 11 PY 2015 VL 451 IS 3 BP 2263 EP 2277 DI 10.1093/mnras/stv1070 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8CL UT WOS:000360833700002 ER PT J AU Sobey, C Young, NJ Hessels, JWT Weltevrede, P Noutsos, A Stappers, BW Kramer, M Bassa, C Lyne, AG Kondratiev, VI Hassall, TE Keane, EF Bilous, AV Breton, RP Griessmeier, JM Karastergiou, A Pilia, M Serylak, M ter Veen, S van Leeuwen, J Alexov, A Anderson, J Asgekar, A Avruch, IM Bell, ME Bentum, MJ Bernardi, G Best, P Birzan, L Bonafede, A Breitling, F Broderick, J Bruggen, M Corstanje, A Carbone, D de Geus, E de Vos, M van Duin, A Duscha, S Eisloffel, J Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Gunst, AW Hamaker, JP Heald, G Hoeft, M Horandel, J Jutte, E Kuper, G Maat, P Mann, G Markoff, S McFadden, R McKay-Bukowski, D McKean, JP Mulcahy, DD Munk, H Nelles, A Norden, MJ Orru, E Paas, H Pandey-Pommier, M Pandey, VN Pietka, G Pizzo, R Polatidis, AG Rafferty, D Renting, A Rottgering, H Rowlinson, A Scaife, AMM Schwarz, D Sluman, J Smirnov, O Steinmetz, M Stewart, A Swinbank, J Tagger, M Tang, Y Tasse, C Thoudam, S Toribio, C Vermeulen, R Vocks, C van Weeren, RJ Wijers, RAMJ Wise, MW Wucknitz, O Yatawatta, S Zarka, P AF Sobey, C. Young, N. J. Hessels, J. W. T. Weltevrede, P. Noutsos, A. Stappers, B. W. Kramer, M. Bassa, C. Lyne, A. G. Kondratiev, V. I. Hassall, T. E. Keane, E. F. Bilous, A. V. Breton, R. P. Griessmeier, J. -M. Karastergiou, A. Pilia, M. Serylak, M. ter Veen, S. van Leeuwen, J. Alexov, A. Anderson, J. Asgekar, A. Avruch, I. M. Bell, M. E. Bentum, M. J. Bernardi, G. Best, P. Birzan, L. Bonafede, A. Breitling, F. Broderick, J. Brueggen, M. Corstanje, A. Carbone, D. de Geus, E. de Vos, M. van Duin, A. Duscha, S. Eisloeffel, J. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Gunst, A. W. Hamaker, J. P. Heald, G. Hoeft, M. Horandel, J. Juette, E. Kuper, G. Maat, P. Mann, G. Markoff, S. McFadden, R. McKay-Bukowski, D. McKean, J. P. Mulcahy, D. D. Munk, H. Nelles, A. Norden, M. J. Orru, E. Paas, H. Pandey-Pommier, M. Pandey, V. N. Pietka, G. Pizzo, R. Polatidis, A. G. Rafferty, D. Renting, A. Rottgering, H. Rowlinson, A. Scaife, A. M. M. Schwarz, D. Sluman, J. Smirnov, O. Steinmetz, M. Stewart, A. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. Thoudam, S. Toribio, C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wijers, R. A. M. J. Wise, M. W. Wucknitz, O. Yatawatta, S. Zarka, P. TI LOFAR discovery of a quiet emission mode in PSR B0823+26 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; pulsars: individual: PSR B0823+26 ID RADIO TELESCOPE OBSERVATION; SINGLE-PULSE OBSERVATIONS; GALACTIC MAGNETIC-FIELD; FREQUENCY-DEPENDENCE; FARADAY-ROTATION; SPIN-DOWN; X-RAY; SUBPULSE MODULATION; TIMING OBSERVATIONS; CRAB PULSAR AB PSR B0823+26, a 0.53-s radio pulsar, displays a host of emission phenomena over time-scales of seconds to (at least) hours, including nulling, subpulse drifting, and mode-changing. Studying pulsars like PSR B0823+26 provides further insight into the relationship between these various emission phenomena and what they might teach us about pulsar magnetospheres. Here we report on the LOFAR (Low-Frequency Array) discovery that PSR B0823+26 has a weak and sporadically emitting 'quiet' (Q) emission mode that is over 100 times weaker (on average) and has a nulling fraction forty-times greater than that of the more regularly-emitting 'bright' (B) mode. Previously, the pulsar has been undetected in the Q mode, and was assumed to be nulling continuously. PSR B0823+26 shows a further decrease in average flux just before the transition into the B mode, and perhaps truly turns off completely at these times. Furthermore, simultaneous observations taken with the LOFAR, Westerbork, Lovell, and Effelsberg telescopes between 110 MHz and 2.7 GHz demonstrate that the transition between the Q mode and B mode occurs within one single rotation of the neutron star, and that it is concurrent across the range of frequencies observed. C1 [Sobey, C.; Noutsos, A.; Kramer, M.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Sobey, C.; Hessels, J. W. T.; Bassa, C.; Kondratiev, V. I.; Pilia, M.; van Leeuwen, J.; Asgekar, A.; Bentum, M. J.; de Geus, E.; de Vos, M.; van Duin, A.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Heald, G.; Kuper, G.; Maat, P.; McFadden, R.; McKean, J. P.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Renting, A.; Sluman, J.; Tang, Y.; Toribio, C.; Vermeulen, R.; Wise, M. W.; Yatawatta, S.] ASTRON Netherlands Inst Radio Astron, NL-7990 AA Dwingeloo, Netherlands. [Young, N. J.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa. [Young, N. J.; Weltevrede, P.; Stappers, B. W.; Kramer, M.; Lyne, A. G.] Univ Manchester, Sch Phys & Astron, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Hessels, J. W. T.; van Leeuwen, J.; Carbone, D.; Markoff, S.; Swinbank, J.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Kondratiev, V. I.] Russian Acad Sci, PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Hassall, T. E.; Breton, R. P.; Broderick, J.; Mulcahy, D. D.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Keane, E. F.] Swinburne Univ Technol, Ctr Astrophys & Supercomputing, Hawthorn, Vic 3122, Australia. [Keane, E. F.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Bilous, A. V.; ter Veen, S.; Corstanje, A.; Falcke, H.; Horandel, J.; Nelles, A.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Griessmeier, J. -M.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Griessmeier, J. -M.] Univ Orleans, CNRS, Observ Paris, Stn Radioastron Nancay,INSU,OSUC,USR 704, F-18330 Nancay, France. [Karastergiou, A.; Fender, R.; Stewart, A.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Serylak, M.] Univ Western Cape, Dept Phys & Astron, ZA-7535 Bellville, South Africa. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.] Helmholtz Zentrum Potsdam, GFZ, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore 560099, Karnataka, India. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; Heald, G.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bell, M. E.; Rowlinson, A.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bentum, M. J.] Univ Twente, NL-7500 AE Enschede, Netherlands. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Birzan, L.; Garrett, M. A.; Rafferty, D.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bonafede, A.; Brueggen, M.] Univ Hamburg, D-21029 Hamburg, Germany. [Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [de Geus, E.] SmarterVis BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Ferrari, C.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Lagrange,UMR7293, F-06300 Nice, France. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, FI-99600 Sodankyla, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, Ctr Informat Technol, NL-9747 AJ Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Tasse, C.; Zarka, P.] Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France. RP Sobey, C (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM sobey@astron.nl RI Kondratiev, Vladislav/N-1105-2015; Breton, Rene/A-5536-2017; Yatawatta, Sarod/E-6037-2013; OI Kondratiev, Vladislav/0000-0001-8864-7471; Breton, Rene/0000-0001-8522-4983; Swinbank, John/0000-0001-9445-1846; Wijers, Ralph/0000-0002-3101-1808; Yatawatta, Sarod/0000-0001-5619-4017; Bilous, Anna/0000-0002-7177-6987; van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft (DFG) [FOR 1254]; National Research Foundation (NRF); NWO Vidi fellowship; ERC [337062]; STFC consolidated grant; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX We thank the Deutsche Forschungsgemeinschaft (DFG) for funding this work within the research unit FOR 1254 'Magnetisation of Interstellar and Intergalactic Media: The Prospects of Low-Frequency Radio Observations'. NY acknowledges support from the National Research Foundation (NRF). JWTH acknowledges funding from an NWO Vidi fellowship and ERC Starting Grant 'DRAGNET' (337062). The LOFAR was designed and constructed by ASTRON, the Netherlands Institute for Radio Astronomy, and 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 WSRT is operated by ASTRON/NWO. Observations with the Lovell Telescope are supported through an STFC consolidated grant. This work is partly based on observations with the 100-m telescope of the Max-Planck-Institut fur Radioastronomie at Effelsberg. We would like to thank R. Karuppusamy for his help with the Effelsberg observations. CF acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. The majority of the plots were created using the PSRCHIVE PYTHON interface, and the PYTHON package MATPLOTLIB (Hunter 2007). NR 86 TC 7 Z9 7 U1 0 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 AUG 11 PY 2015 VL 451 IS 3 BP 2493 EP 2506 DI 10.1093/mnras/stv1066 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8CL UT WOS:000360833700018 ER PT J AU Devaney, J Barrett, B Barrett, F Redmond, J O'Halloran, J AF Devaney, John Barrett, Brian Barrett, Frank Redmond, John O'Halloran, John TI Forest Cover Estimation in Ireland Using Radar Remote Sensing: A Comparative Analysis of Forest Cover Assessment Methodologies SO PLOS ONE LA English DT Article ID LAND-COVER; ALOS-PALSAR; TROPICAL DEFORESTATION; MAPPING DEFORESTATION; BRAZILIAN AMAZONIA; BOREAL FORESTS; SPATIAL DATA; CLASSIFICATION; BACKSCATTER; BIOMASS AB Quantification of spatial and temporal changes in forest cover is an essential component of forest monitoring programs. Due to its cloud free capability, Synthetic Aperture Radar (SAR) is an ideal source of information on forest dynamics in countries with near-constant cloud-cover. However, few studies have investigated the use of SAR for forest cover estimation in landscapes with highly sparse and fragmented forest cover. In this study, the potential use of L-band SAR for forest cover estimation in two regions (Longford and Sligo) in Ireland is investigated and compared to forest cover estimates derived from three national (Forestry2010, Prime2, National Forest Inventory), one pan-European (Forest Map 2006) and one global forest cover (Global Forest Change) product. Two machine-learning approaches (Random Forests and Extremely Randomised Trees) are evaluated. Both Random Forests and Extremely Randomised Trees classification accuracies were high (98.1-98.5%), with differences between the two classifiers being minimal (<0.5%). Increasing levels of post classification filtering led to a decrease in estimated forest area and an increase in overall accuracy of SAR-derived forest cover maps. All forest cover products were evaluated using an independent validation dataset. For the Longford region, the highest overall accuracy was recorded with the Forestry2010 dataset (97.42%) whereas in Sligo, highest overall accuracy was obtained for the Prime2 dataset (97.43%), although accuracies of SAR-derived forest maps were comparable. Our findings indicate that spaceborne radar could aid inventories in regions with low levels of forest cover in fragmented landscapes. The reduced accuracies observed for the global and pan-continental forest cover maps in comparison to national and SAR-derived forest maps indicate that caution should be exercised when applying these datasets for national reporting. C1 [Devaney, John; O'Halloran, John] Univ Coll Cork UCC, Sch Biol Earth & Environm Sci BEES, Cork, Ireland. [Barrett, Brian] Univ Coll Cork UCC, Sch Geog & Archaeol, Cork, Ireland. [Barrett, Frank; Redmond, John] Dept Agr Food & Marine, Forest Serv, Johnstown Castle, Wexford, Ireland. RP Devaney, J (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf, Edgewater, MD 21037 USA. EM devaneyj@si.edu OI Devaney, John/0000-0002-7676-0378 FU Science, Technology, Research and Innovation for the Environment (STRIVE) Programme [2011-CCRP-FS-1.1]; Irish Government under National Development Plan (NDP) FX This study has been prepared as part of the Science, Technology, Research and Innovation for the Environment (STRIVE) Programme (Grant No. 2011-CCRP-FS-1.1). The programme is financed by the Irish Government under the National Development Plan (NDP) 2007-2013 and is administered by the Environmental Protection Agency (www.epa.ie). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 89 TC 0 Z9 0 U1 3 U2 35 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 AUG 11 PY 2015 VL 10 IS 8 AR e0133583 DI 10.1371/journal.pone.0133583 PG 27 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO7PP UT WOS:000359353300008 PM 26262681 ER PT J AU Sherratt, E Castaneda, MD Garwood, RJ Mahler, DL Sanger, TJ Herrel, A de Queiroz, K Losos, JB AF Sherratt, Emma Castaneda, Maria del Rosario Garwood, Russell J. Mahler, D. Luke Sanger, Thomas J. Herrel, Anthony de Queiroz, Kevin Losos, Jonathan B. TI Amber fossils demonstrate deep-time stability of Caribbean lizard communities SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE adaptive radiation; ecomorph; Hispaniola; Miocene; Anolis ID DOMINICAN AMBER; ANOLIS-LIZARDS; PHYLOGENETIC-RELATIONSHIPS; IGUANIAN LIZARDS; MORPHOLOGICAL DIVERSIFICATION; ECOLOGICAL OPPORTUNITY; ISLAND LIZARDS; EVOLUTION; DIVERSITY; SERIES AB Whether the structure of ecological communities can exhibit stability over macroevolutionary timescales has long been debated. The similarity of independently evolved Anolis lizard communities on environmentally similar Greater Antillean islands supports the notion that community evolution is deterministic. However, a dearth of Caribbean Anolis fossils-only three have been described to date-has precluded direct investigation of the stability of anole communities through time. Here we report on an additional 17 fossil anoles in Dominican amber dating to 15-20 My before the present. Using data collected primarily by X-ray microcomputed tomography (X-ray micro-CT), we demonstrate that the main elements of Hispaniolan anole ecomorphological diversity were in place in the Miocene. Phylogenetic analysis yields results consistent with the hypothesis that the ecomorphs that evolved in the Miocene are members of the same ecomorph clades extant today. The primary axes of ecomorphological diversity in the Hispaniolan anole fauna appear to have changed little between the Miocene and the present, providing evidence for the stability of ecological communities over macroevolutionary timescales. C1 [Sherratt, Emma] Univ New England, Sch Environm & Rural Sci, Armidale, NSW 2351, Australia. [Sherratt, Emma; Castaneda, Maria del Rosario; Losos, Jonathan B.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Sherratt, Emma; Castaneda, Maria del Rosario; Losos, Jonathan B.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Garwood, Russell J.] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England. [Mahler, D. Luke] Univ Calif Davis, Ctr Populat Biol, Davis, CA 95616 USA. [Sanger, Thomas J.] Univ Florida, Dept Mol Genet & Microbiol, Gainesville, FL 32610 USA. [Herrel, Anthony] Museum Natl Hist Nat, Dept Ecol & Gest Biodiversite, UMR 7179, F-75231 Paris, France. [Herrel, Anthony] Univ Ghent, Evolutionary Morphol Vertebrates, B-9000 Ghent, Belgium. [de Queiroz, Kevin] Smithsonian Inst, Natl Museum Amer Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Sherratt, E (reprint author), Univ New England, Sch Environm & Rural Sci, Armidale, NSW 2351, Australia. EM emma.sherratt@gmail.com RI Herrel, Anthony/C-3712-2013; Sherratt, Emma/A-9931-2011 OI Herrel, Anthony/0000-0003-0991-4434; Sherratt, Emma/0000-0003-2164-7877 FU National Science Foundation FX We thank those who allowed us access to amber fossils for study: G. Bechly, J. Calbeto, L. Costeur, M. Cusanovich, G. Greco, M. Greco, D. Grimaldi, M. Halonen, and J. Work. We especially thank E. Morone for providing access to more than half of the fossils examined for this study. We thank J. Klaczko, and G. Gartner for providing support and discussions and J. Casart for assisting with data collection. Scan data were also provided by R. Boistel, M. Polcyn, L. Jacobs, M. Colbert, and R. Ketcham. We thank the National Science Foundation for support. NR 56 TC 4 Z9 4 U1 5 U2 26 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 AUG 11 PY 2015 VL 112 IS 32 BP 9961 EP 9966 DI 10.1073/pnas.1506516112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO6RY UT WOS:000359285100060 PM 26216976 ER PT J AU Ali, ZS Parsons, AR Zheng, HX Pober, JC Liu, A Aguirre, JE Bradley, RF Bernardi, G Carilli, CL Cheng, C DeBoer, DR Dexter, MR Grobbelaar, J Horrell, J Jacobs, DC Klima, P MacMahon, DHE Maree, M Moore, DF Razavi, N Stefan, II Walbrugh, WP Walker, A AF Ali, Zaki S. Parsons, Aaron R. Zheng, Haoxuan Pober, Jonathan C. Liu, Adrian Aguirre, James E. Bradley, Richard F. Bernardi, Gianni Carilli, Chris L. Cheng, Carina DeBoer, David R. Dexter, Matthew R. Grobbelaar, Jasper Horrell, Jasper Jacobs, Daniel C. Klima, Pat MacMahon, David H. E. Maree, Matthys Moore, David F. Razavi, Nima Stefan, Irina I. Walbrugh, William P. Walker, Andre TI PAPER-64 CONSTRAINTS ON REIONIZATION: THE 21 cm POWER SPECTRUM AT z=8.4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; early universe; instrumentation: interferometers; intergalactic medium ID STAR-FORMING GALAXIES; ULTRA DEEP FIELD; SIMILAR-TO 20; NORTH CELESTIAL POLE; COSMIC REIONIZATION; INTERGALACTIC MEDIUM; FOREGROUND REMOVAL; CENTIMETER FLUCTUATIONS; REDUNDANCY CALIBRATION; CROSS-CORRELATION AB In this paper, we report new limits on 21 cm emission from cosmic reionization based on a 135 day observing campaign with a 64-element deployment of the Donald C. Backer Precision Array for Probing the Epoch of Reionization in South Africa. This work extends the work presented in Parsons et al. with more collecting area, a longer observing period, improved redundancy-based calibration, improved fringe-rate filtering, and updated power-spectral analysis using optimal quadratic estimators. The result is a new 2 sigma upper limit on Delta(2)(k) of (22.4 mK)(2) in the range 0.15 < k < 0.5h Mpc(-1) at z = 8.4. This represents a three-fold improvement over the previous best upper limit. As we discuss in more depth in a forthcoming paper, this upper limit supports and extends previous evidence against extremely cold reionization scenarios. We conclude with a discussion of implications for future 21 cm reionization experiments, including the newly funded Hydrogen Epoch of Reionization Array. C1 [Ali, Zaki S.; Parsons, Aaron R.; Liu, Adrian; Cheng, Carina] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Parsons, Aaron R.; DeBoer, David R.; Dexter, Matthew R.; MacMahon, David H. E.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Zheng, Haoxuan] MIT, Dept Phys, Cambridge, MA 02139 USA. [Pober, Jonathan C.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Liu, Adrian] Berkeley Ctr Cosmol Phys, Berkeley, CA USA. [Aguirre, James E.; Moore, David F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bradley, Richard F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA USA. [Bradley, Richard F.; Klima, Pat] Natl Radio Astron Observ, Charlottesville, VA USA. [Bradley, Richard F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Bernardi, Gianni; Grobbelaar, Jasper; Horrell, Jasper; Maree, Matthys; Walbrugh, William P.; Walker, Andre] Sq Kilometer Array, Cape Town, South Africa. [Bernardi, Gianni] Rhodes Univ, Dept Phys & Elect, Grahamstown, South Africa. [Bernardi, Gianni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carilli, Chris L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Carilli, Chris L.; Razavi, Nima; Stefan, Irina I.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Jacobs, Daniel C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. RP Ali, ZS (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. OI Pober, Jonathan/0000-0002-3492-0433 FU National Science Foundation (NSF) [0804508, 1129258, 1125558]; NSF [1352519, 1302774, 1401708]; Mount Cuba Astronomical Association FX PAPER is supported by grants from the National Science Foundation (NSF; awards 0804508, 1129258, and 1125558). A.R.P., J.C.P., and D.C.J. would like to acknowledge NSF support (awards 1352519, 1302774, and 1401708, respectively). J.E.A. would like to acknowledge a generous grant from the Mount Cuba Astronomical Association for computing resources. We graciously thank SKA-SA for site infrastructure and observing support. We also thank interns Monde Manzini and Ruvano Casper from Durban University of Technology, who helped expand the array from 32 to 64 antennas. Thanks also to Josh Dillon for helpful discussions on optimal quadratic estimators. NR 107 TC 64 Z9 64 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 AUG 10 PY 2015 VL 809 IS 1 AR 61 DI 10.1088/0004-637X/809/1/61 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500061 ER PT J AU Bai, XN Caprioli, D Sironi, L Spitkovsky, A AF Bai, Xue-Ning Caprioli, Damiano Sironi, Lorenzo Spitkovsky, Anatoly TI MAGNETOHYDRODYNAMIC-PARTICLE-IN-CELL METHOD FOR COUPLING COSMIC RAYS WITH A THERMAL PLASMA: APPLICATION TO NON-RELATIVISTIC SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; instabilities; magnetohydrodynamics (MHD); methods: numerical; plasmas; shock waves ID UNSPLIT GODUNOV METHOD; MAGNETIC-FIELD AMPLIFICATION; HYBRID SIMULATIONS; SUPERNOVA-REMNANTS; ION-ACCELERATION; FILAMENTATION INSTABILITY; CONSTRAINED TRANSPORT; ASTROPHYSICAL SHOCKS; PROTOPLANETARY DISKS; COLLISIONLESS SHOCKS AB We formulate a magnetohydrodynamic-particle-in-cell (MHD-PIC) method for describing the interaction between collisionless cosmic ray (CR) particles and a thermal plasma. The thermal plasma is treated as a fluid, obeying equations of ideal MHD, while CRs are treated as relativistic Lagrangian particles subject to the Lorentz force. Backreaction from CRs to the gas is included in the form of momentum and energy feedback. In addition, we include the electromagnetic feedback due to CR-induced Hall effect that becomes important when the electron-ion drift velocity of the background plasma induced by CRs approaches the Alfven velocity. Our method is applicable on scales much larger than the ion inertial length, bypassing the microscopic scales that must be resolved in conventional PIC methods, while retaining the full kinetic nature of the CRs. We have implemented and tested this method in the Athena MHD code, where the overall scheme is second-order accurate and fully conservative. As a first application, we describe a numerical experiment to study particle acceleration in non-relativistic shocks. Using a simplified prescription for ion injection, we reproduce the shock structure and the CR energy spectra obtained with more self-consistent hybrid-PIC simulations, but at substantially reduced computational cost. We also show that the CR-induced Hall effect reduces the growth rate of the Bell instability and affects the gas dynamics in the vicinity of the shock front. As a step forward, we are able to capture the transition of particle acceleration from non-relativistic to relativistic regimes, with momentum spectrum f (p) proportional to p(-4) connecting smoothly through the transition, as expected from the theory of Fermi acceleration. C1 [Bai, Xue-Ning; Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. [Caprioli, Damiano; Spitkovsky, Anatoly] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS 51, Cambridge, MA 02138 USA. EM xbai@cfa.harvard.edu RI Caprioli, Damiano/I-6582-2012 OI Caprioli, Damiano/0000-0003-0939-8775 FU NASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF2-51301.001-A]; NASA [NAS 5-26555, NNX14AQ34G, NAS8-03060]; NASA through Einstein Fellowship grant - Chandra X-ray Center [PF1-120090]; Simons Foundation [267233, 291817]; XSEDE grant [TG-AST140001] FX We thank the anonymous referee for a very useful report that led to several improvements to the paper, particularly on code implementation, convergence checks, and overall clarity. X.-N.B. is supported by NASA through Hubble Fellowship grant HST-HF2-51301.001-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. D.C. is supported by NASA grant NNX14AQ34G. L.S. is supported by NASA through Einstein Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This work was partially supported by Simons Foundation (grants 267233 and 291817 to AS), and was facilitated by Max Planck/Princeton Center for Plasma Physics. Computation for this work was performed on computational resources supported by PICSciE and the OIT's High Performance Computing Center at Princeton University. This work also used resources on Stampede at Texas Advanced Computing Center through XSEDE grant TG-AST140001. NR 65 TC 9 Z9 9 U1 1 U2 7 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 AUG 10 PY 2015 VL 809 IS 1 AR 55 DI 10.1088/0004-637X/809/1/55 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500055 ER PT J AU Barclay, T Quintana, EV Adams, FC Ciardi, DR Huber, D Foreman-Mackey, D Montet, BT Caldwell, D AF Barclay, Thomas Quintana, Elisa V. Adams, Fred C. Ciardi, David R. Huber, Daniel Foreman-Mackey, Daniel Montet, Benjamin T. Caldwell, Douglas TI THE FIVE PLANETS IN THE KEPLER-296 BINARY SYSTEM ALL ORBIT THE PRIMARY: A STATISTICAL AND ANALYTICAL ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; methods: data analysis; methods: statistical; planetary systems; stars: individual (Kepler-296, KIC 11497958, KOI-1422); techniques: photometric ID POTENTIAL TRANSIT SIGNALS; CANDIDATE HOST STARS; EARTH-SIZED PLANET; SOLAR-TYPE STARS; HABITABLE ZONE; BAYESIAN-INFERENCE; MISSION DATA; DENSE CORES; DARK CLOUDS; M DWARFS AB Kepler-296 is a binary star system with two M-dwarf components separated by 0 ''.2. Five transiting planets have been confirmed to be associated with the Kepler-296 system; given the evidence to date, however, the planets could in principle orbit either star. This ambiguity has made it difficult to constrain both the orbital and physical properties of the planets. Using both statistical and analytical arguments, this paper shows that all five planets are highly likely to orbit the primary star in this system. We performed a Markov-Chain Monte Carlo simulation using a five transiting planet model, leaving the stellar density and dilution with uniform priors. Using importance sampling, we compared the model probabilities under the priors of the planets orbiting either the brighter or the fainter component of the binary. A model where the planets orbit the brighter component, Kepler-296A, is strongly preferred by the data. Combined with our assertion that all five planets orbit the same star, the two outer planets in the system, Kepler-296 Ae and Kepler-296 Af, have radii of 1.53 +/- 0.26 and 1.80 +/- 0.31 R-circle plus, respectively, and receive incident stellar fluxes of 1.40 +/- 0.23 and 0.62 +/- 0.10 times the incident flux the Earth receives from the Sun. This level of irradiation places both planets within or close to the circumstellar habitable zone of their parent star. C1 [Barclay, Thomas; Quintana, Elisa V.; Caldwell, Douglas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Barclay, Thomas] Bay Area Environm Res Inst, Petaluma, CA 94952 USA. [Adams, Fred C.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel; Caldwell, Douglas] SETI Inst, Mountain View, CA 94043 USA. [Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Foreman-Mackey, Daniel] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Montet, Benjamin T.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barclay, T (reprint author), NASA, Ames Res Ctr, M-S 244-30, Moffett Field, CA 94035 USA. OI Montet, Benjamin/0000-0001-7516-8308; Ciardi, David/0000-0002-5741-3047 FU NASA Science Mission Directorate; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA Keck PI Data Award; W. M. Keck Foundation; NASA Senior Fellowship at the Ames Research Center; National Science Foundation Graduate Research Fellowship [DGE1144469]; Australian Research Council [DE140101364]; National Aeronautics and Space Administration [NNX14AB92G] FX This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission Directorate. We would like to express our gratitude to all those who have worked on the Kepler pipeline over the many years of the Kepler mission. Some Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute (STScI). 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 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. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Some of the 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. 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. E.V.Q. is supported by a NASA Senior Fellowship at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE1144469. 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. NR 62 TC 13 Z9 13 U1 3 U2 11 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 AUG 10 PY 2015 VL 809 IS 1 DI 10.1088/0004-637X/809/1/7 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500007 ER PT J AU Barnacka, A Geller, MJ Dell'Antonio, IP Benbow, W AF Barnacka, Anna Geller, Margaret J. Dell'Antonio, Ian P. Benbow, Wystan TI RESOLVING THE HIGH-ENERGY UNIVERSE WITH STRONG GRAVITATIONAL LENSING: THE CASE OF PKS 1830-211 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: jets; gamma-rays: jets; gravitational lensing: strong; methods: data analysis; techniques: high angular resolution; quasars: individual (PKS 1820-211) ID LARGE-AREA TELESCOPE; GAMMA-RAY FLARES; MOLECULAR ABSORPTION-LINES; SYNCHROTRON-PROTON BLAZAR; RADIO-SOURCE PKS1830-211; FERMI-DETECTED BLAZARS; TIME-DELAY DISTANCES; HUBBLE CONSTANT; LUMINOUS BLAZARS; M87 JET AB Gravitational lensing is a potentially powerful tool for elucidating the origin of gamma-ray emission from distant sources. Cosmic lenses magnify the emission from distant sources and produce time delays between mirage images. Gravitationally induced time delays depend on the position of the emitting regions in the source plane. The Fermi/LAT telescope continuously monitors the entire sky and detects gamma-ray flares, including those from gravitationally lensed blazars. Therefore, temporal resolution at gamma-ray energies can be used to measure these time delays, which, in turn, can be used to resolve the origin of the gamma-ray flares spatially. We provide a guide to the application and Monte Carlo simulation of three techniques for analyzing these unresolved light curves: the autocorrelation function, the double power spectrum, and the maximum peak method. We apply these methods to derive time delays from the gamma-ray light curve of the gravitationally lensed blazar PKS 1830-211. The result of temporal analysis combined with the properties of the lens from radio observations yield an improvement in spatial resolution at gamma-ray energies by a factor of 10,000. We analyze four active periods. For two of these periods the emission is consistent with origination from the core, and for the other two the data suggest that the emission region is displaced from the core by more than similar to 1.5 kpc. For the core emission, the gamma-ray time delays, 23 +/- 0.5 days and 19.7 +/- 1.2 days, are consistent with the radio time delay of 26(-5)(+4) days. C1 [Barnacka, Anna; Geller, Margaret J.; Benbow, Wystan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnacka, Anna] Jagiellonian Univ, Astron Observ, Krakow, Poland. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Barnacka, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 20, Cambridge, MA 02138 USA. EM abarnacka@cfa.harvard.edu OI Barnacka, Anna/0000-0001-5655-4158; Geller, Margaret/0000-0002-9146-4876 FU Department of Energy Office of Science; NASA; Smithsonian Astrophysical Observatory; NCN grant [DEC-2011/01/M/ST9/01891]; Smithsonian Institution FX A. B. is supported by the Department of Energy Office of Science, NASA & the Smithsonian Astrophysical Observatory with financial support from the NCN grant DEC-2011/01/M/ ST9/01891. M.J.G. is supported by the Smithsonian Institution. NR 109 TC 5 Z9 5 U1 0 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 AUG 10 PY 2015 VL 809 IS 1 AR 100 DI 10.1088/0004-637X/809/1/100 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500100 ER PT J AU Bromley, BC Kenyon, SJ AF Bromley, Benjamin C. Kenyon, Scott J. TI EVOLUTION OF A RING AROUND THE PLUTO-CHARON BINARY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Kuiper belt: general; planet-disk interactions; planets and satellites: formation; planets and satellites: individual (Pluto); planets and satellites: rings ID GIANT IMPACT ORIGIN; TRANSITING CIRCUMBINARY PLANETS; ECCENTRIC STELLAR BINARIES; BODY-COAGULATION CODE; SATURNS RINGS; ACCRETION DISKS; PLANETESIMAL SWARM; TIDAL EVOLUTION; GASEOUS NEBULA; KUIPER-BELT AB We consider the formation of satellites around the Pluto-Charon binary. An early collision between the two partners likely produced the binary and a narrow ring of debris, out of which arose the moons Styx, Nix, Kerberos, and Hydra. How the satellites emerged from the compact ring is uncertain. Here we show that a particle ring spreads from physical collisions and collective gravitational scattering, similar to migration. Around a binary, these processes take place in the reference frames of "most circular" orbits, akin to circular ones in a Keplerian potential. Ring particles damp to these orbits and avoid destructive collisions. Damping and diffusion also help particles survive dynamical instabilities driven by resonances with the binary. In some situations, particles become trapped near resonances that sweep outward with the tidal evolution of the Pluto-Charon binary. With simple models and numerical experiments, we show how the Pluto-Charon impact ring may have expanded into a broad disk, out of which grew the circumbinary moons. In some scenarios, the ring can spread well beyond the orbit of Hydra, the most distant moon, to form a handful of smaller satellites. If these small moons exist, New Horizons will find them. C1 [Bromley, Benjamin C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bromley, BC (reprint author), Univ Utah, Dept Phys & Astron, 115 S 1400 E,Rm 201, Salt Lake City, UT 84112 USA. EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA [NNX10AF35G, NNX11AM37G] FX We are grateful for the comments of an anonymous referee that resulted in a number of improvements to our presentation. We thank NASA for support through the Astrophysics Theory and Origins of Solar Systems programs (grant NNX10AF35G) and through the Outer Planets Program (grant NNX11AM37G). We are also grateful to NASA for a generous allotment of supercomputer time on the "discover" cluster. NR 131 TC 1 Z9 1 U1 0 U2 8 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 AUG 10 PY 2015 VL 809 IS 1 AR 88 DI 10.1088/0004-637X/809/1/88 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500088 ER PT J AU Ciardi, DR Van Eyken, JC Barnes, JW Beichman, CA Carey, SJ Crockett, CJ Eastman, J Johns-Krull, CM Howell, SB Kane, SR Mclane, JN Plavchan, P Prato, L Stauffer, J Van Belle, GT Von Braun, K AF Ciardi, David R. Van Eyken, Julian C. Barnes, Jason W. Beichman, Charles A. Carey, Sean J. Crockett, Christopher J. Eastman, Jason Johns-Krull, Christopher M. Howell, Steve B. Kane, Stephen R. Mclane, Jacob N. . Plavchan, Peter Prato, L. Stauffer, John Van Belle, Gerard T. Von Braun, Kaspar TI FOLLOW-UP OBSERVATIONS OF PTFO 8-8695: A 3 MYR OLD T TAURI STAR HOSTING A JUPITER-MASS PLANETARY CANDIDATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (PTFO 8-8695, 2MASS J05250755+0134243, CVSO 30); stars: pre-main sequence ID SPIN-ORBIT MISALIGNMENT; RADIAL-VELOCITY; ORION PROJECT; LIGHT-CURVE; TRANSIT; VARIABILITY; SYSTEM; SEARCH; BINARY; OCCULTATIONS AB We present Spitzer 4.5 mu m light curve observations, Keck NIRSPEC radial velocity observations, and LCOGT optical light curve observations of PTFO 8-8695, which may host a Jupiter-sized planet in a very short orbital period (0.45 days). Previous work by van Eyken et al. and Barnes et al. predicts that the stellar rotation axis and the planetary orbital plane should precess with a period of 300-600 days. As a consequence, the observed transits should change shape and depth, disappear, and reappear with the precession. Our observations indicate the long-term presence of the transit events (> 3 years), and that the transits indeed do change depth, disappear and reappear. The Spitzer observations and the NIRSPEC radial velocity observations (with contemporaneous LCOGT optical light curve data) are consistent with the predicted transit times and depths for the M-k = 0.34 M-circle dot precession model and demonstrate the disappearance of the transits. An LCOGT optical light curve shows that the transits do reappear approximately 1 year later. The observed transits occur at the times predicted by a straight-forward propagation of the transit ephemeris. The precession model correctly predicts the depth and time of the Spitzer transit and the lack of a transit at the time of the NIRSPEC radial velocity observations. However, the precession model predicts the return of the transits approximately 1 month later than observed by LCOGT. Overall, the data are suggestive that the planetary interpretation of the observed transit events may indeed be correct, but the precession model and data are currently insufficient to confirm firmly the planetary status of PTFO 8-8695b. C1 [Ciardi, David R.; Van Eyken, Julian C.; Beichman, Charles A.] NASA Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA. [Van Eyken, Julian C.] Univ Calif Santa Barbara, LCOGT, Santa Barbara, CA 93106 USA. [Barnes, Jason W.; Eastman, Jason] Cumbres Observ Global Telescope Network, Goleta, CA USA. [Barnes, Jason W.] Univ Idaho, Moscow, ID 83843 USA. [Carey, Sean J.; Stauffer, John] Spitzer Sci Ctr Caltech, Pasadena, CA USA. [Crockett, Christopher J.] Sci News, Washington, DC 20036 USA. [Eastman, Jason] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johns-Krull, Christopher M.] Rice Univ, Houston, TX USA. [Howell, Steve B.] NASA Ames Res Ctr, Mountain View, CA USA. [Kane, Stephen R.] San Francisco State Univ, San Francisco, CA 94132 USA. [Mclane, Jacob N. .; Prato, L.; Van Belle, Gerard T.; Von Braun, Kaspar] Lowell Observ, Flagstaff, AZ 86001 USA. [Plavchan, Peter] Missouri State Univ, Springfield, MO USA. RP Ciardi, DR (reprint author), NASA Exoplanet Sci Inst Caltech, Pasadena, CA 91125 USA. EM ciardi@ipac.caltech.edu RI Barnes, Jason/B-1284-2009; OI Barnes, Jason/0000-0002-7755-3530; Eastman, Jason/0000-0003-3773-5142; Ciardi, David/0000-0002-5741-3047 FU W. M. Keck Foundation; Las Cumbres Observatory Global Telescope Network; NASA; National Aeronautics and Space Administration under the Exoplanet Exploration Program; National Aeronautics and Space Administration FX D.R.C. would like to dedicate this paper to his dad Robert A. Ciardi (1940-2013). Robert Ciardi had a passion for learning and knowledge and, in particular, for science. While not able to pursue a career in science for himself, he never stopped thinking and growing, and through his love and encouragement, D.R.C. was able to pursue his own love of exploration and science. In many ways, Robert Ciardi was more excited about this discovery than the authors on this paper. He will be greatly missed. Thank you, Dad. 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 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. This research has made use of the LCOGT Archive, which is operated by the California Institute of Technology, under contract with the Las Cumbres Observatory Global Telescope Network. 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. 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. Portions of this work were performed at the California Institute of Technology under contract with the National Aeronautics and Space Administration. NR 58 TC 8 Z9 8 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 AUG 10 PY 2015 VL 809 IS 1 AR 42 DI 10.1088/0004-637X/809/1/42 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500042 ER PT J AU Fukui, A Gould, A Sumi, T Bennett, DP Bond, IA Han, C Suzuki, D Beaulieu, JP Batista, V Udalski, A Street, RA Tsapras, Y Hundertmark, M Abe, F Bhattacharya, A Freeman, M Itow, Y Ling, CH Koshimoto, N Masuda, K Matsubara, Y Muraki, Y Ohnishi, K Philpott, LC Rattenbury, N Saito, T Sullivan, DJ Tristram, PJ Yonehara, A Choi, JY Christie, GW DePoy, DL Dong, SB Drummond, J Gaudi, BS Hwang, KH Kavka, A Lee, CU McCormick, J Natusch, T Ngan, H Park, H Pogge, RW Shin, IG Tan, TG Yee, JC Szymanski, MK Pietrzynski, G Soszynski, I Poleski, R Kozlowski, S Pietrukowicz, P Ulaczyk, K Wyrzykowski, L Bramich, DM Browne, P Dominik, M Horne, K Ipatov, S Kains, N Snodgrass, C Steele, IA AF Fukui, A. Gould, A. Sumi, T. Bennett, D. P. Bond, I. A. Han, C. Suzuki, D. Beaulieu, J. -P. Batista, V. Udalski, A. Street, R. A. Tsapras, Y. Hundertmark, M. Abe, F. Bhattacharya, A. Freeman, M. Itow, Y. Ling, C. H. Koshimoto, N. Masuda, K. Matsubara, Y. Muraki, Y. Ohnishi, K. Philpott, L. C. Rattenbury, N. Saito, T. Sullivan, D. J. Tristram, P. J. Yonehara, A. Choi, J. -Y. Christie, G. W. DePoy, D. L. Dong, Subo Drummond, J. Gaudi, B. S. Hwang, K. -H. Kavka, A. Lee, C. -U. McCormick, J. Natusch, T. Ngan, H. Park, H. Pogge, R. W. Shin, I-G. Tan, T. -G. Yee, J. C. Szymanski, M. K. Pietrzynski, G. Soszynski, I. Poleski, R. Kozlowski, S. Pietrukowicz, P. Ulaczyk, K. Wyrzykowski, L. Bramich, D. M. Browne, P. Dominik, M. Horne, K. Ipatov, S. Kains, N. Snodgrass, C. Steele, I. A. CA MOA Collaboration FUN Collaboration OGLE Collaboration RoboNet Collaboration TI OGLE-2012-BLG-0563Lb: A SATURN-MASS PLANET AROUND AN M DWARF WITH THE MASS CONSTRAINED BY SUBARU AO IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: gaseous planets; stars: late-type; techniques: high angular resolution; techniques: photometric ID MAGNIFICATION MICROLENSING EVENTS; SOLAR-TYPE STARS; MILKY-WAY BULGE; GALACTIC BULGE; JUPITER/SATURN ANALOG; MODEL ATMOSPHERES; HIGH-RESOLUTION; EXTINCTION MAP; MAIN-SEQUENCE; GIANT PLANETS AB We report the discovery of a microlensing exoplanet OGLE-2012-BLG-0563Lb with the planet-star mass ratio of similar to 1 x 10(-3). Intensive photometric observations of a high-magnification microlensing event allow us to detect a clear signal of the planet. Although no parallax signal is detected in the light curve, we instead succeed at detecting the flux from the host star in high-resolution JHK'-band images obtained by the Subaru/AO188 and Infrared Camera and Spectrograph instruments, allowing us to constrain the absolute physical parameters of the planetary system. With the help of spectroscopic information about the source star obtained during the high-magnification state by Bensby et al., we find that the lens system is located at 1.3(-0.8)(+0.6) kpc from us, and consists of an M dwarf (0.34(-0.20)(+0.12)M(circle dot)) orbited by a Saturn-mass planet (0.39(-0.23)(+0.14)M(Jup)) at the projected separation of 0.74(-0.42)(+0.26)AU (close model) or 4.3(-2.5)(+1.5)AU (wide model). The probability of contamination in the host star's flux, which would reduce the masses by a factor of up to three, is estimated to be 17%. This possibility can be tested by future high-resolution imaging. We also estimate the (J - K-s) and (H - K-s) colors of the host star, which are marginally consistent with a low metallicity mid-to-early M dwarf, although further observations are required for the metallicity to be conclusive. This is the fifth sub-Jupiter-mass (0.2 < m(p)/M-Jup < 1) microlensing planet around an M dwarf with the mass well constrained. The relatively rich harvest of sub-Jupiters around M dwarfs is contrasted with a possible paucity of similar to 1-2 Jupiter-mass planets around the same type of star, which can be explained by the planetary formation process in the core-accretion scheme. C1 [Fukui, A.] Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, Kamogatacho, Okayama 7190232, Japan. [Sumi, T.; Koshimoto, N.] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. [Bennett, D. P.; Suzuki, D.; Bhattacharya, A.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Ling, C. H.] Massey Univ, Inst Informat & Math Sci, Auckland, New Zealand. [Abe, F.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Freeman, M.; Rattenbury, N.] Univ Auckland, Dept Phys, Auckland, New Zealand. [Sullivan, D. J.] Victoria Univ, Sch Chem & Phys Sci, Wellington, New Zealand. [Ohnishi, K.] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Philpott, L. C.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V6T 1Z4, Canada. [Saito, T.] Tokyo Metropolitan Coll Ind Technol, Tokyo 1168523, Japan. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Yonehara, A.] Kyoto Sangyo Univ, Dept Phys, Fac Sci, Kita Ku, Kyoto, Kyoto 6038555, Japan. [Gould, A.; Gaudi, B. S.; Kavka, A.; Pogge, R. W.; Yee, J. C.; Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Han, C.; Choi, J. -Y.; Hwang, K. -H.; Park, H.; Shin, I-G.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. [Christie, G. W.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland, New Zealand. [DePoy, D. L.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Dong, Subo] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Drummond, J.] Possum Observ, Patutahi, New Zealand. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [McCormick, J.] Farm Cove Observ, Ctr Backyard Astrophys, Auckland, New Zealand. [Natusch, T.] AUT Univ, Auckland, New Zealand. [Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Udalski, A.; Szymanski, M. K.; Pietrzynski, G.; Soszynski, I.; Poleski, R.; Kozlowski, S.; Pietrukowicz, P.; Ulaczyk, K.; Wyrzykowski, L.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Beaulieu, J. -P.; Batista, V.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Street, R. A.; Tsapras, Y.] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Univ Heidelberg ZAH, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. [Tsapras, Y.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Browne, P.; Dominik, M.; Horne, K.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Hundertmark, M.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Hundertmark, M.] Univ Copenhagen, Nat Hist Museum, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Ipatov, S.] Russian Acad Sci, Vernadsky Inst Geochem & Analyt Chem, Moscow 119991, Russia. [Ipatov, S.] Russian Acad Sci, Space Res Inst, Moscow 119991, Russia. [Kains, N.] European So Observ, D-85748 Garching, Germany. [Kains, N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Snodgrass, C.] Open Univ, Dept Phys Sci, Planetary & Space Sci, Milton Keynes MK7 6AA, Bucks, England. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. RP Fukui, A (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Ooaza Honjyo, Kamogatacho, Okayama 7190232, Japan. EM gould@astronomy.ohio-state.edu; gwchristie@christie.org.nz; depoy@physics.tamu.edu; farmcoveobs@xtra.co.nz; tim.natusch@aut.ac.nz RI Hundertmark, Markus/C-6190-2015; Watanabe, Makoto/E-3667-2016; Kozlowski, Szymon/G-4799-2013; OI Hundertmark, Markus/0000-0003-0961-5231; Watanabe, Makoto/0000-0002-3656-4081; Kozlowski, Szymon/0000-0003-4084-880X; Dominik, Martin/0000-0002-3202-0343; Tan, Thiam-Guan/0000-0001-5603-6895; Snodgrass, Colin/0000-0001-9328-2905 FU Astrobiology Project of the Center for Novel Science Initiatives (CNSI), National Institutes of Natural Sciences (NINS) [AB261005]; JSPS [JSPS23103002, JSPS24253004, JSPS26247023]; Creative Research Initiative Program of National Research Foundation of Korea [2009-0081561]; "Strategic Priority Research Program-The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [09000000]; National Science Centre, Poland [MAESTRO 2014/14/A/ST9/00121]; European Union [268421]; Qatar Foundation from QNRF grant [NPRP-09-476-1-078]; [JSPS25103508]; [23340064] FX This paper is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. A.F. thanks Oscar A. Gonzalez for kindly providing VVV data. A.F. was supported by the Astrobiology Project of the Center for Novel Science Initiatives (CNSI), National Institutes of Natural Sciences (NINS; Grant Number AB261005). T.S. acknowledges the financial support from the JSPS, JSPS23103002, JSPS24253004, and JSPS26247023. The MOA project is supported by grants JSPS25103508 and 23340064. NJR is a Royal Society of New Zealand Rutherford Discovery Fellow. Work by C.H. was supported by Creative Research Initiative Program (2009-0081561) of National Research Foundation of Korea. S.D. is supported by "the Strategic Priority Research Program-The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (grant No. 09000000). The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. C.S. received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 268421. K.A., D.M.B., M.D., K.H., M.H., C.L., C.S., R.A.S., and Y.T. would like to thank the Qatar Foundation for support from QNRF grant NPRP-09-476-1-078. NR 69 TC 10 Z9 10 U1 0 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 AUG 10 PY 2015 VL 809 IS 1 AR 74 DI 10.1088/0004-637X/809/1/74 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500074 ER PT J AU Gopalan, G Vrtilek, SD Bornn, L AF Gopalan, Giri Vrtilek, Saeqa Dil Bornn, Luke TI CLASSIFYING X-RAY BINARIES: A PROBABILISTIC APPROACH SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; pulsars: general; stars: black holes; stars: neutron; X-rays: binaries ID LINEAR ALGEBRA; PERFORMANCE; MISSION; CATALOG AB In X-ray binary star systems consisting of a compact object that accretes material from an orbiting secondary star, there is no straightforward means to decide whether the compact object is a black hole or a neutron star. To assist in this process, we develop a Bayesian statistical model that makes use of the fact that X-ray binary systems appear to cluster based on their compact object type when viewed from a three-dimensional coordinate system derived from X-ray spectral data where the first coordinate is the ratio of counts in the mid-to low-energy band (color 1), the second coordinate is the ratio of counts in the high-to low-energy band (color 2), and the third coordinate is the sum of counts in all three bands. We use this model to estimate the probabilities of an X-ray binary system containing a black hole, non-pulsing neutron star, or pulsing neutron star. In particular, we utilize a latent variable model in which the latent variables follow a Gaussian process prior distribution, and hence we are able to induce the spatial correlation which we believe exists between systems of the same type. The utility of this approach is demonstrated by the accurate prediction of system types using Rossi X-ray Timing Explorer All Sky Monitor data, but it is not flawless. In particular, non-pulsing neutron systems containing "bursters" that are close to the boundary demarcating systems containing black holes tend to be classified as black hole systems. As a byproduct of our analyses, we provide the astronomer with the public R code which can be used to predict the compact object type of XRBs given training data. C1 [Gopalan, Giri; Bornn, Luke] Harvard Univ, Dept Stat, Cambridge, MA 02138 USA. [Vrtilek, Saeqa Dil] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bornn, Luke] Simon Fraser Univ, Dept Stat & Actuarial Sci, Burnaby, BC V5A 1S6, Canada. RP Gopalan, G (reprint author), Harvard Univ, Dept Stat, One Oxford St, Cambridge, MA 02138 USA. FU Smithsonian Institution CGPS grant FX We acknowledge the Harvard ICHASC for their helpful feedback. Additionally, G.G. and S.D.V. acknowledge partial support through a Smithsonian Institution CGPS grant to SDV. NR 27 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 AUG 10 PY 2015 VL 809 IS 1 AR 40 DI 10.1088/0004-637X/809/1/40 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500040 ER PT J AU Greiner, J Fox, DB Schady, P Kruhler, T Trenti, M Cikota, A Bolmer, J Elliott, J Delvaux, C Perna, R Afonso, P Kann, DA Klose, S Savaglio, S Schmidl, S Schweyer, T Tanga, M Varela, K AF Greiner, J. Fox, D. B. Schady, P. Kruehler, T. Trenti, M. Cikota, A. Bolmer, J. Elliott, J. Delvaux, C. Perna, R. Afonso, P. Kann, D. A. Klose, S. Savaglio, S. Schmidl, S. Schweyer, T. Tanga, M. Varela, K. TI GAMMA-RAY BURSTS TRACE UV METRICS OF STAR FORMATION OVER 3 < z < 5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: high-redshift; galaxies: luminosity function; mass function; galaxies: star formation; gamma-ray burst: general ID MASS-METALLICITY RELATION; LY-ALPHA EMITTERS; GALAXY LUMINOSITY FUNCTION; DEEP FIELD CAMPAIGN; GRB HOST GALAXIES; APPROXIMATE-TO 3; FORMING GALAXIES; OPTICAL AFTERGLOW; FORMATION RATES; SPITZER OBSERVATIONS AB We present the first uniform treatment of long duration gamma-ray burst (GRB) host galaxy detections and upper limits over the redshift range 3 < z < 5, a key epoch for observational and theoretical efforts to understand the processes, environments, and consequences of early cosmic star formation (SF). We contribute deep imaging observations of 13 GRB positions yielding the discovery of 8 new host galaxies. We use this data set in tandem with previously published observations of 31 further GRB positions to estimate or constrain the host galaxy rest-frame ultraviolet (UV; lambda = 1600 angstrom) absolute magnitudes M-UV. We then use the combined set of 44 M-UV estimates and limits to construct the M-UV luminosity function (LF) for GRB host galaxies over 3 < z < 5 and compare it to expectations from Lyman break galaxy (LBG) photometric surveys with the Hubble Space Telescope. Adopting standard prescriptions for the luminosity dependence of galaxy dust obscuration (and hence, total SF rate), we find that our LF is compatible with LBG observations over a factor of 600x in host luminosity, from M-UV = -22.5 mag to >-15.6 mag, and with extrapolations of the assumed Schechter-type LF well beyond this range. We review proposed astrophysical and observational biases for our sample, and find that they are for the most part minimal. We therefore conclude, as the simplest interpretation of our results, that GRBs successfully trace UV metrics of cosmic SF over the range 3 < z < 5. Our findings suggest that GRBs provide an accurate picture of star formation processes from z approximate to 3 out to the highest redshifts. C1 [Greiner, J.; Schady, P.; Bolmer, J.; Elliott, J.; Delvaux, C.; Savaglio, S.; Schweyer, T.; Tanga, M.; Varela, K.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Greiner, J.] Tech Univ Munich, Excellence Cluster Universe, D-85748 Garching, Germany. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Ctr Theoret & Observat Cosmol, University Pk, PA 16802 USA. [Fox, D. B.] Penn State Univ, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA. [Kruehler, T.] European So Observ, Santiago 19, Chile. [Trenti, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Trenti, M.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Trenti, M.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Cikota, A.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Bolmer, J.; Schweyer, T.] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany. [Elliott, J.] Harvard Smithsonian Ctr Astrophys, Astrophys Data Syst, Cambridge, MA 02138 USA. [Perna, R.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Afonso, P.] Amer River Coll, Dept Phys & Astron, Sacramento, CA 95841 USA. [Kann, D. A.; Klose, S.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Savaglio, S.] Univ Calabria, I-87036 Arcavacata Di Rende, Italy. RP Greiner, J (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM jcg@mpe.mpg.de; dfox@psu.edu; pschady@mpe.mpg.de; tkruehle@eso.org; michele.trenti@unimelb.edu.au; aleksandar.cikota@student.uibk.ac.at; jan@bolmer.de; jonathan.elliott@cfa.harvard.edu; delvaux@mpe.mpg.de; rosalba.perna@stonybrook.edu; afonsop@arc.losrios.edu; klose@tls-tautenburg.de; sandra.savaglio@googlemail.com; schmidl@tls-tautenburg.de; mohit@mpe.mpg.de; kvarela@mpe.mpg.de OI Trenti, Michele/0000-0001-9391-305X; Savaglio, Sandra/0000-0003-2354-3238 FU Sofja Kovalevskaja Award from the Alexander von Humboldt Foundation Germany; NSF [AST 1414246, HST-GO-13831.011-A]; DFG [KI 766/16-1, SA 2001/2-1]; Thuringer Ministerium fur Bildung, Wissenschaft und Kultur [FKZ 12010-514]; Bundesministerium fur Wirtschaft and Technologie through DLR (Deutsches Zentrum fur Luft- und Raumfahrt e.V.) [FKZ 50 OR 1211]; EXTraS; European Union [607452]; Leibniz-Prize (DFG) [HA 1850/28-1] FX The authors acknowledge astrostatistical consulting support from E. Feigelson. D.B.F. expresses appreciation to MPE Directors K. Nandra and R. Bender for administrative support of his sabbatical stay at MPE, where this collaboration was initiated. P.S. and M.T. acknowledge support through the Sofja Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation Germany. R.P. acknowledges co-funding through NSF grant No. AST 1414246 and HST-GO-13831.011-A.S.K. acknowledges support by DFG grant KI 766/16-1 and SSc support by the Thuringer Ministerium fur Bildung, Wissenschaft und Kultur under FKZ 12010-514. S.Sa. acknowledges support from the Bundesministerium fur Wirtschaft and Technologie through DLR (Deutsches Zentrum fur Luft- und Raumfahrt e.V.) FKZ 50 OR 1211. K.V. acknowledges support by DFG grant SA 2001/2-1, and C.D. acknowledges support through EXTraS, funded from the European Union's Seventh Framework Programme for research, technological development and demonstration under grant agreement No. 607452. A.C. is grateful for support of his visit to MPE Garching. Partial funding for GROND (hardware and personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). NR 125 TC 14 Z9 14 U1 0 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 AUG 10 PY 2015 VL 809 IS 1 AR 76 DI 10.1088/0004-637X/809/1/76 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500076 ER PT J AU MacGregor, MA Wilner, DJ Andrews, SM Lestrade, JF Maddison, S AF MacGregor, Meredith A. Wilner, David J. Andrews, Sean M. Lestrade, Jean-Franois Maddison, Sarah TI THE EPSILON ERIDANI SYSTEM RESOLVED BY MILLIMETER INTERFEROMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (epsilon Eridani); submillimeter: planetary systems ID MAIN-SEQUENCE STARS; ELEMENT-OF ERIDANI; YOUNG SOLAR-SYSTEM; DEBRIS DISK; ALMA OBSERVATIONS; SUBMILLIMETER GALAXIES; COLLISIONAL CASCADES; ALPHA CENTAURI; KUIPER-BELT; PLANET AB We present observations of. Eridani from the Submillimeter Array (SMA) at 1.3 mm and from the Australia Telescope Compact Array at 7 mm that reach an angular resolution of similar to 4 '' (13 AU). These first millimeter interferometer observations of epsilon Eridani, which hosts the closest debris disk to the Sun, reveal two distinct emission components: (1) the well-known outer dust belt, which, although patchy, is clearly resolved in the radial direction, and (2) an unresolved source coincident with the position of the star. We use direct model-fitting of the millimeter visibilities to constrain the basic properties of these two components. A simple Gaussian shape for the outer belt fit to the SMA data results in a radial location of 64.4(-3.0)(+2.4) AU and FWHM of 20.2(-8.2)(+6.0) AU (fractional width Delta R/R = 0.3). Similar results are obtained taking a power law radial emission profile for the belt, though the power law index cannot be usefully constrained. Within the noise obtained (0.2 mJy beam(-1)), these data are consistent with an axisymmetric belt model and show no significant azimuthal structure that might be introduced by unseen planets in the system. These data also limit any stellocentric offset of the belt to <9 AU, which disfavors the presence of giant planets on highly eccentric (>0.1) and wide (10's of AU) orbits. The flux density of the unresolved central component exceeds predictions for the stellar photosphere at these long wavelengths, by a marginally significant amount at 1.3 mm but by a factor of a few at 7 mm (with brightness temperature 13000 +/- 1600 K for a source size of the optical stellar radius). We attribute this excess emission to ionized plasma from a stellar corona or chromosphere. C1 [MacGregor, Meredith A.; Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lestrade, Jean-Franois] CNRS, LERMA, Observ Paris, F-75014 Paris, France. [Maddison, Sarah] Swinburne Univ, Ctr Astrophys & Supercomp, Melbourne, Vic, Australia. RP MacGregor, MA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mmacgregor@cfa.harvard.edu OI MacGregor, Meredith/0000-0001-7891-8143 FU National Science Foundation Graduate Research Fellowship [DGE1144152]; Swinburne Centre for Astrophysics Supercomputing; Universite Claude Bernard Lyon 1; Smithsonian Institution; Academia Sinica FX M.A.M acknowledges support from a National Science Foundation Graduate Research Fellowship (DGE1144152) and from the Swinburne Centre for Astrophysics & Supercomputing. D.J.W. thanks the Swinburne Visiting Researcher Scheme. S.T.M. acknowledges the support of the visiting professorship scheme from the Universite Claude Bernard Lyon 1. 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. We thank Mark Gurwell and Scott Paine for discussions about the Submillimeter Array primary beam shape. NR 53 TC 8 Z9 8 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 AUG 10 PY 2015 VL 809 IS 1 AR 47 DI 10.1088/0004-637X/809/1/47 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500047 ER PT J AU Montet, BT Morton, TD Foreman-Mackey, D Johnson, JA Hogg, DW Bowler, BP Latham, DW Bieryla, A Mann, AW AF Montet, Benjamin T. Morton, Timothy D. Foreman-Mackey, Daniel Johnson, John Asher Hogg, David W. Bowler, Brendan P. Latham, David W. Bieryla, Allyson Mann, Andrew W. TI STELLAR AND PLANETARY PROPERTIES OF K2 CAMPAIGN 1 CANDIDATES AND VALIDATION OF 17 PLANETS, INCLUDING A PLANET RECEIVING EARTH-LIKE INSOLATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; planetary systems; planets and satellites: detection; stars: fundamental parameters ID INTEGRAL-FIELD SPECTROGRAPH; FALSE-POSITIVE RATE; DIGITAL SKY SURVEY; M DWARFS; ADAPTIVE OPTICS; LIGHT CURVES; HOST-STARS; KEPLER; COOL; SYSTEM AB The extended Kepler mission, K2, is now providing photometry of new fields every three months in a search for transiting planets. In a recent study, Foreman-Mackey and collaborators presented a list of 36 planet candidates orbiting 31 stars in K2 Campaign 1. In this contribution, we present stellar and planetary properties for all systems. We combine ground-based seeing-limited survey data and adaptive optics imaging with an automated transit analysis scheme to validate 21 candidates as planets, 17 for the first time, and identify 6 candidates as likely false positives. Of particular interest is K2-18 (EPIC 201912552), a bright (K = 8.9) M2.8 dwarf hosting a 2.23 +/- 0.25 R-circle plus planet with T-eq = 272 +/- 15 K and an orbital period of 33 days. We also present two new open-source software packages which enable this analysis. The first, isochrones, is a flexible tool for fitting theoretical stellar models to observational data to determine stellar properties using a nested sampling scheme to capture the multimodal nature of the posterior distributions of the physical parameters of stars that may plausibly be evolved. The second is vespa, a new general-purpose procedure to calculate false positive probabilities and statistically validate transiting exoplanets. C1 [Montet, Benjamin T.; Bowler, Brendan P.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Montet, Benjamin T.; Johnson, John Asher; Latham, David W.; Bieryla, Allyson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morton, Timothy D.] Princeton Univ, Dept Astrophys, Princeton, NJ 08544 USA. [Foreman-Mackey, Daniel; Hogg, David W.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Foreman-Mackey, Daniel; Hogg, David W.] NYU, Ctr Data Sci, New York, NY 10003 USA. [Hogg, David W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Mann, Andrew W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Montet, BT (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. EM btm@astro.caltech.edu OI Montet, Benjamin/0000-0001-7516-8308; Latham, David/0000-0001-9911-7388 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; National Science Foundation Graduate Research Fellowship [DGE-1144469]; David and Lucile Packard Foundation; National Science Foundation [IIS-1124794]; National Aeronautics and Space Administration [NNX12AI50G, NNX14AE11G]; Moore-Sloan Data Science Environment at NYU; 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 We thank Roberto Sanchis-Ojeda (Berkeley), Dan Huber (Sydney) and Jeff Coughlin (SETI) for conversations and suggestions which improved the quality of this manuscript. We also thank Keivan Stassun (Vanderbilt) for his insights into stellar parameters and the rate of subgiant contamination for both Kepler and K2, which significantly improved this work. We thank the anonymous referee for their comments and suggestions. We are grateful to the entire Kepler team, past and present. Their tireless efforts were all essential to the tremendous success of the mission and the successes of K2 present and future. 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. 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 includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This paper includes data collected by the Sloan Digital Sky Survey. 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. B.T.M. is supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1144469. J.A.J. is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. D.F. M. and D.W.H. were partially supported by the National Science Foundation (grant IIS-1124794), the National Aeronautics and Space Administration (grant NNX12AI50G), and the Moore-Sloan Data Science Environment at NYU. T. D. M. is supported by the National Aeronautics and Space Administration (grant NNX14AE11G). NR 73 TC 21 Z9 21 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 AUG 10 PY 2015 VL 809 IS 1 AR 25 DI 10.1088/0004-637X/809/1/25 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500025 ER PT J AU Oronsaye, SI Ord, SM Bhat, NDR Tremblay, SE McSweeney, SJ Tingay, SJ van Straten, W Jameson, A Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kaplan, DL Lonsdale, CJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Wayth, RB Webster, RL Williams, A Williams, CL AF Oronsaye, S. I. Ord, S. M. Bhat, N. D. R. Tremblay, S. E. McSweeney, S. J. Tingay, S. J. van Straten, W. Jameson, A. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kaplan, D. L. Lonsdale, C. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. TI SIMULTANEOUS OBSERVATIONS OF GIANT PULSES FROM THE CRAB PULSAR, WITH THE MURCHISON WIDEFIELD ARRAY AND PARKES RADIO TELESCOPE: IMPLICATIONS FOR THE GIANT PULSE EMISSION MECHANISM SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Crab Nebula); ISM: structure; pulsars: general; pulsars: individual (Crab pulsar); scattering ID NEBULA PULSAR; INTERSTELLAR SCINTILLATION; STATISTICAL PROPERTIES; NP 0532; UNIVERSE; SCATTERING; SPECTRA; VARIABILITY; FREQUENCIES; DISPERSION AB We report on observations of giant pulses from the Crab pulsar performed simultaneously with the Parkes radio telescope and the incoherent combination of the Murchison Widefield Array (MWA) antenna tiles. The observations were performed over a duration of approximately one hour at a center frequency of 1382 MHz with 340 MHz bandwidth at Parkes, and at a center frequency of 193 MHz with 15 MHz bandwidth at the MWA. Our analysis has led to the detection of 55 giant pulses at the MWA and 2075 at Parkes above a threshold of 3.5 sigma and 6.5 sigma, respectively. We detected 51% of the MWA giant pulses at the Parkes radio telescope, with spectral indices in the range of -3.6 > alpha > -4.9 (S-nu alpha nu(alpha)). We present a Monte Carlo analysis supporting the conjecture that the giant pulse emission in the Crab is intrinsically broadband, the less than 100% correlation being due to the relative sensitivities of the two instruments and the width of the spectral index distribution. Our observations are consistent with the hypothesis that the spectral index of giant pulses is drawn from normal distribution of standard deviation 0.6, but with a mean that displays an evolution with frequency from -3.00 at 1382 MHz, to -2.85 at 192 MHz. C1 [Oronsaye, S. I.; Ord, S. M.; Bhat, N. D. R.; Tremblay, S. E.; McSweeney, S. J.; Tingay, S. J.; Wayth, R. B.; Williams, A.] Curtin Univ, ICRAR, Bentley, WA 6102, Australia. [Oronsaye, S. I.; Ord, S. M.; Bhat, N. D. R.; Tremblay, S. E.; Tingay, S. J.; van Straten, W.; Jameson, A.; Mitchell, D. A.; Subrahmanyan, R.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [van Straten, W.; Jameson, A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bernardi, G.] SKASA, ZA-7405 Pinelands, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Mitchell, D. A.] CASS, Epping, NSW 1710, Australia. [Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Oronsaye, SI (reprint author), Curtin Univ, ICRAR, Bentley, WA 6102, Australia. RI Deshpande, Avinash/D-4868-2012; Wayth, Randall/B-2444-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Udayashankar , N/D-4901-2012; OI Wayth, Randall/0000-0002-6995-4131; M, Manjunath/0000-0001-8710-0730; van Straten, Willem/0000-0003-2519-7375 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; Victoria University of Wellington (IBM Shared University Research Grant) FX We would like to thank Haydon Knight for useful contributions during the preparation of this paper. 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 MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. This research was conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. NR 57 TC 5 Z9 5 U1 1 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 AUG 10 PY 2015 VL 809 IS 1 AR 51 DI 10.1088/0004-637X/809/1/51 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500051 ER PT J AU Osten, RA Wolk, SJ AF Osten, Rachel A. Wolk, Scott J. TI CONNECTING FLARES AND TRANSIENT MASS-LOSS EVENTS IN MAGNETICALLY ACTIVE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: flare; stars: late-type; stars: mass-loss ID EXTREME-ULTRAVIOLET-EXPLORER; X-RAY FLARES; ANGULAR-MOMENTUM LOSS; MAIN-SEQUENCE STARS; AD LEONIS; FREQUENCY-DISTRIBUTIONS; ENERGY PARTITION; STELLAR FLARES; ALPHA EMISSION; SOLAR-FLARES AB We explore the ramification of associating the energetics of extreme magnetic reconnection events with transient mass-loss in a stellar analogy with solar eruptive events. We establish energy partitions relative to the total bolometric radiated flare energy for different observed components of stellar flares and show that there is rough agreement for these values with solar flares. We apply an equipartition between the bolometric radiated flare energy and kinetic energy in an accompanying mass ejection, seen in solar eruptive events and expected from reconnection. This allows an integrated flare rate in a particular waveband to be used to estimate the amount of associated transient mass-loss. This approach is supported by a good correspondence between observational flare signatures on high flaring rate stars and the Sun, which suggests a common physical origin. If the frequent and extreme flares that young solar-like stars and low-mass stars experience are accompanied by transient mass-loss in the form of coronal mass ejections, then the cumulative effect of this mass-loss could be large. We find that for young solar-like stars and active M dwarfs, the total mass lost due to transient magnetic eruptions could have significant impacts on disk evolution, and thus planet formation, and also exoplanet habitability. C1 [Osten, Rachel A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Osten, Rachel A.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. RP Osten, RA (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM osten@stsci.edu FU NASA (Chandra) [NAS8-03060] FX R.A.O. acknowledges the useful discussions which took place at the International Space Science Institute workshop on Energy Partition in Solar and Stellar Flares for helping to frame elements of the study. S.J.W. was supported by NASA contract NAS8-03060 (Chandra). NR 70 TC 9 Z9 9 U1 0 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 AUG 10 PY 2015 VL 809 IS 1 AR 79 DI 10.1088/0004-637X/809/1/79 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500079 ER PT J AU Pober, JC Ali, ZS Parsons, AR McQuinn, M Aguirre, JE Bernardi, G Bradley, RF Carilli, CL Cheng, C DeBoer, DR Dexter, MR Furlanetto, SR Grobbelaar, J Horrell, J Jacobs, DC Klima, PJ Kohn, SA Liu, A MacMahon, DHE Maree, M Mesinger, A Moore, DF Razavi-Ghods, N Stefan, II Walbrugh, WP Walker, A Zheng, HX AF Pober, Jonathan C. Ali, Zaki S. Parsons, Aaron R. McQuinn, Matthew Aguirre, James E. Bernardi, Gianni Bradley, Richard F. Carilli, Chris L. Cheng, Carina DeBoer, David R. Dexter, Matthew R. Furlanetto, Steven R. Grobbelaar, Jasper Horrell, Jasper Jacobs, Daniel C. Klima, Patricia J. Kohn, Saul A. Liu, Adrian MacMahon, David H. E. Maree, Matthys Mesinger, Andrei Moore, David F. Razavi-Ghods, Nima Stefan, Irina I. Walbrugh, William P. Walker, Andre Zheng, Haoxuan TI PAPER-64 CONSTRAINTS ON REIONIZATION. II. THE TEMPERATURE OF THE z=8.4 INTERGALACTIC MEDIUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; galaxies: high-redshift; intergalactic medium ID STAR-FORMING GALAXIES; LY-ALPHA EMITTERS; MURCHISON-WIDEFIELD-ARRAY; FORMATION RATE INDICATOR; CM POWER SPECTRUM; X-RAY BINARIES; COSMIC REIONIZATION; 21-CM FLUCTUATIONS; REDSHIFT Z; EPOCH AB We present constraints on both the kinetic temperature of the intergalactic medium (IGM) at z = 8.4, and on models for heating the IGM at high-redshift with X-ray emission from the first collapsed objects. These constraints are derived using a semi-analytic method to explore the new measurements of the 21 cm power spectrum from the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER), which were presented in a companion paper, Ali et al. Twenty-one cm power spectra with amplitudes of hundreds of mK2 can be generically produced if the kinetic temperature of the IGM is significantly below the temperature of the cosmic microwave background (CMB); as such, the new results from PAPER place lower limits on the IGM temperature at z = 8.4. Allowing for the unknown ionization state of the IGM, our measurements find the IGM temperature to be above approximate to 5 K for neutral fractions between 10% and 85%, above approximate to 7 K for neutral fractions between 15% and 80%, or above approximate to 10 K for neutral fractions between 30% and 70%. We also calculate the heating of the IGM that would be provided by the observed high redshift galaxy population, and find that for most models, these galaxies are sufficient to bring the IGM temperature above our lower limits. However, there are significant ranges of parameter space that could produce a signal ruled out by the PAPER measurements; models with a steep drop-off in the star formation rate density at high redshifts or with relatively low values for the X-ray to star formation rate efficiency of high redshift galaxies are generally disfavored. The PAPER measurements are consistent with (but do not constrain) a hydrogen spin temperature above the CMB temperature, a situation which we find to be generally predicted if galaxies fainter than the current detection limits of optical/NIR surveys are included in calculations of X-ray heating. C1 [Pober, Jonathan C.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Ali, Zaki S.; Parsons, Aaron R.; Cheng, Carina; Liu, Adrian] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Parsons, Aaron R.; DeBoer, David R.; Dexter, Matthew R.; MacMahon, David H. E.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [McQuinn, Matthew] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Aguirre, James E.; Kohn, Saul A.; Moore, David F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bernardi, Gianni; Grobbelaar, Jasper; Horrell, Jasper; Maree, Matthys; Walbrugh, William P.; Walker, Andre] SKA SA, Pinelands, South Africa. [Bernardi, Gianni] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, Gianni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bradley, Richard F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA USA. [Bradley, Richard F.; Klima, Patricia J.] Natl Radio Astron Observ, Charlottesville, VA USA. [Bradley, Richard F.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Carilli, Chris L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Carilli, Chris L.; Razavi-Ghods, Nima; Stefan, Irina I.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Furlanetto, Steven R.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Jacobs, Daniel C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Liu, Adrian] Berkeley Ctr Cosmol Phys, Berkeley, CA USA. [Mesinger, Andrei] Scuola Normale Super Pisa, Pisa, Italy. [Zheng, Haoxuan] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Pober, JC (reprint author), Univ Washington, Dept Phys, Seattle, WA 98195 USA. OI Pober, Jonathan/0000-0002-3492-0433 FU National Science Foundation (NSF) [0804508, 1129258, 1125558]; NSF [1302774, 1352519, 1401708]; Mount Cuba Astronomical Association FX PAPER is supported by grants from the National Science Foundation (NSF; awards 0804508, 1129258, and 1125558). J.C.P., A.R.P., and D.C.J. would like to acknowledge NSF support (awards 1302774, 1352519, and 1401708, respectively). J.E.A. would like to acknowledge a generous grant from the Mount Cuba Astronomical Association for computing resources. We graciously thank SKA-SA for onsite infrastructure and observing support. In addition we would like to thank our South African interns Monde Manzini and Ruvano Casper from Durban University of Technology (DUT), who helped build out the array from 32 antennas to the 64 antennas this analysis was based on. The authors would also like to thank Anson D'Aloisio, Adam Lidz, Jordan Mirocha, and Jonathan Pritchard for very helpful and fruitful conversations, Brant Robertson for providing the quantitative error contours in the R15 model, and our reviewer for helpful suggestions for better quantifying the effects of certain approximations in our work. NR 71 TC 23 Z9 23 U1 0 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 AUG 10 PY 2015 VL 809 IS 1 AR 62 DI 10.1088/0004-637X/809/1/62 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500062 ER PT J AU Rugheimer, S Kaltenegger, L Segura, A Linsky, J Mohanty, S AF Rugheimer, S. Kaltenegger, L. Segura, A. Linsky, J. Mohanty, S. TI EFFECT OF UV RADIATION ON THE SPECTRAL FINGERPRINTS OF EARTH-LIKE PLANETS ORBITING M STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; planets and satellites: atmospheres; planets and satellites: terrestrial planets; stars: low-mass ID EXOPLANET HOST STARS; WEBB-SPACE-TELESCOPE; EXTRA-SOLAR PLANETS; DIGITAL SKY SURVEY; HIGH-LEVEL CLOUDS; K-BAND SPECTRA; M-DWARFS; HABITABLE ZONE; SUPER-EARTHS; MAGNETIC ACTIVITY AB We model the atmospheres and spectra of Earth-like planets orbiting the entire grid of M dwarfs for active and inactive stellar models with T-eff = 2300 K to T-eff = 3800 K and for six observed MUSCLES M dwarfs with UV radiation data. We set the Earth-like planets at the 1 AU equivalent distance and show spectra from the visible to IR (0.4-20 mu m) to compare detectability of features in different wavelength ranges with the. James Webb Space Telescope and other future ground- and spaced-based missions to characterize exo-Earths. We focus on the effect of UV activity levels on detectable atmospheric features that indicate habitability on Earth, namely, H2O, O-3, CH4, N2O, and CH3Cl. To observe signatures of life-O-2/O-3 in combination with reducing species like CH4-we find that early and active M dwarfs are the best targets of the M star grid for future telescopes. The O-2 spectral feature at 0.76 mu m is increasingly difficult to detect in reflected light of later M dwarfs owing to low stellar flux in that wavelength region. N2O, another biosignature detectable in the IR, builds up to observable concentrations in our planetary models around M dwarfs with low UV flux. CH3Cl could become detectable, depending on the depth of the overlapping N2O feature. We present a spectral database of Earth-like planets around cool stars for directly imaged planets as a framework for interpreting future light curves, direct imaging, and secondary eclipse measurements of the atmospheres of terrestrial planets in the habitable zone. to design and assess future telescope capabilities. C1 [Rugheimer, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rugheimer, S.; Kaltenegger, L.] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA. [Kaltenegger, L.] MPIA, D-69117 Heidelberg, Germany. [Segura, A.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Linsky, J.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Linsky, J.] NIST, Boulder, CO 80309 USA. [Mohanty, S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab 1010, London SW7 2AZ, England. RP Rugheimer, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Rugheimer, Sarah/0000-0003-1620-7658 FU DFG [ENP KA 3142/1-1]; Simons Foundation [290357]; NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584] FX We especially thank Andrew West and Evgenya L. Shkolnik for useful conversations about M dwarfs. We also would like to thank Kevin France for discussions concerning the MUSCLES database. This work has made use of the MUSCLES M dwarf UV radiation field database. We would also like to acknowledge support from DFG funding ENP KA 3142/1-1 and the Simons Foundation (290357, Kaltenegger).; The UV radiation field for AD Leo was obtained from the Multimission Archive at the Space Telescope Science Institute (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 NAG5-7584 and by other grants and contracts. NR 93 TC 16 Z9 16 U1 5 U2 25 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 AUG 10 PY 2015 VL 809 IS 1 AR 57 DI 10.1088/0004-637X/809/1/57 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500057 ER PT J AU Sesar, B Bovy, J Bernard, EJ Caldwell, N Cohen, JG Fouesneau, M Johnson, CI Ness, M Ferguson, AMN Martin, NF Price-Whelan, AM Rix, HW Schlafly, EF Burgett, WS Chambers, KC Flewelling, H Hodapp, KW Kaiser, N Magnier, EA Platais, I Tonry, JL Waters, C Wyse, RFG AF Sesar, Branimir Bovy, Jo Bernard, Edouard J. Caldwell, Nelson Cohen, Judith G. Fouesneau, Morgan Johnson, Christian I. Ness, Melissa Ferguson, Annette M. N. Martin, Nicolas F. Price-Whelan, Adrian M. Rix, Hans-Walter Schlafly, Edward F. Burgett, William S. Chambers, Kenneth C. Flewelling, Heather Hodapp, Klaus W. Kaiser, Nick Magnier, Eugene A. Platais, Imants Tonry, John L. Waters, Christopher Wyse, Rosemary F. G. TI THE NATURE AND ORBIT OF THE OPHIUCHUS STREAM SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure; globular clusters: general ID DIGITAL SKY SURVEY; STELLAR STREAM; TIDAL STREAMS; PROPER-MOTION; GLOBULAR-CLUSTERS; ORPHAN STREAM; STAR-CLUSTERS; USNO-B; MILKY; CATALOG AB The Ophiuchus stream is a recently discovered stellar tidal stream in the Milky Way. We present high-quality spectroscopic data for 14 stream member stars obtained using the Keck and MMT telescopes. We confirm the stream as a fast moving (v(los) similar to 290 km s(-1)), kinematically cold group (sigma v(los) less than or similar to 1 km s(-1)) of alpha-enhanced and metal-poor stars ([alpha/Fe] similar to 0.4 dex, [Fe/H] similar to -2.0 dex). Using a probabilistic technique, we model the stream simultaneously in line-of-sight velocity, color-magnitude, coordinate, and proper motion space, and so determine its distribution in 6D phase-space. We find that the stream extends in distance from 7.5 to 9 kpc from the Sun; it is 50 times longer than wide, merely appearing highly foreshortened in projection. The analysis of the stellar population contained in the stream suggests that it is similar to 12 Gyr old, and that its initial stellar mass was similar to 2 x 10(4) M-circle dot (or at least greater than or similar to 7 x 10(3) M-circle dot). Assuming a fiducial Milky Way potential, we fit an orbit to the stream that matches the observed phase-space distribution, except for some tension in the proper motions: the stream has an orbital period of similar to 350 Myr, and is on a fairly eccentric orbit (e similar to 0.66) with a pericenter of similar to 3.5 kpc and an apocenter of similar to 17 kpc. The phase-space structure and stellar population of the stream show that its progenitor must have been a globular cluster that was disrupted only similar to 240 Myr ago. We do not detect any significant overdensity of stars along the stream that would indicate the presence of a progenitor, and conclude that the stream is all that is left of the progenitor. C1 [Sesar, Branimir; Fouesneau, Morgan; Ness, Melissa; Martin, Nicolas F.; Rix, Hans-Walter; Schlafly, Edward F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. [Bernard, Edouard J.; Ferguson, Annette M. N.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Caldwell, Nelson; Johnson, Christian I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cohen, Judith G.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Martin, Nicolas F.] Univ Strasbourg, CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France. [Price-Whelan, Adrian M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Burgett, William S.] GMTO Corp, Pasadena, CA 91101 USA. [Chambers, Kenneth C.; Flewelling, Heather; Hodapp, Klaus W.; Kaiser, Nick; Magnier, Eugene A.; Tonry, John L.; Waters, Christopher] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Platais, Imants; Wyse, Rosemary F. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Sesar, B (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM bsesar@mpia.de OI Bernard, Edouard/0000-0002-8722-225X; Chambers, Kenneth /0000-0001-6965-7789; Schlafly, Edward Ford/0000-0002-3569-7421 FU European Research Council under the European Union [321035]; Clay Fellowship; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877, 11-44155]; W. M. Keck Foundation FX B.S. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC Grant Agreement n. [321035]. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. A.P.W. is supported by a National Science Foundation Graduate Research Fellowship under Grant No. 11-44155. The Pan-STARRS1 Surveys (PS1) 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 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 Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), and the Los Alamos National Laboratory. 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. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. NR 65 TC 6 Z9 6 U1 0 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 AUG 10 PY 2015 VL 809 IS 1 AR 59 DI 10.1088/0004-637X/809/1/59 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500059 ER PT J AU Sullivan, PW Winn, JN Berta-Thompson, ZK Charbonneau, D Deming, D Dressing, CD Latham, DW Levine, AM McCullough, PR Morton, T Ricker, GR Vanderspek, R Woods, D AF Sullivan, Peter W. Winn, Joshua N. Berta-Thompson, Zachory K. Charbonneau, David Deming, Drake Dressing, Courtney D. Latham, David W. Levine, Alan M. McCullough, Peter R. Morton, Timothy Ricker, George R. Vanderspek, Roland Woods, Deborah TI THE TRANSITING EXOPLANET SURVEY SATELLITE: SIMULATIONS OF PLANET DETECTIONS AND ASTROPHYSICAL FALSE POSITIVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: detection; space vehicles: instruments; surveys ID INTERMEDIATE-MASS STARS; FINITE INTEGRATION TIME; MAIN-SEQUENCE STARS; LUMINOSITY FUNCTION; ECLIPSING BINARIES; PHOTOMETRIC SURVEYS; EXTRASOLAR PLANETS; SPACE-TELESCOPE; GALACTIC DISK; DATA RELEASE AB The Transiting Exoplanet Survey Satellite (TESS) is a NASA-sponsored Explorer mission that will perform a wide-field survey for planets that transit bright host stars. Here, we predict the properties of the transiting planets that TESS will detect along with the EB stars that produce false-positive photometric signals. The predictions are based on Monte Carlo simulations of the nearby population of stars, occurrence rates of planets derived from Kepler, and models for the photometric performance and sky coverage of the TESS cameras. We expect that TESS will find approximately 1700 transiting planets from 2 x 10(5) pre-selected target stars. This includes 556 planets smaller than twice the size of Earth, of which 419 are hosted by M dwarf stars and 137 are hosted by FGK dwarfs. Approximately 130 of the R < 2 R-circle plus planets will have host stars brighter than K-s = 9. Approximately 48 of the planets with R < 2 R-circle plus lie within or near the habitable zone (0.2 < S/S-circle plus < 2); between 2 and 7 such planets have host stars brighter than K-s = 9. We also expect approximately 1100 detections of planets with radii 2-4 R-circle plus, and 67 planets larger than 4 R-circle plus. Additional planets larger than 2 R-circle plus can be detected around stars that are not among the pre-selected target stars, because TESS will also deliver full-frame images at a 30-minute cadence. The planet detections are accompanied by over 1000 astrophysical false positives. We discuss how TESS data and ground-based observations can be used to distinguish the false positives from genuine planets. We also discuss the prospects for follow-up observations to measure the masses and atmospheres of the TESS planets. C1 [Sullivan, Peter W.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sullivan, Peter W.; Winn, Joshua N.; Berta-Thompson, Zachory K.; Levine, Alan M.; Ricker, George R.; Vanderspek, Roland] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Charbonneau, David; Dressing, Courtney D.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [McCullough, Peter R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [McCullough, Peter R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Morton, Timothy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Woods, Deborah] MIT, Lincoln Lab, Lexington, MA 02420 USA. RP Sullivan, PW (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. OI Berta-Thompson, Zachory/0000-0002-3321-4924 FU National Aeronautics and Space Administration; National Science Foundation FX We are grateful to the referee, Scott Gaudi, for providing constructive criticism that has led to improvements in this paper. We thank the members of the TESS Science Team for their contributions to the mission. In particular, Jacob Bean, Tabetha Boyajian, Eric Gaidos, Daniel Huber, Geoffrey Marcy, Roberto Sanchis-Ojeda, and Keivan Stassun provided helpful comments on the manuscript, and discussions with Jon Jenkins helped inform our approach to the simulations. We acknowledge Anthony Smith, Kristin Clark, and Michael Chrisp at MIT-Lincoln Laboratory for their respective roles in the project management, systems engineering, and optical design for the TESS payload. In addition, Barry Burke and Vyshnavi Suntharalingam at MIT-LL provided useful input to the PSF model. We thank Leo Girardi for adding the TESS bandpass to the TRILEGAL simulation and for providing a perl script to facilitate the queries. We also thank Gibor Basri for sharing the stellar variability data from Kepler. 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 the National Aeronautics and Space Administration and the National Science Foundation. NR 82 TC 39 Z9 39 U1 1 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 AUG 10 PY 2015 VL 809 IS 1 AR 77 DI 10.1088/0004-637X/809/1/77 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500077 ER PT J AU Valencic, LA Smith, RK AF Valencic, Lynne A. Smith, Randall K. TI INTERSTELLAR DUST PROPERTIES FROM A SURVEY OF X-RAY HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; X-rays: ISM ID COLOR-MAGNITUDE DIAGRAMS; GLOBULAR-CLUSTER SYSTEM; PULSAR 4U 1538-52; SOURCE CYGNUS X-2; OPTICAL COUNTERPART; NEUTRON-STAR; CENTAURUS X-3; BLACK-HOLE; METAL-RICH; GRS 1915+105 AB Interstellar dust grains produce X-ray halos around bright sources due to small-angle X-ray scattering. Numerous studies have examined these halos, but no systematic study has yet tested the available halo data against the large number of well-defined dust models in circulation. We have therefore obtained the largest sample to date of X-ray dust halos from XMM-Newton and Chandra, and fitted them with 14 commonly used dust grain models, including comparisons with the optical extinction, A(V), where available in the literature. Our main conclusions are summarized as follows. (1) Comparing A(V) with N-H values measured via X-ray spectral fits, we find a ratio of A(V)/N-H (10(21) cm(-2)) = 0.48 +/- 0.06, in agreement with previous work. (2) Out of 35 halos, 27 could be fit by one or more grain models, with the most successful models having maximum grain radius a(max) < 0.4 mu m and fewer large grains than the less successful models. This suggests that the diffuse ISM does not contain a signicant presence of grains with a(max) > 0.5 mu m. (3) Most halos were best fit assuming a single dust cloud dominated the scattering, rather than smoothly distributed dust along the sightline. (4) Eight sources could not be fit with the models considered here, most of which were along distant (d > 5 kpc) sight lines through the Galactic thin disk. (5) Some sight lines had halos with observed X-ray scattering optical depth tau(sca)/AV that were signicantly different than expected. This may result from an inhomogeneous dust distribution across the halo extraction area. C1 [Valencic, Lynne A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Valencic, Lynne A.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Smith, Randall K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Valencic, LA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM lynne.a.valencic@nasa.gov FU NASA [NNX10AE04G, NNX10AD10G]; Chandra grant [GO7-8142B] FX The authors thank the anonymous referee for many insightful comments that significantly improved this work. They also gratefully acknowledge helpful discussions with Eli Dwek and Fred Seward. Financial support for this work was made possible by NASA Grants NNX10AE04G and NNX10AD10G and Chandra grant GO7-8142B. NR 146 TC 5 Z9 5 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 AUG 10 PY 2015 VL 809 IS 1 AR 66 DI 10.1088/0004-637X/809/1/66 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500066 ER PT J AU Welsh, WF Orosz, JA Short, DR Cochran, WD Endl, M Brugamyer, E Haghighipour, N Buchhave, LA Doyle, LR Fabrycky, DC Hinse, TC Kane, SR Kostov, V Mazeh, T Mills, SM Muller, TWA Quarles, B Quinn, SN Ragozzine, D Shporer, A Steffen, JH Tal-Or, L Torres, G Windmiller, G Borucki, WJ AF Welsh, William F. Orosz, Jerome A. Short, Donald R. Cochran, William D. Endl, Michael Brugamyer, Erik Haghighipour, Nader Buchhave, Lars A. Doyle, Laurance R. Fabrycky, Daniel C. Hinse, Tobias Cornelius Kane, Stephen R. Kostov, Veselin Mazeh, Tsevi Mills, Sean M. Mueller, Tobias W. A. Quarles, Billy Quinn, Samuel N. Ragozzine, Darin Shporer, Avi Steffen, Jason H. Tal-Or, Lev Torres, Guillermo Windmiller, Gur Borucki, William J. TI KEPLER 453 b-THE 10th KEPLER TRANSITING CIRCUMBINARY PLANET SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: eclipsing; planets and satellites: detection; planets and satellites: dynamical evolution and stability; stars: individual (KIC 9632895, Kepler-453) ID MAIN-SEQUENCE STARS; CLOSE BINARY-SYSTEMS; LOW-MASS; LIGHT CURVES; HIERARCHICAL TRIPLE; ECLIPSING BINARIES; ROTATION PERIODS; STELLAR ROTATION; TIDAL EVOLUTION; HABITABLE ZONES AB We present the discovery of Kepler-453 b, a 6.2 R-circle plus planet in a low-eccentricity, 240.5 day orbit about an eclipsing binary. The binary itself consists of a 0.94 and 0.195 M-circle dot pair of stars with an orbital period of 27.32 days. The plane of the planet's orbit is rapidly precessing, and its inclination only becomes sufficiently aligned with the primary star in the latter portion of the Kepler data. Thus three transits are present in the second half of the light curve, but none of the three conjunctions that occurred during the first half of the light curve produced observable transits. The precession period is similar to 103 years, and during that cycle, transits are visible only similar to 8.9% of the time. This has the important implication that for every system like Kepler-453 that we detect, there are similar to 11.5 circumbinary systems that exist but are not currently exhibiting transits. The planet's mass is too small to noticeably perturb the binary, and consequently its mass is not measurable with these data; however, our photodynamical model places a 1 sigma upper limit of 16 M-circle plus. With a period 8.8 times that of the binary, the planet is well outside the dynamical instability zone. It does, however, lie within the habitable zone of the binary, making it the third of 10 Kepler circumbinary planets to do so. C1 [Welsh, William F.; Orosz, Jerome A.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Cochran, William D.; Endl, Michael; Brugamyer, Erik] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 USA. [Buchhave, Lars A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Doyle, Laurance R.] SETI Inst, Mountain View, CA 94043 USA. [Doyle, Laurance R.] Principia Coll, IMoP, Elsah, IL 62028 USA. [Fabrycky, Daniel C.; Mills, Sean M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hinse, Tobias Cornelius] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hinse, Tobias Cornelius] Armagh Observ, Armagh BT61 9DG, North Ireland. [Kane, Stephen R.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Kostov, Veselin] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Mazeh, Tsevi; Tal-Or, Lev] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Mueller, Tobias W. A.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Quarles, Billy; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Ragozzine, Darin] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Steffen, Jason H.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM wwelsh@mail.sdsu.edu; jorosz@mail.sdsu.edu OI Buchhave, Lars A./0000-0003-1605-5666 FU Institute for Astronomy; NASA Astrobiology Institute at the University of Hawaii-Manoa; National Science Foundation [AST-1109928]; NASA's Kepler Participating Scientist Program [NNX12AD23G]; Origins of Solar Systems Program [NNX13AI76G]; Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Program; KASI (Korea Astronomy and Space Science Institute) [2013-9-400-0/2014-1-400-06]; Northern Ireland Department of Culture, Arts and Leisure (DCAL); NASA ADAP grant [NNX13AF20G]; NASA Origins grant [NNX12AQ62G]; Astrobiology Institute under Institute for Astronomy, University of Hawaii [NNA09DA77]; HST grant [HST-GO-12548.06-A]; NASA from the Space Telescope Science Institute [HST-GO-12548.06-A]; NASA [NAS5-26555]; European Research Council under the EU's Seventh Framework Programme (ERC Grant) [291352]; NASA Postdoctoral Program; NSF grant [AST-1007992]; NASA, Science Mission Directorate FX We thank the ApJ Editors for their patience and the anonymous referee for suggestions that helped improve this paper. We thank Amy McQuillan of Tel Aviv University for assistance with the measurement of the ACF, and Justice Bruursema for assisting with the WIYN observations. W.F.W. thanks the Institute for Astronomy and the NASA Astrobiology Institute at the University of Hawaii-Manoa for their support and kind hospitality during his sabbatical visit when part of this project was carried out. W.F.W. and J.A.O. gratefully acknowledge support from the National Science Foundation via grant AST-1109928, and from NASA's Kepler Participating Scientist Program (NNX12AD23G) and Origins of Solar Systems Program (NNX13AI76G). T.C.H. gratefully acknowledges financial support from the Korea Research Council for Fundamental Science and Technology (KRCF) through the Young Research Scientist Fellowship Program and financial support from KASI (Korea Astronomy and Space Science Institute) grant number 2013-9-400-0/2014-1-400-06. Numerical computations were partly carried out using the SFI/HEA Irish Centre for High-End Computing (ICHEC) and the KMTNet computing cluster at the Korea Astronomy and Space Science Institute. Astronomical research at the Armagh Observatory is funded by the Northern Ireland Department of Culture, Arts and Leisure (DCAL). N.H. acknowledges support from the NASA ADAP grant NNX13AF20G, NASA Origins grant NNX12AQ62G, Astrobiology Institute under Cooperative Agreement NNA09DA77 at the Institute for Astronomy, University of Hawaii, and HST grant HST-GO-12548.06-A. Support for program HST-GO-12548.06-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, Incorporated, under NASA contract NAS5-26555. T.M. gratefully acknowledges support of from the European Research Council under the EU's Seventh Framework Programme (ERC Grant Agreement No. 291352). B.Q. gratefully acknowledges the support of the NASA Postdoctoral Program. J.H.S. acknowledges the support from NASA's Kepler Participating Scientist Program (NNX12AD23G). G.T. acknowledges partial support from NSF grant AST-1007992. The authors acknowledge the outstanding work of David Ciardi (NExScI/Caltech) in organizing and maintaining the Kepler Community Follow-up Observing Program (CFOP) website.26 We also thank Phil Lucas for organizing the UKIRT J-band observations of the Kepler field available on the CFOP website. 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. Kepler was competitively selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. NR 79 TC 20 Z9 20 U1 0 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 AUG 10 PY 2015 VL 809 IS 1 AR 26 DI 10.1088/0004-637X/809/1/26 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500026 ER PT J AU Willis, S Guzman, A Marengo, M Smith, HA Martinez, R Allen, L AF Willis, S. Guzman, A. Marengo, M. Smith, H. A. Martinez, R. Allen, L. TI THE SCHMIDT LAW IN SIX GALACTIC MASSIVE STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; stars: formation ID NEARBY MOLECULAR CLOUDS; SPITZER-SPACE-TELESCOPE; HERSCHEL HI-GAL; MILKY-WAY; NGC 6334; FORMATION RATES; ARRAY CAMERA; COMPLEX; GALAXIES; EXTINCTION AB We present a census of young stars in five massive star-forming regions in the 4th Galactic quadrant, G305, G326-4, G326-6, G333 (RCW 106), and G351, and combine this census with an earlier census of young stars in NGC 6334. Each region was observed at J, H, and K-s with the NOAO Extremely Wide-Field Infrared Imager and combined with deep observations taken with the Infrared Array Camera (IRAC) on board the Spitzer Space Telescope at the wavelengths 3.6 and 4.5 mu m. We derived a five band point-source catalog containing >200,000 infrared sources in each region. We have identified a total of 2871 YSO candidates, 363 Class I YSOs, and 2508 Class II YSOs. We mapped the column density of each cloud using observations from Herschel between 160 and 500 mu m and near-infrared extinction maps in order to determine the average gas surface density above A(V) > 2. We study the surface density of the YSOs and the star-formation rate as a function of the column density within each cloud and compare them to the results for nearby star-forming regions. We find a range in power-law indices across the clouds, with the dispersion in the local relations in an individual cloud much lower than the average over the six clouds. We find the average over the six clouds to be Sigma(SFR) similar to Sigma(2.15 +/- 0.41)(gas) and power-law exponents ranging from 1.77 to 2.86, similar to the values derived within nearby star-forming regions, including Taurus and Orion. The large dispersion in the power-law relations between individual Milky Way molecular clouds reinforces the idea that there is not a direct universal connection between Sigma(gas) and a cloud's observed star-formation rate. C1 [Willis, S.; Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. [Willis, S.; Guzman, A.; Smith, H. A.; Martinez, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Willis, S (reprint author), Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. EM swillis@cfa.harvard.edu OI Guzman, Andres/0000-0003-0990-8990 FU NASA [1407, NNX12AI55G, NNX10AD68G]; JPL-RSA [1369565]; National Aeronautics and Space Administration's Earth Science Technology Office [NCC5-626] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. 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 NCC5-626 between NASA and the California Institute of Technology. Montage is maintained by the NASA/IPAC Infrared Science Archive. S.W. acknowledges partial support from NASA grants NNX12AI55G and NNX10AD68G, and JPL-RSA 1369565. S.W. and H.A.S. acknowledge partial support from NASA Grants NNX12AI55G and NNX10AD68G, and JPL-RSA 1369565. NR 52 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 AUG 10 PY 2015 VL 809 IS 1 AR 87 DI 10.1088/0004-637X/809/1/87 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR9DN UT WOS:000361653500087 ER PT J AU Kaplan, DL Tingay, SJ Manoharan, PK Macquart, JP Hancock, P Morgan, J Mitchell, DA Ekers, RD Wayth, RB Trott, C Murphy, T Oberoi, D Cairns, IH Feng, L Kudryavtseva, N Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Gaensler, BM Greenhill, LJ Walker, NH Hazelton, BJ Hollitt, MJ Lonsdale, CJ McWhirter, SR Morales, MF Morgan, E Ord, SM Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Webster, RL Williams, A Williams, CL AF Kaplan, D. L. Tingay, S. J. Manoharan, P. K. Macquart, J. P. Hancock, P. Morgan, J. Mitchell, D. A. Ekers, R. D. Wayth, R. B. Trott, C. Murphy, T. Oberoi, D. Cairns, I. H. Feng, L. Kudryavtseva, N. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Gaensler, B. M. Greenhill, L. J. Walker, N. Hurley Hazelton, B. J. Hollitt, M. Johnston Lonsdale, C. J. McWhirter, S. R. Morales, M. F. Morgan, E. Ord, S. M. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Webster, R. L. Williams, A. Williams, C. L. TI MURCHISON WIDEFIELD ARRAY OBSERVATIONS OF ANOMALOUS VARIABILITY: A SERENDIPITOUS NIGHT-TIME DETECTION OF INTERPLANETARY SCINTILLATION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE radio continuum: galaxies; scattering; Sun: coronal mass ejections (CMEs); Sun: heliosphere; techniques: interferometric ID RADIO-SOURCES; INTERSTELLAR SCINTILLATION; CATALOG; VELOCITIES AB We present observations of high-amplitude rapid (2 s) variability toward two bright, compact extragalactic radio sources out of several hundred of the brightest radio sources in one of the 30 degrees x 30 degrees Murchison Widefield Array (MWA) Epoch of Reionization fields using the MWA at 155 MHz. After rejecting intrinsic, instrumental, and ionospheric origins we consider the most likely explanation for this variability to be interplanetary scintillation (IPS), likely the result of a large coronal mass ejection propagating from the Sun. This is confirmed by roughly contemporaneous observations with the Ooty Radio Telescope. We see evidence for structure on spatial scales ranging from <1000 to >10(6) km. The serendipitous night-time nature of these detections illustrates the new regime that the MWA has opened for IPS studies with sensitive night-time, wide-field, low-frequency observations. This regime complements traditional dedicated strategies for observing IPS and can be utilized in real-time to facilitate dedicated follow-up observations. At the same time, it allows large-scale surveys for compact (arcsec) structures in low-frequency radio sources despite the 2' resolution of the array. C1 [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Tingay, S. J.; Macquart, J. P.; Hancock, P.; Morgan, J.; Wayth, R. B.; Trott, C.; Kudryavtseva, N.; Walker, N. Hurley; Ord, S. M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Tingay, S. J.; Macquart, J. P.; Hancock, P.; Mitchell, D. A.; Wayth, R. B.; Trott, C.; Murphy, T.; Gaensler, B. M.; Ord, S. M.; Subrahmanyan, R.; Webster, R. L.] Tata Inst Fundamental Res, ARC Ctr Excellence All Sky Astrophys CAASTRO, Ooty 643001, India. [Manoharan, P. K.; Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Radio Astron Ctr, Ooty 643001, India. [Mitchell, D. A.; Ekers, R. D.] CASS, Epping, NSW 1710, Australia. [Murphy, T.; Cairns, I. H.; Gaensler, B. M.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Feng, L.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Hollitt, M. Johnston] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Kaplan, DL (reprint author), Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. EM kaplan@uwm.edu RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Hurley-Walker, Natasha/B-9520-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; OI Wayth, Randall/0000-0002-6995-4131; Cairns, Iver/0000-0001-6978-9765; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; M, Manjunath/0000-0001-8710-0730; Gaensler, Bryan/0000-0002-3382-9558; Kaplan, David/0000-0001-6295-2881; Murphy, Tara/0000-0002-2686-438X; Kudryavtseva, Nadia/0000-0002-1372-0942; Ekers, Ron/0000-0002-3532-9928; Hancock, Paul/0000-0002-4203-2946 FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; NSF [AST-1412421]; ISRO; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from the IBM; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Western Australian State government FX We thank an anonymous referee for a thorough and thoughtful review. We thank B. Jackson, C. Loi, and A. Rowlinson for helpful conversations. 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 MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). D.L.K. is additionally supported by NSF grant AST-1412421. P.K.M. acknowledges partial support from ISRO. Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 40 TC 4 Z9 5 U1 0 U2 7 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 AUG 10 PY 2015 VL 809 IS 1 AR L12 DI 10.1088/2041-8205/809/1/L12 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO7EJ UT WOS:000359321900012 ER PT J AU Taniguchi, Y Kajisawa, M Kobayashi, MAR Nagao, T Shioya, Y Scoville, NZ Sanders, DB Capak, PL Koekemoer, AM Toft, S McCracken, HJ Le Fevre, O Tasca, L Sheth, K Renzini, A Lilly, S Carollo, M Kovac, K Ilbert, O Schinnerer, E Fu, H Tresse, L Griffiths, RE Civano, F AF Taniguchi, Yoshiaki Kajisawa, Masaru Kobayashi, Masakazu A. R. Nagao, Tohru Shioya, Yasuhiro Scoville, Nick Z. Sanders, David B. Capak, Peter L. Koekemoer, Anton M. Toft, Sune McCracken, Henry J. Le Fevre, Olivier Tasca, Lidia Sheth, Kartik Renzini, Alvio Lilly, Simon Carollo, Marcella Kovac, Katarina Ilbert, Olivier Schinnerer, Eva Fu, Hai Tresse, Laurence Griffiths, Richard E. Civano, Francesca TI DISCOVERY OF MASSIVE, MOSTLY STAR FORMATION QUENCHED GALAXIES WITH EXTREMELY LARGE Ly alpha EQUIVALENT WIDTHS AT z similar to 3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; early universe; galaxies: evolution; galaxies: formation; galaxies: high-redshift ID EVOLUTION SURVEY COSMOS; QUIESCENT GALAXIES; STELLAR POPULATIONS; EMITTING GALAXIES; DROPOUT GALAXIES; SOURCE CATALOG; FIELD; REDSHIFT; EMITTERS; PROGENITORS AB We report a discovery of six massive galaxies with both extremely large Ly alpha equivalent widths (EWs) and evolved stellar populations at z similar to 3. These MAssive Extremely STrong Ly alpha emitting Objects (MAESTLOs) have been discovered in our large-volume systematic survey for strong Ly alpha emitters (LAEs) with 12 optical intermediate-band data taken with Subaru/Suprime-Cam in the COSMOS field. Based on the spectral energy distribution fitting analysis for these LAEs, it is found that these MAESTLOs have (1) large rest-frame EWs of EW0 (Ly alpha) similar to 100-300 angstrom, (2) M-star similar to 10(10.5) -10(11.1) M-circle dot, and (3) relatively low specific star formation rates of SFR/M-star similar to 0.03-1 Gyr(-1). Three of the six MAESTLOs have extended Ly alpha emission with a radius of several kiloparsecs, although they show very compact morphology in the HST/ACS images, which correspond to the rest-frame UV continuum. Since the MAESTLOs do not show any evidence for active galactic nuclei, the observed extended Ly alpha emission is likely to be caused by a star formation process including the superwind activity. We suggest that this new class of LAEs, MAESTLOs, provides a missing link from star-forming to passively evolving galaxies at the peak era of the cosmic star formation history. C1 [Taniguchi, Yoshiaki; Kajisawa, Masaru; Kobayashi, Masakazu A. R.; Nagao, Tohru; Shioya, Yasuhiro] Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. [Kajisawa, Masaru] Ehime Univ, Grad Sch Sci & Engn, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. [Scoville, Nick Z.; Capak, Peter L.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Sanders, David B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Capak, Peter L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Toft, Sune] Univ Copenhagen, Dark Cosmol Ctr, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [McCracken, Henry J.] Univ Paris 06, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Le Fevre, Olivier; Tasca, Lidia; Ilbert, Olivier; Tresse, Laurence] Aix Marseille Univ, LAM, CNRS, UMR 7326, F-13388 Marseille, France. [Sheth, Kartik] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Renzini, Alvio] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Lilly, Simon; Carollo, Marcella; Kovac, Katarina] Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. [Schinnerer, Eva] MPI Astron, D-69117 Heidelberg, Germany. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52245 USA. [Griffiths, Richard E.] Univ Hawaii, Phys & Astron, Hilo, HI 96720 USA. [Civano, Francesca] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, Francesca] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Taniguchi, Y (reprint author), Ehime Univ, Res Ctr Space & Cosm Evolut, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. EM tani@cosmos.phys.sci.ehime-u.ac.jp FU JSPS [15340059, 17253001, 19340046, 23244031, 23654068, 25707010] FX We would like to thank both the Subaru and HST staff for their invaluable help, as well as all members of the COSMOS team. We would also like to thank the anonymous referee for valuable suggestions and comments. We also thank Alex Hagen for kindly providing us with the information of their LAEs. This work was financially supported in part by JSPS (Y.T.: 15340059, 17253001, 19340046, and 23244031; T.N.: 23654068 and 25707010). Data analysis was in part carried out on the common use data analysis computer system at the Astronomy Data Center, ADC, of the National Astronomical Observatory of Japan. NR 36 TC 5 Z9 5 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 AUG 10 PY 2015 VL 809 IS 1 AR L7 DI 10.1088/2041-8205/809/1/L7 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO7EJ UT WOS:000359321900007 ER PT J AU Arora, BS Morgan, J Ord, SM Tingay, SJ Hurley-Walker, N Bell, M Bernardi, G Bhat, NDR Briggs, F Callingham, JR Deshpande, AA Dwarakanath, KS Ewall-Wice, A Feng, L For, BQ Hancock, P Hazelton, BJ Hindson, L Jacobs, D Johnston-Hollitt, M Kapinska, AD Kudryavtseva, N Lenc, E McKinley, B Mitchell, D Oberoi, D Offringa, AR Pindor, B Procopio, P Riding, J Staveley-Smith, L Wayth, RB Wu, C Zheng, Q Bowman, JD Cappallo, RJ Corey, BE Emrich, D Goeke, R Greenhill, LJ Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Morales, MF Morgan, E Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF Arora, B. S. Morgan, J. Ord, S. M. Tingay, S. J. Hurley-Walker, N. Bell, M. Bernardi, G. Bhat, N. D. R. Briggs, F. Callingham, J. R. Deshpande, A. A. Dwarakanath, K. S. Ewall-Wice, A. Feng, L. For, B. -Q. Hancock, P. Hazelton, B. J. Hindson, L. Jacobs, D. Johnston-Hollitt, M. Kapinska, A. D. Kudryavtseva, N. Lenc, E. McKinley, B. Mitchell, D. Oberoi, D. Offringa, A. R. Pindor, B. Procopio, P. Riding, J. Staveley-Smith, L. Wayth, R. B. Wu, C. Zheng, Q. Bowman, J. D. Cappallo, R. J. Corey, B. E. Emrich, D. Goeke, R. Greenhill, L. J. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Morales, M. F. Morgan, E. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI Ionospheric Modelling using GPS to Calibrate the MWA. I: Comparison of First Order Ionospheric Effects between GPS Models and MWA Observations SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE atmospheric effects; techniques: interferometric ID TOTAL ELECTRON-CONTENT AB We compare first-order (refractive) ionospheric effects seen by the MWA with the ionosphere as inferred from GPS data. The first-order ionosphere manifests itself as a bulk position shift of the observed sources across an MWA field of view. These effects can be computed from global ionosphere maps provided by GPS analysis centres, namely the CODE. However, for precision radio astronomy applications, data from local GPS networks needs to be incorporated into ionospheric modelling. For GPS observations, the ionospheric parameters are biased by GPS receiver instrument delays, among other effects, also known as receiver DCBs. The receiver DCBs need to be estimated for any non-CODE GPS station used for ionosphere modelling. In this work, single GPS station-based ionospheric modelling is performed at a time resolution of 10 min. Also the receiver DCBs are estimated for selected Geoscience Australia GPS receivers, located at Murchison Radio Observatory, Yarragadee, Mount Magnet and Wiluna. The ionospheric gradients estimated from GPS are compared with that inferred from MWA. The ionospheric gradients at all the GPS stations show a correlation with the gradients observed with the MWA. The ionosphere estimates obtained using GPS measurements show promise in terms of providing calibration information for the MWA. C1 [Arora, B. S.; Morgan, J.; Ord, S. M.; Tingay, S. J.; Hurley-Walker, N.; Bhat, N. D. R.; Hancock, P.; Kudryavtseva, N.; Wayth, R. B.; Emrich, D.; Lynch, M. J.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Callingham, J. R.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Briggs, F.; McKinley, B.; Offringa, A. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Callingham, J. R.; Mitchell, D.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Callingham, J. R.; Hancock, P.; Kapinska, A. D.; Lenc, E.; McKinley, B.; Mitchell, D.; Procopio, P.; Staveley-Smith, L.; Wayth, R. B.; Subrahmanyan, R.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Deshpande, A. A.; Dwarakanath, K. S.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Ewall-Wice, A.; Feng, L.; Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [For, B. -Q.; Kapinska, A. D.; Staveley-Smith, L.; Wu, C.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Hindson, L.; Johnston-Hollitt, M.; Zheng, Q.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Jacobs, D.; Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Mitchell, D.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [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. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Waterson, M.] Jodrell Bank Observ, SKA Org Headquarters, Macclesfield SK11 9DL, Cheshire, England. RP Arora, BS (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. EM balwinderarora@gmail.com RI Wayth, Randall/B-2444-2013; Dwarakanath, K /D-4876-2012; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Kapinska, Anna/B-3999-2014; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; Staveley-Smith, Lister/A-1683-2011 OI Lenc, Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942; Callingham, Joseph/0000-0002-7167-1819; Hancock, Paul/0000-0002-4203-2946; /0000-0002-0086-7363; Wayth, Randall/0000-0002-6995-4131; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Kapinska, Anna/0000-0002-5289-5729; Staveley-Smith, Lister/0000-0002-8057-0294 FU US National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington from IBM Shared University Research Grant [MED-E1799]; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia; Western Australian State government; CSIRO; National Collaborative Research Infrastructure Strategy; Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited FX The authors wish to thank Anthony Willis from National Research Council of Canada for the valuable discussions. This scientific work makes use of the MRO, operated by Commonwealth Scientific and Industrial Research Organisation (CSIRO). We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the CSIRO, National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 50 TC 4 Z9 4 U1 1 U2 9 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 AUG 10 PY 2015 VL 32 AR e029 DI 10.1017/pasa.2015.29 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO8RU UT WOS:000359439300001 ER PT J AU Waring, BG Alvarez-Cansino, L Barry, KE Becklund, KK Dale, S Gei, MG Keller, AB Lopez, OR Markesteijn, L Mangan, S Riggs, CE Rodriguez-Ronderos, ME Segnitz, RM Schnitzer, SA Powers, JS AF Waring, Bonnie G. Alvarez-Cansino, Leonor Barry, Kathryn E. Becklund, Kristen K. Dale, Sarah Gei, Maria G. Keller, Adrienne B. Lopez, Omar R. Markesteijn, Lars Mangan, Scott Riggs, Charlotte E. Rodriguez-Ronderos, Maria Elizabeth Segnitz, R. Max Schnitzer, Stefan A. Powers, Jennifer S. TI Pervasive and strong effects of plants on soil chemistry: a meta-analysis of individual plant 'Zinke' effects SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE individual plant effects; plant-soil interactions; spatial heterogeneity ID ORGANIC-MATTER DYNAMICS; PUBLICATION BIAS; DECIDUOUS TREES; FOREST; DECOMPOSITION; NUTRIENTS; NITROGEN; CARBON; INPUTS; HETEROGENEITY AB Plant species leave a chemical signature in the soils below them, generating fine-scale spatial variation that drives ecological processes. Since the publication of a seminal paper on plant-mediated soil heterogeneity by Paul Zinke in 1962, a robust literature has developed examining effects of individual plants on their local environments (individual plant effects). Here, we synthesize this work using meta-analysis to show that plant effects are strong and pervasive across ecosystems on six continents. Overall, soil properties beneath individual plants differ from those of neighbours by an average of 41%. Although the magnitudes of individual plant effects exhibit weak relationships with climate and latitude, they are significantly stronger in deserts and tundra than forests, and weaker in intensively managed ecosystems. The ubiquitous effects of plant individuals and species on local soil properties imply that individual plant effects have a role in plant soil feedbacks, linking individual plants with biogeochemical processes at the ecosystem scale. C1 [Waring, Bonnie G.; Becklund, Kristen K.; Gei, Maria G.; Riggs, Charlotte E.; Powers, Jennifer S.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Powers, Jennifer S.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. [Alvarez-Cansino, Leonor; Schnitzer, Stefan A.] Marquette Univ, Dept Biol Sci, Milwaukee, WI 53201 USA. [Alvarez-Cansino, Leonor; Lopez, Omar R.; Markesteijn, Lars; Mangan, Scott; Schnitzer, Stefan A.; Powers, Jennifer S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Alvarez-Cansino, Leonor] Univ Bayreuth, Dept Plant Ecol, D-95440 Bayreuth, Germany. [Barry, Kathryn E.; Rodriguez-Ronderos, Maria Elizabeth] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA. [Dale, Sarah] Nurture Lakeland, Staveley, Cumbria, England. [Keller, Adrienne B.] Indiana Univ, Dept Biol, Bloomington, IN USA. [Lopez, Omar R.] Inst Invest Cient & Serv Alta Tecnol, Clayton, Panama. [Markesteijn, Lars] Univ Oxford, Dept Zool, Oxford OX1 3PS, England. [Mangan, Scott] Washington Univ, Dept Biol, St Louis, MO 63130 USA. [Segnitz, R. Max] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. RP Powers, JS (reprint author), Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. EM powers@umn.edu OI Waring, Bonnie/0000-0002-8457-5164 FU NSF [DEB-1019441, DEB-1053237, DEB-0845071, DEB-1019436]; Sistema Nacional de Investigacion (SNI) de SENACYT FX This work was supported by NSF grants DEB-1019441 and DEB-1053237 to J.S.P., and grants nos DEB-0845071 and DEB-1019436 to S.A.S., and funding from Sistema Nacional de Investigacion (SNI) de SENACYT to O.R.L. NR 44 TC 5 Z9 5 U1 4 U2 28 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 AUG 7 PY 2015 VL 282 IS 1812 BP 91 EP 98 AR 20151001 DI 10.1098/rspb.2015.1001 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CS7ZM UT WOS:000362305500011 PM 26224711 ER PT J AU Erwin, DH AF Erwin, Douglas H. TI David M. Raup (1933-2015) OBITUARY SO NATURE LA English DT Biographical-Item C1 [Erwin, Douglas H.] Natl Museum Nat Hist, Dept Palaeobiol, Smithsonian Inst, Washington, DC 20560 USA. [Erwin, Douglas H.] Santa Fe Inst, Santa Fe, NM USA. RP Erwin, DH (reprint author), Natl Museum Nat Hist, Dept Palaeobiol, Smithsonian Inst, Washington, DC 20560 USA. EM erwind@si.edu NR 1 TC 0 Z9 0 U1 1 U2 6 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 AUG 6 PY 2015 VL 524 IS 7563 BP 36 EP 36 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO2QS UT WOS:000359002300021 PM 26245575 ER PT J AU Lemaitre, R Tavares, M AF Lemaitre, Rafael Tavares, Marcos TI New taxonomic and distributional information on hermit crabs (Crustacea: Anomura: Paguroidea) from the Gulf of Mexico, Caribbean Sea, and Atlantic coast of South America SO ZOOTAXA LA English DT Article DE Crustacea; Paguroidea; hermit crabs; new records; taxonomy; distribution; Gulf of Mexico; Caribbean Sea; Brazil; Atlantic South America ID GENUS PAGURISTES CRUSTACEA; A. MILNE-EDWARDS; FAMILY PAGURIDAE CRUSTACEA; TROPICAL WESTERN ATLANTIC; DECAPODA ANOMURA; PROVENZANOI GROUP; AREOPAGURISTES RAHAYU; TOMOPAGURUS CRUSTACEA; ANNOTATED CHECKLIST; MOLECULAR ANALYSIS AB A collection of Paguroidea recently obtained during deep-water expeditions along the coast of Brazil, forms the basis of this report. Of the 14 species reported from Brazil, 11 represent range extensions to the south, and one, Michelopagurus atlanticus (Bouvier, 1922), is a first record for the western Atlantic. The specimens were compared with types and western Atlantic materials deposited in various major museums. A diagnosis and illustrations are presented for each of seven species found to be poorly or insufficiently known. New material and information is reported for two additional species that occur in Brazil but not found in the recent deep-water collections: Clibanarius symmetricus (Randall, 1840) and Mixtopagurus paradoxus A. Milne-Edwards, 1880. Remarkable and unique color photographs of live or fresh specimens of Allodardanus bredini Haig & Provenzano, 1965, Bathynarius anomalus (A. Milne-Edwards & Bouvier, 1893), Pylopagurus discoidalis (A. Milne-Edwards, 1880), Paguristes spinipes A. Milne-Edwards, 1880, Parapagurus pilosimanus Smith, 1876, and P. alaminos Lemaitre, 1986, are presented. A review of published records and museum collections of the terrestrial Coenobita clypeatus (Fabricius, 1787), has shown that the southern range limit of this species does not extend beyond the southern Caribbean and Trinidad and Tobago, and thus does not occur on the Brazilian coast as previously believed. A distribution map of C. clypeatus is provided based on specimens in the collections of the National Museum of Natural History, Smithsonian Institution. New distribution records in the Gulf of Mexico and southern Caribbean, and morphological information, are included for Pagurus rotundimanus Wass, 1963, a species originally described from the Florida Keys but rarely reported since. Relevant remarks on the taxonomy, morphology, and distribution of all these species are included. The revised list of Paguroidea known from Brazil is updated, and now includes a total of 62 species in the families Pylochelidae (1), Diogenidae (27), Paguridae (28), and Parapaguridae (6). A synopsis of primary taxonomic works on western Atlantic Paguroidea is also presented. C1 [Lemaitre, Rafael] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Tavares, Marcos] Univ Sao Paulo, Museu Zool, BR-04263000 Sao Paulo, SP, Brazil. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM lemaitrr@si.edu; mdst@usp.br RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico or CNpQ [301806/2010-1]; Petroleo Brasileiro S.A. or PETROBRAS [4600224970]; National Geographic Society's Committee for Research and Exploration [9102-12] FX This study was made possibly, in part, by research grants for studies on the systematics of decapod crustaceans provided to MT by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico or CNpQ (Grant #301806/2010-1) and Petroleo Brasileiro S.A. or PETROBRAS (Grant #4600224970); and grants for DROP provided by the Smithsonian Institution's Consortium for Understanding and Sustaining a Biodiverse Planet, and the National Geographic Society's Committee for Research and Exploration (Grant #9102-12). We profusely thank the following individuals and their institutions: B.B. Brown, photographer with the Willemstad Seaquarium in Curacao, for allowing use of his outstanding images; P. Clark and H. Taylor (both NHM), for providing information and the photograph of Broderip's gastropod shells with the Coenobita specimens; D.L. Felder (ULLZ), for sharing photographs and information of specimens form his collections; Joel Braga (MZUSP), for photographs of species of Parapagurus; and J. Harasewych (USNM), for identification of the shells of Melongena melongena. The enthusiasm and cooperation of the DROP team in Curacao who collected specimens on board the Curasub and provided valuable information, are gratefully acknowledged; these include: C. Baldwin and C. Castillo (both USNM), B. B. Brown, and A. "Dutch" Schrier. Valuable specimens and/or information were also supplied by: M. Wicksten (Texas A&M University, College Station Texas); G. Navas and A. Bermudez (both Universidad de Cartagena, Colombia); and F. Mantelatto and M. Negri (both Faculty of Philosophy, Sciences and Letters at Ribeirao Preto, University of Sao Paulo) for specimens and information. This study is Ocean Heritage Foundation/Curacao Sea Aquarium/Substation Curacao contribution #16. NR 186 TC 3 Z9 3 U1 1 U2 19 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 AUG 4 PY 2015 VL 3994 IS 4 BP 451 EP 506 PG 56 WC Zoology SC Zoology GA CO7SD UT WOS:000359361200001 PM 26250287 ER PT J AU Bizau, JM Cubaynes, D Guilbaud, S Al Shorman, MM Gharaibeh, MF Ababneh, IQ Blancard, C McLaughlin, BM AF Bizau, J. M. Cubaynes, D. Guilbaud, S. Al Shorman, M. M. Gharaibeh, M. F. Ababneh, I. Q. Blancard, C. McLaughlin, B. M. TI K-shell photoionization of O+ and O2+ ions: Experiment and theory SO PHYSICAL REVIEW A LA English DT Article ID X-RAY SPECTROSCOPY; PHOTOABSORPTION CROSS-SECTIONS; LOW-LYING STATES; R-MATRIX THEORY; INTERSTELLAR-MEDIUM; OSCILLATOR-STRENGTHS; OXYGEN IONS; RESONANCE PHOTOIONIZATION; ISOELECTRONIC SEQUENCE; ELECTRON-IMPACT AB Absolute cross sections for the single and double K-shell photoionization of carbonlike O2+ and nitrogenlike O+ ions were measured in the 526-620-eV photon energy range by employing the ion-photon merged-beam technique at the SOLEIL synchrotron radiation facility. High-resolution spectroscopy up to E/Lambda E approximate to 5300 was achieved. Rich resonance structures observed in the experimental spectra are analyzed and identified with the aid of R-matrix and multiconfiguration Dirac-Fock (MCDF) methods. For these two atomic oxygen ions of particular astrophysical interest we characterized the strong 1s -> 2p and the weaker 1s -> np (n > 2) resonances observed. A detailed comparison of the energies of the 1s -> 2p resonances in the first members of the oxygen isonuclear sequence measured by synchrotron based experiments and the Chandra and XMM-Newton x-ray satellites is presented. C1 [Bizau, J. M.; Cubaynes, D.; Guilbaud, S.; Al Shorman, M. M.] Univ Paris 11, CNRS UMR 8214, ISMO, F-91405 Orsay, France. [Bizau, J. M.; Cubaynes, D.] Synchrotron SOLEIL LOrme Merisiers, F-91192 Gif Sur Yvette, France. [Gharaibeh, M. F.] Qatar Univ, Dept Math Stat & Phys, Doha, Qatar. [Ababneh, I. Q.] Jordan Univ Sci & Technol, Dept Phys, Irbid 22110, Jordan. [Blancard, C.] CEA DAM DIF, F-91297 Arpajon, France. [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Bizau, JM (reprint author), Univ Paris 11, CNRS UMR 8214, ISMO, Batiment 350, F-91405 Orsay, France. EM jean-marc.bizau@u-psud.fr; b.mclaughlin@qub.ac.uk FU Scientific Research Support Fund, Jordan [Bas/2/02/2010]; SESAME - Lounsbery Foundation; U.S. National Science Foundation; RTRA network Triangle de la Physique; Queen's University Belfast; Office of Science of the U.S. Department of Energy [DE-AC05-00OR22725] FX The authors thank the SOLEIL staff and in particular E. Antonsson of the PLEIADES beam line for helpful assistance during the measurements, and J. Bozek and M. Patanen for their help in the energy calibration of the beam line. M.F.G. acknowledges funding from the Scientific Research Support Fund, Jordan, under Contract No. Bas/2/02/2010. I.Q.A. acknowledges financial support from the SESAME - Lounsbery Foundation for a training fellowship. B.M.M. acknowledges support from the U.S. National Science Foundation through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, the RTRA network Triangle de la Physique, and a visiting research fellowship (VRF) from Queen's University Belfast. We thank E. T. Kennedy for a careful reading of the manuscript and constructive comments. J. C. Raymond and R. K. Smith at the Harvard-Smithsonian Center for Astrophysics are acknowledged for many helpful discussions on the astrophysical applications. The R-matrix computational 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. This research also used resources of the Oak Ridge Leadership Computing Facility at the Oak Ridge National Laboratory, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC05-00OR22725. NR 58 TC 5 Z9 5 U1 5 U2 21 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 AUG 3 PY 2015 VL 92 IS 2 AR 023401 DI 10.1103/PhysRevA.92.023401 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CO1MO UT WOS:000358919600006 ER PT J AU Li, DH Shi, W Munroe, TA Gong, L Kong, XY AF Li, Dong-He Shi, Wei Munroe, Thomas A. Gong, Li Kong, Xiao-Yu TI Concerted Evolution of Duplicate Control Regions in the Mitochondria of Species of the Flatfish Family Bothidae (Teleostei: Pleuronectiformes) SO PLOS ONE LA English DT Article ID MAXIMUM-LIKELIHOOD; DNA-SEQUENCE; GENOME; REPLICATION; SNAKE; REARRANGEMENTS; PLATYSTERNON; MITOGENOME; PHYLOGENY; ORIGINS AB Mitogenomes of flatfishes (Pleuronectiformes) exhibit the greatest diversity of gene rearrangements in teleostean fishes. Duplicate control regions (CRs) have been found in the mito-genomes of two flatfishes, Samariscus latus (Samaridae) and Laeops lanceolata (Bothidae), which is rare in teleosts. It has been reported that duplicate CRs have evolved in a concerted fashion in fishes and other animals, however, whether concerted evo-lution exists in flatfishes remains unknown. In this study, based on five newly sequenced and six previously reported mitogenomes of lefteye flounders in the Bothidae, we explored whether duplicate CRs and concerted evolution exist in these species. Results based on the present study and previous reports show that four out of eleven bothid species examined have duplicate CRs of their mitogenomes. The core regions of the duplicate CRs of mitogenomes in the same species have identical, or nearly identical, sequences when compared to each other. This pattern fits the typical characteristics of concerted evolution. Additionally, phylogenetic and ancestral state reconstruction analysis also provided evidence to support the hypothesis that duplicate CRs evolved concertedly. The core region of concerted evolution is situated at the conserved domains of the CR of the mitogenome from the termination associated sequences (TASs) to the conserved sequence blocks (CSBs). Commonly, this region is con-sidered to regulate mitochondrial replication and transcription. Thus, we hypothesize that the cause of concerted evolution of the duplicate CRs in the mtDNAs of these four bothids may be related to some function of the conserved sequences of the CRs during mitochondrial rep-lication and transcription. We hope our results will provide fresh insight into the molecular mechanisms related to replication and evolution of mitogenomes. C1 [Li, Dong-He; Shi, Wei; Gong, Li; Kong, Xiao-Yu] Chinese Acad Sci, Key Lab Trop Marine Bio resources & Ecol, South China Sea Inst Oceanol, Guangzhou 510301, Guangdong, Peoples R China. [Li, Dong-He; Shi, Wei; Gong, Li; Kong, Xiao-Yu] Chinese Acad Sci, Guangdong Prov Key Lab Appl Marine Biol, South China Sea Inst Oceanol, Guangzhou 510301, Guangdong, Peoples R China. [Li, Dong-He; Shi, Wei; Gong, Li] South China Sea Bioresource Exploitat & Utilizat, Guangzhou 510301, Guangdong, Peoples R China. [Li, Dong-He; Gong, Li] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Munroe, Thomas A.] NOAA, Natl Systemat Lab NMFS, Smithsonian Inst NHB, Washington, DC 20013 USA. RP Shi, W (reprint author), Chinese Acad Sci, Key Lab Trop Marine Bio resources & Ecol, South China Sea Inst Oceanol, Guangzhou 510301, Guangdong, Peoples R China. EM shiwei@scsio.ac.cn; xykong@scsio.ac.cn FU Natural Science Foundation of China [31471979, 41206134, 30870283]; Science and Technology Planning Project of Guangdong Province, China [2014B030301064] FX This work was supported by the Natural Science Foundation of China (grant numbers 31471979, 41206134, 30870283) and Science and Technology Planning Project of Guangdong Province, China (2014B030301064). NR 49 TC 2 Z9 2 U1 2 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 AUG 3 PY 2015 VL 10 IS 8 AR e0134580 DI 10.1371/journal.pone.0134580 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO1UY UT WOS:000358942400029 PM 26237419 ER PT J AU Archambault, S Archer, A Beilicke, M Benbow, W Bird, R Biteau, J Bouvier, A Bugaev, V Cardenzana, JV Cerruti, M Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Errando, M Falcone, A Feng, Q Finley, JP Fleischhack, H Fortin, P Fortson, L Furniss, A Gillanders, GH Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Humensky, TB Johnson, CA Kaaret, P Kar, P Kertzman, M Khassen, Y Kieda, D Krause, M Krennrich, F Kumar, S Lang, MJ Maier, G McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Santander, M Sembroski, GH Shahinyan, K Smith, AW Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Vincent, S Wakely, SP Weinstein, A Welsing, R Wilhelm, A Williams, DA Zitzer, B Hughes, ZD AF Archambault, S. Archer, A. Beilicke, M. Benbow, W. Bird, R. Biteau, J. Bouvier, A. Bugaev, V. Cardenzana, J. V. Cerruti, M. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Errando, M. Falcone, A. Feng, Q. Finley, J. P. Fleischhack, H. Fortin, P. Fortson, L. Furniss, A. Gillanders, G. H. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Humensky, T. B. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krause, M. Krennrich, F. Kumar, S. Lang, M. J. Maier, G. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. 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. Weinstein, A. Welsing, R. Wilhelm, A. Williams, D. A. Zitzer, B. Hughes, Z. D. CA Veritas Collaboration TI VERITAS DETECTION OF gamma-RAY FLARING ACTIVITY FROM THE BL LAC OBJECT 1ES 1727+502 DURING BRIGHT MOONLIGHT OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (1ES 1727+502); galaxies: active; gamma rays: galaxies; radiation mechanisms: non-thermal ID LARGE-AREA TELESCOPE; SELF-COMPTON MODEL; SPECTRAL ENERGY-DISTRIBUTION; LACERTAE OBJECTS; GALACTIC NUCLEI; HOST GALAXIES; SOURCE CATALOG; CRAB-NEBULA; TEV BLAZARS; FERMI ERA AB During moonlit nights, observations with ground-based Cherenkov telescopes at very high energies (VHEs, E > 100 GeV) are constrained since the photomultiplier tubes (PMTs) in the telescope camera are extremely sensitive to the background moonlight. Observations with the VERITAS telescopes in the standard configuration are performed only with a moon illumination less than 35% of full moon. Since 2012, the VERITAS collaboration has implemented a new observing mode under bright moonlight, by either reducing the voltage applied to the PMTs (reduced-high-voltage; RHV configuration), or by utilizing UV-transparent filters. While these operating modes result in lower sensitivity and increased energy thresholds, the extension of the available observing time is useful for monitoring variable sources such as blazars and sources requiring spectral measurements at the highest energies. In this paper we report the detection of gamma-ray flaring activity from the BL Lac object 1ES 1727+502 during RHV observations. This detection represents the first evidence of VHE variability from this blazar. The integral flux is (1.1 +/- 0.2) x 10(-11) cm(-2) s(-1) above 250 GeV, which is about five times higher than the low-flux state. The detection triggered additional VERITAS observations during standard dark-time. Multiwavelength observations with the FLWO 48 '' telescope, and the Swift and Fermi satellites are presented and used to produce the first spectral energy distribution (SED) of this object during gamma-ray flaring activity. The SED is then fitted with a standard synchrotron-self-Compton model, placing constraints on the properties of the emitting region and of the acceleration mechanism at the origin of the relativistic particle population in the jet. C1 [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Beilicke, M.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Biteau, J.; Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.; Hughes, Z. D.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Bouvier, A.; Furniss, A.; Johnson, C. A.; Williams, D. A.; Hughes, Z. D.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Krennrich, F.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Fleischhack, H.; Krause, M.; Maier, G.; de Bhroithe, A. O'Faolain; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Vincent, S.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Connolly, M. P.; Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; 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. [Errando, M.; Mukherjee, R.; Santander, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Humensky, T. B.; Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kar, P.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McArthur, S.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys Sci & Engn, Anderson, IN 46012 USA. [Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [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 Appl Sci, Cork, Ireland. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Archambault, S (reprint author), McGill Univ, Dept Phys, 3600 Univ St, Montreal, PQ H3A 2T8, Canada. EM matteo.cerruti@cfa.harvard.edu; griffins@physics.mcgill.ca RI Nieto, Daniel/J-7250-2015; OI Nieto, Daniel/0000-0003-3343-0755; Pueschel, Elisa/0000-0002-0529-1973 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland (SFI) [10/RFP/AST2748]; STFC in the U.K. FX The authors wish to thank Kari Nilsson for useful discussions about the host-galaxy contribution, as well as the anonymous referee for his/her comments which improved the present work. 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, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the U.K. 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. NR 88 TC 6 Z9 6 U1 0 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 AUG 1 PY 2015 VL 808 IS 2 AR 110 DI 10.1088/0004-637X/808/2/110 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400005 ER PT J AU Buchhave, LA Latham, DW AF Buchhave, Lars A. Latham, David W. TI THE METALLICITIES OF STARS WITH AND WITHOUT TRANSITING PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; surveys; techniques: spectroscopic ID HOST STARS; KEPLER; MASS; SPECTROSCOPY AB Host star metallicities have been used to infer observational constraints on planet formation throughout the history of the exoplanet field. The giant planet metallicity correlation has now been widely accepted, but questions remain as to whether the metallicity correlation extends to the small terrestrial-sized planets. Here, we report metallicities for a sample of 518 stars in the Kepler field that have no detected transiting planets and compare their metallicity distribution to a sample of stars that hosts small planets (R-p < 1.7 R-circle plus). Importantly, both samples have been analyzed in a homogeneous manner using the same set of tools (Stellar Parameters Classification tool). We find the average metallicity of the sample of stars without detected transiting planets to be [m/H](SNTP,dwarf) = -0.02 +/- 0.02 dex and the sample of stars hosting small planets to be [m/H](STP) = -0.02 +/- 0.02 dex. The average metallicities of the two samples are indistinguishable within the uncertainties, and the two-sample Kolmogorov-Smirnov test yields a p-value of 0.68 (0.41 sigma), indicating a failure to reject the null hypothesis that the two samples are drawn from the same parent population. We conclude that the homogeneous analysis of the data presented here supports the hypothesis that stars hosting small planets have a metallicity similar to stars with no known transiting planets in the same area of the sky. C1 [Buchhave, Lars A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Buchhave, LA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Buchhave, Lars A./0000-0003-1605-5666; Latham, David/0000-0001-9911-7388 NR 26 TC 17 Z9 17 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 AUG 1 PY 2015 VL 808 IS 2 AR 187 DI 10.1088/0004-637X/808/2/187 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400083 ER PT J AU Civano, F Hickox, RC Puccetti, S Comastri, A Mullaney, JR Zappacosta, L LaMassa, SM Aird, J Alexander, DM Ballantyne, DR Bauer, FE Brandt, WN Boggs, SE Christensen, FE Craig, WW Del-Moro, A Elvis, M Forster, K Gandhi, P Grefenstette, BW Hailey, CJ Harrison, FA Lansbury, GB Luo, B Madsen, K Saez, C Stern, D Treister, E Urry, MC Wik, DR Zhang, W AF Civano, F. Hickox, R. C. Puccetti, S. Comastri, A. Mullaney, J. R. Zappacosta, L. LaMassa, S. M. Aird, J. Alexander, D. M. Ballantyne, D. R. Bauer, F. E. Brandt, W. N. Boggs, S. E. Christensen, F. E. Craig, W. W. Del-Moro, A. Elvis, M. Forster, K. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Lansbury, G. B. Luo, B. Madsen, K. Saez, C. Stern, D. Treister, E. Urry, M. C. Wik, D. R. Zhang, W. TI THE NuSTAR EXTRAGALACTIC SURVEYS: OVERVIEW AND CATALOG FROM THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: nuclei; X-rays: general ID ACTIVE GALACTIC NUCLEI; X-RAY LUMINOSITY; MEDIUM-SENSITIVITY SURVEY; POINT-SOURCE CATALOG; CHANDRA DEEP SURVEY; COMPTON-THICK AGN; SWIFT-BAT SURVEY; ALL-SKY SURVEY; XMM-NEWTON; HELLAS2XMM SURVEY AB To provide the census of the sources contributing to the X-ray background peak above 10 keV, Nuclear Spectroscopic Telescope Array (NuSTAR) is performing extragalactic surveys using a three-tier "wedding cake" approach. We present the NuSTAR survey of the COSMOS field, the medium sensitivity, and medium area tier, covering 1.7 deg(2) and overlapping with both Chandra and XMM-Newton data. This survey consists of 121 observations for a total exposure of similar to 3 Ms. To fully exploit these data, we developed a new detection strategy, carefully tested through extensive simulations. The survey sensitivity at 20% completeness is 5.9, 2.9, and 6.4 x 10(-14) erg cm(-2) s(-1) in the 3-24, 3-8, and 8-24 keV bands, respectively. By combining detections in 3 bands, we have a sample of 91 NuSTAR sources with 10(42)-10(45.5) erg s(-1) luminosities and redshift z = 0.04-2.5. Thirty-two sources are detected in the 8-24 keV band with fluxes similar to 100 times fainter than sources detected by Swift-BAT. Of the 91 detections, all but 4 are associated with a Chandra and/or XMM-Newton point-like counterpart. One source is associated with an extended lower energy X-ray source. We present the X-ray (hardness ratio and luminosity) and optical-to-X-ray properties. The observed fraction of candidate Compton-thick active galactic nuclei measured from the hardness ratio is between 13%-20%. We discuss the spectral properties of NuSTAR J100259+0220.6 (ID 330) at z = 0.044, with the highest hardness ratio in the entire sample. The measured column density exceeds 10(24) cm(-2), implying the source is Compton-thick. This source was not previously recognized as such without the >10 keV data. C1 [Civano, F.; LaMassa, S. M.; Urry, M. C.] Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Zappacosta, L.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Aird, J.; Alexander, D. M.; Del-Moro, A.; Gandhi, P.; Lansbury, G. B.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Aird, J.] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F. E.; Luo, B.; Saez, C.] Pontificia Univ Catolica Chile, Inst Astrofis, Fac Fis, Santiago 22, Chile. [Bauer, F. E.; Luo, B.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Forster, K.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Gandhi, P.] Univ Southampton, Sch Phys Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wik, D. R.; Zhang, W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Civano, F (reprint author), Yale Ctr Astron & Astrophys, 260 Whitney Ave, New Haven, CT 06520 USA. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835; Comastri, Andrea/0000-0003-3451-9970; Ballantyne, David/0000-0001-8128-6976; Urry, Meg/0000-0002-0745-9792 FU National Aeronautics and Space Administration; NASA [11-ADAP110218, GO3-14150C]; Science and Technology Facilities Council [ST/I001573/1]; NSF [AST 1008067]; NuSTAR grant [44A-1092750]; NASA ADP grant [NNX10AC99G]; V. M. Willaman Endowment; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT [1141218, 1120061]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Center of Excellence in Astrophysics and Associated Technologies; ASI/INAF [I/037/12/0] FX We thank the anonymous referee for interesting comments and A. Goulding and M. Rose for useful discussions. This work 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 acknowledge support from the NASA grants 11-ADAP110218 and GO3-14150C (FC); from the Science and Technology Facilities Council ST/I001573/1 (ADM, DMA); NSF award AST 1008067 (DRB); NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment (WNB, BL); CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB); the Center of Excellence in Astrophysics and Associated Technologies (PFB 06) and by the FONDECYT regular grant 1120061 (ET); financial support under ASI/INAF contract I/037/12/0 (LZ). NR 96 TC 10 Z9 10 U1 0 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 AUG 1 PY 2015 VL 808 IS 2 AR 185 DI 10.1088/0004-637X/808/2/185 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400081 ER PT J AU Dumusque, X Pepe, F Lovis, C Latham, DW AF Dumusque, Xavier Pepe, Francesco Lovis, Christophe Latham, David W. TI CHARACTERIZATION OF A SPURIOUS ONE-YEAR SIGNAL IN HARPS DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: detectors; instrumentation: spectrographs; methods: data analysis; planets and satellites: terrestrial planets; techniques: radial velocities ID EARTH-LIKE PLANETS; SOLAR-LIKE OSCILLATIONS; ALPHA-CENTAURI-B; RADIAL-VELOCITY; MASS PLANET; I.; SEARCH; STARS; SUN AB The HARPS spectrograph is showing an extreme stability, close to the m s(-1) level, over more than 10 years of data. However, the radial velocities of some stars are contaminated by a spurious one-year signal with an amplitude that can be as high as a few m s(-1). This signal is in opposition of phase with the revolution of Earth around the Sun and can be explained by the deformation of spectral lines crossing block stitchings of the CCD when the spectrum of an observed star is alternatively blueshifted and redshifted due to the motion of Earth around the Sun. This annual perturbation can be suppressed by either removing those affected spectral lines from the correlation mask used by the cross-correlation technique to derive precise radial velocities, or by simply fitting a yearly sinusoid to the radial velocity data. This is mandatory if we want to detect long-period low-amplitude signals in the HARPS radial velocities of quiet solar-type stars. C1 [Dumusque, Xavier; Latham, David W.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Pepe, Francesco; Lovis, Christophe] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. RP Dumusque, X (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM xdumusque@cfa.harvard.edu FU NASA from MIT [5710003554] FX We thank the referee for valuable comments and suggestions that improved the first version of the paper. X.D. thanks NASA's Transiting Exoplanet Survey Satellite (TESS) mission for partial support via sub-award 5710003554 from MIT to SAO. We are grateful to all of the technical and scientific collaborators of the HARPS Consortium, ESO Headquarters, and ESO La Silla who have contributed their extraordinary passion and valuable work to the success of the HARPS project. NR 25 TC 8 Z9 8 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 AUG 1 PY 2015 VL 808 IS 2 AR 171 DI 10.1088/0004-637X/808/2/171 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400066 ER PT J AU Favre, C Bergin, EA Neill, JL Crockett, NR Zhang, QZ Lis, DC AF Favre, Cecile Bergin, Edwin A. Neill, Justin L. Crockett, Nathan R. Zhang, Qizhou Lis, Dariusz C. TI THE DISTRIBUTION OF DEUTERATED FORMALDEHYDE WITHIN ORION-KL SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual objects (Orion-KL); ISM: molecules; line: identification ID EXTRAORDINARY SOURCES HEXOS; LIMITED MILLIMETER SURVEY; LINE SURVEY; SUBMILLIMETER ARRAY; HERSCHEL OBSERVATIONS; THERMAL-DESORPTION; ORGANIC-MOLECULES; PROPER MOTIONS; STAR-FORMATION; HOT CORE AB We report the first high angular resolution imaging (3 ''.4 x 3 ''.0) of deuterated formaldehyde (HDCO) toward Orion- KL, carried out with the Submillimeter Array. We find that the spatial distribution of the formaldehyde emission systematically differs from that of methanol: while methanol is found toward the inner part of the region, HDCO is found in colder gas that wraps around the methanol emission on four sides. The HDCO/H2CO ratios are determined to be 0.003- 0.009 within the region, up to an order of magnitude higher than the D/H measured for methanol. These findings strengthen the previously suggested hypothesis that there are differences in the chemical pathways leading to HDCO (via deuterated gas- phase chemistry) and deuterated methanol (through conversion of formaldehyde into methanol on the surface of icy grain mantles). C1 [Favre, Cecile; Bergin, Edwin A.; Neill, Justin L.] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. [Zhang, Qizhou] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lis, Dariusz C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lis, Dariusz C.] Univ Paris 06, Sorbonne Univ, CNRS, LERMA,Observ Paris,PSL Res Univ, F-75014 Paris, France. CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. EM cfavre@umich.edu OI Zhang, Qizhou/0000-0003-2384-6589 FU NASA by JPL/Caltech FX Support for this work was provided by NASA (Herschel OT funding) through an award issued by JPL/Caltech. This paper makes use of SMA data. C.F. thanks Tzu-Cheng Peng for helpful discussions. NR 76 TC 1 Z9 1 U1 0 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 AUG 1 PY 2015 VL 808 IS 2 AR 155 DI 10.1088/0004-637X/808/2/155 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400050 ER PT J AU Jiang, XJ Liu, HYB Zhang, QZ Wang, JZ Zhang, ZY Li, J Gao, Y Gu, QS AF Jiang, Xue-Jian Liu, Hauyu Baobab Zhang, Qizhou Wang, Junzhi Zhang, Zhi-Yu Li, Juan Gao, Yu Gu, Qiusheng TI SMA OBSERVATIONS OF C2H IN HIGH-MASS STAR-FORMING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; molecular processes; stars: early-type; stars: formation; stars: individual (G10.6-0.4, ON1, W33, and AFGL 490) ID SPATIALLY-RESOLVED CHEMISTRY; CARBON-CHAIN MOLECULES; H-II REGIONS; OB CLUSTERS; INFRARED OBSERVATIONS; INTERSTELLAR CLOUDS; PHYSICAL STRUCTURE; DENSITY STRUCTURE; DUST CONTINUUM; HII REGION AB C2H is a representative hydrocarbon that is abundant and ubiquitous in the interstellar medium. To study its chemical properties, we present Submillimeter Array observations of the C2H N = 3-2 and. HC3N J = 30-29 transitions. and the 1.1 mm continuum emission toward four OB cluster-forming regions, AFGL 490, ON 1, W33 Main, and G10.6-0.4, which cover a bolometric luminosity range of similar to 10(3)-10(6) L-circle dot. We found that on large scales, the C2H emission traces the dense molecular envelope. However, for all observed sources, the peaks of C2H emission are offset by several times. 104 AU from the peaks of 1.1 mm continuum emission, where the most luminous stars are located. By comparing the distribution and profiles of C2H hyperfine lines and the 1.1 mm continuum emission, we find that the C2H column density (and abundance) around the 1.1 mm continuum peaks is lower than those in the ambient gas envelope. Chemical models suggest that C2H might be transformed to other species owing to increased temperature and density;. thus, its reduced abundance could be the signpost of the heated molecular gas in the similar to 10(4) AU vicinity around the embedded high-mass stars. Our results support such theoretical prediction for centrally embedded similar to 10(3)-10(6) L-circle dot OB star-forming cores, while future higher-resolution observations are required to examine the C2H transformation around the localized sites of high-mass star formation. C1 [Jiang, Xue-Jian; Gao, Yu] Chinese Acad Sci, Purple Mt Observ, 2 W Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Gao, Yu] Chinese Acad Sci, Key Lab Radio Astron, 2 W Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jiang, Xue-Jian; Gu, Qiusheng] Nanjing Univ, Minist Educ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. [Jiang, Xue-Jian; Gu, Qiusheng] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China. [Liu, Hauyu Baobab] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Wang, Junzhi; Li, Juan] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Zhang, Zhi-Yu] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Zhang, Zhi-Yu] ESO, D-85748 Munich, Germany. RP Jiang, XJ (reprint author), Chinese Acad Sci, Purple Mt Observ, 2 W Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China. EM xjjiang@pmo.ac.cn OI Zhang, Qizhou/0000-0003-2384-6589; Liu, Hauyu Baobab/0000-0003-2300-2626; Zhang, Zhiyu/0000-0002-7299-2876 FU National Natural Science Foundation of China [11390373, 11273015, 11133001, 11328301]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; National Basic Research Program (973 program) [2013CB834905]; Specialized Research Fund for the Doctoral Program of Higher Education [20100091110009]; European Research Council (ERC) FX We acknowledge the SMA staff for their help during and after the observations. X.J. thanks Keping Qiu for informative discussions on the source ON 1. This work is supported under the National Natural Science Foundation of China (grants 11390373, 11273015, 11133001, and 11328301), the Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (grant XDB09000000), the National Basic Research Program (973 program No. 2013CB834905), and Specialized Research Fund for the Doctoral Program of Higher Education (20100091110009). Z.-Y.Z. acknowledges support from the European Research Council (ERC) in the form of Advanced Grant. COSMICISM. This research made use of Matplotlib (Hunter 2007) and APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. NR 74 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 AUG 1 PY 2015 VL 808 IS 2 AR 114 DI 10.1088/0004-637X/808/2/114 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400009 ER PT J AU Jones, DE Kashyap, VL van Dyk, DA AF Jones, David E. Kashyap, Vinay L. van Dyk, David A. TI DISENTANGLING OVERLAPPING ASTRONOMICAL SOURCES USING SPATIAL AND SPECTRAL INFORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; techniques: image processing; X-rays: stars ID BAYESIAN-ANALYSIS; UNCERTAINTIES; COMPUTATION; CALIBRATION; MIXTURES; COUNTS; MODELS; FIELDS; LIMITS AB We present a powerful new algorithm that combines both spatial information (event locations and the point-spread function) and spectral information (photon energies) to separate photons from overlapping sources. We use Bayesian statistical methods to simultaneously infer the number of overlapping sources, to probabilistically separate the photons among the sources, and to fit the parameters describing the individual sources. Using the Bayesian joint posterior distribution, we are able to coherently quantify the uncertainties associated with all these parameters. The advantages of combining spatial and spectral information are demonstrated through a simulation study. The utility of the approach is then illustrated by analysis of observations of FK Aqr and FL Aqr with the XMM-Newton Observatory and the central region of the Orion Nebula Cluster with the Chandra X-ray Observatory. C1 [Jones, David E.] Harvard Univ, Dept Stat, 1 Oxford St, Cambridge, MA 02138 USA. [Kashyap, Vinay L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dyk, David A.] Univ London Imperial Coll Sci Technol & Med, Dept Math, Stat Sect, London SW7 2AZ, England. RP Jones, DE (reprint author), Harvard Univ, Dept Stat, 1 Oxford St, Cambridge, MA 02138 USA. EM djones@fas.harvard.edu FU Smithsonian Competitive Grants Program for Science Fund [40488100HH0043]; CHASC International Astrostatistics Center; NSF [DMS 1208791, DMS 1209232]; Harvard Statistics Department; NASA [NAS8-03060]; Chandra grant [AR0-11001X]; Wolfson Research Merit Award by British Royal Society; Marie-Curie Career Integration Grant by European Commission FX This work was supported by the Smithsonian Competitive Grants Program for Science Fund 40488100HH0043 and was conducted under the auspices of the CHASC International Astrostatistics Center. CHASC is supported by NSF grants DMS 1208791 and DMS 1209232. D.E.J. acknowledges support from the Harvard Statistics Department, V.L.K. from a NASA contract to the Chandra X-Ray Center NAS8-03060 and from Chandra grant AR0-11001X, and D.v.D. from a Wolfson Research Merit Award provided by the British Royal Society and from a Marie-Curie Career Integration Grant provided by the European Commission. In addition, we thank CHASC members for many helpful discussions, especially Xiao-Li Meng, Andreas Zezas, Aneta Siemiginowska, Lazhi Wang, and Alex Blocker. 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 AUG 1 PY 2015 VL 808 IS 2 AR 137 DI 10.1088/0004-637X/808/2/137 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400032 ER PT J AU Mullaney, JR Del-Moro, A Aird, J Alexander, DM Civano, FM Hickox, RC Lansbury, GB Ajello, M Assef, R Ballantyne, DR Balokovic, M Bauer, FE Brandt, WN Boggs, SE Brightman, M Christensen, FE Comastri, A Craig, WW Elvis, M Forster, K Gandhi, P Grefenstette, BW Hailey, CJ Harrison, FA Koss, M LaMassa, SM Luo, B Madsen, KK Puccetti, S Saez, C Stern, D Treister, E Urry, CM Wik, DR Zappacosta, L Zhang, W AF Mullaney, J. R. Del-Moro, A. Aird, J. Alexander, D. M. Civano, F. M. Hickox, R. C. Lansbury, G. B. Ajello, M. Assef, R. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Brandt, W. N. Boggs, S. E. Brightman, M. Christensen, F. E. Comastri, A. Craig, W. W. Elvis, M. Forster, K. Gandhi, P. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Koss, M. LaMassa, S. M. Luo, B. Madsen, K. K. Puccetti, S. Saez, C. Stern, D. Treister, E. Urry, C. M. Wik, D. R. Zappacosta, L. Zhang, W. TI THE NuSTAR EXTRAGALACTIC SURVEYS: INITIAL RESULTS AND CATALOG FROM THE EXTENDED CHANDRA DEEP FIELD SOUTH SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; galaxies: active; galaxies: evolution; X-rays: galaxies; X-rays: general ID ACTIVE GALACTIC NUCLEI; POINT-SOURCE CATALOG; HARD X-RAYS; MS SOURCE CATALOGS; SWIFT-BAT SURVEY; NUMBER COUNTS; BACKGROUND SPECTRUM; LUMINOSITY FUNCTION; SPACE DENSITY; BLACK-HOLES AB We present the initial results and the source catalog from the Nuclear Spectroscopic Telescope Array (NuSTAR) survey of the Extended Chandra Deep Field South (hereafter, ECDFS)-currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full approximate to 30' x 30' area of this field to a maximum depth of approximate to 360 ks (approximate to 220 ks when corrected for vignetting at 3-24 keV), reaching sensitivity limits of approximate to 1.3 x 10(-14) erg s(-1) cm(-2) (3-8 keV), approximate to 3.4 x 10(-14) erg s(-1) cm(-2) (8-24 keV), and approximate to 3.0 x 10(-14) erg s(-1) cm(-2) (3-24 keV). A total of 54 sources are detected over the full field, although five of these are found to lie below our significance threshold once contaminating flux from neighboring (i.e., blended) sources is taken into account. Of the remaining 49 that are significant, 19 are detected in the 8-24 keV band. The 8-24 to 3-8 keV band ratios of the 12 sources that are detected in both bands span the range 0.39-1.7, corresponding to a photon index range of Gamma approximate to 0.5-2.3, with a median photon index of (Gamma) over bar = 1.70 +/- 0.52. The redshifts of the 49 sources in our main sample span the range z = 0.21-2.7, and their rest-frame 10-40 keV luminosities (derived from the observed 8-24 keV fluxes) span the range L10-40 keV (0.7-300) 10 erg s(-1), sampling below the "knee" of the X-ray luminosity function out to z similar to 0.8-1. Finally, we identify one NuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclear activity at infrared wavelengths and thus may represent a genuine, new X-ray source detected by NuSTAR in the ECDFS. C1 [Mullaney, J. R.; Del-Moro, A.; Aird, J.; Alexander, D. M.; Lansbury, G. B.; Gandhi, P.] Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. [Mullaney, J. R.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Aird, J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Civano, F. M.; LaMassa, S. M.; Urry, C. M.] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Civano, F. M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Civano, F. M.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Ajello, M.; Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Assef, R.] Univ Diego Portales, Nucleo Astron, Fac Ingn, Santiago, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Brightman, M.; Forster, K.; Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gandhi, P.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, M.] Swiss Fed Inst Technol, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.; Zappacosta, L.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Rome, Italy. [Saez, C.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wik, D. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Wik, D. R.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Zhang, W.] West Virginia Wesleyan Coll, Phys & Engn Dept, Buckhannon, WV 26201 USA. RP Mullaney, JR (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, South Rd, Durham DH1 3LE, England. RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Puccetti, Simonetta/0000-0002-2734-7835; Koss, Michael/0000-0002-7998-9581; Comastri, Andrea/0000-0003-3451-9970; Ballantyne, David/0000-0001-8128-6976; Urry, Meg/0000-0002-0745-9792; Lansbury, George/0000-0002-5328-9827 FU National Aeronautics and Space Administration; Science and Technology Facilities Council [ST/I001573/1]; Institute of Advanced Study, Durham University; ERC; NASA [11-ADAP11-0218, GO3-14150C]; NSF [AST 1008067]; NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; V. M. Willaman Endowment; CONICYT-Chile [Basal-CATA PFB-06/2007]; FONDECYT [1141218, 1120061]; "EMBIGGEN" Anillo [ACT1101]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; ASI/INAF [I/037/12/0 011/13]; NASA Headquarters under the NASA Earth and Space Science Fellowship Program [NNX14AQ07H] FX We thank the anonymous referee for their careful reading of the manuscript and comments that improved the clarity of the text. This work 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). A.D.M. and D.M.A. gratefully acknowledge financial support from the Science and Technology Facilities Council (ST/I001573/1). J.A. acknowledges support from a COFUND Junior Research Fellowship from the Institute of Advanced Study, Durham University, and ERC Advanced Grant FEEDBACK at the University of Cambridge. F.M.C. acknowledges support from NASA grants 11-ADAP11-0218 and GO3-14150C. D.R.B. is supported in part by NSF award AST 1008067. W.N.B. and B.L. thank NuSTAR grant 44A-1092750, NASA ADP grant NNX10AC99G, and the V. M. Willaman Endowment. We acknowledge support from CONICYT-Chile grants Basal-CATA PFB-06/2007 (FEB), FONDECYT 1141218 (FEB) and 1120061 (ET), and "EMBIGGEN" Anillo ACT1101 (FEB, ET); and the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (FEB). Support for the work of E.T. was also provided by the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). A.C., S.P., and L.Z. acknowledge support from the ASI/INAF grant I/037/12/0 011/13. A.C. acknowledges the Caltech Kingsley visitor program. M.B. acknowledges support from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. NR 79 TC 7 Z9 7 U1 1 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 AUG 1 PY 2015 VL 808 IS 2 AR 184 DI 10.1088/0004-637X/808/2/184 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400080 ER PT J AU Simon, JB Hughes, AM Flaherty, KM Bai, XN Armitage, PJ AF Simon, Jacob B. Hughes, A. Meredith Flaherty, Kevin M. Bai, Xue-Ning Armitage, Philip J. TI SIGNATURES OF MRI-DRIVEN TURBULENCE IN PROTOPLANETARY DISKS: PREDICTIONS FOR ALMA OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; line: profiles; magnetohydrodynamics (MHD); protoplanetary disks; turbulence ID ANGULAR-MOMENTUM TRANSPORT; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; VERTICAL MAGNETIC-FIELD; UNSPLIT GODUNOV METHOD; T TAURI DISKS; ACCRETION DISKS; MAGNETOROTATIONAL-INSTABILITY; CONSTRAINED TRANSPORT; OUTER REGIONS; HD 163296 AB Spatially resolved observations of molecular line emission have the potential to yield unique constraints on the nature of turbulence within protoplanetary disks. Using a combination of local non-ideal magnetohydrodynamics (MHD) simulations and radiative transfer calculations, tailored to properties of the disk around HD 163296, we assess the ability of ALMA to detect turbulence driven by the magnetorotational instability (MRI). Our local simulations show that the MRI produces small-scale turbulent velocity fluctuations that increase in strength with height above the mid-plane. For a set of simulations at different disk radii, we fit a Maxwell-Boltzmann distribution to the turbulent velocity and construct a turbulent broadening parameter as a function of radius and height. We input this broadening into radiative transfer calculations to quantify observational signatures of MRI-driven disk turbulence. We find that the ratio of the peak line flux to the flux at line center is a robust diagnostic of turbulence that is only mildly degenerate with systematic uncertainties in disk temperature. For the CO(3-2) line, which we expect to probe the most magnetically active slice of the disk column, variations in the predicted peak-to-trough ratio between our most and least turbulent models span a range of approximately 15%. Additional independent constraints can be derived from the morphology of spatially resolved line profiles, and we estimate the resolution required to detect turbulence on different spatial scales. We discuss the role of lower optical depth molecular tracers, which trace regions closer to the disk mid-plane where velocities in MRI-driven models are systematically lower. C1 [Simon, Jacob B.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. [Simon, Jacob B.; Armitage, Philip J.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Simon, Jacob B.; Armitage, Philip J.] NIST, Boulder, CO 80309 USA. [Hughes, A. Meredith; Flaherty, Kevin M.] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Bai, Xue-Ning] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Armitage, Philip J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Simon, JB (reprint author), Southwest Res Inst, Dept Space Studies, Boulder, CO 80302 USA. EM jbsimon.astro@gmail.com FU NASA [NNX13AI58G, NNX13AI32G, NAS 5-26555, NAS5-26555]; NSF [AST 1313021]; Space Telescope Science Institute [HST-AR-12814]; California Institute of Technology (Caltech); Jet Propulsion Laboratory (JPL) - NASA; NASA from the Space Telescope Science Institute [HST-HF-51301.01-A]; XSEDE [TG-AST120062, TG-AST140001] FX We thank Daniel R. Wik, Matt Kunz, Steve Balbus, Jeremy Goodman, and Richard Nelson for useful discussions and suggestions regarding this work. We also thank the referee, whose suggestions greatly enhanced the quality of this work. We acknowledge support from NASA through grants NNX13AI58G (P.J.A.) and NNX13AI32G (A.M.H., K.M.F.), from the NSF through grant AST 1313021 (P.J.A.), and from grant HST-AR-12814 (P.J.A.) awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contact NAS 5-26555. J.B.S.'s support was provided in part under contract with the California Institute of Technology (Caltech) and the Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. X.N.B. acknowledges support for program number HST-HF-51301.01-A provided by NASA through a Hubble Fellowship grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. This research was supported by an allocation of advanced computing resources provided by the National Science Foundation. The computations were performed on Kraken at the National Institute for Computational Sciences and Maverick at the Texas Advanced Computing Center through XSEDE grant TG-AST120062 and on Stampede at the Texas Advanced Computing Center through XSEDE grant TG-AST140001. NR 86 TC 8 Z9 8 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 AUG 1 PY 2015 VL 808 IS 2 AR 180 DI 10.1088/0004-637X/808/2/180 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400076 ER PT J AU Strader, J Dupree, AK Smith, GH AF Strader, Jay Dupree, A. K. Smith, Graeme H. TI THE 10830 angstrom HELIUM LINE AMONG EVOLVED STARS IN THE GLOBULAR CLUSTER M4 SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: individual (M4); stars: chromospheres ID RED GIANT STARS; MULTIPLE STELLAR POPULATIONS; OMEGA-CENTAURI; MAIN-SEQUENCE; CHROMOSPHERIC ACTIVITY; ABUNDANCE VARIATIONS; MASS OUTFLOW; ATMOSPHERES; PHOTOMETRY; METALLICITIES AB Helium is a pivotal element in understanding the multiple main sequences and extended horizontal branches observed in some globular clusters. Here we present a spectroscopic study of helium in the nearby globular cluster Messier 4 (M4). We have obtained spectra of the chromospheric He I 10830 angstrom line in 16 red horizontal branch (RHB), red giant branch, and asymptotic giant branch stars. Clear He I absorption or emission is present in most of the stars. Effective temperature is the principal parameter that correlates with 10830 angstrom line strength. Stars with T-eff < 4450 K do not exhibit the helium line. RHB stars, which are the hottest stars in our sample, all have strong He I line absorption. A number of these stars show very broad 10830 angstrom lines with shortward extensions indicating outflows as high as 80-100 km s(-1) and the possibility of mass loss. We have also derived [Na/Fe] and [Al/Fe] abundances to see whether these standard tracers of "second generation" cluster stars are correlated with He I line strength. Unlike the case for our previous study of omega Cen, no clear correlation is observed. This may be because the sample does not cover the full range of abundance variations found in M4, or simply because the physical conditions in the chromosphere, rather than the helium abundance, primarily determine the He I 10830 angstrom line strength. A larger sample of high-quality He I spectra of both "first" and "second" generation red giants within a narrow range of T-eff and luminosity is needed to test for the subtle spectroscopic variations in He I expected in M4. C1 [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, Graeme H.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Strader, J (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM strader@pa.msu.edu; adupree@cfa.harvard.edu; graeme@ucolick.org FU National Aeronautics and Space Administration; National Science Foundation FX We thank an anonymous referee for comments that improved the paper. We thank Ben Hendricks for generously providing us with photometry and his differential reddening map of the field of M4. We also thank Christian Johnson for facilitating the Python reduction of a MIKE spectrum. This publication makes use of data products from 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 paper is partially nased on observations obtained 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), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 45 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 AUG 1 PY 2015 VL 808 IS 2 AR 124 DI 10.1088/0004-637X/808/2/124 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400019 ER PT J AU Tamura, Y Kawabe, R Shimajiri, Y Tsukagoshi, T Nakajima, Y Oasa, Y Wilner, DJ Chandler, CJ Saigo, K Tomida, K Yun, MS Taniguchi, A Kohno, K Hatsukade, B Aretxaga, I Austermann, JE Dickman, R Ezawa, H Goss, WM Hayashi, M Hughes, DH Hiramatsu, M Inutsuka, S Ogasawara, R Ohashi, N Oshima, T Scott, KS Wilson, GW AF Tamura, Y. Kawabe, R. Shimajiri, Y. Tsukagoshi, T. Nakajima, Y. Oasa, Y. Wilner, D. J. Chandler, C. J. Saigo, K. Tomida, K. Yun, M. S. Taniguchi, A. Kohno, K. Hatsukade, B. Aretxaga, I. Austermann, J. E. Dickman, R. Ezawa, H. Goss, W. M. Hayashi, M. Hughes, D. H. Hiramatsu, M. Inutsuka, S. Ogasawara, R. Ohashi, N. Oshima, T. Scott, K. S. Wilson, G. W. TI EXTREMELY BRIGHT SUBMILLIMETER GALAXIES BEYOND THE LUPUS-I STAR-FORMING REGION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst; ISM: individual objects (Lupus-I Molecular Cloud); submillimeter: galaxies ID 1ST HYDROSTATIC CORE; DEEP FIELD SOUTH; RADIATION HYDRODYNAMIC MODEL; STRONGLY LENSED GALAXIES; CLERK MAXWELL TELESCOPE; ALL-SKY SURVEY; GOODS-S FIELD; NUMBER COUNTS; INTERSTELLAR-MEDIUM; SOURCE CATALOG AB We report detections of two candidate distant submillimeter galaxies (SMGs), MM J154506.4-344318 and MM J154132.7-350320, which are discovered in the AzTEC/ASTE 1.1 mm survey toward the Lupus-I star-forming region. The two objects have 1.1 mm flux densities of 43.9 and 27.1 mJy, and have Herschel/SPIRE counterparts as well. The Submillimeter Array counterpart to the former SMG is identified at 890 mu m and 1.3 mm. Photometric redshift estimates using all available data from the mid-infrared to the radio suggest that the redshifts of the two SMGs are z(photo) similar or equal to 4-5 and 3, respectively. Near-infrared objects are found very close to the SMGs and they are consistent with low-z ellipticals, suggesting that the high apparent luminosities can be attributed to gravitational magnification. The cumulative number counts at S-1.1mm >= 25 mJy, combined with the other two 1.1 mm brightest sources, are 0.70(-0.34)(+0.56) deg(-2), which is consistent with a model prediction that accounts for flux magnification due to strong gravitational lensing. Unexpectedly, a z > 3 SMG and a Galactic dense starless core (e.g., a first hydrostatic core) could be similar in the mid-infrared to millimeter spectral energy distributions and spatial structures at least at greater than or similar to 1 ''. This indicates that it is necessary to distinguish the two possibilities by means of broadband photometry from the optical to centimeter and spectroscopy to determine the redshift, when a compact object is identified toward Galactic star-forming regions. C1 [Tamura, Y.; Kohno, K.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Kawabe, R.; Hayashi, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Kawabe, R.] Grad Univ Adv Studies SOKENDAI, Sch Sci, Dept Astron, Mitaka, Tokyo 1818588, Japan. [Kawabe, R.] Joint ALMA Observ, Santiago 7630355, Chile. [Shimajiri, Y.] Univ Paris Diderot, Lab AIM, CEA DSM CNRS, IRFU Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Shimajiri, Y.; Oshima, T.] Natl Astron Observ Japan, Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan. [Tsukagoshi, T.] Ibaraki Univ, Inst Astrophys & Planetary Sci, Mito, Ibaraki 3108512, Japan. [Nakajima, Y.] Hitotsubashi Univ, Tokyo 1868601, Japan. [Oasa, Y.] Saitama Univ, Fac Educ, Saitama 3888570, Japan. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandler, C. J.; Dickman, R.; Goss, W. M.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Saigo, K.; Hatsukade, B.; Ezawa, H.; Hiramatsu, M.; Ogasawara, R.] Natl Astron Observ Japan, Chile Observ, Mitaka, Tokyo 1818588, Japan. [Tomida, K.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Tomida, K.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Yun, M. S.; Wilson, G. W.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kohno, K.] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Aretxaga, I.] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Austermann, J. E.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Hayashi, M.] Grad Univ Adv Studies SOKENDAI, Sch Math & Phys Sci, Kanagawa 2400193, Japan. [Inutsuka, S.] Nagoya Univ, Dept Phys, Nagoya, Aichi 4648602, Japan. [Ohashi, N.] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Scott, K. S.] Natl Radio Astron Observ, North Amer ALMA Sci Ctr, Charlottesville, VA 22903 USA. RP Tamura, Y (reprint author), Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. EM ytamura@ioa.s.u-tokyo.ac.jp OI Tomida, Kengo/0000-0001-8105-8113 FU KAKENHI [25103503]; JSPS [09J05537, 09J00159]; Commonwealth of Australia; Smithsonian Institution; Academia Sinica; NASA; National Aeronautics and Space Administration; National Science Foundation FX We acknowledge the anonymous referee for many useful suggetions. We are grateful to the ASTE team for making the observations possible. We thank M. Bethermin and I. Shimizu for making the model number counts available. The study is partially supported by KAKENHI (No. 25103503). Y.S. and K.T. are supported by the JSPS Research Fellowship for Young Scientists (Nos. 09J05537 and 09J00159, respectively). This work is based on observations and archival data made with the following telescopes and facilities. The ASTE telescope is operated by National Astronomical Observatory of Japan. The Australia Telescope Compact Array is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. NRAO is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. The 45 m radio telescope and the Nobeyama Millimeter Array are operated by Nobeyama Radio Observatory, a branch of National Astronomical Observatory of Japan. 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 Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Subaru Telescope is operated by National Astronomical Observatory of Japan. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K. 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 the National Aeronautics and Space Administration and the National Science Foundation. NR 118 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 AUG 1 PY 2015 VL 808 IS 2 AR 121 DI 10.1088/0004-637X/808/2/121 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400016 ER PT J AU Tripathi, A Kratter, KM Murray-Clay, RA Krumholz, MR AF Tripathi, Anjali Kratter, Kaitlin M. Murray-Clay, Ruth A. Krumholz, Mark R. TI SIMULATED PHOTOEVAPORATIVE MASS LOSS FROM HOT JUPITERS IN 3D (vol 808, 173, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Tripathi, Anjali; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kratter, Kaitlin M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Kratter, Kaitlin M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murray-Clay, Ruth A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Tripathi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM atripathi@cfa.harvard.edu NR 1 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 AUG 1 PY 2015 VL 808 IS 2 AR 159 DI 10.1088/0004-637X/811/2/159 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400069 ER PT J AU Tripathi, A Kratter, KM Murray-Clay, RA Krumholz, MR AF Tripathi, Anjali Kratter, Kaitlin M. Murray-Clay, Ruth A. Krumholz, Mark R. TI SIMULATED PHOTOEVAPORATIVE MASS LOSS FROM HOT JUPITERS IN 3D SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; planet-star interactions; planets and satellites: atmospheres; planets and satellites: gaseous planets ID EXTRASOLAR PLANET HD209458B; HD 189733B; X-RAY; TRANSIT OBSERVATIONS; ESCAPING ATMOSPHERE; GIANT PLANETS; HII-REGIONS; LYMAN-ALPHA; BOW SHOCKS; HYDROGEN AB Ionizing stellar photons heat the upper regions of planetary atmospheres, driving atmospheric mass loss. Gas escaping from several hot, hydrogen-rich planets has been detected using UV and X-ray transmission spectroscopy. Because these planets are tidally locked, and thus asymmetrically irradiated, escaping gas is unlikely to be spherically symmetric. In this paper, we focus on the effects of asymmetric heating on local outflow structure. We use the Athena code for hydrodynamics to produce 3D simulations of hot Jupiter mass loss that jointly model wind launching and stellar heating via photoionization. Our fiducial planet is an inflated, hot Jupiter with radius R-p = 2.14R(Jup) and mass M-p = 0.53M(Jup). We irradiate the initially neutral, atomic hydrogen atmosphere with 13.6 eV photons and compute the outflow's ionization structure. There are clear asymmetries in the atmospheric outflow, including a neutral shadow on the planet's nightside. Given an incident ionizing UV flux comparable to that of the Sun, we find a steady-state mass loss rate of similar to 2 x 10(10) g s(-1). The total mass loss rate and the outflow substructure along the substellar ray show good agreement with earlier 1D models, for two different fluxes. Our 3D data cube can be used to generate the outflow's extinction spectrum during transit. As a proof of concept, we find absorption of stellar Lya at Doppler-shifted velocities of up to +/- 50 km s(-1). Our work provides a starting point for further 3D models that can be used to predict observable signatures of hot Jupiter mass loss. C1 [Tripathi, Anjali; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. [Kratter, Kaitlin M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Kratter, Kaitlin M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murray-Clay, Ruth A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Krumholz, Mark R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Tripathi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM atripathi@cfa.harvard.edu OI Krumholz, Mark/0000-0003-3893-854X FU National Science Foundation [DGE-1144152]; NASA - Space Telescope Science Institute [HF-51306.01]; NASA [NAS 5-26555]; NSF [AST-1411536, AST-0955300] FX We thank Xuening Bai, Jim Stone, and James Owen for helpful discussions. We are grateful to the referee for helpful comments that improved the paper. A.T. was supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1144152. K.M.K. was supported in part by NASA through Hubble Fellowship grant no. HF-51306.01 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. R.A.M. acknowledges support from NSF grant AST-1411536. M.R.K. acknowledges support from NSF grant AST-0955300. The computations in this paper were run on the Smithsonian Institution High Performance Cluster (SI/HPC) and the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 61 TC 9 Z9 9 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 AUG 1 PY 2015 VL 808 IS 2 AR 173 DI 10.1088/0004-637X/808/2/173 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400068 ER PT J AU Williams, PKG Berger, E AF Williams, P. K. G. Berger, E. TI THE ROTATION PERIOD AND MAGNETIC FIELD OF THE T DWARF 2MASSI J1047539+212423 MEASURED FROM PERIODIC RADIO BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; radio continuum: stars; stars: individual (2MASSI J1047539+212423) ID SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ANGULAR-MOMENTUM EVOLUTION; ELECTRON-CYCLOTRON MASER; MAIN-SEQUENCE STARS; ALL-SKY SURVEY; BROWN DWARFS; X-RAY; ULTRACOOL DWARFS; BRIGHTNESS VARIATIONS; EMISSION AB Periodic radio bursts from very low mass stars and brown dwarfs simultaneously probe their magnetic and rotational properties. The brown dwarf 2MASSI J1047539+212423 (2M 1047+21) is currently the only T dwarf (T6.5) detected at radio wavelengths. Previous observations of this source with the Arecibo observatory revealed intermittent, 100%-polarized radio pulses similar to those detected from other brown dwarfs, but were unable to constrain a pulse periodicity; previous Very Large Array (VLA) observations detected quiescent emission a factor of similar to 100 times fainter than the Arecibo pulses but no additional events. Here we present 14 hr of VLA observations of this object that reveal a series of pulses at similar to 6 GHz with highly variable profiles, showing that the pulsing behavior evolves on time scales that are both long and short compared to the rotation period. We measure a periodicity of similar to 1.77 hr and identify it with the rotation period. This is just the sixth rotation period measurement in a late T dwarf, and the first obtained in the radio. We detect a pulse at 10 GHz as well, suggesting that the magnetic field strength of 2M 1047+21 reaches at least 3.6 kG. Although this object is the coolest and most rapidly rotating radio-detected brown dwarf to date, its properties appear continuous with those of other such objects, suggesting that the generation of strong magnetic fields and radio emission may continue to even cooler objects. Further studies of this kind will help to clarify the relationships between mass, age, rotation, and magnetic activity at and beyond the end of the main sequence, where both theories and observational data are currently scarce. C1 [Williams, P. K. G.; Berger, E.] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RP Williams, PKG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pwilliams@cfa.harvard.edu OI Williams, Peter/0000-0003-3734-3587 FU National Science Foundation [AST-1008361] FX We thank the referee, Alex Wolszczan, for an insightful report that improved the paper. We acknowledge support for this work from the National Science Foundation through Grant AST-1008361. The VLA is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; NASA's Astrophysics Data System; and Astropy, a community-developed core Python package for astronomy (Astropy Collaboration et al. 2013). NR 60 TC 10 Z9 10 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 AUG 1 PY 2015 VL 808 IS 2 AR 189 DI 10.1088/0004-637X/808/2/189 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA DF0BA UT WOS:000371002400085 ER PT J AU Chase, JM Powell, KI Knight, TM AF Chase, Jonathan M. Powell, Kristin I. Knight, Tiffany M. TI 'Bigger data' on scale-dependent effects of invasive species on biodiversity cannot overcome confounded analyses: a comment on Stohlgren & Rejmanek (2014) SO BIOLOGY LETTERS LA English DT Letter ID AREA RELATIONSHIPS; DIVERSITY; PLANTS AB A recent study by Stohlgren & Rejmanek (SR: Stohlgren TJ, Rejmanek M. 2014 Biol. Lett. 10. (doi:10.1098/rsb1.2013.0939)) purported to test the generality of a recent finding of scale-dependent effects of invasive plants on native diversity; dominant invasive plants decreased the intercept and increased the slope of the species area relationship. SR (2014) find little correlation between invasive species cover and the slopes and intercepts of SARs across a diversity of sites. We show that the analyses of SR (2014) are inappropriate because of confounding causality. C1 [Chase, Jonathan M.; Knight, Tiffany M.] German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany. [Powell, Kristin I.] Smithsonian Trop Res Inst, Forest Global Earth Observ, Ctr Trop Forest Sci, Washington, DC 20560 USA. [Knight, Tiffany M.] Washington Univ, Dept Biol, St Louis, MO 63130 USA. RP Chase, JM (reprint author), German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany. EM jonathan.chase@idiv.de NR 10 TC 1 Z9 1 U1 4 U2 15 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD AUG 1 PY 2015 VL 11 IS 8 AR 20150103 DI 10.1098/rsbl.2015.0103 PG 3 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CT4SR UT WOS:000362798100005 ER PT J AU Marra, PP Cohen, EB Loss, SR Rutter, JE Tonra, CM AF Marra, Peter P. Cohen, Emily B. Loss, Scott R. Rutter, Jordan E. Tonra, Christopher M. TI A call for full annual cycle research in animal ecology SO BIOLOGY LETTERS LA English DT Article DE annual cycle; seasonal interaction; research bias ID CARRY-OVER; MIGRATORY BIRDS; CLIMATE-CHANGE; MORTALITY; TRACKING AB For vertebrates, annual cycles are organized into a series of breeding and non-breeding periods that vary in duration and location but are inextricably linked biologically. Here, we show that our understanding of the fundamental ecology of four vertebrate classes has been limited by a severe breeding season research bias and that studies of individual and population-level responses to natural and anthropogenic change would benefit from a full annual cycle perspective. Recent emergence of new analytical and technological tools for studying individual and population-level animal movement could help reverse this bias. To improve understanding of species biology and reverse the population declines of many vertebrate species, a concerted effort to move beyond single season research is vital. C1 [Marra, Peter P.; Cohen, Emily B.; Loss, Scott R.; Rutter, Jordan E.; Tonra, Christopher M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. RP Marra, PP (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, POB 37012 MRC 5503, Washington, DC 20013 USA. EM marrap@si.edu RI Tonra, Christopher/B-1620-2013 FU NSF; US Fish and Wildlife Service's Migratory Bird Program; Upper Midwest/Great Lakes LCC; Smithsonian's Didden Fellowship FX Funding was provided by NSF, US Fish and Wildlife Service's Migratory Bird Program, Upper Midwest/Great Lakes LCC and Smithsonian's Didden Fellowship. NR 25 TC 26 Z9 27 U1 9 U2 27 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD AUG 1 PY 2015 VL 11 IS 8 AR 20150552 DI 10.1098/rsbl.2015.0552 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CT4SR UT WOS:000362798100007 ER PT J AU Girard, JN Garsden, H Starck, JL Corbel, S Woiselle, A Tasse, C McKean, JP Bobin, J AF Girard, J. N. Garsden, H. Starck, J. L. Corbel, S. Woiselle, A. Tasse, C. McKean, J. P. Bobin, J. TI Sparse representations and convex optimization as tools for LOFAR radio interferometric imaging SO JOURNAL OF INSTRUMENTATION LA English DT Article; Proceedings Paper CT 2nd International Summer School on Intelligent Signal Processing for Frontier Research and Industry CY JUL 14-25, 2014 CL Univ Paris Diderot Campus, Paris, FRANCE HO Univ Paris Diderot Campus DE Image processing; Interferometry; Antennas ID WIDE-FIELD; SPLITTING METHODS; ALGORITHM; RECONSTRUCTION; CALIBRATION; ASTRONOMY; DECONVOLUTION; POLARIMETRY; PROJECTION; ARRAYS AB Compressed sensing theory is slowly making its way to solve more and more astronomical inverse problems. We address here the application of sparse representations, convex optimization and proximal theory to radio interferometric imaging. First, we expose the theory behind interferometric imaging, sparse representations and convex optimization, and second, we illustrate their application with numerical tests with SASIR, an implementation of the FISTA, a Forward-Backward splitting algorithm hosted in a LOFAR imager. Various tests have been conducted in Garsden et al., 2015. The main results are: i) an improved angular resolution (super resolution of a factor approximate to 2) with point sources as compared to CLEAN on the same data, ii) correct photometry measurements on a field of point sources at high dynamic range and iii) the imaging of extended sources with improved fidelity. SASIR provides better reconstructions (five time less residuals) of the extended emission as compared to CLEAN. With the advent of large radiotelescopes, there is scope for improving classical imaging methods with convex optimization methods combined with sparse representations. C1 [Girard, J. N.; Starck, J. L.; Corbel, S.; Bobin, J.] CEA, Serv Astrophys, F-91190 Gif Sur Yvette, France. [Garsden, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Woiselle, A.] Sagem Safran, F-75512 Paris 15, France. [Tasse, C.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. [McKean, J. P.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. RP Girard, JN (reprint author), CEA, Serv Astrophys, Bat 709, F-91190 Gif Sur Yvette, France. EM julien.girard@cea.fr OI Starck, Jean-Luc/0000-0003-2177-7794 NR 58 TC 1 Z9 1 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-0221 J9 J INSTRUM JI J. Instrum. PD AUG PY 2015 VL 10 AR C08013 DI 10.1088/1748-0221/10/08/C08013 PG 19 WC Instruments & Instrumentation SC Instruments & Instrumentation GA CS8ZP UT WOS:000362378700013 ER PT J AU Newman, R Kaplan, E Derrick, M AF Newman, Richard Kaplan, Emily Derrick, Michele TI MOPA MOPA: SCIENTIFIC ANALYSIS AND HISTORY OF AN UNUSUAL SOUTH AMERICAN RESIN USED BY THE INKA AND ARTISANS IN PASTO, COLOMBIA SO JOURNAL OF THE AMERICAN INSTITUTE FOR CONSERVATION LA English DT Article DE Mopa mopa; Inka; Qero; Pasto; Elaeagia; Pyrolysis gas chromatography-mass spectrometry; Liquid chromatography-mass spectrometry ID MASS-SPECTROMETRY AB A native South American phenolic resin commonly called mopa mopa was used for many centuries in two cultural contexts, by artisans in the region of Pasto, Colombia (where it is still used), and by the Inka in Peru, where it was used to decorate ceremonial drinking cups known as qeros. It was softened to a rubbery state by heating in water, mixed with colorants, stretched into thin layers and applied as inlay to decorate wooden surfaces of various kinds of objects. The resin comes from trees of the genus Elaeagia, which grows in mountainous regions of western South America from Colombia to Ecuador. Botanical specimens from the two species that are the most likely sources of mopa mopa, Elaeagia pastoensis and Elaeagia utilis, were analyzed along with samples from colonial period objects made in Pasto and samples from Inka qeros. Species-specific identification of the resin is often possible, with E. pastoensis being utilized in Pasto and (probably) E. utilis by the Inka. This conclusion has important implications for the possible connection between the use of mopa mopa in the two widely separated areas. C1 [Newman, Richard; Derrick, Michele] Museum Fine Arts, Sci Res Lab, Boston, MA 02115 USA. [Kaplan, Emily] Smithsonian Natl Museum Amer Indian, Cultural Resources Ctr, New York, NY USA. RP Newman, R (reprint author), Museum Fine Arts, Sci Res Lab, 465 Huntington Ave, Boston, MA 02115 USA. EM rnewman@mfa.org; kaplane@si.edu; mderrick@mfa.org NR 53 TC 0 Z9 0 U1 0 U2 0 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0197-1360 EI 1945-2330 J9 J AM INST CONSERV JI J. Am. Inst. Conserv. PD AUG PY 2015 VL 54 IS 3 BP 123 EP 148 DI 10.1179/1945233015Y.0000000005 PG 26 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CT0NR UT WOS:000362493500002 ER PT J AU Babb, JF Sadeghpour, H Kirby, K AF Babb, James F. Sadeghpour, Hossein Kirby, Kate TI Alexander Dalgarno obituary SO PHYSICS TODAY LA English DT Biographical-Item C1 [Babb, James F.; Sadeghpour, Hossein] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kirby, Kate] Amer Phys Soc, College Pk, MD USA. RP Babb, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0031-9228 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD AUG PY 2015 VL 68 IS 8 BP 63 EP 63 PG 1 WC Physics, Multidisciplinary SC Physics GA CS7SZ UT WOS:000362287300019 ER PT J AU Cohen, O AF Cohen, O. TI Quantifying the Difference Between the Flux-Tube Expansion Factor at the Source Surface and at the Alfv,n Surface Using a Global MHD Model for the Solar Wind SO SOLAR PHYSICS LA English DT Article DE Magnetic fields; Models - Solar wind; Theory - Velocity fields; Solar wind ID NONSPHERICAL SOURCE-SURFACE; MAGNETIC-FIELD; CORONA; HELIOSPHERE; MAGNETOHYDRODYNAMICS; PREDICTION; WAVES AB The potential-field approximation has been providing a fast and computationally inexpensive estimation for the solar corona's global magnetic-field geometry for several decades. In contrast, more physics-based global magnetohydrodynamic (MHD) models have been used for a similar purpose, while being much more computationally expensive. Here, we investigate the difference in the field geometry between a global MHD model and the potential-field source-surface model (PFSSM) by tracing individual magnetic field lines in the MHD model from the Alfv,n surface (AS), through the source surface (SS), all the way to the field-line footpoint, and then back to the source surface in the PFSSM. We also compare the flux-tube expansion at two points at the SS and the AS along the same radial line. We study the effect of solar cycle variations, the order of the potential-field harmonic expansion, and different magnetogram sources. We find that the flux-tube expansion factor is consistently smaller at the AS than at the SS for solar minimum and the fast solar wind, but it is consistently larger for solar maximum and the slow solar wind. We use the Wang-Sheeley-Arge model to calculate the associated wind speed for each field line and propagate these solar-wind speeds to 1 AU. We find a deviation of more than five hours in the arrival time between the two models for 20 % of the field lines in the solar minimum case and for 40 % of the field lines in the solar maximum case. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ocohen@cfa.harvard.edu OI Cohen, Ofer/0000-0003-3721-0215 FU NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI FX Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. NR 33 TC 5 Z9 5 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD AUG PY 2015 VL 290 IS 8 BP 2245 EP 2263 DI 10.1007/s11207-015-0739-3 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS3WY UT WOS:000362007300006 ER PT J AU Jurcsik, J Smitola, P Hajdu, G Sodor, A Nuspl, J Kolenberg, K Furesz, G Moor, A Kun, E Pal, A Bakos, J Kelemen, J Kovacs, T Kriskovics, L Sarneczky, K Szalai, T Szing, A Vida, K AF Jurcsik, J. Smitola, P. Hajdu, G. Sodor, A. Nuspl, J. Kolenberg, K. Furesz, G. Moor, A. Kun, E. Pal, A. Bakos, J. Kelemen, J. Kovacs, T. Kriskovics, L. Sarneczky, K. Szalai, T. Szing, A. Vida, K. TI OVERTONE AND MULTI-MODE RR LYRAE STARS IN THE GLOBULAR CLUSTER M3 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE globular clusters: individual (M3); stars: horizontal-branch; stars: oscillations; stars: variables: RR Lyrae ID GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG; HORIZONTAL-BRANCH STARS; LARGE-MAGELLANIC-CLOUD; VARIABLE-STARS; GALACTIC BULGE; CLASSICAL CEPHEIDS; CCD PHOTOMETRY; LIGHT CURVES; MODULATION AB The overtone and multi-mode RR Lyrae stars in the globular cluster M3 are studied using a 200 day long, B, V, and I-C time-series photometry obtained in 2012. 70% of the 52 overtone variables observed show some kind of multi-periodicity (with additional frequency at f(0.61) = f(1O)/0.61 frequency ratio, Blazhko effect, double/multi-mode pulsation, and period doubling). A signal at the 0.587 frequency ratio to the fundamental-mode frequency is detected in the double-mode star, V13, which may be identified as the second radial overtone mode. If this mode identification is correct, than V13 is the first RR Lyrae star showing triple-mode pulsation of the first three radial modes. Either the Blazhko effect or the f(0.61) frequency (or both of these phenomena) appears in seven double-mode stars. The P-1O/P-F period ratio of RRd stars showing the Blazhko effect are anomalous. A displacement of the main frequency component at the fundamental mode with the value of modulation frequency (or its half), is detected in three Blazhko RRd stars that are parallel with the appearance of the overtone-mode pulsation. The f(0.61) frequency appears in RRc stars that lie at the blue side of the double-mode region and in RRd stars, raising the suspicion that its occurrence may be connected to double-mode pulsation. The changes of the Blazhko and double-mode properties of the stars are also reviewed using the recent and archive photometric data. C1 [Jurcsik, J.; Smitola, P.; Sodor, A.; Nuspl, J.; Moor, A.; Pal, A.; Bakos, J.; Kelemen, J.; Kovacs, T.; Kriskovics, L.; Sarneczky, K.; Vida, K.] Hungarian Acad Sci, Konkoly Observ, H-1525 Budapest, Hungary. [Hajdu, G.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Hajdu, G.] Inst Milenio Astrofis, Santiago, Chile. [Kolenberg, K.] Katholieke Univ Leuven, Inst Astron, B-3001 Heverlee, Belgium. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Furesz, G.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kun, E.] Univ Szeged, Dept Theoret Phys, H-6720 Szeged, Hungary. [Kun, E.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. [Kun, E.] Univ Szeged, Astron Observ, H-6720 Szeged, Hungary. [Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Szing, A.] Univ Szeged, Baja Observ, H-6500 Baja, Hungary. RP Jurcsik, J (reprint author), Hungarian Acad Sci, Konkoly Observ, POB 67, H-1525 Budapest, Hungary. EM jurcsik@konkoly.hu OI Hajdu, Gergely/0000-0003-0594-9138 FU Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientifica Milenio [IC210009]; Proyecto Basal [PFB-06/2007]; Fondecyt [1141141]; CONICYT [Anillo ACT1101]; Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme [PIOF 255267 SAS-RRL]; OTKA grant [K-83790]; MTA CSFK Lendulet Disk Research Group; Lendulet program of the HAS; Hungarian OTKA grant [K-104607]; ESA PECS [4000110889/14/NL/NDe]; [LP2012-31]; [K-109276] FX The authors would like to express their acknowledgment to the referee for the notes, questions, and comments, which helped us improve the clarity and quality of the paper. G.H. acknowledges support by the Ministry for the Economy, Development, and Tourisms Programa Iniciativa Cientifica Milenio through grant IC210009, awarded to the Millennium Institute of Astrophysics; by Proyecto Basal PFB-06/2007; by Fondecyt grant 1141141; and by grants CONICYT Anillo ACT1101 CONICYT-PCHA/Doctorado Nacional/2014-63140099. K.K. is supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme (PIOF 255267 SAS-RRL). N.J. acknowledges the OTKA K-83790 grant; M.A. the grant of the MTA CSFK Lendulet Disk Research Group; and A.P. the LP2012-31, K-109276, and K-104607 grants. K.S. has been supported by the Lendulet-2009 program of the HAS, the Hungarian OTKA grant K-104607, and the ESA PECS Contract No. 4000110889/14/NL/NDe. NR 58 TC 6 Z9 6 U1 0 U2 5 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 AUG PY 2015 VL 219 IS 2 AR 25 DI 10.1088/0067-0049/219/2/25 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CS2CY UT WOS:000361876600011 ER PT J AU Thongkittidilok, C Tharasanit, T Songsasen, N Sananmuang, T Buarpung, S Techakumphu, M AF Thongkittidilok, Chommanart Tharasanit, Theerawat Songsasen, Nucharin Sananmuang, Thanida Buarpung, Sirirak Techakumphu, Mongkol TI Epidermal growth factor improves developmental competence and embryonic quality of singly cultured domestic cat embryos SO JOURNAL OF REPRODUCTION AND DEVELOPMENT LA English DT Article DE Blastocyst; Cat; Epidermal growth factor (EGF); Epidermal growth factor receptor (EGFR); Single-embryo culture ID IN-VITRO CULTURE; CELL-CYCLE PROGRESSION; BOVINE EMBRYOS; GENE-EXPRESSION; PREIMPLANTATION EMBRYOS; OOCYTE MATURATION; EGF; RECEPTOR; DENSITY; COCULTURE AB This study examined the influence of EGF on the expression of EGF receptors (EGFR) and developmental competence of embryos cultured individually versus those cultured in groups. Cat oocytes were in vitro matured and fertilized (IVM/IVF), and cleaved embryos were randomly assigned to one of seven culture conditions: one group each in which embryos were subjected to group culture supplemented with or without 5 ng/ml EGF and five groups in which embryos were subjected to single-embryo culture supplemented with EGF (0, 5, 25, 50 or 100 ng/ml). Morulae, blastocysts and hatching blastocysts were assessed at days 5 and 7; post IVF, respectively, and total blastocyst cell numbers were assessed at day 7. Relative mRNA expressions of EGFR of 2-4-cell embryos, 8-16-cell embryos, morulae and blastocysts cultured in groups or singly with or without EGF supplementation were examined. OCT3/4 and Ki67 in blastocysts derived from the group or single-embryo culture systems with or without EGF supplementation were localized. A higher rate of embryos cultured in groups developed to blastocysts than individually incubated cohorts. Although EGF increased blastocyst formation in the single-embryo culture system, EGF did not affect embryo development in group culture. Expression levels of EGFR decreased in morulae and blastocysts cultured with EGF. An increased ratio of Ki67-positive cells to the total number of cells in the blastocyst was observed in singly cultured embryos in the presence of EGF. However, EGF did not affect the expression of OCT3/4. These findings indicate that EGF enhanced developmental competence of cat embryos cultured singly by stimulating cell proliferation and modulating the EGFR expression at various developmental stages. C1 [Thongkittidilok, Chommanart; Tharasanit, Theerawat; Buarpung, Sirirak; Techakumphu, Mongkol] Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok 10330, Thailand. [Songsasen, Nucharin] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ft Belvoir, VA 22630 USA. [Sananmuang, Thanida] Rajamangala Univ Technol, Fac Vet Med, Chon Buri 20110, Thailand. RP Techakumphu, M (reprint author), Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok 10330, Thailand. EM tmongkol@chula.ac.th FU Royal Golden Jubilee Ph.D. Program, Thailand Research Fund (TRF) [PHD0032/2553]; 90th Anniversary of Chulalongkorn University Fund; [TRF-RSA5680028] FX C Thongkittidilok is the recipient of a grant from the Royal Golden Jubilee Ph.D. Program (PHD0032/2553), Thailand Research Fund (TRF). This research was financially supported by the 90th Anniversary of Chulalongkorn University Fund and TRF-RSA5680028. Finally, the authors would like to thank the Veterinary Public Health Division of the Bangkok Metropolitan Administration, Thailand, for sample collection. NR 69 TC 3 Z9 3 U1 0 U2 4 PU SOCIETY REPRODUCTION & DEVELOPMENT-SRD PI TSUKUBA PA C/O KAZUHIRO KIKUCHI, PHD DVM, NATL INST AGROBIOLOGICAL SCIENCES KANNONDAI 2-1-2, TSUKUBA, IBARAKI 305-8602, JAPAN SN 0916-8818 J9 J REPROD DEVELOP JI J. Reprod. Dev. PD AUG PY 2015 VL 61 IS 4 BP 269 EP 276 PG 8 WC Agriculture, Dairy & Animal Science; Reproductive Biology SC Agriculture; Reproductive Biology GA CR3YR UT WOS:000361269500004 PM 25985792 ER PT J AU Frye, JA Robbins, RK AF Frye, Jennifer A. Robbins, Robert K. TI Is the globally rare frosted elfin butterfly (Lycaenidae) two genetically distinct host plant races in Maryland? DNA evidence from cast larval skins provides an answer SO JOURNAL OF INSECT CONSERVATION LA English DT Article DE Callophrys irus; Wild indigo; Lupine; Host plant races; Mitochondrial CO1 DNA barcodes; Deer ID CALLOPHRYS-IRUS; LEPIDOPTERA; SPECIATION; CATERPILLARS; LUPINE AB Frosted elfin butterfly caterpillars (Callophrys irus) eat either lupine (Lupinus perennis) or wild indigo (Baptisia tinctoria) legumes. Data from larval behavior, adult morphology, demographics, and phenology have led to the suggestion that lupine-feeding populations are genetically distinct from wild indigo-feeding populations. Frosted elfins are of conservation concern throughout their range in the eastern half of North America, and the possibility of host plant races-in which females pass genetically determined oviposition preferences to their daughters-complicates assessments of this vulnerable species. The maternal inheritance of mitochondrial DNA sequences makes CO1 an excellent gene to determine if genetically distinct host plant races have evolved in frosted elfins. In this paper, we extracted DNA using cast larval skins, a non-lethal, minimal-disturbance method appropriate for insects of conservation concern. Fifty eggs and caterpillars were taken from the field, reared in the lab until molting, and then returned to the plant on which they were found. Over 80 % of individuals had DNA successfully sequenced from their cast larval skins. The sequences allowed unequivocal identification. Neither the lupine-feeding nor wild indigo-feeding populations formed monophyletic clusters because many lupine-feeding and wild-indigo feeding individuals shared the same CO1 658 base pair sequence. An isolated population from the mountains of western Maryland was also not genetically distinct from a coastal population 345 km to the east. These results show the usefulness of using cast larval skins as a non-lethal source of DNA in listed species and suggest that frosted elfins are generalist feeders of lupine and wild indigo and are not comprised of two genetically distinct host plant races. C1 [Frye, Jennifer A.] Maryland Dept Nat Resources, Nat Heritage Program, Wye Mills, MD 21601 USA. [Robbins, Robert K.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Frye, JA (reprint author), Maryland Dept Nat Resources, Nat Heritage Program, 909 Wye Mills Rd, Wye Mills, MD 21601 USA. EM Jennifer.frye@maryland.gov; RobbinsR@SI.edu FU State Wildlife Grant from the US Fish and Wildlife Service; Department of Entomology, NMNH, Smithsonian Institution FX We thank the following individuals for their assistance in all aspects of field work: Paula Becker, Danny Thomas, Chris Frye, John Moulis, Kyle Rambo, Wes Knapp, Joe Fehrer Sara Tangren, and numerous volunteers from the Maryland DNR and the Nature Conservancy, most notably Jeff Bacon, Gordon and Mary Burton, David Hindle, Gary Marine, Tom Ogden, Margaret Schultz, Robert Turk and Tom Ogden. We thank Brian Harris and Margaret Rosati at Smithsonian for technical support, and Scott Miller (who urged us to use cast larval skins as a source for mitochondrial DNA), Paul Goldstein, and Karie Darrow for helpful advice. Dana Limpert at Maryland DNR provided mapmaking expertise, and Jeremy deWaard at Guelph greatly facilitated the sequencing of our samples. For reviewing and commenting on the manuscript, we are grateful to Robert Busby, Paul Goldstein, Scott Miller, Richard Smith, and David Wagner. Two anonymous reviewers and the Editor made many helpful suggestions, for which we are grateful. This project was funded in part through a State Wildlife Grant from the US Fish and Wildlife Service, and through the Department of Entomology, NMNH, Smithsonian Institution. NR 33 TC 2 Z9 2 U1 3 U2 9 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1366-638X EI 1572-9753 J9 J INSECT CONSERV JI J. Insect Conserv. PD AUG PY 2015 VL 19 IS 4 BP 607 EP 615 DI 10.1007/s10841-015-9783-4 PG 9 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA CQ8IF UT WOS:000360850000001 ER PT J AU Betremieux, Y Kaltenegger, L AF Betremieux, Yan Kaltenegger, Lisa TI Refraction in planetary atmospheres: improved analytical expressions and comparison with a new ray-tracing algorithm SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; atmospheric effects; methods: analytical; methods: numerical; planets and satellites: atmospheres ID EARTH GJ 1214B; LUNAR ECLIPSE OBSERVATIONS; TRANSMISSION SPECTROSCOPY; RAYLEIGH-SCATTERING; SUPER-EARTHS; WATER-VAPOR; TRANSIT; EXOPLANET; SPECTRUM; SEARCH AB Atmospheric refraction affects to various degrees exoplanet transit, lunar eclipse, as well as stellar occultation observations. Exoplanet retrieval algorithms often use analytical expressions for the column abundance along a ray traversing the atmosphere as well as for the deflection of that ray, which are first-order approximations valid for low densities in a spherically symmetric homogeneous isothermal atmosphere. We derive new analytical formulae for both of these quantities, which are valid for higher densities, and use them to refine and validate a new ray-tracing algorithm which can be used for arbitrary atmospheric temperature-pressure profiles. We illustrate with simple isothermal atmospheric profiles the consequences of our model for different planets: temperate Earth-like and Jovian-like planets, as well as HD 189733b, and GJ1214b. We find that, for both hot exoplanets, our treatment of refraction does not make much of a difference to pressures as high as 10 atm, but that it is important to consider the variation of gravity with altitude for GJ1214b. However, we find that the temperate atmospheres have an apparent scaleheight significantly smaller than their actual density scaleheight at densities larger than 1 amagat, thus increasing the difficulty of detecting spectral features originating in these regions. These denser atmospheric regions form a refractive boundary layer where column abundances and ray deflection increases dramatically with decreasing impact parameter. This refractive boundary layer mimics a surface, and none of the techniques mentioned above can probe atmospheric regions denser than about 4 amagat on these temperate planets. C1 [Betremieux, Yan; Kaltenegger, Lisa] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Betremieux, Y (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM betremieux@mpia.de FU DFG [ENP Ka 3142/1-1]; National Aeronautics and Space Administration FX The authors acknowledge support from DFG funding ENP Ka 3142/1-1. 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 43 TC 2 Z9 2 U1 1 U2 6 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 AUG 1 PY 2015 VL 451 IS 2 BP 1268 EP 1283 DI 10.1093/mnras/stv1078 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000009 ER PT J AU Li, GJ Naoz, S Kocsis, B Loeb, A AF Li, Gongjie Naoz, Smadar Kocsis, Bence Loeb, Abraham TI Implications of the eccentric Kozai-Lidov mechanism for stars surrounding supermassive black hole binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: kinematics and dynamics; galaxies: nuclei ID HIERARCHICAL 3-BODY SYSTEMS; TIDAL DISRUPTION EVENTS; GALACTIC-CENTER; STELLAR-SYSTEMS; RESONANT RELAXATION; SECULAR EVOLUTION; TEST PARTICLE; HOT JUPITERS; AGN DISCS; MASS AB An enhanced rate of stellar tidal disruption events (TDEs) may be an important characteristic of supermassive black hole (SMBH) binaries at close separations. Here, we study the evolution of the distribution of stars around an SMBH binary due to the eccentric Kozai-Lidov (EKL) mechanism, including octupole effects and apsidal precession caused by the stellar mass distribution and general relativity. We identify a region around one of the SMBHs in the binary where the EKL mechanism drives stars to high eccentricities, which ultimately causes the stars to either scatter off the second SMBH or get disrupted. For SMBH masses 10(7) and 10(8) M-circle dot, the TDE rate can reach similar to 10(-2) yr(-1) and deplete a region of the stellar cusp around the secondary SMBH in similar to 0.5 Myr. As a result, the final geometry of the stellar distribution between 0.01 and 0.1 pc around the secondary SMBH is a torus. These effects may be even more prominent in nuclear stellar clusters hosting a supermassive and an intermediate mass black hole. C1 [Li, Gongjie; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Naoz, Smadar] Univ Calif Los Angeles, Div Astron & Astrophys, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Kocsis, Bence] Inst Adv Study, Princeton, NJ 08540 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 RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NSF [AST-1312034]; W. M. Keck Foundation Fund of the Institute for Advanced Study; NASA [NNX11AF29G, NNX14AM24G] FX This work was supported in part by NSF grant AST-1312034. BK was supported in part by the W. M. Keck Foundation Fund of the Institute for Advanced Study and NASA grants NNX11AF29G and NNX14AM24G. The numerical calculations were performed at the Harvard-Smithsonian Center for Astrophysics, the Institute for Theory and Computation, on Harvard Odyssey cluster. NR 95 TC 11 Z9 11 U1 1 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 AUG 1 PY 2015 VL 451 IS 2 BP 1341 EP 1349 DI 10.1093/mnras/stv1031 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000016 ER PT J AU Zhu, YC Narayan, R Sadowski, A Psaltis, D AF Zhu, Yucong Narayan, Ramesh Sadowski, Aleksander Psaltis, Dimitrios TI HERO - A 3D general relativistic radiative post-processor for accretion discs around black holes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; radiative transfer; methods: numerical ID FLUX-LIMITED DIFFUSION; MONTE-CARLO METHOD; PROTOPLANETARY DISKS; NEUTRINO TRANSPORT; TRANSFER EQUATION; HYDRODYNAMICS; CODE; SIMULATIONS; ALGORITHM; DIMENSIONS AB HERO (Hybrid Evaluator for Radiative Objects) is a 3D general relativistic radiative transfer code which has been tailored to the problem of analysing radiation from simulations of relativistic accretion discs around black holes. HERO is designed to be used as a post-processor. Given some fixed fluid structure for the disc (i.e. density and velocity as a function of position from a hydrodynamic or magnetohydrodynamic simulation), the code obtains a self-consistent solution for the radiation field and for the gas temperatures using the condition of radiative equilibrium. The novel aspect of HERO is that it combines two techniques: (1) a short-characteristics (SC) solver that quickly converges to a self-consistent disc temperature and radiation field, with (2) a long-characteristics (LC) solver that provides a more accurate solution for the radiation near the photosphere and in the optically thin regions. By combining these two techniques, we gain both the computational speed of SC and the high accuracy of LC. We present tests of HERO on a range of 1D, 2D, and 3D problems in flat space and show that the results agree well with both analytical and benchmark solutions. We also test the ability of the code to handle relativistic problems in curved space. Finally, we discuss the important topic of ray defects, a major limitation of the SC method, and describe our strategy for minimizing the induced error. C1 [Zhu, Yucong; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sadowski, Aleksander] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Psaltis, Dimitrios] Univ Arizona, Tucson, AZ 85721 USA. RP Zhu, YC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yzhu@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST1312651]; NASA [NNX 14AB47G, NAS8-03060]; NASA - Chandra X-ray Center [PF4-150126]; NSF XSEDE [TG-AST080026N] FX We would like to thank Nathan Roth, Jack Steiner, Jonathan McKinney, James Guillonchon, Jeff McClintock, Yan-Fei Jiang, Javier Garcia, Eric Keto, and Jiachen Jiang for their excellent insights on radiative transfer and comments/suggestions regarding HERO. We also thank our anonymous referee for their many suggestions that have greatly improved the cohesiveness of this paper (especially their recommendations of several relativistic benchmark tests). RN and YZ acknowledge support from NSF grant AST1312651 and NASA grant NNX 14AB47G. AS acknowledges support for this work by NASA through Einstein Post-doctoral Fellowships PF4-150126, awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Finally, we are grateful for support from NSF XSEDE grant TG-AST080026N, the NASA HEC Programme, and the Harvard Odyssey cluster for providing computing resources used in developing this code. NR 87 TC 8 Z9 8 U1 0 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 AUG 1 PY 2015 VL 451 IS 2 BP 1661 EP 1681 DI 10.1093/mnras/stv1046 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000041 ER PT J AU Dey, A Torrey, P Rubin, KHR Ben Zhu, G Suresh, J AF Dey, Arjun Torrey, Paul Rubin, Kate H. R. Ben Zhu, Guangtun Suresh, Joshua TI On the cosmic evolution of Fe/Mg in QSO absorption line systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: haloes; intergalactic medium; quasars: absorption lines ID MG II ABSORBERS; DIGITAL SKY SURVEY; MASS-METALLICITY RELATION; DELAY-TIME DISTRIBUTION; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; SIMILAR-TO 0.5; GALACTIC OUTFLOWS; COSMOLOGICAL SIMULATIONS AB We investigate the variation of the ratio of the equivalent widths of the Fe II lambda 2600 line to the Mg II lambda lambda 2796, 2803 doublet as a function of redshift in a large sample of absorption lines drawn from the Johns Hopkins University - Sloan Digital Sky Survey Absorption Line Catalog. We find that despite large scatter, the observed ratio shows a trend where the equivalent width ratio R = W-Fe II/W-Mg II decreases monotonically with increasing redshift z over the range 0.55 <= z <= 1.90. Selecting the subset of absorbers where the signal-to-noise ratio of the MgII equivalent width W-Mg II is >= 3 and modelling the equivalent width ratio distribution as a Gaussian, we find that the mean of the Gaussian distribution varies as R proportional to (-0.045 +/- 0.005)z. We discuss various possible reasons for the trend. A monotonic trend in the Fe/Mg abundance ratio is predicted by a simple model where the abundances of Mg and Fe in the absorbing clouds are assumed to be the result of supernova (SN) ejecta and where the cosmic evolution in the SNIa and core-collapse SN rates is related to the cosmic star formation rate. If the trend in R reflects the evolution in the abundances, then it is consistent with the predictions of the simple model. C1 [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Torrey, Paul] CALTECH, Pasadena, CA 91125 USA. [Torrey, Paul] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rubin, Kate H. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ben Zhu, Guangtun; Suresh, Joshua] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Dey, A (reprint author), Harvard Univ, Radcliffe Inst Adv Study, Byerly Hall,8 Garden St, Cambridge, MA 02138 USA. EM dey@noao.edu OI Zhu, Guangtun/0000-0002-7574-8078; Torrey, Paul/0000-0002-5653-0786 FU 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; NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF2-51351, NAS 5-26555]; National Optical Astronomy Observatory (NOAO) FX This research made use of the JHU-SDSS Metal Absorption Line Catalog (ZM13), which is based on the SDSS DR7 (Abazajian et al. 2009), and the NIST Atomic Spectra Database (Kramida et al. 2013). We thank Dr Brice Menard for useful advice and for putting together such a scientifically useful resource. AD thanks Joan Najita for assistance with the ASURV package and Tom Matheson for useful comments on the manuscript. We are grateful to the referee for a constructive report that resulted in improving this paper. Funding for the SDSS and SDSS-II was 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/. GBZ acknowledges partial support provided by NASA through Hubble Fellowship grant #HST-HF2-51351 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under contract NAS 5-26555. AD's research activities are supported by the National Optical Astronomy Observatory (NOAO). AD thanks the Radcliffe Institute for Advanced Study and the Institute for Theory and Computation at Harvard University for their generous support during the period when this paper was written. NOAO is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 62 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 AUG 1 PY 2015 VL 451 IS 2 BP 1806 EP 1814 DI 10.1093/mnras/stv604 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000052 ER PT J AU Silverman, JM Vinko, J Marion, GH Wheeler, JC Barna, B Szalai, T Mulligan, BW Filippenko, AV AF Silverman, Jeffrey M. Vinko, Jozsef Marion, G. H. Wheeler, J. Craig Barna, Barnabas Szalai, Tamas Mulligan, Brian W. Filippenko, Alexei V. TI High-velocity features of calcium and silicon in the spectra of Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: spectroscopic; supernovae: general ID HUBBLE-SPACE-TELESCOPE; TIME OPTICAL-SPECTRA; LOW-LUMINOSITY HOST; WHITE-DWARF STAR; SN 2011FE; LIGHT CURVES; SPECTROSCOPIC OBSERVATIONS; COSMOLOGICAL CONSTRAINTS; CIRCUMSTELLAR MATERIAL; DIVERSITY AB 'High-velocity features' (HVFs) are spectral features in Type Ia supernovae (SNe Ia) that have minima indicating significantly higher (by greater than about 6000 km s-1) velocities than typical 'photospheric-velocity features' (PVFs). The PVFs are absorption features with minima indicating typical photospheric (i.e. bulk ejecta) velocities (usually similar to 9000-15 000 km s(-1) near B-band maximum brightness). In this work, we undertake the most in-depth study of HVFs ever performed. The data set used herein consists of 445 low-resolution optical and near-infrared (NIR) spectra (at epochs up to 5 d past maximum brightness) of 210 low-redshift SNe Ia that follow the 'Phillips relation'. A series of Gaussian functions is fit to the data in order to characterize possible HVFs of Ca II H&K, Si II lambda 6355, and the Ca II NIR triplet. The temporal evolution of the velocities and strengths of the PVFs and HVFs of these three spectral features is investigated, as are possible correlations with other SN Ia observables. We find that while HVFs of Ca II are regularly observed (except in underluminous SNe Ia, where they are never found), HVFs of Si II lambda 6355 are significantly rarer, and they tend to exist at the earliest epochs and mostly in objects with large photospheric velocities. It is also shown that stronger HVFs of Si II lambda 6355 are found in objects that lack C II absorption at early times and that have red ultraviolet/optical colours near maximum brightness. These results lead to a self-consistent connection between the presence and strength of HVFs of Si II lambda 6355 and many other mutually correlated SN Ia observables, including photospheric velocity. C1 [Silverman, Jeffrey M.; Vinko, Jozsef; Marion, G. H.; Wheeler, J. Craig; Mulligan, Brian W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Vinko, Jozsef; Barna, Barnabas; Szalai, Tamas] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Silverman, JM (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jsilverman@astro.as.utexas.edu FU W. M. Keck Foundation; NASA; NSF [AST-1302771, AST 11-09801, AST-1211916, PHY-1066293]; Hungarian OTKA [NN 107637, PD 112325]; Christopher R. Redlich Fund; TABASGO Foundation FX We thank the referee, M. J. Childress, for useful comments and stimulating discussion that helped improve this paper, R. J. Foley, K. Maguire, A. A. Miller, and L. Wang for useful discussions, and the staffs at the Lick, Keck, and McDonald Observatories for their assistance with the observations. The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Marcario LRS is named for Mike Marcario of High Lonesome Optics who fabricated several optics for the instrument but died before its completion. The LRS is a joint project of the HET partnership and the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico. 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 NASA; 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. 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. JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. JV and TS are supported by Hungarian OTKA Grants NN 107637 and PD 112325, respectively. JCW's supernova group at UT Austin is supported by NSF Grant AST 11-09801. AVF is grateful for support from the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. Some work on this paper was done in the hospitable climate of the Aspen Center for Physics that is supported by NSF Grant PHY-1066293. NR 121 TC 17 Z9 17 U1 0 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 AUG 1 PY 2015 VL 451 IS 2 BP 1973 EP 2014 DI 10.1093/mnras/stv1011 PG 42 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8BB UT WOS:000360830000065 ER PT J AU Castelli, F Kurucz, RL Cowley, CR AF Castelli, F. Kurucz, R. L. Cowley, C. R. TI New Mn II energy levels from the STIS-HST spectrum of the HgMn star HD175640 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE line: identification; atomic data; stars: atmospheres; stars: chemically peculiar; stars: individual: HD 175640 ID OSCILLATOR-STRENGTHS; TRANSITION-PROBABILITIES; CHI-LUPI; GA-II; ULTRAVIOLET TRANSITIONS; LIFETIME MEASUREMENTS; IONIZED GOLD; ATOMIC DATA; PD II; LINES AB Aims. The NIST database lists several Mn II lines that were observed in the laboratory but not classified. They cannot be used in spectrum synthesis because their atomic line data are unknown. These lines are concentrated in the 2380-2700 angstrom interval. We aimed to assign energy levels and log gf values to these lines. Methods. Semi-empirical line data for Mn II computed by Kurucz were used to synthesize the ultraviolet spectrum of the slow-rotating, HgMn star HD175640. The spectrum was compared with the high-resolution spectrum observed with the HST-STIS equipment. A UVES spectrum covering the 3050-10 000 angstrom region was also examined. Results. We determined a total of 73 new energy levels, 58 from the STIS spectrum of HD175640 and another 15 from the UVES spectrum. The new energy levels give rise to numerous new computed lines. We have identified more than 50% of the unclassified lines listed in the NIST database and have changed the assignment of another 24 lines. An abundance analysis of the star HD175640, based on the comparison of observed and computed ultraviolet spectra in the 1250-3040 angstrom interval, is the by-product of this study on Mn II. C1 [Castelli, F.] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy. [Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cowley, C. R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Castelli, F (reprint author), Osserv Astron Trieste, Ist Nazl Astrofis, Via Tiepolo 11, I-34143 Trieste, Italy. EM castelli@oats.inaf.it; rkurucz@cfa.harvard.edu; cowley@umich.edu NR 47 TC 2 Z9 2 U1 0 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A10 DI 10.1051/0004-6361/201525903 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200010 ER PT J AU Falstad, N Gonzalez-Alfonso, E Aalto, S van der Werf, PP Fischer, J Veilleux, S Melendez, M Farrah, D Smith, HA AF Falstad, N. Gonzalez-Alfonso, E. Aalto, S. van der Werf, P. P. Fischer, J. Veilleux, S. Melendez, M. Farrah, D. Smith, H. A. TI Herschel spectroscopic observations of the compact obscured nucleus in Zw 049.057 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules; galaxies: ISM; galaxies: individual: Zw 049.057; line: formation; infrared: galaxies; submillimeter: galaxies ID LUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; WATER-VAPOR; NGC 4418; MOLECULAR OUTFLOWS; RADIATION PRESSURE; MARKARIAN 231; DISSOCIATIVE RECOMBINATION; ROTATIONAL-EXCITATION AB Context. The luminous infrared galaxy Zw 049.057 contains a compact obscured nucleus where a considerable amount of the galaxy's luminosity is generated. This nucleus contains a dusty environment that is rich in molecular gas. One approach to probing this kind of environment and to revealing what is hidden behind the dust is to study the rotational lines of molecules that couple well with the infrared radiation emitted by the dust. Aims. We probe the physical conditions in the core of Zw 049.057 and establish the nature of its nuclear power source (starburst or active galactic nucleus). Methods. We observed Zw 049.057 with the Photodetector Array Camera and Spectrometer (PACS) and the Spectral and Photometric Imaging Receiver (SPIRE) onboard the Herschel Space Observatory in rotational lines of H2O, (H2O)-O-18, OH, (OH)-O-18, and [O I]. We modeled the unresolved core of the galaxy using a spherically symmetric radiative transfer code. To account for the different excitation requirements of the various molecular transitions, we use multiple components and different physical conditions. Results. We present the full high-resolution SPIRE FTS spectrum of Zw 049.057, along with relevant spectral scans in the PACS range. We find that a minimum of two different components (nuclear and extended) are required in order to account for the rich molecular line spectrum of Zw 049.057. The nuclear component has a radius of 10-30 pc, a very high infrared surface brightness (similar to 10(14) L-circle dot kpc(-2)), warm dust (T-d > 100 K), and a very large H-2 column density (N-H2 = 10(24) - 10(25) cm(-2)). The modeling also indicates high nuclear H2O (similar to 5 x 10(-6)) and OH (similar to 4 x 10(-6)) abundances relative to H-2 as well as a low O-16/O-18-ratio of 50-100. We also find a prominent infall signature in the [O I] line. We tentatively detect a 500 km s(-1) outflow in the H2O 3(13) -> 2(02) line. Conclusions. The high surface brightness of the core indicates the presence of either a buried active galactic nucleus or a very dense nuclear starburst. The estimated column density towards the core of Zw 049.057 indicates that it is Compton-thick, making a buried X-ray source difficult to detect even in hard X-rays. We discuss the elevated H2O abundance in the nucleus in the context of warm grain and gas-phase chemistry. The H2O abundance is comparable to that of other compact (ultra-)luminous infrared galaxies such as NGC 4418 and Arp 220 - and also to hot cores in the Milky Way. The enhancement of O-18 is a possible indicator that the nucleus of Zw 049.057 is in a similar evolutionary stage as the nuclei of Arp 220 - and more advanced than NGC 4418. We discuss the origin of the extreme nuclear gas concentration and note that the infalling gas detected in [O I] implies that the gas reservoir in the central region of Zw 049.057 is being replenished. If confirmed, the H2O outflow suggests that the nucleus is in a stage of rapid evolution. C1 [Falstad, N.; Aalto, S.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain. [van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Fischer, J.] US Navy, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Veilleux, S.; Melendez, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Falstad, N (reprint author), Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. EM niklas.falstad@chalmers.se FU Swedish National Space Board [145/11:1B, 285/12, 145/11:1-3]; US-ONR; NHSC/ JPL [1456609] FX We thank the anonymous referee for a thorough and constructive report that helped improve the paper. N.F. and S.A. thank the Swedish National Space Board for generous grant support (grant numbers 145/11:1B, 285/12 and 145/11:1-3). Basic research in IR astronomy at NRL is funded by the US-ONR; J.F. acknowledges support from NHSC/ JPL subcontract 1456609. NR 102 TC 7 Z9 7 U1 0 U2 1 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A52 DI 10.1051/0004-6361/201526114 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200052 ER PT J AU Forbrich, J Lada, CJ Lombardi, M Roman-Zuniga, C Alves, J AF Forbrich, Jan Lada, Charles J. Lombardi, Marco Roman-Zuniga, Carlos Alves, Joao TI Smoke in the Pipe Nebula: dust emission and grain growth in the starless core FeSt 1-457 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; stars: formation; submillimeter: ISM; infrared: ISM; radio lines: ISM ID NEAR-INFRARED SURVEY; SPECTRAL INDEX; EXTINCTION MAPS; TEMPERATURE; NOISE; SUBMILLIMETER; POPULATION; HERSCHEL; DENSITY; APEX AB Context. The availability of submillimeter dust emission data in an unprecedented number of bands provides us with new opportunities to investigate the properties of interstellar dust in nearby clouds. Aims. The nearby Pipe Nebula is an ideal laboratory to study starless cores. We here aim to characterize the dust properties of the FeSt 1-457 core, as well as the relation between the dust and the dense gas, using Herschel, Planck, 2MASS, ESO Very Large Telescope, APEX-Laboca, and IRAM 30 m data. Methods. We derive maps of submillimeter dust optical depth and effective dust temperature from Herschel data that were calibrated against Planck. After calibration, we then fit a modified blackbody to the long-wavelength Herschel data, using the Planck-derived dust opacity spectral index beta, derived on scales of 30' (or similar to 1 pc). We use this model to make predictions of the submillimeter flux density at 850 mu m, and we compare these in turn with APEX-Laboca observations. Our method takes into account any additive zeropoint offsets between the Herschel/Planck and Laboca datasets. Additionally, we compare the dust emission with near-infrared extinction data, and we study the correlation of high-density-tracing N2H+ emission with the coldest and densest dust in FeSt 1-457. Results. A comparison of the submillimeter dust optical depth and near-infrared extinction data reveals evidence for an increased submillimeter dust opacity at high column densities, interpreted as an indication of grain growth in the inner parts of the core. Additionally, a comparison of the Herschel dust model and the Laboca data reveals that the frequency dependence of the submillimeter opacity, described by the spectral index beta, does not change. A single beta that is only slightly different from the Planck-derived value is sufficient to describe the data, beta = 1.53 +/- 0.07. We apply a similar analysis to Barnard 68, a core with significantly lower column densities than FeSt 1-457, and we do not find evidence for grain growth but also a single beta. Finally, our previously reported finding of a correlation of N2H+ emission with lower effective dust temperatures is confirmed for FeSt 1-457 in mapping observations. Conclusions. While we find evidence for grain growth from the dust opacity in FeSt 1-457, we find no evidence for significant variations in the dust opacity spectral index beta on scales 0.02 < x < 1 pc (or 36 '' < x < 30'). The correction to the Planck-derived dust beta that we find in both cases is on the order of the measurement error, not including any systematic errors, and it would thus be reasonable to directly apply the dust beta from the Planck all-sky dust model. As a corollary, reliable effective temperature maps can be derived which would be otherwise affected by beta variations. Finally, we note that the angular resolution of extinction maps for the study of nearby starless cores remains unsurpassed. C1 [Forbrich, Jan; Alves, Joao] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Forbrich, Jan; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Roman-Zuniga, Carlos] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22860, Baja California, Mexico. RP Forbrich, J (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. EM jan.forbrich@univie.ac.at RI Roman-Zuniga, Carlos/F-6602-2016; OI Roman-Zuniga, Carlos/0000-0001-8600-4798; LOMBARDI, MARCO/0000-0002-3336-4965 FU Austrian Science Fund (FWF) FX We thank an anonymous referee for comments that helped us to clarify and significantly improve the paper, Ralf Launhardt for insightful discussions, Arnaud Belloche, Giorgio Siringo, and Axel Weiss for help with the Laboca data analysis, and Ted Bergin for providing us with the TRAM data from the Aguti et al. (2007) paper. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. APEX is a collaboration between Max Planck Institut fur Radioastronomie (MPIfR), Onsala Space Observatory (OSO), and the European Southern Observatory (ESO). This publication in A&A is supported by the Austrian Science Fund (FWF). NR 40 TC 3 Z9 3 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 AUG PY 2015 VL 580 AR A114 DI 10.1051/0004-6361/201425375 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200114 ER PT J AU La Palombara, N Esposito, P Mereghetti, S Novara, G Tiengo, A AF La Palombara, N. Esposito, P. Mereghetti, S. Novara, G. Tiengo, A. TI Follow-up observations of X-ray emitting hot subdwarf stars: the He-rich sdO BD+37 degrees 1977 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: early-type; stars: individual: BD+37 degrees 1977; subdwarfs; X-rays: stars ID PHOTON IMAGING CAMERA; EXTREME HELIUM STARS; SUBLUMINOUS O-STARS; WHITE-DWARF; STELLAR WINDS; MASS-LOSS; COMPACT COMPANION; XMM-NEWTON; HD 49798; EVOLUTION AB We report on the results of the first XMM-Newton satellite observation of the luminous and helium-rich O-type subdwarf BD+37 degrees 1977 carried out in April 2014. X-ray emission is detected with a flux of about 4 x 10(-14) erg cm(-2) s(-1) (0.2-1.5 keV), corresponding to a f(X)/f(bol) ratio similar to 10(-7); the source spectrum is very soft, and is well fit by the sum of two plasma components at different temperatures. Both characteristics are in agreement with what is observed in the main-sequence early-type stars, where the observed X-ray emission is due to turbulence and shocks in the stellar wind. A smaller but still significant stellar wind has also been observed in BD+37 degrees 1977; therefore, we suggest that in this case the detected X-ray flux has the same origin. C1 [La Palombara, N.; Esposito, P.; Mereghetti, S.; Novara, G.; Tiengo, A.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Novara, G.; Tiengo, A.] IUSS, I-27100 Pavia, Italy. [Tiengo, A.] Ist Nazl Fis Nucl, Sez Pavia, I-27100 Pavia, Italy. RP La Palombara, N (reprint author), Ist Astrofis Spaziale & Fis Cosm Milano, INAF, Via Bassini 15, I-20133 Milan, Italy. EM nicola@iasf-milano.inaf.it OI La Palombara, Nicola/0000-0001-7015-6359 FU ESA Member States; NASA FX This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. P.E. acknowledges a Fulbright Research Scholar grant administered by the US-Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. NR 40 TC 3 Z9 3 U1 0 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 AUG PY 2015 VL 580 AR A56 DI 10.1051/0004-6361/201526141 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200056 ER PT J AU Mancini, L Hartman, JD Penev, K Bakos, GA Brahm, R Ciceri, S Henning, T Csubry, Z Bayliss, D Zhou, G Rabus, M de Val-Borro, M Espinoza, N Jordan, A Suc, V Bhatti, W Schmidt, B Sato, B Tan, TG Wright, DJ Tinney, CG Addison, BC Noyes, RW Lazar, J Papp, I Sari, P AF Mancini, L. Hartman, J. D. Penev, K. Bakos, G. A. Brahm, R. Ciceri, S. Henning, Th. Csubry, Z. Bayliss, D. Zhou, G. Rabus, M. de Val-Borro, M. Espinoza, N. Jordan, A. Suc, V. Bhatti, W. Schmidt, B. Sato, B. Tan, T. G. Wright, D. J. Tinney, C. G. Addison, B. C. Noyes, R. W. Lazar, J. Papp, I. Sari, P. TI HATS-13b and HATS-14b: two transiting hot Jupiters from the HATSouth survey SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; stars: fundamental parameters; techniques: radial velocities; techniques: photometric; stars: individual: HATS-13 (aka GSC6928-00497); stars: individual: HATS-14 (aka GSC6926-00259) ID PLANETARY PARAMETERS; EXTRASOLAR PLANETS; SURFACE GRAVITIES; KEPLER FIELD; LIGHT CURVES; G STAR; STELLAR; TELESCOPE; MASS; SPECTROGRAPH AB We report the discovery of HATS-13b and HATS-14b, which are two hot-Jupiter transiting planets discovered by the HATSouth survey. The host stars are quite similar to each other (HATS-13: V = 13.9 mag, M-star = 0.96 M-circle dot, R-star = 0.89 R-circle dot, T-eff approximate to 5500 K, [Fe/H] = 0.05; HATS-14: V = 13.8 mag, M-star = 0.97 M-circle dot, R-star = 0.93 R-circle dot, T-eff approximate to 5350 K, [Fe/H] = 0.33) and both the planets orbit around them with a period of similar to 3 days and a separation of similar to 0.04 au. However, even though they are irradiated in a similar way, the physical characteristics of the two planets are very different. HATS-13b, with a mass of M-p = 0.543 +/- 0.072 M-J and a radius of R-p = 1.212 +/- 0.035 R-J, appears as an inflated planet, while HATS-14b, having a mass of M-p = 1.071 +/- 0.070 M-J and a radius of R-p = 1.039 +/- 0.032 R-J, is only slightly larger in radius than Jupiter. C1 [Mancini, L.; Ciceri, S.; Henning, Th.; Rabus, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hartman, J. D.; Penev, K.; Bakos, G. A.; Csubry, Z.; de Val-Borro, M.; Bhatti, W.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Brahm, R.; Rabus, M.; Espinoza, N.; Jordan, A.; Suc, V.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Brahm, R.; Espinoza, N.; Jordan, A.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bayliss, D.] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Zhou, G.; Schmidt, B.] Australian Natl Univ, Canberra, ACT 0200, Australia. [Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Wright, D. J.; Tinney, C. G.; Addison, B. C.] Univ New S Wales, Sch Phys, Exoplanetary Sci Grp, Sydney, NSW 2052, Australia. [Tinney, C. G.] UNSW, Sch Phys, Australian Ctr Astrobiol, Exoplanetary Sci UNSW, Sydney, NSW, Australia. [Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, H-1121 Budapest, Hungary. RP Mancini, L (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM mancini@mpia.de OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Tinney, Christopher/0000-0002-7595-0970; Tan, Thiam-Guan/0000-0001-5603-6895 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX09AB29G, NNX12AH91H, NNX13AQ62G]; FONDECYT [1130857]; BASAL CATA [PFB-06]; Millenium Science Initiative, Chilean Ministry of Economy [IC120009]; CONICYT-PCHA/Doctorado Nacional; "Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; ARC Laureate Fellowship [FL0992131]; Robert Martin Ayers Sciences Fund; [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 telescopes at the ESO Observatory of La Silla. 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 2.2m 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 Regis Lachaume for his technical assistance during the observations at the MPG 2.2m Telescope. We are grateful to P. Sackett for her help in the early phase of the HATSouth project. The reduced light curves presented in this work will be made available at the CDS (http://cdsweb.u-strasbg.fr/). We acknowledge the use of the following internet-based resources: the ESO Digitized Sky Survey; the TEPCat catalog; the SIMBAD data base operated at CDS, Strasbourg, France; and the arXiv scientific paper preprint service operated by Cornell University. NR 56 TC 6 Z9 6 U1 1 U2 7 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 AUG PY 2015 VL 580 AR A63 DI 10.1051/0004-6361/201526069 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200063 ER PT J AU Morosan, DE Gallagher, PT Zucca, P O'Flannagain, A Fallows, R Reid, H Magdalenic, J Mann, G Bisi, MM Kerdraon, A Konovalenko, AA MacKinnon, AL Rucker, HO Thide, B Vocks, C Alexov, A Anderson, J Asgekar, A Avruch, IM Bentum, MJ Bernardi, G Bonafede, A Breitling, F Broderick, JW Brouw, WN Butcher, HR Ciardi, B de Geus, E Eisloffel, J Falcke, H Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hessels, JWT Hoeft, M Karastergiou, A Kondratiev, VI Kuper, G van Leeuwen, J McKay-Bukowski, D McKean, JP Munk, H Orru, E Paas, H Pizzo, R Polatidis, AG Scaife, AMM Sluman, J Tasse, C Toribio, MC Vermeulen, R Zarka, P AF Morosan, D. E. Gallagher, P. T. Zucca, P. O'Flannagain, A. Fallows, R. Reid, H. Magdalenic, J. Mann, G. Bisi, M. M. Kerdraon, A. Konovalenko, A. A. MacKinnon, A. L. Rucker, H. O. Thide, B. Vocks, C. Alexov, A. Anderson, J. Asgekar, A. Avruch, I. M. Bentum, M. J. Bernardi, G. Bonafede, A. Breitling, F. Broderick, J. W. Brouw, W. N. Butcher, H. R. Ciardi, B. de Geus, E. Eisloeffel, J. Falcke, H. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hessels, J. W. T. Hoeft, M. Karastergiou, A. Kondratiev, V. I. Kuper, G. van Leeuwen, J. McKay-Bukowski, D. McKean, J. P. Munk, H. Orru, E. Paas, H. Pizzo, R. Polatidis, A. G. Scaife, A. M. M. Sluman, J. Tasse, C. Toribio, M. C. Vermeulen, R. Zarka, P. TI LOFAR tied-array imaging and spectroscopy of solar S bursts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: radio radiation; Sun: particle emission; Sun: magnetic fields ID III RADIO-BURSTS; FINE-STRUCTURE; CORONA; POLARIZATION; FREQUENCY; RADIATION; DENSITY; SPIKES AB Context. The Sun is an active source of radio emission that is often associated with energetic phenomena ranging from nanoflares to coronal mass ejections (CMEs). At low radio frequencies (<100 MHz), numerous millisecond duration radio bursts have been reported, such as radio spikes or solar S bursts (where S stands for short). To date, these have neither been studied extensively nor imaged because of the instrumental limitations of previous radio telescopes. Aims. Here, LOw Frequency ARray (LOFAR) observations were used to study the spectral and spatial characteristics of a multitude of S bursts, as well as their origin and possible emission mechanisms. Methods. We used 170 simultaneous tied-array beams for spectroscopy and imaging of S bursts. Since S bursts have short timescales and fine frequency structures, high cadence (similar to 50 ms) tied-array images were used instead of standard interferometric imaging, that is currently limited to one image per second. Results. On 9 July 2013, over 3000 S bursts were observed over a time period of similar to 8 h. S bursts were found to appear as groups of short-lived (<1 s) and narrow-bandwidth (similar to 2.5 MHz) features, the majority drifting at similar to 3.5 MHz s(-1) and a wide range of circular polarisation degrees (2-8 times more polarised than the accompanying Type III bursts). Extrapolation of the photospheric magnetic field using the potential field source surface (PFSS) model suggests that S bursts are associated with a trans-equatorial loop system that connects an active region in the southern hemisphere to a bipolar region of plage in the northern hemisphere. Conclusions. We have identified polarised, short-lived solar radio bursts that have never been imaged before. They are observed at a height and frequency range where plasma emission is the dominant emission mechanism, however, they possess some of the characteristics of electron-cyclotron maser emission. C1 [Morosan, D. E.; Gallagher, P. T.; Zucca, P.; O'Flannagain, A.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. [Fallows, R.; Asgekar, A.; Bentum, M. J.; Brouw, W. N.; de Geus, E.; Falcke, H.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hessels, J. W. T.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; McKean, J. P.; Munk, H.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Toribio, M. C.; Vermeulen, R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Reid, H.; MacKinnon, A. L.] Univ Glasgow, SUPA, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Magdalenic, J.] Royal Observ Belgium, SIDC, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium. [Mann, G.; Vocks, C.; Breitling, F.] Leibniz Inst Astrophys Potsdam AIR, D-14482 Potsdam, Germany. [Bisi, M. M.] Harwell Oxford, RAE Space Sci & Technol Facil Council, Rutherford Appleton Lab, Oxford OX11 OQX, Oxon, England. [Kerdraon, A.; Tasse, C.; Zarka, P.] Observ Paris, LESIA, UMR 8109, CNRS, F-92195 Meudon, France. [Konovalenko, A. A.] Inst Radio Astron, UA-61002 Kharkov, Ukraine. [Rucker, H. O.] Austrian Acad Sci, Commiss Astron, A-8042 Graz, Austria. [Thide, B.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.] Hehnholtz Zentrum Potsdam, DeutschesGeoForschunesZentrum GFZ, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore 560099, Karnataka, India. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; Brouw, W. N.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bentum, M. J.] Univ Twente, NL-7522 NB Enxhede, Netherlands. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bonafede, A.] Univ Hamburg, D-21029 Hamburg, Germany. [Broderick, J. W.; Karastergiou, A.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Broderick, J. W.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Obs, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [de Geus, E.] SmarterVision BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thnringer Landessternwarte, D-07778 Tautenburg, Germany. [Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Garrett, M. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmeier, J.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Griessmeier, J.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS,INSU,USR 704,OSUC, F-18330 Nancay, France. [Hessels, J. W. T.; van Leeuwen, J.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, CIT, NL-9700 CA Groningen, Netherlands. RP Morosan, DE (reprint author), Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. EM morosand@tcd.ie RI Ciardi, Benedetta/N-7625-2015; Gallagher, Peter/C-7717-2011; Kondratiev, Vladislav/N-1105-2015 OI Gallagher, Peter/0000-0001-9745-0400; Kondratiev, Vladislav/0000-0001-8864-7471 FU Government of Ireland studentship from the Irish Research Council (IRC); Non-Foundation Scholarship; Trinity College Dublin; Innovation Academy; IRC New Foundations; SUPA Advanced Fellowship; STFC [ST/L000741/1] FX This work has been supported by a Government of Ireland studentship from the Irish Research Council (IRC), the Non-Foundation Scholarship awarded by Trinity College Dublin, the Innovation Academy and the IRC New Foundations. Hamish Reid is supported by a SUPA Advanced Fellowship and an STFC grant ST/L000741/1. We would finally like to acknowledge the LOFAR telescope. 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. NR 29 TC 3 Z9 3 U1 1 U2 7 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 AUG PY 2015 VL 580 AR A65 DI 10.1051/0004-6361/201526064 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200065 ER PT J AU Pinilla, P Birnstiel, T Walsh, C AF Pinilla, P. Birnstiel, T. Walsh, C. TI Sequential planet formation in the HD 100546 protoplanetary disk? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE protoplanetary disks; circumstellar matter; planet-disk interactions ID TRANSITIONAL DISKS; DUST GRAINS; CIRCUMSTELLAR DISK; EMBEDDED PLANETS; GIANT PLANETS; SOLAR NEBULA; HERBIG AE/BE; SAO 206462; GAP EDGES; COMPANION AB Context. The disk around the Herbig Ae star, HD 100546, shows structures that suggest the presence of two companions in the disk at similar to 10 and similar to 70 AU. The outer companion seems to be in the act of formation. Aims. Our aims are to provide constraints on the age of the planets in HD 100546 and to explore the potential evidence for sequential planet formation in transition disks such as HD 100546. Methods. We compare the recent resolved continuum observations of the disk around HD 100546 with the results of dust evolution simulations using an analytical prescription for the shapes of gaps carved by massive planets. Results. An inner pressure bump must have been present since early in the disk lifetime to have good agreement between the dust evolution models and the continuum observations of HD 100546. This pressure bump may have resulted from the presence of a very massive planet (similar to 20 M-Jup), which formed early in the inner disk (r similar to 10 AU). If only this single planet exists, the disk is likely to be old, comparable to the stellar age (similar to 5-10 Myr). Another possible explanation is an additional massive planet in the outer disk (r similar to 70 AU): either a low- mass outer planet (less than or similar to 5 M-Jup) injected at early times, or a higher mass outer planet (greater than or similar to 15 M-Jup) formed very recently, traps the right amount of dust in pressure bumps to reproduce the observations. In the latter case, the disk could be much younger (similar to 3.0 Myr). Conclusions. In the case in which two massive companions are embedded in the disk around HD 100546, as suggested in the literature, the outer companion could be at least greater than or similar to 2.5 Myr younger than the inner companion. C1 [Pinilla, P.; Walsh, C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pinilla, P (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM pinilla@strw.leidenuniv.nl OI Birnstiel, Tilman/0000-0002-1899-8783 FU Koninklijke Nederlandse Akademie van Wetenschappen (KNAW) professor prize; NASA Origins of Solar Systems grant [NNX12AJ04G]; Netherlands Organisation for Scientific Research (NWO) [639.041.335]; Netherlands Research School for Astronomy (NOVA); Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize; European Union A-ERC grant [291141 CHEMPLAN] FX The authors are very grateful to E. F. van Dishoeck and D. Harsono for all their comments and fruitful discussions. We thank to S. Bruderer for providing his data for the disk temperature and C. Wright for the ATCA data. P. P. is supported by Koninklijke Nederlandse Akademie van Wetenschappen (KNAW) professor prize to Ewine van Dishoeck. T.B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. C.W. acknowledges support from the Netherlands Organisation for Scientific Research (NWO, grant number 639.041.335). Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize, and by the European Union A-ERC grant 291141 CHEMPLAN. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00863.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. NR 75 TC 4 Z9 4 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR A105 DI 10.1051/0004-6361/201425539 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200105 ER PT J AU Santos, NC Adibekyan, V Mordasini, C Benz, W Delgado-Mena, E Dorn, C Buchhave, L Figueira, P Mortier, A Pepe, F Santerne, A Sousa, SG Udry, S AF Santos, N. C. Adibekyan, V. Mordasini, C. Benz, W. Delgado-Mena, E. Dorn, C. Buchhave, L. Figueira, P. Mortier, A. Pepe, F. Santerne, A. Sousa, S. G. Udry, S. TI Constraining planet structure from stellar chemistry: the cases of CoRoT-7, Kepler-10, and Kepler-93 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; planets and satellites: detection; stars: abundances; techniques: spectroscopic ID MASS-RADIUS RELATIONSHIPS; 100 EARTH MASSES; COMPOSITIONAL DIVERSITY; CHEMICAL-COMPOSITION; TERRESTRIAL PLANETS; GIANT PLANETS; ROCKY PLANET; STARS; METALLICITY; ABUNDANCES AB Aims. We explore the possibility that the stellar relative abundances of different species can be used to constrain the bulk abundances of known transiting rocky planets. Methods. We use high resolution spectra to derive stellar parameters and chemical abundances for Fe, Si, Mg, O, and C in three stars hosting low mass, rocky planets: CoRoT-7, Kepler-10, and Kepler-93. These planets follow the same line along the mass-radius diagram, pointing toward a similar composition. The derived abundance ratios are compared with the solar values. With a simple stoichiometric model, we estimate the iron mass fraction in each planet, assuming stellar composition. Results. We show that in all cases, the iron mass fraction inferred from the mass-radius relationship seems to be in good agreement with the iron abundance derived from the host star's photospheric composition. Conclusions. The results suggest that stellar abundances can be used to add constraints on the composition of orbiting rocky planets. C1 [Santos, N. C.; Adibekyan, V.; Delgado-Mena, E.; Figueira, P.; Santerne, A.; Sousa, S. G.] Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, P-4150762 Oporto, Portugal. [Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4169007 Oporto, Portugal. [Mordasini, C.; Benz, W.; Dorn, C.] Univ Bern, Inst Phys, CH-3012 Bern, Switzerland. [Buchhave, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Mortier, A.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Pepe, F.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. RP Santos, NC (reprint author), Univ Porto, CAUP, Inst Astrofis & Ciencias Espaco, Rua Estrelas, P-4150762 Oporto, Portugal. EM nuno@astro.up.pt RI Delgado Mena, Elisa/M-9178-2013; dorn, caroline/R-1864-2016; Figueira, Pedro/J-4916-2013; Adibekyan, Vardan/I-5026-2013; OI Delgado Mena, Elisa/0000-0003-4434-2195; Figueira, Pedro/0000-0001-8504-283X; Adibekyan, Vardan/0000-0002-0601-6199; Santerne, Alexandre/0000-0002-3586-1316; Buchhave, Lars A./0000-0003-1605-5666 FU Fundacao para a Ciencia e a Tecnologia (FCT) [UID/FIS/04434/2013]; FCT through Investigador FCT by FEDER through the program "Programa Operacional de Factores de Competitividade - COMPETE" [IF/01037/201, IF/00169/2012, IF/00028/2014]; FCT through POPH/FSE (EC) by FEDER through the program "Programa Operacional de Factores de Competitividade - COMPETE"; FCT [IF/01037/2013CP1191/CT0001, SFRH/BPD/76606/2011, SFRH/BPD/70574/2010]; EU under a Marie Curie Intra-European Fellowship for Career Development [627202]; Swiss National Science Foundation [BSSGI0_155816]; European Union Seventh Framework Program (FP7) [313014] FX We would like to thank the anonymous referee for the useful comments and suggestions. This work was supported by Fundacao para a Ciencia e a Tecnologia (FCT) through the research grant UID/FIS/04434/2013. P.F., N.C.S., and S.G.S. also acknowledge support from FCT through Investigador FCT contracts of reference IF/01037/2013, IF/00169/2012, and IF/00028/2014, and POPH/FSE (EC) by FEDER funding through the program "Programa Operacional de Factores de Competitividade - COMPETE". P.F. acknowledges support from FCT in the form of project reference IF/01037/2013CP1191/CT0001. A.S. is supported by the EU under a Marie Curie Intra-European Fellowship for Career Development with reference FP7-PEOPLE-2013-IEF, number 627202. E.D.M. and V.A. acknowledge the support from FCT in form of the grants SFRH/BPD/76606/2011 and SFRH/BPD/70574/2010. This work results within the collaboration of the COST Action TD 1308. C.M. acknowledges the support from the Swiss National Science Foundation under grant BSSGI0_155816. A.M. received funding from the European Union Seventh Framework Program (FP7/2007-2013) under grant agreement number 313014 (ETAEARTH). NR 48 TC 14 Z9 14 U1 0 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2015 VL 580 AR L13 DI 10.1051/0004-6361/201526850 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CP6TD UT WOS:000360020200158 ER PT J AU Heer, K Helbig-Bonitz, M Fernandes, RG Mello, MAR Kalko, EKV AF Heer, Katrin Helbig-Bonitz, Maria Fernandes, Renato G. Mello, Marco A. R. Kalko, Elisabeth K. V. TI Effects of land use on bat diversity in a complex plantation-forest landscape in northeastern Brazil SO JOURNAL OF MAMMALOGY LA English DT Article DE acoustic monitoring; Atlantic Forest; fragmentation; land use; matrix habitat; mist netting ID AERIAL INSECTIVOROUS BATS; TROPICAL RAIN-FOREST; ATLANTIC FOREST; PHYLLOSTOMID BATS; SPECIES-DIVERSITY; LEVEL RESPONSES; STURNIRA-LILIUM; BRIDGE ISLANDS; FRAGMENT SIZE; EATING BATS AB In fragmented areas, the persistence of different species depends on their ability to use the surrounding matrix either as a corridor or as a foraging habitat. We assessed how species richness and abundance of Neotropical bats differ among forest fragments and rubber plantations under different management regimes. Our study site was located in a heterogeneous agricultural area in the Atlantic Forest of Bahia, northeastern Brazil. By combining mist netting and acoustic monitoring as complementary techniques, we caught 28 phyllostomid species and recorded 21 aerial insectivorous species, which either forage in open space or close to forests. Open space species were equally abundant and diverse in all land use types. In contrast, assemblages of phyllostomid and aerial insectivorous forest species differed significantly among habitats, with the highest species richness recorded in forest fragments. We identified a number of forest specialists in forest fragments, which indicates a relatively intact bat fauna. In intensively used rubber-cacao plantation, we found surprisingly high bat abundance and diversity, despite the shortage of resources for bats. Our results also indicate that patches of secondary vegetation around rubber plantations are important landscape features for bats and might contribute to the persistence of highly diverse bat assemblages. We suggest that bats do not perceive plantations as a hostile matrix, but probably use them as corridors between forest fragments and patches of secondary vegetation. C1 [Heer, Katrin; Helbig-Bonitz, Maria; Mello, Marco A. R.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Heer, Katrin] Univ Marburg, Conservat Biol, D-35043 Marburg, Germany. [Heer, Katrin] Univ Marburg, Dept Ecol, D-35043 Marburg, Germany. [Fernandes, Renato G.] Univ Fed Mato Grosso, Ctr Ciencias Biol Saude, Dept Biol, BR-79070900 Campo Grande, MS, Brazil. [Mello, Marco A. R.] Univ Fed Minas Gerais, Inst Ciencias Biol, Dept Biol Geral, BR-31270901 Belo Horizonte, MG, Brazil. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Heer, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM katrin.heer@uni-marburg.de; maria.helbig@uni-ulm.de RI Mello, Marco/B-1095-2008 OI Mello, Marco/0000-0002-9098-9427 FU German National Academic Foundation; Ulm University; Humboldt Foundation (AvH) [1134644]; Sao Paulo Research Foundation (FAPESP) [06/00265-0, 05/00587-5, 07/50633-9]; Federal University of Minas Gerais (UFMG) [PRPq 01/2013, 14/2013, 02/2014]; Minas Gerais Research Foundation (FAPEMIG) [APQ-01043-13]; Brazilian Research Council (CNPq) [472372/2013-0]; Research Program on Atlantic Forest Biodiversity (PPBio-MA/CNPq); Ecotone Inc. ("Do Science and Get Support Program"); Center for Biodiversity Studies of the Michelin Ecological Reserve FX We thank M. Tschapka, K. M. Flesher, K. Jung, J. Dolezil, S. C. Renner, M. Knornschild, L. Opgenoorth, and R. Brandl for their help with data analysis and for commenting on earlier versions of the manuscript. KH was financed by the German National Academic Foundation. MARM was sponsored by Ulm University, Humboldt Foundation (AvH, 1134644), Sao Paulo Research Foundation (FAPESP, 06/00265-0, 05/00587-5; 07/50633-9), Federal University of Minas Gerais (UFMG, PRPq 01/2013, 14/2013, 02/2014), Minas Gerais Research Foundation (FAPEMIG, APQ-01043-13), Brazilian Research Council (CNPq, 472372/2013-0), Research Program on Atlantic Forest Biodiversity (PPBio-MA/CNPq), and Ecotone Inc. ("Do Science and Get Support Program"). The research permit was given by the Chico Mendes Institute for Biodiversity (SISBIO 19053-1). Logistical and financial support in Brazil was provided by the Center for Biodiversity Studies of the Michelin Ecological Reserve. NR 73 TC 3 Z9 3 U1 3 U2 47 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD AUG PY 2015 VL 96 IS 4 BP 720 EP 731 DI 10.1093/jmammal/gyv068 PG 12 WC Zoology SC Zoology GA CQ4NW UT WOS:000360582700010 ER PT J AU Quiroga-Carmona, M Woodman, N AF Quiroga-Carmona, Marcial Woodman, Neal TI A new species of Cryptotis (Mammalia, Eulipotyphla, Soricidae) from the Sierra de Perija, Venezuelan-Colombian Andes SO JOURNAL OF MAMMALOGY LA English DT Article DE Blarinini; Cryptotis thomasi species group; neotropical shrews; Soricinae; Soricomorpha; South America ID SMALL-EARED SHREW; GENUS CRYPTOTIS; SORICOMORPHA SORICIDAE AB The Sierra de Perija is the northern extension of the Cordillera Oriental of the Andes and includes part of the border between Colombia and Venezuela. The population of small-eared shrews (Mammalia, Eulipotyphla, Soricidae, Cryptotis) inhabiting the Sierra de Perija previously was known from only a single skull from an individual collected in Colombia in 1989. This specimen had been referred to alternatively as C. thomasi and C. meridensis, but a more precise definition of the known Colombian and Venezuelan species of Cryptotis has since excluded the Sierra de Perija population from any named species. The recent collection of a specimen from the Venezuelan slope of Sierra de Perija prompted us to re-evaluate the taxonomic status of this population and determine its relationship with other Andean shrews. Our examination of the available specimens revealed that they possess a unique suite of morphological and morphometrical characters, and we describe the Sierra de Perija population as a new species in the predominantly South American C. thomasi species group. Recognition of this new species adds to our knowledge of this genus in South America and to the biodiversity of the Sierra de Perija. C1 [Quiroga-Carmona, Marcial] Univ Carabobo, Fac Expt Ciencias & Tecnol, Dept Biol, Valencia 2005, Venezuela. [Quiroga-Carmona, Marcial] Inst Venezolano Invest Cient, Ctr Ecol, Caracas 1020A, Venezuela. [Woodman, Neal] Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Quiroga-Carmona, M (reprint author), Univ Carabobo, Fac Expt Ciencias & Tecnol, Dept Biol, Valencia 2005, Venezuela. EM marcialquiroga@gmail.com OI Woodman, Neal/0000-0003-2689-7373 FU Fundacion Provita through Iniciativa de Especies Amenazadas (IEA) FX We thank the Fundacion Provita for partial sponsorship of this work through Iniciativa de Especies Amenazadas (IEA). We thank the following curators and collections managers for loans or for permission to examine specimens under their care: R. Voss (AMNH); P. Jenkins, L. Tomsett, and R. Portela-Miguez (BMNH); P. Soriano and J. Murillo (CVULA); F. Bisbal and J. Sanchez (EBRG); L. R. Heaney, B. D. Patterson, J. Phelps, and W. T. Stanley (FMNH); A. Cadena and H. Lopez-Arevalo (ICN); R. M. Timm (KU); R. Calchi and D. Prieto (MBLUZ); C. Ferreira and M. Salazar (MBUCV); J. M. Chupasko and M. Omura (MCZ); A. Ferrer (MHNLS); G. Pothet, M. Tranier, and C. Denys, Museum National d'HistoireNaturelle, Paris (MNHN); C. Cuartas-Calles and C. Delgado-V. (MUA); J. Eger and B. Lim (ROM). Special thanks to F. Rojas-Runjaic (MHNLS) for providing the paratype specimen (and its photographs), and J. Molinari for allowing work in his laboratory during this research. G. D'Elia and R. D. Fischer provided valuable comments on previous versions of this manuscript. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the United States government. NR 37 TC 4 Z9 4 U1 1 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD AUG PY 2015 VL 96 IS 4 BP 800 EP 809 DI 10.1093/jmammal/gyv085 PG 10 WC Zoology SC Zoology GA CQ4NW UT WOS:000360582700017 ER PT J AU Salvador-Reyes, LA Sneed, J Paul, VJ Luesch, H AF Salvador-Reyes, Lilibeth A. Sneed, Jennifer Paul, Valerie J. Luesch, Hendrik TI Amantelides A and B, Polyhydroxylated Macrolides with Differential Broad-Spectrum Cytotoxicity from a Guamanian Marine Cyanobacteriurn SO JOURNAL OF NATURAL PRODUCTS LA English DT Article ID STEREOCHEMISTRY; MACROLACTONE; AMPHIDINOLS; METABOLITE; TOLYTOXIN AB Cytotoxicity-guided fractionation of a Guamanian cyanobacterial collection yielded the new compounds amantelides A (1) and B (2). These polyketides are characterized by a 40-membered macrolactone ring consisting of a 1,3-diol and contiguous 1,5-diol units and a tert-butyl substituent. Amantelide A (1) displayed potent cytotoxicity with submicromolar IC50 against HT29 colorectal adenocarcinoma and He La cervical carcinoma cell lines. Acetylation of the hydroxy group at C-33 in 2 caused a close to 10-fold decrease in potency. Exhaustive acetylation of the hydroxy groups abrogated the antiproliferative activity of amantelide A (1) by 20-67-fold. Further bioactivity assessment of 1 against bacterial pathogens and marine fungi indicated a broad spectrum of bioactivity. C1 [Salvador-Reyes, Lilibeth A.; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Luesch, Hendrik] Univ Florida, Ctr Nat Prod, Drug Discovery & Dev CNPD3, Gainesville, FL 32610 USA. [Salvador-Reyes, Lilibeth A.] Univ Philippines, Inst Marine Sci, UP Diliman, Quezon City 1101, Philippines. [Sneed, Jennifer; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, 1345 Ctr Dr, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health; NIGMS [P41GM086210]; NCI [R01CA172310]; University of the Philippines Office of the Vice Chancellor for Research and Development; UP Balik Ph.D. program FX This research was supported by the National Institutes of Health, NIGMS grant P41GM086210, and NCI grant R01CA172310. L.A.S.R acknowledges funding support from the University of the Philippines Office of the Vice Chancellor for Research and Development and the UP Balik Ph.D. program. We are grateful to N. Engene for taxonomic assessment of the cyanobacterium and R. Ratnayake for acquiring the NOE spectra. This is contribution #1000 from the Smithsonian Marine Station at Fort Pierce. NR 20 TC 5 Z9 5 U1 2 U2 14 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0163-3864 EI 1520-6025 J9 J NAT PROD JI J. Nat. Prod. PD AUG PY 2015 VL 78 IS 8 BP 1957 EP 1962 DI 10.1021/acs.jnatprod.5b00293 PG 6 WC Plant Sciences; Chemistry, Medicinal; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy GA CQ7HN UT WOS:000360773700019 PM 26204500 ER PT J AU Chang, AL Deck, AK Malm, PD Attoe, S Willits, K Sullivan, LJ Morgan, SG AF Chang, Andrew L. Deck, Anna K. Malm, Preston D. Attoe, Sarikka Willits, Karissa Sullivan, Lindsay J. Morgan, Steven G. TI CURRENT AND FUTURE FRESHWATER FLOW CONTROL OF OLYMPIA OYSTER POPULATION DEMOGRAPHY IN THE SAN FRANCISCO ESTUARY SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Chang, Andrew L.] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Deck, Anna K.; Malm, Preston D.; Attoe, Sarikka; Willits, Karissa; Morgan, Steven G.] Univ Calif Davis, Bodega Marine Lab, Bodega Bay, CA 94923 USA. [Deck, Anna K.] San Francisco Bay Natl Estuarine Res Reserve, Tiburon, CA 94920 USA. [Sullivan, Lindsay J.] San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. RI Chang, Andrew/J-8058-2016 OI Chang, Andrew/0000-0002-7870-285X NR 0 TC 0 Z9 0 U1 0 U2 4 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 618 EP 618 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500089 ER PT J AU Grosholz, ED Bible, J Ceballos, E Chang, AL Cheng, BS Deck, A Ferner, M Latta, M Wasson, K Zabin, C AF Grosholz, E. D. Bible, J. Ceballos, E. Chang, A. L. Cheng, B. S. Deck, A. Ferner, M. Latta, M. Wasson, K. Zabin, C. TI UNDERSTANDING ENVIRONMENTAL CONDITIONS THAT SUPPORT SUSTAINABLE OLYMPIA OYSTER POPULATIONS: INFORMING RESTORATION AND CONSERVATION SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Grosholz, E. D.; Zabin, C.] Univ Calif Davis, Dept Environm Sci & Policy MORE, Davis, CA USA. [Bible, J.; Cheng, B. S.] Univ Calif Davis, Bodega Marine Lab, MORE, Davis, CA USA. [Ceballos, E.; Chang, A. L.; Zabin, C.] Smithsonian Environm Res Ctr, Tiburon, CA USA. [Deck, A.; Ferner, M.] San Francisco Bay Natl Estuarine Res Reserve, Tiburon, CA USA. [Latta, M.] Calif State Coastal Conservancy, Oakland, CA USA. [Wasson, K.] Elkhorn Slough Natl Estuarine Res Reserve, Watsonville, CA USA. RI Chang, Andrew/J-8058-2016 OI Chang, Andrew/0000-0002-7870-285X NR 0 TC 0 Z9 0 U1 1 U2 5 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 637 EP 637 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500144 ER PT J AU Kiriakopolos, SL Zabin, CJ Martin, L Obernolte, R Abbott, R Grosholz, ED AF Kiriakopolos, Stephanie L. Zabin, Chela J. Martin, Lara Obernolte, Rena Abbott, Robert Grosholz, Edwin D. TI VARIATION IN NATIVE OYSTER (OSTREA LURIDA) PERFORMANCE BETWEEN AND WITHIN TWO RESTORATION SITES IN SAN FRANCISCO BAY SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Kiriakopolos, Stephanie L.; Zabin, Chela J.; Martin, Lara; Grosholz, Edwin D.] Univ Calif Davis, Davis, CA 95616 USA. [Kiriakopolos, Stephanie L.] San Francisco State Univ, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. [Zabin, Chela J.] Smithsonian Environm Res Ctr, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. [Martin, Lara] San Francisco Bay Natl Estuarine Res Reserve, Romberg Tiburon Ctr, Tiburon, CA 94920 USA. [Obernolte, Rena] Isla Arena Consulting, Emeryville, CA USA. [Abbott, Robert] ENVIRON, San Francisco, CA 94111 USA. NR 0 TC 0 Z9 0 U1 2 U2 3 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 648 EP 648 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500177 ER PT J AU Wasson, K Chang, AL Deck, A Dinnel, P Dudas, S Ferner, M Grosholz, T Ruesink, J Trimble, A Schaaf, DV Zabin, C Zacherl, D AF Wasson, Kerstin Chang, Andrew L. Deck, Anna Dinnel, Paul Dudas, Sarah Ferner, Matthew Grosholz, Ted Ruesink, Jennifer Trimble, Alan Schaaf, Dick Vander Zabin, Chela Zacherl, Danielle TI VARIANCE IN RECRUITMENT OF OLYMPIA OYSTERS ACROSS WEST COAST ESTUARIES SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Wasson, Kerstin] Elkhorn Slough Natl Estuarine Res Reserve, Watsonville, CA 95076 USA. [Chang, Andrew L.; Zabin, Chela] Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Deck, Anna; Ferner, Matthew] San Francisco Bay Natl Estuarine Res Reserve, Tiburon, CA 94920 USA. [Dinnel, Paul] Skagit Cty Marine Resources Comm, Mt Vernon, WA 98273 USA. [Dudas, Sarah] Ctr Shellfish Res, Nanaimo, BC V9R 5S5, Canada. [Grosholz, Ted; Zabin, Chela] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Ruesink, Jennifer; Trimble, Alan] Univ Washington, Seattle, WA 98195 USA. [Schaaf, Dick Vander] Nat Conservancy Oregon, Portland, OR 97214 USA. [Zacherl, Danielle] Calif State Univ Fullerton, Fullerton, CA 92831 USA. RI Chang, Andrew/J-8058-2016 OI Chang, Andrew/0000-0002-7870-285X NR 0 TC 0 Z9 0 U1 0 U2 3 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 689 EP 689 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500296 ER PT J AU Zabin, C Wasson, K Fork, S AF Zabin, Chela Wasson, Kerstin Fork, Susanne TI RESTORATION OF NATIVE OYSTERS IN A HIGHLY INVADED ESTUARY SO JOURNAL OF SHELLFISH RESEARCH LA English DT Meeting Abstract C1 [Zabin, Chela] Univ Calif Davis, Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Zabin, Chela] Univ Calif Davis, Environm Sci & Policy Dept, Tiburon, CA 94920 USA. [Wasson, Kerstin; Fork, Susanne] Elkhorn Slough Natl Estuarine Res Reserve, Watsonville, CA 95039 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU NATL SHELLFISHERIES ASSOC PI GROTON PA C/O DR. SANDRA E. SHUMWAY, UNIV CONNECTICUT, 1080 SHENNECOSSETT RD, GROTON, CT 06340 USA SN 0730-8000 EI 1943-6319 J9 J SHELLFISH RES JI J. Shellfish Res. PD AUG PY 2015 VL 34 IS 2 BP 694 EP 694 PG 1 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CQ2DV UT WOS:000360410500309 ER PT J AU Loh, TL Jaafar, Z AF Loh, Tse-Lynn Jaafar, Zeehan TI Turning the tide on bottom trawling SO AQUATIC CONSERVATION-MARINE AND FRESHWATER ECOSYSTEMS LA English DT Editorial Material C1 [Loh, Tse-Lynn] John G Shedd Aquarium, Daniel P Haerther Ctr Conservat & Res, Chicago, IL 60605 USA. [Jaafar, Zeehan] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. [Jaafar, Zeehan] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore. RP Loh, TL (reprint author), John G Shedd Aquarium, Daniel P Haerther Ctr Conservat & Res, 1200 South Lake Shore Dr, Chicago, IL 60605 USA. EM tloh@sheddaquarium.org OI Loh, Tse-Lynn/0000-0003-1360-1991 NR 4 TC 1 Z9 1 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1052-7613 EI 1099-0755 J9 AQUAT CONSERV JI Aquat. Conserv.-Mar. Freshw. Ecosyst. PD AUG PY 2015 VL 25 IS 4 BP 581 EP 583 DI 10.1002/aqc.2563 PG 3 WC Environmental Sciences; Marine & Freshwater Biology; Water Resources SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Water Resources GA CQ2QC UT WOS:000360445100010 ER PT J AU Ceron-Souza, I Gonzalez, EG Schwarzbach, AE Salas-Leiva, DE Rivera-Ocasio, E Toro-Perea, N Bermingham, E McMillan, WO AF Ceron-Souza, Ivania Gonzalez, Elena G. Schwarzbach, Andrea E. Salas-Leiva, Dayana E. Rivera-Ocasio, Elsie Toro-Perea, Nelson Bermingham, Eldredge Owen McMillan, W. TI Contrasting demographic history and gene flow patterns of two mangrove species on either side of the Central American Isthmus SO ECOLOGY AND EVOLUTION LA English DT Article DE Avicennia germinans; bottleneck; climate change; comparative phylogeography; gene flow; last glacial maximum; mangroves; Neotropics; population genetic structure; Rhizophora mangle ID MULTILOCUS GENOTYPE DATA; SEA-LEVEL RISE; GULF-OF-MEXICO; MAXIMUM-LIKELIHOOD-ESTIMATION; RHIZOPHORA-MANGLE; TROPICAL ATLANTIC; CHILLING TEMPERATURES; POPULATION EXPANSION; COALESCENT APPROACH; COMPUTER-PROGRAM AB Comparative phylogeography offers a unique opportunity to understand the interplay between past environmental events and life-history traits on diversification of unrelated but co-distributed species. Here, we examined the effects of the quaternary climate fluctuations and palaeomarine currents and present-day marine currents on the extant patterns of genetic diversity in the two most conspicuous mangrove species of the Neotropics. The black (Avicennia germinans, Avicenniaceae) and the red (Rhizophora mangle, Rhizophoraceae) mangroves have similar geographic ranges but are very distantly related and show striking differences on their life-history traits. We sampled 18 Atlantic and 26 Pacific locations for A.germinans (N=292) and R.mangle (N=422). We performed coalescence simulations using microsatellite diversity to test for evidence of population change associated with quaternary climate fluctuations. In addition, we examined whether patterns of genetic variation were consistent with the directions of major marine (historical and present day) currents in the region. Our demographic analysis was grounded within a phylogeographic framework provided by the sequence analysis of two chloroplasts and one flanking microsatellite region in a subsample of individuals. The two mangrove species shared similar biogeographic histories including: (1) strong genetic breaks between Atlantic and Pacific ocean basins associated with the final closure of the Central American Isthmus (CAI), (2) evidence for simultaneous population declines between the mid-Pleistocene and early Holocene, (3) asymmetric historical migration with higher gene flow from the Atlantic to the Pacific oceans following the direction of the palaeomarine current, and (4) contemporary gene flow between West Africa and South America following the major Atlantic Ocean currents. Despite the remarkable differences in life-history traits of mangrove species, which should have had a strong influence on seed dispersal capability and, thus, population connectivity, we found that vicariant events, climate fluctuations and marine currents have shaped the distribution of genetic diversity in strikingly similar ways. C1 [Ceron-Souza, Ivania; Owen McMillan, W.] Smithsonian Trop Res Inst, Apartado 084303092, Panama. [Ceron-Souza, Ivania] Univ Puerto Rico, San Juan, PR 00931 USA. [Gonzalez, Elena G.] MNCN CSIC, Dept Biodiversidad & Biol Evolut, Madrid 28006, Spain. [Schwarzbach, Andrea E.] Univ Texas Brownsville, Dept Biomed, Brownsville, TX 78520 USA. [Salas-Leiva, Dayana E.] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Salas-Leiva, Dayana E.] USDA ARS, Natl Germplasm Repository, SHRS, Miami, FL 33158 USA. [Rivera-Ocasio, Elsie] Univ Puerto Rico Bayamon, Dept Biol, Bayamon, PR 00959 USA. [Toro-Perea, Nelson] Univ Valle, Genet Sect, Dept Biol, Cali 25360, Colombia. [Bermingham, Eldredge] Patricia & Phillip Frost Museum Sci, Miami, FL USA. RP Ceron-Souza, I (reprint author), Oregon State Univ, Dept Bot & Plant Pathol, 2082 Cordley Hall, Corvallis, OR 97331 USA. EM iviceron@gmail.com RI Gonzalez, Elena/E-4465-2013 OI Gonzalez, Elena/0000-0002-4614-3889 FU Smithsonian Tropical Research Institute (STRI); University of Puerto Rico - Rio Piedras Campus (CREST-CATEC); University of Puerto Rico - Rio Piedras Campus (NSF-EPSCor); NSF [DEB 640279]; U.S. EPA-Science to Achieve Results (STAR) program [U915985] FX This work had the financial support from the Smithsonian Tropical Research Institute (STRI), the University of Puerto Rico - Rio Piedras Campus (CREST-CATEC and NSF-EPSCor) to ICS, NSF grants (DEB 640279) to WOM, and the U.S. EPA-Science to Achieve Results (STAR) program (Grant # U915985) to ERO. NR 83 TC 2 Z9 2 U1 3 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD AUG PY 2015 VL 5 IS 16 BP 3486 EP 3499 DI 10.1002/ece3.1569 PG 14 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA CP8XD UT WOS:000360177400022 PM 26380680 ER PT J AU Mouttham, L Fortune, JE Comizzoli, P AF Mouttham, Lara Fortune, Joanne E. Comizzoli, Pierre TI Damage to fetal bovine ovarian tissue caused by cryoprotectant exposure and vitrification is mitigated during tissue culture SO JOURNAL OF ASSISTED REPRODUCTION AND GENETICS LA English DT Article; Proceedings Paper CT International Conference on Fertility Preservation - Freezing of oocytes, embryos and ovarian tissue: focus on fertility management and fertility preservation CY JAN 16-17, 2015 CL Brussels, BELGIUM SP ISFP DE Ovarian tissue; Vitrification; Primordial follicle activation; Gamete rescue; Cryopreservation ID IN-VITRO CULTURE; NEEDLE IMMERSED VITRIFICATION; SOLID-SURFACE VITRIFICATION; PRIMORDIAL FOLLICLES; PREANTRAL FOLLICLES; FOLLICULAR-GROWTH; CRYOPRESERVATION; INITIATION; TRANSPLANTATION; PRESERVATION AB The objective of this study is to characterize the impact of exposure to cryoprotectants followed by vitrification on primordial follicle survival and activation using a fetal bovine model. In the first study, fetal bovine cortical pieces were exposed to cryoprotectants with or without sucrose and cultured up to 7 days in the presence or absence of insulin. In the second study, cortical pieces were exposed to cryoprotectants with or without sucrose, vitrified, and cultured up to 7 days after warming in the presence or absence of insulin. Viability and morphology of follicles, as well as proliferation and/or DNA repair in ovarian tissue were analyzed. When compared to non-exposed controls, normal follicular morphology was affected in groups exposed to cryoprotectants only immediately post-exposure and after 1 day of culture, but improved by day 3 and did not significantly differ by day 7. Similarly, normal follicular morphology was compromised in vitrified groups after warming and on day 1 compared to controls, but improved by days 3 and 7. Proliferation and/or DNA repair in ovarian tissue was not affected by vitrification in this model. Cryoprotectant exposure and vitrification of ovarian tissue did not impair the activation of primordial follicles in response to insulin, although activation was delayed relative to non-exposed controls. Interestingly, sucrose had no noticeable protective effect. Vitrified fetal bovine ovarian tissue has the intrinsic capacity to mitigate the immediate damage to primordial follicles' morphology and retains the capacity to activate. These findings provide a basis for a successful cryopreservation protocol for ovarian cortical tissue in other species including humans. C1 [Mouttham, Lara; Comizzoli, Pierre] Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Mouttham, Lara; Fortune, Joanne E.] Cornell Univ, Dept Biomed Sci, Ithaca, NY USA. RP Comizzoli, P (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. EM moutthaml@si.edu; comizzolip@si.edu FU United States Department of Agriculture Multistate Project [NE-1227] FX This research was supported by the United States Department of Agriculture Multistate Project (NE-1227). NR 50 TC 1 Z9 1 U1 0 U2 6 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 AUG PY 2015 VL 32 IS 8 BP 1239 EP 1250 DI 10.1007/s10815-015-0543-x PG 12 WC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology SC Genetics & Heredity; Obstetrics & Gynecology; Reproductive Biology GA CQ4AV UT WOS:000360547300013 PM 26249553 ER PT J AU Ielpi, A Gibling, MR Bashforth, AR Dennar, CI AF Ielpi, Alessandro Gibling, Martin R. Bashforth, Arden R. Dennar, Chinemerem I. TI IMPACT OF VEGETATION ON EARLY PENNSYLVANIAN FLUVIAL CHANNELS: INSIGHT FROM THE JOGGINS FORMATION OF ATLANTIC CANADA SO JOURNAL OF SEDIMENTARY RESEARCH LA English DT Article ID BOSS POINT FORMATION; NOVA-SCOTIA; CORDAITALEAN TREES; OKAVANGO DELTA; FOSSIL CLIFFS; NEW-BRUNSWICK; WOODY DEBRIS; ALLUVIAL ARCHITECTURE; CENTRAL AUSTRALIA; MARINE INFLUENCE AB Riparian vegetation profoundly influences modern fluvial channels in a variety of ways, depending on the life-history strategies of different plant types, disturbance frequency, and drainage conditions of available habitats. Direct evidence for these dynamic relationships is usually cryptic in ancient deposits. We report evidence for interactions between rivers and in situ vegetation for selected sites in the lower Pennsylvanian Joggins Formation of Atlantic Canada, encompassing fixed, meandering, and distributary channels originally up to 6 m deep. Channel bodies are associated with a suite of fossilized plant remains, specifically lycopsids that preferred stable wetland settings, disturbance-tolerant calamitaleans, and slow-growing, long-lived cordaitaleans. Vegetation was effective in stabilizing banks and bars and promoting aggradation. Lycopsids and calamitalean groves colonized the channel bed during periods of reduced flow, drawing on the groundwater table, and mounds around upright trunks indicate that they formed bar nuclei after flow resumed. Bank-attached bars with lateral-accretion sets contain upright trees, which may have stabilized inclined sediment surfaces, and trees present between small distributary channels may have formed vegetated islands. Erect lycopsids rooted below the channel base project up into the channel fill, where they formed obstacles and nucleated sediment mounds in active channels. On channel cutbanks, upright lycopsids are tilted towards the channel, and early formed rhizoconcretions are associated with deep cordaitalean root systems in the tops of channel fills. These features imply that vegetation contributed to stabilization of sediment surfaces. The predominance of in situ over transported plant remains suggests that these low-flow-strength rivers had limited ability to erode and entrain large woody debris, especially for small channels with strengthened banks. We infer that patterns of interaction between vegetation and rivers with a range of fluvial style broadly resembled those of today. By the early Pennsylvanian, rivers had moved from a geomorphic and biogeomorphic mode of operation into a fully ecological mode with prominent feedback loops between vegetation and fluvial processes. Vegetation is commonly poorly preserved in fluvial systems but should be incorporated into facies models for Pennsylvanian and younger strata, possibly also for some Devonian and Mississippian formations. C1 [Ielpi, Alessandro; Gibling, Martin R.; Dennar, Chinemerem I.] Dalhousie Univ, Dept Earth Sci, Halifax, NS B3H 4R2, Canada. [Bashforth, Arden R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. RP Ielpi, A (reprint author), Geol Survey Canada, 601 Booth St, Ottawa, ON K1A 0E8, Canada. EM alessandro.ielpi@nrcan.gc.ca FU Natural Sciences and Engineering Research Council of Canada (NSERC); NSERC FX The authors are greatly indebted to Rhea Hurnik for field support and to the Joggins Fossil Centre for logistical assistance. We thank reviewer Christopher Fielding, an anonymous reviewer, and editors Gregory Nadon and James MacEachern for insightful comments. Research was supported by a Discovery Grant to MRG from the Natural Sciences and Engineering Research Council of Canada (NSERC). AI and ARB acknowledge the support of Postdoctoral Fellowships from NSERC. The research was carried out under a Heritage Research Permit from the Nova Scotia Department of Communities, Culture and Heritage. NR 130 TC 3 Z9 3 U1 4 U2 16 PU SEPM-SOC SEDIMENTARY GEOLOGY PI TULSA PA 6128 EAST 38TH ST, STE 308, TULSA, OK 74135-5814 USA SN 1527-1404 EI 1938-3681 J9 J SEDIMENT RES JI J. Sediment. Res. PD AUG PY 2015 VL 85 IS 8 BP 999 EP 1018 DI 10.2110/jsr.2015.50 PG 20 WC Geology SC Geology GA CP8QT UT WOS:000360159900005 ER PT J AU van der Sar, T Casola, F Walsworth, R Yacoby, A AF van der Sar, Toeno Casola, Francesco Walsworth, Ronald Yacoby, Amir TI Nanometre-scale probing of spin waves using single-electron spins SO NATURE COMMUNICATIONS LA English DT Article ID AMBIENT CONDITIONS; NANOSCALE RESOLUTION; MAGNETIC-RESONANCE; MAGNETOMETRY; SENSITIVITY; SKYRMIONS AB Pushing the frontiers of condensed-matter magnetism requires the development of tools that provide real-space, few-nanometre-scale probing of correlated-electron magnetic excitations under ambient conditions. Here we present a practical approach to meet this challenge, using magnetometry based on single nitrogen-vacancy centres in diamond. We focus on spin-wave excitations in a ferromagnetic microdisc, and demonstrate local, quantitative and phase-sensitive detection of the spin-wave magnetic field at similar to 50 nm from the disc. We map the magnetic-field dependence of spin-wave excitations by detecting the associated local reduction in the disc's longitudinal magnetization. In addition, we characterize the spin-noise spectrum by nitrogen-vacancy spin relaxometry, finding excellent agreement with a general analytical description of the stray fields produced by spin-spin correlations in a 2D magnetic system. These complementary measurement modalities pave the way towards imaging the local excitations of systems such as ferromagnets and antiferromagnets, skyrmions, atomically assembled quantum magnets, and spin ice. C1 [van der Sar, Toeno; Casola, Francesco; Walsworth, Ronald; Yacoby, Amir] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Casola, Francesco; Walsworth, Ronald] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yacoby, A (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM yacoby@physics.harvard.edu FU DARPA QuASAR program; National Science Foundation; Swiss National Science Foundation FX We acknowledge support of the DARPA QuASAR program and the National Science Foundation. F.C. acknowledges support from the Swiss National Science Foundation. NR 38 TC 12 Z9 12 U1 4 U2 43 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 AUG PY 2015 VL 6 AR 7886 DI 10.1038/ncomms8886 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CQ1GE UT WOS:000360344500005 PM 26249673 ER PT J AU Engene, N Tronholm, A Salvador-Reyes, LA Luesch, H Paul, VJ AF Engene, Niclas Tronholm, Ana Salvador-Reyes, Lilibeth A. Luesch, Hendrik Paul, Valerie J. TI CALDORA PENICILLATA GEN. NOV., COMB. NOV (CYANOBACTERIA), A PANTROPICAL MARINE SPECIES WITH BIOMEDICAL RELEVANCE SO JOURNAL OF PHYCOLOGY LA English DT Article DE dolastatin 10; largazole; Lyngbya; natural products; Phormidium; phylogenetics; secondary metabolites; Symploca; symplostatin 1 ID STRAINS CYANOBACTERIA; POLYPHASIC APPROACH; MAXIMUM-LIKELIHOOD; GENETIC DIVERSITY; DOLASTATIN 10; RNA GENES; OSCILLATORIALES; PHORMIDIUM; SEQUENCES; LARGAZOLE AB Many tropical marine cyanobacteria are prolific producers of bioactive secondary metabolites with ecological relevance and promising pharmaceutical applications. One species of chemically rich, tropical marine cyanobacteria that was previously identified as Symploca hydnoides or Symploca sp. corresponds to the traditional taxonomic definition of Phormidium penicillatum. In this study, we clarified the taxonomy of this biomedically and ecologically important cyanobacterium by comparing recently collected specimens with the original type material and the taxonomic description of P. penicillatum. Molecular phylogenetic analyses of the 16S rRNA gene and the 16S-23S internal transcribed spacer regions showed that P. penicillatum formed an independent clade sister to the genus Symploca, and distantly related to Phormidium and Lyngbya. We propose the new genus Caldora for this clade, with Caldora penicillata comb. nov. as the type species and designate as the epitype the recently collected strain FK13-1. Furthermore, the production of bioactive secondary metabolites among various geographically dispersed collections of C. penicillata showed that this species consistently produced the metabolite dolastatin 10 and/or the related compound symplostatin 1, which appear to be robust autapomorphic characters and chemotaxonomic markers for this taxon. C1 [Engene, Niclas] Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. [Tronholm, Ana; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Salvador-Reyes, Lilibeth A.] Univ Philippines Diliman, Inst Marine Sci, Quezon City 1101, Philippines. [Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Luesch, Hendrik] Univ Florida, Ctr Nat Prod Drug Discovery & Dev, Gainesville, FL 32610 USA. RP Engene, N (reprint author), Florida Int Univ, Dept Biol Sci, Miami, FL 33199 USA. EM nengene@fiu.edu FU Smithsonian Marine Science Network; NIH [R01CA172310] FX This research project was funded by the Smithsonian Marine Science Network (NE) and in part by the NIH (R01CA172310). Field collections were supported by the Carmabi Research Station (Curacao), Carrie Bow Cay Field Station (Belize), Mote Marine Laboratory (Summerland Key, FL), Smithsonian Marine Station (Ft. Pierce, FL), and the Council on International Educational Exchange Research Station (Bonaire). We acknowledge the governments of Curacao, Belize, Honduras, and Bonaire for permits to collect cyanobacteria. Research activities in the Florida Keys National Marine Sanctuary occurred under permit FKNMS-2013-023 (VP) and FKNMS-2011-007 (B. Lapointe). Field collections were partly supported by a NMNH Small Grant (VP) for Bonaire and Curacao, Mote Protect our Reefs Grants for the Florida Keys (VP), and by the Summit Foundation through the Centre for Marine Studies for Honduras (S. Box). We thank R. Ritson-Williams, S. Reed, and B. Lapointe for help with sampling, as well as A. Wood, B. Lapointe and Z. Foltz for underwater photography. We thank K. A. Miller and the late P. C. Silva at the University and Jepson Herbaria of the University of California at Berkeley for lending isotypes, W. Gerwick and T. Byrum for sharing the Symploca reference strain, and K. McPhail for providing the Leptolyngbya sp. strain PAC-10-03. We are very grateful to L. Le Gall and L. Kervran at PC for the loan of specimens of P. penicillatum. We also thank B. Brooks for help with deposition of specimens at US. We are also grateful to A. Economou-Amilli for help with botanical nomenclature. We thank M. Zubia, O. De Clerck, and T. Sauvage for providing us with valuable information about samples from Reunion. We gratefully acknowledge H. Reichardt and the staff at the SMSFP for general lab assistance. All SEM imaging was performed at the USDA Horticultural research laboratory with the assistance of J. Piraino. All gene sequencing was performed at the Laboratories of Analytical Biology of the NMNH thanks to J. Hunt and L. Weight. We thank A. Wright and P. Winder at Harbor Branch Oceanographic Institute at Florida Atlantic University for usage of LCMS and NMR, and S. Gunasekera for analytical assistance. SMSFP contribution no. 994 and CCRE contribution no. 974. NR 57 TC 3 Z9 3 U1 0 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 EI 1529-8817 J9 J PHYCOL JI J. Phycol. PD AUG PY 2015 VL 51 IS 4 BP 670 EP 681 DI 10.1111/jpy.12309 PG 12 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA CP5JY UT WOS:000359918800008 PM 26327714 ER PT J AU Hernandez-Kantun, JJ Rindi, F Adey, WH Heesch, S Pena, V Le Gall, L Gabrielson, PW AF Hernandez-Kantun, Jazmin J. Rindi, Fabio Adey, Walter H. Heesch, Svenja Pena, Viviana Le Gall, Line Gabrielson, Paul W. TI SEQUENCING TYPE MATERIAL RESOLVES THE IDENTITY AND DISTRIBUTION OF THE GENERITYPE LITHOPHYLLUM INCRUSTANS, AND RELATED EUROPEAN SPECIES L. HIBERNICUM AND L. BATHYPORUM (CORALLINALES, RHODOPHYTA) SO JOURNAL OF PHYCOLOGY LA English DT Article DE anatomy; Lithophyllum bathyporum; Lithophyllum hibernicum; Lithophyllum incrustans; psbA; rbcL; rhodolith; taxonomy; type specimens ID PHILIPPI,R.A. ORIGINAL COLLECTIONS; TAXONOMIC REASSESSMENT; NORTHEAST PACIFIC; SP-NOV; DNA; DIVERSITY; ATLANTIC; NUCLEAR; NAMES; MELOBESIOIDEAE AB DNA sequences from type material in the nongeniculate coralline genus Lithophyllum were used to unambiguously link some European species names to field-collected specimens, thus providing a great advance over morpho-anatomical identification. In particular, sequence comparisons of rbcL, COI and psbA genes from field-collected specimens allowed the following conclusion: the generitype species, L. incrustans, occurs mostly as subtidal rhodoliths and crusts on both Atlantic and Mediterranean coasts, and not as the common, NE Atlantic, epilithic, intertidal crust reported in the literature. The heterotypic type material of L. hibernicum was narrowed to one rhodolith belonging in Lithophyllum. As well as occurring as a subtidal rhodolith, L. hibernicum is a common, epilithic and epizoic crust in the intertidal zone from Ireland south to Mediterranean France. A set of four features distinguished L. incrustans from L. hibernicum, including epithallial cell diameter, pore canal shape of sporangial conceptacles and sporangium height and diameter. An rbcL sequence of the lectotype of Lithophyllum bathyporum, which was recently proposed to accommodate Atlantic intertidal collections of L. incrustans, corresponded to a distinct taxon hitherto known only from Brittany as the subtidal, bisporangial, lectotype, but also occurs intertidally in Atlantic Spain. Specimens from Ireland and France morpho-anatomically identified as L. fasciculatum and a specimen from Cornwall likewise identified as L. duckerae were resolved as L. incrustans and L. hibernicum, respectively. C1 [Hernandez-Kantun, Jazmin J.; Adey, Walter H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Hernandez-Kantun, Jazmin J.; Heesch, Svenja] Natl Univ Ireland, Ryan Inst, Irish Seaweed Res Grp, Galway, Ireland. [Rindi, Fabio] Univ Politecn Marche, Dipartimento Sci Vita & Ambiente, I-60131 Ancona, Italy. [Pena, Viviana] Univ A Coruna, Fac Ciencias, BIOCOST Res Grp, Dept Biol Anim Biol Vexetal & Ecol, La Coruna 15071, Spain. [Pena, Viviana; Le Gall, Line] Univ Paris 04, Museum Natl Hist Nat, EPHE,UMR ISYEB CNRS 7205, UPMC,Equipe Explorat Especes & Evolut,Inst Systma, F-75005 Paris, France. [Pena, Viviana] Univ Ghent, Phycol Res Grp, B-9000 Ghent, Belgium. [Gabrielson, Paul W.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Gabrielson, Paul W.] Univ N Carolina, Herbarium, Chapel Hill, NC 27599 USA. RP Hernandez-Kantun, JJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166 POB 37012, Washington, DC 20560 USA. EM jaz1083@gmail.com RI Le Gall, Line/E-1884-2014; OI Le Gall, Line/0000-0001-7807-4569; Heesch, Svenja/0000-0002-4531-0921; Pena, Viviana/0000-0001-7003-3850 FU National Council for Science and Technology, Mexico [CONACyT-211950]; SEP (Secretariat for Public Education, Mexico); Marine Institute (Ireland) as part of the National Marine Biodiscovery Program (Beaufort Award for Marine Biodiscovery); European Community through the FP6 [NMP3-CT-2003-505758]; National University of Ireland, Galway through the Thomas Crawford Award; M.I.U.R. (Italian Ministry for Education, Universities and Research) through a P.R.I.N.; postdoctoral program Axudas de apoio a etapa inicial de formacion posdoutoral do Plan I2C (Xunta de Galicia); British Phycological Society; Spain's Ministerio de Economia y Competitividad [CGL2009-09495/BOS]; Action Transversale du Museum National d'Histoire Naturelle; network "Bibliotheque du Vivant" - CNRS; Museum National d'Histoire Naturelle; INRA; CEA (Centre National de Sequencage) FX We are very grateful to the following curators for the loan of type material essential to this research: J. Wilbraham (BM), Dr. E. Smets (L), and Dr. K. Hassel (TRH). Jacques Grall, Christine Maggs, Jason Hall-Spencer, Line Le Gall, Conxi Rodriguez-Prieto, Ignacio Barbara, Pilar Diaz, Antonio Secilla, Meadhbh Moriarty, Ricardo Bermejo Lacida, Alex Wan, Benoit Queguineur, Julia Nunn, and Marie Pazoutova are gratefully acknowledged for the collection of samples and/or assistance in the field. We thank P. Lalor for assistance with SEM images, Prof. J. Brodie for revising early versions of the manuscript, and the reviewers for helpful comments and suggestions; JHK was supported by a PhD scholarship from CONACyT-211950 (National Council for Science and Technology, Mexico) and SEP (Secretariat for Public Education, Mexico). Financial support was received from the Marine Institute (Ireland) as part of the National Marine Biodiscovery Program (Beaufort Award for Marine Biodiscovery to the National University of Ireland, Galway), from the European Community through the FP6-funded project HIPPOCRATES (NMP3-CT-2003-505758), from the National University of Ireland, Galway through the Thomas Crawford Award, and from the M.I.U.R. (Italian Ministry for Education, Universities and Research) through a P.R.I.N. 2011 project (Coastal bioconstructions: structure, function and management). VP acknowledges support by the postdoctoral program Axudas de apoio a etapa inicial de formacion posdoutoral do Plan I2C (Xunta de Galicia), and projects funded by British Phycological Society (Small Grant Scheme-Project Award 2011-2012) and Spain's Ministerio de Economia y Competitividad (CGL2009-09495/BOS, partially founded by ERDF); molecular data provided by VP were produced at the Service de Systematique Moleculaire of the Museum National d'Histoire Naturelle (CNRS - UMS 2700) with funds provided by Action Transversale du Museum National d'Histoire Naturelle ("Taxonomie moleculaire: DNA Barcode et gestion durable des collections," "Biodiversite actuelle et fossile. Crises, stress, restaurations et panchronisme: le message systematique" and "Emergences") and network "Bibliotheque du Vivant" funded by CNRS, Museum National d'Histoire Naturelle, INRA and CEA (Centre National de Sequencage). PWG thanks Dr. T. Vision (University of North Carolina, Chapel Hill) for use of lab space and equipment and Dr. D.W. Freshwater (DNA Analysis Core Facility, Center for Marine Sciences, University of North Carolina, Wilmington) for DNA sequencing. NR 68 TC 7 Z9 7 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 EI 1529-8817 J9 J PHYCOL JI J. Phycol. PD AUG PY 2015 VL 51 IS 4 BP 791 EP 807 DI 10.1111/jpy.12319 PG 17 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA CP5JY UT WOS:000359918800017 PM 26986797 ER PT J AU Mullins, P Pugh, R Vaught, J AF Mullins, Piper Pugh, Rebecca Vaught, Jim TI Following up on ISBER 2015: Call for Environmental Biobanking Papers SO BIOPRESERVATION AND BIOBANKING LA English DT Editorial Material C1 [Mullins, Piper] Smithsonian Inst, Pan Smithsonian Gyo Initiat, Washington, DC 20560 USA. [Pugh, Rebecca] NIST, Charleston, SC USA. RP Mullins, P (reprint author), Smithsonian Inst, Pan Smithsonian Gyo Initiat, Washington, DC 20560 USA. EM jvaught@liebertpub.com NR 0 TC 1 Z9 1 U1 1 U2 1 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1947-5535 EI 1947-5543 J9 BIOPRESERV BIOBANK JI Biopreserv. Biobank. PD AUG 1 PY 2015 VL 13 IS 4 BP 229 EP 230 DI 10.1089/bio.2015.29013.pm PG 2 WC Cell Biology; Chemistry, Applied; Medical Laboratory Technology SC Cell Biology; Chemistry; Medical Laboratory Technology GA CP0TX UT WOS:000359589800001 PM 26280500 ER PT J AU Merrill, RM Dasmahapatra, KK Davey, JW Dell'Aglio, DD Hanly, JJ Huber, B Jiggins, CD Joron, M Kozak, KM Llaurens, V Martin, SH Montgomery, SH Morris, J Nadeau, NJ Pinharanda, AL Rosser, N Thompson, MJ Vanjari, S Wallbank, RWR Yu, Q AF Merrill, R. M. Dasmahapatra, K. K. Davey, J. W. Dell'Aglio, D. D. Hanly, J. J. Huber, B. Jiggins, C. D. Joron, M. Kozak, K. M. Llaurens, V. Martin, S. H. Montgomery, S. H. Morris, J. Nadeau, N. J. Pinharanda, A. L. Rosser, N. Thompson, M. J. Vanjari, S. Wallbank, R. W. R. Yu, Q. TI The diversification of Heliconius butterflies: what have we learned in 150 years? SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Review DE adaptation; ecological genomics; gene flow; magic traits; mimicry; Nymphalidae; porous species; reproductive isolation; sensory ecology; speciation ID PASSION-VINE BUTTERFLIES; INSECT MUSHROOM BODIES; WITH-GENE-FLOW; MULLERIAN MIMICRY; WARNING-COLOR; HYBRID ZONES; HOST-PLANT; ECOLOGICAL SPECIATION; LINKAGE MAP; LEPIDOPTERA NYMPHALIDAE AB Research into Heliconius butterflies has made a significant contribution to evolutionary biology. Here, we review our understanding of the diversification of these butterflies, covering recent advances and a vast foundation of earlier work. Whereas no single group of organisms can be sufficient for understanding life's diversity, after years of intensive study, research into Heliconiushas addressed a wide variety of evolutionary questions. We first discuss evidence for widespread gene flow betweenHeliconius species and what this reveals about the nature of species. We then address the evolution and diversity of warning patterns, both as the target of selection and with respect to their underlying genetic basis. The identification of major genes involved in mimetic shifts, and homology at these loci between distantly related taxa, has revealed a surprising predictability in the genetic basis of evolution. In the final sections, we consider the evolution of warning patterns, and Heliconius diversity more generally, within a broader context of ecological and sexual selection. We consider how different traits and modes of selection can interact and influence the evolution of reproductive isolation. C1 [Merrill, R. M.; Davey, J. W.; Dell'Aglio, D. D.; Hanly, J. J.; Jiggins, C. D.; Kozak, K. M.; Martin, S. H.; Nadeau, N. J.; Pinharanda, A. L.; Thompson, M. J.; Vanjari, S.; Wallbank, R. W. R.; Yu, Q.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Merrill, R. M.; Jiggins, C. D.; Joron, M.] Smithsonian Trop Res Inst, Panama City, Panama. [Dasmahapatra, K. K.; Huber, B.; Morris, J.; Rosser, N.] Univ York, Dept Biol, York YO10 5DD, N Yorkshire, England. [Huber, B.; Joron, M.; Llaurens, V.] Univ Paris 04, ISYEB UMR CNRS 7205, Museum Natl Hist Nat, MNHN,UPMC,EPHE,Inst Systemat,Evolut,Biodiversite, Paris, France. [Joron, M.] Univ Montpellier 3, CEFE UMR 5175, Ctr Ecol Fonct & Evolut, EPHE,CNRS, Montpellier 5, France. [Montgomery, S. H.] UCL, Dept Genet Evolut & Environm, London, England. [Nadeau, N. J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Thompson, M. J.] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. [Yu, Q.] Chongqing Univ, Sch Life Sci, Chongqing 630044, Peoples R China. RP Merrill, RM (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM r.merrill@zoo.cam.ac.uk RI Jiggins, Chris/B-9960-2008; Martin, Simon/D-1410-2011; Nadeau, Nicola/E-1149-2011; OI Jiggins, Chris/0000-0002-7809-062X; Martin, Simon/0000-0002-0747-7456; Nadeau, Nicola/0000-0002-9319-921X; Kozak, Krzysztof/0000-0001-8980-3173; Davey, John/0000-0002-1017-9775; Dasmahapatra, Kanchon Kumar/0000-0002-2840-7019 FU Junior Research Fellowship at King's College, Cambridge; Balfour Studentship, University of Cambridge; Research Fellowship at St John's College, Cambridge; Research Fellowship from the Royal Commission for the Exhibition of 1851; Agence Nationale de la Recherche (France); Biology and Biotechnology Research Council (UK); British Ecological Society; European Research Council; Natural Environment Research Council (UK); Smithsonian Tropical Research Institute FX RMM is funded by a Junior Research Fellowship at King's College, Cambridge. KMK is supported by the Balfour Studentship, University of Cambridge; SHMa by a Research Fellowship at St John's College, Cambridge; and SHMo by a Research Fellowship from the Royal Commission for the Exhibition of 1851. Our work on Heliconius has been additionally supported by the Agence Nationale de la Recherche (France), the Biology and Biotechnology Research Council (UK), the British Ecological Society, the European Research Council, the Natural Environment Research Council (UK), and the Smithsonian Tropical Research Institute. We are grateful to Steven van Belleghem, Markus Moest, Brett Seymoure and Timothy Thurman for comments on the manuscript, and the wider Heliconius community for years of stimulating discussion and collaboration. We also thank Hanna Kokko, David Pfennig and a further anonymous reviewer, whose comments greatly improved this manuscript. This review was conceived by RMM and CDJ, and the first draft was written during an enjoyable retreat to North Wales. We would like to thank the trustees of Pen-y-Clip, Fachwen, for accommodating us. NR 239 TC 17 Z9 17 U1 23 U2 130 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X EI 1420-9101 J9 J EVOLUTION BIOL JI J. Evol. Biol. PD AUG PY 2015 VL 28 IS 8 BP 1417 EP 1438 DI 10.1111/jeb.12672 PG 22 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CP0ZS UT WOS:000359606200001 PM 26079599 ER PT J AU Vaslet, A Phillips, DL France, CAM Feller, IC Baldwin, CC AF Vaslet, A. Phillips, D. L. France, C. A. M. Feller, I. C. Baldwin, C. C. TI Trophic behaviour of juvenile reef fishes inhabiting interlinked mangrove-seagrass habitats in offshore mangrove islets SO JOURNAL OF FISH BIOLOGY LA English DT Article DE fish foraging habitats; gut contents; marine ecosystems; SIAR; SIBER; stable isotopes ID ISOTOPE MIXING MODELS; INCORPORATING CONCENTRATION-DEPENDENCE; STABLE-ISOTOPE; RELATIVE IMPORTANCE; FEEDING HABITATS; BEDS; COMMUNITIES; ESTUARINE; DIETARY; CARBON AB Stable isotope (C-13 and N-15) and gut content analyses were used to investigate size-related feeding habits of four reef fishes (the beaugregory Stegastes leucostictus, the french grunt Haemulon flavolineatum, the schoolmaster snapper Lutjanus apodus and the yellowtail snapper Ocyurus chrysurus) inhabiting an offshore (non-estuarine) mangrove islet off Belize, Central America. Comparisons of isotopic niche space and Schoener diet similarity index suggested a low to moderate degree of niche overlap between fish size groups. The C-13 gradient between mangrove and seagrass prey as well as results of Bayesian mixing models revealed that sampled fishes relied mostly on seagrass prey items. Only small and large juveniles of the carnivorous species L. apodus derived a part of their diet from mangroves by targeting mangrove-associated Grapsidae crabs and fish prey, respectively. Isotopic niche shifts were particularly obvious for carnivorous fishes that ingested larger prey items (Xanthidae crabs and fishes) during their ontogeny. The utilization of mangrove food resources is less than expected and depends on the ecology and life history of the fish species considered. This research highlights that mangrove-derived carbon contributed relatively little to the diets of four fish taxa from an offshore mangrove islet. C1 [Vaslet, A.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Phillips, D. L.] US EPA, Natl Hlth & Environm Effects Res Lab, Western Ecol Div, Corvallis, OR 97333 USA. [France, C. A. M.] Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Feller, I. C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Baldwin, C. C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Vaslet, A (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM amandine.vaslet@gmail.com OI Feller, Ilka/0000-0002-6391-1608 FU Marine Science Network Grant from the Smithsonian Institution FX The authors thank V. Paul, Z. Foltz, W. Lee and all the staff of Smithsonian Marine Station at Fort Pierce FL (SMSFP) for their assistance and access to laboratory facilities. We thank C. McIvor of the U.S. Geological Survey, St Petersburg, FL, and anonymous referees for their constructive review of the manuscript. This research was funded by a Marine Science Network Grant from the Smithsonian Institution through a Postdoctoral fellowship to A.V. D.L.P.'s time was provided by the U.S. Environmental Protection Agency. This document has been subjected to the Agency's peer and administrative review, and it has been approved for publication as an EPA document. This is contribution number #997 from the SMSFP and contribution number #975 from the Smithsonian's Caribbean Coral Reef Ecosystems Program. NR 57 TC 1 Z9 1 U1 6 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1112 EI 1095-8649 J9 J FISH BIOL JI J. Fish Biol. PD AUG PY 2015 VL 87 IS 2 BP 256 EP 273 DI 10.1111/jfb.12715 PG 18 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA CO8LS UT WOS:000359421400004 PM 26084450 ER PT J AU Hong, T AF Hong, Terry TI Wind/Pinball 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 AUG PY 2015 VL 140 IS 13 BP 87 EP 89 PG 3 WC Information Science & Library Science SC Information Science & Library Science GA CO7IS UT WOS:000359333400135 ER PT J AU Hong, T AF Hong, Terry TI The Investigation 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 AUG PY 2015 VL 140 IS 13 BP 87 EP 87 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA CO7IS UT WOS:000359333400131 ER PT J AU Kelley, AL de Rivera, CE Grosholz, ED Ruiz, GM Yamada, SB Gillespie, G AF Kelley, Amanda L. de Rivera, Catherine E. Grosholz, Edwin D. Ruiz, Gregory M. Yamada, Sylvia Behrens Gillespie, Graham TI Thermogeographic variation in body size of Carcinus maenas, the European green crab SO MARINE BIOLOGY LA English DT Article ID EASTERN BERING-SEA; DROSOPHILA-MELANOGASTER; CHIONOECETES-OPILIO; PHENOTYPIC PLASTICITY; SALINITY PREFERENCE; BRACHYURAN CRABS; FEMALE SIZE; COPES RULE; SHORE CRAB; TEMPERATURE AB Populations that span a large geographic range often experience a thermal gradient that can differentially affect the phenotypic response of individuals across the population. Variation in temperature has been shown to affect the final adult size of ectotherms, which is referred to as the temperature-size rule for ectotherms. Body size is a fundamentally important trait, as it can impact physiological performance, fecundity, longevity, and macroecological patterns. Hence, temperature may affect body size across a range, which can in turn influence maintenance of populations and ecological interactions. Here, we test whether biogeographic differences in size (carapace width) exist for a recent invasion of the non-native European green crab, Carcinus maenas, along the west coast of North America. We assembled trapping and temperature data collected from 10 sites along the western North American coast over a 5-year period. We also conducted a literature review of C. maenas size across their native range. Our results indicate that adult body size shows negative correlation with environmental temperature in both the native and invaded ranges, conforming to the temperature-size rule for ectotherms. Given the short time since colonization and lack of evident genetic structure across the invasive range, it may be that phenotypic plasticity in response to environmental temperature is driving this relationship. Forces that shape the phenotypic trajectory of species may play an important role in both invasion dynamics and subsequent ecological impacts. C1 [Kelley, Amanda L.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [de Rivera, Catherine E.; Ruiz, Gregory M.] Portland State Univ, Dept Environm Sci & Management, Portland, OR 97201 USA. [Grosholz, Edwin D.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Yamada, Sylvia Behrens] Oregon State Univ, Integrat Biol, Corvallis, OR 97331 USA. [Gillespie, Graham] Fisheries & Oceans Canada, Sci Branch, Pacific Reg Pacific Biol Stn, Nanaimo, BC V9T 6N7, Canada. RP Kelley, AL (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM amanda.kelley@lifesci.ucsb.edu OI Ruiz, Gregory/0000-0003-2499-441X FU UC Exotic Pest and Disease Program; Oceans and Fisheries, Canada; Pacific Marine Fisheries Commission; NSF Graduate Research Fellowship Grant [220005]; NOAA [NA06OAR4170261, NA06OAR4170159, NA07OAR4170501, NA08OAR4170927]; Alaska Department of Fish and Game [IHP-07-146] FX We would like to thank in no particular order: Brian Steves for the Bio-ORACLE temperature data extraction, Scott Groth of the Oregon Department of Fish and Wildlife, and the staff and faculty of the Oregon Institute of Marine Biology for their hospitality while sampling in Coos Bay, and W. McClees for creating Fig. 1. For their help in collecting data, we also thank: B. Kordas, A. Larson, C. Coleman-Hulbert, S. Attoe, I. Clarke, B. Turner, B. Cheng, D. Kimbro, A. Bakus, A. Deck. We also thank R. Preisler and K. Wasson for generously providing the data from Elkhorn Slough, and P. Coelho for CW data from Portugal. Financial support was provided (in part) by UC Exotic Pest and Disease Program, Oceans and Fisheries, Canada, the Pacific Marine Fisheries Commission, NSF Graduate Research Fellowship Grant to ALK, Grant Number 220005, NOAA (Grant #NA06OAR4170261, NA06OAR4170159, NA07OAR4170501, NA08OAR4170927), and Alaska Department of Fish and Game (#IHP-07-146). NR 63 TC 2 Z9 2 U1 5 U2 25 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 AUG PY 2015 VL 162 IS 8 BP 1625 EP 1635 DI 10.1007/s00227-015-2698-5 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CO7ZV UT WOS:000359384600010 ER PT J AU Tepolt, CK Palumbi, SR AF Tepolt, C. K. Palumbi, S. R. TI Transcriptome sequencing reveals both neutral and adaptive genome dynamics in a marine invader SO MOLECULAR ECOLOGY LA English DT Article DE adaptation; invasive species; natural selection and contemporary evolution; neutral processes; population genetics - empirical; transcriptomics ID SNAIL LITTORINA-SAXATILIS; CRABS CARCINUS-MAENAS; POPULATION-STRUCTURE; LOCAL ADAPTATION; GENE FLOW; RANGE EXPANSION; GREEN CRAB; DROSOPHILA-SUBOBSCURA; ECOLOGICAL DIVERGENCE; BIOLOGICAL INVASIONS AB Species invasions cause significant ecological and economic damage, and genetic information is important to understanding and managing invasive species. In the ocean, many invasive species have high dispersal and gene flow, lowering the discriminatory power of traditional genetic approaches. High-throughput sequencing holds tremendous promise for increasing resolution and illuminating the relative contributions of selection and drift in marine invasion, but has not yet been used to compare the diversity and dynamics of a high-dispersal invader in its native and invaded ranges. We test a transcriptome-based approach in the European green crab (Carcinus maenas), a widespread invasive species with high gene flow and a well-known invasion history, in two native and five invasive populations. A panel of 10809 transcriptome-derived nuclear SNPs identified significant population structure among highly bottlenecked invasive populations that were previously undifferentiated with traditional markers. Comparing the full data set and a subset of 9246 putatively neutral SNPs strongly suggested that non-neutral processes are the primary driver of population structure within the species' native range, while neutral processes appear to dominate in the invaded range. Non-neutral native range structure coincides with significant differences in intraspecific thermal tolerance, suggesting temperature as a potential selective agent. These results underline the importance of adaptation in shaping intraspecific differences even in high geneflow marine invasive species. They also demonstrate that high-throughput approaches have broad utility in determining neutral structure in recent invasions of such species. Together, neutral and non-neutral data derived from high-throughput approaches may increase the understanding of invasion dynamics in high-dispersal species. C1 [Tepolt, C. K.; Palumbi, S. R.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. RP Tepolt, CK (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM carolyn.tepolt@gmail.com FU Partnership for the Interdisciplinary Study of Coastal Oceans; Myers Trust; Explorer's Club Exploration Fund; Lerner Gray Memorial Fund of the American Museum of Natural History; Vice Provost for Graduate Education at Stanford; Eugene C. and Aileen E. Haderlie Memorial Fund; National Science Foundation [1210057]; National Defense Science and Engineering Grant; Stanford Graduate Fellowship; Stanford Center for Computational, Evolutionary, and Human Genomics Fellowship; Smithsonian Institution Biodiversity Genomics Fellowship FX We sincerely thank John Lee; the Bamfield Marine Centre; Greg Ruiz and the Smithsonian Environmental Research Center; the Rutgers University Marine Field Station; the Darling Marine Center; Iain McGaw and the Ocean Sciences Centre; Joao Canning-Clode and the Laboratorio Maritimo da Guia; and Henrik Glenner and the Espegrend Marine Biological Station. We are grateful for support from the Partnership for the Interdisciplinary Study of Coastal Oceans, the Myers Trust, the Explorer's Club Exploration Fund, the Lerner Gray Memorial Fund of the American Museum of Natural History, the Vice Provost for Graduate Education at Stanford, the Eugene C. and Aileen E. Haderlie Memorial Fund, and a National Science Foundation Doctoral Dissertation Improvement Grant (1210057). CKT was supported on this project by a National Defense Science and Engineering Grant, a Stanford Graduate Fellowship, and a Stanford Center for Computational, Evolutionary, and Human Genomics Fellowship; she is currently supported by a Smithsonian Institution Biodiversity Genomics Fellowship. We also thank two anonymous reviewers for their thoughtful comments which significantly improved this manuscript. NR 83 TC 7 Z9 7 U1 7 U2 62 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 AUG PY 2015 VL 24 IS 16 BP 4145 EP 4158 DI 10.1111/mec.13294 PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA CO7QM UT WOS:000359355900008 PM 26118396 ER PT J AU Christopher Monckton Brenchley Soon, WWH Legates, DR Briggs, WM AF Christopher Monckton Brenchley Soon, Willie W. -H. Legates, David R. Briggs, William M. TI Keeping it simple: the value of an irreducibly simple climate model SO SCIENCE BULLETIN LA English DT Article DE Climate change; Climate sensitivity; Climate models; Global warming; Temperature feedbacks ID PALEOCENE THERMAL MAXIMUM; SENSITIVITY; TRENDS; TEMPERATURES; VARIABILITY; PREDICTION AB Richardson et al. (Sci Bull, 2015. doi:10.1007/s11434-015-0806-z) suggest that the irreducibly simple climate model described in Monckton of Brenchley et al. (Sci Bull 60:122-135, 2015. doi:10.1007/s11434-014-0699-2) was not validated against observations, relying instead on synthetic test data based on underestimated global warming, illogical parameter choice and near-instantaneous response at odds with ocean warming and other observations. However, the simple model, informed by its authors' choice of parameters, usually hindcasts observed temperature change more closely than the general-circulation models, and finds high climate sensitivity implausible. With IPCC's choice of parameters, the model is further validated in that it duly replicates IPCC's sensitivity interval. Also, fast climate system response is consistent with near-zero or net-negative temperature feedback. Given the large uncertainties in the initial conditions and evolutionary processes determinative of climate sensitivity, subject to obvious caveats a simple sensitivity-focused model need not, and the present model does not, exhibit significantly less predictive skill than the general-circulation models. C1 [Christopher Monckton Brenchley] Sci & Publ Policy Inst, Haymarket, VA 20169 USA. [Soon, Willie W. -H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Legates, David R.] Univ Delaware, Dept Geog, Newark, DE 19716 USA. RP Christopher Monckton Brenchley (reprint author), Sci & Publ Policy Inst, Haymarket, VA 20169 USA. EM monckton@mail.com NR 74 TC 0 Z9 0 U1 2 U2 10 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 2095-9273 EI 2095-9281 J9 SCI BULL JI Sci. Bull. PD AUG PY 2015 VL 60 IS 15 BP 1378 EP 1390 DI 10.1007/s11434-015-0856-2 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CP0HY UT WOS:000359557600010 ER PT J AU Bayliss, D Hartman, JD Bakos, GA Penev, K Zhou, G Brahm, R Rabus, M Jordan, A Mancini, L de Val-Borro, M Bhatti, W Espinoza, N Csubry, Z Howard, AW Fulton, BJ Buchhave, LA Henning, T Schmidt, B Ciceri, S Noyes, RW Isaacson, H Marcy, GW Suc, V Lazar, J Papp, I Sari, P AF Bayliss, D. Hartman, J. D. Bakos, G. A. Penev, K. Zhou, G. Brahm, R. Rabus, M. Jordan, A. Mancini, L. de Val-Borro, M. Bhatti, W. Espinoza, N. Csubry, Z. Howard, A. W. Fulton, B. J. Buchhave, L. A. Henning, T. Schmidt, B. Ciceri, S. Noyes, R. W. Isaacson, H. Marcy, G. W. Suc, V. Lazar, J. Papp, I. Sari, P. TI HATS-8b: A LOW-DENSITY TRANSITING SUPER-NEPTUNE SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HATS-8); techniques: photometric; techniques: spectroscopic ID HOT JUPITERS; K STAR; MASS; STELLAR; EXOPLANETS; TELESCOPE; PLANETS; KEPLER; FIELD; POPULATION AB HATS-8b is a low density transiting super-Neptune discovered as part of the HATSouth project. The planet orbits its solar-like G-dwarf host (V = 14.03 +/- 0.10, T-eff = 5679 +/- 50 K) with a period of 3.5839 days. HATS-8b is the third lowest-mass transiting exoplanet to be discovered from a wide-field ground-based search, and with a mass of 0.138 +/- 0.019 M-J it is approximately halfway between the masses of Neptune and Saturn. However, HATS-8b has a radius of 0.873(-0.075)(+0.123) R-J, resulting in a bulk density of just 0.259 +/- 0.091 g cm(-3). The metallicity of the host star is super-solar ([Fe/H] = 0.210 +/- 0.080), providing evidence against the idea that low-density exoplanets form from metal-poor environments. The low density and large radius of HATS-8b results in an atmospheric scale height of almost 1000 km, and in addition to this there is an excellent reference star of nearly equal magnitude at just 19 '' separation in the sky. These factors make HATS-8b an exciting target for future atmospheric characterization studies, particularly for long-slit transmission spectroscopy. C1 [Bayliss, D.; Zhou, G.] Univ Geneva, Observ Astronom, CH-1290 Versoix, Switzerland. [Bayliss, D.; Schmidt, B.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Hartman, J. D.; Bakos, G. A.; Penev, K.; de Val-Borro, M.; Bhatti, W.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Brahm, R.; Rabus, M.; Jordan, A.; Espinoza, N.; Suc, V.] Catholic Univ Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Brahm, R.; Jordan, A.; Espinoza, N.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Rabus, M.; Henning, T.; Ciceri, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Howard, A. W.; Fulton, B. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Buchhave, L. A.; Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L. A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Isaacson, H.; Marcy, G. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Bayliss, D (reprint author), Univ Geneva, Observ Astronom, 51 Ch Maillettes, CH-1290 Versoix, Switzerland. EM daniel.bayliss@unige.ch; rbrahm@astro.puc.cl OI Jordan, Andres/0000-0002-5389-3944; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Bakos, Gaspar/0000-0001-7204-6727; Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI [NSF/AST-0723074]; NASA [NNX09AB29G/NNX12AH91H, NNX13AQ62G]; internal Princeton funds; FONDECYT [1130857]; BASAL CATA [PFB-06]; "Millennium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; CONICYT-PCHA/Doctorado Nacional; NSF Graduate Research Fellowship [2014184874]; Chilean Telescope Allocation Committee (CNTAC) [CN2012A-61, CN2013A-171, CN2014A-104]; W. M. Keck Foundation; ARC Laureate Fellowship [FL0992131]; National Aeronautics and Space Administration; [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/NNX12AH91H and internal Princeton funds. 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 Millennium 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 "Millennium 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. B.J.F. acknowledges support from the NSF Graduate Research Fellowship grant No. 2014184874. 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. Operations at the MPG 2.2m Telescope are jointly performed by the Max Planck Gesellschaft and the European Southern Observatory. This work is based on observations made with ESO Telescopes at the La Silla Observatory. Observations from the du Pont and Swope telescopes were taken as part of programs CN2012A-61, CN2013A-171, and CN2014A-104, awarded by the Chilean Telescope Allocation Committee (CNTAC). This paper also uses observations obtained using the facilities of the Las Cumbres Observatory Global Telescope. The radial velocity 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. Work at the Australian National University is supported by the ARC Laureate Fellowship grant FL0992131. 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 8 Z9 8 U1 1 U2 12 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 AUG PY 2015 VL 150 IS 2 AR 49 DI 10.1088/0004-6256/150/2/49 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900010 ER PT J AU Jenkins, JM Twicken, JD Batalha, NM Caldwell, DA Cochran, WD Endl, M Latham, DW Esquerdo, GA Seader, S Bieryla, A Petigura, E Ciardi, DR Marcy, GW Isaacson, H Huber, D Rowe, JF Torres, G Bryson, ST Buchhave, L Ramirez, I Wolfgang, A Li, J Campbell, JR Tenenbaum, P Sanderfer, D Henze, CE Catanzarite, JH Gilliland, RL Borucki, WJ AF Jenkins, Jon M. Twicken, Joseph D. Batalha, Natalie M. Caldwell, Douglas A. Cochran, William D. Endl, Michael Latham, David W. Esquerdo, Gilbert A. Seader, Shawn Bieryla, Allyson Petigura, Erik Ciardi, David R. Marcy, Geoffrey W. Isaacson, Howard Huber, Daniel Rowe, Jason F. Torres, Guillermo Bryson, Stephen T. Buchhave, Lars Ramirez, Ivan Wolfgang, Angie Li, Jie Campbell, Jennifer R. Tenenbaum, Peter Sanderfer, Dwight Henze, Christopher E. Catanzarite, Joseph H. Gilliland, Ronald L. Borucki, William J. TI DISCOVERY AND VALIDATION OF Kepler-452b: A 1.6 R phi SUPER EARTH EXOPLANET IN THE HABITABLE ZONE OF A G2 STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: statistical; planets and satellites: detection; stars: fundamental parameters; stars: individual (Kepler-452b, KIC 8311864, KOI7016.01) ID POTENTIAL TRANSIT SIGNALS; FALSE POSITIVES; MISSION DATA; SOPHIE VELOCIMETRY; EXTRASOLAR PLANETS; BLEND SCENARIOS; Y-2 ISOCHRONES; HARPS SEARCH; MILKY-WAY; SYSTEM AB We report on the discovery and validation of Kepler-452b, a transiting planet identified by a search through the 4 years of data collected by NASA's Kepler Mission. This possibly rocky 1.63(-0.20)(+0.23) R-circle plus every 384.843 (+0.007)(-0.012) days, the longest orbital period for a small (R-P < 2 R-circle plus) transiting exoplanet to date. The likelihood that this planet has a rocky composition lies between 49% and 62%. The star has an effective temperature of 5757 +/- 85 K and a log g of 4.32 +/- 0.09. At a mean orbital separation of 1.046 (-0.015) (+0.019) AU, this small planet is well within the optimistic habitable zone of its star (recent Venus/early Mars), experiencing only 10% more flux than Earth receives from the Sun today, and slightly outside the conservative habitable zone (runaway greenhouse/maximum greenhouse). The star is slightly larger and older than the Sun, with a present radius of 1.11 (-0.09) (+0.15) R-circle dot and an estimated age of similar to 6 Gyr. Thus, Kepler-452b has likely always been in the habitable zone and should remain there for another similar to 3 Gyr. C1 [Jenkins, Jon M.; Twicken, Joseph D.; Batalha, Natalie M.; Caldwell, Douglas A.; Seader, Shawn; Rowe, Jason F.; Bryson, Stephen T.; Li, Jie; Tenenbaum, Peter; Sanderfer, Dwight; Henze, Christopher E.; Catanzarite, Joseph H.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Twicken, Joseph D.; Caldwell, Douglas A.; Seader, Shawn; Huber, Daniel; Rowe, Jason F.; Li, Jie; Tenenbaum, Peter; Catanzarite, Joseph H.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.; Endl, Michael; Ramirez, Ivan] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Cochran, William D.; Endl, Michael; Ramirez, Ivan] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Latham, David W.; Esquerdo, Gilbert A.; Bieryla, Allyson; Torres, Guillermo; Buchhave, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Petigura, Erik; Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Buchhave, Lars] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Wolfgang, Angie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Campbell, Jennifer R.] NASA, Wyle Labs, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. RP Jenkins, JM (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jon.Jenkins@nasa.gov NR 89 TC 32 Z9 36 U1 18 U2 61 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 AUG PY 2015 VL 150 IS 2 AR 56 DI 10.1088/0004-6256/150/2/56 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900017 ER PT J AU Johnson, CI Rich, RM Pilachowski, CA Caldwell, N Mateo, M Bailey, JI Crane, JD AF Johnson, Christian I. Rich, R. Michael Pilachowski, Catherine A. Caldwell, Nelson Mateo, Mario Bailey, John I., III Crane, Jeffrey D. TI A SPECTROSCOPIC ANALYSIS OF THE GALACTIC GLOBULAR CLUSTER NGC 6273 (M19) SO ASTRONOMICAL JOURNAL LA English DT Article DE globular clusters: general; globular clusters: individual (NGC 6273, M19); stars: abundances ID MULTIPLE STELLAR POPULATIONS; METAL-POOR STARS; HUBBLE-SPACE-TELESCOPE; RED GIANT BRANCH; DWARF SPHEROIDAL GALAXY; MILKY-WAY BULGE; SODIUM-ABUNDANCE VARIATIONS; SELF-ENRICHMENT SCENARIO; NEUTRON-CAPTURE ELEMENTS; COLOR-MAGNITUDE DIAGRAMS AB A combined effort utilizing spectroscopy and photometry has revealed the existence of a new globular cluster class. These "anomalous" clusters, which we refer to as "iron-complex" clusters, are differentiated from normal clusters by exhibiting large (greater than or similar to 0.10 dex) intrinsic metallicity dispersions, complex sub-giant branches, and correlated [Fe/H] and s-process enhancements. In order to further investigate this phenomenon, we have measured radial velocities and chemical abundances for red giant branch stars in the massive, but scarcely studied, globular cluster NGC 6273. The velocities and abundances were determined using high resolution (R similar to 27,000) spectra obtained with the Michigan/Magellan Fiber System (M2FS) and MSpec spectrograph on the Magellan-Clay 6.5 m telescope at Las Campanas Observatory. We find that NGC 6273 has an average heliocentric radial velocity of +144.49 km s(-1) (sigma = 9.64 km s(-1)) and an extended metallicity distribution ([Fe/H] = -1.80 to -1.30) composed of at least two distinct stellar populations. Although the two dominant populations have similar [Na/Fe], [Al/Fe], and [alpha/Fe] abundance patterns, the more metal-rich stars exhibit significant [La/Fe] enhancements. The [La/Eu] data indicate that the increase in [La/Fe] is due to almost pure s-process enrichment. A third more metal-rich population with low [X/Fe] ratios may also be present. Therefore, NGC 6273 joins clusters such as omega Centauri, M2, M22, and NGC 5286 as a new class of iron-complex clusters exhibiting complicated star formation histories. C1 [Johnson, Christian I.; Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Pilachowski, Catherine A.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Mateo, Mario; Bailey, John I., III] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Crane, Jeffrey D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Johnson, CI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-15, Cambridge, MA 02138 USA. EM cjohnson@cfa.harvard.edu; rmr@astro.ucla.edu; catyp@astro.indiana.edu; ncaldwell@cfa.harvard.edu; mmateo@umich.edu; baileyji@umich.edu; crane@obs.carnegiescience.edu OI Pilachowski, Catherine/0000-0002-3007-206X FU National Aeronautics and Space Administration; National Science Foundation [AST-1413755, AST-1412673, AST-0923160]; Clay Fellowship; Daniel Kirkwood Research Fund at Indiana University FX This research has made use of NASA's Astrophysics Data System Bibliographic Services. This publication has made 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 the National Aeronautics and Space Administration and the National Science Foundation. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. R.M.R. acknowledges support from the National Science Foundation (AST-1413755 and AST-1412673). C.A.P. gratefully acknowledges support from the Daniel Kirkwood Research Fund at Indiana University and from the National Science Foundation (AST-1412673). M.M. is grateful for support from the National Science Foundation to develop M2FS (AST-0923160) and carry out the observations reported here (AST-1312997), and to the University of Michigan for its direct support of M2FS construction and operation. NR 176 TC 11 Z9 11 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 AUG PY 2015 VL 150 IS 2 AR 63 DI 10.1088/0004-6256/150/2/63 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900024 ER PT J AU Young, KE Young, CH Lai, SP Dunham, MM Evans, NJ AF Young, Kaisa E. Young, Chadwick H. Lai, Shih-Ping Dunham, Michael M. Evans, Neal J., II TI THE SPITZER c2d SURVEY OF LARGE, NEARBY, INTERSTELLAR CLOUDS. XII. THE PERSEUS YSO POPULATION AS OBSERVED WITH IRAC AND MIPS SO ASTRONOMICAL JOURNAL LA English DT Article DE dust, extinction; infrared: stars; ISM: individual objects (IC 348, NGC 1333 Perseus); stars: formation ID STAR-FORMING REGIONS; 1ST HYDROSTATIC CORE; YOUNG STELLAR POPULATION; MOLECULAR CLOUD; LEGACY CLOUDS; SPACE-TELESCOPE; DISK POPULATION; FORMATION RATES; COLUMN DENSITY; H2O MASERS AB The Spitzer Space Telescope mapped the Perseus molecular cloud complex with the Infrared Array Camera (IRAC) and the Multi-Band Imaging Photometer for Spitzer (MIPS) as part of the c2d Spitzer Legacy project. This paper combines the observations from both instruments giving an overview of low-mass star formation across Perseus from 3.6 to 70 mu m. We provide an updated list of young stellar objects (YSOs) with new classifications and source fluxes from previous works, identifying 369 YSOs in Perseus with the Spitzer data set. By synthesizing the IRAC and MIPS maps of Perseus and building on the work of previous papers in this series, we present a current census of star formation across the cloud and within smaller regions. Sixty-seven percent of the YSOs are associated with the young clusters NGC 1333 and IC 348. The majority of the star formation activity in Perseus occurs in the regions around the clusters to the eastern and western ends of the cloud complex. The middle of the cloud is nearly empty of YSOs despite containing regions of high visual extinction. The western half of Perseus contains three-quarters of the total number of embedded YSOs (Class 0+I and Flat spectral energy distribution sources) in the cloud and nearly as many embedded YSOs as Class II and III sources. Class II and III objects greatly outnumber Class 0+I objects in eastern Perseus and IC 348. These results are consistent with previous age estimates for the clusters. Across the cloud, 56% of YSOs and 91% of the Class 0+I and Flat sources are in areas where A(v) >= 5 mag, indicating a possible extinction threshold for star formation. C1 [Young, Kaisa E.; Young, Chadwick H.] Nicholls State Univ, Dept Phys Sci, Thibodaux, LA 70310 USA. [Lai, Shih-Ping] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Lai, Shih-Ping] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Young, KE (reprint author), Nicholls State Univ, Dept Phys Sci, POB 2022, Thibodaux, LA 70310 USA. EM kaisa.young@nicholls.edu; chad.young@nicholls.edu; slai@phys.nthu.edu.tw; mdunham@cfa.harvard.edu; nje@astro.as.utexas.edu FU Spitzer Legacy Science Program; NASA [1224608, 1230782, 1230779, 1407]; Louisiana Space Consortium Research Enhancement Award through NASA EPSCoR [NNX10AI40H]; Submillimeter Array through an SMA postdoctoral fellowship; National Science Foundation [AST-1109116] FX Support for this work, part of the Spitzer Legacy Science Program, was provided by NASA through contracts 1224608, 1230782, and 1230779 issued by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. K.E.Y. and C.H.Y. acknowledge support from a Louisiana Space Consortium Research Enhancement Award through NASA EPSCoR grant number NNX10AI40H. M.M. D. acknowledges support from the Submillimeter Array through an SMA postdoctoral fellowship. N.J.E. acknowledges support from a grant from the National Science Foundation, AST-1109116. We would like to thank the anonymous referee for comments that improved the focus and clarity of this work. NR 68 TC 8 Z9 8 U1 0 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 AUG PY 2015 VL 150 IS 2 AR 40 DI 10.1088/0004-6256/150/2/40 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0QL UT WOS:000358856900001 ER PT J AU Garcia, JA Dauser, T Steiner, JF McClintock, JE Keck, ML Wilms, J AF Garcia, Javier A. Dauser, Thomas Steiner, James F. McClintock, Jeffrey E. Keck, Mason L. Wilms, Joern TI ON ESTIMATING THE HIGH-ENERGY CUTOFF IN THE X-RAY SPECTRA OF BLACK HOLES VIA REFLECTION SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; atomic processes; black hole physics ID ACCRETION DISK; COMPTONIZATION MODELS; NUSTAR; LINE; GALAXIES; SPIN; OSSE AB The fundamental parameters describing the coronal spectrum of an accreting black hole are the slope Gamma of the power-law continuum and the energy E-cut at which it rolls over. Remarkably, this latter parameter can be accurately measured for values as high as 1 MeV by modeling the spectrum of X-rays reflected from a black hole accretion disk at energies below 100 keV. This is possible because the details in the reflection spectrum, rich in fluorescent lines and other atomic features, are very sensitive to the spectral shape of the hardest coronal radiation illuminating the disk. We show that by fitting simultaneous NuSTAR (3-79 keV) and low-energy (e.g., Suzaku) data with the most recent version of our reflection model relxill one can obtain reasonable constraints on E-cut at energies from tens of keV up to 1 MeV, for a source as faint as 1 mCrab in a 100 ks observation. C1 [Garcia, Javier A.; Steiner, James F.; McClintock, Jeffrey E.; Keck, Mason L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dauser, Thomas; Wilms, Joern] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, Thomas; Wilms, Joern] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Keck, Mason L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. RP Garcia, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; thomas.dauser@sternwarte.uni-erlangen.de; jsteiner@head.cfa.harvard.edu; keckm@bu.edu RI Wilms, Joern/C-8116-2013; XRAY, SUZAKU/A-1808-2009; OI Wilms, Joern/0000-0003-2065-5410; Garcia, Javier/0000-0003-3828-2448 FU NASA [NNX11AD08G, HST-HF-51315.01] FX J.G. and J.E.M. acknowledge the support of NASA grant NNX11AD08G. J.F.S. has been supported by NASA Hubble Fellowship HST-HF-51315.01. NR 32 TC 7 Z9 7 U1 0 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 AUG 1 PY 2015 VL 808 IS 2 AR L37 DI 10.1088/2041-8205/808/2/L37 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1TS UT WOS:000358938800005 ER PT J AU Lee, PC Wildt, DE Comizzoli, P AF Lee, Pei-Chih Wildt, David E. Comizzoli, Pierre TI Nucleolar Translocation of Histone Deacetylase 2 Is Involved in Regulation of Transcriptional Silencing in the Cat Germinal Vesicle SO BIOLOGY OF REPRODUCTION LA English DT Article DE domestic cat; gamete biology; germinal vesicle; oocyte; transcription ID IN-VITRO MATURATION; DEVELOPMENTAL COMPETENCE; OOCYTE GROWTH; CHROMATIN CONFIGURATIONS; MEIOTIC COMPETENCE; BOVINE OOCYTES; MOUSE OOCYTES; DOMESTIC CAT; FERTILITY PRESERVATION; RIBOSOME BIOGENESIS AB Histone deacetylase 2 (HDAC2) is a key transcriptional coregulator that is suspected to play a role during oogenesis. It is known that RNA transcription in the cat germinal vesicle (GV) stops during folliculogenesis at the late antral follicle stage and is unrelated to histone deacetylation or chromatin condensation. The objective of the present study was to determine if and how HDAC2 participates in transcription regulation in the cat GV. Spatiotemporal HDAC2 protein expression was examined by immunostaining oocytes from primary to large antral follicles. HDAC2 was detected in the majority of GVs within oocytes from early, small, and large antral follicles. At early and small antral stages, HDAC2 was found primarily in the GV's nucleoplasm. There then was a significant shift in HDAC2 localization into the nucleolus, mostly in oocytes from large antral follicles. Assessments revealed that transcription was active in oocytes that contained nucleoplasm-localized HDAC2, whereas nucleolar-bound HDAC2 was associated with loss of both global transcription and ribosomal RNA presence at all antral stages. When oocytes were exposed to the HDAC inhibitor valproic acid, results indicated that HDAC regulated transcriptional activity in the nucleoplasm, but not in the nucleolus. Collective results suggest that nucleolar translocation of HDAC2 is associated with transcriptional silencing in the GV, thereby likely contributing to an oocyte's acquisition of competence. C1 Smithsonian Conservat Biol Inst, Ctr Species Survival, Washington, DC 20013 USA. Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. RP Comizzoli, P (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012,MRC 5502, Washington, DC 20013 USA. EM comizzolip@si.edu FU National Center for Research Resources, a component of the National Institutes of Health (NIH) [R01 RR026064]; Office of Research Infrastructure Programs/Office of the Director [R01 OD010948] FX Supported by the National Center for Research Resources (R01 RR026064), a component of the National Institutes of Health (NIH), and currently by the Office of Research Infrastructure Programs/Office of the Director (R01 OD010948). NR 61 TC 3 Z9 3 U1 2 U2 5 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 EI 1529-7268 J9 BIOL REPROD JI Biol. Reprod. PD AUG 1 PY 2015 VL 93 IS 2 AR 33 DI 10.1095/biolreprod.115.129106 PG 9 WC Reproductive Biology SC Reproductive Biology GA CO8UT UT WOS:000359448300008 PM 26108793 ER PT J AU Jacquet, J Estes, J Jackson, J Johnson, AE Knowlton, N Mcclenachan, L Pauly, D Sala, E AF Jacquet, Jennifer Estes, James Jackson, Jeremy Johnson, Ayana E. Knowlton, Nancy Mcclenachan, Loren Pauly, Daniel Sala, Enric TI Ocean Calamities: Hyped Litany or Legitimate Concern? SO BIOSCIENCE LA English DT Letter ID EUTROPHICATION; FISHERIES C1 [Jacquet, Jennifer] NYU, Dept Environm Studies, New York, NY 10003 USA. [Estes, James] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Jackson, Jeremy] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Jackson, Jeremy] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA. [Johnson, Ayana E.] Waitt Inst, Washington, DC USA. [Knowlton, Nancy] Natl Museum Nat Hist, Washington, DC 20560 USA. [Mcclenachan, Loren] Colby Coll, Dept Environm Studies, Waterville, ME 04901 USA. [Pauly, Daniel] Univ British Columbia, Sea Us, Vancouver, BC V5Z 1M9, Canada. [Sala, Enric] Natl Geog Soc, Washington, DC USA. RP Jacquet, J (reprint author), NYU, Dept Environm Studies, New York, NY 10003 USA. EM jacquet@nyu.edu NR 8 TC 2 Z9 2 U1 4 U2 29 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 AUG PY 2015 VL 65 IS 8 BP 745 EP 746 DI 10.1093/biosci/biv087 PG 2 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CO5FA UT WOS:000359183800002 ER PT J AU Pistone, M Arzilli, F Dobson, KJ Cordonnier, B Reusser, E Ulmer, P Marone, F Whittington, AG Mancini, L Fife, JL Blundy, JD AF Pistone, Mattia Arzilli, Fabio Dobson, Katherine J. Cordonnier, Benoit Reusser, Eric Ulmer, Peter Marone, Federica Whittington, Alan G. Mancini, Lucia Fife, Julie L. Blundy, Jonathan D. TI Gas-driven filter pressing in magmas: Insights into in-situ melt segregation from crystal mushes SO GEOLOGY LA English DT Article ID GENERATION; RHEOLOGY; SYSTEM AB Gas-driven filter pressing is the process of melt expulsion from a volatile-saturated crystal mush, induced by the buildup and subsequent release of gas pressure. Filter pressing is inferred to play a major role in magma fractionation at shallow depths (<10 km) by moving melt and gas relative to the solid, crystalline framework. However, the magmatic conditions at which this process operates remain poorly constrained. We present novel experimental data that illustrate how the crystal content of the mush affects the ability of gas-driven filter pressing to segregate melt. Hydrous haplogranite (2.1 wt% water in the melt) and dacite (4.2 wt% water in the melt) crystal mushes, with a wide range of crystallinities (34-80 vol% crystals), were investigated using in-situ, high-temperature (500-800 degrees C) synchrotron X-ray tomographic microscopy with high spatial (3 mm/pixel) and temporal resolution (similar to 8 s per three-dimensional data set). Our experimental results show that gas-driven filter pressing operates only below the maximum packing of bubbles and crystals (similar to 74 vol%). Above this threshold, the mush tends to fracture and gas escapes via fractures. Therefore, the efficiency of gas-driven filter pressing is promoted close to the percolation threshold and in situations where a mush inflates slowly relative to build-up of pressure and expulsion of melt. Such observations offer a likely explanation for the production of eruptible, crystal-poor magmas within Earth's crust. C1 [Pistone, Mattia] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Pistone, Mattia; Blundy, Jonathan D.] Univ Bristol, Sch Earth Sci, Bristol BS8 1RJ, Avon, England. [Arzilli, Fabio; Mancini, Lucia] Elettra Sincrotrone Trieste SCpA, I-34149 Basovizza, Italy. [Arzilli, Fabio] Ist Nazl Geofis & Vulcanol, Sez Pisa, I-56126 Pisa, Italy. [Dobson, Katherine J.] Univ Munich, Dept Earth & Environm Sci, D-80333 Munich, Germany. [Reusser, Eric; Ulmer, Peter] ETH, Dept Earth Sci, CH-8092 Zurich, Switzerland. [Marone, Federica; Fife, Julie L.] Paul Scherrer Inst, Swiss Light Source, CH-5232 Villigen, Switzerland. [Whittington, Alan G.] Univ Missouri, Dept Geol Sci, Geol Sci 101, Columbia, MO 65211 USA. RP Pistone, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th St & Constitut Ave NW, Washington, DC 20560 USA. RI Marone, Federica/J-4420-2013; Dobson, Katherine/I-1223-2016; OI Dobson, Katherine/0000-0003-2272-626X; Mancini, Lucia/0000-0003-2416-3464; Pistone, Mattia/0000-0001-7560-3146 FU EU Transnational Access Programme (CALIPSO) [312284]; European Research Council Advanced Grant CRITMAG; EXTREMA European Cooperation in Science and Technology (COST) Action [MP1207] FX The EU Transnational Access Programme (CALIPSO; number 312284; FP7/2007-2013), the European Research Council Advanced Grant CRITMAG, and EXTREMA European Cooperation in Science and Technology (COST) Action MP1207 supported the work. We acknowledge C. Clapham, D. Hawley, U. Graber, G. Mikuljan, and G. Robert for technical support; D. Baker, M. Polacci, L. Caricchi, and D. Giordano for discussions; and R. Holdsworth, D. Floess, and two anonymous reviewers for their helpful comments. NR 18 TC 16 Z9 16 U1 1 U2 12 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 AUG PY 2015 VL 43 IS 8 BP 699 EP 702 DI 10.1130/G36766.1 PG 4 WC Geology SC Geology GA CO2VK UT WOS:000359014600011 ER PT J AU Bayer, FM Cairns, SD Cordeiro, RTS Perez, CD AF Bayer, Frederick M. Cairns, Stephen D. Cordeiro, Ralf T. S. Perez, Carlos D. TI New records of the genus Callogorgia (Anthozoa: Octocorallia) in the western Atlantic, including the description of a new species SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE Deep-water corals; octocorals; Primnoidae; south Atlantic; Cnidaria; continental slope ID GULF-OF-MEXICO; DEEP; SEA AB Based on material collected during oceanographic campaigns in the western Atlantic from 1958 to 2011, two species of primnoid octocorals belonging to the genus Callogorgia were identified: Callogorgia americana and Callogorgia arawak sp. nov. These species are described and illustrated herein and their geographic and bathymetric are given. This is the first record of the genus in the south-western Atlantic. Additionally, the elevation of C. americana americana and C. a. delta to species level is proposed, keeping Callogorgia gilberti, C. delta and C. americana as separate species. C1 [Bayer, Frederick M.; Cairns, Stephen D.] Natl Museum Nat Hist, Smithsonian, Dept Invertebrate Zool, Washington, DC 20560 USA. [Cordeiro, Ralf T. S.] Univ Fed Pernambuco, Posgrad Biol Anim, BR-50670901 Recife, PE, Brazil. [Perez, Carlos D.] Univ Fed Pernambuco, Ctr Acad Vitoria, BR-55608680 Bela Vista, Vitoria de Sant, Brazil. RP Cordeiro, RTS (reprint author), Univ Fed Pernambuco, Posgrad Biol Anim, BR-50670901 Recife, PE, Brazil. EM ralfts@gmail.com FU CNPq - Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [Edital PROTAX 2010 - 562320/2010-5]; FACEPE - Fundacao de Amparo a Ciencia e Tecnologia do Estado de Pernambuco [APQ-0828-2.04/12] FX The work was supported by CNPq - Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (Grant - Edital PROTAX 2010 - 562320/2010-5) and FACEPE - Fundacao de Amparo a Ciencia e Tecnologia do Estado de Pernambuco (Grant - APQ-0828-2.04/12). NR 16 TC 3 Z9 3 U1 1 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD AUG PY 2015 VL 95 IS 5 BP 905 EP 911 DI 10.1017/S0025315414001957 PG 7 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CO0NJ UT WOS:000358848400005 ER PT J AU Beck, AW Lawrence, DJ Peplowski, PN Prettyman, TH McCoy, TJ McSween, HY Toplis, MJ Yamashita, N AF Beck, Andrew W. Lawrence, David J. Peplowski, Patrick N. Prettyman, Thomas H. McCoy, Timothy J. McSween, Harry Y., Jr. Toplis, Michael J. Yamashita, Naoyuki TI Using HED meteorites to interpret neutron and gamma-ray data from asteroid4 Vesta SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DAWN MISSION; COLLISIONAL HISTORY; POLYMICT BRECCIAS; LUNAR-SURFACE; PARENT BODY; CONSTRAINTS; HOWARDITE; EUCRITE; CRYSTALLIZATION; SPECTROMETER AB Here, we construct a comprehensive howardite, eucrite, and diogenite (HED) bulk chemistry data set to compare with Dawn data. Using the bulk chemistry data set, we determine four gamma-ray/neutron parameters in the HEDs (1) relative fast neutron counts (fast counts), (2) macroscopic thermal neutron absorption cross section (absorption), (3) a high-energy gamma-ray compositional parameter (C-p), and (4) Fe abundance. These correspond to the four measurements of Vesta made by Dawn's Gamma Ray and Neutron Detector (GRaND) that can be used to discern HED lithologic variability on the Vestan surface. We investigate covariance between fast counts and average atomic mass (< A >) in the meteorite data set, where a strong correlation (r(2)=0.99) is observed, and we demonstrate that systematic offsets from the fast count/< A > trend are linked to changes in Fe and Ni concentrations. To compare the meteorite and GRaND data, we investigate and report covariance among fast counts, absorption, C-p, and Fe abundance in the HED meteorite data set. We identify several GRaND measurement spaces where the Yamato type B diogenites are distinct from all other HED lithologies, including polymict mixtures. The type B's are diogenites that are enriched in Fe+pigeonite+diopside +/- plagioclase, relative to typical, orthopyroxenitic diogenites. We then compare these results to GRaND data and demonstrate that regions north of similar to 70 degrees N latitude on Vesta (including the north pole) are consistent with type B diogenites. We propose two models to explain type B diogenite compositions in the north (1) deposition as Rheasilvia ejecta, or (2) type B plutons that were emplaced at shallow depths in the north polar region and sampled by local impacts. Lastly, using principal component (PC) analysis, we identify unique PC spaces for all HED lithologies, indicating that the corresponding GRaND measurables may be used to produce comprehensive lithologic maps for Vesta. C1 [Beck, Andrew W.; Lawrence, David J.; Peplowski, Patrick N.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Prettyman, Thomas H.; Yamashita, Naoyuki] Planetary Sci Inst, Tucson, AZ 85719 USA. [McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [McSween, Harry Y., Jr.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Toplis, Michael J.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Toplis, Michael J.] IRAP, CNRS, F-31400 Toulouse, France. RP Beck, AW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Johns Hopkins Rd, Laurel, MD 20723 USA. EM andrew.beck@jhuapl.edu RI Beck, Andrew/J-7215-2015; Peplowski, Patrick/I-7254-2012; Lawrence, David/E-7463-2015; OI Beck, Andrew/0000-0003-4455-2299; Peplowski, Patrick/0000-0001-7154-8143; Lawrence, David/0000-0002-7696-6667; Prettyman, Thomas/0000-0003-0072-2831 FU NASA Discovery Program Office; Dawn at Vesta participating scientist grants FX The Dawn mission is led by the University of California, Los Angeles, and managed by the Jet Propulsion Laboratory (JPL), Pasadena, California under the auspices of the NASA Discovery Program Office. Support for this work was provided by Dawn at Vesta participating scientist grants to DJL and TJM, work by HYM and THP was carried out under contract with the NASA JPL. We thank Christina Viviano-Beck for her help with IDL programming. We also thank Andy Tindle for the use of his element to oxide software, and Nicole Lunning and Sheri Singerling for their assistance in compiling HED data. This manuscript was significantly improved by comments from the reviewer, Tomohiro Usui. NR 59 TC 8 Z9 8 U1 3 U2 7 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 AUG PY 2015 VL 50 IS 8 BP 1311 EP 1337 DI 10.1111/maps.12467 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CO7QW UT WOS:000359356900001 ER PT J AU Corrigan, CM Lunning, NG Friedrich, JM McCoy, TJ AF Corrigan, C. M. Lunning, N. G. Friedrich, J. M. McCoy, T. J. TI AN H CHONDRITE CLAST IN AN LL CHONDRITE: IMPACT MELT OR INCIPIENT PARTIAL MELT? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Corrigan, C. M.; McCoy, T. J.] NMNH, Smithsonian Inst, Washington, DC 20560 USA. [Lunning, N. G.] Univ Tennessee, Knoxville, TN 37996 USA. [Friedrich, J. M.] Fordham Univ, New York, NY 10023 USA. EM corriganc@si.edu NR 18 TC 0 Z9 0 U1 1 U2 1 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 AUG PY 2015 VL 50 SU 1 SI SI MA 5283.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900067 ER PT J AU Kita, NT Tenner, TJ Ushikubo, T Bouvier, A Wadhwa, M Bullock, ES MacPherson, GJ AF Kita, N. T. Tenner, T. J. Ushikubo, T. Bouvier, A. Wadhwa, M. Bullock, E. S. MacPherson, G. J. TI WHY DO U-PB AGES OF CHONDRULES AND CAIs HAVE MORE SPREAD THAN THEIR (26)AL AGES? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab ID SOLAR PROTOPLANETARY DISK C1 [Kita, N. T.; Tenner, T. J.] Univ Wisconsin, Madison, WI 53706 USA. [Ushikubo, T.] JAMSTEC, Kochi 7838502, Japan. [Bouvier, A.] Univ Western Ontario, London, ON N6A 3K7, Canada. [Wadhwa, M.] Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ 85287 USA. [Bullock, E. S.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA. EM noriko@geology.wisc.edu NR 10 TC 0 Z9 0 U1 1 U2 2 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 AUG PY 2015 VL 50 SU 1 SI SI MA 5360.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900166 ER PT J AU Mayne, RG Mccoy, TJ AF Mayne, R. G. McCoy, T. J. TI PALLASITES: DOES DENSITY MATTER AFTER ALL? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Mayne, R. G.] Texas Christian Univ, Monnig Meteorite Collect, Ft Worth, TX 76109 USA. [McCoy, T. J.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. EM r.g.mayne@tcu.edu NR 6 TC 0 Z9 0 U1 2 U2 2 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 AUG PY 2015 VL 50 SU 1 SI SI MA 5222.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900214 ER PT J AU McCoy, TJ Bullock, ES AF McCoy, T. J. Bullock, E. S. TI VOLATILE-RICH PHASES IN AUBRITES: CLUES TO UNDERSTANDING THE MINERALOGY OF MERCURY? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [McCoy, T. J.; Bullock, E. S.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Bullock, E. S.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. NR 9 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 AUG PY 2015 VL 50 SU 1 SI SI MA 5280.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900215 ER PT J AU Sanborn, ME Yin, QZ Schrader, DL AF Sanborn, M. E. Yin, Q-Z Schrader, D. L. TI AQUEOUS ALTERATION AND ITS EFFECT ON epsilon Cr-54: AN INVESTIGATION OF CR1 AND CR2 CHONDRITES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 78th Annual Meeting of the Meteoritical-Society CY JUL 27-31, 2015 CL Berkeley, CA SP Meteorit Soc, Barringer Crater Co, Natl Aeronaut & Space Adm, Inst Space & Astronaut Sci, Japan Aerosp Explorat Agcy, Japan Polar Res Assoc, Natl Inst Polar Res, NASA Mars Program Off, Agilent Technologies, CAMECA, Lockheed Martin Space Syst Co, Natl Electrostat Corp, TESCAN, Int Meteorite Collectors Assoc, Planetary Studies Fdn, Lunar & Planetary Inst, Univ Calif, Space Sci Lab C1 [Sanborn, M. E.; Yin, Q-Z] Univ Calif Davis, Dept Earth & Planetary Sci, Davis, CA 95616 USA. [Schrader, D. L.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. [Schrader, D. L.] Arizona State Univ, SESE, Tempe, AZ 85281 USA. EM mesanborn@ucdavis.edu NR 8 TC 0 Z9 0 U1 1 U2 2 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 AUG PY 2015 VL 50 SU 1 SI SI MA 5157.pdf PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN7CR UT WOS:000358591900286 ER PT J AU Pikovski, I Zych, M Costa, F Brukner, C AF Pikovski, Igor Zych, Magdalena Costa, Fabio Brukner, Caslav TI Universal decoherence due to gravitational time dilation SO NATURE PHYSICS LA English DT Article ID SPIN BATH; QUANTUM; PARTICLES; GRAVITY; INTERFERENCE; REDUCTION; DYNAMICS; CLOCKS; OPTICS; MODELS AB The physics of low-energy quantum systems is usually studied without explicit consideration of the background spacetime. Phenomena inherent to quantum theory in curved spacetime, such as Hawking radiation, are typically assumed to be relevant only for extreme physical conditions: at high energies and in strong gravitational fields. Here we consider low-energy quantum mechanics in the presence of gravitational time dilation and show that the latter leads to the decoherence of quantum superpositions. Time dilation induces a universal coupling between the internal degrees of freedom and the centre of mass of a composite particle. The resulting correlations lead to decoherence in the particle position, even without any external environment. We also show that the weak time dilation on Earth is already sufficient to affect micrometre-scale objects. Gravity can therefore account for the emergence of classicality and this effect could in principle be tested in future matter-wave experiments. C1 [Pikovski, Igor; Zych, Magdalena; Costa, Fabio; Brukner, Caslav] Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, A-1090 Vienna, Austria. [Pikovski, Igor; Zych, Magdalena; Costa, Fabio; Brukner, Caslav] Austrian Acad Sci, IQOQI, A-1090 Vienna, Austria. [Pikovski, Igor] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Pikovski, Igor] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Zych, Magdalena; Costa, Fabio] Univ Queensland, Sch Math & Phys, Ctr Engn Quantum Syst, St Lucia, Qld 4072, Australia. RP Pikovski, I (reprint author), Univ Vienna, Fac Phys, Vienna Ctr Quantum Sci & Technol VCQ, Boltzmanngasse 5, A-1090 Vienna, Austria. EM igor.pikovski@cfa.harvard.edu RI Zych, Magdalena/G-4007-2014; Costa, Fabio/G-3746-2014; OI Zych, Magdalena/0000-0002-8356-7613; Costa, Fabio/0000-0002-6547-6005; Pikovski, Igor/0000-0002-9441-2553 FU Austrian Science Fund (FWF) through the doctoral program Complex Quantum Systems (CoQuS); Vienna Center for Quantum Science and Technology (VCQ); SFB FoQuS; Foundational Questions Institute (FQXi); John Templeton Foundation; Australian Research Council Centre of Excellence for Engineered Quantum Systems [CE110001013]; European Commission through RAQUEL [323970]; COST Action [MP1209]; [24621] FX We thank M. Arndt, M. Aspelmeyer, L. Diosi and M. Vanner for discussions and S. Eibenberger for providing us with the illustration of the TPPF20 molecule. This work was supported by the Austrian Science Fund (FWF) through the doctoral program Complex Quantum Systems (CoQuS), the Vienna Center for Quantum Science and Technology (VCQ), the SFB FoQuS and the Individual Project 24621, by the Foundational Questions Institute (FQXi), the John Templeton Foundation, the Australian Research Council Centre of Excellence for Engineered Quantum Systems (grant number CE110001013), the European Commission through RAQUEL (No. 323970) and the COST Action MP1209. NR 32 TC 25 Z9 25 U1 5 U2 23 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1745-2473 EI 1745-2481 J9 NAT PHYS JI Nat. Phys. PD AUG PY 2015 VL 11 IS 8 BP 668 EP + DI 10.1038/NPHYS3366 PG 7 WC Physics, Multidisciplinary SC Physics GA CO0OQ UT WOS:000358851900021 ER PT J AU Marques, AC Garcia, J Ames, CL AF Marques, Antonio Carlos Garcia, Jimena Ames, Cheryl Lewis TI Internal fertilization and sperm storage in cnidarians: a response to Orr and Brennan SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter DE copulation; box jellyfish; Cubozoa; plankton ID CARYBDEA-SIVICKISI; REPRODUCTION; EVOLUTION; BEHAVIOR; CUBOZOA C1 [Marques, Antonio Carlos; Garcia, Jimena] Univ Sao Paulo, Inst Biosci, BR-05508090 Sao Paulo, Brazil. [Marques, Antonio Carlos; Garcia, Jimena] Univ Sao Paulo, Ctr Marine Biol, BR-05508090 Sao Paulo, Brazil. [Marques, Antonio Carlos] Univ Sao Paulo, Ctr Marine Biol, BR-11600000 Sao Paulo, Brazil. [Ames, Cheryl Lewis] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Ames, Cheryl Lewis] Univ Maryland, Biol Sci Grad Program, BEES Concentrat, College Pk, MD 20742 USA. RP Marques, AC (reprint author), Univ Sao Paulo, Inst Biosci, R Matao Tr 14, BR-05508090 Sao Paulo, Brazil. EM marques@ib.usp.br RI Marques, Antonio/E-8049-2011 OI Marques, Antonio/0000-0002-2884-0541 NR 11 TC 2 Z9 2 U1 1 U2 25 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 AUG PY 2015 VL 30 IS 8 BP 435 EP 436 DI 10.1016/j.tree.2015.06.002 PG 2 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CO7GX UT WOS:000359328700001 PM 26115932 ER PT J AU Fugere, V O'Mara, MT Page, RA AF Fugere, Vincent Teague O'Mara, M. Page, Rachel A. TI Perceptual bias does not explain preference for prey call adornment in the frog-eating bat SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Eavesdropping; Perceptual bias; Receiver bias; Prey detection; Predator-prey interaction; Fringe-lipped bat; Tungara frog ID FEMALE MATE CHOICE; TRACHOPS-CIRRHOSUS; SEXUAL SELECTION; MATING SIGNALS; TUNGARA FROGS; LOCALIZATION PERFORMANCE; PHYSALAEMUS-PUSTULOSUS; EAVESDROPPING BAT; FORAGING BEHAVIOR; SENSORY ECOLOGY AB Eavesdropping predators sometimes show preferences for certain prey signal variants, yet the ultimate and proximate reasons for such preferences are often unclear. The fringe-lipped bat, Trachops cirrhosus, eavesdrops on the advertisement calls of male tA(0)ngara frogs, Physalaemus pustulosus, and shows a marked preference for complex (adorned) calls over simple (non-adorned) calls. We hypothesized that this preference stems from perceptual biases in the sensory and/or cognitive systems of T. cirrhosus. To test this hypothesis, we conducted a series of preference experiments in which we presented bats with various modified simple calls, each altered to possess one of the acoustic properties that distinguish complex calls from simple calls. We reasoned that if perceptual bias accounts for the bat's preference for complex calls, then a novel stimulus with similar acoustic properties to the complex call should be attractive as well (i.e., the preference should be permissive). Except for weak evidence suggesting that the longer duration of complex calls could contribute to their greater attractiveness to T. cirrhosus, we did not find any indication that perceptual biases account for this eavesdropper preference. Instead, we suggest that T. cirrhosus developed their preference for call complexity because eavesdropping on complex calls provides greater fitness benefits than eavesdropping on simple calls, for example, because eavesdropping on complex calls may increase probability of prey capture and/or lead to more profitable food patches. C1 [Fugere, Vincent] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Fugere, Vincent; Teague O'Mara, M.; Page, Rachel A.] Smithsonian Trop Res Inst, Balboa Ancon 03092, Panama. [Teague O'Mara, M.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Teague O'Mara, M.] Univ Konstanz, Dept Biol & Zukunftskolleg, Constance, Germany. RP Fugere, V (reprint author), McGill Univ, Dept Biol, 1205 Ave Docteur Penfield, Montreal, PQ H3A 1B1, Canada. EM vincent.fugere@mail.mcgill.ca OI O'Mara, M. Teague/0000-0002-6951-1648 FU Smithsonian Tropical Research Institute; Fonds de Recherche du Qurbec-Nature et Technologies; Natural Sciences and Engineering Research Council of Canada; Vanier Canada Graduate Fellowship Program FX The authors would like to thank the government of the Republic of Panama for their permission to work in Gamboa and Soberania National Park and the Smithsonian Tropical Research Institute for providing critical logistical support and infrastructure. Sara Troxell, Sean Griffin, Martha Moscoso, and Patricia Jones helped with capturing and caring for bats. The authors are also grateful to Michael J. Ryan for supplying the tungara frog recordings and to Ximena Bernal, Patricia Jones, Michael Caldwell, Michael J. Ryan, Christian Voigt, Gloriana Chaverri, and two anonymous reviewers for their constructive comments on previous versions of the manuscript. This study was supported by the Smithsonian Tropical Research Institute, the Fonds de Recherche du Qurbec-Nature et Technologies, the Natural Sciences and Engineering Research Council of Canada, and the Vanier Canada Graduate Fellowship Program. NR 62 TC 1 Z9 1 U1 2 U2 21 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-5443 EI 1432-0762 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD AUG PY 2015 VL 69 IS 8 BP 1353 EP 1364 DI 10.1007/s00265-015-1949-2 PG 12 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA CN8ZK UT WOS:000358734700012 ER PT J AU Wurzburger, N Wright, SJ AF Wurzburger, Nina Wright, S. Joseph TI Fine-root responses to fertilization reveal multiple nutrient limitation in a lowland tropical forest SO ECOLOGY LA English DT Article DE Barro Colorado Nature Monument, Panama; fine roots; mycorrhizal fungi; nitrogen; phosphorus; potassium; root functional traits; specific root length; tissue density; tropical forest ID ARBUSCULAR MYCORRHIZAL FUNGI; RAIN-FOREST; PHOSPHORUS LIMITATION; TREE GROWTH; POTASSIUM ADDITION; SOIL NUTRIENTS; NITROGEN; TRAITS; DYNAMICS; PATTERNS AB Questions remain as to which soil nutrients limit primary production in tropical forests. Phosphorus (P) has long been considered the primary limiting element in lowland forests, but recent evidence demonstrates substantial heterogeneity in response to nutrient addition, highlighting a need to understand and diagnose nutrient limitation across diverse forests. Fine-root characteristics including their abundance, functional traits, and mycorrhizal symbionts can be highly responsive to changes in soil nutrients and may help to diagnose nutrient limitation. Here, we document the response of fine roots to long-term nitrogen (N), P, and potassium (K) fertilization in a lowland forest in Panama. Because this experiment has demonstrated that N and K together limit tree growth and P limits fine litter production, we hypothesized that fine roots would also respond to nutrient addition. Specifically we hypothesized that N, P, and K addition would reduce the biomass, diameter, tissue density, and mycorrhizal colonization of fine roots, and increase nutrient concentration in root tissue. Most morphological root traits responded to the single addition of K and the paired addition of N and P, with the greatest response to all three nutrients combined. The addition of N, P, and K together reduced fine-root biomass, length, and tissue density, and increased specific root length, whereas root diameter remained unchanged. Nitrogen addition did not alter root N concentration, but P and K addition increased root P and K concentration, respectively. Mycorrhizal colonization of fine roots declined with N, increased with P, and was unresponsive to K addition. Although plant species composition remains unchanged after 14 years of fertilization, fine-root characteristics responded to N, P, and K addition, providing some of the strongest stand-level responses in this experiment. Multiple soil nutrients regulate fine-root abundance, morphological and chemical traits, and their association with mycorrhizal fungi in a species-rich lowland tropical forest. C1 [Wurzburger, Nina] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. RP Wurzburger, N (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. EM ninawurz@uga.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU University of Georgia; Odum School of Ecology; Smithsonian Tropical Research Institute FX This study was funded by the University of Georgia, the Odum School of Ecology and the Smithsonian Tropical Research Institute. We gratefully acknowledge Courtney Collins, Kelly Andersen, and Rufino Gonzalez for their assistance in the field; Shialoh Wilson, Tierney O'Sullivan, and Brice Howell for assistance in the laboratory; and Sarah Batterman and Lars Hedin for their assistance and support during a pilot study that led to this work. We thank two anonymous reviewers for their constructive comments on the manuscript. NR 61 TC 9 Z9 9 U1 12 U2 87 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD AUG PY 2015 VL 96 IS 8 BP 2137 EP 2146 DI 10.1890/14-1362.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CN5FF UT WOS:000358454500012 PM 26405739 ER PT J AU Touchon, JC McCoy, MW Landberg, T Vonesh, JR Warkentin, KM AF Touchon, Justin C. McCoy, Michael W. Landberg, Tobias Vonesh, James R. Warkentin, Karen M. TI Putting mu/g in a new light: plasticity in life history switch points reflects fine-scale adaptive responses SO ECOLOGY LA English DT Article DE Agalychnis callidryas; Anura; growth; life history switch point; mesocosm experiment; mortality; Neotropical treefrog; phenotypic plasticity; predator-induced variation; Smithsonian Tropical Research Institute, Gamboa, Panama; timing of metamorphosis ID RED-EYED TREEFROG; INDUCED PHENOTYPIC PLASTICITY; PREDATION RISK; TRADE-OFFS; DEVELOPMENTAL PLASTICITY; AMPHIBIAN METAMORPHOSIS; HATCHING AGE; REEF FISHES; GROWTH-RATE; PREY AB Life history theory predicts that organisms with complex life cycles should transition between life stages when the ratio of growth rate (g) to risk of mortality (mu) in the current stage falls below that in the subsequent stage. Empirical support for this idea has been mixed. Implicit in both theory and empirical work is that the risk of mortality in the subsequent stage is unknown. However, some embryos and larvae of both vertebrates and invertebrates assess cues of post-transition predation risk and alter the timing of hatching or metamorphosis accordingly. Furthermore, although life history switch points of prey have traditionally been treated as discrete shifts in morphology or habitat, for many organisms they are continuous transitional periods within which the timing of specific developmental and behavioral events can be plastic. We studied red-eyed treefrogs (Agalychnis callidryas), which detect predators of both larvae and metamorphs, to test if plastic changes during the process of metamorphosis could reconcile the mismatch between life history theory and empirical data and if plasticity in an earlier stage transition (hatching) would affect plasticity at a subsequent stage transition (metamorphosis). We reared tadpoles from hatching until metamorphosis in a full-factorial cross of two hatching ages (early-vs. late-hatched) and the presence or absence of free-roaming predators of larvae (giant water bugs) and metamorphs (fishing spiders). Hatching age affected the times from oviposition to tail resorption and from hatching to emergence onto land, but did not alter responses to predators or developmental stage at emergence. Tadpoles did not alter their age at emergence or tail resorption in response to larval or metamorph predators, despite the fact that predators reduced tadpole density by similar to 30%. However, developmental stage at emergence and time needed to complete metamorphosis in the terrestrial environment were plastic and consistent with predictions of the "minimize mu/g'' framework. Our results demonstrate that likely adaptive changes in life history transitions occur at previously unappreciated timescales. Consideration of plasticity in the developmental timing of ecologically important events within metamorphosis, rather than treating it as a discrete switch point, may help to reconcile inconsistencies between empirical studies of predator effects and expectations of long-standing ecological theory. C1 [Touchon, Justin C.] Vassar Coll, Dept Biol, Poughkeepsie, NY 12604 USA. [Touchon, Justin C.; McCoy, Michael W.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. [Landberg, Tobias] Arcadia Univ, Dept Biol, Glenside, PA 19038 USA. [Landberg, Tobias; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. RP Touchon, JC (reprint author), Vassar Coll, Dept Biol, 124 Raymond Ave, Poughkeepsie, NY 12604 USA. EM jutouchon@vassar.edu RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU National Science Foundation [DEB-0717220, DEB-0716923]; Boston University; Virginia Commonwealth University; East Carolina University; STRI FX We thank the Smithsonian Tropical Research Institute (STRI) for logistical support and the Autoridad Nacional del Ambiente de Panama for research permit SC/A-16-10. This research was conducted under Boston University IACUC protocol #08-011. We thank S. Bouchard, J. Charbonnier, Z. Costa, K. Cohen, R. Greene, C. Jenney, C. Noss, M. Palmer, S. Schleier, and B. Willink for assistance with the experiment and two anonymous reviewers for helpful comments on the manuscript. This research was funded by the National Science Foundation (DEB-0717220 to J. R. Vonesh and DEB-0716923 to K. M. Warkentin), Boston University, Virginia Commonwealth University, East Carolina University, and STRI. NR 54 TC 1 Z9 1 U1 5 U2 24 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD AUG PY 2015 VL 96 IS 8 BP 2192 EP 2202 DI 10.1890/14-1301.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CN5FF UT WOS:000358454500017 PM 26405744 ER PT J AU Carmichael, SK Zorn, BT Santelli, CM Roble, LA Carmichael, MJ Brauer, SL AF Carmichael, Sarah K. Zorn, Bryan T. Santelli, Cara M. Roble, Leigh A. Carmichael, Mary J. Braeuer, Suzanna L. TI Nutrient input influences fungal community composition and size and can stimulate manganese (II) oxidation in caves SO ENVIRONMENTAL MICROBIOLOGY REPORTS LA English DT Article ID COAL-MINE DRAINAGE; SP STRAIN KR21-2; MICROBIAL DIVERSITY; LASCAUX CAVE; MN(II) OXIDATION; MOLECULAR-IDENTIFICATION; KARTCHNER CAVERNS; LECHUGUILLA CAVE; QUANTITATIVE PCR; DESERT VARNISH AB Little is known about the fungal role in biogeochemical cycling in oligotrophic ecosystems. This study compared fungal communities and assessed the role of exogenous carbon on microbial community structure and function in two southern Appalachian caves: an anthropogenically impacted cave and a near-pristine cave. Due to carbon input from shallow soils, the anthropogenically impacted cave had an order of magnitude greater fungal and bacterial quantitative-polymerase chain reaction (qPCR) gene copy numbers, had significantly greater community diversity, and was dominated by ascomycotal phylotypes common in early phase, labile organic matter decomposition. Fungal assemblages in the near-pristine cave samples were dominated by Basidiomycota typically found in deeper soils (and/or in late phase, recalcitrant organic matter decomposition), suggesting more oligotrophic conditions. In situ carbon and manganese (II) [Mn(II)] addition over 10 weeks resulted in growth of fungal mycelia followed by increased Mn(II) oxidation. A before/after comparison of the fungal communities indicated that this enrichment increased the quantity of fungal and bacterial cells, yet decreased overall fungal diversity. Anthropogenic carbon sources can therefore dramatically influence the diversity and quantity of fungi, impact microbial community function, and stimulate Mn(II) oxidation, resulting in a cascade of changes that can strongly influence nutrient and trace element biogeochemical cycles in karst aquifers. C1 [Carmichael, Sarah K.] Appalachian State Univ, Dept Geol, Boone, NC 28608 USA. [Zorn, Bryan T.; Braeuer, Suzanna L.] Appalachian State Univ, Dept Biol, Boone, NC 28608 USA. [Santelli, Cara M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Roble, Leigh A.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Carmichael, Mary J.] Wake Forest Univ, Dept Biol, Winston Salem, NC 27109 USA. RP Brauer, SL (reprint author), Appalachian State Univ, Dept Biol, Boone, NC 28608 USA. EM brauersl@appstate.edu OI Santelli, Cara/0000-0001-8617-0008 FU Appalachian State University, NC; Smithsonian Institution; NC Space Grant Graduate Research Fellowship FX The authors thank Dr. Charles Pepe-Ranney, Dr. Michael Madritch and Dr. Matt Estep for assistance with sequencing and data processing, and Dr. John Walker and Zack Anderson for assistance with fungal analyses. Dr. Jeffrey Post performed selected mu-XRD analyses and mineral phase identifications. Additionally, the authors are extremely grateful for assistance provided by Melanie Hoff, Milton Starnes and John Rossi for facilitating visits to the cave sites. Partial support was provided by Appalachian State University, NC Space Grant New Investigators Awards to SK Carmichael and SL Brauer, a small grant from the Smithsonian Institution awarded to CM Santelli and through a NC Space Grant Graduate Research Fellowship awarded to MJ Carmichael. NR 101 TC 0 Z9 0 U1 5 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1758-2229 J9 ENV MICROBIOL REP JI Environ. Microbiol. Rep. PD AUG PY 2015 VL 7 IS 4 BP 592 EP 605 DI 10.1111/1758-2229.12291 PG 14 WC Environmental Sciences; Microbiology SC Environmental Sciences & Ecology; Microbiology GA CN5XM UT WOS:000358506800001 PM 25865809 ER PT J AU Glenn, DR Lee, K Park, H Weissleder, R Yacoby, A Lukin, MD Lee, H Walsworth, RL Connolly, CB AF Glenn, David R. Lee, Kyungheon Park, Hongkun Weissleder, Ralph Yacoby, Amir Lukin, Mikhail D. Lee, Hakho Walsworth, Ronald L. Connolly, Colin B. TI Single-cell magnetic imaging using a quantum diamond microscope SO NATURE METHODS LA English DT Article ID PROTEIN AB We apply a quantum diamond microscope for detection and imaging of immunomagnetically labeled cells. This instrument uses nitrogen-vacancy (NV) centers in diamond for correlated magnetic and fluorescence imaging. Our device provides single-cell resolution and a field of view (similar to 1 mm(2)) two orders of magnitude larger than that of previous NV imaging technologies, enabling practical applications. To illustrate, we quantified cancer biomarkers expressed by rare tumor cells in a large population of healthy cells. C1 [Glenn, David R.; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, Kyungheon; Weissleder, Ralph; Lee, Hakho] Massachusetts Gen Hosp, Ctr Syst Biol, Boston, MA 02114 USA. [Park, Hongkun; Yacoby, Amir; Lukin, Mikhail D.; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Park, Hongkun] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Park, Hongkun; Walsworth, Ronald L.] Harvard Univ, Ctr Brain Sci, Cambridge, MA 02138 USA. [Weissleder, Ralph] Harvard Univ, Sch Med, Dept Syst Biol, Boston, MA 02115 USA. [Connolly, Colin B.] Quantum Diamond Technol Inc, Somerville, MA USA. RP Lee, H (reprint author), Massachusetts Gen Hosp, Ctr Syst Biol, Boston, MA 02114 USA. EM hlee@mgh.harvard.edu; rwalsworth@cfa.harvard.edu; cconnolly@quantumdiamondtech.com FU US National Institutes of Health [R01HL113156, U54-CA119349]; US Defense Advanced Research Projects Agency (DARPA) QuASAR program; DARPA SBIR [W31P4Q-13-C-0064] FX The authors thank M.L. McKee for help with electron microscopy, as well as M. Liong and H. Shao for advice on magnetic assay protocols. This work was supported in part by US National Institutes of Health grants R01HL113156 (H.L.) and U54-CA119349 (R.W.) as well as the US Defense Advanced Research Projects Agency (DARPA) QuASAR program and DARPA SBIR contract W31P4Q-13-C-0064. NR 17 TC 19 Z9 19 U1 4 U2 71 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1548-7091 EI 1548-7105 J9 NAT METHODS JI Nat. Methods PD AUG PY 2015 VL 12 IS 8 BP 736 EP U161 DI 10.1038/NMETH.3449 PG 5 WC Biochemical Research Methods SC Biochemistry & Molecular Biology GA CN8ZW UT WOS:000358736100015 PM 26098019 ER PT J AU Zhang, L Rothfels, CJ Ebihara, A Schuettpelz, E Le Pechon, T Kamau, P He, H Zhou, XM Prado, J Field, A Yatskievych, G Gao, XF Zhang, LB AF Zhang, Liang Rothfels, Carl J. Ebihara, Atsushi Schuettpelz, Eric Le Pechon, Timothee Kamau, Peris He, Hai Zhou, Xin-Mao Prado, Jefferson Field, Ashley Yatskievych, George Gao, Xin-Fen Zhang, Li-Bing TI A global plastid phylogeny of the brake fern genus Pteris (Pteridaceae) and related genera in the Pteridoideae SO CLADISTICS LA English DT Review ID MAXIMUM-LIKELIHOOD; CHLOROPLAST DNA; DRYOPTERIS DRYOPTERIDACEAE; ERIOSORUS PTERIDACEAE; EVOLUTIONARY LINEAGES; MODEL SELECTION; SEQUENCES; PARSIMONY; TAENITIDOIDEAE; MONILOPHYTES AB The brake fern genus Pteris belongs to the Pteridaceae subfamily Pteridoideae. It contains 200-250 species distributed on all continents except Antarctica, with its highest species diversity in tropical and subtropical regions. The monophyly of Pteris has long been in question because of its great morphological diversity and because of the controversial relationships of the Australian endemic monospecific genus Platyzoma. The circumscription of the Pteridoideae has likewise been uncertain. Previous studies typically had sparse sampling of Pteris species and related genera and used limited DNA sequence data. In the present study, DNA sequences of six plastid loci of 146 accessions representing 119 species of Pteris (including the type of the genus) and 18 related genera were used to infer a phylogeny using maximum-likelihood, Bayesian-inference and maximum-parsimony methods. Our major results include: (i) the previous uncertain relationships of Platyzoma were due to long-branch attraction; (ii) Afropteris, Neurocallis, Ochropteris and Platyzoma are all embedded within a well-supported Pteris sensu lato; (iii) the traditionally circumscribed Jamesonia is paraphyletic in relation to a monophyletic Eriosorus; (iv) Pteridoideae contains 15 genera: Actiniopteris, Anogramma, Austrogramme, Cerosora, Cosentinia, Eriosorus, Jamesonia, Nephopteris (no molecular data), Onychium, Pityrogramma, Pteris, Pterozonium, Syngramma, Taenitis and Tryonia; and (v) 15 well-supported clades within Pteris are identified, which differ from one another on molecular, morphological and geographical grounds, and represent 15 major evolutionary lineages. (C) The Willi Hennig Society 2014. C1 [Zhang, Liang; Le Pechon, Timothee; Zhou, Xin-Mao; Gao, Xin-Fen] Chinese Acad Sci, Chengdu Inst Biol, Chengdu 610041, Sichuan, Peoples R China. [Rothfels, Carl J.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [Ebihara, Atsushi] Natl Museum Nat & Sci, Dept Bot, Tsukuba, Ibaraki 3050005, Japan. [Schuettpelz, Eric] Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kamau, Peris] Natl Museums Kenya, Dept Bot, Nairobi, Kenya. [He, Hai] Chongqing Normal Univ, Dept Biol, Chongqing 400047, Peoples R China. [Prado, Jefferson] Inst Bot Herbario SP, BR-04301012 Sao Paulo, Brazil. [Field, Ashley] James Cook Univ, Australian Trop Herbarium, Smithfield, Qld 4878, Australia. [Field, Ashley] Queensland Herbarium, Dept Sci Informat Technol Innovat & Arts, Toowong, Qld 4066, Australia. [Yatskievych, George; Zhang, Li-Bing] Missouri Bot Garden, St Louis, MO 63166 USA. RP Gao, XF (reprint author), Chinese Acad Sci, Chengdu Inst Biol, POB 416, Chengdu 610041, Sichuan, Peoples R China. EM xfgao@cib.ac.cn; Libing.Zhang@mobot.org RI Le Pechon, Timothee/N-9247-2013; Prado, Jefferson/C-4766-2012; OI Le Pechon, Timothee/0000-0003-3668-753X; Prado, Jefferson/0000-0003-4783-3125; Schuettpelz, Eric/0000-0003-3891-9904 NR 105 TC 10 Z9 10 U1 2 U2 20 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0748-3007 EI 1096-0031 J9 CLADISTICS JI Cladistics PD AUG PY 2015 VL 31 IS 4 BP 406 EP 423 DI 10.1111/cla.12094 PG 18 WC Evolutionary Biology SC Evolutionary Biology GA CN1KS UT WOS:000358179500002 ER PT J AU Garzon-Lopez, CX Ballesteros-Mejia, L Ordonez, A Bohlman, SA Olff, H Jansen, PA AF Garzon-Lopez, Carol X. Ballesteros-Mejia, Liliana Ordonez, Alejandro Bohlman, Stephanie A. Olff, Han Jansen, Patrick A. TI Indirect interactions among tropical tree species through shared rodent seed predators: a novel mechanism of tree species coexistence SO ECOLOGY LETTERS LA English DT Article DE Apparent competition; apparent mutualism; Astrocaryum standleyanum; Attalea butyracea; Dipteryx oleifera; indirect effects; Janzen-Connell hypothesis; seed predation; shared enemies; tropical forest ID RAIN-FOREST TREE; APPARENT COMPETITION; DENSITY-DEPENDENCE; SPATIAL AUTOCORRELATION; PLANT RECRUITMENT; DISPERSAL; PALM; HERBIVORES; DIVERSITY; SURVIVAL AB The coexistence of numerous tree species in tropical forests is commonly explained by negative dependence of recruitment on the conspecific seed and tree density due to specialist natural enemies that attack seeds and seedlings (Janzen-Connell' effects). Less known is whether guilds of shared seed predators can induce a negative dependence of recruitment on the density of different species of the same plant functional group. We studied 54 plots in tropical forest on Barro Colorado Island, Panama, with contrasting mature tree densities of three coexisting large seeded tree species with shared seed predators. Levels of seed predation were far better explained by incorporating seed densities of all three focal species than by conspecific seed density alone. Both positive and negative density dependencies were observed for different species combinations. Thus, indirect interactions via shared seed predators can either promote or reduce the coexistence of different plant functional groups in tropical forest. C1 [Garzon-Lopez, Carol X.; Ballesteros-Mejia, Liliana; Olff, Han; Jansen, Patrick A.] Univ Groningen, Groningen Inst Evolutionary Life Sci, NL-9700 CC Groningen, Netherlands. [Garzon-Lopez, Carol X.] Fdn Edmund Mach, GIS & Remote Sensing Unit, Res & Innovat Ctr, Dept Biodivers & Mol Ecol, I-38010 San Michele All Adige, TN, Italy. [Ballesteros-Mejia, Liliana] Univ Fed Goias UFG, Lab Genet & Biodiversidade, ICB, BR-74001970 Goiania, Go, Brazil. [Ordonez, Alejandro] Aarhus Univ, Sect Ecoinformat & Biodivers, Dept Biosci, DK-8000 Aarhus C, Denmark. [Bohlman, Stephanie A.; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. RP Garzon-Lopez, CX (reprint author), Univ Groningen, Groningen Inst Evolutionary Life Sci, Box 11103, NL-9700 CC Groningen, Netherlands. EM c.x.garzon@gmail.com RI Olff, Han/A-8516-2008; Garzon-Lopez, Carol/G-6251-2014 OI Olff, Han/0000-0003-2154-3576; Garzon-Lopez, Carol/0000-0002-4099-2740 FU Smithsonian Tropical Research Institute; Ubbo Emmius Scholarship programme; University of Groningen; EU BON (Building the European Biodiversity Observation Network) project; European Union [308454]; European Research Council [ERC-2012-StG-310886-HISTFUNC] FX We thank Erik Vasquez, Helen Esser and Eduardo Medina for their help in the field and laboratory; and Egbert Leigh, Robert Holt and two anonymous reviewers for their very helpful comments. This work was supported by the Smithsonian Tropical Research Institute, the Ubbo Emmius Scholarship programme (CXG) and the Marco Polo funds (LBM) of the University of Groningen. CXG was partially funded by the EU BON (Building the European Biodiversity Observation Network) project, funded by the European Union under the 7th Framework programme, Contract No. 308454. AO was supported by the European Research Council grant ERC-2012-StG-310886-HISTFUNC. NR 51 TC 3 Z9 3 U1 7 U2 62 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 AUG PY 2015 VL 18 IS 8 BP 752 EP 760 DI 10.1111/ele.12452 PG 9 WC Ecology SC Environmental Sciences & Ecology GA CM8NO UT WOS:000357958900002 PM 25939379 ER PT J AU Peay, KG Russo, SE McGuire, KL Lim, ZY Chan, JP Tan, S Davies, SJ AF Peay, Kabir G. Russo, Sabrina E. McGuire, Krista L. Lim, Zhenyu Chan, Ju Ping Tan, Sylvester Davies, Stuart J. TI Lack of host specificity leads to independent assortment of dipterocarps and ectomycorrhizal fungi across a soil fertility gradient SO ECOLOGY LETTERS LA English DT Article DE Borneo; Lambir Hills; mutualism; mycorrhiza; plant-soil feedback; tropical rainforest ID BORNEAN RAIN-FOREST; COMMUNITY STRUCTURE; MYCORRHIZAL FUNGI; TROPICAL FOREST; CO-INVASION; PLANT; ASSOCIATIONS; FEEDBACK; DISTRIBUTIONS; LIMITATION AB Plants interact with a diversity of microorganisms, and there is often concordance in their community structures. Because most community-level studies are observational, it is unclear if such concordance arises because of host specificity, in which microorganisms or plants limit each other's occurrence. Using a reciprocal transplant experiment, we tested the hypothesis that host specificity between trees and ectomycorrhizal fungi determines patterns of tree and fungal soil specialisation. Seedlings of 13 dipterocarp species with contrasting soil specialisationswereseeded into plots crossing soil type and canopy openness. Ectomycorrhizalcolonists were identified by DNA sequencing. After 2.5years, we found no evidence of host specificity. Rather, soil environment was the primary determinant of ectomycorrhizal diversity and composition on seedlings. Despite their close symbiosis, our results show that ectomycorrhizal fungi and tree communities in this Bornean rain forest assembleindependently of host-specific interactions, raising questions about howmutualism shapes the realised niche. C1 [Peay, Kabir G.; Lim, Zhenyu] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Russo, Sabrina E.; Chan, Ju Ping] Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. [McGuire, Krista L.] Columbia Univ, Barnard Coll, Dept Biol, New York, NY 10027 USA. [McGuire, Krista L.] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Tan, Sylvester; Davies, Stuart J.] Smithsonian Inst, Ctr Trop Forest Sci, Washington, DC 20013 USA. RP Peay, KG (reprint author), Stanford Univ, Dept Biol, Stanford, CA 94305 USA. EM kpeay@stanford.edu OI Peay, Kabir/0000-0002-7998-7412 FU National Science Foundation [1249342, 0919136, 1120011] FX This research was supported by National Science Foundation DEB grants 1249342 to KGP, 0919136 to SER and 1120011 to KLM. The authors thank Sarawak Forest Research Corporation and Forest Department Sarawak for permission to conduct research at Lambir and Ms. Januarie Kulis, Park Warden of Lambir Hills National Park, for her support. Tadashi Fukami, the Fukami Lab and Peay Lab gave helpful comments on an early draft. NR 52 TC 18 Z9 18 U1 9 U2 73 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 AUG PY 2015 VL 18 IS 8 BP 807 EP 816 DI 10.1111/ele.12459 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CM8NO UT WOS:000357958900008 PM 26032408 ER PT J AU Allan, E Manning, P Alt, F Binkenstein, J Blaser, S Bluethgen, N Bohm, S Grassein, F Holzel, N Klaus, VH Kleinebecker, T Morris, EK Oelmann, Y Prati, D Renner, SC Rillig, MC Schaefer, M Schloter, M Schmitt, B Schoning, I Schrumpf, M Solly, E Sorkau, E Steckel, J Steffen-Dewenter, I Stempfhuber, B Tschapka, M Weiner, CN Weisser, WW Werner, M Westphal, C Wilcke, W Fischer, M AF Allan, Eric Manning, Pete Alt, Fabian Binkenstein, Julia Blaser, Stefan Bluethgen, Nico Boehm, Stefan Grassein, Fabrice Hoelzel, Norbert Klaus, Valentin H. Kleinebecker, Till Morris, E. Kathryn Oelmann, Yvonne Prati, Daniel Renner, Swen C. Rillig, Matthias C. Schaefer, Martin Schloter, Michael Schmitt, Barbara Schoening, Ingo Schrumpf, Marion Solly, Emily Sorkau, Elisabeth Steckel, Juliane Steffen-Dewenter, Ingolf Stempfhuber, Barbara Tschapka, Marco Weiner, Christiane N. Weisser, Wolfgang W. Werner, Michael Westphal, Catrin Wilcke, Wolfgang Fischer, Markus TI Land use intensification alters ecosystem multifunctionality via loss of biodiversity and changes to functional composition SO ECOLOGY LETTERS LA English DT Article DE Biodiversity-ecosystem functioning; ecosystem services; global change; land use; multifunctionality ID PLANT-SPECIES RICHNESS; GRASSLAND COMMUNITIES; USE INTENSITY; SERVICES; DIVERSITY; PRODUCTIVITY; MANAGEMENT; FERTILIZATION; TRADEOFFS; LANDSCAPE AB Global change, especially land-use intensification, affects human well-being by impacting the delivery of multiple ecosystem services (multifunctionality). However, whether biodiversity loss is a major component of global change effects on multifunctionality in real-world ecosystems, as in experimental ones, remains unclear. Therefore, we assessed biodiversity, functional composition and 14 ecosystem services on 150 agricultural grasslands differing in land-use intensity. We also introduce five multifunctionality measures in which ecosystem services were weighted according to realistic land-use objectives. We found that indirect land-use effects, i.e. those mediated by biodiversity loss and by changes to functional composition, were as strong as direct effects on average. Their strength varied with land-use objectives and regional context. Biodiversity loss explained indirect effects in a region of intermediate productivity and was most damaging when land-use objectives favoured supporting and cultural services. In contrast, functional composition shifts, towards fast-growing plant species, strongly increased provisioning services in more inherently unproductive grasslands. C1 [Allan, Eric; Manning, Pete; Blaser, Stefan; Grassein, Fabrice; Prati, Daniel; Schmitt, Barbara; Fischer, Markus] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. [Allan, Eric] Univ Bern, Ctr Dev & Environm, CH-3012 Bern, Switzerland. [Alt, Fabian; Oelmann, Yvonne; Sorkau, Elisabeth] Univ Tubingen, Geocol, D-72070 Tubingen, Germany. [Binkenstein, Julia; Schaefer, Martin] Univ Freiburg, Dept Ecol & Evolutionary Biol, Fac Biol, D-79104 Freiburg, Germany. [Bluethgen, Nico] Tech Univ Darmstadt, Ecol Networks, Biol, D-64287 Darmstadt, Germany. [Boehm, Stefan; Renner, Swen C.; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Hoelzel, Norbert; Klaus, Valentin H.; Kleinebecker, Till] Univ Munster, Inst Landscape Ecol, D-48149 Munster, Germany. [Morris, E. Kathryn] Xavier Univ, Cincinnati, OH 45207 USA. [Renner, Swen C.] Univ Freiburg, Inst Biol Zool 1, D-79106 Freiburg, Germany. [Renner, Swen C.] Natl Zool Pk, Smithsonian Conservat Biol Ctr, Front Royal, VA 22630 USA. [Rillig, Matthias C.] Free Univ Berlin, Plant Ecol, D-14195 Berlin, Germany. [Rillig, Matthias C.] Berlin Brandenburg Inst Adv Biodivers Res BBIB, D-14195 Berlin, Germany. [Schloter, Michael] Helmholtz Zentrum Munchen, Res Unit Environm Genom, D-85758 Oberschleissheim, Germany. [Schoening, Ingo; Schrumpf, Marion; Solly, Emily] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Steckel, Juliane; Steffen-Dewenter, Ingolf; Weiner, Christiane N.; Werner, Michael] Univ Wurzburg, Dept Anim Ecol & Trop Biol, Bioctr, D-97974 Wurzburg, Germany. [Stempfhuber, Barbara] German Res Ctr Environm Hlth, Helmholtz Zentrum Munchen, Environm Genom, D-85764 Neuherberg, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Weisser, Wolfgang W.] Univ Jena, Inst Ecol, D-07743 Jena, Germany. [Weisser, Wolfgang W.] Tech Univ Munich, Terr Ecol Res Grp, Dept Ecol & Ecosyst Management, Ctr Food & Life Sci Weihenstephan, D-85354 Freising Weihenstephan, Germany. [Westphal, Catrin] Univ Gottingen, Dept Crop Sci, Agroecol, D-37077 Gottingen, Germany. [Wilcke, Wolfgang] Univ Bern, Inst Geog, CH-3012 Bern, Switzerland. [Wilcke, Wolfgang] Karlsruhe Inst Technol, Inst Geog & Geoecol, D-76131 Karlsruhe, Germany. [Fischer, Markus] Senckenberg Gesell Nat Forsch Biodivers & Climate, D-60325 Frankfurt, Germany. [Fischer, Markus] Univ Potsdam, Biodivers Res Systemat Bot, D-14469 Potsdam, Germany. RP Allan, E (reprint author), Univ Bern, Inst Plant Sci, Altenbergrain 21, CH-3013 Bern, Switzerland. EM eric.allan@ips.unibe.ch RI Schoning, Ingo/D-3341-2009; Manning, Peter/I-6523-2012; Bluthgen, Nico/F-5983-2010; Westphal, Catrin/F-9560-2015; Fischer, Markus/C-6411-2008; Weisser, Wolfgang/B-9718-2014; Schrumpf, Marion/C-1671-2013; Oelmann, Yvonne/J-8730-2016; Wilcke, Wolfgang/P-4620-2016; Holzel, Norbert/H-8753-2013; Rillig, Matthias/B-3675-2009; OI Solly, Emily/0000-0002-3157-1805; Renner, Swen/0000-0002-6893-4219; Schoning, Ingo/0000-0002-9830-5026; Manning, Peter/0000-0002-7940-2023; Westphal, Catrin/0000-0002-2615-1339; Fischer, Markus/0000-0002-5589-5900; Weisser, Wolfgang/0000-0002-2757-8959; Oelmann, Yvonne/0000-0003-3513-6568; Wilcke, Wolfgang/0000-0002-6031-4613; Rillig, Matthias/0000-0003-3541-7853; Weiner, Christiane/0000-0003-4013-4663 FU Deutsche Forschungsgemeinschaft Priority Program 1374 'Infrastructure-Biodiversity Exploratories' FX We thank Robert Bagchi, Santiago Soliveres, Owen Petchey and Teja Tscharntke for comments on the manuscript. We also thank the managers of the three exploratories, Sonja Gockel, Kerstin Wiesner and Martin Gorke for their work in maintaining the plot and project infrastructure; Simone Pfeiffer and Christiane Fischer giving support through the central office, Birgitta Konig-Ries and Michael Owonibi for managing the central database, and Eduard Linsenmair, Dominik Hessenmoller, Jens Nieschulze, Francois Buscot, Ernst-Detlef Schulze, and the late Elisabeth Kalko for their role in setting up the Biodiversity Exploratories project. This work was funded by the Deutsche Forschungsgemeinschaft Priority Program 1374 'Infrastructure-Biodiversity Exploratories.' Fieldwork permits were given by the responsible state environmental offices of Baden-Wurttemberg, Thuringen and Brandenburg (according to 72 Brandenburgisches Naturschutzgesetz). NR 47 TC 22 Z9 23 U1 32 U2 206 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 AUG PY 2015 VL 18 IS 8 BP 834 EP 843 DI 10.1111/ele.12469 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CM8NO UT WOS:000357958900011 PM 26096863 ER PT J AU Yingst, RA Russell, P ten Kate, IL Noble, S Graff, T Graham, LD Eppler, D AF Yingst, R. A. Russell, P. ten Kate, I. L. Noble, S. Graff, T. Graham, L. D. Eppler, D. TI Designing remote operations strategies to optimize science mission goals: Lessons learned from the Moon Mars Analog Mission Activities Mauna Kea 2012 field test SO ACTA ASTRONAUTICA LA English DT Article DE Apollo Valley geologic map; Science operations; MER ID MIMOS-II; EXPLORATION; HAWAII; ROVER AB The Moon Mars Analog Mission Activities Mauna Kea 2012 (MMAMA 2012) field campaign aimed to assess how effectively an integrated science and engineering rover team operating on a 24-h planning cycle facilitates high-fidelity science products. The science driver of this field campaign was to determine the origin of a glacially-derived deposit: was the deposit the result of (1) glacial outwash from meltwater; or (2) the result of an ice dam breach at the head of the valley? Lessons learned from MMAMA 2012 science operations include: (1) current rover science operations scenarios tested in this environment provide adequate data to yield accurate derivative products such as geologic maps; (2) instrumentation should be selected based on both engineering and science goals; and chosen during, rather than after, mission definition; and (3) paralleling the tactical and strategic science processes provides significant efficiencies that impact science return. The MER-model concept of operations utilized, in which rover operators were sufficiently facile with science intent to alter traverse and sampling plans during plan execution, increased science efficiency, gave the Science Backroom time to develop mature hypotheses and science rationales, and partially alleviated the problem of data flow being greater than the processing speed of the scientists. (C) 2015 IAA. Published by Elsevier Ltd. on behalf of IAA. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licensesiby-nc-nd/4.0/). C1 [Yingst, R. A.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Russell, P.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20013 USA. [ten Kate, I. L.] Univ Utrecht, Dept Earth Sci, Fac Geosci, Utrecht, Netherlands. [Noble, S.] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Graff, T.] NASA Johnson Space Ctr, Houston, TX 77058 USA. [Graham, L. D.; Eppler, D.] NASA Johnson Space Ctr, Houston, TX 77058 USA. RP Yingst, RA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell St, Tucson, AZ 85719 USA. EM yingst@psi.edu; russellp@si.edu; i.l.tenkate@uu.nl; sarah.noble@nasa.gov; trevor.g.graff@nasa.gov; lee.d.graham@nasa.gov; dean.b.eppler@nasa.gov FU NASA MMAMA program [NNX12AM27G]; MMAMA program grant FX We gratefully acknowledge the work of the Rover Team and their JUNO II rover, which performed like a true wahine koa (warrior woman), making this field test possible. We also acknowledge the comments of Dr. John Moores and an anonymous reviewer that greatly improved this manuscript. This work was supported by NASA MMAMA program, Grant NNX12AM27G to RAY and an additional MMAMA program grant to ILtK. NR 31 TC 1 Z9 1 U1 1 U2 7 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 AUG-SEP PY 2015 VL 113 BP 120 EP 131 DI 10.1016/j.actaastro.2015.02.029 PG 12 WC Engineering, Aerospace SC Engineering GA CL8RA UT WOS:000357240600011 ER PT J AU Powell, LL Cordeiro, NJ Stratford, JA AF Powell, Luke L. Cordeiro, Norbert J. Stratford, Jeffrey A. TI Ecology and conservation of avian insectivores of the rainforest understory: A pantropical perspective SO BIOLOGICAL CONSERVATION LA English DT Article DE Understory insectivores; Rainforests; Pantropical; Fragmentation; Deforestation; Mixed species flocks ID ANT-FOLLOWING BIRDS; BARRO-COLORADO ISLAND; MIXED-SPECIES FLOCKS; TROPICAL FOREST; NEST PREDATION; NEOTROPICAL FOREST; HABITAT FRAGMENTATION; AMAZONIAN BIRDS; MULTISPECIES TERRITORIALITY; BIODIVERSITY CONSERVATION AB Avian insectivores of the tropical rainforest understory ("understory insectivores") are common, diverse, and often sensitive to disturbance of tropical forest, making them useful as sentinels of rainforest ecosystem change. At the 2013 joint American Ornithologists' Union and Cooper Ornithological Society meeting in Chicago, USA, researchers convened a symposium to address the ecology and conservation of understory insectivores. This Special Issue of Biological Conservation is the result of that symposium: a collection of articles that unites our efforts to further understand and conserve understory insectivores. In this introductory paper, we review the diversity and ecology of understory insectivores, identify threats to the guild, discuss hypotheses on drivers of population declines, and make suggestions for future research. Deforestation and forest degradation are the immediate threats to this guild, with agricultural expansion (particularly oil palm plantations), urbanization, road expansion and logging leading the list. Although vulnerabilities of this guild are most evident in the Neotropics, there are few studies from Asia and fewer still from Africa we recommend increased geographic coverage. If we are to understand the vulnerabilities of understory insectivores from a pantropical perspective, researchers should prioritize understanding the most serious threats (e.g., edge effects, deforestation, fragmentation, etc.) and standardize efforts to gauge understory insectivores' response to these threats (e.g., via species richness, abundance, demographic metrics). A coordinated approach by researchers working in tropical rainforests across the globe can help us understand the ecology of understory insectivores and meaningfully apply conservation and management actions. Published by Elsevier Ltd. C1 [Powell, Luke L.; Stratford, Jeffrey A.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011097 Manaus, Amazonas, Brazil. [Powell, Luke L.] Louisiana State Univ, RNR 227, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Powell, Luke L.] Louisiana State Univ, Ctr Agr, Baton Rouge, LA 70803 USA. [Cordeiro, Norbert J.] Roosevelt Univ, Dept Biol Chem & Phys Sci, Chicago, IL 60605 USA. [Cordeiro, Norbert J.] Field Museum, Life Sci Sci & Educ, Chicago, IL 60605 USA. [Stratford, Jeffrey A.] Wilkes Univ, Dept Biol & Hlth Sci, Wilkes Barre, PA 18766 USA. RP Powell, LL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. EM Luke.L.Powell@gmail.com NR 150 TC 17 Z9 17 U1 14 U2 95 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 AUG PY 2015 VL 188 SI SI BP 1 EP 10 DI 10.1016/j.biocon.2015.03.025 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CL8LG UT WOS:000357225600001 ER PT J AU Powell, LL Wolfe, JD Johnson, EI Hines, JE Nichols, JD Stouffer, PC AF Powell, Luke L. Wolfe, Jared D. Johnson, Erik I. Hines, James E. Nichols, James D. Stouffer, Philip C. TI Heterogeneous movement of insectivorous Amazonian birds through primary and secondary forest: A case study using multistate models with radiotelemetry data SO BIOLOGICAL CONSERVATION LA English DT Article DE Amazon; Fidelity fragmentation; Neotropical birds; Secondary forest; Multistate models; Movement probability ID ALTERNATIVE SUCCESSIONAL PATHWAYS; RAIN-FOREST; BRAZILIAN AMAZONIA; CAPTURE-RECAPTURE; SPECIES RESPONSES; NEOTROPICAL BIRDS; UNDERSTORY BIRDS; LANDSCAPE CHANGE; HABITAT QUALITY; MARKED ANIMALS AB Given rates of deforestation, disturbance, and secondary forest accumulation in tropical rainforests, there is a great need to quantify habitat use and movement among different habitats. This need is particularly pronounced for animals most sensitive to disturbance, such as insectivorous understory birds. Here we use multistate capture-recapture models with radiotelemetry data to determine the successional stage at which within-day movement probabilities of Amazonian birds in secondary forest are similar to those in primary forest. We radio-tracked three common understory insectivore species in primary and secondary forest at the Biological Dynamics of Forest Fragments project near Manaus, Brazil: two woodcreepers, Glyphorynchus spirurus (n = 19) and Xiphorhynchus pardalotus (n = 18), and the terrestrial antthrush Formicarius colma (n = 19). Forest age was a strong predictor of fidelity to a given habitat. All three species showed greater fidelity to primary forest than to 8-14-year-old secondary forest, indicating the latter's relatively poor quality. The two woodcreeper species used 12-18-year-old secondary forest in a manner comparable to continuous forest, but F. colma avoided moving even to 27-31-year-old secondary forest the oldest at our site. Our results suggest that managers concerned with less sensitive species can assume that forest reserves connected by 12-18-year-old secondary forest corridors are effectively connected. On the other hand, >30 years are required after land abandonment before secondary forest serves as a primary forest-like conduit for movement by F. colma; more sensitive terrestrial insectivores may take longer still. Published by Elsevier Ltd. C1 [Powell, Luke L.; Wolfe, Jared D.; Johnson, Erik I.; Stouffer, Philip C.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011097 Manaus, Amazonas, Brazil. [Powell, Luke L.; Wolfe, Jared D.; Johnson, Erik I.; Stouffer, Philip C.] Louisiana State Univ, RNR 227, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Powell, Luke L.; Wolfe, Jared D.; Johnson, Erik I.; Stouffer, Philip C.] Louisiana State Univ, Ctr Agr, Baton Rouge, LA 70803 USA. [Hines, James E.; Nichols, James D.] Patuxent Wildlife Res Ctr, USGS Biol Resources Div, Laurel, MD 20708 USA. RP Powell, LL (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. EM Luke.L.Powell@gmail.com FU U.S. National Science Foundation [LTREB 0545491]; American Union of Ornithologists' Research Award; American Union of Ornithologists' Frank M. Chapman Award; Wilson Ornithological Society's Paul A. Stewart Award; American Philosophical Society's Lewis Clark Fund FX We thank Paul Des Brisay, Marconi Cerqueira, Elizabeth Condon, Camila Duarte, Gilberto Fernandez Arellano, Jairo Lopes, Alercio Marajo de Reis, Rachelle McLaughlin, Karl Mokross, Osmaildo, Aida Rodrigues, and Tatiana Straatmann for their contributions in the field. The LSU "Bird Lunch" group, Kristina Cockle, Norbert Cordeiro, Kyle Harms, Michael Kaller, Curtis Marantz, Michael Lefsky, Michael Patten, Scott Saleska, Bret Sandercock, Jeff Stratford, Stefan Woltmann, J. Van Remsen and several anonymous reviewers had important contributions, including insightful reviews and advice on data analyses. We thank the following funding sources: U.S. National Science Foundation (LTREB 0545491), American Union of Ornithologists' Research Award, the American Union of Ornithologists' Frank M. Chapman Award, the Wilson Ornithological Society's Paul A. Stewart Award, and the American Philosophical Society's Lewis & Clark Fund. We conducted this research under ISU Institutional Animal Care and Use Committee approval and under applicable Brazilian permits. This is publication number 660 in the BDFFP technical series and number 37 in the Amazonian ornithology technical series. This manuscript was approved for publication by the Director of the Louisiana Agricultural Experimental Station as manuscript number 2015-241-20967. NR 76 TC 9 Z9 9 U1 6 U2 41 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 AUG PY 2015 VL 188 SI SI BP 100 EP 108 DI 10.1016/j.biocon.2015.01.028 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CL8LG UT WOS:000357225600011 ER PT J AU Yang, XH Cushman, JC Borland, AM Edwards, EJ Wullschleger, SD Tuskan, GA Owen, NA Griffiths, H Smith, JAC De Paoli, HC Weston, DJ Cottingham, R Hartwell, J Davis, SC Silvera, K Ming, R Schlauch, K Abraham, P Stewart, JR Guo, HB Albion, R Ha, JM Lim, SD Wone, BWM Yim, WC Garcia, T Mayer, JA Petereit, J Nair, SS Casey, E Hettich, RL Ceusters, J Ranjan, P Palla, KJ Yin, HF Reyes-Garcia, C Andrade, JL Freschi, L Beltran, JD Dever, LV Boxall, SF Waller, J Davies, J Bupphada, P Kadu, N Winter, K Sage, RF Aguilar, CN Schmutz, J Jenkins, J Holtum, JAM AF Yang, Xiaohan Cushman, John C. Borland, Anne M. Edwards, Erika J. Wullschleger, Stan D. Tuskan, Gerald A. Owen, Nick A. Griffiths, Howard Smith, J. Andrew C. De Paoli, Henrique C. Weston, David J. Cottingham, Robert Hartwell, James Davis, Sarah C. Silvera, Katia Ming, Ray Schlauch, Karen Abraham, Paul Stewart, J. Ryan Guo, Hao-Bo Albion, Rebecca Ha, Jungmin Lim, Sung Don Wone, Bernard W. M. Yim, Won Cheol Garcia, Travis Mayer, Jesse A. Petereit, Juli Nair, Sujithkumar S. Casey, Erin Hettich, Robert L. Ceusters, Johan Ranjan, Priya Palla, Kaitlin J. Yin, Hengfu Reyes-Garcia, Casandra Luis Andrade, Jose Freschi, Luciano Beltran, Juan D. Dever, Louisa V. Boxall, Susanna F. Waller, Jade Davies, Jack Bupphada, Phaitun Kadu, Nirja Winter, Klaus Sage, Rowan F. Aguilar, Cristobal N. Schmutz, Jeremy Jenkins, Jerry Holtum, Joseph A. M. TI A roadmap for research on crassulacean acid metabolism (CAM) to enhance sustainable food and bioenergy production in a hotter, drier world SO NEW PHYTOLOGIST LA English DT Article DE bioenergy; crassulacean acid metabolism (CAM); drought; genomics; photosynthesis; roadmap; synthetic biology; water-use efficiency (WUE) ID COMMON ICE PLANT; CARBON-ISOTOPE RATIOS; PORTULACA-OLERACEA L; MESEMBRYANTHEMUM-CRYSTALLINUM; C-4 PHOTOSYNTHESIS; POPULATION PROJECTIONS; REGULATORY NETWORKS; ADAPTIVE RADIATION; SEDUM-TELEPHIUM; EXPRESSION AB Crassulacean acid metabolism (CAM) is a specialized mode of photosynthesis that features nocturnal CO2 uptake, facilitates increased water-use efficiency (WUE), and enables CAM plants to inhabit water-limited environments such as semi-arid deserts or seasonally dry forests. Human population growth and global climate change now present challenges for agricultural production systems to increase food, feed, forage, fiber, and fuel production. One approach to meet these challenges is to increase reliance on CAM crops, such as Agave and Opuntia, for biomass production on semi-arid, abandoned, marginal, or degraded agricultural lands. Major research efforts are now underway to assess the productivity of CAM crop species and to harness the WUE of CAM by engineering this pathway into existing food, feed, and bioenergy crops. An improved understanding of CAM has potential for high returns on research investment. To exploit the potential of CAM crops and CAM bioengineering, it will be necessary to elucidate the evolution, genomic features, and regulatory mechanisms of CAM. Field trials and predictive models will be required to assess the productivity of CAM crops, while new synthetic biology approaches need to be developed for CAM engineering. Infrastructure will be needed for CAM model systems, field trials, mutant collections, and data management. C1 [Yang, Xiaohan; Borland, Anne M.; De Paoli, Henrique C.; Weston, David J.; Cottingham, Robert; Ranjan, Priya; Palla, Kaitlin J.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. [Cushman, John C.; Albion, Rebecca; Ha, Jungmin; Lim, Sung Don; Wone, Bernard W. M.; Yim, Won Cheol; Garcia, Travis; Mayer, Jesse A.] Univ Nevada, Dept Biochem & Mol Biol, Reno, NV 89557 USA. [Borland, Anne M.; Casey, Erin] Newcastle Univ, Sch Biol, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Edwards, Erika J.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Wullschleger, Stan D.; Nair, Sujithkumar S.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Owen, Nick A.; Griffiths, Howard] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Smith, J. Andrew C.; Beltran, Juan D.] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. [Hartwell, James; Dever, Louisa V.; Boxall, Susanna F.; Waller, Jade; Davies, Jack; Bupphada, Phaitun; Kadu, Nirja] Univ Liverpool, Inst Integrat Biol, Dept Plant Sci, Liverpool L69 7ZB, Merseyside, England. [Davis, Sarah C.] Ohio Univ, Voinovich Sch Leadership & Publ Affairs, Athens, OH 45701 USA. [Davis, Sarah C.] Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. [Silvera, Katia; Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Ming, Ray] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Ming, Ray] Fujian Agr & Forestry Univ, FAFU & UIUC SIB Joint Ctr Genom & Biotechnol, Fuzhou 350002, Peoples R China. [Schlauch, Karen; Petereit, Juli] Univ Nevada, Nevada Ctr Bioinformat, Reno, NV 89557 USA. [Abraham, Paul; Hettich, Robert L.] Oak Ridge Natl Lab, Div Chem Sci, Oak Ridge, TN 37831 USA. [Stewart, J. Ryan] Brigham Young Univ, Dept Plant & Wildlife Sci, Provo, UT 84602 USA. [Guo, Hao-Bo] Univ Tennessee, Dept Biochem & Cellular & Mol Biol, Knoxville, TN 37996 USA. [Ceusters, Johan] Katholieke Univ Leuven, Fac Engn Technol, TC Bioengn Technol, Dept M2S, B-2440 Geel, Belgium. [Yin, Hengfu] Chinese Acad Forestry, Res Inst Subtrop Forestry, Key Lab Forest Genet & Breeding, Fuyang 311400, Peoples R China. [Reyes-Garcia, Casandra; Luis Andrade, Jose] Ctr Invest Cient Yucatan, Colonia Chuburna De Hida 97200, Merida, Mexico. [Freschi, Luciano] Univ Sao Paulo, Dept Bot, BR-05508090 Sao Paulo, Brazil. [Sage, Rowan F.] Univ Toronto, Dept Ecol & Evolutionary Biol, Toronto, ON M5S 3B2, Canada. [Aguilar, Cristobal N.] Univ Autonoma Coahuila, Sch Chem, Dept Food Res, Saltillo, Coahuila, Mexico. [Schmutz, Jeremy; Jenkins, Jerry] HudsonAlpha Inst Biotechnol, Huntsville, AL 35801 USA. [Schmutz, Jeremy] US DOE, Joint Genome Inst, Walnut Creek, CA 94598 USA. [Holtum, Joseph A. M.] James Cook Univ, Coll Marine & Environm Sci, Townsville, Qld 4811, Australia. RP Yang, XH (reprint author), Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN 37831 USA. EM yangx@ornl.gov RI Yin, Hengfu/H-1695-2012; Yang, Xiaohan/A-6975-2011; Abraham, Paul/K-5599-2015; Research ID, CTBCC /O-3564-2014; Hartwell, James/M-7249-2014; Guo, Hao-Bo/B-7486-2009; Yim, Won Cheol/K-9100-2016; Wullschleger, Stan/B-8297-2012; Hettich, Robert/N-1458-2016; Tuskan, Gerald/A-6225-2011; OI Yin, Hengfu/0000-0002-0720-5311; Yang, Xiaohan/0000-0001-5207-4210; De Paoli, Henrique/0000-0001-8494-0603; Hartwell, James/0000-0001-5000-223X; Guo, Hao-Bo/0000-0003-1321-1758; Yim, Won Cheol/0000-0002-7489-0435; Wullschleger, Stan/0000-0002-9869-0446; Hettich, Robert/0000-0001-7708-786X; Tuskan, Gerald/0000-0003-0106-1289; Mayer, Jesse/0000-0001-9839-5001 FU Biotechnology and Biological Sciences Research Council [BB/F009313/1] NR 95 TC 23 Z9 23 U1 11 U2 83 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 AUG PY 2015 VL 207 IS 3 BP 491 EP 504 DI 10.1111/nph.13393 PG 14 WC Plant Sciences SC Plant Sciences GA CM6TZ UT WOS:000357824400005 PM 26153373 ER PT J AU Berger, MA Asgari-Targhi, M DeLuca, EE AF Berger, M. A. Asgari-Targhi, M. DeLuca, E. E. TI Self-organized braiding in solar coronal loops SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID ALFVEN-WAVE TURBULENCE; FLUX TUBES; RECONNECTION; CRITICALITY AB In this paper, we investigate the evolution of braided solar coronal loops. We assume that coronal loops consist of several internal strands which twist and braid about each other. Reconnection between the strands leads to small flares and heating of the loop to x-ray temperatures. Using a method of generating and releasing braid structure similar to a forest fire model, we show that the reconnected field lines evolve to a self-organised critical state. In this state, the frequency distributions of coherent braid sequences as well as flare energies follow power law distributions. We demonstrate how the presence of net helicity in the loop alters the distribution laws. C1 [Berger, M. A.] Univ Exeter, CEMPS, Exeter EX4 4QF, Devon, England. [Asgari-Targhi, M.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Berger, MA (reprint author), Univ Exeter, CEMPS, Exeter EX4 4QF, Devon, England. EM m.berger@exeter.ac.uk RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU Leverhulme Trust [SH-04409]; AIA [SP02H1701R] FX M. Berger is happy to thank the Leverhulme Trust grant SH-04409 which helped support this research. M. Asgari-Targhi and E.E. DeLuca are supported by the AIA contract SP02H1701R. NR 20 TC 0 Z9 0 U1 0 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 EI 1469-7807 J9 J PLASMA PHYS JI J. Plasma Phys. PD AUG PY 2015 VL 81 AR 395810404 DI 10.1017/S0022377815000483 PN 4 PG 13 WC Physics, Fluids & Plasmas SC Physics GA CK7TO UT WOS:000356436400017 ER PT J AU Dieleman, J Van Bocxlaer, B Manntschke, C Nyingi, DW Adriaens, D Verschuren, D AF Dieleman, Jorunn Van Bocxlaer, Bert Manntschke, Claudia Nyingi, Dorothy Wanja Adriaens, Dominique Verschuren, Dirk TI Tracing functional adaptation in African cichlid fishes through morphometric analysis of fossil teeth: exploring the methods SO HYDROBIOLOGIA LA English DT Article DE Cichlidae; Geometric morphometrics; Fish fossils; Adaptive modification; Tooth morphology; Africa ID LAKE MALAWI; PHENOTYPIC PLASTICITY; ADAPTIVE RADIATION; EAST-AFRICA; BODY SHAPE; SPECIATION; TANGANYIKA; EVOLUTION; RECORD AB The sedimentary archive of Crater Lake Challa in East Africa contains abundant fossil teeth of cichlid fishes throughout at least the last 25,000 years. Here, we use morphometric analyses of oral teeth from the two extant Oreochromis species inhabiting Lake Challa to explore the feasibility of tracing adaptive modification of the cichlid trophic apparatus in the lake's fossil record. We compared the performance of semi-landmark analysis (SLM) and elliptic Fourier analysis in capturing morphological variation in oral tooth crowns, and found that SLM, supplemented with tooth shaft measurements, ensured consistency with whole-body landmark analyses. Whole-body and tooth morphology data both allowed to discern between the indigenous Oreochromis hunteri and the recently introduced Oreochromis korogwe. Both species have an oral jaw arrangement of outer-row bicuspid and inner-rows tricuspid teeth, but O. hunteri has generally more slender teeth with a proportionally taller major cusp than O. korogwe, suggesting fine-scaled resource partitioning. Exploratory analysis of three fossil samples showed that the major tooth types of modern-day Oreochromis are also represented in the fossil record. Their total morphological variation is largely restricted to the morphospace occupied by contemporary teeth, suggesting a close functional relationship between ancient populations and their likely descendant, O. hunteri. C1 [Dieleman, Jorunn; Van Bocxlaer, Bert; Manntschke, Claudia; Verschuren, Dirk] Univ Ghent, Dept Biol, Limnol Unit, B-9000 Ghent, Belgium. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Univ Giessen, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. [Nyingi, Dorothy Wanja] Natl Museums Kenya, Ichthyol Sect, Dept Zool, Nairobi, Kenya. [Adriaens, Dominique] Univ Ghent, Dept Biol, Evolutionary Morphol Vertebrates, B-9000 Ghent, Belgium. RP Dieleman, J (reprint author), Univ Ghent, Dept Biol, Limnol Unit, KL Ledeganckstr 35, B-9000 Ghent, Belgium. EM jorunn.dieleman@ugent.be RI Van Bocxlaer, Bert/N-1965-2016 OI Van Bocxlaer, Bert/0000-0003-2033-326X FU CRA program of the Ghent University Research Council; Smithsonian Institution; Alexander von Humboldt Foundation; Flanders Research Foundation FX We thank Caxton Oluseno and the fishermen of Lake Challa for field assistance, Jos Snoeks for taxonomic information and Tom Geerinckx and Philippe Munyandamutsa for help with jaw and teeth preparation protocols. Moritz Muschick and an anonymous referee provided many useful suggestions that substantially improved the paper. The lake-sediment cores used in this study were collected under permit 13/001/11C of the Kenyan Ministry of Education, Science and Technology, in the framework of the European Science Foundation's EuroCLIMATE project CHALLACEA. This work is financed by the CRA program of the Ghent University Research Council to D.V., and by postdoctoral fellowships of the Smithsonian Institution, the Alexander von Humboldt Foundation and the Flanders Research Foundation to B. V. B. NR 54 TC 4 Z9 4 U1 13 U2 30 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD AUG PY 2015 VL 755 IS 1 BP 73 EP 88 DI 10.1007/s10750-015-2218-0 PG 16 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CK2KM UT WOS:000356039300006 ER PT J AU Dangremond, EM AF Dangremond, Emily M. TI Propagule predation by crabs limits establishment of an endemic mangrove SO HYDROBIOLOGIA LA English DT Article DE Seed predation; Refugia; Mangrove; Recruitment; Crab; Pelliciera rhizophorae ID PLANT-POPULATION DYNAMICS; SEED PREDATION; LAND CRABS; INTERTIDAL DISTRIBUTION; RAIN-FOREST; RECRUITMENT; HYPOTHESIS; DOMINANCE; ECOLOGY; DISTRIBUTIONS AB Recruitment of seedlings is crucial to the establishment and maintenance of plant populations and species ranges. Seed predation by crabs is prevalent in mangroves globally, but the importance of predation on mangrove abundance and distribution relative to other factors remain unclear. The rare Neotropical mangrove Pelliciera rhizophorae occurs in freshwater-influenced sites, and may lose many of its propagules to crab predation in other locations. Propagules of P. rhizophorae were placed in either Rhizophora mangle or P. rhizophorae-dominated forests on the Caribbean and Pacific coasts of Panama. On the Caribbean coast, crabs consumed 86.7% of propagules in the R. mangle forest but only 3.3% of propagules in the P. rhizophorae zone. On the Pacific coast, crabs consumed 90% of propagules in the R. mangle zone and 66.7% in the P. rhizophorae zone. When crab exclosures were used, seedling survival did not vary between forest types, suggesting that predation, rather than seedling survival once established, limits P. rhizophorae populations. Rhizophora mangle produces an order of magnitude more propagules per capita than P. rhizophorae and may well satiate its crab predators. The low salinity forest stands may provide a refuge from crab predation for the rare mangrove P. rhizophorae. C1 [Dangremond, Emily M.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. RP Dangremond, EM (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21307 USA. EM dangremonde@si.edu FU National Science Foundation FX Wayne Sousa, Paul Fine, Perry de Valpine, and Ilka Feller and an anonymous reviewer provided helpful comments on early versions of this paper. Sierra Flynn and Jorge Morales helped complete fieldwork. Funding was provided by the National Science Foundation Graduate Research Fellowship Program. Thanks to the Smithsonian Tropical Research Institute for use of their facilities at Punta Galeta and Bocas del Toro. NR 42 TC 1 Z9 1 U1 5 U2 22 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 EI 1573-5117 J9 HYDROBIOLOGIA JI Hydrobiologia PD AUG PY 2015 VL 755 IS 1 BP 257 EP 266 DI 10.1007/s10750-015-2238-9 PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CK2KM UT WOS:000356039300018 ER PT J AU Quinones, AE Wcislo, WT AF Quinones, A. E. Wcislo, W. T. TI Cryptic extended brood care in the facultatively eusocial sweat bee Megalopta genalis SO INSECTES SOCIAUX LA English DT Article DE Extended maternal care; Hygienic behavior; Megalopta genalis; Subsociality; Undertaking behavior; Eusociality ID ASSURED FITNESS RETURNS; ECUADORIA HYMENOPTERA; HALICTIDAE; EVOLUTION; INSECTS; SOCIALITY; LIFE AB As a result of different brood cell provisioning strategies, nest-making insects may differ in the extent to which adults regularly provide extended parental care to their brood beyond nest defense. Mass-provisioning species cache the entire food supply needed for larval development prior to the oviposition and typically seal the brood cell. It is usually assumed that there is no regular contact between the adult(s) and brood. Here, we show that the bee, Megalopta genalis, expresses a form of cryptic brood care, which would not be observed during normal development. Following experimental injections of different provisioning materials into brood cells, foundresses reopened manipulated cells and the brood were aborted in some cases, implying that the foundresses assessed conditions within the cells. In aborted cells, foundresses sometimes laid a second egg after first removing dead larvae, previously stored pollen and contaminants. Our results show that hygienic brood care can be cryptic and hence may be more widespread than previously believed, lending support to the hypothesis that extended parental care is a preadaptation toward eusociality. C1 [Quinones, A. E.] Univ Groningen, Theoret Biol Grp, NL-9747 AG Groningen, Netherlands. [Wcislo, W. T.] Smithsonian Trop Res Inst, Balboa 084303092, Apartado, Panama. RP Quinones, AE (reprint author), Univ Groningen, Theoret Biol Grp, Nijenborgh 7, NL-9747 AG Groningen, Netherlands. EM a.e.quinones.paredes@rug.nl FU Groningen University Fund (GUF); Marco Polo fund; Top master scholarship of the University of Groningen; STRI FX We thank Kate Ihle, Quinn McFrederick and Lizzette Jimenez for their help in the field during the data collection, Esther Chang for her helpful comments on the manuscript and Ido Pen for statistical advice. Finally, we would like to thank Associate Editor Dr. Miriam Richards and three anonymous reviewers for considerable help in improving the manuscript. AEQ was funded by Groningen University Fund (GUF), the Marco Polo fund and the Top master scholarship of the University of Groningen, and additional support was provided by general research funds from STRI to WTW. NR 33 TC 3 Z9 3 U1 1 U2 8 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 AUG PY 2015 VL 62 IS 3 BP 307 EP 313 DI 10.1007/s00040-015-0409-3 PG 7 WC Entomology SC Entomology GA CK5NM UT WOS:000356271800008 ER PT J AU Rabeling, C Schultz, TR Bacci, M Bollazzi, M AF Rabeling, C. Schultz, T. R. Bacci, M., Jr. Bollazzi, M. TI Acromyrmex charruanus: a new inquiline social parasite species of leaf-cutting ants SO INSECTES SOCIAUX LA English DT Article DE Leaf-cutter ants; Fungus-growing ants; Attini; Social parasitism; Inquilinism; Acromyrmex; Pseudoatta ID FUNGUS-GROWING ANTS; HYMENOPTERA-FORMICIDAE; SYMPATRIC SPECIATION; LEAFCUTTER ANT; EVOLUTION; HOST; COLONIES; BEHAVIOR; ATTINI; ORGANIZATION AB Social parasites exploit the colony resources of social species to secure their own survival and reproduction. Social parasites are frequently studied as models for conflict and cooperation as well as for speciation. The eusocial Hymenoptera harbor a diverse array of socially parasitic species with idiosyncratic life history strategies, but it is probably in the ants where social parasites are most speciose and have evolved the highest degrees of morphological and behavioral specialization. In the fungus-growing ants, a total of five obligate social parasites are known: four species are parasites of leaf-cutting ants and one species parasitizes a primitive fungus-growing ant species in the genus Mycocepurus. Here we describe a new species of socially parasitic leaf-cutting ant, Acromyrmex charruanus sp. nov., from Uruguay, and we report initial observations on the parasite's life history as well as on the morphological and behavioral adaptations related to the inquiline syndrome. Our observations suggest that Acromyrmex charruanus is an obligate inquiline social parasite of the thatch-mound-building, leaf-cutting ant Acromyrmex heyeri. Acromyrmex charruanus appears to be tolerant of the host, producing sexual offspring in the presence of the A. heyeri host queen. Queens of A. charruanus appear to reproduce semelparously and sexual offspring are produced during the austral fall (February), which differs significantly from the mating biology of the host species, which reproduces during the southern-hemisphere spring (October-December). We suggest that the diametrically opposed mating seasons of parasite and host might be adaptive, allowing the parasite to avoid competition for resources with the host sexual brood. The morphological and behavioral adaptations of A. charruanus accord with characters observed to arise early during the evolution of other ant inquiline parasite species, and so far we have no evidence for the existence of a worker caste in A. charruanus. Further field studies and behavioral experiments need to confirm our first observations and explore A. charruanus's behavioral ecology, evolution, and life history in more detail. C1 [Rabeling, C.] Univ Rochester, Dept Biol, Rochester, NY 14627 USA. [Schultz, T. R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Bacci, M., Jr.] Sao Paulo State Univ, Ctr Study Social Insects, BR-13506900 Rio Claro, SP, Brazil. [Bollazzi, M.] Univ Republica, Fac Agron, Sect Entomol, Montevideo 12900, Uruguay. RP Rabeling, C (reprint author), Univ Rochester, Dept Biol, Rochester, NY 14627 USA. EM crabeling@gmail.com FU National Science Foundation [DEB-1456964, DEB-0949689]; Harvard Society of Fellows; William F. Milton Fund from the Harvard Medical School; Smithsonian Competitive Grants Program for Science; FAPSP [2011/50226-0]; CNPq [311562/2012-4, 487639/2012-0] FX We gratefully acknowledge the Direccion General de Recursos Naturales Renovables for permission to conduct fieldwork in Uruguay. We thank Naomi Pierce for permission to conduct parts of this study in her laboratory at Harvard University. Sarah Callan and Amelia Harvey kindly assisted in the laboratory. Christian Rabeling was supported by the National Science Foundation (DEB-1456964), the Harvard Society of Fellows, and by the William F. Milton Fund from the Harvard Medical School. Ted Schultz was supported by the National Science Foundation (DEB-0949689, DEB-1456964) and the Smithsonian Competitive Grants Program for Science. Mauricio Bacci Jr. acknowledges support from FAPSP (2011/50226-0) and CNPq (311562/2012-4 and 487639/2012-0). Martin Bollazzi is grateful to Daniel Ramirez from Cambium Forestal for facilitating access to field research sites. NR 95 TC 4 Z9 4 U1 5 U2 29 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 AUG PY 2015 VL 62 IS 3 BP 335 EP 349 DI 10.1007/s00040-015-0406-6 PG 15 WC Entomology SC Entomology GA CK5NM UT WOS:000356271800011 ER PT J AU Ingley, SJ Reina, RG Bermingham, E Johnson, JB AF Ingley, Spencer J. Reina, Ruth G. Bermingham, Eldredge Johnson, Jerald B. TI Phylogenetic analyses provide insights into the historical biogeography and evolution of Brachyrhaphis fishes SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Brachyrhaphis; Phylogeny; Historical biogeography; Ecology; Poeciliidae; Lower Central America ID LIFE-HISTORY; LIVEBEARING FISH; PREDATOR REGIMES; CENTRAL-AMERICA; DNA-SEQUENCES; EPISCOPI POECILIIDAE; GENUS BRACHYRHAPHIS; COMPARATIVE ECOLOGY; UNIQUE FEATURES; MIDDLE MIOCENE AB The livebearing fish genus Brachyrhaphis (Poeciliidae) has become an increasingly important model in evolution and ecology research, yet the phylogeny of this group is not well understood, nor has it been examined thoroughly using modern phylogenetic methods. Here, we present the first comprehensive phylogenetic analysis of Brachyrhaphis by using four molecular markers (3 mtDNA, 1 nucDNA) to infer relationships among species in this genus. We tested the validity of this genus as a monophyletic group using extensive outgroup sampling based on recent phylogenetic hypotheses of Poeciliidae. We also tested the validity of recently described species of Brachyrhaphis that are part of the B. episcopi complex in Panama. Finally, we examined the impact of historical events on diversification of Brachyrhaphis, and made predictions regarding the role of different ecological environments on evolutionary diversification where known historical events apparently fail to explain speciation. Based on our results, we reject the monophyly of Brachyrhaphis, and question the validity of two recently described species (B. hessfeldi and B. roswithae). Historical biogeography of Brachyrhaphis generally agrees with patterns found in other freshwater taxa in Lower Central America, which show that geological barriers frequently predict speciation. Specifically, we find evidence in support of an 'island' mod el of Lower Central American formation, which posits that the nascent isthmus was partitioned by several marine connections before linking North and South America. In some cases where historic events (e.g., vicariance) fail to explain allopatric species breaks in Brachyrhaphis, ecological processes (e.g., divergent predation environments) offer additional insight into our understanding of phylogenetic diversification in this group. (C) 2015 Elsevier Inc. All rights reserved. C1 [Ingley, Spencer J.; Johnson, Jerald B.] Brigham Young Univ, Dept Biol, Evolutionary Ecol Labs, Provo, UT 84602 USA. [Reina, Ruth G.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama. [Johnson, Jerald B.] Brigham Young Univ, Monte L Bean Life Sci Museum, Provo, UT 84602 USA. RP Ingley, SJ (reprint author), Brigham Young Univ, Dept Biol, Evolutionary Ecol Labs, 401 WIDB, Provo, UT 84602 USA. EM sjingley@byu.edu OI Ingley, Spencer/0000-0002-2414-9892 FU National Science Foundation [OISE 0530267]; Smithsonian Tropical Research Institute; Brigham Young University FX We kindly thank those who helped with field and laboratory work needed to complete this study, especially Rigoberto Gonzalez. We are indebted to John Boylan, Ken Normandin and Adrianus Schonewille, for their great help in collecting. Funding for this research was provided by the National Science Foundation (Graduate Research Fellowship awarded to SJI and OISE 0530267 awarded to JBJ), the Smithsonian Tropical Research Institute, and by Brigham Young University. Our manuscript was improved considerably by feedback from two anonymous reviewers and Dr. Guillermo Orti. NR 72 TC 6 Z9 6 U1 6 U2 36 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 AUG PY 2015 VL 89 BP 104 EP 114 DI 10.1016/j.ympev.2015.04.013 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA CJ6YI UT WOS:000355640700009 PM 25916190 ER PT J AU Heim, O Treitler, JT Tschapka, M Knornschild, M Jung, K AF Heim, Olga Treitler, Julia T. Tschapka, Marco Knoernschild, Mirjam Jung, Kirsten TI The Importance of Landscape Elements for Bat Activity and Species Richness in Agricultural Areas SO PLOS ONE LA English DT Article ID SCATTERED TREES; LAND-USE; FORAGING HABITAT; BIRD POPULATIONS; FARMLAND BIRDS; BIODIVERSITY; ECHOLOCATION; INTENSIFICATION; IDENTIFICATION; CONSEQUENCES AB Landscape heterogeneity is regarded as a key factor for maintaining biodiversity and ecosystem function in production landscapes. We investigated whether grassland sites at close vicinity to forested areas are more frequently used by bats. Considering that bats are important consumers of herbivorous insects, including agricultural pest, this is important for sustainable land management. Bat activity and species richness were assessed using repeated monitoring from May to September in 2010 with acoustic monitoring surveys on 50 grassland sites in the Biosphere Reserve Schorfheide-Chorin (North-East Germany). Using spatial analysis (GIS), we measured the closest distance of each grassland site to potentially connecting landscape elements (e.g., trees, linear vegetation, groves, running and standing water). In addition, we assessed the distance to and the percent land cover of forest remnants and urban areas in a 200 m buffer around the recording sites to address differences in the local landscape setting. Species richness and bat activity increased significantly with higher forest land cover in the 200 m buffer and at smaller distance to forested areas. Moreover, species richness increased in proximity to tree groves. Larger amount of forest land cover and smaller distance to forest also resulted in a higher activity of bats on grassland sites in the beginning of the year during May, June and July. Landscape elements near grassland sites also influenced species composition of bats and species richness of functional groups (open, edge and narrow space foragers). Our results highlight the importance of forested areas, and suggest that agricultural grasslands that are closer to forest remnants might be better buffered against outbreaks of agricultural pest insects due to higher species richness and higher bat activity. Furthermore, our data reveals that even for highly mobile species such as bats, a very dense network of connecting elements within the landscape is beneficial to promote activity in open areas and thus assure vital ecosystem function in agricultural landscapes. C1 [Heim, Olga; Treitler, Julia T.; Tschapka, Marco; Knoernschild, Mirjam; Jung, Kirsten] Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. [Tschapka, Marco; Knoernschild, Mirjam] Smithsonian Trop Res Inst, Balboa, Panama. RP Jung, K (reprint author), Univ Ulm, Inst Evolutionary Ecol & Conservat Genom, D-89069 Ulm, Germany. EM kirsten.jung@uni-ulm.de FU German Science Foundation [KA 1241/19-1] FX This work has been funded by the German Science Foundation (http://www.dfg.de), Priority Program 1374 (KA 1241/19-1) to MT. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 56 TC 3 Z9 3 U1 11 U2 101 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 JUL 31 PY 2015 VL 10 IS 7 AR e0134443 DI 10.1371/journal.pone.0134443 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO0JY UT WOS:000358838400119 PM 26231029 ER PT J AU Byers, JE Smith, RS Pringle, JM Clark, GF Gribben, PE Hewitt, CL Inglis, GJ Johnston, EL Ruiz, GM Stachowicz, JJ Bishop, MJ AF Byers, James E. Smith, Rachel S. Pringle, James M. Clark, Graeme F. Gribben, Paul E. Hewitt, Chad L. Inglis, Graeme J. Johnston, Emma L. Ruiz, Gregory M. Stachowicz, John J. Bishop, Melanie J. TI Invasion Expansion: Time since introduction best predicts global ranges of marine invaders SO SCIENTIFIC REPORTS LA English DT Article ID CLIMATE-CHANGE; BIOLOGICAL INVASIONS; PLANT INVASIVENESS; GEOGRAPHIC RANGE; RESIDENCE TIME; NORTH-AMERICA; LIFE-HISTORY; BODY-SIZE; BIVALVES; SUCCESS AB Strategies for managing biological invasions are often based on the premise that characteristics of invading species and the invaded environment are key predictors of the invader's distribution. Yet, for either biological traits or environmental characteristics to explain distribution, adequate time must have elapsed for species to spread to all potential habitats. We compiled and analyzed a database of natural history and ecological traits of 138 coastal marine invertebrate species, the environmental conditions at sites to which they have been introduced, and their date of first introduction. We found that time since introduction explained the largest fraction (20%) of the variability in non-native range size, while traits of the species and environmental variables had significant, but minimal, influence on non-native range size. The positive relationship between time since introduction and range size indicates that non-native marine invertebrate species are not at equilibrium and are still spreading, posing a major challenge for management of coastal ecosystems. C1 [Byers, James E.; Smith, Rachel S.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Pringle, James M.] UNH, Ocean Proc Anal Lab, Durham, NH 03857 USA. [Smith, Rachel S.; Clark, Graeme F.; Johnston, Emma L.] Univ New S Wales, Sch Biol Earth & Environm Sci, Evolut & Ecol Res Ctr, Sydney, NSW 2052, Australia. [Gribben, Paul E.] Univ New S Wales, Sch Biol Earth & Environm Sci, Ctr Marine Bioinnovat, Sydney, NSW 2052, Australia. [Hewitt, Chad L.] Univ Waikato, Sch Sci, Hamilton 3240, New Zealand. [Inglis, Graeme J.] Natl Inst Water & Atmospher Res, Christchurch 8011, New Zealand. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Stachowicz, John J.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. [Bishop, Melanie J.] Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. RP Byers, JE (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. EM jebyers@uga.edu OI Ruiz, Gregory/0000-0003-2499-441X FU Genes to Geosciences Research Centre Macquarie University; Ecology and Evolution Research Centre University of New South Wales (UNSW), UNSW Gold Star Grant; NSF [0961830]; NZ Ministry for Primary Industries; NIWA; National SeaGrant Program; Smithsonian Institution FX Funding provided by Genes to Geosciences Research Centre Macquarie University, Ecology and Evolution Research Centre University of New South Wales (UNSW), UNSW Gold Star Grant Awarded to ELJ, and NSF #0961830 to JEB and JMP. We thank Rick Lumpkin (NOAA Atlantic Oceanographic and Meteorological Laboratory) for sharing data from the Global Drifter Project and Paula Pappalardo for help with plots. Data on New Zealand non-native species were compiled from projects funded by the NZ Ministry for Primary Industries and NIWA. Data collection and synthesis for NEMESIS were supported by the National SeaGrant Program and Smithsonian Institution, and we thank Paul Fofonoff and James Carlton for contributions to this effort. NR 46 TC 5 Z9 5 U1 5 U2 31 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 JUL 31 PY 2015 VL 5 AR 12436 DI 10.1038/srep12436 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN9LS UT WOS:000358770800001 PM 26227803 ER PT J AU Kjer, KM Ware, JL Rust, J Wappler, T Lanfear, R Jermiin, LS Zhou, X Aspock, H Aspock, U Beutel, RG Blanke, A Donath, A Flouri, T Frandsen, PB Kapli, P Kawahara, AY Letsch, H Mayer, C McKenna, DD Meusemann, K Niehuis, O Peters, RS Wiegmann, BM Yeates, DK von Reumont, BM Stamatakis, A Misof, B AF Kjer, K. M. Ware, J. L. Rust, J. Wappler, T. Lanfear, R. Jermiin, L. S. Zhou, X. Aspoeck, H. Aspoeck, U. Beutel, R. G. Blanke, A. Donath, A. Flouri, T. Frandsen, P. B. Kapli, P. Kawahara, A. Y. Letsch, H. Mayer, C. McKenna, D. D. Meusemann, K. Niehuis, O. Peters, R. S. Wiegmann, B. M. Yeates, D. K. von Reumont, B. M. Stamatakis, A. Misof, B. TI Response to Comment on "Phylogenomics resolves the timing and pattern of insect evolution" SO SCIENCE LA English DT Editorial Material ID FOSSIL AB Tong et al. comment on the accuracy of the dating analysis presented in our work on the phylogeny of insects and provide a reanalysis of our data. They replace log-normal priors with uniform priors and add a "roachoid" fossil as a calibration point. Although the reanalysis provides an interesting alternative viewpoint, we maintain that our choices were appropriate. C1 [Kjer, K. M.] Univ Calif Davis, Davis, CA 95616 USA. [Ware, J. L.; Frandsen, P. B.] Rutgers State Univ, New Brunswick, NJ 08903 USA. [Rust, J.; Wappler, T.; Donath, A.; Mayer, C.; Peters, R. S.] Univ Bonn, Bonn, Germany. [Lanfear, R.] Macquarie Univ, Sydney, NSW 2109, Australia. [Jermiin, L. S.; Meusemann, K.; Yeates, D. K.] CSIRO, Canberra, ACT, Australia. [Zhou, X.] BGI Shenzhen, China Natl GeneBank, Shenzhen, Peoples R China. [Zhou, X.] BGI Shenzhen, Shenzhen, Peoples R China. [Aspoeck, H.; Aspoeck, U.; Letsch, H.] Univ Vienna, Vienna, Austria. [Aspoeck, U.] Nat Hist Museum Wien, Vienna, Austria. [Beutel, R. G.] Univ Jena, Phyletischem Museum Jena, D-07745 Jena, Germany. [Blanke, A.] Univ Tsukuba, Tsukuba, Ibaraki 305, Japan. [Donath, A.; Mayer, C.; Meusemann, K.; Niehuis, O.; Peters, R. S.; von Reumont, B. M.; Misof, B.] Zool Forsch Museum Alexander Koenig ZFMK, Bonn, Germany. [Flouri, T.; Kapli, P.; Stamatakis, A.] HITS, Heidelberg, Germany. [Frandsen, P. B.] Smithsonian Inst, Washington, DC 20560 USA. [Kawahara, A. Y.] Univ Florida, Gainesville, FL USA. [McKenna, D. D.] Univ Memphis, Memphis, TN 38152 USA. [Niehuis, O.] Arizona State Univ, Tempe, AZ USA. [Wiegmann, B. M.] N Carolina State Univ, Raleigh, NC 27695 USA. [von Reumont, B. M.] Nat Hist Museum, London SW7 5BD, England. RP Misof, B (reprint author), Zool Forsch Museum Alexander Koenig ZFMK, Bonn, Germany. EM bmisof@uni-bonn.de RI Jermiin, Lars/C-2458-2009; Blanke, Alexander/H-9858-2013; Stamatakis, Alexandros/B-8740-2009; Yeates, David/A-9917-2008 OI Jermiin, Lars/0000-0002-9619-3809; Yeates, David/0000-0001-7729-6143 NR 6 TC 3 Z9 3 U1 11 U2 33 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 JUL 31 PY 2015 VL 349 IS 6247 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN8SP UT WOS:000358713300043 ER PT J AU Heer, K Kalko, EKV Albrecht, L Garcia-Villacorta, R Staeps, FC Herre, EA Dick, CW AF Heer, Katrin Kalko, Elisabeth K. V. Albrecht, Larissa Garcia-Villacorta, Roosevelt Staeps, Felix C. Allen Herre, Edward Dick, Christopher W. TI Spatial Scales of Genetic Structure in Free-Standing and Strangler Figs (Ficus, Moraceae) Inhabiting Neotropical Forests SO PLOS ONE LA English DT Article ID TROPICAL RAIN-FORESTS; MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; FRUIT CHARACTERISTICS; ARTIBEUS-JAMAICENSIS; POLLINATING WASPS; TREE; SOFTWARE; BAT; PHYLOGEOGRAPHY AB Wind-borne pollinating wasps (Agaonidae) can transport fig (Ficus sp., Moraceae) pollen over enormous distances (> 100 km). Because of their extensive breeding areas, Neotropical figs are expected to exhibit weak patterns of genetic structure at local and regional scales. We evaluated genetic structure at the regional to continental scale (Panama, Costa Rica, and Peru) for the free-standing fig species Ficus insipida. Genetic differentiation was detected only at distances > 300 km (Jost's D-est = 0.68 +/- 0.07 & F-ST = 0.30 +/- 0.03 between Mesoamerican and Amazonian sites) and evidence for phylogeographic structure (R-ST>>permuted R-ST) was only significant in comparisons between Central and South America. Further, we assessed local scale spatial genetic structure (SGS, d <= 8 km) in Panama and developed an agent-based model parameterized with data from F. insipida to estimate minimum pollination distances, which determine the contribution of pollen dispersal on SGS. The local scale data for F. insipida was compared to SGS data collected for an additional free-standing fig, F. yoponensis (subgenus Pharmacosycea), and two species of strangler figs, F. citrifolia and F. obtusifolia (subgenus Urostigma) sampled in Panama. All four species displayed significant SGS (mean Sp = 0.014 +/- 0.012). Model simulations indicated that most pollination events likely occur at distances > > 1 km, largely ruling out spatially limited pollen dispersal as the determinant of SGS in F. insipida and, by extension, the other fig species. Our results are consistent with the view that Ficus develops fine-scale SGS primarily as a result of localized seed dispersal and/or clumped seedling establishment despite extensive long-distance pollen dispersal. We discuss several ecological and life history factors that could have species-or subgenus-specific impacts on the genetic structure of Neotropical figs. C1 [Heer, Katrin] Univ Marburg, Fac Biol, Conservat Biol, D-35043 Marburg, Germany. [Heer, Katrin] Univ Marburg, Fac Biol, Dept Ecol, D-35043 Marburg, Germany. [Heer, Katrin; Kalko, Elisabeth K. V.; Albrecht, Larissa] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.; Allen Herre, Edward] Smithsonian Trop Res Inst, Balboa, Panama. [Garcia-Villacorta, Roosevelt] Univ Edinburgh, Inst Mol Plant Sci, Edinburgh EH9 3JH, Midlothian, Scotland. [Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. RP Heer, K (reprint author), Univ Marburg, Fac Biol, Conservat Biol, Karl von Frisch Str 8, D-35043 Marburg, Germany. EM katrin.heer@uni-marburg.de FU German National Merit Foundation (Studienstiftung des Deutschen Volkes); NSF [DEB 0640379] FX The project was funded by a scholarship from the German National Merit Foundation (Studienstiftung des Deutschen Volkes) to KH and NSF funding (DEB 0640379) to CWD. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 78 TC 2 Z9 2 U1 5 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 JUL 30 PY 2015 VL 10 IS 7 AR e0133581 DI 10.1371/journal.pone.0133581 PG 18 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO0JT UT WOS:000358837700026 PM 26226482 ER PT J AU Wilkerson, RC Linton, YM Fonseca, DM Schultz, TR Price, DC Strickman, DA AF Wilkerson, Richard C. Linton, Yvonne-Marie Fonseca, Dina M. Schultz, Ted R. Price, Dana C. Strickman, Daniel A. TI Making Mosquito Taxonomy Useful: A Stable Classification of Tribe Aedini that Balances Utility with Current Knowledge of Evolutionary Relationships SO PLOS ONE LA English DT Article ID RIFT-VALLEY FEVER; EASTERN EQUINE ENCEPHALITIS; ALLIED TAXA DIPTERA; PHYLOGENETIC-RELATIONSHIPS; YELLOW-FEVER; LIFE STAGES; ARBOVIRUS SURVEILLANCE; WUCHERERIA-BANCROFTI; MORPHOLOGICAL DATA; CULICIDAE DIPTERA AB The tribe Aedini (Family Culicidae) contains approximately one-quarter of the known species of mosquitoes, including vectors of deadly or debilitating disease agents. This tribe contains the genus Aedes, which is one of the three most familiar genera of mosquitoes. During the past decade, Aedini has been the focus of a series of extensive morphology-based phylogenetic studies published by Reinert, Harbach, and Kitching (RH&K). Those authors created 74 new, elevated or resurrected genera from what had been the single genus Aedes, almost tripling the number of genera in the entire family Culicidae. The proposed classification is based on subjective assessments of the "number and nature of the characters that support the branches" subtending particular monophyletic groups in the results of cladistic analyses of a large set of morphological characters of representative species. To gauge the stability of RH&K's generic groupings we reanalyzed their data with unweighted parsimony jackknife and maximum-parsimony analyses, with and without ordering 14 of the characters as in RH&K. We found that their phylogeny was largely weakly supported and their taxonomic rankings failed priority and other useful taxon-naming criteria. Consequently, we propose simplified aedine generic designations that 1) restore a classification system that is useful for the operational community; 2) enhance the ability of taxonomists to accurately place new species into genera; 3) maintain the progress toward a natural classification based on monophyletic groups of species; and 4) correct the current classification system that is subject to instability as new species are described and existing species more thoroughly defined. We do not challenge the phylogenetic hypotheses generated by the above-mentioned series of morphological studies. However, we reduce the ranks of the genera and subgenera of RH&K to subgenera or informal species groups, respectively, to preserve stability as new data become available. C1 [Wilkerson, Richard C.; Linton, Yvonne-Marie; Schultz, Ted R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Linton, Yvonne-Marie] Smithsonian Inst, Museum Support Ctr, Walter Reed Biosystemat Unit, Suitland, MD USA. [Linton, Yvonne-Marie] Walter Reed Army Inst Res, Dept Entomol, Silver Spring, MD USA. [Linton, Yvonne-Marie] Uniformed Serv Univ Hlth Sci, Fac Preventat Med & Biometr, Bethesda, MD 20814 USA. [Fonseca, Dina M.; Price, Dana C.] Rutgers State Univ, Dept Entomol, Sch Environm & Biol Sci, New Brunswick, NJ 08903 USA. [Strickman, Daniel A.] Bill & Melinda Gates Fdn, Global Hlth Program, Seattle, WA USA. RP Wilkerson, RC (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, NHB 169, Washington, DC 20560 USA. EM wilkersonr@si.edu OI Fonseca, Dina/0000-0003-4726-7100 NR 104 TC 33 Z9 35 U1 4 U2 15 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 JUL 30 PY 2015 VL 10 IS 7 AR e0133602 DI 10.1371/journal.pone.0133602 PG 26 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CO0JT UT WOS:000358837700027 PM 26226613 ER PT J AU Xu, XG Wang, J Zeng, J Spurr, R Liu, X Dubovik, O Li, L Li, ZQ Mishchenko, MI Siniuk, A Holben, BN AF Xu, Xiaoguang Wang, Jun Zeng, Jing Spurr, Robert Liu, Xiong Dubovik, Oleg Li, Li Li, Zhengqiang Mishchenko, Michael I. Siniuk, Aliaksandr Holben, Brent N. TI Retrieval of aerosol microphysical properties from AERONET photopolarimetric measurements: 2. A new research algorithm and case demonstration SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE AERONET; polarization; aerosol retrieval algorithm; single-scattering albedo; remote sensing; absorption ID SKY RADIANCE MEASUREMENTS; BOUND CONSTRAINED OPTIMIZATION; OPTICAL-PROPERTIES; IMAGING SPECTRORADIOMETER; BIDIRECTIONAL REFLECTANCE; SPACEBORNE MEASUREMENTS; SATELLITE RETRIEVALS; TROPOSPHERIC AEROSOL; INVERSION ALGORITHM; INTEGRAL EQUATIONS AB A new research algorithm is presented here as the second part of a two-part study to retrieve aerosol microphysical properties from the multispectral and multiangular photopolarimetric measurements taken by Aerosol Robotic Network's (AERONET's) new-generation Sun photometer. The algorithm uses an advanced UNified and Linearized Vector Radiative Transfer Model and incorporates a statistical optimization approach. While the new algorithm has heritage from AERONET operational inversion algorithm in constraining a priori and retrieval smoothness, it has two new features. First, the new algorithm retrieves the effective radius, effective variance, and total volume of aerosols associated with a continuous bimodal particle size distribution (PSD) function, while the AERONET operational algorithm retrieves aerosol volume over 22 size bins. Second, our algorithm retrieves complex refractive indices for both fine and coarse modes, while the AERONET operational algorithm assumes a size-independent aerosol refractive index. Mode-resolved refractive indices can improve the estimate of the single-scattering albedo (SSA) for each aerosol mode and thus facilitate the validation of satellite products and chemistry transport models. We applied the algorithm to a suite of real cases over Beijing_RADI site and found that our retrievals are overall consistent with AERONET operational inversions but can offer mode-resolved refractive index and SSA with acceptable accuracy for the aerosol composed by spherical particles. Along with the retrieval using both radiance and polarization, we also performed radiance-only retrieval to demonstrate the improvements by adding polarization in the inversion. Contrast analysis indicates that with polarization, retrieval error can be reduced by over 50% in PSD parameters, 10-30% in the refractive index, and 10-40% in SSA, which is consistent with theoretical analysis presented in the companion paper of this two-part study. C1 [Xu, Xiaoguang; Wang, Jun; Zeng, Jing] Univ Nebraska, Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Spurr, Robert] RT Solut Inc, Cambridge, MA USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dubovik, Oleg] Univ Lille 1, CNRS, Lab Opt Atmospher, F-59655 Villeneuve Dascq, France. [Li, Li; Li, Zhengqiang] Chinese Acad Sci, State Environm Protect Key Lab Satellites Remote, Inst Remote Sensing & Digital Earth, Beijing, Peoples R China. [Mishchenko, Michael I.] NASA Goddard Inst Space Studies, New York, NY USA. [Siniuk, Aliaksandr; Holben, Brent N.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. RP Wang, J (reprint author), Univ Nebraska, Earth & Atmospher Sci, Lincoln, NE 68588 USA. EM jwangjun@gmail.com RI Liu, Xiong/P-7186-2014; Xu, Xiaoguang/B-8203-2016; Wang, Jun/A-2977-2008; OI Liu, Xiong/0000-0003-2939-574X; Xu, Xiaoguang/0000-0001-9583-980X; Wang, Jun/0000-0002-7334-0490; Li, Zhengqiang/0000-0002-7795-3630 FU NASA Earth and Space Science Fellowship; NASA Radiation Sciences Program; NASA Glory Mission Program FX This research is supported by a NASA Earth and Space Science Fellowship managed by Mingying Wei, as well as the NASA Radiation Sciences Program and the Glory Mission Program managed by Hal Maring. We acknowledge the data services provided by the AERONET team at NASA GSFC, and the computational support from the Holland Computing Center at the University of Nebraska. The data presented in the manuscript can be available upon request through email to the corresponding author at jwangjun@gmail.com. J. Zeng and J. Wang also thank Qingyuang Han for inspiring them to conduct this work. NR 80 TC 10 Z9 10 U1 1 U2 14 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 JUL 27 PY 2015 VL 120 IS 14 BP 7079 EP 7098 DI 10.1002/2015JD023113 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900024 ER PT J AU McCormick, B Popp, C Andrews, B Cottrell, E AF McCormick, Brendan Popp, Christoph Andrews, Benjamin Cottrell, Elizabeth TI Ten years of satellite observations reveal highly variable sulphur dioxide emissions at Anatahan Volcano, Mariana Islands SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE volcanic gas; satellite remote sensing; Anatahan volcano ID OZONE MONITORING INSTRUMENT; GROUND-BASED MEASUREMENTS; SOUFRIERE-HILLS VOLCANO; 2003 ERUPTION; SO2 EMISSIONS; SPACE; PLUMES; CHRONOLOGY; FLUX; COMMONWEALTH AB Satellite remote sensing enables continuous multiyear observations of volcanic activity in remote settings. Anatahan (Mariana Islands) is a remote volcano in the western North Pacific. Available ground-based measurements of sulphur dioxide (SO2) gas emissions at Anatahan place it among thelargest volcanic SO2 sources worldwide. These ground-based measurements, however, are restricted to eruptive intervals. Anatahan's activity since 2003 has been dominated temporally by prolonged periods of quiescence. Using 10years of satellite observations from OMI, AIRS, SCIAMACHY, and GOME-2, we report highly variable SO2 emissions within and between eruptive and quiescent intervals at Anatahan. We find close correspondence between levels of activity reported at the volcano and levels of SO2 emissions detected from space. Eruptive SO2 emission rates have a mean value of approximate to 6400td(-1), but frequently are in excess of 20,000td(-1). Conversely, SO2 emissions during quiescent intervals are below the detection limit of space-based sensors and therefore are not likely to exceed approximate to 300td(-1). We show that while Anatahan occupies a quiescent state for 85% of the past 10years, only approximate to 15% of total SO2 emissions over this interval occur during quiescence, with the remaining approximate to 85% released in short duration but intense syn-eruptive degassing. We propose that the integration of multiyear satellite data sets and activity histories are a powerful complement to targeted ground-based campaign measurements in better describing the long-term degassing behavior of remote volcanoes. C1 [McCormick, Brendan; Popp, Christoph; Andrews, Benjamin; Cottrell, Elizabeth] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. RP McCormick, B (reprint author), Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. EM brendanvolc@gmail.com FU Deep Carbon Observatory; Alfred P Sloan Foundation; Smithsonian Global Volcanism Program; Smithsonian Grand Challenges Award FX We acknowledge NASA for making OMI level 2 and AIRS level 1 data products freely available and BIRA/TEMIS for making SCIAMACHY level 2 data products freely available. We are grateful to Caroline Nowlan for providing access to SAO GOME-2 data and to Fred Prata and Simon Carn, respectively, for IDL routines which aided our analysis of AIRS and OMI data. The derived satellite data products presented herein (SO2 mass loadings, emission rates) are included in the supporting information, and more extensive supporting data can be provided by the authors upon request. B.M. and C.P. acknowledge the Deep Carbon Observatory, the Alfred P Sloan Foundation, and the Smithsonian Global Volcanism Program for supporting their postdoctoral fellowships. EC and BA each acknowledge a Smithsonian Grand Challenges Award, and the Global Volcanism Program; EC acknowledges a grant from the Deep Carbon Observatory. We thank Rob Wright and Eric Pilger for their assistance with the MODIS MODVOLC product; Jennifer Jay, Matt Pritchard, and Chuck Wicks for discussions of deformation in the Marianas; and Ed Venzke for discussions of eruption durations in the GVP-VOTW database. Finally, we warmly thank Taryn Lopez, Arlin Krueger, and one anonymous reviewer, for their detailed and constructive comments, which greatly improved the quality of this manuscript. NR 93 TC 3 Z9 3 U1 1 U2 10 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 JUL 27 PY 2015 VL 120 IS 14 BP 7258 EP 7282 DI 10.1002/2014JD022856 PG 25 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA CP3TL UT WOS:000359804900035 ER PT J AU Torres-Herrera, EJ Santos, LF AF Torres-Herrera, E. J. Santos, Lea F. TI Dynamics at the many-body localization transition SO PHYSICAL REVIEW B LA English DT Article ID INVERSE PARTICIPATION RATIO; METAL-INSULATOR-TRANSITION; MOBILITY EDGE; ANDERSON LOCALIZATION; WAVE-PACKET; SYSTEMS; STATES; FLUCTUATIONS; DIFFUSION; PHASE AB The isolated one-dimensional Heisenberg model with static random magnetic fields has become paradigmatic for the analysis of many-body localization. Here, we study the dynamics of this system initially prepared in a highly-excited nonstationary state. Our focus is on the probability for finding the initial state later in time, the so-called survival probability. Two distinct behaviors are identified before equilibration. At short times, the decay is very fast and equivalent to that of clean systems. It subsequently slows down and develops a power-law behavior with an exponent that coincides with the multifractal dimension of the eigenstates. C1 [Torres-Herrera, E. J.; Santos, Lea F.] Yeshiva Univ, Dept Phys, New York, NY 10016 USA. [Torres-Herrera, E. J.] Univ Autonoma Puebla, Inst Fis, Puebla 72570, Mexico. [Santos, Lea F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Torres-Herrera, EJ (reprint author), Yeshiva Univ, Dept Phys, New York, NY 10016 USA. RI Santos, Lea/D-5332-2012 OI Santos, Lea/0000-0001-9400-2709 FU NSF [DMR-1147430]; CONACyT, Mexico FX This work was supported by the NSF Grant No. DMR-1147430. E.J.T.H. acknowledges support from CONACyT, Mexico. L.F.S. thanks the ITAMP hospitality, where part of this work was done. We thank J.A. Mendez-Bermudez and Z. Papic for useful suggestions. NR 65 TC 31 Z9 31 U1 1 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD JUL 24 PY 2015 VL 92 IS 1 AR 014208 DI 10.1103/PhysRevB.92.014208 PG 7 WC Physics, Condensed Matter SC Physics GA CN4YI UT WOS:000358436100001 ER PT J AU Marra, PP Studds, CE Wilson, S Sillett, TS Sherry, TW Holmes, RT AF Marra, Peter P. Studds, Colin E. Wilson, Scott Sillett, T. Scott Sherry, Thomas W. Holmes, Richard T. TI Non-breeding season habitat quality mediates the strength of density-dependence for a migratory bird SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE American redstart; crowding; Setophaga ruticilla; carry-over effects; annual survival ID POPULATION REGULATION; NONBREEDING SEASON; REINTRODUCED POPULATION; AMERICAN REDSTARTS; FOOD AVAILABILITY; LARGE-SCALE; SURVIVAL; CONSEQUENCES; SONGBIRD; SEGREGATION AB Our understanding of when natural populations are regulated during their annual cycle is limited, particularly for migratory species. This information is needed for parametrizing models that can inform management and conservation. Here, we use 14 years of data on colour-marked birds to investigate how conspecific density and habitat quality during the tropical non-breeding period interact to affect body condition and apparent annual survival of a long-distance migratory songbird, the American redstart (Setophaga ruticilla). Body condition and survival of birds in high-quality mangrove habitat declined as density increased. By contrast, body condition improved and survival did not vary as density increased in adjacent, lower quality scrub habitat, although mean condition and survival were almost always lower than in mangrove. High rainfall enhanced body condition in scrub but not in mangrove, suggesting factors such as food availability outweighed consequences of crowding in lower quality habitat. Thus, survival of overwintering redstarts in mangrove habitat, disproportionately males, appears to be regulated by a crowding mechanism based on density-dependent resource competition. Survival of individuals in scrub, mostly females, appears to be limited by density-independent environmental factors but not regulated by crowding. The contrasting effects of density and food limitation on individuals overwintering in adjacent habitats illustrate the complexity of processes operating during the non-breeding period for migratory animals, and emphasize the need for long-term studies of animals in multiple habitats and throughout their annual cycles. C1 [Marra, Peter P.; Studds, Colin E.; Sillett, T. Scott] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. [Studds, Colin E.] Univ Maryland Baltimore Cty, Dept Geog & Environm Syst, Baltimore, MD 21250 USA. [Wilson, Scott] Carleton Univ, Environm Canada, Natl Wildlife Res Ctr, Ottawa, ON K1A 5B6, Canada. [Sherry, Thomas W.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Holmes, Richard T.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. RP Marra, PP (reprint author), Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM marrap@si.edu FU NSF [0717338, 1242584 0649679, 1242588, 9276520, 9625186] FX This study was supported by NSF grants to P.P.M., T.S.S., T.W.S. (0717338, 1242584 0649679, 1242588) and R.T.H. (9276520, 9625186). NR 61 TC 5 Z9 5 U1 6 U2 29 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 JUL 22 PY 2015 VL 282 IS 1811 AR 20150624 DI 10.1098/rspb.2015.0624 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CN8ZS UT WOS:000358735700011 ER PT J AU Rose, M Elvis, M Crenshaw, M Glidden, A AF Rose, Marvin Elvis, Martin Crenshaw, Michael Glidden, Ana TI Intermediate inclinations of type 2 Coronal-Line Forest AGN SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: emission lines; quasars: general; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; REGION; CLASSIFICATION; GALAXIES; SPECTRA; TORUS; VIEW AB Coronal-Line Forest Active Galactic Nuclei (CLiF AGN) are remarkable in the sense that they have a rich spectrum of dozens of coronal emission lines (e.g. [Fe VII], [Fe X] and [Ne V]) in their spectra. Rose, Elvis & Tadhunter suggest that the inner obscuring torus wall is the most likely location of the coronal line region in CLiF AGN, and the unusual strength of the forbidden high-ionization lines is due to a specific AGN-torus inclination angle. Here, we test this suggestion using mid-IR colours (4.6-22 mu m) from the Wide-Field Infrared Survey Explorer for the CLiF AGN. We use the Fischer et al. result that showed that as the AGN-torus inclination becomes more face on, the Spitzer 5.5-30 mu m colours become bluer. We show that the [W2-W4] colours for the CLiF AGN (<[W2-W4]> = 5.92 +/- 0.12) are intermediate between Sloan Digital Sky Survey (SDSS) type 1 (<[W2-W4]> = 5.22 +/- 0.01) and type 2 AGN (<[W2-W4]> = 6.35 +/- 0.03). This implies that the AGN-torus inclinations for the CLiF AGN are indeed intermediate, supporting the work of Rose, Elvis & Tadhunter. The confirmed relation between CLiF AGN and their viewing angle shows that CLiF AGN may be useful for our understanding of AGN unification. C1 [Rose, Marvin; Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Crenshaw, Michael] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Glidden, Ana] MIT, Dept Phys, Cambridge, MA 02139 USA. RP Rose, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mrose@cfa.harvard.edu FU NASA [NNX13AE88G]; Planetary Science Division of the National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX This work was supported in part by NASA grant NNX13AE88G. We thank the referee for useful comments and suggestions which improved this work substantially. The authors acknowledge the data analysis facilities provided by the Starlink Project, which is run by CCLRC on behalf of PPARC. This publication makes use of data products from NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology, funded by the Planetary Science Division of 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. 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. NR 15 TC 5 Z9 5 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 JUL 21 PY 2015 VL 451 IS 1 BP L11 EP L15 DI 10.1093/mnrasl/slv056 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CR4KX UT WOS:000361302000003 ER PT J AU Russell, HR Fabian, AC McNamara, BR Broderick, AE AF Russell, H. R. Fabian, A. C. McNamara, B. R. Broderick, A. E. TI Inside the Bondi radius of M87 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: individual: M87; intergalactic medium X-rays: galaxies: clusters ID RAY-EMITTING GAS; SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEI; NONRADIATIVE ACCRETION FLOWS; CENTRAL DOMINANT GALAXIES; SAGITTARIUS-A-ASTERISK; X-RAY; COOLING FLOWS; VIRGO CLUSTER; XMM-NEWTON AB Chandra X-ray observations of the nearby brightest cluster galaxy M87 resolve the hot gas structure across the Bondi accretion radius of the central supermassive black hole (SMBH), a measurement possible in only a handful of systems but complicated by the bright nucleus and jet emission. By stacking only short frame-time observations to limit pileup, and after subtracting the nuclear point spread function, we analysed the X-ray gas properties within the Bondi radius at 0.12-0.22 kpc (1.5-2.8 arcsec), depending on the black hole mass. Within 2 kpc radius, we detect two significant temperature components, which are consistent with constant values of 2 and 0.9 keV down to 0.15 kpc radius. No evidence was found for the expected temperature increase within similar to 0.25 kpc due to the influence of the SMBH. Within the Bondi radius, the density profile is consistent with rho proportional to r(-1). The lack of a temperature increase inside the Bondi radius suggests that the hot gas structure is not dictated by the SMBH's potential and, together with the shallow density profile, shows that the classical Bondi rate may not reflect the accretion rate on to the SMBH. If this density profile extends in towards the SMBH, the mass accretion rate on to the SMBH could be at least two orders of magnitude less than the Bondi rate, which agrees with Faraday rotation measurements for M87. We discuss the evidence for outflow from the hot gas and the cold gas disc and for cold feedback, where gas cooling rapidly from the hot atmosphere could feed the cirumnuclear disc and fuel the SMBH. At 0.2 kpc radius, the cooler X-ray temperature component represents 20 per cent of the total X-ray gas mass and, by losing angular momentum to the hot gas component, could provide a fuel source of cold clouds within the Bondi radius. C1 [Russell, H. R.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Russell, H. R.; McNamara, B. R.; Broderick, A. E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.; Broderick, A. E.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Russell, HR (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM hrr27@ast.cam.ac.uk FU ERC; Natural Sciences and Engineering Council of Canada; Canadian Space Agency Space Science Enhancement Program; Perimeter Institute for Theoretical Physics; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX We thank the reviewer for helpful and constructive comments. HRR and ACF acknowledge support from ERC Advanced Grant Feedback. BRM acknowledges support from the Natural Sciences and Engineering Council of Canada and the Canadian Space Agency Space Science Enhancement Program. AEB receives financial support from the Perimeter Institute for Theoretical Physics and the Natural Sciences and Engineering Council of Canada through a Discovery Grant. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research and Innovation. We also thank Alastair Edge for helpful discussions. The scientific results reported in this paper are based on data obtained from the Chandra Data Archive. NR 133 TC 14 Z9 14 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 JUL 21 PY 2015 VL 451 IS 1 BP 588 EP 600 DI 10.1093/mnras/stv954 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8AH UT WOS:000360827800044 ER PT J AU Kauffmann, G Huang, ML Moran, S Heckman, TM AF Kauffmann, Guinevere Huang, Mei-Ling Moran, Sean Heckman, Timothy M. TI A systematic study of the inner rotation curves of galaxies observed as part of the GASS and COLD GASS surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: haloes; galaxies: stellar content; galaxies: structure ID DARK-MATTER HALOES; ARECIBO SDSS SURVEY; SPIRAL GALAXIES; MASSIVE GALAXIES; INTERMEDIATE-REDSHIFT; IRREGULAR GALAXIES; LOCAL UNIVERSE; STAR-FORMATION; DISK GALAXIES; STELLAR AB We present a systematic analysis of the rotation curves of 187 galaxies with stellar masses greater than 10(10) M circle dot, with atomic gas masses from the GALEX Arecibo Sloan Survey (GASS) and with follow-up long-slit spectroscopy from the MMT. Our analysis focuses on stellar rotation curves derived by fitting stellar template spectra to the galaxy spectra binned along the slit. In this way, we are able to obtain accurate rotation velocity measurements for a factor of 2 more galaxies than possible with the H alpha line. Galaxies with high atomic gas mass fractions are the most dark-matter-dominated galaxies in our sample and have dark matter halo density profiles that are to first order well described by Navarro Frenk White profiles with an average concentration parameter of 10. The inner slopes of the rotation curves correlate more strongly with stellar population age than with galaxy mass or structural parameters. At fixed stellar mass, the rotation curves of more actively star-forming galaxies have steeper inner slopes than less actively star-forming galaxies. The ratio between the galaxy specific angular momentum and the total specific angular momentum of its dark matter halo, R-j, correlates strongly with galaxy mass, structure and gas content. Low-mass, disc-dominated galaxies with atomic gas mass fractions greater than 20 per cent have median values of R-j of around 1, but massive, bulge-dominated galaxies have R-j = 0.2-0.3. We argue that these trends can be understood in a picture where gas inflows triggered by disc instabilities lead to the formation of passive, bulge-dominated galaxies with low specific angular momentum. C1 [Kauffmann, Guinevere; Huang, Mei-Ling] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Moran, Sean] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Kauffmann, G (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany. EM gamk@mpa-garching.mpg.de NR 40 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 JUL 21 PY 2015 VL 451 IS 1 BP 878 EP 887 DI 10.1093/mnras/stv1014 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ8AH UT WOS:000360827800067 ER PT J AU Wirshing, HH Baker, AC AF Wirshing, Herman H. Baker, Andrew C. TI Molecular and Morphological Species Boundaries in the Gorgonian Octocoral Genus Pterogorgia (Octocorallia: Gorgoniidae) SO PLOS ONE LA English DT Article ID PHYLOGENETIC ANALYSIS; SECONDARY STRUCTURES; DNA-SEQUENCES; CNIDARIA; CORAL; MITOCHONDRIAL; ANTHOZOA; FAMILY; ALCYONACEA; EVOLUTION AB Most gorgonian octocoral species are described using diagnostic characteristics of their sclerites (microscopic skeletal components). Species in the genus Pterogorgia, however, are separated primarily by differences in their calyx and branch morphology. Specimens of a morphologically unusual Pterogorgia collected from Saba Bank in the NE Caribbean Sea were found with calyx morphology similar to P. citrina and branch morphology similar to P. guadalupensis. In order to test morphological species boundaries, and the validity of calyx and branch morphology as systematic characters, a phylogenetic analysis was undertaken utilizing partial gene fragments of three mitochondrial (mtMutS, cytochrome b, and igr4; 726bp total) and two nuclear (ITS2, 166bp; and SRP54 intron, 143bp) loci. The datasets for nuclear and mitochondrial loci contained few phylogenetically informative sites, and tree topologies did not resolve any of the morphological species as monophyletic groups. Instead, the mitochondrial loci and SRP54 each recovered two clades but were slightly incongruent, with a few individuals of P. guadalupensis represented in both clades with SRP54. A concatenated dataset of these loci grouped all P. anceps and P. guadalupensis in a clade, and P. citrina and the Pterogorgia sp. from Saba Bank in a sister clade, but with minimal variation/resolution within each clade. However, in common with other octocoral taxa, the limited genetic variation may not have been able to resolve whether branch variation represents intraspecific variation or separate species. Therefore, these results suggest that there are at least two phylogenetic lineages of Pterogorgia at the species level, and the atypical Pterogorgia sp. may represent an unusual morphotype of P. citrina, possibly endemic to Saba Bank. Branch morphology does not appear to be a reliable morphological character to differentiate Pterogorgia species (e.g., branches "flat" or "3-4 edges" in P. guadalupensis and P. anceps, respectively), and a re-evaluation of species-level characters (e.g., sclerites) is needed. C1 [Wirshing, Herman H.; Baker, Andrew C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, Miami, FL 33149 USA. RP Wirshing, HH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM wirshingh@si.edu FU U.S. National Science Foundation [OCE-0527184]; Rowlands Graduate Fellowship, University of Miami; Knight Graduate Fellowship, University of Miami FX This work was supported by the U.S. National Science Foundation OCE-0527184 to ACB and Rowlands and Knight Graduate Fellowships, University of Miami to HHW. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 1 Z9 1 U1 1 U2 7 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 JUL 21 PY 2015 VL 10 IS 7 AR e0133517 DI 10.1371/journal.pone.0133517 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN6LZ UT WOS:000358547600107 PM 26196389 ER PT J AU Thomaz, AT Arcila, D Orti, G Malabarba, LR AF Thomaz, Andrea T. Arcila, Dahiana Orti, Guillermo Malabarba, Luiz R. TI Molecular phylogeny of the subfamily Stevardiinae Gill, 1858 (Characiformes: Characidae): classification and the evolution of reproductive traits SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Tetras; Neotropical region; "Clade A"; Stevardiinae; Glandulocaudinae; Insemination; Multi-locus phylogeny ID TELEOSTEI OSTARIOPHYSI CHARACIFORMES; GENUS MONOTOCHEIRODON CHARACIFORMES; UPPER RIO PARANA; FISHES TELEOSTEI; HEMIBRYCON CHARACIFORMES; SPECIES TREES; GLANDULOCAUDINAE; SPERM; SEQUENCES; COLOMBIA AB Background: The subfamily Stevardiinae is a diverse and widely distributed clade of freshwater fishes from South and Central America, commonly known as "tetras" (Characidae). The group was named "clade A" when first proposed as a monophyletic unit of Characidae and later designated as a subfamily. Stevardiinae includes 48 genera and around 310 valid species with many species presenting inseminating reproductive strategy. No global hypothesis of relationships is available for this group and currently many genera are listed as incertae sedis or are suspected to be non-monophyletic. Results: We present a molecular phylogeny with the largest number of stevardiine species analyzed so far, including 355 samples representing 153 putative species distributed in 32 genera, to test the group's monophyly and internal relationships. The phylogeny was inferred using DNA sequence data from seven gene fragments (mtDNA: 12S, 16S and COI; nuclear: RAG1, RAG2, MYH6 and PTR). The results support the Stevardiinae as a monophyletic group and a detailed hypothesis of the internal relationships for this subfamily. Conclusions: A revised classification based on the molecular phylogeny is proposed that includes seven tribes and also defines monophyletic genera, including a resurrected genus Eretmobrycon, and new definitions for Diapoma, Hemibrycon, Bryconamericus sensu stricto, and Knodus sensu stricto, placing some small genera as junior synonyms. Inseminating species are distributed in several clades suggesting that reproductive strategy is evolutionarily labile in this group of fishes. C1 [Thomaz, Andrea T.] Univ Michigan, Dept Ecol & Evolutionary Biol EEB, Ann Arbor, MI 48109 USA. [Thomaz, Andrea T.; Malabarba, Luiz R.] Univ Fed Rio Grande do Sul, Dept Zool, BR-90501970 Porto Alegre, RS, Brazil. [Arcila, Dahiana; Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Arcila, Dahiana] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Malabarba, LR (reprint author), Univ Fed Rio Grande do Sul, Dept Zool, Ave Bento Goncalves 9500, BR-90501970 Porto Alegre, RS, Brazil. EM malabarb@ufrgs.br FU DeepFin Student Exchange Program (NSF grant) [DEB-1004765]; NSF grant [DEB-1019308]; CNPQ, Brazilian Government [477318/2012-6, 300705/2010-7] FX Financial support for this study was provided by the DeepFin Student Exchange Program to DA and ATT (NSF grant DEB-1004765), by NSF grant DEB-1019308 (Euteleost Tree of Life) to GO and by CNPQ, Brazilian Government (process 300705/2010-7; 477318/2012-6) to LRM. We thank all collections and people who kindly assisted with the loan of tissues and/or specimens: M. Sabaj Perez (ANSP), N. Lujan and J. Armbruster (AUM), M. Mirande (FML), C. A. Lucena (MCP), R. Covain and S. Fisch-Muller (MHNG), P. A. Buckup and M. Britto (MNRJ), H. Ortega (MUSM), H. Lopez-Fernandez (ROM), R.G. Reina (STRI) and J. Albert (ULL). Thanks to the ichthyologists that helped in confirming the identification of vouchers: T. P. Carvalho, F. Carvalho, J. Anyelo and C. A. Lucena and to J. Burns for providing the unpublished data on the presence or absence of the insemination in some stevardiines. Finally, we are thankful to R. P. Vari and W. Fink for valuable comments on earlier versions of this manuscript. NR 76 TC 7 Z9 8 U1 1 U2 13 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 JUL 21 PY 2015 VL 15 AR 146 DI 10.1186/s12862-015-0403-4 PG 25 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA CN0OM UT WOS:000358113200002 PM 26195030 ER PT J AU Bally, J Mann, RK Eisner, J Andrews, SM Di Francesco, J Hughes, M Johnstone, D Matthews, B Ricci, L Williams, JP AF Bally, John Mann, Rita K. Eisner, Josh Andrews, Sean M. Di Francesco, James Hughes, Meredith Johnstone, Doug Matthews, Brenda Ricci, Luca Williams, Jonathan P. TI ALMA OBSERVATIONS OF THE LARGEST PROTO-PLANETARY DISK IN THE ORION NEBULA, 114-426: A CO SILHOUETTE SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: pre-main sequence ID CIRCUMSTELLAR DISKS; MOLECULAR CLOUD; STAR-FORMATION; GRAIN-GROWTH; PROPLYDS; CLUSTER; PHOTOEVAPORATION; EMISSION; OBJECTS; MASSES AB We present ALMA observations of the largest protoplanetary disk in the Orion Nebula, 114-426. Detectable 345 GHz (856 mu m) dust continuum is produced only in the 350 AU central region of the similar to 1000 AU diameter silhouette seen against the bright Ha background in Hubble Space Telescope images. Assuming optically thin dust emission at 345 GHz, a gas-to-dust ratio of 100, and a grain temperature of 20 K, the disk gas-mass is estimated to be 3.1 +/- 0.6 Jupiter masses. If most solids and ices have been incorporated into large grains, however, this value is a lower limit. The disk is not detected in dense-gas tracers such as HCO+ J = 4-3, HCN J = 4-3, or CS = 7-6. These results may indicate that the 114-426 disk is evolved and depleted in some light organic compounds found in molecular clouds. The CO J = 3-2 line is seen in absorption against the bright 50-80 K background of the Orion A molecular cloud over the full spatial extent and a little beyond the dust continuum emission. The CO absorption reaches a depth of 27 K below the background CO emission at V-LSR approximate to 6.7 km s(-1) similar to 0 ''.52 (210 AU) northeast and 12 K below the background CO emission at V-LSR approximate to 9.7 km s(-1) similar to 0 ''.34 (140 AU) southwest of the suspected location of the central star, implying that the embedded star has a mass less than 1 M-circle dot. C1 [Bally, John] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Mann, Rita K.; Di Francesco, James; Johnstone, Doug; Matthews, Brenda] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Eisner, Josh] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Di Francesco, James; Johnstone, Doug; Matthews, Brenda] Uivers Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Hughes, Meredith] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Ricci, Luca] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96816 USA. RP Bally, J (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, UCB 389, Boulder, CO 80309 USA. EM john.bally@colorado.edu OI Johnstone, Doug/0000-0002-6773-459X; Williams, Jonathan/0000-0001-5058-695X; Di Francesco, James/0000-0002-9289-2450 FU National Science Foundation (NSF) [AST-1009847]; Natural Sciences and Engineering Research Council (NSERC) Discovery Grant; Associated Universities, Inc. FX This research of J.B. was in part supported by National Science Foundation (NSF) grant AST-1009847. D.J. acknowledges support from a Natural Sciences and Engineering Research Council (NSERC) Discovery Grant. This paper uses ALMA data obtained with program ADS/JAO.ALMA#2011.0.00028.S. ALMA is a partnership of the European Southern Observatory (ESO) representing member states, Associated Universities Incorporated (AUI) and the National Radio Astronomy Observatories (NRAO) for the National Science Foundation (NSF) in the USA, NINS in Japan, NRC in Canada, and NSC and ASIAA in Taiwan, in cooperation with the Republic of Chile. The Joint ALMA Observatory (JAO) is operated by ESO (Europe), AUI/NRAO (USA), and NAOJ (Japan). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 30 TC 5 Z9 5 U1 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 69 DI 10.1088/0004-637X/808/1/69 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500069 ER PT J AU Burkhart, B Collins, DC Lazarian, A AF Burkhart, Blakesley Collins, David C. Lazarian, Alex TI OBSERVATIONAL DIAGNOSTICS OF SELF-GRAVITATING MHD TURBULENCE IN GIANT MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: kinematics and dynamics; magnetic fields; magnetohydrodynamics (MHD); molecular data; stars: formation; turbulence ID ADAPTIVE MESH REFINEMENT; INITIAL MASS FUNCTION; SUPERSONIC MAGNETOHYDRODYNAMIC TURBULENCE; DENSITY PROBABILITY-DISTRIBUTION; FIELD STRENGTH FLUCTUATIONS; STAR-FORMATION RATE; ENTROPIC INDEX-Q; INTERSTELLAR TURBULENCE; MAGNETIC-FIELDS; DISTANT HELIOSPHERE AB We study the observable signatures of self-gravitating magnetohydrodynamics (MHD) turbulence by applying the probability density functions (PDFs) and the spatial density power spectrum to synthetic column density maps. We find that there exists three characterizable stages of the evolution of the collapsing cloud which we term "early," "intermediate," and "advanced." At early times, i.e., t < 0.15t(ff), the column density has a power spectral slope similar to nongravitating supersonic turbulence and a lognormal distribution. At an intermediate stage, i.e., 0.15t(ff) < t <= 0.35t(ff), there exist signatures of the first cores in the shallower PDF and power spectrum power-law slopes. The column density PDF power-law tails at these times have line of sight averaged slopes ranging from -2.5 to -1.5 with shallower values belonging to simulations with lower magnetic field strength. The density power spectrum slope becomes shallow and can be characterized by P(k) = A(1)k(beta 2)e(-k/kc), where A(1) describes the amplitude, k(beta 2) describes the classical power-law behavior, and the scale k(c) characterizes the turn over from turbulence dominated to self-gravity dominated. At advanced stages of collapse, i.e., approximate to t > 0.35t(ff), the power spectral slope is positive valued, and a dramatic increase is observed in the PDF moments and the Tsallis incremental PDF parameters, which gives rise to deviations between PDF-sonic Mach number relations. Finally, we show that the imprint of gravity on the density power spectrum can be replicated in non-gravitating turbulence by introducing a delta-function with amplitude equivalent to the maximum valued point in a given self-gravitating map. We find that the turbulence power spectrum restored through spatial filtering of the high density material. C1 [Burkhart, Blakesley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Collins, David C.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Lazarian, Alex] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Burkhart, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA Einstein Fellowship; NSF grant [AST 1212096]; Center for Magnetic Self-organization in Laboratory and Astrophysical Plasmas (CMSO) FX The authors would like to thank the referee for constructive comments and suggestions which greatly improved this paper. B.B. is grateful for support from the NASA Einstein Fellowship. A.L. is supported by the NSF grant AST 1212096. B.B. and A.L. are grateful for support from the Center for Magnetic Self-organization in Laboratory and Astrophysical Plasmas (CMSO). Computer time was provided through NSF TRAC allocations TG-AST090110 and TG-MCA07S014 and the XSEDE allocation TG-AST140008. The computations were performed on Nautilus and Kraken at the National Institute for Computational Sciences (http://www.nics.tennessee.edu/) and on Stampede and Maverick at the Texas Advanced Computing Center (https://www.tacc.utexas.edu). NR 101 TC 11 Z9 11 U1 1 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 JUL 20 PY 2015 VL 808 IS 1 AR 48 DI 10.1088/0004-637X/808/1/48 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500048 ER PT J AU Dunn, JP Wasik, B Holtzclaw, CL Yenerall, D Bautista, M Arav, N Hayes, D Moe, M Ho, LC Dutton, SH AF Dunn, Jay P. Wasik, Branden Holtzclaw, Christin L. Yenerall, David Bautista, Manuel Arav, Nahum Hayes, Daniel Moe, Max Ho, Luis C. Dutton, S. Harper TI DETERMINING THE LOCATIONS OF DUST SOURCES IN FeLoBAL QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; quasars: absorption lines ID BROAD-ABSORPTION-LINE; DIGITAL SKY SURVEY; LARGE TELESCOPE OBSERVATIONS; GALACTIC NUCLEUS FEEDBACK; EMISSION-LINE; REDDENED QUASARS; STELLAR OBJECTS; OUTFLOW CONTRIBUTION; SEYFERT-GALAXIES; SDSS J0318-0600 AB We conduct a spectroscopic search of quasars observed by the Sloan Digital Sky Survey (SDSS) with broad absorption line (BAL) troughs due to Mg II and troughs due to Fe II that simultaneously exhibit strong Balmer narrow emission lines (NELs). We find that in a redshift range of 0.4 <= z <= 0.9, approximately 23 of the 70 Mg II BALs and 4 of a subset of 15 Fe II BALs exhibit strong Balmer emission. We also find significant fractions of Mg II BALs (approximately 23%) and those Mg II BALs with Fe II troughs (approximately 27%) have strong continuum reddening, E(B - V) >= 0.1. From measurements of the Balmer decrement in three objects, we find similarly significant reddening of the NEL region in three of the four objects; the NELs in the fourth object are not measurable. We also include one object in this study not taken from the SDSS sample that shows Fe II absorption and strong narrow emission, but due to measurement uncertainty and low continuum reddening the comparison is consistent but inconclusive. We find a trend in both the Mg II and Fe II BAL samples between the NEL reddening and continuum reddening. Because the narrow line reddening is consistent with the continuum reddening in every object in the two SDSS samples, it suggests that the reddening sources in these objects likely exist at larger radial distances than the narrow line regions from the central nucleus. C1 [Dunn, Jay P.; Wasik, Branden; Holtzclaw, Christin L.; Yenerall, David; Hayes, Daniel; Dutton, S. Harper] Georgia Perimeter Coll, Dept Phys Sci, Dunwoody, GA 30338 USA. [Bautista, Manuel] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Arav, Nahum] Virginia Tech, Dept Phys, Blacksburg, VA 24060 USA. [Moe, Max] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Luis C.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. RP Dunn, JP (reprint author), Georgia Perimeter Coll, Dept Phys Sci, Dunwoody, GA 30338 USA. EM jdunn@gpc.edu FU Kavli Foundation, Peking University; Chinese Academy of Sciences; Carnegie Institution for Science FX L.C.H. acknowledges additional support from the Kavli Foundation, Peking University, the Chinese Academy of Sciences, and the Carnegie Institution for Science. NR 52 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 JUL 20 PY 2015 VL 808 IS 1 AR 94 DI 10.1088/0004-637X/808/1/94 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500094 ER PT J AU Ferre-Mateu, A Mezcua, M Trujillo, I Balcells, M van den Bosch, RCE AF Ferre-Mateu, Anna Mezcua, Mar Trujillo, Ignacio Balcells, Marc van den Bosch, Remco C. E. TI MASSIVE RELIC GALAXIES CHALLENGE THE CO-EVOLUTION OF SUPER-MASSIVE BLACK HOLES AND THEIR HOST GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: evolution; galaxies: formation; galaxies: nuclei; galaxies: stellar content ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; VELOCITY DISPERSION EVOLUTION; STAR-FORMATION HISTORIES; MILES SPECTRAL COVERAGE; SIZE EVOLUTION; ELLIPTIC GALAXIES; MINOR MERGERS; NGC 1277; SCALING RELATIONS AB We study a sample of eight massive galaxies that are extreme outliers (3-5s) in the M-center dot-Mbulge local scaling relation. Two of these galaxies are confirmed to host extremely large super-massive black holes (SMBHs), whereas the virial mass estimates for the other six are also consistent with having abnormally large SMBHs. From the analysis of their star formation histories and their structural properties, we find that all of these extreme outliers can be considered to be relic galaxies from the early (z similar to 2) universe: i.e., they are compact (R-e < 2 kpc) and have purely old stellar populations (t greater than or similar to 10 Gyr). In order to explain the nature of such deviations from the local relations, we propose a scenario in which the hosts of these uber-massive SMBHs are galaxies that have followed a different evolutionary path than the two-phase growth channel assumed for massive galaxies. Once the SMBH and the core of the galaxy are formed at z similar to 2, the galaxy skips the second phase, remaining structurally untouched and without further mass and size increase. We show that if the outliers had followed the normal evolutionary path by growing in size via merger activity, the expected (mild) growth in mass would place them closer to the observed local relations. Our results suggest that the SMBH growth epoch for the most massive galaxies stopped similar to 10 Gyr ago. C1 [Ferre-Mateu, Anna] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Mezcua, Mar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mezcua, Mar; Trujillo, Ignacio] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Mezcua, Mar; Trujillo, Ignacio] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Balcells, Marc] Isaac Newton Grp Telescopes, E-38700 Tenerife, Spain. [van den Bosch, Remco C. E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Ferre-Mateu, A (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA. EM aferre@naoj.org OI van den Bosch, Remco/0000-0002-0420-6159; Ferre-Mateu, Anna/0000-0002-6411-220X; Trujillo, Ignacio/0000-0001-8647-2874; Mezcua, Mar/0000-0003-4440-259X FU Japan Society for the Promotion of Science (JSPS) [23224005]; Spanish Ministerio de Economia y Competitividad (MINECO) [AYA2009-11137, AYA2011-25527, AYA2013-48226-C3-1-P] FX This work was supported by the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for Scientific Research (KAKENHI) Number 23224005 and by the Spanish Ministerio de Economia y Competitividad (MINECO; grants AYA2009-11137, AYA2011-25527, and AYA2013-48226-C3-1-P). NR 72 TC 14 Z9 14 U1 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 79 DI 10.1088/0004-637X/808/1/79 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500079 ER PT J AU Gentry, ES Marshall, HL Hardcastle, MJ Perlman, ES Birkinshaw, M Worrall, DM Lenc, E Siemiginowska, A Urry, CM AF Gentry, Eric S. Marshall, Herman L. Hardcastle, Martin J. Perlman, Eric S. Birkinshaw, Mark Worrall, Diana M. Lenc, Emil Siemiginowska, Aneta Urry, C. Megan TI OPTICAL DETECTION OF THE PICTOR A JET AND TIDAL TAIL: EVIDENCE AGAINST AN IC/CMB JET SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Pictor A); galaxies: jets; X-rays: galaxies ID X-RAY-EMISSION; HUBBLE-SPACE-TELESCOPE; QUASAR JETS; RADIO JETS; 3C 273; CHANDRA; 3C-273; GALAXY; SPECTRA AB New images of the FR II radio galaxy Pictor A from the Hubble Space Telescope reveal a previously undiscovered tidal tail, as well as a number of jet knots coinciding with a known X-ray and radio jet. The tidal tail is approximately 5 '' wide (3 kpc projected), starting 18 '' (12 kpc) from the center of Pictor A, and extends more than 90 '' (60 kpc). The knots are part of a jet observed to be about 4' (160 kpc) long, extending to a bright hotspot. These images are the first optical detections of this jet, and by extracting knot flux densities through three filters, we set constraints on emission models. While the radio and optical flux densities are usually explained by synchrotron emission, there are several emission mechanisms that might be used to explain the X-ray flux densities. Our data rule out Doppler-boosted inverse Compton scattering as a source of the high-energy emission. Instead, we find that the observed emission can be well described by synchrotron emission from electrons with a low-energy index (p similar to 2) that dominates the radio band, while a high-energy index (p similar to 3) is needed for the X-ray band and the transition occurs in the optical/infrared band. This model is consistent with a continuous electron injection scenario. C1 [Gentry, Eric S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Gentry, Eric S.; Marshall, Herman L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hardcastle, Martin J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Birkinshaw, Mark; Worrall, Diana M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Birkinshaw, Mark; Worrall, Diana M.; Siemiginowska, Aneta] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lenc, Emil] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Lenc, Emil] ARC Ctr Excellence All sky Astrophys CAASTRO, Canberra, ACT, Australia. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06511 USA. RP Gentry, ES (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, 1156 High St, Santa Cruz, CA 95064 USA. EM egentry@ucsc.edu; hermanm@space.mit.edu; m.j.hardcastle@herts.ac.uk; eperlman@fit.edu; Mark.Birkinshaw@bristol.ac.uk; D.Worrall@bristol.ac.uk; e.lenc@physics.usyd.edu.au; aneta@head.cfa.harvard.edu; meg.urry@yale.edu OI Gentry, Eric/0000-0002-4906-3745; Birkinshaw, Mark/0000-0002-1858-277X; Lenc, Emil/0000-0002-9994-1593; Urry, Meg/0000-0002-0745-9792; Hardcastle, Martin/0000-0003-4223-1117 FU National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory [SV3-73016]; Chandra X-Ray Center; National Aeronautics Space Administration [NAS8-03060]; [CE110001020] FX We thank the referee for useful feedback that helped improve the quality of this work. Support for this work was provided by the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. The Centre for All-sky Astrophysics (CAASTRO) is an Australian Research Council Centre of Excellence, funded by grant CE110001020. NR 27 TC 5 Z9 5 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 JUL 20 PY 2015 VL 808 IS 1 AR 92 DI 10.1088/0004-637X/808/1/92 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500092 ER PT J AU Matthews, LD Reid, MJ Menten, KM AF Matthews, L. D. Reid, M. J. Menten, K. M. TI NEW MEASUREMENTS OF THE RADIO PHOTOSPHERE OF MIRA BASED ON DATA FROM THE JVLA AND ALMA SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: AGB and post-AGB; stars: atmospheres; stars: fundamental parameters; stars: imaging ID VY CANIS MAJORIS; SYMBIOTIC STARS; VARIABLE-STARS; O-CETI; BINARY; EMISSION; INTERFEROMETRY; CONVECTION; ATMOSPHERE; LUMINOSITY AB We present new measurements of the millimeter wavelength continuum emission from the long period variable Mira (o Ceti) at frequencies of 46, 96, and 229 GHz (lambda approximate to 7, 3, and 1 mm) based on observations obtained with the Jansky Very Large Array (JVLA) and the Atacama Large Millimeter/submillimeter Array (ALMA). The measured millimeter flux densities are consistent with a radio photosphere model derived from previous observations, where flux density S-nu alpha nu(1.86). The stellar disk is resolved, and the measurements indicate a decrease in the size of the radio photosphere at higher frequencies, as expected if the opacity decreases at shorter wavelengths. The shape of the radio photosphere is found to be slightly elongated, with a flattening of similar to 10%-20%. The data also reveal evidence for brightness non-uniformities on the surface of Mira at radio wavelengths. Mira's hot companion, Mira B was detected at all three observed wavelengths, and we measure a radius for its radio-emitting surface of approximate to 2.0 x 10(13) cm. The data presented here highlight the power of the JVLA and ALMA for the study of the atmospheres of evolved stars. C1 [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Matthews, LD (reprint author), MIT, Haystack Observ, Off Route 40, Westford, MA 01886 USA. EM lmatthew@haystack.mit.edu FU Associated Universities, Inc. FX The authors thank T. Kaminski for valuable discussions and E. Greisen for developments in AIPS that aided this work. The JVLA observations presented here were part of NRAO program 14A-026. This paper makes use of the following ALMA data: ADS/JAO.ALMA #2011.0.00014.SV. 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. NR 51 TC 5 Z9 5 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 JUL 20 PY 2015 VL 808 IS 1 AR 36 DI 10.1088/0004-637X/808/1/36 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500036 ER PT J AU Minh, YC Liu, HB Su, YN Hsieh, PY Liu, SY Kim, SS Wright, M Ho, PTP AF Minh, Young Chol Liu, Hauyu Baobab Su, Yu-Nung Hsieh, Pei-Ying Liu, Sheng-Yuan Kim, Sungsoo S. Wright, Melvyn Ho, Paul T. P. TI EMISSION IN THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; ISM: individual objects (Sgr A, Circumnuclear Disk); ISM: molecules; radio lines: ISM; submillimeter: galaxies ID APERTURE SYNTHESIS OBSERVATIONS; SUPERMASSIVE BLACK-HOLE; SGR A-ASTERISK; CIRCUMNUCLEAR DISK; MOLECULAR ENVIRONMENT; STELLAR ORBITS; STAR-FORMATION; INFALLING GAS; CENTER REGION; SIO EMISSION AB The gas traced by the SiO 1-0 emission appears to not have a direct connection or interaction with the circumnuclear disk (CND). In contrast, higher-resolution observations of the SiO 5-4 emission confirm the dissymmetric gas distribution of the CND, as well as a large concentration of gas in the CND's southwest region. In particular, the SiO 5-4 emission peaks toward what is likely the "convergent" position, where the west arc of Sgt A West overlaps with the CND. We think that this is the position where several incoming and outgoing gas flows interact with each other. The high angular resolution (approximate to 1 ''.5) observations of the SiO 5-4 emission show several emission clumps with sizes similar to 2 ''. These clumps have different velocities that may have resulted from a collision with incoming clouds. We confirm that the overall fractional abundance of SiO is about 10-9 relative to the total H-2, and it probably resulted from the large-scale shocks prevalent in the Galactic center region. A comparison of the SiO fractional abundance suggests that in addition to the dense ambient cloud component, which surrounds but does not interact much with the CND, there are separate gas components that have more interactions with the CND. C1 [Minh, Young Chol] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Liu, Hauyu Baobab; Su, Yu-Nung; Hsieh, Pei-Ying; Liu, Sheng-Yuan; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Kim, Sungsoo S.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Kyungki Do, South Korea. [Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Minh, YC (reprint author), Korea Astron & Space Sci Inst, 776 Daeduk Daero, Taejon 305348, South Korea. NR 41 TC 0 Z9 0 U1 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 86 DI 10.1088/0004-637X/808/1/86 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500086 ER PT J AU Mobasher, B Dahlen, T Ferguson, HC Acquaviva, V Barro, G Finkelstein, SL Fontana, A Gruetzbauch, R Johnson, S Lu, Y Papovich, CJ Pforr, J Salvato, M Somerville, RS Wiklind, T Wuyts, S Ashby, MLN Bell, E Conselice, CJ Dickinson, ME Faber, SM Fazio, G Finlator, K Galametz, A Gawiser, E Giavalisco, M Grazian, A Grogin, NA Guo, YC Hathi, N Kocevski, D Koekemoer, AM Koo, DC Newman, JA Reddy, N Santini, P Wechsler, RH AF Mobasher, Bahram Dahlen, Tomas Ferguson, Henry C. Acquaviva, Viviana Barro, Guillermo Finkelstein, Steven L. Fontana, Adriano Gruetzbauch, Ruth Johnson, Seth Lu, Yu Papovich, Casey J. Pforr, Janine Salvato, Mara Somerville, Rachel S. Wiklind, Tommy Wuyts, Stijn Ashby, Matthew L. N. Bell, Eric Conselice, Christopher J. Dickinson, Mark E. Faber, Sandra M. Fazio, Giovanni Finlator, Kristian Galametz, Audrey Gawiser, Eric Giavalisco, Mauro Grazian, Andrea Grogin, Norman A. Guo, Yicheng Hathi, Nimish Kocevski, Dale Koekemoer, Anton M. Koo, David C. Newman, Jeffrey A. Reddy, Naveen Santini, Paola Wechsler, Risa H. TI A CRITICAL ASSESSMENT OF STELLAR MASS MEASUREMENT METHODS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: distances and redshifts; galaxies: high-redshift; galaxies: photometry; surveys ID LYMAN-BREAK GALAXIES; ULTRA-DEEP FIELD; SPACE-TELESCOPE OBSERVATIONS; EXTRAGALACTIC LEGACY SURVEY; STAR-FORMATION HISTORIES; BROAD-BAND PHOTOMETRY; SIMILAR-TO 7; POPULATION SYNTHESIS; LUMINOSITY FUNCTION; NEBULAR EMISSION AB This is the second paper in a series aimed at investigating the main sources of uncertainty in measuring the observable parameters in galaxies from their spectral energy distributions (SEDs). In the first paper we presented a detailed account of the photometric redshift measurements and an error analysis of this process. In this paper we perform a comprehensive study of the main sources of random and systematic error in stellar mass estimates for galaxies, and their relative contributions to the associated error budget. Since there is no prior knowledge of the stellar mass of galaxies (unlike their photometric redshifts), we use mock galaxy catalogs with simulated multi-waveband photometry and known redshift, stellar mass, age and extinction for individual galaxies. The multi-waveband photometry for the simulated galaxies were generated in 13 filters spanning from U-band to mid- infrared wavelengths. Given different parameters affecting stellar mass measurement (photometric signal-to-noise ratios (S/N), SED fitting errors and systematic effects), the inherent degeneracies and correlated errors, we formulated different simulated galaxy catalogs to quantify these effects individually. For comparison, we also generated catalogs based on observed photometric data of real galaxies in the Great Observatories Origins Deep Survey-South field, spanning the same passbands. The simulated and observed catalogs were provided to a number of teams within the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey collaboration to estimate the stellar masses for individual galaxies. A total of 11 teams participated, with different combinations of stellar mass measurement codes/methods, population synthesis models, star formation histories, extinction and age. For each simulated galaxy, the differences between the input stellar masses, M-input, and those estimated by each team, M-est, is defined as Delta log(M) equivalent to log(M-estimated) - log(M-input), and used to identify the most fundamental parameters affecting stellar mass estimate in galaxies, with the following results. (1) No significant bias in Delta log(M) was found among different codes, with all having comparable scatter (sigma(Dlog(M))= 0.136 dex). The estimated stellar mass values are seriously affected by low photometric S/N, with the rms scatter increasing for galaxies with H-AB > 26 mag; (2) A source of error contributing to the scatter in Delta log(M) is found to be due to photometric uncertainties (0.136 dex) and low resolution in age and extinction grids when generating the SED templates; (3) The median of stellar masses among different methods provides a stable measure of the mass associated with any given galaxy (sigma(Delta log(M)) = 0.142 dex); (4) The Delta log(M) values are strongly correlated with deviations in age (defined as the difference between the estimated and expected values), with a weaker correlation with extinction; (5) The rms scatter in the estimated stellar masses due to free parameters (after fixing redshifts and initial mass function) are quantified and found to be sigma(Delta log(M)) = 0.110 dex; (6) Using the observed data, we studied the sensitivity of stellar masses to both the population synthesis codes and inclusion of nebular emission lines and found them to affect the stellar mass by 0.2 and 0.3 dex respectively. C1 [Mobasher, Bahram; Reddy, Naveen] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Dahlen, Tomas; Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Acquaviva, Viviana] CUNY, NYC Coll Technol, Dept Phys, Brooklyn, NY 11201 USA. [Barro, Guillermo; Faber, Sandra M.; Guo, Yicheng; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Finkelstein, Steven L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Fontana, Adriano; Galametz, Audrey; Grazian, Andrea; Santini, Paola] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Gruetzbauch, Ruth] Observ Astron Lisboa, Ctr Astron & Astrophys, P-1349018 Lisbon, Portugal. [Johnson, Seth; Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Lu, Yu; Wechsler, Risa H.] Stanford Univ, Kavli Inst Particle Phys & Cosmol, Stanford, CA 94305 USA. [Papovich, Casey J.] Texas A&M Res Fdn, Dept Phys & Astron, College Stn, TX 77843 USA. [Pforr, Janine; Dickinson, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Salvato, Mara; Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Somerville, Rachel S.; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Wiklind, Tommy] Joint ALMA Observ, Santiago, Chile. [Ashby, Matthew L. N.; Fazio, Giovanni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bell, Eric] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Finlator, Kristian] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-1168 Copenhagen, Denmark. [Hathi, Nimish] LAM Lab Astrophys Marseille, F-13388 Marseille 13, France. [Kocevski, Dale] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Newman, Jeffrey A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Mobasher, B (reprint author), Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. RI Hathi, Nimish/J-7092-2014; OI Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873; Hathi, Nimish/0000-0001-6145-5090; Santini, Paola/0000-0002-9334-8705 NR 44 TC 18 Z9 18 U1 1 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 JUL 20 PY 2015 VL 808 IS 1 AR 101 DI 10.1088/0004-637X/808/1/101 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500101 ER PT J AU Pennucci, TT Possenti, A Esposito, P Rea, N Haggard, D Baganoff, FK Burgay, M Zelati, FC Israel, GL Minter, A AF Pennucci, T. T. Possenti, A. Esposito, P. Rea, N. Haggard, D. Baganoff, F. K. Burgay, M. Zelati, F. Coti Israel, G. L. Minter, A. TI SIMULTANEOUS MULTI-BAND RADIO AND X-RAY OBSERVATIONS OF THE GALACTIC CENTER MAGNETAR SGR 1745-2900 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; pulsars: individual (PSR J1745-2900, SGR 1745-2900); stars: magnetars ID GIGAHERTZ-PEAKED SPECTRA; SAGITTARIUS-A-ASTERISK; CENTER PULSAR POPULATION; SUPERMASSIVE BLACK-HOLE; SOFT GAMMA-REPEATERS; NEUTRON-STARS; FLUX-DENSITY; MAGNETOTHERMAL EVOLUTION; BROADENING MEASUREMENTS; DISPERSION MEASURE AB We report on multi-frequency, wideband radio observations of the Galactic Center magnetar (SGR 1745-2900) with the Green Bank Telescope for similar to 100 days immediately following its initial X-ray outburst in 2013 April. We made multiple simultaneous observations at 1.5, 2.0, and 8.9 GHz, allowing us to examine the magnetar's flux evolution, radio spectrum, and interstellar medium parameters (such as the dispersion measure (DM), the scattering timescale, and its index). During two epochs, we have simultaneous observations from the Chandra X-ray Observatory, which permitted the absolute alignment of the radio and X-ray profiles. As with the two other radio magnetars with published alignments, the radio profile lies within the broad peak of the X-ray profile, preceding the X-ray profile maximum by similar to 0.2 rotations. We also find that the radio spectral index gamma is significantly negative between similar to 2 and 9 GHz; during the final similar to 30 days of our observations gamma similar to -1.4, which is typical of canonical pulsars. The radio flux has not decreased during this outburst, whereas the long-term trends in the other radio magnetars show concomitant fading of the radio and X-ray fluxes. Finally, our wideband measurements of the DMs taken in adjacent frequency bands in tandem are stochastically inconsistent with one another. Based on recent theoretical predictions, we consider the possibility that the DM is frequency-dependent. Despite having several properties in common with the other radio magnetars, such as L-X,L-qui/L-rot less than or similar to 1, an increase in the radio flux during the X-ray flux decay has not been observed thus far in other systems. C1 [Pennucci, T. T.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Possenti, A.; Burgay, M.] Osservatorio Astron Cagliari, I-09047 Cagliari, Italy. [Esposito, P.] INAF, Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rea, N.; Zelati, F. Coti] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Rea, N.] CSIC, IEEC, Inst Space Sci ICE, E-08193 Barcelona, Spain. [Haggard, D.] Amherst Coll, Dept Phys & Astron, Amherst, MA 01002 USA. [Baganoff, F. K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Zelati, F. Coti] Univ Insubria, I-22100 Como, Italy. [Zelati, F. Coti] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Israel, G. L.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Minter, A.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. RP Pennucci, TT (reprint author), Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA. EM pennucci@virginia.edu OI Burgay, Marta/0000-0002-8265-4344; Israel, GianLuca/0000-0001-5480-6438; Esposito, Paolo/0000-0003-4849-5092; Rea, Nanda/0000-0003-2177-6388 FU National Science Foundation [0968296]; US. Department of State; Chandra X-ray Observatory Award [GO3-14121X]; NASA [NAS8-03060, NNX14AC30G]; NWO; European COST Action [MP1304]; [AYA2012-39303]; [SGR2014-1073] FX The authors would like to thank S. Ransom and P. Demorest for useful discussions and comments, as well as A. Bilous for significant contributions and a review of the manuscript. T. T. P. would also like to acknowledge the hospitality of the astronomers at the Osservatorio Astronomico di Cagliari, where this paper began. T. T. P. is supported in part by a National Science Foundation PIRE Grant (0968296) through NANOGrav and is a graduate student at the National Radio Astronomy Observatory (NRAO). The NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. P. E. acknowledges a Fulbright Research Scholar grant administered by the US-Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. The Fulbright Scholar Program is sponsored by the US. Department of State and administered by CIES, a division of IIE. D. H. acknowledges support from Chandra X-ray Observatory Award Number GO3-14121X, operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060, and also by NASA Swift grant NNX14AC30G. N. R. and F. C. Z. are supported by an NWO Vidi Grant (PI: N. Rea) and by the European COST Action MP1304 (NewCOMPSTAR). N. R. acknowledges support by grants AYA2012-39303 and SGR2014-1073. NR 80 TC 4 Z9 4 U1 0 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 JUL 20 PY 2015 VL 808 IS 1 AR 81 DI 10.1088/0004-637X/808/1/81 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500081 ER PT J AU Rubin, KHR Hennawi, JF Prochaska, JX Simcoe, RA Myers, A Lau, MW AF Rubin, Kate H. R. Hennawi, Joseph F. Prochaska, J. Xavier Simcoe, Robert A. Myers, Adam Lau, Marie Wingyee TI DISSECTING THE GASEOUS HALOS OF z similar to 2 DAMPED Ly alpha SYSTEMS WITH CLOSE QUASAR PAIRS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: halos; galaxies: ISM; quasars: absorption lines ID STAR-FORMING GALAXIES; MASS-METALLICITY RELATION; DIGITAL SKY SURVEY; MG II ABSORPTION; OSCILLATION SPECTROSCOPIC SURVEY; GRAVITATIONALLY LENSED QUASAR; OPTICALLY THICK ABSORBERS; BARYONIC STRUCTURE SURVEY; REST-FRAME ULTRAVIOLET; LYMAN BREAK GALAXIES AB We use spectroscopy of close pairs of quasars to study diffuse gas in the circumgalactic medium (CGM) surrounding a sample of 40 damped Ly alpha systems (DLAs). The primary sightline in each quasar pair probes an intervening DLA in the redshift range 1.6 < z(DLA) < 3.6, such that the second quasar sightline then probes Ly alpha, C II, Si II, and C IV absorption in the CGM transverse to the DLA to projected distances R-perpendicular to < 300 kpc. Analysis of the Ly alpha profiles in these CGM sightlines constrains the covering fraction (f(C)) of optically thick H I (having column density N-H (I) > 10(17.2) cm(-2)) to be greater than or similar to 30% within R-perpendicular to < 200 kpc. Strong Si II lambda 1526 absorption with equivalent width W-1526 > 0.2 angstrom occurs with an incidence f(C) (W-1526 > 0.2 angstrom) = 20(-8)(+12) within R-perpendicular to < 100 kpc, indicating that Si II absorption associated with DLAs probes material within a physical distance R-3D less than or similar to 30 kpc. However, we find that strong C IV lambda 1548 absorption is ubiquitous in these environments (f(C)(W-1548 > 0.2 angstrom) = 57(-13)(+12)% within R-perpendicular to < 100 kpc), and in addition exhibits a high degree of kinematic coherence on scales up to similar to 175 kpc. We infer that this high-ionization material arises predominantly in large, quiescent structures extending beyond the scale of the DLA host dark matter halos rather than in ongoing galactic winds. The Ly alpha equivalent width in the DLA-CGM is anticorrelated with R-perpendicular to at > 98% confidence, suggesting that DLAs arise close to the centers of their host halos rather than on their outskirts. Finally, the average Ly alpha, and C II and C IV equivalent widths measured as a function of R-perpendicular to are consistent with those measured around z similar to 2 Lyman break galaxies. Assuming that DLAs trace a galaxy population at lower masses and luminosities, this finding implies that the absorption strength of cool circumgalactic material has a weak dependence on dark matter halo mass at M-h less than or similar to 10(12) M-circle dot. C1 [Rubin, Kate H. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rubin, Kate H. R.; Hennawi, Joseph F.; Prochaska, J. Xavier] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Prochaska, J. Xavier; Lau, Marie Wingyee] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Simcoe, Robert A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Myers, Adam] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82072 USA. RP Rubin, KHR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM krubin@cfa.harvard.edu FU Alexander von Humboldt foundation; German Federal Ministry for Education and Research; National Science Foundation (NSF) [AST-1010004, AST-1109452, AST-1109447, AST-1412981]; W.M. Keck Foundation; Clay Postdoctoral Fellowship FX The authors wish to thank Sara Ellison, Crystal Martin, and George Djorgovski for aiding in collection and reduction of the Keck/ESI spectroscopy used in this study. We also wish to thank the anonymous referee for useful comments which improved the manuscript. It is our pleasure to thank Neil Crighton, Simeon Bird, Jeff Cooke, Claude-Andre Faucher-Giguere, Michele Fumagalli, John O'Meara, Celine Peroux, Ali Rahmati, and Sijing Shen for valuable discussion of this work, and to acknowledge Sijing Shen for sharing the results of her analysis of the CGM properties of the Eris2 simulation. Finally, we are grateful to Art Wolfe for sharing his insight on these results and for his inspiring and pioneering work in this field. K.H.R.R. acknowledges the generous support of the Clay Postdoctoral Fellowship, and J.F.H. acknowledges support from the Alexander von Humboldt foundation in the context of the Sofja Kovalevskaja Award. The Humboldt foundation is funded by the German Federal Ministry for Education and Research. J.X.P. and M.L. acknowledge support from National Science Foundation (NSF) grants AST-1010004, AST-1109452, AST-1109447, and AST-1412981. This paper includes data gathered with the 6.5m Magellan Telescopes located at Las Campanas Observatory, Chile. 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. NR 108 TC 7 Z9 7 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 JUL 20 PY 2015 VL 808 IS 1 AR 38 DI 10.1088/0004-637X/808/1/38 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500038 ER PT J AU Swartz, DA Pavlov, GG Clarke, T Castelletti, G Zavlin, VE Bucciantini, N Karovska, M van der Horst, AJ Yukita, M Weisskopf, MC AF Swartz, Douglas A. Pavlov, George G. Clarke, Tracy Castelletti, Gabriela Zavlin, Vyacheslav E. Bucciantini, Niccolo Karovska, Margarita van der Horst, Alexander J. Yukita, Mihoko Weisskopf, Martin C. TI HIGH SPATIAL RESOLUTION X-RAY SPECTROSCOPY OF THE IC 443 PULSAR WIND NEBULA AND ENVIRONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G189.22+2.90, IC 443); ISM: supernova remnants; stars: neutron; X-rays: individual (CXOU J061705.3+222127); X-rays: ISM ID SUPERNOVA REMNANT IC-443; BOW-SHOCK NEBULAE; VELA PULSAR; EMISSION; ROTATION; SPECTRUM; JET AB Deep Chandra ACIS observations of the region around the putative pulsar, CXOU J061705.3+222127, in the supernova remnant (SNR) IC 443 reveal an similar to 5 '' radius ring-like structure surrounding the pulsar and a jet-like feature oriented roughly north-south across the ring and through the pulsar's location at 06(h)17(m)5(s).200 + 22 degrees 21' 27 ''.52 (J2000.0 coordinates). The observations further confirm that (1) the spectrum and flux of the central object are consistent with a rotation-powered pulsar, (2) the non-thermal spectrum and morphology of the surrounding nebula are consistent with a pulsar wind, and (3) the spectrum at greater distances is consistent with thermal emission from the SNR. The cometary shape of the nebula, suggesting motion toward the southwest, appears to be subsonic: There is no evidence either spectrally or morphologically for a bow shock or contact discontinuity; the nearly circular ring is not distorted by motion through the ambient medium; and the shape near the apex of the nebula is narrow. Comparing this observation with previous observations of the same target, we set a 99% confidence upper limit to the proper motion of CXOU J061705.3+222127 to be less than 44 mas yr(-1) (310 km s(-1) for a distance of 1.5 kpc), with the best-fit (but not statistically significant) projected direction toward the west. C1 [Swartz, Douglas A.; Zavlin, Vyacheslav E.] NASA, USRA, Astrophys Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Pavlov, George G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Clarke, Tracy] Naval Res Lab, Remote Sensing Div, Washington, DC USA. [Castelletti, Gabriela] UBA, CONICET, IAFE, Buenos Aires, DF, Argentina. [Bucciantini, Niccolo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Bucciantini, Niccolo] INFN Sez Firenze, I-50019 Florence, Italy. [Karovska, Margarita] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [van der Horst, Alexander J.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Yukita, Mihoko] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Yukita, Mihoko] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Weisskopf, Martin C.] NASA, Astrophys Off, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Swartz, DA (reprint author), NASA, USRA, Astrophys Off, Marshall Space Flight Ctr, ZP12, Huntsville, AL 35812 USA. RI Yukita, Mihoko/E-4135-2017; OI Bucciantini, Niccolo'/0000-0002-8848-1392 FU National Aeronautics Space Administration [NAS8-03060]; 6.1 Base funding FX The Chandra observations were obtained in response to Chandra Proposal Number 13500093 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. Optical observations were obtained with the SARA Observatory 0.9 m telescope at Kitt Peak, which is owned and operated by the Southeastern Association for Research in Astronomy. Basic research in radio astronomy at the Naval Research Laboratory (TC) is supported by 6.1 Base funding. NR 36 TC 1 Z9 1 U1 1 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 JUL 20 PY 2015 VL 808 IS 1 AR 84 DI 10.1088/0004-637X/808/1/84 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500084 ER PT J AU Temim, T Slane, P Kolb, C Blondin, J Hughes, JP Bucciantini, N AF Temim, Tea Slane, Patrick Kolb, Christopher Blondin, John Hughes, John P. Bucciantini, Niccolo TI LATE-TIME EVOLUTION OF COMPOSITE SUPERNOVA REMNANTS: DEEP CHANDRA OBSERVATIONS AND HYDRODYNAMICAL MODELING OF A CRUSHED PULSAR WIND NEBULA IN SNR G327.1-1.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (G327.1-1.1); ISM: supernova remnants; pulsars: general; radiation mechanisms: non-thermal; stars: neutron ID AREA TELESCOPE OBSERVATIONS; X-RAY; EMISSION AB In an effort to better understand the evolution of composite supernova remnants (SNRs) and the eventual fate of relativistic particles injected by their pulsars, we present a multifaceted investigation of the interaction between a pulsar wind nebula (PWN) and its host SNR G327.1-1.1. Our 350 Chandra X-ray observations of SNR G327.1-1.1 reveal a highly complex morphology: a cometary structure resembling a bow shock, prong-like features extending into large arcs in the SNR interior, and thermal emission from the SNR shell. Spectral analysis of the non-thermal emission offers clues about the origin of the PWN structures, while enhanced abundances in the PWN region provide evidence for a mixing of supernova ejecta with PWN material. The overall morphology and spectral properties of the SNR suggest that the PWN has undergone an asymmetric interaction with the SNR reverse shock (RS), whichcan occur as a result of a density gradient in the ambient medium and/or a moving pulsar that displaces the PWN from the center of the remnant. We present hydrodynamical simulations of G327.1-1.1 that show that its morphology and evolution can be described by a similar to 17,000-year-old composite SNR that expanded into a density gradient with an orientation perpendicular to the pulsar's motion. We also show that the RS/PWN interaction scenario can reproduce the broadband spectrum of the PWN from radio to.-ray wavelengths. The analysis and modeling presented in this work have important implications for our general understanding of the structure and evolution of composite SNRs. C1 [Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Temim, Tea] Univ Maryland, CRESST, College Pk, MD 20742 USA. [Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolb, Christopher; Blondin, John] N Carolina State Univ, Raleigh, NC 27695 USA. [Hughes, John P.] Rutgers State Univ, New Brunswick, NJ 08901 USA. [Bucciantini, Niccolo] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Temim, T (reprint author), NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. OI Bucciantini, Niccolo'/0000-0002-8848-1392; Blondin, John/0000-0001-9691-6803; Temim, Tea/0000-0001-7380-3144 FU NASA [GO2-13075A, NAS8-03060] FX This work was supported by NASA under the grant number GO2-13075A. P.S. acknowledge support from the NASA Contract NAS8-03060. NR 27 TC 2 Z9 2 U1 2 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 JUL 20 PY 2015 VL 808 IS 1 AR 100 DI 10.1088/0004-637X/808/1/100 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO3MS UT WOS:000359062500100 ER PT J AU Cordero, MJ Hansen, CJ Johnson, CI Pilachowski, CA AF Cordero, M. J. Hansen, C. J. Johnson, C. I. Pilachowski, C. A. TI A COMPARATIVE STUDY OF TWO 47 Tuc GIANT STARS WITH DIFFERENT s-PROCESS ENRICHMENT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE globular clusters: individual (47 Tuc); stars: abundances; stars: chemically peculiar ID NEUTRON-CAPTURE ELEMENTS; GLOBULAR-CLUSTERS; ABUNDANCE VARIATIONS; STELLAR POPULATIONS; CHEMICAL ABUNDANCE; HEAVY-ELEMENTS; BRANCH STARS; BARIUM STARS; LARGE-SAMPLE; EVOLUTION AB Here we aim to understand the origin of 47 Tuc's La-rich star Lee 4710. We report abundances for O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, Zn, Y, Zr, Ba, La, Ce, Pr, Nd, and Eu and present a detailed abundance analysis of two 47 Tuc stars with similar stellar parameters but different slow neutron-capture (s-)process enrichment. Star Lee 4710 has the highest known La abundance ratio in this cluster ([La/Fe] = 1.14), and star Lee 4626 is known to have normal s-process abundances (e.g., [Ba/Eu] < 0). The nucleosynthetic pattern of elements with Z greater than or similar to 56 for star Lee 4710 agrees with the predicted yields of a 1.3 M-circle dot asymptotic giant branch (AGB) star. Therefore, Lee 4710 may have been enriched by mass transfer from a more massive AGB companion, which is compatible with its location far away from the center of this relatively metal-rich ([Fe/H] similar to -0.7) globular cluster. A further analysis comparing the abundance pattern of Lee 4710 with data available in the literature reveals that nine out of the similar to 200 47 Tuc stars previously studied show strong s-process enhancements that point toward later enrichment by more massive AGB stars. C1 [Cordero, M. J.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Cordero, M. J.; Hansen, C. J.] Heidelberg Univ, ZAH, D-69117 Heidelberg, Germany. [Hansen, C. J.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pilachowski, C. A.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Cordero, MJ (reprint author), Heidelberg Univ, Zentrum Astron, Astron Rech Inst, Monchhofstr 12-14, D-69120 Heidelberg, Germany. EM mjcorde@ari.uni-heidelberg.de; cjhansen@lsw.uni-heidelberg.de; cjohnson@cfa.harvard.edu; catyp@astro.indiana.edu OI Hansen, Camilla Juul/0000-0002-7277-7922; Pilachowski, Catherine/0000-0002-3007-206X FU German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; VILLUM FONDEN [VKR023371]; Clay Fellowship FX We thank the referee for useful comments. M.J.C. and C.J.H. were supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A4, A5, and A8) of the German Research Foundation (DFG) and C.J.H. also by a research grant (VKR023371) from VILLUM FONDEN. C.I.J. acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. C.J.H. thanks Thomas Masseron for a fruitful discussion. NR 33 TC 3 Z9 3 U1 1 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 JUL 20 PY 2015 VL 808 IS 1 AR L10 DI 10.1088/2041-8205/808/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900010 ER PT J AU Kunder, A Rich, RM Hawkins, K Poleski, R Storm, J Johnson, CI Shen, J Li, ZY Cordero, MJ Nataf, DM Bono, G Walker, AR Koch, A De Propris, R Udalski, A Szymanski, MK Soszynski, I Pietrzynski, G Ulaczyk, K Wyrzykowski, L Pietrukowicz, P Skowron, J Kozlowski, S Mroz, P AF Kunder, Andrea Rich, R. M. Hawkins, K. Poleski, R. Storm, J. Johnson, C. I. Shen, J. Li, Z. -Y. Cordero, M. J. Nataf, D. M. Bono, G. Walker, A. R. Koch, A. De Propris, R. Udalski, A. Szymanski, M. K. Soszynski, I. Pietrzynski, G. Ulaczyk, K. Wyrzykowski, L. Pietrukowicz, P. Skowron, J. Kozlowski, S. Mroz, P. TI A HIGH-VELOCITY BULGE RR LYRAE VARIABLE ON A HALO-LIKE ORBIT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: bulge; Galaxy: formation; Galaxy: halo; Galaxy: kinematics and dynamics; stars: Population II; stars: variables: RR Lyrae ID RED CLUMP STARS; GALACTIC BULGE; LIGHT CURVES; BAADE WINDOW; OGLE-III; GALAXY; METALLICITY; EXTINCTION; MAGNITUDE; DISTANCE AB We report on the RR Lyrae variable star, MACHO 176.18833.411, located toward the Galactic bulge and observed within the data from the ongoing Bulge RR Lyrae Radial Velocity Assay, which has the unusual radial velocity of -372 +/- 8 km s(-1) and true space velocity of -482 +/- 22 km s(-1) relative to the Galactic rest frame. Located less than 1 kpc from the Galactic center and toward a field at (l, b) = (3, -2.5), this pulsating star has properties suggesting it belongs to the bulge RR Lyrae star population, yet a velocity indicating it is abnormal, at least with respect to bulge giants and red clump stars. We show that this star is most likely a halo interloper and therefore suggest that halo contamination is not insignificant when studying metal-poor stars found within the bulge area, even for stars within 1 kpc of the Galactic center. We discuss the possibility that MACHO 176.18833.411 is on the extreme edge of the bulge RR Lyrae radial velocity distribution, and also consider a more exotic scenario in which it is a runaway star moving through the Galaxy. C1 [Kunder, Andrea; Storm, J.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Rich, R. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Hawkins, K.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Poleski, R.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Poleski, R.; Udalski, A.; Szymanski, M. K.; Soszynski, I.; Pietrzynski, G.; Ulaczyk, K.; Wyrzykowski, L.; Pietrukowicz, P.; Skowron, J.; Kozlowski, S.; Mroz, P.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Johnson, C. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shen, J.; Li, Z. -Y.] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Cordero, M. J.] Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Nataf, D. M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Bono, G.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Bono, G.] Rome Astron Observ, INAF, I-00040 Monte Porzio Catone, Italy. [Walker, A. R.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. [Koch, A.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. [De Propris, R.] Univ Turku, Finnish Ctr Astron ESO FINCA, Turku, Finland. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Ulaczyk, K.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Kunder, A (reprint author), Leibniz Inst Astrophys Potsdam AIP, An der Sternwarte 16, D-14482 Potsdam, Germany. RI Skowron, Jan/M-5186-2014; Kozlowski, Szymon/G-4799-2013; OI Skowron, Jan/0000-0002-2335-1730; Kozlowski, Szymon/0000-0003-4084-880X; Storm, Jesper/0000-0002-8627-6096; Hawkins, Keith /0000-0002-1423-2174; Kunder, Andrea/0000-0002-2808-1370; Koch, Andreas/0000-0002-9859-4956 FU National Science Foundation [NSF PHY11-25915, AST-1413755]; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; Polish Ministry of Science and Higher Education through the program "Ideas Plus" [IdP2012 000162]; Clay Fellowship; 973 Program of China [2014CB845700]; National Natural Science Foundation of China [11333003, 11322326, 11403072]; Strategic Priority Research Program "The Emergence of Cosmological Structures" of the Chinese Academy of Sciences [XDB09000000]; Shanghai Sailing Program [14YF1407700] FX We thank the Australian Astronomical Observatory, which has made these observations possible. This research was supported in part by the National Science Foundation under grant No. NSF PHY11-25915. This work was supported by Sonderforschungsbereich SFB 881 "The Milky Way System" (subprojects A4, A5, A8) of the German Research Foundation (DFG). This work has been partially supported by the Polish Ministry of Science and Higher Education through the program "Ideas Plus" award No. IdP2012 000162 to I.S. R.M.R. acknowledges support from grant AST-1413755 from the National Science Foundation. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory.; J.S. acknowledges support from the 973 Program of China under grant No. 2014CB845700, the National Natural Science Foundation of China under grant Nos. 11333003 and 11322326, and the Strategic Priority Research Program "The Emergence of Cosmological Structures" (No. XDB09000000) of the Chinese Academy of Sciences. Z.Y.L. acknowledges support from the National Natural Science Foundation of China under grant No. 11403072 and Shanghai Sailing Program (No. 14YF1407700). This work made use of the facilities of the Center for High performance Computing at Shanghai Astronomical Observatory. Hospitality at APCTP during the 7th Korean Astrophysics Workshop is kindly acknowledged. NR 41 TC 10 Z9 10 U1 2 U2 4 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 JUL 20 PY 2015 VL 808 IS 1 AR L12 DI 10.1088/2041-8205/808/1/L12 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900012 ER PT J AU Mroczkowski, T Kovacs, A Bulbul, E Staguhn, J Benford, DJ Clarke, TE van Weeren, RJ Intema, HT Randall, S AF Mroczkowski, T. Kovacs, A. Bulbul, E. Staguhn, J. Benford, D. J. Clarke, T. E. van Weeren, R. J. Intema, H. T. Randall, S. TI RESOLVING THE MERGING PLANCK CLUSTER PLCK G147.3-16.6 WITH GISMO SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: individual (PLCK G147.3-16.6); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID SPT-SZ SURVEY; GALAXY CLUSTERS; RADIO HALO; ZELDOVICH; GHZ; TELESCOPE; EMISSION AB The Planck satellite has recently completed an all-sky galaxy cluster survey exploiting the thermal Sunyaev-Zel'dovich (SZ) effect to locate some of the most massive systems observable. With a median redshift of < z > = 0.22, the clusters found by Planck at z > 0.3 are proving to be exceptionally massive and/or disturbed systems. One notable Planck discovery at z = 0.645, PLCK G147.3-16.6, has an elongated core and hosts a radio halo, indicating it is likely in the process of merging. We present a 16 ''.5 resolution SZ observation of this high-z merger using the Goddard-IRAM Superconducting 2-Millimeter Observer, and compare it to X-ray follow-up observations with XMM-Newton. We find the SZ pressure substructure is offset from the core components seen in X-ray. We interpret this as possible line of sight temperature or density substructure due to the on-going merger. C1 [Mroczkowski, T.; Clarke, T. E.] US Navy, Res Lab, Washington, DC 20375 USA. [Kovacs, A.] CALTECH, Pasadena, CA 91125 USA. [Kovacs, A.] Univ Minnesota, Inst Astrophys, Minneapolis, MN 55455 USA. [Bulbul, E.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Staguhn, J.; Benford, D. J.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Code 665, Greenbelt, MD 20771 USA. [Staguhn, J.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Mroczkowski, T.] Natl Acad Sci, Natl Res Council, London, England. RP Mroczkowski, T (reprint author), US Navy, Res Lab, 4555 Overlook Ave SW, Washington, DC 20375 USA. EM anthony.mroczkowski.ctr@nrl.navy.mil RI Kovacs, Attila/C-1171-2010; Intema, Huib/D-1438-2012; Benford, Dominic/D-4760-2012; OI Kovacs, Attila/0000-0001-8991-9088; Intema, Huib/0000-0002-5880-2730; Benford, Dominic/0000-0002-9884-4206; Mroczkowski, Tony/0000-0003-3816-5372; van Weeren, Reinout/0000-0002-0587-1660 FU 6.1 Base funding; NASA ADP grant [NNX13AE83G]; NASA through the Einstein Postdoctoral grant by the Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; National Radio Astronomy Observatory, a facility of the National Science Foundation (NSF); NSF [1020981, 1106284]; INSU/CNRS (France); MPG (Germany); IGN (Spain) FX This research was performed while TM held a National Research Council Research Associateship Award at the Naval Research Laboratory (NRL). Basic research in radio astronomy at NRL by TM and TEC is supported by 6.1 Base funding. EB is supported in part by NASA ADP grant NNX13AE83G. RJvW is supported by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. HTI is supported by the National Radio Astronomy Observatory, a facility of the National Science Foundation (NSF) operated under cooperative agreement by Associated Universities, Inc. The GISMO instrument and team are supported through NSF ATI grants 1020981 and 1106284. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). NR 31 TC 1 Z9 1 U1 0 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 JUL 20 PY 2015 VL 808 IS 1 AR L6 DI 10.1088/2041-8205/808/1/L6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900006 ER PT J AU Sandoval, MA Vo, RP Romanowsky, AJ Strader, J Choi, J Jennings, ZG Conroy, C Brodie, JP Foster, C Villaume, A Norris, MA Janz, J Forbes, DA AF Sandoval, Michael A. Vo, Richard P. Romanowsky, Aaron J. Strader, Jay Choi, Jieun Jennings, Zachary G. Conroy, Charlie Brodie, Jean P. Foster, Caroline Villaume, Alexa Norris, Mark A. Janz, Joachim Forbes, Duncan A. TI HIDING IN PLAIN SIGHT: RECORD-BREAKING COMPACT STELLAR SYSTEMS IN THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: fundamental parameters; galaxies: nuclei; galaxies: star clusters: general ID EARLY-TYPE GALAXIES; VIRGO CLUSTER SURVEY; SUSTAINED INATTENTIONAL BLINDNESS; ULTRACOMPACT DWARF GALAXIES; DATA REDUCTION PROCEDURES; MASSIVE STAR-CLUSTERS; GLOBULAR-CLUSTERS; ABUNDANCE RATIOS; AIMSS PROJECT; DATA RELEASE AB Motivated by the recent, serendipitous discovery of the densest known galaxy, M60-UCD1, we present two initial findings from a follow-up search, using the Sloan Digital Sky Survey, Subaru/Suprime-Cam, and Hubble Space Telescope imaging, and SOuthern Astrophysical Research (SOAR)/Goodman spectroscopy. The first object discovered, M59-UCD3, has a similar size to M60-UCD1 (half-light radius of r(h) similar to 20 pc) but is 40% more luminous (M-V similar to 14.6), making it the new densest-known galaxy. The second, M85-HCC1, has a size like a typical globular cluster (GC; r(h) similar to 1.8pc) but is much more luminous (M-V similar to -12.5). This hypercompact cluster is by far the densest confirmed free-floating stellar system, and is equivalent to the densest known nuclear star clusters. From spectroscopy, we find that both objects are relatively young (similar to 9 and similar to 3 Gyr, respectively), with metal-abundances that resemble those of galaxy centers. Their host galaxies show clear signs of large-scale disturbances, and we conclude that these dense objects are the remnant nuclei of recently accreted galaxies. M59-UCD3 is an ideal target for follow-up with high-resolution imaging and spectroscopy to search for an overweight central supermassive black hole as was discovered in M60-UCD1. These findings also emphasize the potential value of ultra-compact dwarfs and massive GCs as tracers of the assembly histories of galaxies. C1 [Sandoval, Michael A.; Vo, Richard P.; Romanowsky, Aaron J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Vo, Richard P.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94131 USA. [Romanowsky, Aaron J.; Brodie, Jean P.] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Choi, Jieun; Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Choi, Jieun; Jennings, Zachary G.; Villaume, Alexa] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Foster, Caroline] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Norris, Mark A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Janz, Joachim; Forbes, Duncan A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RP Sandoval, MA (reprint author), San Jose State Univ, Dept Phys & Astron, One Washington Sq, San Jose, CA 95192 USA. OI Sandoval, Michael/0000-0002-5088-4487; Villaume, Alexa/0000-0003-1887-0621; Foster, Caroline/0000-0003-0247-1204 FU National Science Foundation (NSF) [AST-1109878]; SJSU Undergraduate Research Grants; ARC [DP130100388]; Alfred P. Sloan Foundation; NSF; U. S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbu-kagakusho; Max Planck Society; Higher Education Funding Council for England; Participating Institutions FX We thank the SJSU ASTR-117B class for their endurance through UCD fever, Katy Murphy for helpful discussions, Cindy Tsui for artistic assistance, and the referee for a quick and helpful report. We are immensely grateful for the efforts of SDSS, SDSS-III, and the Hubble Legacy Archive in making their data easily accessible to anyone in the world with an internet connection. This work was supported by National Science Foundation (NSF) grant AST-1109878, by SJSU Undergraduate Research Grants, and by the ARC (DP130100388). It used data from the Subaru telescope (National Astronomical Observatory of Japan) and the Southern Astrophysical Research (SOAR) telescope (joint project of Brasil, NOAO, UNC, MSU). SDSS/SDSS-III was funded by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF, the U. S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbu-kagakusho, the Max Planck Society, and the Higher Education Funding Council for England. NR 49 TC 4 Z9 4 U1 1 U2 3 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 JUL 20 PY 2015 VL 808 IS 1 AR L32 DI 10.1088/2041-8205/808/1/L32 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CN9OO UT WOS:000358778900032 ER PT J AU Bohu, T Santelli, CM Akob, DM Neu, TR Ciobota, V Rosch, P Popp, J Nietzsche, S Kusel, K AF Bohu, Tsing Santelli, Cara M. Akob, Denise M. Neu, Thomas R. Ciobota, Valerian Roesch, Petra Popp, Juergen Nietzsche, Sandor Kuesel, Kirsten TI Characterization of pH dependent Mn(II) oxidation strategies and formation of a bixbyite-like phase by Mesorhizobium australicum T-G1 SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE catalase; low pH; Mn(II) oxidation; multi-copper oxidase; reactive oxygen species ID SP STRAIN SG-1; COAL-MINE DRAINAGE; ENZYMATIC MANGANESE(II) OXIDATION; PUTATIVE MULTICOPPER OXIDASE; MARINE BACILLUS; MN(II)-OXIDIZING BACTERIA; LEPTOTHRIX-DISCOPHORA; MICROBIAL COMMUNITIES; TREATMENT SYSTEMS; ESCHERICHIA-COLI AB Despite the ubiquity of Mn oxides in natural environments, there are only a few observations of biological Mn(II) oxidation at pH <6. The lack of low pH Mn-oxidizing bacteria (MOB) isolates limits our understanding of how pH influences biological Mn(II) oxidation in extreme environments. Here, we report that a novel MOB isolate, Mesorhizobium australicum strain T-G1, isolated from an acidic and metalliferous uranium mining area, can oxidize Mn(II) at both acidic and neutral pH using different enzymatic pathways. X-ray diffraction, Raman spectroscopy, and scanning electron microscopy with energy dispersive X-ray spectroscopy revealed that T-G1 initiated bixbyite-like Mn oxide formation at pH 5.5 which coincided with multi-copper oxidase expression from early exponential phase to late stationary phase. In contrast, reactive oxygen species (ROS), particularly superoxide, appeared to be more important for T-G1 mediated Mn(II) oxidation at neutral pH. ROS was produced in parallel with the occurrence of Mn(II) oxidation at pH 7.2 from early stationary phase. Solid phase Mn oxides did not precipitate, which is consistent with the presence of a high amount of H2O2 and lower activity of catalase in the liquid culture at pH 7.2. Our results show that M. australicum T-G1, an acid tolerant MOB, can initiate Mn(II) oxidation by varying its oxidation mechanisms depending on the pH and may play an important role in low pH manganese biogeochemical cycling. C1 [Bohu, Tsing; Kuesel, Kirsten] Univ Jena, Dept Aquat Geomicrobiol, D-07743 Jena, Germany. [Santelli, Cara M.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Akob, Denise M.] US Geol Survey, Natl Res Program, Reston, VA 22092 USA. [Neu, Thomas R.] UFZ Helmholtz Ctr Environm Res, Dept River Ecol, Magdeburg, Germany. [Ciobota, Valerian; Roesch, Petra; Popp, Juergen] Univ Jena, Inst Phys Chem, D-07743 Jena, Germany. [Ciobota, Valerian; Roesch, Petra; Popp, Juergen] Univ Jena, Abbe Sch Phonton, D-07743 Jena, Germany. [Popp, Juergen] Leibniz Inst Phonton Technol, Jena, Germany. [Nietzsche, Sandor] Univ Jena, Univ Hosp Jena, Ctr Electron Microscopy, D-07743 Jena, Germany. [Kuesel, Kirsten] German Ctr Integrat Biodivers Res iDiv, Leipzig, Germany. RP Kusel, K (reprint author), Univ Jena, Dept Aquat Geomicrobiol, Dornburger Str 159, D-07743 Jena, Germany. EM kirsten.kuesel@uni-jena.de RI iDiv, Deutsches Zentrum/B-5164-2016; OI Akob, Denise/0000-0003-1534-3025; Santelli, Cara/0000-0001-8617-0008 FU German Science Foundation (DFG) [GRK 1257] FX The authors thank Dr. Juanjuan Wang and Dr. Shipeng Lu (Aquatic Geomicrobiology, FSU Jena) for help with sampling. The Laboratories of Analytical Biology of the Smithsonian Institution, USA provided free access to and assistance with Synergy HT Multi-Mode Microplate Reader. We also thank the German Science Foundation (DFG GRK 1257) for funding. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. The authors declare no competing financial interest. NR 89 TC 4 Z9 4 U1 5 U2 28 PU FRONTIERS MEDIA SA PI LAUSANNE PA PO BOX 110, EPFL INNOVATION PARK, BUILDING I, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD JUL 17 PY 2015 VL 6 AR 734 DI 10.3389/fmicb.2015.00734 PG 15 WC Microbiology SC Microbiology GA CN7ZJ UT WOS:000358654900001 PM 26236307 ER PT J AU Nguyen, TL McCarthy, MC Stanton, JF AF Thanh Lam Nguyen McCarthy, Michael C. Stanton, John F. TI Relatively Selective Production of the Simplest Criegee Intermediate in a CH4/O-2 Electric Discharge: Kinetic Analysis of a Plausible Mechanism SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID ACTIVE THERMOCHEMICAL TABLES; ATOMIC NATURAL ORBITALS; TRANSITION-STATE THEORY; REACTION-RATE CONSTANTS; GAUSSIAN-BASIS SETS; GAS-PHASE; AB-INITIO; GENERAL CONTRACTION; O-2; CH2OO AB High -accuracy coupled cluster methods in combination with microcanonical semiclassical transition state theory are used to investigate a plausible formation mechanism of the simplest Criegee intermediate in a CH4/O-2 discharge experiment. Our results suggest that the Criegee intermediate is produced in a three-step process: (i) production of methyl radical by cleavage of a C-H bond of CH4; (ii) association of methyl radical with molecular oxygen to form a vibrationally excited methyl peroxy, which is in a rapid microequilibrium with the reactants; and finally, (iii) H-abstraction of CH3OO by O-2, which results in the formation of cool CH2OO, which has insufficient internal energy to rearrange to dioxirane. C1 [Thanh Lam Nguyen; Stanton, John F.] Univ Texas Austin, Dept Chem, Austin, TX 78712 USA. [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stanton, JF (reprint author), Univ Texas Austin, Dept Chem, Mail Stop A5300, Austin, TX 78712 USA. EM jfstanton@mail.utexas.edu FU Robert A. Welch Foundation [F-1283]; U.S. Department of Energy, Office of Basic Energy Sciences [DE-FG02-07ER15884]; NSF [CHE-1058063] FX J.F.S. and T.L.N. are supported by the Robert A. Welch Foundation (Grant F-1283). This material is based on the work supported by the U.S. Department of Energy, Office of Basic Energy Sciences under Award Number DE-FG02-07ER15884. M.C.M. is supported by NSF Grant No. CHE-1058063. NR 51 TC 3 Z9 3 U1 9 U2 23 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD JUL 16 PY 2015 VL 119 IS 28 BP 7197 EP 7204 DI 10.1021/jp510554g PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CN3PA UT WOS:000358337600014 PM 25405528 ER PT J AU Liu, H Xu, QY He, PC Santiago, LS Yang, KM Ye, Q AF Liu, Hui Xu, Qiuyuan He, Pengcheng Santiago, Louis S. Yang, Keming Ye, Qing TI Strong phylogenetic signals and phylogenetic niche conservatism in ecophysiological traits across divergent lineages of Magnoliaceae SO SCIENTIFIC REPORTS LA English DT Article ID HYDRAULIC ARCHITECTURE; WATER RELATIONS; FUNCTIONAL CONVERGENCE; CORRELATED EVOLUTION; CANOPY TREES; LEAF; ECOLOGY; PLANT; EFFICIENCY; BIOLOGY AB The early diverged Magnoliaceae shows a historical temperate-tropical distribution among lineages indicating divergent evolution, yet which ecophysiological traits are phylogenetically conserved, and whether these traits are involved in correlated evolution remain unclear. Integrating phylogeny and 20 ecophysiological traits of 27 species, from the four largest sections of Magnoliaceae, we tested the phylogenetic signals of these traits and the correlated evolution between trait pairs. Phylogenetic niche conservatism (PNC) in water-conducting and nutrient-use related traits was identified, and correlated evolution of several key functional traits was demonstrated. Among the three evergreen sections of tropical origin, Gwillimia had the lowest hydraulic-photosynthetic capacity and the highest drought tolerance compared with Manglietia and Michelia. Contrastingly, the temperate centred deciduous section, Yulania, showed high rates of hydraulic conductivity and photosynthesis at the cost of drought tolerance. This study elucidated the regulation of hydraulic and photosynthetic processes in the temperate-tropical adaptations for Magnoliaceae species, which led to strong phylogenetic signals and PNC in ecophysiological traits across divergent lineages of Magnoliaceae. C1 [Liu, Hui; Xu, Qiuyuan; He, Pengcheng; Ye, Qing] Chinese Acad Sci, South China Bot Garden, Key Lab Vegetat Restorat & Management Degraded Ec, Guangzhou 510650, Guangdong, Peoples R China. [Xu, Qiuyuan; He, Pengcheng] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Santiago, Louis S.] Univ Calif Riverside, Bot & Plant Sci, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Yang, Keming] Chinese Acad Sci, Hort Ctr, South China Bot Garden, Guangzhou 510520, Guangdong, Peoples R China. RP Xu, QY (reprint author), Chinese Acad Sci, South China Bot Garden, Key Lab Vegetat Restorat & Management Degraded Ec, Xingke Rd 723, Guangzhou 510650, Guangdong, Peoples R China. EM qye@scbg.ac.cn RI Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 FU National Natural Science Foundation of China [31300334]; Natural Science Foundation of Guangdong Province [S2013040015044]; Chinese Academy of Sciences through its Hundred Talent Program and Knowledge Innovation Project [KSCX2-EW-J-28]; Scientific Research Foundation for the Returned Overseas Chinese Scholars, State Education Ministry of China FX We thank Ronghua Li and Shidan Zhu for their assistance in lab work and discussion. This work was funded by the National Natural Science Foundation of China (31300334), the Natural Science Foundation of Guangdong Province (S2013040015044) and the Chinese Academy of Sciences through its Hundred Talent Program and Knowledge Innovation Project (KSCX2-EW-J-28), and the Scientific Research Foundation for the Returned Overseas Chinese Scholars, State Education Ministry of China. NR 62 TC 5 Z9 5 U1 5 U2 46 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 JUL 16 PY 2015 VL 5 AR 12246 DI 10.1038/srep12246 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CM9GH UT WOS:000358014900001 PM 26179320 ER PT J AU Cramer, KL Leonard-Pingel, JS Rodriguez, F Jackson, JBC AF Cramer, Katie L. Leonard-Pingel, Jill S. Rodriguez, Felix Jackson, Jeremy B. C. TI Molluscan subfossil assemblages reveal the long-term deterioration of coral reef environments in Caribbean Panama SO MARINE POLLUTION BULLETIN LA English DT Article DE Barbatia cancellaria; Bocas del Toro; Dendostrea frons; Historical ecology; Water quality ID BOCAS-DEL-TORO; CENTRAL-AMERICA; THALASSIA COMMUNITIES; SPECIES RICHNESS; HUMAN IMPACTS; WEST-INDIES; ECOLOGY; GASTROPODS; CONVERGENCE; RADIOCARBON AB Caribbean reef corals have declined sharply since the 1980s, but the lack of prior baseline data has hindered identification of drivers of change. To assess anthropogenic change in reef environments over the past century, we tracked the composition of subfossil assemblages of bivalve and gastropod mollusks excavated from pits below lagoonal and offshore reefs in Bocas del Toro, Panama. The higher prevalence of (a) infaunal suspension-feeding bivalves and herbivorous and omnivorous gastropods in lagoons and (b) epifaunal and suspension-feeding bivalves and carnivorous and suspension-feeding gastropods offshore reflected the greater influence of land-based nutrients/sediments within lagoons. Temporal changes indicated deteriorating environmental conditions pre-1960 in lagoons and post-1960 offshore, with offshore communities becoming more similar to lagoonal ones since 1960. Relative abundances of dominant bivalve species tracked those of their coral hosts, revealing broader ecosystem effects of coral community change. The nature and timing of changes implicate land-based runoff in reef deterioration. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Cramer, Katie L.; Rodriguez, Felix; Jackson, Jeremy B. C.] Smithsonian Trop Res Inst, Balboa, Panama. [Cramer, Katie L.; Jackson, Jeremy B. C.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Leonard-Pingel, Jill S.] Washington & Lee Univ, Lexington, VA 24450 USA. [Jackson, Jeremy B. C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Cramer, KL (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM kcramer@ucsd.edu; j.leonardpingel@gmail.com; rodriguezf@si.edu; jeremybcjackson@gmail.com FU Smithsonian Institution; NSF Integrative Graduate Education and Research Traineeship; Center for Marine Biodiversity and Conservation at Scripps Institution of Oceanography; University of California Academic Senate; PADI Foundation's Project AWARE FX We thank C. Angioletti, E. Ochoa, G. Jacome, P. Gondola, J. Morales, and C. Degracia for help in the laboratory and field in Panama, T. Guilderson for conducting radiocarbon analyses and assisting with calibrations to calendar ages, H. Guzman for his help with interpretation of study results, and Minerals Resources Department and National Authority for the Environment of Panama and C. De Leon for providing collection permits. Study supported by Smithsonian Institution, NSF Integrative Graduate Education and Research Traineeship, Center for Marine Biodiversity and Conservation at Scripps Institution of Oceanography, University of California Academic Senate, and PADI Foundation's Project AWARE. NR 68 TC 3 Z9 3 U1 2 U2 12 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 JUL 15 PY 2015 VL 96 IS 1-2 BP 176 EP 187 DI 10.1016/j.marpolbul.2015.05.031 PG 12 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA CM0DP UT WOS:000357348900031 PM 26031382 ER PT J AU Najita, JR Andrews, SM Muzerolle, J AF Najita, Joan R. Andrews, Sean M. Muzerolle, James TI Demographics of transition discs in Ophiuchus and Taurus SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: formation; protoplanetary discs; circumstellar matter; stars: formation; stars: pre-main-sequence ID YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; SUBMILLIMETER CONTINUUM FLUX; CIRCUMSTELLAR DUST DISKS; MASS ACCRETION RATES; RHO-OPHIUCHI; MOLECULAR CLOUD; PROTOPLANETARY DISKS; X-RAY AB Transition disc systems are young stars that appear to be on the verge of dispersing their protoplanetary discs. We explore the nature of these systems by comparing the stellar accretion rates (M) over dot(*) and disc masses M-d of transition discs and normal T Tauri stars in Taurus and Ophiuchus. After controlling for the known dependences of (M) over dot(*) and M-d on age, (M) over dot(*) on stellar mass and M-d on the presence of stellar or substellar companions, we find that the normal T Tauri stars show a trend of (M) over dot(*) increasing with M-d. The transition discs tend to have higher average disc masses than normal T Tauri stars as well as lower accretion rates than normal T Tauri stars of the same disc mass. These results are most consistent with the interpretation that the transition discs have formed objects massive enough to alter the accretion flow, i.e. single or multiple giant planets. Several Ophiuchus T Tauri stars that are not known transition disc systems also have very low accretion rates for their disc masses. We speculate on the possible nature of these sources. C1 [Najita, Joan R.] Natl Opt Astron Observ, 950 Cherry Ave, Tucson, AZ 85719 USA. [Najita, Joan R.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muzerolle, James] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Najita, JR (reprint author), Natl Opt Astron Observ, 950 Cherry Ave, Tucson, AZ 85719 USA. EM najita@noao.edu; sandrews@cfa.harvard.edu; muzerol@stsci.edu NR 108 TC 14 Z9 14 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 JUL 11 PY 2015 VL 450 IS 4 BP 3559 EP 3567 DI 10.1093/mnras/stv839 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000014 ER PT J AU Glennie, A Jonker, PG Fender, RP Nagayama, T Pretorius, ML AF Glennie, A. Jonker, P. G. Fender, R. P. Nagayama, T. Pretorius, M. L. TI Two fast X-ray transients in archival Chandra data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: flare; stars: late-type; infrared: stars; X-rays: bursts ID POINT-SOURCE CATALOG; MASSIVE BLACK-HOLES; ALL-SKY SURVEY; TIDAL DISRUPTION; WHITE-DWARFS; GALAXY; FLARE; EMISSION; ROTATION; SAMPLE AB We present the discovery of two new X-ray transients in archival Chandra data. The first transient, XRT 110103, occurred in 2011 January and shows a sharp rise of at least three orders of magnitude in count rate in less than 10 s, a flat peak for about 20 s and decays by two orders of magnitude in the next 60 s. We find no optical or infrared counterpart to this event in pre-existing survey data or in an observation taken by the Simultaneous-3color InfraRed Imager for Unbiased Survey (SIRIUS) instrument at the Infrared Survey Facility similar to 2.1 yr after the transient, providing limiting magnitudes of J > 18.1, H > 17.6 and K-s > 16.3. This event shows similarities to the transient previously reported in Jonker et al. which was interpreted as the possible tidal disruption of a white dwarf by an intermediate-mass black hole. We discuss the possibility that these transients originate from the same type of event. If we assume these events are related a rough estimate of the rates gives 1.4 x 10(5) per year over the whole sky with a peak 0.3-7 keV X-ray flux greater than 2 x 10(-10) erg cm(-2) s(-1). The second transient, XRT 120830, occurred in 2012 August and shows a rise of at least three orders of magnitude in count rate and a subsequent decay of around one order of magnitude all within 10 s, followed by a slower quasi-exponential decay over the remaining 30 ks of the observation. We detect a likely infrared counterpart with magnitudes J = 16.70 +/- 0.06, H = 15.92 +/- 0.04 and K-s = 15.37 +/- 0.06 which shows an average proper motion of 74 +/- 19 mas yr(-1) compared to archival 2MASS observations. The JHK(s) magnitudes, proper motion and X-ray flux of XRT 120830 are consistent with a bright flare from a nearby late M or early L dwarf. C1 [Glennie, A.; Fender, R. P.; Pretorius, M. L.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nagayama, T.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Nagayama, T.] Kagoshima Univ, Dept Sci & Engn, Korimoto, Kagoshima, Japan. RP Glennie, A (reprint author), Univ Oxford, Dept Phys, Oxford OX1 3RH, England. EM aidan.glennie@astro.ox.ac.uk FU European Research Council [267697]; National Aeronautics and Space Administration; National Science Foundation FX This project was funded in part by European Research Council Advanced Grant 267697 '4 pi sky: Extreme Astrophysics with Revolutionary Radio Telescopes.'; 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 the National Aeronautics and Space Administration and the National Science Foundation. NR 33 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 JUL 11 PY 2015 VL 450 IS 4 BP 3765 EP 3770 DI 10.1093/mnras/stv801 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000028 ER PT J AU D'Ammando, F Orienti, M Tavecchio, F Ghisellini, G Torresi, E Giroletti, M Raiteri, CM Grandi, P Aller, M Aller, H Gurwell, MA Malaguti, G Pian, E Tosti, G AF D'Ammando, F. Orienti, M. Tavecchio, F. Ghisellini, G. Torresi, E. Giroletti, M. Raiteri, C. M. Grandi, P. Aller, M. Aller, H. Gurwell, M. A. Malaguti, G. Pian, E. Tosti, G. TI Unveiling the nature of the gamma-ray emitting active galactic nucleus PKS 0521-36 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: PKS0521-36; galaxies: nuclei; quasars: general; gamma-rays: galaxies; gamma-rays: general ID LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; SOURCE CATALOG; COMPLETE SAMPLE; RADIO GALAXIES; EGRET CATALOG; LAC OBJECTS; SKY SURVEY; FERMI-LAT; NGC 1275 AB PKS 0521-36 is an active galactic nucleus (AGN) with uncertain classification. We investigate the properties of this source from radio to gamma-rays. The broad emission lines in the optical and ultraviolet bands and steep radio spectrum indicate a possible classification as an intermediate object between broad-line radio galaxies (BLRG) and steep spectrum radio quasars (SSRQ). On pc-scales PKS 0521-36 shows a knotty structure similar to misaligned AGN. The core dominance and the gamma-ray properties are similar to those estimated for other SSRQ and BLRG detected in gamma-rays, suggesting an intermediate viewing angle with respect to the observer. In this context the flaring activity detected from this source by Fermi-Large Area Telescope between 2010 June and 2012 February is very intriguing. We discuss the gamma-ray emission of this source in the framework of the structured jet scenario, comparing the spectral energy distribution (SED) of the flaring state in 2010 June with that of a low state. We present three alternative models corresponding to three different choices of the viewing angles theta(v) = 6 degrees, 15 degrees, and 20 degrees. We obtain a good fit for the first two cases, but the SED obtained with theta(v) = 15 degrees if observed at a small angle does not resemble that of a typical blazar since the synchrotron emission should dominate by a large factor (similar to 100) the inverse Compton component. This suggests that a viewing angle between 6 degrees and 15 degrees is preferred, with the rapid variability observed during gamma-ray flares favouring a smaller angle. However, we cannot rule out that PKS 0521-36 is the misaligned counterpart of a synchrotron-dominated blazar. C1 [D'Ammando, F.] Univ Bologna, Dipartimento Fis Astron, I-40127 Bologna, Italy. [D'Ammando, F.; Orienti, M.; Giroletti, M.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Tavecchio, F.; Ghisellini, G.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. [Torresi, E.; Grandi, P.; Malaguti, G.] INAF, Ist Astrofis Spaziale Fis Cosm, I-40129 Bologna, Italy. [Raiteri, C. M.] INAF, Osservatorio Astron Torino, I-10025 Pino Torinese, TO, Italy. [Aller, M.; Aller, H.] Univ Michigan, Ann Arbor, MI 48109 USA. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pian, E.] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Tosti, G.] INFN Sezione Perugia, I-06123 Perugia, Italy. RP D'Ammando, F (reprint author), Univ Bologna, Dipartimento Fis Astron, Via Ranzani 1, I-40127 Bologna, Italy. EM dammando@ira.inaf.it OI Grandi, Paola/0000-0003-1848-6013; Malaguti, Giuseppe/0000-0001-9872-3378; Ghisellini, Gabriele/0000-0002-0037-1974 FU Smithsonian Institution; Academia Sinica; University of Michigan; National Science Foundation [AST-0607523]; NASA [NNX09AU16G, NNX10AP16G, NNX11AO13G, NNX13AP18G] FX We thank the Swift team for making these observations possible, the duty scientists, and science planners. 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. This research has made use of data from the University of Michigan Radio Astronomy Observatory which has been supported by the University of Michigan and by a series of grants from the National Science Foundation, most recently AST-0607523. This research was supported in part by NASA Fermi Guest Investigator awards NNX09AU16G, NNX10AP16G, NNX11AO13G, and NNX13AP18G. Part of this work is based on archival data, software, or online service provided by ASI Science Data Center (ASDC). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank S. Digel, D. J. Thompson, J. Perkins, D. Gasparrini, and the anonymous referee for useful comments and suggestions. NR 82 TC 2 Z9 2 U1 0 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 JUL 11 PY 2015 VL 450 IS 4 BP 3975 EP 3990 DI 10.1093/mnras/stv909 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000046 ER PT J AU Zhuravleva, I Churazov, E Arevalo, P Schekochihin, AA Allen, SW Fabian, AC Forman, WR Sanders, JS Simionescu, A Sunyaev, R Vikhlinin, A Werner, N AF Zhuravleva, I. Churazov, E. Arevalo, P. Schekochihin, A. A. Allen, S. W. Fabian, A. C. Forman, W. R. Sanders, J. S. Simionescu, A. Sunyaev, R. Vikhlinin, A. Werner, N. TI Gas density fluctuations in the Perseus Cluster: clumping factor and velocity power spectrum SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE turbulence; methods: observational; methods: statistical; techniques: image processing; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; RELAXED GALAXY CLUSTERS; XMM-NEWTON OBSERVATIONS; JET-INFLATED BUBBLES; X-RAY SPECTROSCOPY; INTRACLUSTER MEDIUM; ELLIPTIC GALAXIES; COSMOLOGICAL SIMULATIONS; COOLING FLOWS; NGC 1275 AB X-ray surface brightness fluctuations in the core of the Perseus Cluster are analysed, using deep observations with the Chandra observatory. The amplitude of gas density fluctuations on different scales is measured in a set of radial annuli. It varies from 7 to 12 per cent on scales of similar to 10-30 kpc within radii of 30-220 kpc from the cluster centre. Using a statistical linear relation between the observed amplitude of density fluctuations and predicted velocity, the characteristic velocity of gas motions on each scale is calculated. The typical amplitudes of the velocity outside the central 30 kpc region are 90-140 km s(-1) on similar to 20-30 kpc scales and 70-100 km s(-1) on smaller scales similar to 7-10 kpc. The velocity power spectrum ( PS) is consistent with cascade of turbulence and its slope is in a broad agreement with the slope for canonical Kolmogorov turbulence. The gas clumping factor estimated from the PS of the density fluctuations is lower than 7-8 per cent for radii similar to 30-220 kpc from the centre, leading to a density bias of less than 3-4 per cent in the cluster core. Uncertainties of the analysis are examined and discussed. Future measurements of the gas velocities with the Astro-H, Athena and Smart-X observatories will directly measure the gas density-velocity perturbation relation and further reduce systematic uncertainties in this analysis. C1 [Zhuravleva, I.; Allen, S. W.; Werner, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Zhuravleva, I.; Allen, S. W.; Werner, N.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.] Space Res Inst IKI, Moscow 117997, Russia. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Schekochihin, A. A.] Univ Oxford, Rudolf Peierls Ctr Theoret Phys, Oxford OX1 3NP, England. [Schekochihin, A. A.] Univ Oxford Merton Coll, Oxford OX1 4JD, England. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Forman, W. R.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Simionescu, A.] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa 2525210, Japan. RP Zhuravleva, I (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 452 Lomita Mall, Stanford, CA 94305 USA. EM zhur@stanford.edu; churazov@mpa-arching.mpg.de; arevalo.patricia@gmail.com RI Churazov, Eugene/A-7783-2013; OI Sanders, Jeremy/0000-0003-2189-4501; Forman, William/0000-0002-9478-1682 FU NASA, Chandra X-ray Observatory Center [AR4-15013X]; NASA [NAS8-03060]; US Department of Energy [DE-AC02-76SF00515]; Suzaku grants [NNX12AE05G, NNX13AI49G]; FONDECYT [1140304]; Russian Scientific Foundation [14-22-00271] FX Support for this work was provided by the NASA through Chandra award number AR4-15013X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the NASA under contract NAS8-03060. SWA acknowledges support from the US Department of Energy under contract number DE-AC02-76SF00515. IZ and NW are partially supported from Suzaku grants NNX12AE05G and NNX13AI49G. PA acknowledges financial support from FONDECYT grant 1140304. EC and RS are partly supported by grant No. 14-22-00271 from the Russian Scientific Foundation. NR 79 TC 17 Z9 17 U1 1 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 JUL 11 PY 2015 VL 450 IS 4 BP 4184 EP 4197 DI 10.1093/mnras/stv900 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000062 ER PT J AU Torres, MAP Jonker, PG Miller-Jones, JCA Steeghs, D Repetto, S Wu, JF AF Torres, M. A. P. Jonker, P. G. Miller-Jones, J. C. A. Steeghs, D. Repetto, S. Wu, Jianfeng TI VLT spectroscopy of the black hole candidate Swift J1357.2-0933 in quiescence SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; binaries: close; stars: individual: Swift J1357.2-0933; X-rays: binaries ID X-RAY BINARY; ACCRETION DISKS; GRO J0422+32; XMM-NEWTON; ORBITAL PERIOD; MASS; SUPERHUMPS; EMISSION; XTE-J1118+480; COMPANION AB We present time-resolved optical spectroscopy of the counterpart to the high-inclination black hole low-mass X-ray binary Swift J1357.2-0933 in quiescence. Absorption features from the mass donor star were not detected. Instead the spectra display prominent broad double-peaked H alpha emission and weaker He I emission lines. From the H alpha peak-to-peak separation, we constrain the radial velocity semi-amplitude of the donor star to K-2 > 789 km s(-1). Further analysis through radial velocity and equivalent width measurements indicates that the H alpha line is free of variability due to S-wave components or disc eclipses. From our data and previous observations during outburst, we conclude that long-term radial velocity changes ascribed to a precessing disc were of low amplitude or not present. This implies that the centroid position of the line should closely represent the systemic radial velocity, gamma. Using the derived gamma = -150 km s(-1) and the best available limits on the source distance, we infer that the black hole is moving towards the plane in its current Galactic orbit unless the proper motion is substantial. Finally, the depth of the central absorption in the double-peaked profiles adds support for Swift J1357.2-0933 as a high-inclination system. On the other hand, we argue that the low hydrogen column density inferred from X-ray fitting suggests that the system is not seen edge-on. C1 [Torres, M. A. P.; Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Torres, M. A. P.; Jonker, P. G.; Repetto, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6525 AJ Nijmegen, Netherlands. [Torres, M. A. P.] European So Observ, Santiago 19001, Chile. [Miller-Jones, J. C. A.] Curtin Univ, Internat Ctr Radio Astron Res, Perth, WA 6845, Australia. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Wu, Jianfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torres, MAP (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM M.Torres@sron.nl RI Miller-Jones, James/B-2411-2013 OI Miller-Jones, James/0000-0003-3124-2814 FU Australian Research Council (ARC) [FT140101082, DP120102393]; STFC [PP/D005914/1, ST/I001719/1] FX We thank the anonymous referee for useful comments on the manuscript. We would like to thank Remco de Kok for an independent search for the cross-correlation signal from the donor star in J1357.2 and Jorge Casares for providing us with spectral templates used in these analysis. JCAMJ is the recipient of an Australian Research Council (ARC) Future Fellowship (FT140101082), and also acknowledges support from an ARC Discovery Grant (DP120102393). DS acknowledges support from STFC through an Advanced Fellowship (PP/D005914/1) as well as grant ST/I001719/1 NR 60 TC 4 Z9 4 U1 0 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 JUL 11 PY 2015 VL 450 IS 4 BP 4292 EP 4300 DI 10.1093/mnras/stv720 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CQ7YY UT WOS:000360824000071 ER PT J AU Aikawa, Y Furuya, K Nomura, H Qi, CH AF Aikawa, Yuri Furuya, Kenji Nomura, Hideko Qi, Chunhua TI ANALYTICAL FORMULAE OF MOLECULAR ION ABUNDANCES AND THE N2H+ RING IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; protoplanetary disks ID RADIATION HYDRODYNAMIC MODEL; DENSE INTERSTELLAR CLOUDS; PROTOSTELLAR COLLAPSE; HYDROGEN EMISSION; IONIZATION RATE; RAY IONIZATION; GRAIN-GROWTH; COSMIC-RAYS; CHEMISTRY; CO AB We investigate the chemistry of ion molecules in protoplanetary disks, motivated by the detection of the N2H+ ring around TW Hya. While the ring inner radius coincides with the CO snow line, it is not apparent why N2H+ is abundant outside the CO snow line in spite of the similar sublimation temperatures of CO and N-2. Using the full gas-grain network model, we reproduced the N2H+ ring in a disk model with millimeter grains. The chemical conversion of CO and N-2 to less volatile species (sink effect hereinafter) is found to affect the N2H+ distribution. Since the efficiency of the sink depends on various parameters such as activation barriers of grain-surface reactions, which are not well constrained, we also constructed the no-sink model; the total (gas and ice) CO and N-2 abundances are set constant, and their gaseous abundances are given by the balance between adsorption and desorption. Abundances of molecular ions in the no-sink model are calculated by analytical formulae, which are derived by analyzing the full-network model. The N2H+ ring is reproduced by the no-sink model, as well. The 2D (R-Z) distribution of N2H+, however, is different among the full-network model and no-sink model. The column density of N2H+ in the no-sink model depends sensitively on the desorption rate of CO and N-2. and the cosmic-ray flux. We also found that N2H+ abundance can peak at the temperature slightly below the CO sublimation, even if the desorption energies of CO and N-2 are the same. C1 [Aikawa, Yuri] Univ Tsukuba, Ctr Computat Sci, Tsukuba, Ibaraki 3058577, Japan. [Furuya, Kenji] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Nomura, Hideko] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Aikawa, Y (reprint author), Univ Tsukuba, Ctr Computat Sci, 1-1-1 Tennoudai, Tsukuba, Ibaraki 3058577, Japan. EM aikawa@ccs.tsukuba.ac.jp FU JSPS KAKENHI Grant [23103004, 23103005, 23540266, 25400229]; Japan Society for the Promotion of Science (JSPS) FX We thank Karin Oberg and Catherine Walsh for helpful discussions. We thank the anonymous referee for his/her constructive comments. This work was supported by JSPS KAKENHI Grant Numbers 23103004, 23103005, 23540266, and 25400229. Numerical calculation was partly conducted using SR16000 at YITP in Kyoto University for numerical calculations. K.F. is supported by the Research Fellowship from the Japan Society for the Promotion of Science (JSPS). NR 53 TC 5 Z9 5 U1 0 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 JUL 10 PY 2015 VL 807 IS 2 AR 120 DI 10.1088/0004-637X/807/2/120 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000006 ER PT J AU Akiyama, K Lu, RS Fish, VL Doeleman, SS Broderick, AE Dexter, J Hada, K Kino, M Nagai, H Honma, M Johnson, MD Algaba, JC Asada, K Brinkerink, C Blundell, R Bower, GC Cappallo, R Crew, GB Dexter, M Dzib, SA Freund, R Friberg, P Gurwell, M Ho, PTP Inoue, M Krichbaum, TP Loinard, L MacMahon, D Marrone, DP Moran, JM Nakamura, M Nagar, NM Ortiz-Leon, G Plambeck, R Pradel, N Primiani, RA Rogers, AEE Roy, AL SooHoo, J Tavares, JL Tilanus, RPJ Titus, M Wagner, J Weintroub, J Yamaguchi, P Young, KH Zensus, A Ziurys, LM AF Akiyama, Kazunori Lu, Ru-Sen Fish, Vincent L. Doeleman, Sheperd S. Broderick, Avery E. Dexter, Jason Hada, Kazuhiro Kino, Motoki Nagai, Hiroshi Honma, Mareki Johnson, Michael D. Algaba, Juan C. Asada, Keiichi Brinkerink, Christiaan Blundell, Ray Bower, Geoffrey C. Cappallo, Roger Crew, Geoffrey B. Dexter, Matt Dzib, Sergio A. Freund, Robert Friberg, Per Gurwell, Mark Ho, Paul T. P. Inoue, Makoto Krichbaum, Thomas P. Loinard, Laurent MacMahon, David Marrone, Daniel P. Moran, James M. Nakamura, Masanori Nagar, Neil M. Ortiz-Leon, Gisela Plambeck, Richard Pradel, Nicolas Primiani, Rurik A. Rogers, Alan E. E. Roy, Alan L. SooHoo, Jason Tavares, Jonathan-Leon Tilanus, Remo P. J. Titus, Michael Wagner, Jan Weintroub, Jonathan Yamaguchi, Paul Young, Ken H. Zensus, Anton Ziurys, Lucy M. TI 230 GHz VLBI OBSERVATIONS OF M87: EVENT-HORIZON-SCALE STRUCTURE DURING AN ENHANCED VERY-HIGH-ENERGY gamma-RAY STATE IN 2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (M87); galaxies: jets; radio continuum: galaxies; techniques: high angular resolution; techniques: interferometric ID SUPERMASSIVE BLACK-HOLE; SAGITTARIUS-A-ASTERISK; ADVECTION-DOMINATED ACCRETION; ACTIVE GALACTIC NUCLEI; SIMILAR-TO-10 SCHWARZSCHILD RADII; HIGH-FREQUENCY VLBI; TEV EMISSION; JET BASE; UNIFIED SCHEMES; X-RAY AB We report on 230 GHz (1.3 mm) very long baseline interferometry (VLBI) observations of M87 with the Event Horizon Telescope using antennas on Mauna Kea in Hawaii, Mt. Graham in Arizona, and Cedar Flat in California. For the first time, we have acquired 230 GHz VLBI interferometric phase information on M87 through measurement of the closure phase on the triangle of long baselines. Most of the measured closure phases are consistent with 0 degrees as expected by physically motivated models for 230 GHz structure such as jet models and accretion disk models. The brightness temperature of the event-horizon-scale structure is similar to 1 x 10(10) K derived from the compact flux density of similar to 1 Jy and the angular size of similar to 40 mu as similar to 5.5 R-s, which is broadly consistent with the peak brightness of the radio cores at 1-86 GHz located within similar to 10(2) R-s. Our observations occurred in the middle of an enhancement in very-high-energy (VHE) gamma-ray flux, presumably originating in the vicinity of the central black hole. Our measurements, combined with results of multi-wavelength observations, favor a scenario in which the VHE region has an extended size of similar to 20-60 R-s. C1 [Akiyama, Kazunori] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Akiyama, Kazunori; Hada, Kazuhiro; Nagai, Hiroshi; Honma, Mareki] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Lu, Ru-Sen; Fish, Vincent L.; Doeleman, Sheperd S.; Cappallo, Roger; Crew, Geoffrey B.; Rogers, Alan E. E.; SooHoo, Jason; Titus, Michael] MIT, Haystack Observ, Westford, MA 01886 USA. [Lu, Ru-Sen; Dzib, Sergio A.; Krichbaum, Thomas P.; Roy, Alan L.; Wagner, Jan; Zensus, Anton] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Doeleman, Sheperd S.; Johnson, Michael D.; Blundell, Ray; Gurwell, Mark; Moran, James M.; Primiani, Rurik A.; Weintroub, Jonathan; Yamaguchi, Paul; Young, Ken H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Broderick, Avery E.] Perimeter Inst Theoret Phys, North Waterloo, ON N2L 2Y5, Canada. [Broderick, Avery E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N21 3G1, Canada. [Dexter, Jason] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Hada, Kazuhiro] INAF Ist Radioastron, I-40129 Bologna, Italy. [Kino, Motoki; Algaba, Juan C.; Wagner, Jan] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. [Honma, Mareki] Grad Univ Adv Studies, Mitaka, Tokyo 1818588, Japan. [Algaba, Juan C.; Asada, Keiichi; Ho, Paul T. P.; Inoue, Makoto; Nakamura, Masanori; Pradel, Nicolas] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Brinkerink, Christiaan; Tilanus, Remo P. J.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Bower, Geoffrey C.] Acad Sinica, Inst Astron & Astrophys, Hilo, HI 96720 USA. [Dexter, Matt; MacMahon, David; Plambeck, Richard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Dzib, Sergio A.; Loinard, Laurent; Ortiz-Leon, Gisela] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Freund, Robert; Marrone, Daniel P.; Ziurys, Lucy M.] Univ Arizona, Arizona Radio Observ, Steward Observ, Tucson, AZ 85721 USA. [Friberg, Per] Joint Astron Ctr, James Clerk Maxwell Telescope, Hilo, HI 96720 USA. [Nagar, Neil M.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Tavares, Jonathan-Leon] Inst Nacl Astrofis Opt & Electr, Puebla 72000, Mexico. [Tilanus, Remo P. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Akiyama, K (reprint author), Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan. EM kazunori.akiyama@nao.ac.jp FU Japan Society for the Promotion of Science (JSPS); Perimeter Institute for Theoretical Physics; Natural Sciences and Engineering Research Council of Canada; DGAPA; UNAM; CONACyT (Mexico); National Science Foundation (NSF); Gordon and Betty Moore Foundation [GMBF-3561]; NSF University Radio Observatories (URO) program [AST 1140030]; Smithsonian Institution; Academia Sinica; NSF; CARMA partner universities; MEXT/JSPS KAKENHI [24540242, 25120007, 25120008]; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX We would like to thank an anonymous referee for many constructive suggestions to improve the paper. K. Akiyama thanks Dr. Akihiro Doi, Prof. Alan Marscher, Dr. Svetlana Jorstad, and Dr. Jose L. Gomez for fruitful discussions on scientific interpretations. K. Akiyama and K. H. are supported by a Grant-in-Aid for Research Fellows of the Japan Society for the Promotion of Science (JSPS). A. E. B. receives financial support from the Perimeter Institute for Theoretical Physics and the Natural Sciences and Engineering Research Council of Canada through a Discovery Grant. L. L. and G. O. L. acknowledge the support of DGAPA, UNAM, and CONACyT (Mexico). Event Horizon Telescope work at the MIT Haystack Observatory and the Harvard Smithsonian Center for Astrophysics is supported by grants from the National Science Foundation (NSF) and through an award from the Gordon and Betty Moore Foundation (GMBF-3561). The Arizona Radio Observatory (ARO) is partially supported through the NSF University Radio Observatories (URO) program under grant No. AST 1140030. 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. Funding for ongoing CARMA development and operations is supported by the NSF and the CARMA partner universities. Event Horizon Telescope work at the Mizusawa VLBI Observatory is financially supported by the MEXT/JSPS KAKENHI Grant Numbers 24540242, 25120007, and 25120008. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research and Innovation. This work has benefited from open source technology shared by the Collaboration for Astronomy Signal Processing and Electronics Research (CASPER) and from equipment donated by Xilinx Inc. NR 92 TC 17 Z9 16 U1 2 U2 8 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 JUL 10 PY 2015 VL 807 IS 2 AR 150 DI 10.1088/0004-637X/807/2/150 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000036 ER PT J AU Asgari-Targhi, M Schmelz, JT Imada, S Pathak, S Christian, GM AF Asgari-Targhi, M. Schmelz, J. T. Imada, S. Pathak, S. Christian, G. M. TI MODELING OF HOT PLASMA IN THE SOLAR ACTIVE REGION CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; Sun: UV radiation ID EUV IMAGING SPECTROMETER; ALFVEN-WAVE TURBULENCE; FIELD TEMPERATURE DISTRIBUTIONS; AN ATOMIC DATABASE; X-RAY TELESCOPE; CORONAL LOOPS; EMISSION MEASURE; HINODE; DYNAMICS; MOTIONS AB Magnetically confined plasma with temperatures >= 5 MK are a feature of hot coronal loops observed in the core of active regions. In this paper, using observations and MHD modeling of coronal loops, we investigate whether wave heating (Alternating Current) models can describe the high temperature loops observed in the active region of 2012 September 7. We construct three-dimensional MHD models for the Alfven wave turbulence within loops with high temperature. We find that for the Alfven waves to create enough turbulence to heat the corona, the rms velocity at the footpoints must be 5-6 km s(-1). We conclude that the Alfven wave turbulence model may be a candidate for explaining how the hot loops are heated, provided the loops have a high velocity at their photospheric footpoints. C1 [Asgari-Targhi, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schmelz, J. T.; Pathak, S.; Christian, G. M.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Imada, S.] Nagoya Univ, Solar Terr Environm Lab, Chikusa Ku, Nagoya, Aichi 4648601, Japan. RP Asgari-Targhi, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 15, Cambridge, MA 02138 USA. FU UK's Engineering and Physical Sciences Research Council [EP/I034327/1] FX We thank the referee for comments which helped to improve the paper. We thank Adriaan A. van Ballegooijen for discussions and comments that helped improve the paper. We are most grateful to Alex Voss from the School of Computer Science at the University of St. Andrews for his support with the computational work, which was funded by the UK's Engineering and Physical Sciences Research Council (EP/I034327/1). NR 55 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 JUL 10 PY 2015 VL 807 IS 2 AR 146 DI 10.1088/0004-637X/807/2/146 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000032 ER PT J AU Cheung, MCM Boerner, P Schrijver, CJ Testa, P Chen, F Peter, H Malanushenko, A AF Cheung, Mark C. M. Boerner, P. Schrijver, C. J. Testa, P. Chen, F. Peter, H. Malanushenko, A. TI THERMAL DIAGNOSTICS WITH THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD THE SOLAR DYNAMICS OBSERVATORY: A VALIDATED METHOD FOR DIFFERENTIAL EMISSION MEASURE INVERSIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: observational; plasmas; radiation mechanisms: thermal; Sun: activity; Sun: atmosphere; Sun: corona ID ACTIVE-REGION; TEMPERATURE STRUCTURE; MAGNETIC-FIELD; FUNDAMENTAL LIMITATIONS; PLASMAS. APPLICATION; ATOMIC DATABASE; FLUX EMERGENCE; CORONAL LOOPS; SIMULATIONS; SPECTRA AB We present a new method for performing differential emission measure (DEM) inversions on narrow-band EUV images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. The method yields positive definite DEM solutions by solving a linear program. This method has been validated against a diverse set of thermal models of varying complexity and realism. These include (1) idealized Gaussian DEM distributions, (2) 3D models of NOAA Active Region 11158 comprising quasi-steady loop atmospheres in a nonlinear force-free field, and (3) thermodynamic models from a fully compressible, 3D MHD simulation of active region (AR) corona formation following magnetic flux emergence. We then present results from the application of the method to AIA observations of Active Region 11158, comparing the region's thermal structure on two successive solar rotations. Additionally, we show how the DEM inversion method can be adapted to simultaneously invert AIA and Hinode X-ray Telescope data, and how supplementing AIA data with the latter improves the inversion result. The speed of the method allows for routine production of DEM maps, thus facilitating science studies that require tracking of the thermal structure of the solar corona in time and space. C1 [Cheung, Mark C. M.; Boerner, P.; Schrijver, C. J.; Malanushenko, A.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Testa, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, F.; Peter, H.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Malanushenko, A.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80301 USA. RP Cheung, MCM (reprint author), Lockheed Martin Solar & Astrophys Lab, 3251 Hanover St Bldg 252, Palo Alto, CA 94304 USA. EM cheung@lmsal.com RI Chen, Feng/B-1968-2012 OI Chen, Feng/0000-0002-1963-5319 FU NASA's SDO/AIA contract [NNG04EA00C]; NASA [NNX14AI14G] FX The authors acknowledge support from NASA's SDO/AIA contract (NNG04EA00C) to LMSAL. AIA is an instrument on board the Solar Dynamics Observatory, a mission for NASA's Living With a Star program. Additionally, M.C.M.C., P.T. and A.M. acknowledge support from NASA's Heliophysics Grand Challenges Research grant (NNX14AI14G). The authors wish to thank members of the Hinode/XRT team (especially M. Weber and K. Reeves) for valuable discussions about joint AIA/XRT inversions. Furthermore, we wish to thank H. Warren, J. Plowman, S. White, and the anonymous referee for helpful comments that led to improvements in this work. NR 60 TC 8 Z9 9 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 JUL 10 PY 2015 VL 807 IS 2 AR 143 DI 10.1088/0004-637X/807/2/143 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000029 ER PT J AU Espaillat, C Andrews, S Powell, D Feldman, D Qi, C Wilner, D D'Alessio, P AF Espaillat, C. Andrews, S. Powell, D. Feldman, D. Qi, C. Wilner, D. D'Alessio, P. TI THE TRANSITIONAL DISK AROUND IRAS 04125+2902 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: planetary systems; planet-disk interactions; planets and satellites: formation; protoplanetary disks; stars: pre-main sequence; submillimeter: planetary systems ID T-TAURI STARS; MAIN-SEQUENCE STARS; AURIGA MOLECULAR CLOUD; MASS ACCRETION RATES; SPITZER IRS SPECTRA; ALL-SKY SURVEY; PROTOPLANETARY DISKS; PRETRANSITIONAL DISKS; YOUNG OBJECTS; GRAIN-GROWTH AB Resolved submillimeter imaging of transitional disks is increasingly revealing the complexity of disk structure. Here, we present the first high-resolution submillimeter image of a recently identified transitional disk around IRAS 04125+2902 in the Taurus star-forming region. We measure an inner disk hole of similar to 20 AU around IRAS 04125+2902 by simultaneously modeling new 880 mu m Submillimeter Array data along with an existing spectral energy distribution supplemented by new Discovery Channel Telescope photometry. We also constrain the outer radius of the dust disk in IRAS 04125+2902 to similar to 50-60 AU. Such a small dust disk could be attributed to initial formation conditions, outward truncation by an unseen companion, or dust evolution in the disk. Notably, the dust distribution of IRAS 04125+2902 resembles a narrow ring (Delta R similar to 35 AU) composed of large dust grains at the location of the disk wall. Such narrow dust rings are also seen in other transitional disks and may be evidence of dust trapping in pressure bumps, possibly produced by planetary companions. More sensitive submillimeter observations of the gas are necessary to further probe the physical mechanisms at work in shaping the spatial distribution of large dust in this disk. Interestingly, the IRAS 04125+2902 disk is significantly fainter than other transitional disks that have been resolved at submillimeter wavelengths, hinting that more objects with large disk holes may exist at the faint end of the submillimeter luminosity distribution that await detection with more sensitive imaging telescopes. C1 [Espaillat, C.; Feldman, D.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Andrews, S.; Powell, D.; Qi, C.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. RP Espaillat, C (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM cce@bu.edu FU Smithsonian Institution; Academia Sinica; University of Maryland; University of Toledo; Northern Arizona University; Discovery Communications, Inc., Boston University FX We thank the referee for comments that helped to improve the paper. We thank Nuria Calvet, Ramiro Franco-Hernanndez, Elise Furlan, and Melissa McClure for discussions. We thank Adam Kraus for sharing results before publication. The SMA 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 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. These results made use of the Discovery Channel Telescope at Lowell Observatory, supported by Discovery Communications, Inc., Boston University, the University of Maryland, the University of Toledo and Northern Arizona University. Finally, a special recognition of the contribution of Paola D'Alessio, who passed away in November of 2013. She is greatly missed as a scientist, colleague, and friend. Paola would have been happy to see her research continue to have an important impact in the star formation community. NR 103 TC 3 Z9 3 U1 0 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 JUL 10 PY 2015 VL 807 IS 2 AR 156 DI 10.1088/0004-637X/807/2/156 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000042 ER PT J AU Keisler, R Hoover, S Harrington, N Henning, JW Ade, PAR Aird, KA Austermann, JE Beall, JA Bender, AN Benson, BA Bleem, LE Carlstrom, JE Chang, CL Chiang, HC Cho, HM Citron, R Crawford, TM Crites, AT de Haan, T Dobbs, MA Everett, W Gallicchio, J Gao, J George, EM Gilbert, A Halverson, NW Hanson, D Hilton, GC Holder, GP Holzapfel, WL Hou, Z Hrubes, JD Huang, N Hubmayr, J Irwin, KD Knox, L Lee, AT Leitch, EM Li, D Luong-Van, D Marrone, DP McMahon, JJ Mehl, J Meyer, SS Mocanu, L Natoli, T Nibarger, JP Novosad, V Padin, S Pryke, C Reichardt, CL Ruhl, JE Saliwanchik, BR Sayre, JT Schaffer, KK Shirokoff, E Smecher, G Stark, AA Story, KT Tucker, C Vanderlinde, K Vieira, JD Wang, G Whitehorn, N Yefremenko, V Zahn, O AF Keisler, R. Hoover, S. Harrington, N. Henning, J. W. Ade, P. A. R. Aird, K. A. Austermann, J. E. Beall, J. A. Bender, A. N. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Chiang, H. C. Cho, H-M. Citron, R. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Everett, W. Gallicchio, J. Gao, J. George, E. M. Gilbert, A. Halverson, N. W. Hanson, D. Hilton, G. C. Holder, G. P. Holzapfel, W. L. Hou, Z. Hrubes, J. D. Huang, N. Hubmayr, J. Irwin, K. D. Knox, L. Lee, A. T. Leitch, E. M. Li, D. Luong-Van, D. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Natoli, T. Nibarger, J. P. Novosad, V. Padin, S. Pryke, C. Reichardt, C. L. Ruhl, J. E. Saliwanchik, B. R. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Smecher, G. Stark, A. A. Story, K. T. Tucker, C. Vanderlinde, K. Vieira, J. D. Wang, G. Whitehorn, N. Yefremenko, V. Zahn, O. TI MEASUREMENTS OF SUB-DEGREE B-MODE POLARIZATION IN THE COSMIC MICROWAVE BACKGROUND FROM 100 SQUARE DEGREES OF SPTPOL DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations ID SOUTH-POLE TELESCOPE; LARGE-SCALE STRUCTURE; CMB POLARIZATION; POWER SPECTRUM; ANISOTROPIES; TEMPERATURE; COMPUTATION; PARAMETERS; PHYSICS; RADIO AB We present a measurement of the B-mode polarization power spectrum (the BB spectrum) from 100 deg(2) of sky observed with SPTpol, a polarization-sensitive receiver currently installed on the South Pole Telescope. The observations used in this work were taken during 2012 and early 2013 and include data in spectral bands centered at 95 and 150 GHz. We report the BB spectrum in five bins in multipole space, spanning the range 300 <= l <= 2300, and for three spectral combinations: 95 GHz x 95 GHz, 95 GHz x 150 GHz, and 150 GHz x 150 GHz. We subtract small (<0.5 sigma in units of statistical uncertainty) biases from these spectra and account for the uncertainty in those biases. The resulting power spectra are inconsistent with zero power but consistent with predictions for the BB spectrum arising from the gravitational lensing of E-mode polarization. If we assume no other source of BB power besides lensed B modes, we determine a preference for lensed B modes of 4.9 sigma. After marginalizing over tensor power and foregrounds, namely, polarized emission from galactic dust and extragalactic sources, this significance is 4.3 sigma. Fitting for a single parameter, A(lens), that multiplies the predicted lensed B-mode spectrum, and marginalizing over tensor power and foregrounds, we find A(lens) = 1.08 +/- 0.26, indicating that our measured spectra are consistent with the signal expected from gravitational lensing. The data presented here provide the best measurement to date of the B-mode power spectrum on these angular scales. C1 [Keisler, R.; Irwin, K. D.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Keisler, R.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Hoover, S.; Henning, J. W.; Bender, A. N.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Citron, R.; Crawford, T. M.; Crites, A. T.; Gallicchio, J.; Hou, Z.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Schaffer, K. K.; Shirokoff, E.; Story, K. T.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Hoover, S.; Bleem, L. E.; Carlstrom, J. E.; Natoli, T.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Harrington, N.; de Haan, T.; George, E. M.; Holzapfel, W. L.; Huang, N.; Lee, A. T.; Reichardt, C. L.; Whitehorn, N.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Henning, J. W.; Austermann, J. E.; Everett, W.; Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Ade, P. A. R.; Tucker, C.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Austermann, J. E.; Beall, J. A.; Gao, J.; Hilton, G. C.; Hubmayr, J.; Li, D.; Nibarger, J. P.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Bender, A. N.; Dobbs, M. A.; Gilbert, A.; Hanson, D.; Holder, G. P.; Smecher, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Bender, A. N.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Mehl, J.; Wang, G.; Yefremenko, V.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Shirokoff, E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Carlstrom, J. E.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Chiang, H. C.] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Durban, South Africa. [Cho, H-M.; Li, D.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Crites, A. T.; Padin, S.] CALTECH, Pasadena, CA 91125 USA. [Dobbs, M. A.] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Novosad, V.] Argonne Natl Lab, Div Mat Sci, Argonne, IL 60439 USA. [Pryke, C.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Smecher, G.] Three Speed Log Inc, Vancouver, BC V6A 2J8, Canada. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron Astrophys, Toronto, ON M5S 3H4, Canada. [Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Keisler, R (reprint author), Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM rkeisler@stanford.edu RI Novosad, V /J-4843-2015; OI CRAWFORD, THOMAS/0000-0001-9000-5013; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [PLR-1248097, AST-1402161]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation through Grant GBMF [947]; Natural Sciences and Engineering Research Council of Canada; Canadian Institute for Advanced Research; Canada Research Chairs program; Fermi Research Alliance, LLC [De-AC02-07CH11359]; U.S. Department of Energy; NSF [AST-0956135]; UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne); Argonne, a U.S. Department of Energy Office of Science Laboratory [DE-AC02-06CH11357]; Argonne Center for Nanoscale Materials; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX The South Pole Telescope program 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. The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and Canada Research Chairs program. J.W.H. is supported by the National Science Foundation under Award No. AST-1402161. B.B. is supported by the Fermi Research Alliance, LLC, under Contract No. De-AC02-07CH11359 with the U.S. Department of Energy. The CU Boulder group acknowledges support from NSF AST-0956135. This work is also supported by the U.S. Department of Energy. Work at Argonne National Lab is supported by UChicago Argonne, LLC, Operator of Argonne National Laboratory (Argonne). Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated under Contract No. DE-AC02-06CH11357. We also acknowledge support from the Argonne Center for Nanoscale Materials. 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. The data analysis pipeline uses the scientific python stack (Jones et al. 2001; Hunter 2007; van der Walt et al. 2011) and the HDF5 file format (The HDF Group 1997). NR 56 TC 33 Z9 33 U1 1 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 JUL 10 PY 2015 VL 807 IS 2 AR 151 DI 10.1088/0004-637X/807/2/151 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000037 ER PT J AU Skibba, RA Coil, AL Mendez, AJ Blanton, MR Bray, AD Cool, RJ Eisenstein, DJ Guo, H Miyaji, T Moustakas, J Zhu, GT AF Skibba, Ramin A. Coil, Alison L. Mendez, Alexander J. Blanton, Michael R. Bray, Aaron D. Cool, Richard J. Eisenstein, Daniel J. Guo, Hong Miyaji, Takamitsu Moustakas, John Zhu, Guangtun TI DARK MATTER HALO MODELS OF STELLAR MASS-DEPENDENT GALAXY CLUSTERING IN PRIMUS+DEEP2 AT 0.2 < z < 1.2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: evolution; galaxies: halos; large-scale structure of universe; methods: analytical; methods: statistical AB We utilize Lambda CDM halo occupation models of galaxy clustering to investigate the evolving stellar mass dependent clustering of galaxies in the PRIsm MUlti-object Survey (PRIMUS) and DEEP2 Redshift Survey over the past eight billion years of cosmic time, between 0.2 < z < 1.2. These clustering measurements provide new constraints on the connections between dark matter halo properties and galaxy properties in the context of the evolving large-scale structure of the universe. Using both an analytic model and a set of mock galaxy catalogs, we find a strong correlation between central galaxy stellar mass and dark matter halo mass over the range M-halo similar to 10(11)-10(13)h(-1) M-circle dot, approximately consistent with previous observations and theoretical predictions. However, the stellar-to-halo mass relation and the mass scale where star formation efficiency reaches a maximum appear to evolve more strongly than predicted by other models, including models based primarily on abundance-matching constraints. We find that the fraction of satellite galaxies in halos of a given mass decreases significantly from z similar to 0.5 to z similar to 0.9, partly due to the fact that halos at fixed mass are rarer at higher redshift and have lower abundances. We also find that the M-1/M-min ratio, a model parameter that quantifies the critical mass above which halos host at least one satellite, decreases from approximate to 20 at z similar to 0 to approximate to 13 at z similar to 0.9. Considering the evolution of the subhalo mass function vis-a-vis satellite abundances, this trend has implications for relations between satellite galaxies and halo substructures and for intracluster mass, which we argue has grown due to stripped and disrupted satellites between z similar to 0.9 and z similar to 0.5. C1 [Skibba, Ramin A.; Coil, Alison L.; Mendez, Alexander J.] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Mendez, Alexander J.; Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bray, Aaron D.; Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cool, Richard J.] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA. [Guo, Hong] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Miyaji, Takamitsu] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. RP Skibba, RA (reprint author), Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM raminskibba@gmail.com RI Guo, Hong/J-5797-2015; OI Guo, Hong/0000-0003-4936-8247; Zhu, Guangtun/0000-0002-7574-8078; Miyaji, Takamitsu/0000-0002-7562-485X FU NSF CAREER award [AST-1055081]; UNAM-DGAPA PAPIIT [IN110209]; CONACyT [83564]; NSF [PHYS-1066293, AST-0607701, 0908246, 0908442, 0908354]; NASA [08-ADP08-0019] FX R.A.S. and A.L.C. acknowledge support from the NSF CAREER award AST-1055081. T.M. is supported by UNAM-DGAPA PAPIIT IN110209 and CONACyT Grant #83564. We thank the Aspen Center for Physics, which has been supported by NSF grant PHYS-1066293, for hospitality during the summer 2014 workshop on the "Galaxy-Halo Connection Across Cosmic Time," where some of this work was completed. We acknowledge Peter Behroozi, Andrew Hearin, Alexie Leauthaud, Ravi Sheth, and Doug Watson for valuable discussions about our models and results, and we thank Idit Zehavi and Zheng Zheng for helpful comments on a previous draft. We also thank the anonymous referee for valuable recommendations that improved the quality of the paper. We acknowledge Scott Burles and Kenneth Wong for their contributions to the PRIMUS project. Funding for PRIMUS has been provided by NSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA grant 08-ADP08-0019. NR 0 TC 12 Z9 12 U1 0 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 JUL 10 PY 2015 VL 807 IS 2 AR 152 DI 10.1088/0004-637X/807/2/152 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000038 ER PT J AU Su, YN van Ballegooijen, A McCauley, P Ji, HS Reeves, KK DeLuca, EE AF Su, Yingna van Ballegooijen, Adriaan McCauley, Patrick Ji, Haisheng Reeves, Katharine K. DeLuca, Edward E. TI MAGNETIC STRUCTURE AND DYNAMICS OF THE ERUPTING SOLAR POLAR CROWN PROMINENCE ON 2012 MARCH 12 SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: corona; Sun: coronal mass ejections (CMEs); Sun: filaments; prominences; Sun: magnetic fields ID CORONAL MASS EJECTIONS; FLUX ROPES; RECONNECTION OUTFLOWS; ACTIVE REGIONS; CURRENT SHEET; FILAMENT; FLARES; FIELD; MODEL; ONSET AB We present an investigation of the polar crown prominence that erupted on 2012 March 12. This prominence is observed at the southeast limb by the Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA; end-on view) and displays a quasi-vertical thread structure. A bright U-shaped or horn-like structure is observed surrounding the upper portion of the prominence at 171 angstrom before the eruption and becomes more prominent during the eruption. The disk view of STEREOB shows that this long prominence is composed of a series of vertical threads and displays a half-loop-like structure during the eruption. We focus on the magnetic support of the prominence vertical threads by studying the structure and dynamics of the prominence before and during the eruption using observations from SDO and STEREO_B. We also construct a series of magnetic field models (sheared arcade model, twisted flux rope model, and unstable model with hyperbolic flux tube). Various observational characteristics appear to be in favor of the twisted flux rope model. We find that the flux rope supporting the prominence enters the regime of torus instability at the onset of the fast-rise phase, and signatures of reconnection (posteruption arcade, new U-shaped structure, rising blobs) appear about one hour later. During the eruption, AIA observes dark ribbons seen in absorption at 171 angstrom corresponding to the bright ribbons shown at 304 angstrom, which might be caused by the erupting filament material falling back along the newly reconfigured magnetic fields. Brightenings at the inner edge of the erupting prominence arcade are also observed in all AIA EUV channels, which might be caused by the heating due to energy released from reconnection below the rising prominence. C1 [Su, Yingna; Ji, Haisheng] Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China. [Su, Yingna; van Ballegooijen, Adriaan; McCauley, Patrick; Reeves, Katharine K.; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Su, YN (reprint author), Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Sci, Nanjing 210008, Jiangsu, Peoples R China. EM ynsu@pmo.ac.cn RI McCauley, Patrick/P-7747-2015; DeLuca, Edward/L-7534-2013; OI McCauley, Patrick/0000-0002-1450-7350; DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen, Adriaan/0000-0002-5622-3540; Reeves, Katharine/0000-0002-6903-6832 FU LMSAL [SP02H1701R]; NASA [NNX12AI30G]; Natural Science Foundation of China (NSFC) [11333009, 11173062, 11473071]; Youth Fund of Jiangsu [BK20141043]; Chinese Academy of Sciences FX We thank the referee for helpful comments to improve the manuscript. Y.N.S. is grateful to Drs. Cheng Fang, Bernhard Kliem, Xin Cheng, Eric Priest, and Bin Chen for valuable discussions. We thank the teams of SDO/AIA, SDO/HMI, STEREO/EUVI for providing the valuable data. The STEREO and HMI data are downloaded via the Virtual Solar Observatory and the Joint Science Operations Center. This project is partially supported under contract SP02H1701R from LMSAL to SAO as well as NASA grant NNX12AI30G. This work is also supported by the Natural Science Foundation of China (NSFC) No. 11333009, 11173062, 11473071, and the Youth Fund of Jiangsu No. BK20141043. Y.N.S. is also supported by the "One hundred talent project" of the Chinese Academy of Sciences. NR 71 TC 9 Z9 9 U1 0 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 JUL 10 PY 2015 VL 807 IS 2 AR 144 DI 10.1088/0004-637X/807/2/144 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO2EB UT WOS:000358967000030 ER PT J AU Estrada, C Degner, EC Rojas, EI Wcislo, WT Van Bael, SA AF Estrada, Catalina Degner, Ethan C. Rojas, Enith I. Wcislo, William T. Van Bael, Sunshine A. TI The role of endophyte diversity in protecting plants from defoliation by leaf-cutting ants SO CURRENT SCIENCE LA English DT Article DE Atta colombica; Colletotrichum tropicale; fungal community; herbivory; symbiosis ID IN-VITRO INTERACTIONS; FUNGAL ENDOPHYTES; FUSARIUM-VERTICILLIOIDES; FOLIAR ENDOPHYTES; SYMBIOTIC FUNGI; USTILAGO-MAYDIS; SALICYLIC-ACID; PATHOGEN; RESISTANCE; TRAITS AB Plants host a vast diversity of fungal symbionts inside their tissues that live in close proximity with each other to form rich and dynamic communities. Although endophytes can affect plant-herbivore interactions in several ways, it is still not known to what extent such effects are influenced by the properties of endophyte communities or by particular species traits. Here we compared the effects of high versus low foliar fungal endophyte diversity on the preferences of laboratory and wild colonies of leaf-cutting ants. We found that when endophyte densities were high, the ants responded similarly to leaves hosting one endophyte species, Colletotrichum tropicale, or those hosting a species-rich endophyte community. Results were also consistent when comparing the laboratory versus wild ant colonies. We discuss the significance of these results with respect to the ecological effects of plant-endophyte interactions in natural and agricultural ecosystems. C1 [Estrada, Catalina; Degner, Ethan C.; Rojas, Enith I.; Wcislo, William T.; Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Panama City, Panama. [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. RP Estrada, C (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM estradac@si.edu FU Smithsonian Institute Scholarly Studies Program; STRI Internship; NSF [DEB-0949602]; SENACYT [FID10-091] FX We thank M. Caballero and F. Santos (STRI) for laboratory support. This work was funded by the Smithsonian Institute Scholarly Studies Program to W.T.W. and S.A.V.; Restricted Endowment Funds to C.E., S.A.V. and W.T.W.; postdoctoral Fellowship to C.E., STRI Internship to E.C.D., NSF DEB-0949602 to S.A.V. and W.T.W. and SENACYT FID10-091 to S.A.V. and W.T.W. We also thank Panama's Authority on the Environment (ANAM), for permission to undertake this research. NR 44 TC 2 Z9 3 U1 8 U2 45 PU INDIAN ACAD SCIENCES PI BANGALORE PA C V RAMAN AVENUE, SADASHIVANAGAR, P B #8005, BANGALORE 560 080, INDIA SN 0011-3891 J9 CURR SCI INDIA JI Curr. Sci. PD JUL 10 PY 2015 VL 109 IS 1 BP 55 EP 61 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN2JR UT WOS:000358247500015 ER PT J AU Zhang, Y Cao, QS Rubenstein, DI Zang, S Songer, M Leimgruber, P Chu, HJ Cao, J Li, K Hu, DF AF Zhang, Yongjun Cao, Qing S. Rubenstein, Daniel I. Zang, Sen Songer, Melissa Leimgruber, Peter Chu, Hongjun Cao, Jie Li, Kai Hu, Defu TI Water Use Patterns of Sympatric Przewalski's Horse and Khulan: Interspecific Comparison Reveals Niche Differences SO PLOS ONE LA English DT Article ID SOCIAL-ORGANIZATION; ECOLOGY; POPULATION; MONGOLIA; BEHAVIOR; TAKHI AB Acquiring water is essential for all animals, but doing so is most challenging for desert-living animals. Recently Przewalski's horse has been reintroduced to the desert area in China where the last wild surviving member of the species was seen before it vanished from China in the 1960s. Its reintroduction placed it within the range of a close evolutionary relative, the con-generic Khulan. Determining whether or not these two species experience competition and whether or not such competition was responsible for the extinction of Przewalski's horses in the wild over 50 years ago, requires identifying the fundamental and realized niches of both species. We remotely monitored the presence of both species at a variety of water points during the dry season in Kalamaili Nature Reserve, Xinjiang, China. Przewalski's horses drank twice per day mostly during daylight hours at low salinity water sources while Khulans drank mostly at night usually at high salinity water points or those far from human residences. Spatial and temporal differences in water use enables coexistence, but suggest that Przewalski's horses also restrict the actions of Khulan. Such differences in both the fundamental and realized niches were associated with differences in physiological tolerances for saline water and human activity as well as differences in aggression and dominance. C1 [Zhang, Yongjun; Zang, Sen; Chu, Hongjun; Li, Kai; Hu, Defu] Beijing Forestry Univ, Coll Nat Conservat, Beijing, Peoples R China. [Cao, Qing S.; Rubenstein, Daniel I.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Cao, Qing S.; Songer, Melissa; Leimgruber, Peter] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Chu, Hongjun] Altai Forestry Bur, Altai, Xinjiang, Peoples R China. [Cao, Jie] Xinjiang Forestry Dept, Wild Horse Breeding Ctr, Urumqi, Xinjiang, Peoples R China. RP Hu, DF (reprint author), Beijing Forestry Univ, Coll Nat Conservat, Beijing, Peoples R China. EM hudf@bjfu.edu.cn RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU National Natural Science Foundation of China [30970545]; National Science Foundation [NSF-IIS-0705311]; Association of Zoos and Aquarium's Conservation Endowment Fund [11-1059] FX National Natural Science Foundation of China (Grant No. 30970545); National Science Foundation (NSF-IIS-0705311); Association of Zoos and Aquarium's Conservation Endowment Fund (Grant No. 11-1059). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 53 TC 2 Z9 2 U1 1 U2 17 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 JUL 10 PY 2015 VL 10 IS 7 AR e0132094 DI 10.1371/journal.pone.0132094 PG 17 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1FD UT WOS:000358162300091 PM 26161909 ER PT J AU Kristensen, LE Bergin, EA AF Kristensen, Lars E. Bergin, Edwin A. TI TRACING EMBEDDED STELLAR POPULATIONS IN CLUSTERS AND GALAXIES USING MOLECULAR EMISSION: METHANOL AS A SIGNATURE OF THE LOW-MASS END OF THE IMF SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: jets and outflows; line: profiles; stars: formation; stars: winds, outflows ID SPATIALLY-RESOLVED CHEMISTRY; STAR-FORMATION RATES; NEARBY GALAXIES; PROTOSTARS; EVOLUTION; OUTFLOWS; CLOUDS; CORE; II.; GAS AB Most low-mass protostars form in clusters, in particular high-mass clusters; however, how low-mass stars form in high-mass clusters and what the mass distribution is are still open questions both in our own Galaxy and elsewhere. To access the population of forming embedded low-mass protostars observationally, we propose using molecular outflows as tracers. Because the outflow emission scales with mass, the effective contrast between low-mass protostars and their high-mass cousins is greatly lowered. In particular, maps of methanol emission at 338.4 GHz (J = 7(0)-6(0) A(+)) in low-mass clusters illustrate that this transition is an excellent probe of the low-mass population. We present here a model of a forming cluster where methanol emission is assigned to every embedded low-mass protostar. The resulting model image of methanol emission is compared to recent ALMA observations toward a high-mass cluster and the similarity is striking: the toy model reproduces observations to better than a factor of two and suggests that approximately 50% of the total flux originates in low-mass outflows. Future fine-tuning of the model will eventually make it a tool for interpreting the embedded low-mass population of distant regions within our own Galaxy and ultimately higher-redshift starburst galaxies, not just for methanol emission but also water and high-J CO. C1 [Kristensen, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Kristensen, LE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lkristensen@cfa.harvard.edu RI Kristensen, Lars E/F-4774-2011 OI Kristensen, Lars E/0000-0003-1159-3721 NR 30 TC 0 Z9 0 U1 0 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 JUL 10 PY 2015 VL 807 IS 2 AR L25 DI 10.1088/2041-8205/807/2/L25 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8HC UT WOS:000357938600005 ER PT J AU Thyagarajan, N Jacobs, DC Bowman, JD Barry, N Beardsley, AP Bernardi, G Briggs, F Cappallo, RJ Carroll, P Deshpande, AA de Oliveira-Costa, A Dillon, JS Ewall-Wice, A Feng, L Greenhill, LJ Hazelton, BJ Hernquist, L Hewitt, JN Hurley-Walker, N Johnston-Hollitt, M Kaplan, DL Kim, HS Kittiwisit, P Lenc, E Line, J Loeb, A Lonsdale, CJ McKinley, B McWhirter, SR Mitchell, DA Morales, MF Morgan, E Neben, AR Oberoi, D Offringa, AR Ord, SM Paul, S Pindor, B Pober, JC Prabu, T Procopio, P Riding, J Shankar, NU Sethi, SK Srivani, KS Subrahmanyan, R Sullivan, IS Tegmark, M Tingay, SJ Trott, CM Wayth, RB Webster, RL Williams, A Williams, CL Wyithe, JSB AF Thyagarajan, Nithyanandan Jacobs, Daniel C. Bowman, Judd D. Barry, N. Beardsley, A. P. Bernardi, G. Briggs, F. Cappallo, R. J. Carroll, P. Deshpande, A. A. de Oliveira-Costa, A. Dillon, Joshua S. Ewall-Wice, A. Feng, L. Greenhill, L. J. Hazelton, B. J. Hernquist, L. Hewitt, J. N. Hurley-Walker, N. Johnston-Hollitt, M. Kaplan, D. L. Kim, Han-Seek Kittiwisit, P. Lenc, E. Line, J. Loeb, A. Lonsdale, C. J. McKinley, B. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Neben, A. R. Oberoi, D. Offringa, A. R. Ord, S. M. Paul, Sourabh Pindor, B. Pober, J. C. Prabu, T. Procopio, P. Riding, J. Shankar, N. Udaya Sethi, Shiv K. Srivani, K. S. Subrahmanyan, R. Sullivan, I. S. Tegmark, M. Tingay, S. J. Trott, C. M. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. Wyithe, J. S. B. TI CONFIRMATION OF WIDE-FIELD SIGNATURES IN REDSHIFTED 21 cm POWER SPECTRA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; dark ages, reionization, first stars; large-scale structure of universe; methods: statistical; radio continuum: galaxies; techniques: interferometric ID MURCHISON WIDEFIELD ARRAY; CENTIMETER FLUCTUATIONS; INTERGALACTIC MEDIUM; DARK-AGES; 150 MHZ; REIONIZATION; EPOCH; FOREGROUNDS; EMISSION; 21-CM AB We confirm our recent prediction of the "pitchfork" foreground signature in power spectra of high-redshift 21 cm measurements where the interferometer is sensitive to large-scale structure on all baselines. This is due to the inherent response of a wide-field instrument and is characterized by enhanced power from foreground emission in Fourier modes adjacent to those considered to be the most sensitive to the cosmological H I signal. In our recent paper, many signatures from the simulation that predicted this feature were validated against Murchison Widefield Array (MWA) data, but this key pitchfork signature was close to the noise level. In this paper, we improve the data sensitivity through the coherent averaging of 12 independent snapshots with identical instrument settings and provide the first confirmation of the prediction with a signal-to-noise ratio > 10. This wide-field effect can be mitigated by careful antenna designs that suppress sensitivity near the horizon. Simple models for antenna apertures that have been proposed for future instruments such as the Hydrogen Epoch of Reionization Array and the Square Kilometre Array indicate they should suppress foreground leakage from the pitchfork by similar to 40 dB relative to the MWA and significantly increase the likelihood of cosmological signal detection in these critical Fourier modes in the three-dimensional power spectrum. C1 [Thyagarajan, Nithyanandan; Jacobs, Daniel C.; Bowman, Judd D.; Kittiwisit, P.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Barry, N.; Beardsley, A. P.; Carroll, P.; Hazelton, B. J.; Morales, M. F.; Pober, J. C.; Sullivan, I. S.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.; Greenhill, L. J.; Hernquist, L.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Briggs, F.; Offringa, A. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Paul, Sourabh; Prabu, T.; Shankar, N. Udaya; Sethi, Shiv K.; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [de Oliveira-Costa, A.; Dillon, Joshua S.; Ewall-Wice, A.; Feng, L.; Hewitt, J. N.; Morgan, E.; Neben, A. R.; Tegmark, M.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hurley-Walker, N.; Ord, S. M.; Tingay, S. J.; Trott, C. M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Kim, Han-Seek; Line, J.; McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Lenc, E.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Mitchell, D. A.] CASS, Epping, NSW 1710, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. RP Thyagarajan, N (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM t_nithyanandan@asu.edu RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Udayashankar , N/D-4901-2012; Hurley-Walker, Natasha/B-9520-2013; Sethi, Shiv/D-4893-2012; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; OI Jacobs, Daniel/0000-0002-0917-2269; Thyagarajan, Nithyanandan/0000-0003-1602-7868; Lenc, Emil/0000-0002-9994-1593; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; M, Manjunath/0000-0001-8710-0730; Wyithe, Stuart/0000-0001-7956-9758; KIM, HANSIK/0000-0002-5507-5769; /0000-0002-0086-7363 FU U.S. National Science Foundation (NSF) [AST-1109257]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1401708]; NSF Astronomy and Astrophysics Fellowship [AST-1302774]; NSF [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (via New Zealand Ministry of Economic Development and an IBM Shared University Research Grant) [MED-E1799]; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia - Western Australian State government FX This work was supported by the U.S. National Science Foundation (NSF) through award AST-1109257. D.C.J. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1401708. J.C.P. is supported by an NSF Astronomy and Astrophysics Fellowship under award AST-1302774. This 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 MWA comes from the NSF (awards: AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 50 TC 19 Z9 19 U1 0 U2 5 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 JUL 10 PY 2015 VL 807 IS 2 AR L28 DI 10.1088/2041-8205/807/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8HC UT WOS:000357938600008 ER PT J AU Trakhtenbrot, B Urry, CM Civano, F Rosario, DJ Elvis, M Schawinski, K Suh, H Bongiorno, A Simmons, BD AF Trakhtenbrot, Benny Urry, C. Megan Civano, Francesca Rosario, David J. Elvis, Martin Schawinski, Kevin Suh, Hyewon Bongiorno, Angela Simmons, Brooke D. TI An over-massive black hole in a typical star-forming galaxy, 2 billion years after the Big Bang SO SCIENCE LA English DT Article ID ACTIVE GALACTIC NUCLEI; HOST GALAXIES; HIGH-REDSHIFT; COSMIC EVOLUTION; STELLAR MASS; GROWTH-RATE; NGC 1277; COEVOLUTION; FIELD; M87 AB Supermassive black holes (SMBHs) and their host galaxies are generally thought to coevolve, so that the SMBH achieves up to about 0.2 to 0.5% of the host galaxy mass in the present day. The radiation emitted from the growing SMBH is expected to affect star formation throughout the host galaxy. The relevance of this scenario at early cosmic epochs is not yet established. We present spectroscopic observations of a galaxy at redshift z = 3.328, which hosts an actively accreting, extremely massive BH, in its final stages of growth. The SMBH mass is roughly one-tenth the mass of the entire host galaxy, suggesting that it has grown much more efficiently than the host, contrary to models of synchronized coevolution. The host galaxy is forming stars at an intense rate, despite the presence of a SMBH-driven gas outflow. C1 [Trakhtenbrot, Benny; Schawinski, Kevin] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Urry, C. Megan; Civano, Francesca] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Urry, C. Megan] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Civano, Francesca; Elvis, Martin; Suh, Hyewon] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosario, David J.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Suh, Hyewon] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Bongiorno, Angela] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Simmons, Brooke D.] Oxford Astrophys, Oxford OX1 3RH, England. RP Trakhtenbrot, B (reprint author), ETH, Inst Astron, Dept Phys, Wolfgang Pauli Str 27, CH-8093 Zurich, Switzerland. EM benny.trakhtenbrot@phys.ethz.ch OI Bongiorno, Angela/0000-0002-0101-6624; Schawinski, Kevin/0000-0001-5464-0888; Simmons, Brooke/0000-0001-5882-3323; Urry, Meg/0000-0002-0745-9792 FU W. M. Keck Foundation; European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO program [179.A-2005]; Swiss National Science Foundation [PP00P2 138979/1]; NASA [GO3-14150C]; NASA Chandra [GO2-13127X] FX The new MOSFIRE 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. We thank M. Kassis and the rest of the staff at the W. M. Keck observatories at Waimea, HI, for their support during the observing run. We 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. Some of the analysis presented here is based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO program ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. We are grateful to A. Faisst and M. Onodera for their assistance with the acquisition and reduction of the MOSFIRE data. We thank S. Tacchella, J. Woo, and W. Hartley for their assistance with some of the evolutionary calculations. K.S. gratefully acknowledges support from Swiss National Science Foundation Professorship grant PP00P2 138979/1. F.C. acknowledges financial support by the NASA grant GO3-14150C. M.E. acknowledges financial support by the NASA Chandra grant GO2-13127X. B.T. is a Zwicky Fellow at the ETH Zurich. NR 29 TC 16 Z9 16 U1 0 U2 7 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 JUL 10 PY 2015 VL 349 IS 6244 BP 168 EP 171 DI 10.1126/science.aaa4506 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CM4OM UT WOS:000357664300038 PM 26160942 ER PT J AU Alles, A Buchert, T Al Roumi, F Wiegand, A AF Alles, Alexandre Buchert, Thomas Al Roumi, Fosca Wiegand, Alexander TI Lagrangian theory of structure formation in relativistic cosmology. III. Gravitoelectric perturbation and solution schemes at any order SO PHYSICAL REVIEW D LA English DT Article ID FRIEDMAN-LEMAITRE COSMOLOGIES; NON-LINEAR THEORY; GRAVITATIONAL-INSTABILITY; ZELDOVICH APPROXIMATION; EXPANDING UNIVERSE; NEWTONIAN COSMOLOGY; GENERAL-RELATIVITY; PANCAKE THEORY; WEYL TENSOR; DYNAMICS AB The relativistic generalization of the Newtonian Lagrangian perturbation theory is investigated. In previous works, the first-order trace solutions that are generated by the spatially projected gravitoelectric part of the Weyl tensor were given together with extensions and applications for accessing the nonperturbative regime. We furnish here construction rules to obtain from Newtonian solutions the gravitoelectric class of relativistic solutions, for which we give the complete perturbation and solution schemes at any order of the perturbations. By construction, these schemes generalize the complete hierarchy of solutions of the Newtonian Lagrangian perturbation theory. C1 [Alles, Alexandre; Buchert, Thomas; Al Roumi, Fosca] Univ Lyon 1, CNRS, Ctr Rech Astrophys Lyon, Observ Lyon,UMR 5574, F-69230 St Genis Laval, France. [Alles, Alexandre; Buchert, Thomas; Al Roumi, Fosca] Ecole Normale Super Lyon, F-69230 St Genis Laval, France. [Wiegand, Alexander] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. [Wiegand, Alexander] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Alles, A (reprint author), Univ Lyon 1, CNRS, Ctr Rech Astrophys Lyon, Observ Lyon,UMR 5574, 9 Ave Charles Andre, F-69230 St Genis Laval, France. EM alexandre.alles@ens-lyon.fr; buchert@ens-lyon.fr; fosca.al_roumi@ens-lyon.fr; jwiegand@cfa.harvard.edu OI Buchert, Thomas/0000-0002-0828-3901 FU Lyon Institute of Origins [ANR-10-LABX-66]; Ecole Doctorale Lyon; French-Bavarian Cooperation Center; BFHZ Munich; DFG [WI 4501/1-1] FX The work of A. A., T. B., and F. R. was conducted within the "Lyon Institute of Origins" under Grant No. ANR-10-LABX-66. A. A. and F. R. acknowledge support by the Ecole Doctorale Lyon. T. B. and F. R. acknowledge student exchange support from the French-Bavarian Cooperation Center, BFHZ Munich http://www.bayern-france.org/. A. W. acknowledges the hospitality of the Harvard CfA where part of this work was done. Part of the work of A. W. was supported by the German research organization DFG, Grant No. WI 4501/1-1. Special thanks go to Leo Brunswic, Martin Kerscher, Mikolaj Korzynski, Pierre Mourier, Slava Mukhanov, Jan Ostrowski, Cornelius Rampf, Herbert Wagner, and the referee for fruitful discussions and valuable remarks. NR 46 TC 6 Z9 6 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD JUL 9 PY 2015 VL 92 IS 2 AR 023512 DI 10.1103/PhysRevD.92.023512 PG 18 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CM4FF UT WOS:000357639100003 ER PT J AU Baldeck, CA Asner, GP Martin, RE Anderson, CB Knapp, DE Kellner, JR Wright, SJ AF Baldeck, Claire A. Asner, Gregory P. Martin, Robin E. Anderson, Christopher B. Knapp, David E. Kellner, James R. Wright, S. Joseph TI Operational Tree Species Mapping in a Diverse Tropical Forest with Airborne Imaging Spectroscopy SO PLOS ONE LA English DT Article ID VECTOR DOMAIN DESCRIPTION; REMOTE-SENSING IMAGES; HYPERSPECTRAL DATA; LIDAR DATA; AERIAL-PHOTOGRAPHY; CLASSIFICATION; DISCRIMINATION; IDENTIFICATION; LEAF; BIODIVERSITY AB Remote identification and mapping of canopy tree species can contribute valuable information towards our understanding of ecosystem biodiversity and function over large spatial scales. However, the extreme challenges posed by highly diverse, closed-canopy tropical forests have prevented automated remote species mapping of non-flowering tree crowns in these ecosystems. We set out to identify individuals of three focal canopy tree species amongst a diverse background of tree and liana species on Barro Colorado Island, Panama, using airborne imaging spectroscopy data. First, we compared two leading singleclass classification methods-binary support vector machine (SVM) and biased SVM-for their performance in identifying pixels of a single focal species. From this comparison we determined that biased SVM was more precise and created a multi-species classification model by combining the three biased SVM models. This model was applied to the imagery to identify pixels belonging to the three focal species and the prediction results were then processed to create a map of focal species crown objects. Crown-level cross-validation of the training data indicated that the multi-species classification model had pixel-level producer's accuracies of 94-97% for the three focal species, and field validation of the predicted crown objects indicated that these had user's accuracies of 94-100%. Our results demonstrate the ability of high spatial and spectral resolution remote sensing to accurately detect non-flowering crowns of focal species within a diverse tropical forest. We attribute the success of our model to recent classification and mapping techniques adapted to species detection in diverse closed-canopy forests, which can pave the way for remote species mapping in a wider variety of ecosystems. C1 [Baldeck, Claire A.; Asner, Gregory P.; Martin, Robin E.; Anderson, Christopher B.; Knapp, David E.] Carnegie Inst Sci, Dept Plant Biol, Dept Global Ecol, Stanford, CA 94305 USA. [Kellner, James R.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Washington, DC USA. RP Baldeck, CA (reprint author), Carnegie Inst Sci, Dept Plant Biol, Dept Global Ecol, 290 Panama St, Stanford, CA 94305 USA. EM cbaldeck@carnegiescience.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Avatar Alliance Foundation; Gordon and Betty Moore Foundation; John D. and Catherine R. MacArthur Foundation; Grantham Foundation for the Protection of the Environment; W. M. Keck Foundation; Margaret A. Cargill Foundation FX This study has been supported by the Avatar Alliance Foundation, Gordon and Betty Moore Foundation, John D. and Catherine R. MacArthur Foundation, Grantham Foundation for the Protection of the Environment, W. M. Keck Foundation, Margaret A. Cargill Foundation, Mary Anne Nyburg Baker and G. Leonard Baker Jr., and William R. Hearst III. There are no grant numbers or URLs. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 58 TC 8 Z9 8 U1 10 U2 40 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 JUL 8 PY 2015 VL 10 IS 7 AR e0118403 DI 10.1371/journal.pone.0118403 PG 21 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1EJ UT WOS:000358159700001 PM 26153693 ER PT J AU Todaro, MA Dal Zotto, M Leasi, F AF Todaro, M. Antonio Dal Zotto, Matteo Leasi, Francesca TI An Integrated Morphological and Molecular Approach to the Description and Systematisation of a Novel Genus and Species of Macrodasyida (Gastrotricha) SO PLOS ONE LA English DT Article ID ITALIAN MARINE GASTROTRICHA; RIBOSOMAL-RNA GENES; NERVOUS-SYSTEM; PAUCITUBULATINA GASTROTRICHA; DACTYLOPODOLA-BALTICA; MEDITERRANEAN SEA; MUSCULAR SYSTEM; CHAETONOTIDA; PHYLOGENY; FRESH AB Background Gastrotricha systematics is in a state of flux mainly due to the conflicts between cladistic studies base on molecular markers and the classical systematisation based on morphological traits. In sandy samples from Thailand, we found numerous macrodasyidan gastrotrichs belonging to an undescribed species of difficult taxonomic affiliation. The abundance and original nature of the specimens prompted us to undertake a deep survey of both morphological and molecular traits aiming at a reliable systematisation of the new taxon. Methodology/Principal Findings Using several microscopical techniques we investigated the external and internal anatomy, including the muscular and nervous systems of the new species. Additional specimens were used to obtain the 18S rRNA gene sequence; molecular data was analysed cladistically in conjunction with data from additional species belonging to the near complete Macrodasyida taxonomic spectrum. Specimens are vermiform, up to 806 mu m in total length, and show a well-defined head equipped with peculiar leaf-like sensorial organs and a single-lobed posterior end. The adhesive apparatus includes anterior, ventrolateral, dorsal and posterior tubes. Pharynx is about 1/4 of the total length and shows pores at its posterior 3/4. Adult specimens exhibit maturing eggs and a bulky, muscular caudal organ, but do not show sperm nor the frontal organ. Musculature and nervous system organisation resemble the usual macrodasyidan plan; however, the somatic circular muscles of the intestinal region surround all other muscular components and a third FMRFamide-IR commissure ventral to the pharyngo-intestinal junction appear to be an autoapomorphic traits of the new species. Conclusions/Significance While the anatomical characteristics of the Asian specimens appear so unique to grant the establishment of a new taxon, for which the name Thaidasys tongiorgii gen. et sp. nov. is proposed, the result of phylogenetic analyses based on the 18S rRNA gene unites the new genus with the family Macrodasyidae. C1 [Todaro, M. Antonio; Dal Zotto, Matteo] Univ Modena & Reggio Emilia, Dept Life Sci, Modena, Italy. [Dal Zotto, Matteo] Consorzio Interuniv Ctr Biol Marina & Ecol Applic, Livorno, Italy. [Leasi, Francesca] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Todaro, MA (reprint author), Univ Modena & Reggio Emilia, Dept Life Sci, Modena, Italy. EM antonio.todaro@unimore.it RI LEASI, FRANCESCA/E-4361-2017 FU TIOME project (MAT, PI) FX Funding for this research was provided by the TIOME project (MAT, PI); the study falls within the framework of the strategic research line Environment, food and health (WP2) - of UNIMORE. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 4 Z9 5 U1 2 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 JUL 8 PY 2015 VL 10 IS 7 AR e0130278 DI 10.1371/journal.pone.0130278 PG 32 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1EJ UT WOS:000358159700027 PM 26153694 ER PT J AU Borregaard, J Komar, P Kessler, EM Lukin, MD Sorensen, AS AF Borregaard, J. Komar, P. Kessler, E. M. Lukin, M. D. Sorensen, A. S. TI Long-distance entanglement distribution using individual atoms in optical cavities SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM COMMUNICATION; NOISY CHANNELS; LINEAR OPTICS; CRYPTOGRAPHY; PURIFICATION; ENSEMBLES; REPEATERS; SECURITY; NETWORK; STATES AB Individual atoms in optical cavities can provide an efficient interface between stationary qubits and flying qubits (photons), which is an essential building block for quantum communication. Furthermore, cavity-assisted controlled-not (CNOT) gates can be used for swapping entanglement to long distances in a quantum repeater setup. Nonetheless, dissipation introduced by the cavity during the CNOT may increase the experimental difficulty in obtaining long-distance entanglement distribution using these systems. We analyze and compare a number of cavity-based repeater schemes combining various entanglement generation schemes and cavity-assisted CNOT gates. We find that a scheme, where high-fidelity entanglement is first generated in a two-photon detection scheme and then swapped to long distances using a recently proposed heralded controlled-Z (CZ) gate, exhibits superior performance compared to the other schemes. The heralded gate moves the effect of dissipation from the fidelity to the success probability of the gate thereby enabling high-fidelity entanglement swapping. As a result, high-rate entanglement distribution can be achieved over long distances even for low cooperativities of the atom-cavity systems. This high-fidelity repeater is shown to outperform the other cavity-based schemes by up to two orders of magnitude in the rate for realistic parameters and large distances (1000 km). C1 [Borregaard, J.; Sorensen, A. S.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Borregaard, J.; Komar, P.; Kessler, E. M.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kessler, E. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Borregaard, J (reprint author), Univ Copenhagen, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen O, Denmark. RI Sorensen, Anders/L-1868-2013 OI Sorensen, Anders/0000-0003-1337-9163 FU Lundbeck Foundation; Carlsberg Foundation; NSF; CUA; DARPA; AFOSR MURI; ARL; European Research Council under the European Unions Seventh Framework Programme (FP) through SIQS [600645]; ERC Grant QIOS [306576] FX A.S. would like to thank Naomi H. Nickerson for helpful discussions. We gratefully acknowledge the support from the Lundbeck Foundation, the Carlsberg Foundation, NSF, CUA, DARPA, AFOSR MURI, and ARL. The research leading to these results has also received funding from the European Research Council under the European Unions Seventh Framework Programme (FP/2007-2003) through SIQS (Grant No. 600645) and ERC Grant QIOS (Grant No. 306576). NR 37 TC 3 Z9 3 U1 1 U2 19 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD JUL 8 PY 2015 VL 92 IS 1 AR 012307 DI 10.1103/PhysRevA.92.012307 PG 15 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA CM4DI UT WOS:000357634000003 ER PT J AU Aiello, BR Iriarte-Diaz, J Blob, RW Butcher, MT Carrano, MT Espinoza, NR Main, RP Ross, CF AF Aiello, B. R. Iriarte-Diaz, J. Blob, R. W. Butcher, M. T. Carrano, M. T. Espinoza, N. R. Main, R. P. Ross, C. F. TI Bone strain magnitude is correlated with bone strain rate in tetrapods: implications for models of mechanotransduction SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE bone mechanotransduction; bone fluid flow; bone strain; strain rate ID FLOW-INDUCED MECHANOTRANSDUCTION; SKELETAL STRUCTURAL ADAPTATIONS; MECHANICAL USAGE SATMU; REDEFINING WOLFF LAW; IN-VIVO STRAINS; MOTOR UNITS; TERRESTRIAL LOCOMOTION; CORTICAL BONE; PERICELLULAR MATRIX; PSEUDEMYS-CONCINNA AB Hypotheses suggest that structural integrity of vertebrate bones is maintained by controlling bone strain magnitude via adaptive modelling in response to mechanical stimuli. Increased tissue-level strain magnitude and rate have both been identified as potent stimuli leading to increased bone formation. Mechanotransduction models hypothesize that osteocytes sense bone deformation by detecting fluid flow-induced drag in the bone's lacunar-canalicular porosity. This model suggests that the osteocyte's intracellular response depends on fluid-flow rate, a product of bone strain rate and gradient, but does not provide a mechanism for detection of strain magnitude. Such a mechanism is necessary for bone modelling to adapt to loads, because strain magnitude is an important determinant of skeletal fracture. Using strain gauge data from the limb bones of amphibians, reptiles, birds and mammals, we identified strong correlations between strain rate and magnitude across clades employing diverse locomotor styles and degrees of rhythmicity. The breadth of our sample suggests that this pattern is likely to be a common feature of tetrapod bone loading. Moreover, finding that bone strain magnitude is encoded in strain rate at the tissue level is consistent with the hypothesis that it might be encoded in fluid-flow rate at the cellular level, facilitating bone adaptation via mechanotransduction. C1 [Aiello, B. R.; Ross, C. F.] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Iriarte-Diaz, J.] Univ Illinois, Dept Oral Biol, Chicago, IL 60612 USA. [Blob, R. W.; Espinoza, N. R.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Butcher, M. T.] Youngstown State Univ, Dept Biol Sci, Youngstown, OH 44555 USA. [Carrano, M. T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Main, R. P.] Purdue Univ, Coll Vet Med, Dept Basic Med Sci, W Lafayette, IN 47907 USA. [Main, R. P.] Purdue Univ, Weldon Sch Biomed Engn, W Lafayette, IN 47907 USA. RP Aiello, BR (reprint author), Univ Chicago, Dept Organismal Biol & Anat, 1025 E 57Th St, Chicago, IL 60637 USA. EM braiello@uchicago.edu; rossc@uchicago.edu RI Carrano, Matthew/C-7601-2011; Iriarte-Diaz, Jose/A-2486-2008 OI Carrano, Matthew/0000-0003-2129-1612; Iriarte-Diaz, Jose/0000-0003-3566-247X FU National Science Foundation [DGE-0903637, IOB-0517340, BCS-010913] FX This material is based on work supported by the National Science Foundation under grants DGE-0903637 (an Integrative Graduate Education and Research Traineeship supporting B.R.A), IOB-0517340 (to R.W.B.) and BCS-010913 (to C.F.R.). NR 76 TC 1 Z9 1 U1 2 U2 9 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 JUL 7 PY 2015 VL 282 IS 1810 AR 20150321 DI 10.1098/rspb.2015.0321 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CM5HY UT WOS:000357719500009 ER PT J AU de Silva, P Miranda, R Bernal, XE AF de Silva, Priyanka Miranda, Roberto Bernal, Ximena E. TI First report of mite parasitization in frog-biting midges (Corethrella species) SO INTERNATIONAL JOURNAL OF ACAROLOGY LA English DT Article DE frog-biting midges; Corethrellidae; Hydrachnidae; mite parasitism ID LARVAL WATER MITES; MATING SUCCESS; ACARINE PARASITES; SEX BIASES; ARRENURUS; DIPTERA; MOSQUITOS; CULICIDAE; ODONATA; ECTOPARASITISM AB Water mites (Acari: Hydrachnidiae) were collected from males of frog-biting midges (Corethrellidae) in Gamboa, Panama. All Corethrella squamifemora males collected were parasitized with water mites. The mites were attached to the soft tissues of the thoracic region of the midges. No mites were found on female frog-biting midges of the same species. This study is the first report of mite parasitization in frog-biting midges. C1 [de Silva, Priyanka] Univ Peradeniya, Fac Sci, Dept Zool, Peradeniya, Sri Lanka. [Miranda, Roberto] Inst Conmemorat Gorgas Estudios Salud, Entomol Med, Calidonia Panama, Panama. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Bernal, Ximena E.] Smithsonian Trop Res Inst, Balboa, Panama. RP de Silva, P (reprint author), Univ Peradeniya, Fac Sci, Dept Zool, Peradeniya, Sri Lanka. EM depriyanka@pdn.ac.lk; mirandarjc@gmail.com; xbernal@purdue.edu FU National Science Foundation, Directorate for Biological Sciences [1433990] FX This work was supported by the National Science Foundation, Directorate for Biological Sciences [IOS#1433990]. NR 36 TC 0 Z9 0 U1 1 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 530 WALNUT STREET, STE 850, PHILADELPHIA, PA 19106 USA SN 0164-7954 EI 1945-3892 J9 INT J ACAROL JI Int. J. Acarol. PD JUL 4 PY 2015 VL 41 IS 5 BP 389 EP 392 DI 10.1080/01647954.2015.1046922 PG 4 WC Entomology SC Entomology GA CP2KE UT WOS:000359705100003 ER PT J AU Wegner, G Onofrio, R AF Wegner, Gary A. Onofrio, Roberto TI Higgs shifts from electron-positron annihilations near neutron stars SO EUROPEAN PHYSICAL JOURNAL C LA English DT Article ID GAMMA-RAY BURSTS; KONUS EXPERIMENT DATA; HIGH-RESOLUTION SPECTROSCOPY; GALACTIC-CENTER REGION; RADIATION; CYCLOTRON; MODEL; MASS; SPECTRUM; FEATURES AB We discuss the potential for using neutron stars to determine bounds on the Higgs-Kretschmann coupling by looking at peculiar shifts in gamma-ray spectroscopic features. In particular, we reanalyze multiple lines observed in GRB781119 detected by two gamma-ray spectrometers, and derive an upper bound on the Higgs-Kretschmann coupling that is much more constraining than the one recently obtained from white dwarfs. This calls for targeted analyses of spectra of gamma-ray bursts from more recent observatories, dedicated searches for differential shifts on electron-positron and proton-antiproton annihilation spectra in proximity of compact sources, and signals of electron and proton cyclotron lines from the same neutron star. C1 [Wegner, Gary A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Wegner, G (reprint author), Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. EM gary.a.wegner@dartmouth.edu; onofrior@gmail.com FU SCOAP3 FX Funded by SCOAP3. NR 74 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1434-6044 EI 1434-6052 J9 EUR PHYS J C JI Eur. Phys. J. C PD JUL 4 PY 2015 VL 75 IS 7 AR 307 DI 10.1140/epjc/s10052-015-3523-5 PG 7 WC Physics, Particles & Fields SC Physics GA CM1ZT UT WOS:000357479900001 ER PT J AU Opresko, DM AF Opresko, D. M. TI New species of black corals (Cnidaria: Anthozoa: Antipatharia) from New Zealand and adjacent regions SO NEW ZEALAND JOURNAL OF ZOOLOGY LA English DT Article DE Antipathidae; Aphanipathidae; black corals; new species; New Zealand; Schizopathidae; taxonomy ID SOUTHERN FJORDS; POPULATION-STRUCTURE; FIORDENSIS AB Seven new species of antipatharian corals are described from the territorial waters of New Zealand and adjacent regions. Differential diagnoses are given and comparisons are made to related nominal species. Described as new are: Antipathes leptocrada; Antipathes craticulata; Asteriopathes octocrada; Phanopathes zealandica; Tetrapathes latispina; Parantipathes dodecasticha; and Parantipathes robusta.http://zoobank.org/urn:lsid:zoobank.org:pub:DCF9A2BD-63DE-4240-AA4E-0B8BE7E095F1 C1 [Opresko, D. M.] Smithsonian Inst, Dept Invertebrate Zool, US Natl Museum Nat Hist, Washington, DC 20560 USA. RP Opresko, DM (reprint author), Smithsonian Inst, Dept Invertebrate Zool, US Natl Museum Nat Hist, Washington, DC 20560 USA. EM dmopresko@hotmail.com FU New Zealand Foundation for Research, Science and Technology; Ministry of Fisheries; NOAA Satellite Operations Facility; United States Department of Justice (DoJ); DoJ FX Samples from cruises KAH0011, TAN0205 and TAN0413 were supplied by the NIWA Invertebrate Collection and were collected as part of a research programme 'Seamounts: their importance to fisheries and marine ecosystems', undertaken by the NIWA and funded by the former New Zealand Foundation for Research, Science and Technology and with additional funding from the Ministry of Fisheries and NOAA Satellite Operations Facility.; The author also wishes to thank S Cairns, W Keel, C Bright, W Moser and P Greenhall for their assistance during visits to the USNMNH. The photomicrographs were prepared in the SEM Laboratory of the USNMNH; SD Whittaker of the USNMNH kindly assisted in the SEM operation. DM Opresko is a Research Associate of the USNMNH, and gratefully acknowledges that affiliation. Funding for this project was provided, in part, by a United States Department of Justice (DoJ) grant to the Smithsonian Institution. The author is very appreciative of the DoJ's support of black coral research at the Smithsonian. Sincere thanks also go to T Molodtsova and M Bo for reviewing the manuscript and providing many useful comments and suggestions, and to Jonathan Banks and Marie Hodgkinson for their editorial assistance. Permission to use the photo of Antipathes densa (see Fig. 3A) was kindly provided by Nikoletta Helidonis of Bayerischen Akademie der Wissenschaften. NR 31 TC 0 Z9 0 U1 2 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0301-4223 EI 1175-8821 J9 NEW ZEAL J ZOOL JI N. Z. J. Zool. PD JUL 3 PY 2015 VL 42 IS 3 BP 145 EP 164 DI 10.1080/03014223.2015.1051550 PG 20 WC Zoology SC Zoology GA CX3OI UT WOS:000365608200002 ER PT J AU Deutsch, JI AF Deutsch, James I. TI Stanley Kubrick: new perspectives SO HISTORICAL JOURNAL OF FILM RADIO AND TELEVISION 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. EM deutschj@si.edu NR 1 TC 0 Z9 0 U1 1 U2 2 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0143-9685 EI 1465-3451 J9 HIST J FILM RADIO TV JI Hist. J. Film Radio Telev. PD JUL 3 PY 2015 VL 35 IS 3 BP 518 EP 519 DI 10.1080/01439685.2015.1059611 PG 2 WC Film, Radio, Television SC Film, Radio & Television GA CP2IA UT WOS:000359699500009 ER PT J AU Egan, AN Pan, B AF Egan, Ashley N. Pan, Bo TI Resolution of polyphyly in Pueraria (Leguminosae, Papilionoideae): The creation of two new genera, Haymondia and Toxicopueraria, the resurrection of Neustanthus, and a new combination in Teyleria SO PHYTOTAXA LA English DT Article DE classification; Fabaceae; Glycininae; Phaseoleae; taxonomy AB Recent molecular phylogenetic studies (Egan et al., in prep.) have demonstrated widespread polyphyly within the genus Pueraria. A new classification is presented here that delineates monophyletic groups previously considered congeneric with Pueraria. This taxonomic treatment provides several new species combinations and a more natural circumscription of Pueraria by reinstating the genus Neustanthus, transferring one species to Teyleria and establishing two new genera: Haymondia and Toxicopueraria. C1 [Egan, Ashley N.] Smithsonian Inst NMNH, Dept Bot, US Natl Herbarium US, Washington, DC 20560 USA. [Pan, Bo] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Ctr Integrat Conservat, Mengla 666303, Yunnan, Peoples R China. RP Egan, AN (reprint author), Smithsonian Inst NMNH, Dept Bot, US Natl Herbarium US, MRC 166,10th & Constitut Ave, Washington, DC 20560 USA. EM egana@si.edu FU East Carolina University; Smithsonian Institution; National Science Foundation (NSF) [DEB 1120186/1352217]; Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts [WQ20110491035] FX A.N. Egan thanks the staff and affiliates of the Forest Herbarium, the Royal Thai Forest Department, and the Flora of Thailand Project for help and support in field collection efforts and herbarium access and specimen loans, especially Kongkanda Chayamarit, Rachun Pooma, Sukontip Sirimongkol, Thaveechok Jumruschay, Voradol Chamchumroon, Nannapat Pattharahirantricin, and Rumrada Meeboonya, in no particular order, as well as Xin-Fen Gao and Bo Xu from Chengdu Institute of Biology for aid in field collections in China. Bo Pan thanks Jian-Tao Yin, Shi-Shun Zhou, Yun-Hong Tan, Qiang Liu, Hong Wang, Han Lai, Li Wang from Xishuangbanna Botanical Garden, Jing-Hua Wang from Herbarium of Kunming Institute of Botany, Si-Rong Yi from Chongqing Institute of Medicinal Plants, and Li He from Beijing Forestry University for their support in both herbarium and field work. Illustrations were beautifully provided by Alice Tangerini of the U.S. National Herbarium, Smithsonian Institution. Thanks to Christopher Puttock, a research associate at the Smithsonian Institution, Sue Sherman-Broyles of Cornell University, and Ruth P. Clark of Royal Botanic Gardens, Kew for helpful comments on the manuscript. A.N. Egan was supported in part by funding from East Carolina University, Smithsonian Institution, and the National Science Foundation (NSF DEB 1120186/1352217). Bo Pan was funded by Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts (WQ20110491035). NR 0 TC 1 Z9 1 U1 0 U2 1 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 JUL 3 PY 2015 VL 218 IS 3 BP 201 EP 226 PG 26 WC Plant Sciences SC Plant Sciences GA CO2YA UT WOS:000359021900001 ER PT J AU Egan, AN Pan, B AF Egan, Ashley N. Pan, Bo TI Pueraria stracheyi, a new synonym to Apios carnea (Fabaceae) SO PHYTOTAXA LA English DT Article DE Leguminosae; taxonomy; India; Sir Richard Strachey; Shuteria AB Pueraria stracheyi has long been recognized as erroneously placed in the genus Pueraria. Here we examined the history behind this collection, past hypotheses concerning its taxonomic affinities, and morphological and ecological comparisons with Shuteria and Apios carnea, wherein we conclude that Pueraria stracheyi represents a synonym of the latter. C1 [Egan, Ashley N.] Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, Washington, DC 20560 USA. [Pan, Bo] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Ctr Integrat Conservat, Mengla 666303, Yunnan, Peoples R China. RP Egan, AN (reprint author), Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, MRC 166,10th & Constitut Ave, Washington, DC 20560 USA. EM egana@si.edu FU East Carolina University; Smithsonian Institution; National Science Foundation [NSF DEB 1120186/1352217]; Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts [WQ20110491035] FX The authors thank the curators and staff of herbaria E, K, and US for access to facilities and collections. A.N. Egan was supported in part by funding from East Carolina University, Smithsonian Institution, and the National Science Foundation (NSF DEB 1120186/1352217). Bo Pan was funded by Xishuangbanna Tropical Botanical Garden through the Recruitment Program of Foreign Experts (WQ20110491035). NR 23 TC 1 Z9 1 U1 0 U2 1 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 JUL 2 PY 2015 VL 218 IS 2 BP 147 EP 155 DI 10.11646/phytotaxa.218.2.4 PG 9 WC Plant Sciences SC Plant Sciences GA CM7EI UT WOS:000357852800004 ER PT J AU Skog, LE Clark, JL AF Skog, Laurence E. Clark, John L. TI NOVAE GESNERIACEAE NEOTROPICARUM XIX: A third, new species of the elusive Anetanthus found in Guyana SO PHYTOTAXA LA English DT Article DE Biodiversity; Classification; Guyana; Taxonomy AB A new species of Anetanthus (Gesneriaceae) is described from Guyana as A. disjuncta. A discussion of the known species is provided as well as a key to the known taxa. C1 [Skog, Laurence E.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Clark, John L.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. RP Skog, LE (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA. EM skogl@si.edu; jlc@ua.edu FU National Science Foundation [DEB-841958, DEB-0949169] FX This study was supported by funds from the National Science Foundation (DEB-841958 and DEB-0949169). We are grateful to the Biological Diversity of the Guiana Shield Program (Smithsonian Institution's Department of Botany) and especially field collectors H. David Clarke and Terry Henkel for many years of exploratory collecting that resulted in discoveries such as the one published here. We also are grateful for the line drawings prepared by Alice Tangerini, staff illustrator in the Smithsonian Institution's Department of Botany. NR 14 TC 0 Z9 0 U1 0 U2 0 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 JUL 2 PY 2015 VL 218 IS 2 BP 177 EP 183 DI 10.11646/phytotaxa.218.2.8 PG 7 WC Plant Sciences SC Plant Sciences GA CM7EI UT WOS:000357852800008 ER PT J AU Zhang, WT Shih, CK Labandeira, CC Ren, D AF Zhang, Wei-Ting Shih, Chung-Kun Labandeira, Conrad C. Ren, Dong TI A new taxon of a primitive moth (Insecta: Lepidoptera: Eolepidopterigidae) from the latest Middle Jurassic of northeastern China SO JOURNAL OF PALEONTOLOGY LA English DT Article AB A new genus and species, Aclemus patulus n. gen. n. sp., is described based on a new specimen collected from the latest Middle Jurassic Jiulongshan Formation in Inner Mongolia, China. Based on a combination of characters from this fossil, including a homonomous fore-and hindwing, a 3-branched media vein, wings lacking long cilia on their margins; and a cross-vein absent between subcosta and radius, we establish a new genus assigned to the Eolepidopterigidae. In addition, the diagnosis of Longcapitalis excelsus Zhang, Shih, Labandeira and Ren 2013, is emended based on new fossil material. C1 [Zhang, Wei-Ting] Shijiazhuang Univ Econ, Geosci Museum, Shijiazhuang 050031, Peoples R China. [Zhang, Wei-Ting; Shih, Chung-Kun; Labandeira, Conrad C.; Ren, Dong] Capital Normal Univ, Key Lab Insect Evolut & Environm Changes, Beijing 100048, Peoples R China. [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. RP Zhang, WT (reprint author), Shijiazhuang Univ Econ, Geosci Museum, Shijiazhuang 050031, Peoples R China. EM zhangweitinghao@163.com; chungkun.shih@gmail.com; labandec@si.edu; rendong@mail.cnu.edu.cn FU National Basic Research Program of China (973 Program) [2012CB821906]; National Natural Science Foundation of China [31172143, 31230065, 31272352, 41272006, 41402009]; Project of the Great Wall Scholar and KEY project of the Beijing Municipal Commission of Education [KZ201310028033]; Natural Science Foundation of Hebei Province [D2015403010]; China Geological Survey [1212011120115]; PhD Research Startup Foundation of Shijiazhuang University of Economics [BQ201319] FX This research was supported by the National Basic Research Program of China (973 Program) (grant 2012CB821906), National Natural Science Foundation of China (grants 31172143, 31230065, 31272352, 41272006 and 41402009), Project of the Great Wall Scholar and KEY project of the Beijing Municipal Commission of Education (grant KZ201310028033), Natural Science Foundation of Hebei Province (grant D2015403010), China Geological Survey (grant 1212011120115), and the PhD Research Startup Foundation of Shijiazhuang University of Economics (No. BQ201319). This is contribution 264 of the Evolution of Terrestrial Ecosystems Consortium of the National Museum of Natural History, in Washington, D.C., U.S.A. NR 21 TC 1 Z9 1 U1 1 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 2015 VL 89 IS 4 BP 617 EP 621 DI 10.1017/jpa.2015.39 PG 5 WC Paleontology SC Paleontology GA DF5LL UT WOS:000371393100007 ER PT J AU Amaya-Marquez, M Skog, LE Kvist, LP AF Amaya-Marquez, Marisol Skog, Laurence E. Kvist, Lars Peter TI TWO NEW SPECIES AND TWO NEW VARIETIES OF COLUMNEA (GESNERIACEAE) SO CALDASIA LA English DT Article DE Columnea chocoensis; Columnea stilesiana; Columnea ericae; Gesneriaceae; Choco Biogeographical Region ID CLASSIFICATION AB In this paper two new species of Gesneriaceae (genus Columnea) are described and illustrated. Columnea chocoensis is distributed in the Colombian departments of Choco and Valle del Cauca, while its variety, C. chocoensis var. altaquerensis is restricted to the Department of Narino, Colombia. Columnea stilesiana was found in La Serrania de Los Paraguas located in the Cordillera Occidental between the Choco and Valle del Cauca Departments in Colombia. Further, Columnea archidonae is here considered a variety of C. ericae; Columnea ericae var. archidonae is distributed in Colombia and Ecuador, in forests at elevations higher than those in which the typical variety is found. C1 [Amaya-Marquez, Marisol] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, DC, Colombia. [Skog, Laurence E.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Kvist, Lars Peter] Univ Aarhus, Inst Biol Sci, DK-8000 Aarhus C, Denmark. RP Amaya-Marquez, M (reprint author), Univ Nacl Colombia, Inst Ciencias Nat, Apartado 7495, Bogota, DC, Colombia. EM mamayam@unal.edu.co; skogl@si.edu; lp@hels-gym.dk NR 7 TC 0 Z9 0 U1 1 U2 1 PU INST CIENCIAS NATURALES, MUSEO HISTORIA NATURAL PI BOGOTA PA FAC CIENCIAS, UNIV NACIONAL COLOMBIA, APARTADO 7495, BOGOTA, 00000, COLOMBIA SN 0366-5232 J9 CALDASIA JI Caldasia PD JUL-DEC PY 2015 VL 37 IS 2 BP 233 EP 250 PG 18 WC Plant Sciences; Multidisciplinary Sciences; Zoology SC Plant Sciences; Science & Technology - Other Topics; Zoology GA DB3SC UT WOS:000368430800001 ER PT J AU Furth, DG Savini, V Chaboo, CS AF Furth, David G. Savini, Vilma Chaboo, Caroline S. TI Beetles (Coleoptera) of Peru: A Survey of the Families. Chrysomelidae: Alticinae (Flea Beetles) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article C1 [Furth, David G.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Savini, Vilma] Cent Univ Venezuela, Muse Inst Zool Agr, Fac Agron, Maracay 2101A, Venezuela. [Chaboo, Caroline S.] Univ Kansas, Div Entomol, Biodivers Inst, Lawrence, KS 66045 USA. RP Chaboo, CS (reprint author), Univ Kansas, Div Entomol, Biodivers Inst, 1501 Crestline Dr,Suite 140, Lawrence, KS 66045 USA. EM cschaboo@ku.edu FU NSF-EPSCoR [66928]; University of Kansas Department of Ecology and Evolutionary Biology-General Research Fund FX We acknowledge NSF-EPSCoR #66928 (PI: CS Chaboo) for supporting the Peru beetle project and the University of Kansas Department of Ecology and Evolutionary Biology-General Research Fund (PI: CS Chaboo) for funding this publication. NR 24 TC 1 Z9 1 U1 0 U2 0 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 EI 1937-2353 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JUL PY 2015 VL 88 IS 3 BP 368 EP 374 PG 7 WC Entomology SC Entomology GA DA0QB UT WOS:000367501100008 ER PT J AU Chaboo, CS Staines, CL AF Chaboo, C. S. Staines, C. L. TI Beetles (Coleoptera) of Peru: A Survey of the Families. Chrysomelidae: Cassidinae Gyllenhal sensu lato SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article C1 [Chaboo, C. S.] Univ Kansas, Biodivers Inst, Div Entomol, Lawrence, KS 66045 USA. [Staines, C. L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Chaboo, CS (reprint author), Univ Kansas, Biodivers Inst, Div Entomol, 1501 Crestline Dr,Suite 140, Lawrence, KS 66045 USA. EM cschaboo@ku.edu FU NSF-EPSCoR [66928]; University of Kansas' Department of Ecology and Evolutionary Biology-General Research Fund FX We acknowledge NSF-EPSCoR #66928 (PI: CS Chaboo) for supporting the 'Beetles of Peru' project and the University of Kansas' Department of Ecology and Evolutionary Biology-General Research Fund (PI: CS Chaboo) for funding this publication. NR 17 TC 1 Z9 1 U1 0 U2 0 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 USA SN 0022-8567 EI 1937-2353 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD JUL PY 2015 VL 88 IS 3 BP 387 EP 398 PG 12 WC Entomology SC Entomology GA DA0QB UT WOS:000367501100012 ER PT J AU Salazar-Porzio, M AF Salazar-Porzio, Margaret TI The ecology of arts and humanities education: Bridging the worlds of universities and museums SO ARTS AND HUMANITIES IN HIGHER EDUCATION LA English DT Article DE Arts and humanities; experiential learning; higher education; mentorship; museums; partnerships; public history AB In recent years, colleges and universities have been talking seriously about civic learning, but other stakeholders, particularly public arts, culture, and humanities institutions, must be part of the conversation in order to create a context for learning that develops the skills of graduates in robust ways that reflect the full promise of liberal education. This piece places museums within the ecology of higher education through the experiences of faculty, curators, and students in one of the most museum-rich regions in the nation, Washington, DC. Students bridge the worlds of higher education and museums as research fellows, interns, and young professionals. Their experiences provide a window into thinking about the roles of faculty and curator mentors and the importance of finding the intersections between higher education and museums in the ecology of arts and humanities learning and practice. C1 [Salazar-Porzio, Margaret] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20013 USA. RP Salazar-Porzio, M (reprint author), Smithsonian Inst, 14th St,Constitution Ave,NW MRC 615,POB 37012, Washington, DC 20013 USA. EM salazar-porziom@si.edu NR 41 TC 0 Z9 0 U1 3 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1474-0222 EI 1741-265X J9 ARTS HUM HIGH EDUC JI Arts Hum. High. Educ. PD JUL PY 2015 VL 14 IS 3 SI SI BP 274 EP 292 DI 10.1177/1474022215583949 PG 19 WC Education & Educational Research SC Education & Educational Research GA CV3NZ UT WOS:000364167200004 ER PT J AU Coquillon, N Staples, J AF Coquillon, Naomi Staples, James TI Webcasting for Secondary Students: Notes from the Field SO JOURNAL OF MUSEUM EDUCATION LA English DT Article AB This article argues that webcasting holds great potential to connect students to museum content and to their peers while building content knowledge and skills. The authors outline the opportunities and challenges of webcasts for secondary students by discussing their experience with the National Museum of American History's National Youth Summit webcast series. C1 [Coquillon, Naomi] Smithsonians Natl Museum Amer Hist NMAH, Youth & Teacher Programs, Washington, DC 20001 USA. [Staples, James] Cent Audiovisual Branch, Smithsonian, DC USA. RP Coquillon, N (reprint author), Smithsonians Natl Museum Amer Hist NMAH, Youth & Teacher Programs, Washington, DC 20001 USA. NR 7 TC 0 Z9 0 U1 1 U2 2 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 1059-8650 EI 2051-6169 J9 J MUS EDUC JI J. Museum Education PD JUL PY 2015 VL 40 IS 2 BP 110 EP 118 PG 9 WC Education & Educational Research SC Education & Educational Research GA CU9YH UT WOS:000363902500004 ER PT J AU Smith, LF Smith, JK Arcand, KK Smith, RK Bookbinder, JA AF Smith, Lisa F. Smith, Jeffrey K. Arcand, Kimberly K. Smith, Randall K. Bookbinder, Jay A. TI Aesthetics and Astronomy: How Museum Labels Affect the Understanding and Appreciation of Deep-Space Images SO CURATOR-THE MUSEUM JOURNAL LA English DT Article ID SCIENCE MUSEUM; PERCEPTION; PAINTINGS AB How can we best communicate to museum visitors the science that underlies the incredible images of space that are generated through the data collected from satellites and observatories? The Aesthetics and Astronomy Group, a collection of astrophysicists, space image developers, science communication experts, and research psychologists, has studied how individuals respond to space-image descriptions when viewing images on websites such as the Astronomy Picture of the Day and the Chandra telescope site. In this article, we turn our attention to the communication of scientific information in museum settings, in particular where the exhibit is comprised solely of images. We developed a traveling exhibition of space images expressly for this purpose, and interviewed 167 visitors to the exhibition at four major science museums. We asked the visitors what types of labels they preferred, what they would like to see in labels, and what impressed them about the images. The results of our efforts are presented here. C1 [Smith, Lisa F.] Univ Otago, Coll Educ, Dunedin, New Zealand. [Smith, Jeffrey K.] Univ Otago, Dunedin, New Zealand. [Smith, Randall K.] Smithsonian Astrophys Observ, Div High Energy Astrophys, Cambridge, MA USA. [Bookbinder, Jay A.] Smithsonian Astrophys Observ, Div High Energy Astrophys, Cambridge, MA USA. RP Smith, LF (reprint author), Univ Otago, Coll Educ, Dunedin, New Zealand. EM lisa.smith@otago.ac.nz; jeffrey.smith@otago.ac.nz; kkowal@cfa.harvard.edu; rsmith@cfa.harvard.edu; jbookbinder@cfa.harvard.edu NR 21 TC 0 Z9 0 U1 2 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JUL PY 2015 VL 58 IS 3 BP 283 EP 297 DI 10.1111/cura.12114 PG 15 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6PV UT WOS:000363655600004 ER PT J AU Chan, S Cope, A AF Chan, Sebastian Cope, Aaron TI Strategies against Architecture: Interactive Media and Transformative Technology at the Cooper Hewitt, Smithsonian Design Museum SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB After being closed for three years, the Cooper Hewitt, Smithsonian Design Museum reopened at the end of 2014 a transformed museum in a renovated heritage building: Andrew Carnegie's former home on the Upper East Side of New York City. New galleries, a collection that was being rapidly digitized, a new brand, and a desire for new audiences drove the museum to rethink and reposition its role as a design museum. At the core of the new museum is a digital platform, built in-house, that connects collection-and patron-management systems to in-gallery and online experiences. These have allowed the museum to redesign everything from object labels and vitrines to the fundamentals of the "visitor experience." This paper explores in detail the process, the decisions made-and resulting tradeoffs-during each stage of the process. In so doing, it reveals the challenges of collaborating with internal and external capacities, operating internationally with online collaboration tools, and rapid prototyping. C1 [Chan, Sebastian] Smithsonian Design Museum, Cooper Hewitt, Digital & Emerging Media, New York, NY 10128 USA. [Cope, Aaron] Smithsonian Design Museum, Cooper Hewitt, New York, NY USA. RP Chan, S (reprint author), Smithsonian Design Museum, Cooper Hewitt, Digital & Emerging Media, New York, NY 10128 USA. EM seb@freshandnew.org; aaron@aaronland.net NR 33 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JUL PY 2015 VL 58 IS 3 BP 353 EP 368 DI 10.1111/cura.12118 PG 16 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6PV UT WOS:000363655600008 ER PT J AU Woodman, N AF Woodman, Neal TI Shippingport, Kentucky, is the type locality for the white-footed mouse, Peromyscus leucopus (Rafinesque, 1818) (Mammalia: Rodentia: Cricetidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Muroidea; Neotominae; systematics; taxonomy AB The white-footed mouse, Musculus leucopus Rafinesque, 1818 (= Peromyscus leucopus), is a common small mammal that is widespread in the eastern and central United States. Its abundance in many habitats renders it ecologically important, and its status as a reservoir for hantavirus and Lyme disease gives the species medical and economic significance. The recognition of two cytotypes and up to 17 morphological subspecies of P. leucopus indicates considerable variation in the species, and to understand this variation, it is important that the nominate subspecies be adequately defined so as to act as a standard for comparison. Relevant to this standard for the white-footed mouse is its type locality, which has generally been accepted to be either the vague "pine barrens of Kentucky'' or the mouth of the Ohio River. Newly assembled information regarding the life and travels of Constantine S. Rafinesque, the North American naturalist who described P. leucopus, establishes that Rafinesque observed this species in July 1818 while visiting Shippingport, Kentucky, which is now within the city limits of Louisville, Jefferson Co., Kentucky. Shippingport is therefore the actual type locality for this species. C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, MRC 111,POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 39 TC 1 Z9 1 U1 1 U2 7 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL PY 2015 VL 128 IS 2 BP 152 EP 163 DI 10.2988/0006-324X-128.2.152 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CS8VL UT WOS:000362367500003 ER PT J AU Shockley, FW Thomas, MC AF Shockley, Floyd W. Thomas, Michael C. TI Notes on the taxonomic identity of Trogosita pusillima Mannerheim, 1843, with transfer from Laemophloeidae and synonymy under Holoparamecus depressus Curtis, 1833 (Endomychidae: Merophysiinae) SO PAN-PACIFIC ENTOMOLOGIST LA English DT Editorial Material C1 [Shockley, Floyd W.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Thomas, Michael C.] Florida Dept Agr & Consumer Serv, Florida State Collect Arthropods, Div Plant Ind Entomol, Gainesville, FL 32614 USA. RP Shockley, FW (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, POB 37012,MRC 165, Washington, DC 20013 USA. EM ShockleyF@si.edu; Michael.Thomas@FreshFromFlorida.com NR 10 TC 0 Z9 0 U1 0 U2 0 PU PACIFIC COAST ENTOMOL SOC PI SAN FRANCISCO PA C/O CALIFORNIA ACADEMY SCIENCES, 875 HOWARD STREET, SAN FRANCISCO, CA 94103-3009 USA SN 0031-0603 EI 2162-0237 J9 PAN-PAC ENTOMOL JI Pan-Pacific Entomol. PD JUL PY 2015 VL 91 IS 3 BP 278 EP 280 PG 3 WC Entomology SC Entomology GA CS8AE UT WOS:000362307300006 ER PT J AU Richardson, DJ Moser, WE Hammond, CI Lazo-Wasem, EA AF Richardson, Dennis J. Moser, William E. Hammond, Charlotte I. Lazo-Wasem, Eric A. TI New Host and Geographic Distribution Records for Glossiphoniid Leeches Associated with Turtles in Southern New England SO COMPARATIVE PARASITOLOGY LA English DT Article DE Placobdella ali; Placobdella hollensis; Helobdella papillata; Helobdella modesta; Helobdella lineata; Chelydra serpentina; Sternotherus odoratus; common snapping turtle; stinkpot turtle; common musk turtle; Massachusetts; Rhode Island; Hirudinida; Hirudinea; Leech; Glossiphoniidae ID MITOCHONDRIAL GENE-SEQUENCES; HIRUDINIDA GLOSSIPHONIIDAE; MOLECULAR CHARACTERIZATION; HELOBDELLA-MODESTA; MORPHOLOGICAL DATA; PHYLOGENY AB During the summer of 2013, collection of glossiphoniid leeches from turtles in southern New England U.S.A. revealed several new host associations and geographic distribution records. Placobdella ali is reported for the first time from Massachusetts and Rhode Island. Placobdella hollensis is reported for the first time from mainland Rhode Island and for the first time from the common snapping turtle (Chelydra serpentina) and the stinkpot turtle or common musk turtle (Sternotherus odoratus). Helobdella papillata and Helobdella modesta were collected from common snapping turtles, and Helobdella lineata was collected from a stinkpot turtle. Data on the frequency of association of Helobdella spp. with aquatic vertebrates suggest that although Helobdella spp. are not parasitic, a symbiotic relationship likely exists between Helobdella spp. and their hosts, the nature of which is yet to be elucidated. C1 [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Dept Biol Sci, Hamden, CT 06518 USA. [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Richardson, DJ (reprint author), Quinnipiac Univ, Dept Biol Sci, 275 Mt Carmel Ave, Hamden, CT 06518 USA. EM Dennis.Richardson@quinnipiac.edu; moserw@si.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu NR 19 TC 1 Z9 1 U1 1 U2 5 PU HELMINTHOLOGICAL SOC WASHINGTON PI LAWRENCE PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS 66044 USA SN 1525-2647 EI 1938-2952 J9 COMP PARASITOL JI Comp. Parasitol. PD JUL PY 2015 VL 82 IS 2 BP 240 EP 243 PG 4 WC Parasitology; Zoology SC Parasitology; Zoology GA CR7VT UT WOS:000361560600010 ER PT J AU Condit, R AF Condit, Richard TI Extracting Environmental Benefits from a New Canal in Nicaragua: Lessons from Panama SO PLOS BIOLOGY LA English DT Article ID 21ST-CENTURY AB Biologists have raised objections to a new canal in Nicaragua, but in this Essay I argue that dire predictions of environmental catastrophe are exaggerated. I present an alternative view based on my research experience in Panama, where Canal operations foster forest conservation. Currently in Nicaragua, the rate of forest loss is so rapid that the canal cannot make it worse. Rather, I contend, adoption of international standards in canal construction could lead to net environmental and social benefits for the country. C1 Smithsonian Trop Res Inst, Panama City, Panama. RP Condit, R (reprint author), Smithsonian Trop Res Inst, Panama City, Panama. EM conditr@gmail.com NR 20 TC 5 Z9 5 U1 6 U2 25 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1545-7885 J9 PLOS BIOL JI PLoS. Biol. PD JUL PY 2015 VL 13 IS 7 AR e1002208 DI 10.1371/journal.pbio.1002208 PG 7 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA CQ5BA UT WOS:000360617100020 PM 26214182 ER PT J AU Wurst, C Wann, S Thompson, R Keller, A Maixner, F Allam, A Finch, C Frohlich, B Kaplan, H Lombardi, G Sutherland, L Sutherland, J Watson, L Cox, S Miyamoto, M Narula, J Stewart, A Thomas, G Zink, A AF Wurst, C. Wann, S. Thompson, R. Keller, A. Maixner, F. Allam, A. Finch, C. Frohlich, B. Kaplan, H. Lombardi, G. Sutherland, L. Sutherland, J. Watson, L. Cox, S. Miyamoto, M. Narula, J. Stewart, A. Thomas, G. Zink, A. TI ATHEROSCLEROSIS IN ANCIENT MUMMIFIED HUMAN REMAINS: LINKING GENETIC PREDISPOSITION WITH THE OCCURRENCE OF CALCIFIED PLAQUES SO ATHEROSCLEROSIS LA English DT Meeting Abstract CT 83rd Congress of the European-Atherosclerosis-Society (EAS) CY MAR 22-25, 2015 CL Glasgow, SCOTLAND SP European Atherosclerosis Soc C1 [Wurst, C.; Maixner, F.; Zink, A.] Inst Mummies & Iceman, European Acad Bozen Bolzano, Bolzano, Italy. [Wann, S.] Columbia St Marys Healthcare, Cardiovasc Grp, Milwaukee, WI USA. [Thompson, R.] St Lukes Mid Amer Heart Inst, Cardiol, Kansas City, MO USA. [Keller, A.] Clin Bioinformat, Dept Clin Bioinformat, Saarbrucken, Germany. [Allam, A.] Al Azahr Univ, Cairo, Egypt. [Finch, C.] Univ So Calif, Davis Sch Gerontol, Los Angeles, CA USA. [Frohlich, B.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kaplan, H.] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. [Lombardi, G.] Univ Peruana Cayetano Heredia, Lima, Peru. [Sutherland, L.] Newport Q3 Diagnost Ctr, Newport Beach, CA USA. [Sutherland, J.] Saddleback Mem Med Ctr, Laguna Hills, CA USA. [Watson, L.] Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. [Cox, S.] Univ Cambridge, Dept Archeol, Cambridge, England. [Miyamoto, M.] Mission Internal Med Grp, Mission Viejo, CA USA. [Narula, J.] Icahn Sch Med Mt Sinai, Zena & Michael A Wiener Cardiovasc Inst, New York, NY 10029 USA. [Stewart, A.] Univ Ottawa, Inst Heart, John & Jennifer Ruddy Canadian Cardiovasc Genet, Ottawa, ON, Canada. [Thomas, G.] Univ Calif Irvine, Mem Care Heart & Vasc Inst, Long Beach, CA USA. RI Zink, Albert/P-4024-2015 OI Zink, Albert/0000-0002-1461-747X NR 0 TC 0 Z9 0 U1 0 U2 3 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0021-9150 EI 1879-1484 J9 ATHEROSCLEROSIS JI Atherosclerosis PD JUL PY 2015 VL 241 IS 1 MA EAS-0863 BP E140 EP E140 PG 1 WC Cardiac & Cardiovascular Systems; Peripheral Vascular Disease SC Cardiovascular System & Cardiology GA CP7WS UT WOS:000360100600463 ER PT J AU Loi, ST Trott, CM Murphy, T Cairns, IH Bell, M Hurley-Walker, N Morgan, J Lenc, E Offringa, AR Feng, L Hancock, PJ Kaplan, DL Kudryavtseva, N Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Gaensler, BM Goeke, R Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Waterson, M Wayth, RB Webster, RL Whitney, AR Williams, A Williams, CL AF Loi, Shyeh Tjing Trott, Cathryn M. Murphy, Tara Cairns, Iver H. Bell, Martin Hurley-Walker, Natasha Morgan, John Lenc, Emil Offringa, A. R. Feng, L. Hancock, P. J. Kaplan, D. L. Kudryavtseva, N. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Gaensler, B. M. Goeke, R. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Waterson, M. Wayth, R. B. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI Power spectrum analysis of ionospheric fluctuations with the Murchison Widefield Array SO RADIO SCIENCE LA English DT Article DE Murchison Widefield Array; ionosphere; power spectrum ID ATMOSPHERIC GRAVITY-WAVES; RADIO-INTERFEROMETER ARRAY; WHISTLER DUCTS; STRONG SCINTILLATIONS; ELECTRIC-FIELDS; F-REGION; 74 MHZ; PLASMASPHERE; DISTURBANCES; CALIBRATION AB Low-frequency, wide field-of-view (FOV) radio telescopes such as the Murchison Widefield Array (MWA) enable the ionosphere to be sampled at high spatial completeness. We present the results of the first power spectrum analysis of ionospheric fluctuations in MWA data, where we examined the position offsets of radio sources appearing in two data sets. The refractive shifts in the positions of celestial sources are proportional to spatial gradients in the electron column density transverse to the line of sight. These can be used to probe plasma structures and waves in the ionosphere. The regional (10-100km) scales probed by the MWA, determined by the size of its FOV and the spatial density of radio sources (typically thousands in a single FOV), complement the global (100-1000km) scales of GPS studies and local (0.01-1km) scales of radar scattering measurements. Our data exhibit a range of complex structures and waves. Some fluctuations have the characteristics of traveling ionospheric disturbances, while others take the form of narrow, slowly drifting bands aligned along the Earth's magnetic field. C1 [Loi, Shyeh Tjing; Murphy, Tara; Cairns, Iver H.; Lenc, Emil; Bernardi, G.; Bowman, J. D.; Cappallo, R. J.; Corey, B. E.; Deshpande, A. A.; Gaensler, B. M.; Greenhill, L. J.; Hazelton, B. J.; Johnston-Hollitt, M.; Kasper, J. C.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Morales, M. F.; Oberoi, D.; Prabu, T.; Rogers, A. E. E.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.; Webster, R. L.; Whitney, A. R.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Loi, Shyeh Tjing; Trott, Cathryn M.; Murphy, Tara; Bell, Martin; Lenc, Emil; Offringa, A. R.; Hancock, P. J.; Bowman, J. D.; Briggs, F.; Gaensler, B. M.; Mitchell, D. A.; Ord, S. M.; Roshi, A.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys, Sydney, NSW, Australia. [Trott, Cathryn M.; Hurley-Walker, Natasha; Morgan, John; Hancock, P. J.; Kudryavtseva, N.; Cappallo, R. J.; Corey, B. E.; Emrich, D.; Kratzenberg, E.; Lonsdale, C. J.; Lynch, M. J.; McWhirter, S. R.; Ord, S. M.; Rogers, A. E. E.; Tingay, S. J.; Waterson, M.; Wayth, R. B.; Whitney, A. R.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA, Australia. [Bell, Martin; Deshpande, A. A.; Mitchell, D. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] CSIRO Astron & Space Sci, Epping, NSW, Australia. [Offringa, A. R.; Briggs, F.; Gaensler, B. M.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Offringa, A. R.; Hazelton, B. J.; Morales, M. F.] ASTRON Netherlands Inst Radio Astron, Dwingeloo, Netherlands. [Feng, L.; Goeke, R.; Johnston-Hollitt, M.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kaplan, D. L.; Kasper, J. C.] Univ Wisconsin, Dept Phys, Milwaukee, WI USA. [Bernardi, G.; Oberoi, D.] Square Kilometre Array South Africa, Cape Town, South Africa. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [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. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Gaensler, B. M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON, Canada. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. RP Loi, ST (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. EM sloi5113@uni.sydney.edu.au RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Udayashankar , N/D-4901-2012; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; OI Cairns, Iver/0000-0001-6978-9765; Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942; Hancock, Paul/0000-0002-4203-2946; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; Loi, Shyeh Tjing/0000-0002-6528-4548; Murphy, Tara/0000-0002-2686-438X FU U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientic Research [FA9550-0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research grant) [MED-E1799]; Australian Federal government via the National Collaborative Research Infrastructure Strategy; Australian Federal government via the Education Investment Fund; Australian Federal government via the Australia India Strategic Research Fund; Australian Federal government via the Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia - Western Australian State government; Australian Research Council DECRA award [DE140100316]; [DP110101587]; [DP140103933]; [AST-1412421] FX The data supporting this paper are available upon request submitted via email to the corresponding author at sloi5113@uni.sydney.edu.au. This scientific work makes use of the Murchison Radio-astronomy Observatory. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for the MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientic Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research grant). The Australian Federal government provides additional support via the National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. I.H.C. acknowledges the support of grants DP110101587 and DP140103933. C.M.T. is supported by an Australian Research Council DECRA award, DE140100316. D.L.K. acknowledges the support of grant AST-1412421. NR 92 TC 8 Z9 8 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD JUL PY 2015 VL 50 IS 7 BP 574 EP 597 DI 10.1002/2015RS005711 PG 24 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA CP7NQ UT WOS:000360075300002 ER PT J AU Neben, AR Bradley, RF Hewitt, JN Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Deshpande, AA Goeke, R Greenhill, LJ Hazelton, BJ Johnston-Hollitt, M Kaplan, DL Lonsdale, CJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Wayth, RB Webster, RL Williams, A Williams, CL AF Neben, A. R. Bradley, R. F. Hewitt, J. N. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Deshpande, A. A. Goeke, R. Greenhill, L. J. Hazelton, B. J. Johnston-Hollitt, M. Kaplan, D. L. Lonsdale, C. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Wayth, R. B. Webster, R. L. Williams, A. Williams, C. L. TI Measuring phased-array antenna beampatterns with high dynamic range for the Murchison Widefield Array using 137MHz ORBCOMM satellites SO RADIO SCIENCE LA English DT Article DE antenna arrays; radio astronomy; antennas ID POWER SPECTRUM MEASUREMENTS; REIONIZATION; EPOCH; COSMOLOGY; PRECISION; FOREGROUNDS; HOLOGRAPHY; TELESCOPE; PATTERN; MODEL AB Detection of the fluctuations in a 21cm line emission from neutral hydrogen during the Epoch of Reionization in thousand hour integrations poses stringent requirements on calibration and image quality, both of which necessitate accurate primary beam models. The Murchison Widefield Array (MWA) uses phased-array antenna elements which maximize collecting area at the cost of complexity. To quantify their performance, we have developed a novel beam measurement system using the 137MHz ORBCOMM satellite constellation and a reference dipole antenna. Using power ratio measurements, we measure the in situ beampattern of the MWA antenna tile relative to that of the reference antenna, canceling the variation of satellite flux or polarization with time. We employ angular averaging to mitigate multipath effects (ground scattering) and assess environmental systematics with a null experiment in which the MWA tile is replaced with a second-reference dipole. We achieve beam measurements over 30dB dynamic range in beam sensitivity over a large field of view (65% of the visible sky), far wider and deeper than drift scans through astronomical sources allow. We verify an analytic model of the MWA tile at this frequency within a few percent statistical scatter within the full width at half maximum. Toward the edges of the main lobe and in the sidelobes, we measure tens of percent systematic deviations. We compare these errors with those expected from known beamforming errors. C1 [Neben, A. R.; Hewitt, J. N.; Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bradley, R. F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA USA. [Bradley, R. F.] Natl Radio Astron Observ, Charlottesville, VA USA. [Bernardi, G.; Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bernardi, G.] Square Kilometre Array South Africa, Cape Town, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI USA. [Mitchell, D. A.] CSIRO Astron & Space Sci, Epping, NSW, Australia. [Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Wayth, R. B.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys, Sydney, NSW, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Ord, S. M.; Tingay, S. J.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA, Australia. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3052, Australia. RP Neben, AR (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM abrahamn@mit.edu RI Wayth, Randall/B-2444-2013; Udayashankar , N/D-4901-2012; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012 OI Wayth, Randall/0000-0002-6995-4131; M, Manjunath/0000-0001-8710-0730; FU NSF [AST-0821321]; Marble Astrophysics Fund; MIT School of Science; U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-Sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; Raman Research Institute; Australian National University; Victoria University of Wellington from the New Zealand Ministry of Economic Development [MED-E1799]; Victoria University of Wellington (from the IBM Shared University Research grant) [MED-E1799]; Australian Federal government via the Commonwealth Scientific and Industrial Research Organisation (CSIRO); Australian Federal government via the National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australian Federal government via the Australia India Strategic Research Fund; Australian Federal government via the Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Curtin University; University of Western Australia - Western Australian State government FX This work was supported by NSF grant AST-0821321, the Marble Astrophysics Fund, and the MIT School of Science. We thank Pat Klima, Bang Dinh Nhan, and the staff at the National Radio Astronomy Observatory-Green Bank for assistance in setting up and debugging our experiment and Haoxuan Zheng, Aaron Ewall-Wice, Josh Dillon, Lu Feng, and Daniel Jacobs for helpful discussions. We thank Nithyanandan Thyagarajan, Josh Dillon, Adrian Sutinjo, Tim Colegate, and the anonymous referees for very helpful comments on our manuscript. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We would like to extend our appreciation to Ed LeFave, Alan Fenn, David Bruno, John Glover, and Jeffrey Herd at MIT Lincoln Laboratory for their support of anechoic chamber tests of MWA prototype antenna tiles. 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 MWA comes from the U.S. National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-Sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a joint venture of Curtin University and the University of Western Australia, funded by the Western Australian State government. Data on which figures and tables herein are based may be obtained by contacting the corresponding author Abraham Neben (abrahamn@mit.edu). NR 58 TC 14 Z9 14 U1 2 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 EI 1944-799X J9 RADIO SCI JI Radio Sci. PD JUL PY 2015 VL 50 IS 7 BP 614 EP 629 DI 10.1002/2015RS005678 PG 16 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA CP7NQ UT WOS:000360075300004 ER PT J AU Hacker, BC AF Hacker, Barton C. TI A Cultural History of Firearms in the Age of Empire SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Hacker, Barton C.] Amer Museum Nat Hist, Smithsonian Inst, Washington, DC 20001 USA. RP Hacker, BC (reprint author), Amer Museum Nat Hist, Smithsonian Inst, Washington, DC 20001 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2015 VL 56 IS 3 BP 754 EP 755 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA CQ0AK UT WOS:000360256800011 ER PT J AU Sneed, JM Harrison, SJ Houk, LJ Paul, VJ AF Sneed, J. M. Harrison, S. J. Houk, L. J. Paul, V. J. TI Macroalgae may interrupt important cues for coral larval settlement SO PLANTA MEDICA LA English DT Meeting Abstract CT Annual Meeting of the American-Society-of-Pharmacognosy CY JUL 25-29, 2015 CL CO SP Amer Soc Pharmacognosy C1 [Sneed, J. M.; Harrison, S. J.; Houk, L. J.; Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 0 U2 4 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 EI 1439-0221 J9 PLANTA MED JI Planta Med. PD JUL PY 2015 VL 81 IS 11 MA IL22 BP 862 EP 862 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA CP6AP UT WOS:000359967000036 ER PT J AU Cai, W Salvador-Reyes, LA Zhang, W Matthew, S Ratnayake, R Paul, VJ Dang, LH Luesch, H AF Cai, W. Salvador-Reyes, L. A. Zhang, W. Matthew, S. Ratnayake, R. Paul, V. J. Dang, L. H. Luesch, H. TI Discovery, synthesis, and biological evaluation of apratyramide, a marine-derived transcriptional stimulator of VEGF-A SO PLANTA MEDICA LA English DT Meeting Abstract CT Annual Meeting of the American-Society-of-Pharmacognosy CY JUL 25-29, 2015 CL CO SP Amer Soc Pharmacognosy C1 [Cai, W.; Salvador-Reyes, L. A.; Zhang, W.; Matthew, S.; Ratnayake, R.; Luesch, H.] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Cai, W.; Ratnayake, R.; Dang, L. H.; Luesch, H.] Univ Florida, Ctr Nat Prod Drug Discovery & Dev CNPD3, Gainesville, FL 32610 USA. [Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Dang, L. H.] Univ Florida, Dept Med, Gainesville, FL 32610 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 EI 1439-0221 J9 PLANTA MED JI Planta Med. PD JUL PY 2015 VL 81 IS 11 MA CL6 BP 872 EP 872 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA CP6AP UT WOS:000359967000085 ER PT J AU Cai, W Salvador-Reyes, LA Zhang, W Matthew, S Ratnayake, R Paul, VJ Dang, LH Luesch, H AF Cai, W. Salvador-Reyes, L. A. Zhang, W. Matthew, S. Ratnayake, R. Paul, V. J. Dang, L. H. Luesch, H. TI Discovery, synthesis, and biological evaluation of apratyramide, a marine-derived transcriptional stimulator of VEGF-A SO PLANTA MEDICA LA English DT Meeting Abstract CT Annual Meeting of the American-Society-of-Pharmacognosy CY JUL 25-29, 2015 CL CO SP Amer Soc Pharmacognosy C1 [Cai, W.; Salvador-Reyes, L. A.; Zhang, W.; Matthew, S.; Ratnayake, R.; Luesch, H.] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Cai, W.; Ratnayake, R.; Dang, L. H.; Luesch, H.] Univ Florida, Ctr Nat Prod Drug Discovery & Dev CNPD3, Gainesville, FL 32610 USA. [Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Dang, L. H.] Univ Florida, Dept Med, Gainesville, FL 32611 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 EI 1439-0221 J9 PLANTA MED JI Planta Med. PD JUL PY 2015 VL 81 IS 11 MA PK9 BP 897 EP 897 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA CP6AP UT WOS:000359967000203 ER PT J AU Al-Awadhi, FH Paul, V Luesch, H AF Al-Awadhi, F. H. Paul, V Luesch, H. TI Isolation, structure elucidation and biological evaluation of novel cathepsin inhibitors from marine cyanobacteria SO PLANTA MEDICA LA English DT Meeting Abstract CT Annual Meeting of the American-Society-of-Pharmacognosy CY JUL 25-29, 2015 CL CO SP Amer Soc Pharmacognosy C1 [Al-Awadhi, F. H.; Luesch, H.] Univ Florida, Dept Med Chem, Gainesville, FL USA. [Luesch, H.] Univ Florida, Ctr Nat Prod Drug Discovery & Dev CNPD3, Gainesville, FL USA. [Paul, V] Smithsonian Marine Stn, Ft Pierce, FL USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 EI 1439-0221 J9 PLANTA MED JI Planta Med. PD JUL PY 2015 VL 81 IS 11 MA PQ18 BP 912 EP 912 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA CP6AP UT WOS:000359967000267 ER PT J AU Eiseman, CS Blyth, JA Smith, DR AF Eiseman, Charles S. Blyth, Julia A. Smith, David R. TI NOTES ON FOUR ANEMONE-FEEDING INSECTS IN THE EASTERN UNITED STATES (DIPTERA: AGROMYZIDAE; HYMENOPTERA: TENTHREDINIDAE; LEPIDOPTERA: NOCTUIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Anemone acutiloba; Anemone quinquefolia; Cerastis tenebrifera; hepatica; leafmining; Monophadnus aequalis; Phytomyza multifidae; Pnigalio flavipes; Pnigalio pallipes; Pseudodineura parva; sawfly ID MOUNTAINS NATIONAL-PARK; SAWFLIES AB Pseudodineura parva (Norton) (Hymenoptera: Tenthredinidae: Nematinae), Phytomyza multifidae Sehgal (Diptera: Agromyzidae), and Cerastis tenebrifera (Walker) (Lepidoptera: Noctuidae) were reared from wood anemone (Ranunculaceae: Anemone quinquefolia L.), and Monophadnus aequalis MacGillivray (Hymenoptera: Tenthredinidae: Blennocampinae) from sharp-lobed hepatica (A. acutiloba (DC.) G. Lawson) for the first time. The rearing of P. multifidae represents a new U.S. record, and the sawfly records extend the known range of both species south to northwestern Alabama. Details of rearings of all four species are provided, along with descriptions of the sawfly larvae. Two parasitoids, Pnigalio flavipes (Ashmead) and P. pallipes (Provancher) (Eulophidae), were reared from Phytomyza multifidae. C1 [Smith, David R.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20560 USA. RP Eiseman, CS (reprint author), 276 Old Wendell Rd, Northfield, MA 01360 USA. EM ceiseman@gmail.com; sawfly2@aol.com FU Nantucket Biodiversity Initiative FX We thank the Nantucket Biodiversity Initiative for financial and other support for leafminer surveys on Nantucket; the Nantucket Conservation Foundation for permission to collect insects at Squam Farm; Jim and Faye Lacefield, Tuscumbia, AL, for allowing us to collect specimens at their beautiful nature preserve; Owen Lonsdale, Canadian National Collection of Insects, Arachnids and Nematodes, Ottawa, ON, for identification of the agromyzids; Christer Hansson, Lund University, Lund, Sweden, for identification of the eulophids; Samuel Jaffe, Keene, NH, and David L. Wagner, Department of Ecology and Evolutionary Biology, University of Connecticut, Storrs, CT, for assistance in identifying the moth; and John T. Lill, Department of Biological Sciences, George Washington University, Washington, D.C., for reviewing the manuscript. NR 20 TC 1 Z9 1 U1 1 U2 3 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 JUL PY 2015 VL 117 IS 3 BP 281 EP 289 DI 10.4289/0013-8797.117.3.281 PG 9 WC Entomology SC Entomology GA CP7GC UT WOS:000360054200002 ER PT J AU Goldstein, PZ Morita, S Capshaw, G AF Goldstein, Paul Z. Morita, Shelah Capshaw, Grace TI STASIS AND FLUX AMONG SATURNIIDAE AND SPHINGIDAE (LEPIDOPTERA) ON MASSACHUSETTS' OFFSHORE ISLANDS AND THE POSSIBLE ROLE OF COMPSILURA CONCINNATA (MEIGEN) (DIPTERA: TACHINIDAE) AS AN AGENT OF MAINLAND NEW ENGLAND MOTH DECLINES SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Eacles imperialis; moth declines; Martha's Vineyard; Nantucket; Eizabeth Islands; faunal change; non-target impacts ID USA; CONSERVATION; PATTERNS; HISTORY AB The lepidopteran fauna of Massachusetts' offshore islands (USA), particularly Martha's Vineyard and Nantucket, has been well characterized, and comprises intact assemblages of disjunct, regionally rare, habitat-specialized, and otherwise threatened species that have declined elsewhere in New England. These include the only persistent and extant population of Eacles imperialis Drury (Saturniidae: Ceratocampinae) in New England, one of at least three ceratocampines to have undergone partial or total extirpation from the region. Examining historical and recent records within two groups-Saturniidae and Sphingidae-that have exhibited varying degrees of flux over time, we compare these islands and identify taxonomic and ecological components of their faunas that appear historically volatile. After reviewing suspected agents of these declines, including the introduced generalist parasitoid Compsilura concinnata (Diptera: Tachinidae), we present preliminary tachinid capture data which suggest that C. concinnata has not been established where E. imperialis persists. C1 [Goldstein, Paul Z.] USDA, Systemat Entomol Lab, Natl Museum Nat Hist, Washington, DC 20013 USA. [Morita, Shelah] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Capshaw, Grace] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. RP Goldstein, PZ (reprint author), USDA, Systemat Entomol Lab, Natl Museum Nat Hist, POB 37012,MRC 168, Washington, DC 20013 USA. EM paul.goldstein@ars.usda.gov FU Edey Foundation (West Tisbury, MA); USDA; University of Maryland FX Norm Woodley (Systematic Entomology Laboratory [SEL], USDA) kindly provided determinations of tachinids during the course of this work; his help and that of Gary Ouellette (SEL), who generating maps for this paper, is most gratefully acknowledged. Tim Simmons (Massachusetts Natural Heritage & Endangered Species Program) has been an active leader in the protection and study of Eacles imperialis in particular and of threatened invertebrates and their habitats in Massachusetts generally for 30 years. He and Mike Nelson (also MNHESP) have generated vigorous discussion and contributed enormous effort towards our understanding threats to the New England lepidopteran fauna and meeting the conservation challenges they present. David Gregg and Mark Mello contributed detailed observations of saturniids on the Elizabeth Islands and elsewhere; Jeff Boettner (UMASS) contributed numerous observations of tachinids and saturniids alike; Megan Ottens-Sargent of Aquinnah, MA contributed the only modern (26 June 2015) Martha's Vineyard record of Sphinx kalmiae. The tachinid "by-catch" specimens on which the basic data presented here are based were sampled under funding from the Edey Foundation (West Tisbury, MA) to The Trustees of Reservations and PZG. During the preparation of this manuscript PZG was supported in part by a cooperative agreement between USDA and University of Maryland. Jeff Boetner and David Wagner provided helpful reviews of this paper. NR 38 TC 2 Z9 2 U1 4 U2 8 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 JUL PY 2015 VL 117 IS 3 BP 347 EP 366 DI 10.4289/0013-8797.117.3.347 PG 20 WC Entomology SC Entomology GA CP7GC UT WOS:000360054200004 ER PT J AU Henry, TJ Dellape, PM Scudder, GGE AF Henry, Thomas J. Dellape, Pablo M. Scudder, G. G. E. TI RESURRECTION OF THE GENERA CROPHIUS STAL AND MAYANA DISTANT FROM SYNONYMY UNDER ANOMALOPTERA AMYOT AND SERVILLE, DESCRIPTION OF A NEW GENUS, AND A KEY TO THE NEW WORLD OXYCARENID GENERA (HEMIPTERA: HETEROPTERA: OXYCARENIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Hemiptera; oxycarenids; diagnoses; photographs; key; new genus; new combinations; revised status ID METOPOPLAX-DITOMOIDES COSTA; LYGAEOIDEA OXYCARENIDAE; RECORD; COTTON; PEST AB The largely New World genus Crophius Stal, revised status, and Mayana Distant, revised status, are resurrected from synonymy with the genus Anomaloptera Amyot and Serville, which is restricted to contain only the type species, A. helianthemi Amyot and Serville, from the western Mediterranean Region. Mayana, previously also considered a junior synonym of Crophius, is resurrected to contain M. costatus Distant, the type species, M. diruptus Distant, and M. formosus (Van Duzee), new combination, transferred from Crophius. Neocrophius, new genus, is established to accommodate Neocrophius heidemanni (Van Duzee), new combination, the type species, transferred from Crophius, and Neocrophius singularis (Brailovsky and Barrera), new combination, transferred from Anomaloptera. The genera Crophius, Mayana, and Neocrophius are described and diagnosed and dorsal habitus images and a key are provided to help distinguish the nine New World genera. C1 [Henry, Thomas J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Dellape, Pablo M.] Univ Nacl La Plata, Fac Ciencias Nat & Museo, Div Entomol, RA-1900 La Plata, Argentina. [Scudder, G. G. E.] Univ British Columbia, Beaty Biodivers Ctr, Vancouver, BC V6T 1Z4, Canada. [Scudder, G. G. E.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. 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; pdellape@gmail.com; scudder@zoology.ubc.ca OI Dellape, Pablo M./0000-0002-6914-1026 NR 40 TC 2 Z9 2 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 JUL PY 2015 VL 117 IS 3 BP 367 EP 380 DI 10.4289/0013-8797.117.3.367 PG 14 WC Entomology SC Entomology GA CP7GC UT WOS:000360054200005 ER PT J AU Huang, YM Rueda, LM AF Huang, Yiau-Min Rueda, Leopoldo M. TI PSEUDALBUGINOSUS, A NEW SUBGENUS OF AEDES, AND A REDESCRIPTION OF AEDES (PSEUDALBUGINOSUS) GRJEBINEI HAMON, TAUFFLIEB, AND MAILLOT (DIPTERA: CULICIDAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Pseudalbuginosus; new subgenus; Aedes grjebinei; characteristics; systematics; Culicidae; Gabon ID AFROTROPICAL REGION DIPTERA; ALLIED TAXA DIPTERA; LIFE STAGES; MORPHOLOGICAL DATA; AEDINI DIPTERA; PICTORIAL KEY; CLASSIFICATION; PHYLOGENY; OCHLEROTATUS AB Pseudalbuginosus, a new subgenus of Aedes Meigen, is characterized and diagnosed. Aedes grjebinei Hamon, Taufflieb, and Maillot is removed from the subgenus Aedimorphus Theobald and placed in the new monotypic subgenus Pseudalbuginosus on the basis of a critical study of all known specimens. The adult male and the male genitalia of Ae. (Pseudalbuginosus) grjebinei are described, with the illustration of the genitalia and images of the proboscis and maxillary palpi. Its affinity to other subgenera of the genus Aedes is discussed. Information on type data, distribution, bionomics, medical importance and a taxonomic discussion of this species are presented. C1 [Huang, Yiau-Min] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Rueda, Leopoldo M.] Smithsonian Inst, Museum Support Ctr, WRBU, Suitland, MD 20746 USA. [Rueda, Leopoldo M.] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD 20910 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA. EM huangy@si.edu; ruedapol@si.edu NR 18 TC 0 Z9 0 U1 1 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 JUL PY 2015 VL 117 IS 3 BP 381 EP 388 DI 10.4289/0013-8797.117.3.381 PG 8 WC Entomology SC Entomology GA CP7GC UT WOS:000360054200006 ER PT J AU Wolski, A Henry, TJ AF Wolski, Andrzej Henry, Thomas J. TI REVIEW AND A NEW SUBFAMILY PLACEMENT OF THE PLANT BUG GENUS ISOMETOCORIS CARVALHO AND SAILER, 1954 (HEMIPTERA: HETEROPTERA: MIRIDAE), WITH THE DESCRIPTION OF A NEW SPECIES FROM BRAZIL SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article ID BALTIC AMBER; CYLAPINAE; REVISION; ISOMETOPINAE; PSALLOPINAE; INSECTA; GENERA AB The genus Isometocoris Carvalho and Sailer is reviewed and I. penicillus, new species, from Brazil is described. Diagnoses of the genus and included species I. blantoni Carvalho and Sailer and I. penicillus, n. sp., are given; a color adult habitus photo of both Isometocoris species, male genitalic drawings of Isometocoris penicillus n. sp., and scanning electron micrographs of selected structures of I. blantoni are provided; and an identification key is given to help distinguish the two included species. Isometocoris is transferred from the subfamily Psallopinae to the Cylapinae, where it is placed in the tribe Fulviini. Psallopinae is reduced to tribal level (Psallopini, new status) within the Cylapinae, and relationships among Cylapinae, Isometopinae, and Psallopinae are discussed. C1 [Wolski, Andrzej] Opole Univ, Dept Biosystemat, PL-45052 Opole, Poland. [Henry, Thomas J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. RP Wolski, A (reprint author), Opole Univ, Dept Biosystemat, Oleska 22, PL-45052 Opole, Poland. EM miridae78@gmail.com; thomas.henry@ars.usda.gov NR 31 TC 4 Z9 5 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 JUL PY 2015 VL 117 IS 3 BP 407 EP 418 DI 10.4289/0013-8797.117.3.407 PG 12 WC Entomology SC Entomology GA CP7GC UT WOS:000360054200009 ER PT J AU Beaty, LE Nyarko, K Bernal, XE AF Beaty, Lynne E. Nyarko, Kwesi Bernal, Ximena E. TI Light-induced changes in pigmentation through ontogeny in cane toad tadpoles (Rhinella marina) SO HERPETOLOGICAL JOURNAL LA English DT Article DE aposematic; Bufo marinus; camouflage; melanophore; ontogeny; pigment changes; toxicity ID SPECIES AMBYSTOMA-BARBOURI; COLOR-CHANGE; BUFO-MARINUS; XENOPUS TADPOLE; PREDATION RISK; MELANOPHORES; METAMORPHOSIS; HETEROCHRONY; PALATABILITY; ANURANS AB Light-induced pigmentation changes are widespread among tadpole species. In this study we characterised light-induced changes in melanin dispersion through development in cane toad tadpoles (Rhinella marina). We describe a pattern of light-induced pigmentation change in which tadpoles are darker in the presence of light and lighter in darkness until the onset of metamorphosis. This pattern contrasts with that of other non-bufonid tadpole species, but mimics the pattern of pigment change exhibited by embryonic anurans. We discuss our results in light of the ontogenetic changes in toxicity to evaluate the photoresponse of cane toad tadpole pigments as a potential aposematic signal, neotenic trait, and thermal adaptation. C1 [Beaty, Lynne E.] Oklahoma State Univ, Dept Zool, Stillwater, OK 74078 USA. [Nyarko, Kwesi] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Bernal, Ximena E.] Smithsonian Trop Res Inst, Gamboa, Panama. RP Beaty, LE (reprint author), Oklahoma State Univ, Dept Zool, Stillwater, OK 74078 USA. EM lynne.beaty@okstate.edu NR 44 TC 0 Z9 0 U1 4 U2 9 PU BRITISH HERPETOL SOC PI LONDON PA C/O ZOOL SOC LONDON REGENTS PARK, LONDON NW1 4RY, ENGLAND SN 0268-0130 J9 HERPETOL J JI Herpetolog. J. PD JUL PY 2015 VL 25 IS 3 BP 191 EP 195 PG 5 WC Zoology SC Zoology GA CO8DI UT WOS:000359394800010 ER PT J AU Liszt, HS Guzman, VV Pety, J Gerin, M Neufeld, DA Gratier, P AF Liszt, H. S. Guzman, V. V. Pety, J. Gerin, M. Neufeld, D. A. Gratier, P. TI Widespread galactic CF+ absorption: detection toward W49 with the Plateau de Bure Interferometer SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: molecules ID DIFFUSE INTERSTELLAR-MEDIUM; TRANSLUCENT CLOUDS; COMPARATIVE CHEMISTRY; MOLECULAR-HYDROGEN; GAS; ABUNDANCE; CARBON; MODELS AB Aims. We study the usefulness of CF+ as a tracer of the regions where C+ and H-2 coexist in the interstellar medium. Methods. We used the Plateau de Bure Interferometer to synthesize CF+ J = 1-0 absorption at 102.6 GHz toward the core of the distant HII region W49N at l = 43.2 degrees, b = 0.0 degrees, and we modeled the fluorine chemistry in diffuse/translucent molecular gas. Results. We detected CF+ absorption over a broad range of velocity showing that CF+ is widespread in the H-2-bearing Galactic disk gas. Conclusions. Originally detected in dense gas in the Orion Bar and Horsehead PDR (Photon-Dominated Region) CF+ was subsequently detected in absorption from diffuse and translucent clouds seen toward BL Lac and 3C 111. Here we showed that CF+ is distributed throughout the diffuse and translucent molecular disk gas with N(CF+)/N(H-2) = 1.5-2.0 x 10(-10), increasing to N(CF+)/N(H-2) = 3.5 x 10(-10) in one cloud at 39 km s(-1) having higher N(H-2) approximate to 3 x 10(21) cm(-2). Models of the fluorine chemistry reproduce the observed column densities and relative abundance of HF, from which CF+ forms, but generally overpredict the column density of CF+ by factors of 1.4-4. We show that a free space photodissociation rate Gamma greater than or similar to 10(-9) s(-1), comparable to that of CH, might account for much of the discrepancy but a recent calculation finds a value about ten times smaller. In the heavily blended and kinematically complex spectra seen toward W49, CF+ absorption primarily traces the peaks of the H2 distribution. C1 [Liszt, H. S.] Rat Radio Astron Observ, Charlottesville, VA 22903 USA. [Guzman, V. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pety, J.; Gerin, M.] CNRS, UMR 8112, Observ Paris, F-75014 Paris, France. [Pety, J.; Gerin, M.] Ecole Normale Super, LERMA LRA, F-75005 Paris, France. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Gratier, P.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Gratier, P.] CNRS, UMR 5804, LAB, F-33270 Floirac, France. RP Liszt, HS (reprint author), Rat Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM hliszt@nrao.edu OI PETY, Jerome/0000-0003-3061-6546 FU CNRS program "Physique et Chimie du Milieu Interstellaire" (PCMI); European Research Council [336474] FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. IRAM is operated by CNRS (France), MPG (Germany) and IGN (Spain). This work was supported by the CNRS program "Physique et Chimie du Milieu Interstellaire" (PCMI). P.G. acknowledges funding by the European Research Council (Starting Grant 3DICE, grant agreement 336474, PI: V. Wakelam). We thank Fabrice Dayou and Evelyne Roueff for communicating the result of their calculation of the CF+ photdissociation rate prior to publication. NR 35 TC 3 Z9 3 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 JUL PY 2015 VL 579 AR A12 DI 10.1051/0004-6361/201526232 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100024 ER PT J AU Popesso, P Biviano, A Finoguenov, A Wilman, D Salvato, M Magnelli, B Gruppioni, C Pozzi, F Rodighiero, G Ziparo, F Berta, S Elbaz, D Dickinson, M Lutz, D Altieri, B Aussel, H Cimatti, A Fadda, D Ilbert, O Le Floch, E Nordon, R Poglitsch, A Genel, S Xu, CK AF Popesso, P. Biviano, A. Finoguenov, A. Wilman, D. Salvato, M. Magnelli, B. Gruppioni, C. Pozzi, F. Rodighiero, G. Ziparo, F. Berta, S. Elbaz, D. Dickinson, M. Lutz, D. Altieri, B. Aussel, H. Cimatti, A. Fadda, D. Ilbert, O. Le Floch, E. Nordon, R. Poglitsch, A. Genel, S. Xu, C. K. TI The role of massive halos in the star formation history of the Universe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: star formation; galaxies: groups: general ID INFRARED LUMINOSITY FUNCTIONS; DEEP-FIELD-SOUTH; HIERARCHICAL GALAXY FORMATION; GALACTIC NUCLEUS FEEDBACK; SUPERMASSIVE BLACK-HOLES; REST-FRAME ULTRAVIOLET; X-RAY GROUPS; FORMING GALAXIES; COSMOS FIELD; SPITZER VIEW AB Context. The most striking feature of the cosmic star formation history (CSFH) of the Universe is a dramatic drop in the star formation (SF) activity after z similar to 1. Aims. In this work we investigate whether the very same process of assembly and growth of structures is one of the major drivers of the observed decline in the Universe's SF activity. Methods. We study the contribution to the CSFH of galaxies in halos of different masses. This is done by studying the total SF ratehalo mass-redshift plane from redshift 0 to redshift similar to 1.6 in a sample of 57 groups and clusters by using the deepest available mid- and far-infrared surveys conducted with Spitzer MIPS and Herschel PACS and SPIRE, on blank (ECDFS, CDFN, and the COSMOS) and cluster fields. Results. Our results show that low mass groups (M-halo similar to 6 x 10(12) - 6 x 10(13) M-circle dot) provide a 60-80% contribution to the CSFH at z similar to 1. This contribution has declined faster than the CSFH in the past 8 billion years to less than 10% at z < 0.3, where the overall SF activity is sustained by lower mass halos. More massive systems (M-halo > 6 x 10(13) M-circle dot) provide only a marginal contribution (<10%) at any epoch. A simplified abundance-matching method shows that the large contribution of low mass groups at z similar to 1 is due to a large fraction (>50%) of very massive, highly star-forming main sequence galaxies. Below z similar to 1 a quenching process must take place in massive halos to cause the observed faster suppression of their SF activity. Such a process must be a slow one, though, since most of the models implementing a rapid quenching of the SF activity in accreting satellites significantly underpredict the observed SF level in massive halos at any redshift. This would rule out short time-scale mechanisms such as ram pressure stripping. Instead, starvation or the satellite's transition from cold to hot accretion would provide a quenching timescale of 1 to few Gyr that is more consistent with the observations. Conclusions. Our results suggest a scenario in which, owing to the structure formation process, more and more galaxies experience the group environment and the associated quenching process in the past 8 billion years. This leads to the progressive suppression of their SF activity so that it shapes the CSFH below z similar to 1. C1 [Popesso, P.] Excellence Cluster Universe, D-85748 Garching, Germany. [Popesso, P.; Finoguenov, A.; Wilman, D.; Salvato, M.; Magnelli, B.; Ziparo, F.; Berta, S.; Lutz, D.; Nordon, R.; Poglitsch, A.] Max Planck Inst Extraterr Phys MPE, D-85741 Garching, Germany. [Biviano, A.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Gruppioni, C.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Rodighiero, G.; Cimatti, A.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Elbaz, D.; Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Aussel, H.; Le Floch, E.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Altieri, B.] ESA, European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Fadda, D.] Caltech 100 22, NASA, Herschel Sci Ctr, Pasadena, CA 91125 USA. [Ilbert, O.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Genel, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Xu, C. K.] Caltech 100 22, IPAC, Pasadena, CA 91125 USA. RP Popesso, P (reprint author), Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany. EM popesso@mpe.mpg.de OI Gruppioni, Carlotta/0000-0002-5836-4056; Wilman, David/0000-0002-1822-4462; Rodighiero, Giulia/0000-0002-9415-2296 FU BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI (Italy); CICYT/MCYT (Spain); NASA; Sloan Foundation; NSF; US Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council of England FX The authors thank G. Zamorani for the very useful comments on an early draft of this paper. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, 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 (Italy), and CICYT/MCYT (Spain). We gratefully acknowledge the contributions of the entire COSMOS collaboration consisting of more than 100 scientists. More information about the COSMOS survey is available at http://www.astro.caltech.edu/similar to cosmos. This research has made use of NASA's Astrophysics Data System, of NED, which is operated by JPL/Caltech, under contract with NASA, and of SDSS, which has been funded by the Sloan Foundation, NSF, the US Department of Energy, NASA, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council of England. The SDSS is managed by the participating institutions (www.sdss.org/collaboration/credits.html). NR 112 TC 6 Z9 6 U1 3 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A132 DI 10.1051/0004-6361/201424715 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100144 ER PT J AU Schady, P Kruhler, T Greiner, J Graham, JF Kann, DA Bolmer, J Delvaux, C Elliott, J Klose, S Knust, F Guelbenzu, AN Rau, A Rossi, A Savaglio, S Schmidl, S Schweyer, T Sudilovsky, V Tanga, M Tanvir, NR Varela, K Wiseman, P AF Schady, P. Kruehler, T. Greiner, J. Graham, J. F. Kann, D. A. Bolmer, J. Delvaux, C. Elliott, J. Klose, S. Knust, F. Guelbenzu, A. Nicuesa Rau, A. Rossi, A. Savaglio, S. Schmidl, S. Schweyer, T. Sudilovsky, V. Tanga, M. Tanvir, N. R. Varela, K. Wiseman, P. TI Super-solar metallicity at the position of the ultra-long GRB 130925A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: individual: GRB 130925A; galaxies: individual: GRB 130925A; galaxies: abundances; dust, extinction ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; STAR-FORMING GALAXIES; HOST GALAXIES; MASSIVE STARS; INTERSTELLAR-MEDIUM; REDSHIFT EVOLUTION; DEEP SURVEY; AFTERGLOW; STELLAR AB Over the last decade there has been immense progress in the follow-up of short and long gamma-ray bursts (GRBs), resulting in a significant rise in the detection rate of X-ray and optical afterglows, in the determination of GRB redshifts, and of the identification of the underlying host galaxies. Nevertheless, our theoretical understanding of the progenitors and central engines powering these vast explosions is lagging behind, and a newly identified class of ultra-long GRBs has fuelled speculation on the existence of a new channel of GRB formation. In this paper we present high signal-to-noise X-Shooter observations of the host galaxy of GRB 130925A, which is the fourth unambiguously identified ultra-long GRB, with prompt X-ray emission detected for similar to 20 ks. The GRB line of sight was close to the host galaxy nucleus, and our spectroscopic observations cover this region along the bulge/disk of the galaxy and a bright star-forming region within the outskirts of the galaxy. From our broad wavelength coverage, we obtain accurate metallicity and dust-extinction measurements at the galaxy nucleus and at an outer star-forming region, and measure a super-solar metallicity at both locations, placing this galaxy within the 10-20% most metal-rich GRB host galaxies. Such a high metal enrichment has significant implications on the progenitor models of both long and ultra-long GRBs, although the edge-on orientation of the host galaxy does not allow us to rule out a large metallicity variation along our line of sight. The spatially resolved spectroscopic observations presented in this paper off er important insight into variations in the metal and dust abundance within GRB host galaxies. However, they also illustrate the need for integral field unit observations on a larger sample of GRB host galaxies of a variety of metallicities to provide a more quantitative view on the relation between the GRB circumburst environment and the galaxy-whole properties. C1 [Schady, P.; Greiner, J.; Graham, J. F.; Bolmer, J.; Delvaux, C.; Elliott, J.; Knust, F.; Rau, A.; Savaglio, S.; Schmidl, S.; Schweyer, T.; Tanga, M.; Varela, K.; Wiseman, P.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kruehler, T.] European So Observ, Santiago 19, Chile. [Kann, D. A.; Klose, S.; Guelbenzu, A. Nicuesa] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Bolmer, J.; Schweyer, T.] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany. [Elliott, J.; Sudilovsky, V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rossi, A.] CNR, Area Ric, INAF IASF Bologna, I-40129 Bologna, Italy. [Savaglio, S.] Univ Calabria, Dept Phys, I-87036 Arcavacata Di Rende, Italy. [Savaglio, S.] European So Observ, D-85748 Garching, Germany. [Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Schady, P (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany. EM pschady@mpe.mpg.de RI Rossi, Andrea/N-4674-2015; OI Wiseman, Philip/0000-0002-3073-1512; Rossi, Andrea/0000-0002-8860-6538; Elliott, Jonathan/0000-0001-8043-4965; Kruehler, Thomas/0000-0002-8682-2384; Savaglio, Sandra/0000-0003-2354-3238 FU Alexander von Humboldt Foundation of Germany; DFG [KI 766/16-1]; EXTraS from the European Union [60752]; Thuringer Ministerium fur Bildung, Wissenschaft ind Kultur [FKZ 12010-514]; TLS Tautenburg; Leibniz-Prize (DFG) [HA 1850/28-1]; [091.A-0703] FX P.S. acknowledges support through the Sofja Kovalevskaja Award from the Alexander von Humboldt Foundation of Germany. J.F.G., M.T. and P.W. acknowledge support through the Sofja Kovalevskaja Award to P. Schady from the Alexander von Humboldt Foundation of Germany. S.K. and A.N.G. acknowledge support of DFG grant KI 766/16-1. C.D. acknowledges support through EXTraS, funded from the European Union's Seventh Framework Programme for research, technological development and demonstration under grant agreement No. 60752. S.S. acknowledges support by the Thuringer Ministerium fur Bildung, Wissenschaft ind Kultur under FKZ 12010-514. D.A.K. acknowledges TLS Tautenburg for financial support. Part of the funding for GROND (both hardware as well as personel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). This study is based on data acquired at ESO, Programme ID 091.A-0703. NR 102 TC 5 Z9 5 U1 0 U2 7 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2015 VL 579 AR A126 DI 10.1051/0004-6361/201526060 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100138 ER PT J AU Shulevski, A Morganti, R Barthel, PD Murgia, M van Weeren, RJ White, GJ Bruggen, M Kunert-Bajraszewska, M Jamrozy, M Best, PN Rottgering, HJA Chyzy, KT de Gasperin, F Birzan, L Brunetti, G Brienza, M Rafferty, DA Anderson, J Beck, R Deller, A Zarka, P Schwarz, D Mahony, E Orru, E Bell, ME Bentum, MJ Bernardi, G Bonafede, A Breitling, F Broderick, JW Butcher, HR Carbone, D Ciardi, B de Geus, E Duscha, S Eisloffel, J Engels, D Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Heald, G Hoeft, M Horandel, J Horneffer, A van der Horst, AJ Intema, H Juette, E Karastergiou, A Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G Maat, P Mann, G McFadden, R McKay-Bukowski, D McKean, JP Meulman, H Mulcahy, DD Munk, H Norden, MJ Paas, H Pandey-Pommier, M Pizzo, R Polatidis, AG Reich, W Rowlinson, A Scaife, AMM Serylak, M Sluman, J Smirnov, O Steinmetz, M Swinbank, J Tagger, M Tang, Y Tasse, C Thoudam, S Toribio, MC Vermeulen, R Vocks, C Wijers, RAMJ Wise, MW Wucknitz, O AF Shulevski, A. Morganti, R. Barthel, P. D. Murgia, M. van Weeren, R. J. White, G. J. Brueggen, M. Kunert-Bajraszewska, M. Jamrozy, M. Best, P. N. Rottgering, H. J. A. Chyzy, K. T. de Gasperin, F. Birzan, L. Brunetti, G. Brienza, M. Rafferty, D. A. Anderson, J. Beck, R. Deller, A. Zarka, P. Schwarz, D. Mahony, E. Orru, E. Bell, M. E. Bentum, M. J. Bernardi, G. Bonafede, A. Breitling, F. Broderick, J. W. Butcher, H. R. Carbone, D. Ciardi, B. de Geus, E. Duscha, S. Eisloeffel, J. Engels, D. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Heald, G. Hoeft, M. Horandel, J. Horneffer, A. van der Horst, A. J. Intema, H. Juette, E. Karastergiou, A. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. Maat, P. Mann, G. McFadden, R. McKay-Bukowski, D. McKean, J. P. Meulman, H. Mulcahy, D. D. Munk, H. Norden, M. J. Paas, H. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Reich, W. Rowlinson, A. Scaife, A. M. M. Serylak, M. Sluman, J. Smirnov, O. Steinmetz, M. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. Thoudam, S. Toribio, M. C. Vermeulen, R. Vocks, C. Wijers, R. A. M. J. Wise, M. W. Wucknitz, O. TI The peculiar radio galaxy 4C 35.06: a case for recurrent AGN activity? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radio continuum: galaxies; galaxies: active; radio lines: galaxies; galaxies: individual: 4C 35.06 ID H I ABSORPTION; SKY SURVEY; GALACTIC NUCLEI; CLUSTER GALAXIES; BLACK-HOLES; GAS; ACCRETION; SCALE; POWER; LOFAR AB Using observations obtained with the LOw Fequency ARray (LOFAR), the Westerbork Synthesis Radio Telescope (WSRT) and archival Very Large Array (VLA) data, we have traced the radio emission to large scales in the complex source 4C 35.06 located in the core of the galaxy cluster Abell 407. At higher spatial resolution (similar to 4"), the source was known to have two inner radio lobes spanning 31 kpc and a diffuse, low-brightness extension running parallel to them, offset by about 11 kpc (in projection). At 62 MHz, we detect the radio emission of this structure extending out to 210 kpc. At 1.4 GHz and intermediate spatial resolution (similar to 30"), the structure appears to have a helical morphology. We have derived the characteristics of the radio spectral index across the source. We show that the source morphology is most likely the result of at least two episodes of AGN activity separated by a dormant period of around 35 Myr. The outermost regions of radio emission have a steep spectral index (alpha < -1), indicative of old plasma. We connect the spectral index properties of the resolved source structure with the integrated flux density spectral index of 4C 35.06 and suggest an explanation for its unusual integrated flux density spectral shape (a moderately steep power law with no discernible spectral break), possibly providing a proxy for future studies of more distant radio sources through inferring their detailed spectral index properties and activity history from their integrated spectral indices. The AGN is hosted by one of the galaxies located in the cluster core of Abell 407. We propose that it is intermittently active as it moves in the dense environment in the cluster core. In this scenario, the AGN turned on sometime in the past, and has produced the helical pattern of emission, possibly a sign of jet precession/merger during that episode of activity. Using LOFAR, we can trace the relic plasma from that episode of activity out to greater distances from the core than ever before. Using the the WSRT, we detect HI in absorption against the center of the radio source. The absorption profile is relatively broad (FWHM of 288 km s(-1)), similar to what is found in other clusters. The derived column density is N-HI similar to 4 x 10(20) cm(-2) for a T-spin = 100 K. This detection supports the connection - already suggested for other restarted radio sources - between the presence of cold gas and restarting activity. The cold gas appears to be dominated by a blue-shifted component although the broad HI profile could also include gas with different kinematics. Understanding the duty cycle of the radio emission as well as the triggering mechanism for starting (or restarting) the radio-loud activity can provide important constraints to quantify the impact of AGN feedback on galaxy evolution. The study of these mechanisms at low frequencies using morphological and spectral information promises to bring new important insights in this field. C1 [Shulevski, A.; Morganti, R.; Barthel, P. D.; Brienza, M.; Heald, G.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Shulevski, A.; Morganti, R.; Brienza, M.; Deller, A.; Mahony, E.; Orru, E.; Bentum, M. J.; de Geus, E.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Heald, G.; Kondratiev, V. I.; Kuper, G.; Maat, P.; McFadden, R.; McKean, J. P.; Meulman, H.; Munk, H.; Norden, M. J.; Pizzo, R.; Polatidis, A. G.; Sluman, J.; Tang, Y.; Toribio, M. C.; Vermeulen, R.; Wise, M. W.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Murgia, M.] INAF Osservatorio Astron Cagliari, I-09047 Cagliari, Italy. [van Weeren, R. J.; Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, RAL Space, Didcot OX11 0QX, Oxon, England. [Brueggen, M.; de Gasperin, F.; Birzan, L.; Rafferty, D. A.; Bonafede, A.; Engels, D.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Kunert-Bajraszewska, M.] NCU, Fac Phys Astron & Informat, Torun Ctr Astron, PL-87100 Torun, Poland. [Jamrozy, M.; Chyzy, K. T.] Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland. [Best, P. N.] Royal Observ, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rottgering, H. J. A.; Garrett, M. A.; Intema, H.] Leiden Univ, Leiden Observ, NL-2333 RA Leiden, Netherlands. [Anderson, J.] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Beck, R.; Kramer, M.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bell, M. E.; Horneffer, A.; Rowlinson, A.] CSIRO Australia Telescope Natl Facil, Epping, NSW 53121, Australia. [Bentum, M. J.] Univ Twente, NL-7522 NB Enschede, Netherlands. [Breitling, F.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Broderick, J. W.; Fender, R.; Karastergiou, A.; Mann, G.; Serylak, M.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Broderick, J. W.; Mulcahy, D. D.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Carbone, D.; van der Horst, A. J.; Swinbank, J.; Wijers, R. A. M. J.; Wise, M. W.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [McKay-Bukowski, D.] SmarterVis BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Falcke, H.; Horandel, J.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Univ Orleans, CNRS, LPC2E, F-45071 Orleans 2, France. [Griessmeier, J.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS,INSU,USR 704,OSUC, F-18330 Nancay, France. [Intema, H.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Kondratiev, V. I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Kramer, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Kuniyoshi, M.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo, Japan. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, CIT, NL-9747 AJ Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Smirnov, O.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Zarka, P.; Tasse, C.] Observ Paris, UMR CNRS 8109, LESIA, F-92195 Meudon, France. [Brunetti, G.] INAF, IRA, I-40129 Bologna, Italy. [Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, CNRS, Observ Cote Azur,UMR 7293, F-06300 Nice, France. RP Shulevski, A (reprint author), Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands. EM shulevski@astron.nl; morganti@astron.nl; pdb@astro.rug.nl RI Kunert-Bajraszewska, Magdalena/F-9060-2014; Ciardi, Benedetta/N-7625-2015; Intema, Huib/D-1438-2012; Kondratiev, Vladislav/N-1105-2015; OI Intema, Huib/0000-0002-5880-2730; Brunetti, Gianfranco/0000-0003-4195-8613; Mahony, Elizabeth/0000-0002-5053-2828; de Gasperin, Francesco/0000-0003-4439-2627; Deller, Adam/0000-0001-9434-3837; Kondratiev, Vladislav/0000-0001-8864-7471; Swinbank, John/0000-0001-9445-1846; Murgia, Matteo/0000-0002-4800-0806; Wijers, Ralph/0000-0002-3101-1808; van Weeren, Reinout/0000-0002-0587-1660; Shulevski, Aleksandar/0000-0002-1827-0469 FU Netherlands Foundation for Scientific Research (NWO); National Aeronautics and Space Administration; European Research Council under the European Union [RADIOLIFE-320745]; NASA [PF2-130104, NAS8-03060]; Chandra X-ray Center 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. Data taken with the Westerbork Synthesis Radio Telescope were part of this work. It is operated by ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands Foundation for Scientific Research (NWO). 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 VLA images used in this work were produced as part of the NRAO VLA Archive Survey, (c) AUI/NRAO. This research has made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. R.M. gratefully acknowledges support from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant RADIOLIFE-320745. R.Jv.W. acknowledges the support by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 66 TC 4 Z9 4 U1 0 U2 1 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 JUL PY 2015 VL 579 AR A27 DI 10.1051/0004-6361/201425416 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0XL UT WOS:000358877100039 ER PT J AU Alam, S Albareti, FD Prieto, CA Anders, F Anderson, SF Anderton, T Andrews, BH Armengaud, E Aubourg, E Bailey, S Basu, S Bautista, JE Beaton, RL Beers, TC Bender, CF Berlind, AA Beutler, F Bhardwaj, V Bird, JC Bizyaev, D Blake, CH Blanton, MR Blomqvist, M Bochanski, JJ Bolton, AS Bovy, J Bradley, AS Brandt, WN Brauer, DE Brinkmann, J Brown, PJ Brownstein, JR Burden, A Burtin, E Busca, NG Cai, Z Capozzi, D Rosell, AC Carr, MA Carrera, R Chambers, KC Chaplin, WJ Chen, YC Chiappini, C Chojnowski, SD Chuang, CH Clerc, N Comparat, J Covey, K Croft, RAC Cuesta, AJ Cunha, K da Costa, LN Da Rio, N Davenport, JRA Dawson, KS De Lee, N Delubac, T Deshpande, R Dhital, S Dutra-Ferreira, L Dwelly, T Ealet, A Ebelke, GL Edmondson, EM Eisenstein, DJ Ellsworth, T Elsworth, Y Epstein, CR Eracleous, M Escoffier, S Esposito, M Evans, ML Fan, XH Fernandez-Alvar, E Feuillet, D Ak, NF Finley, H Finoguenov, A Flaherty, K Fleming, SW Font-Ribera, A Foster, J Frinchaboy, PM Galbraith-Frew, JG Garcia, RA Garcia-Hernandez, DA Perez, AEG Gaulme, P Ge, J Genova-Santos, R Georgakakis, A Ghezzi, L Gillespie, BA Girardi, L Goddard, D Gontcho, SGA Hernandez, JIG Grebel, EK Green, PJ Grieb, JN Grieves, N Gunn, JE Guo, H Harding, P Hasselquist, S Hawley, SL Hayden, M Hearty, FR Hekker, S Ho, S Hogg, DW Holley-Bockelmann, K Holtzman, JA Honscheid, K Huber, D Huehnerhoff, J Ivans, II Jiang, LH Johnson, JA Kinemuchi, K Kirkby, D Kitaura, F Klaene, MA Knapp, GR Kneib, JP Koenig, XP Lam, CR Lan, TW Lang, DT Laurent, P Le Goff, JM Leauthaud, A Lee, KG Lee, YS Licquia, TC Liu, J Long, DC Lopez-Corredoira, M Lorenzo-Oliveira, D Lucatello, S Lundgren, B Lupton, RH Mack, CE Mahadevan, S Maia, MAG Majewski, SR Malanushenko, E Malanushenko, V Manchado, A Manera, M Mao, QQ Maraston, C Marchwinski, RC Margala, D Martell, SL Martig, M Masters, KL Mathur, S McBride, CK McGehee, PM McGreer, ID McMahon, RG Menard, B Menzel, ML Merloni, A Meszaros, S Miller, AA Miralda-Escude, J Miyatake, H Montero-Dorta, AD More, S Morganson, E Morice-Atkinson, X Morrison, HL Mosser, B Muna, D Myers, AD Nandra, K Newman, JA Neyrinck, M Nguyen, DC Nichol, RC Nidever, DL Noterdaeme, P Nuza, SE O'Connell, JE O'Connell, RW O'Connell, R Ogando, RLC Olmstead, MD Oravetz, AE Oravetz, DJ Osumi, K Owen, R Padgett, DL Padmanabhan, N Paegert, M Palanque-Delabrouille, N Pan, KK Parejko, JK Paris, I Park, C Pattarakijwanich, P Pellejero-Ibanez, M Pepper, J Percival, WJ Perez-Fournon, I Perez-Rafols, I Petitjean, P Pieri, MM Pinsonneault, MH de Mello, GFP Prada, F Prakash, A Price-Whelan, AM Protopapas, P Raddick, MJ Rahman, M Reid, BA Rich, J Rix, HW Robin, AC Rockosi, CM Rodrigues, TS Rodriguez-Torres, S Roe, NA Ross, AJ Ross, NP Rossi, G Ruan, JJ Rubino-Martin, JA Rykoff, ES Salazar-Albornoz, S Salvato, M Samushia, L Sanchez, AG Santiago, B Sayres, C Schiavon, RP Schlegel, DJ Schmidt, SJ Schneider, DP Schultheis, M Schwope, AD Scoccola, CG Scott, C Sellgren, K Seo, HJ Serenelli, A Shane, N Shen, Y Shetrone, M Shu, YP Aguirre, VS Sivarani, T Skrutskie, MF Slosar, A Smith, VV Sobreira, F Souto, D Stassun, KG Steinmetz, M Stello, D Strauss, MA Streblyanska, A Suzuki, N Swanson, MEC Tan, JC Tayar, J Terrien, RC Thakar, AR Thomas, D Thomas, N Thompson, BA Tinker, JL Tojeiro, R Troup, NW Vargas-Magana, M Vazquez, JA Verde, L Viel, M Vogt, NP Wake, DA Wang, J Weaver, BA Weinberg, DH Weiner, BJ White, M Wilson, JC Wisniewski, JP Wood-Vasey, WM Yeche, C York, DG Zakamska, NL Zamora, O Zasowski, G Zehavi, I Zhao, GB Zheng, Z Zhou, X Zhou, ZM Zou, H Zhu, GT AF Alam, Shadab Albareti, Franco D. Allende Prieto, Carlos Anders, F. Anderson, Scott F. Anderton, Timothy Andrews, Brett H. Armengaud, Eric Aubourg, Eric Bailey, Stephen Basu, Sarbani Bautista, Julian E. Beaton, Rachael L. Beers, Timothy C. Bender, Chad F. Berlind, Andreas A. Beutler, Florian Bhardwaj, Vaishali Bird, Jonathan C. Bizyaev, Dmitry Blake, Cullen H. Blanton, Michael R. Blomqvist, Michael Bochanski, John J. Bolton, Adam S. Bovy, Jo Bradley, A. Shelden Brandt, W. N. Brauer, D. E. Brinkmann, J. Brown, Peter J. Brownstein, Joel R. Burden, Angela Burtin, Etienne Busca, Nicolas G. Cai, Zheng Capozzi, Diego Rosell, Aurelio Carnero Carr, Michael A. Carrera, Ricardo Chambers, K. C. Chaplin, William James Chen, Yen-Chi Chiappini, Cristina Chojnowski, S. Drew Chuang, Chia-Hsun Clerc, Nicolas Comparat, Johan Covey, Kevin Croft, Rupert A. C. Cuesta, Antonio J. Cunha, Katia da Costa, Luiz N. Da Rio, Nicola Davenport, James R. A. Dawson, Kyle S. De Lee, Nathan Delubac, Timothee Deshpande, Rohit Dhital, Saurav Dutra-Ferreira, Leticia Dwelly, Tom Ealet, Anne Ebelke, Garrett L. Edmondson, Edward M. Eisenstein, Daniel J. Ellsworth, Tristan Elsworth, Yvonne Epstein, Courtney R. Eracleous, Michael Escoffier, Stephanie Esposito, Massimiliano Evans, Michael L. Fan, Xiaohui Fernandez-Alvar, Emma Feuillet, Diane Ak, Nurten Filiz Finley, Hayley Finoguenov, Alexis Flaherty, Kevin Fleming, Scott W. Font-Ribera, Andreu Foster, Jonathan Frinchaboy, Peter M. Galbraith-Frew, J. G. Garcia, Rafael A. Garcia-Hernandez, D. A. Garcia Perez, Ana E. Gaulme, Patrick Ge, Jian Genova-Santos, R. Georgakakis, A. Ghezzi, Luan Gillespie, Bruce A. Girardi, Leo Goddard, Daniel Gontcho, Satya Gontcho A. Gonzalez Hernandez, Jonay I. Grebel, Eva K. Green, Paul J. Grieb, Jan Niklas Grieves, Nolan Gunn, James E. Guo, Hong Harding, Paul Hasselquist, Sten Hawley, Suzanne L. Hayden, Michael Hearty, Fred R. Hekker, Saskia Ho, Shirley Hogg, David W. Holley-Bockelmann, Kelly Holtzman, Jon A. Honscheid, Klaus Huber, Daniel Huehnerhoff, Joseph Ivans, Inese I. Jiang, Linhua Johnson, Jennifer A. Kinemuchi, Karen Kirkby, David Kitaura, Francisco Klaene, Mark A. Knapp, Gillian R. Kneib, Jean-Paul Koenig, Xavier P. Lam, Charles R. Lan, Ting-Wen Lang, Dustin Laurent, Pierre Le Goff, Jean-Marc Leauthaud, Alexie Lee, Khee-Gan Lee, Young Sun Licquia, Timothy C. Liu, Jian Long, Daniel C. Lopez-Corredoira, Martin Lorenzo-Oliveira, Diego Lucatello, Sara Lundgren, Britt Lupton, Robert H. Mack, Claude E., III Mahadevan, Suvrath Maia, Marcio A. G. Majewski, Steven R. Malanushenko, Elena Malanushenko, Viktor Manchado, A. Manera, Marc Mao, Qingqing Maraston, Claudia Marchwinski, Robert C. Margala, Daniel Martell, Sarah L. Martig, Marie Masters, Karen L. Mathur, Savita McBride, Cameron K. McGehee, Peregrine M. McGreer, Ian D. McMahon, Richard G. Menard, Brice Menzel, Marie-Luise Merloni, Andrea Meszaros, Szabolcs Miller, Adam A. Miralda-Escude, Jordi Miyatake, Hironao Montero-Dorta, Antonio D. More, Surhud Morganson, Eric Morice-Atkinson, Xan Morrison, Heather L. Mosser, Benoit Muna, Demitri Myers, Adam D. Nandra, Kirpal Newman, Jeffrey A. Neyrinck, Mark Nguyen, Duy Cuong Nichol, Robert C. Nidever, David L. Noterdaeme, Pasquier Nuza, Sebastian E. O'Connell, Julia E. O'Connell, Robert W. O'Connell, Ross Ogando, Ricardo L. C. Olmstead, Matthew D. Oravetz, Audrey E. Oravetz, Daniel J. Osumi, Keisuke Owen, Russell Padgett, Deborah L. Padmanabhan, Nikhil Paegert, Martin Palanque-Delabrouille, Nathalie Pan, Kaike Parejko, John K. Paris, Isabelle Park, Changbom Pattarakijwanich, Petchara Pellejero-Ibanez, M. Pepper, Joshua Percival, Will J. Perez-Fournon, Ismael Perez-Rafols, Ignasi Petitjean, Patrick Pieri, Matthew M. Pinsonneault, Marc H. Porto de Mello, Gustavo F. Prada, Francisco Prakash, Abhishek Price-Whelan, Adrian M. Protopapas, Pavlos Raddick, M. Jordan Rahman, Mubdi Reid, Beth A. Rich, James Rix, Hans-Walter Robin, Annie C. Rockosi, Constance M. Rodrigues, Thaise S. Rodriguez-Torres, Sergio Roe, Natalie A. Ross, Ashley J. Ross, Nicholas P. Rossi, Graziano Ruan, John J. Rubino-Martin, J. A. Rykoff, Eli S. Salazar-Albornoz, Salvador Salvato, Mara Samushia, Lado Sanchez, Ariel G. Santiago, Basilio Sayres, Conor Schiavon, Ricardo P. Schlegel, David J. Schmidt, Sarah J. Schneider, Donald P. Schultheis, Mathias Schwope, Axel D. Scoccola, C. G. Scott, Caroline Sellgren, Kris Seo, Hee-Jong Serenelli, Aldo Shane, Neville Shen, Yue Shetrone, Matthew Shu, Yiping Aguirre, V. Silva Sivarani, Thirupathi Skrutskie, M. F. Slosar, Anze Smith, Verne V. Sobreira, Flavia Souto, Diogo Stassun, Keivan G. Steinmetz, Matthias Stello, Dennis Strauss, Michael A. Streblyanska, Alina Suzuki, Nao Swanson, Molly E. C. Tan, Jonathan C. Tayar, Jamie Terrien, Ryan C. Thakar, Aniruddha R. Thomas, Daniel Thomas, Neil Thompson, Benjamin A. Tinker, Jeremy L. Tojeiro, Rita Troup, Nicholas W. Vargas-Magana, Mariana Vazquez, Jose A. Verde, Licia Viel, Matteo Vogt, Nicole P. Wake, David A. Wang, Ji Weaver, Benjamin A. Weinberg, David H. Weiner, Benjamin J. White, Martin Wilson, John C. Wisniewski, John P. Wood-Vasey, W. M. Yeche, Christophe York, Donald G. Zakamska, Nadia L. Zamora, O. Zasowski, Gail Zehavi, Idit Zhao, Gong-Bo Zheng, Zheng Zhou, Xu Zhou, Zhimin Zou, Hu Zhu, Guangtun TI THE ELEVENTH AND TWELFTH DATA RELEASES OF THE SLOAN DIGITAL SKY SURVEY: FINAL DATA FROM SDSS-III SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atlases; catalogs; surveys ID OSCILLATION SPECTROSCOPIC SURVEY; GALACTIC EVOLUTION EXPERIMENT; BARYON ACOUSTIC-OSCILLATIONS; LOW-MASS STELLAR; 1ST DATA RELEASE; SOLAR-LIKE STARS; FIXED-DELAY INTERFEROMETRY; CATALOG ARCHIVE SERVER; BROWN DWARF CANDIDATE; MAIN-SEQUENCE STARS AB The third generation of the Sloan Digital Sky Survey (SDSS-III) took data from 2008 to 2014 using the original SDSS wide-field imager, the original and an upgraded multi-object fiber-fed optical spectrograph, a new near-infrared high-resolution spectrograph, and a novel optical interferometer. All of the data from SDSS-III are now made public. In particular, this paper describes Data Release 11 (DR11) including all data acquired through 2013 July, and Data Release 12 (DR12) adding data acquired through 2014 July (including all data included in previous data releases), marking the end of SDSS-III observing. Relative to our previous public release (DR10), DR12 adds one million new spectra of galaxies and quasars from the Baryon Oscillation Spectroscopic Survey (BOSS) over an additional 3000 deg(2) of sky, more than triples the number of H-band spectra of stars as part of the Apache Point Observatory (APO) Galactic Evolution Experiment (APOGEE), and includes repeated accurate radial velocity measurements of 5500 stars from the Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS). The APOGEE outputs now include the measured abundances of 15 different elements for each star. In total, SDSS-III added 5200 deg(2) of ugriz imaging; 155,520 spectra of 138,099 stars as part of the Sloan Exploration of Galactic Understanding and Evolution 2 (SEGUE-2) survey; 2,497,484 BOSS spectra of 1,372,737 galaxies, 294,512 quasars, and 247,216 stars over 9376 deg(2); 618,080 APOGEE spectra of 156,593 stars; and 197,040 MARVELS spectra of 5513 stars. Since its first light in 1998, SDSS has imaged over 1/3 of the Celestial sphere in five bands and obtained over five million astronomical spectra. C1 [Alam, Shadab; Croft, Rupert A. C.; Ho, Shirley; Lang, Dustin; O'Connell, Ross; Osumi, Keisuke; Vargas-Magana, Mariana] Carnegie Mellon Univ, Dept Phys, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Albareti, Franco D.; Chuang, Chia-Hsun; Comparat, Johan; Prada, Francisco; Rodriguez-Torres, Sergio] Univ Autonoma Madrid, Inst Fis Teor, UAM CSIC, E-28049 Madrid, Spain. [Allende Prieto, Carlos; Carrera, Ricardo; Esposito, Massimiliano; Fernandez-Alvar, Emma; Garcia-Hernandez, D. A.; Garcia Perez, Ana E.; Genova-Santos, R.; Gonzalez Hernandez, Jonay I.; Lopez-Corredoira, Martin; Manchado, A.; Pellejero-Ibanez, M.; Perez-Fournon, Ismael; Rubino-Martin, J. A.; Scoccola, C. G.; Streblyanska, Alina; Zamora, O.] IAC, E-38200 Tenerife, Spain. [Allende Prieto, Carlos; Carrera, Ricardo; Esposito, Massimiliano; Fernandez-Alvar, Emma; Garcia-Hernandez, D. A.; Garcia Perez, Ana E.; Genova-Santos, R.; Gonzalez Hernandez, Jonay I.; Lopez-Corredoira, Martin; Manchado, A.; Pellejero-Ibanez, M.; Perez-Fournon, Ismael; Rubino-Martin, J. A.; Scoccola, C. G.; Streblyanska, Alina; Zamora, O.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Anders, F.; Brauer, D. E.; Chiappini, Cristina; Kitaura, Francisco; Mack, Claude E., III; Nuza, Sebastian E.; Schwope, Axel D.; Steinmetz, Matthias] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Anderson, Scott F.; Bhardwaj, Vaishali; Bochanski, John J.; Davenport, James R. A.; Eracleous, Michael; Evans, Michael L.; Hawley, Suzanne L.; Owen, Russell; Ruan, John J.; Sayres, Conor] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Anderton, Timothy; Bolton, Adam S.; Brownstein, Joel R.; Dawson, Kyle S.; Ellsworth, Tristan; Galbraith-Frew, J. G.; Guo, Hong; Ivans, Inese I.; Montero-Dorta, Antonio D.; Olmstead, Matthew D.; Shu, Yiping; Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Andrews, Brett H.; Epstein, Courtney R.; Johnson, Jennifer A.; Muna, Demitri; Pinsonneault, Marc H.; Schmidt, Sarah J.; Sellgren, Kris; Tayar, Jamie; Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Andrews, Brett H.; Licquia, Timothy C.; Newman, Jeffrey A.; Prakash, Abhishek; Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. [Armengaud, Eric; Burtin, Etienne; Laurent, Pierre; Le Goff, Jean-Marc; Palanque-Delabrouille, Nathalie; Rich, James; Rossi, Graziano; Yeche, Christophe] CEA, Ctr Saclay, Irfu SPP, F-91191 Gif Sur Yvette, France. [Aubourg, Eric; Bautista, Julian E.; Busca, Nicolas G.] Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS IN2P3,CEA IRFU, F-75205 Paris, France. [Bailey, Stephen; Beutler, Florian; Bhardwaj, Vaishali; Font-Ribera, Andreu; Reid, Beth A.; Roe, Natalie A.; Schlegel, David J.; White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Basu, Sarbani; Koenig, Xavier P.; Wang, Ji] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Beaton, Rachael L.; Ebelke, Garrett L.; Garcia Perez, Ana E.; Lam, Charles R.; Majewski, Steven R.; O'Connell, Robert W.; Shane, Neville; Skrutskie, M. F.; Troup, Nicholas W.; Wilson, John C.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Beaton, Rachael L.; Shen, Yue] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [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. [Bender, Chad F.; Brandt, W. N.; Deshpande, Rohit; Eracleous, Michael; Ak, Nurten Filiz; Hearty, Fred R.; Mahadevan, Suvrath; Marchwinski, Robert C.; Schneider, Donald P.; Terrien, Ryan C.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Bender, Chad F.; Deshpande, Rohit; Mahadevan, Suvrath; Marchwinski, Robert C.; Terrien, Ryan C.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. [Berlind, Andreas A.; Bird, Jonathan C.; Holley-Bockelmann, Kelly; Mack, Claude E., III; Mao, Qingqing; Paegert, Martin; Pepper, Joshua; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Bizyaev, Dmitry; Bradley, A. Shelden; Brinkmann, J.; Gaulme, Patrick; Huehnerhoff, Joseph; Kinemuchi, Karen; Klaene, Mark A.; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Audrey E.; Oravetz, Daniel J.; Pan, Kaike] Apache Point Observ, Sunspot, NM 88349 USA. [Bizyaev, Dmitry; Chojnowski, S. Drew; Feuillet, Diane; Hasselquist, Sten; Hayden, Michael; Holtzman, Jon A.; Kinemuchi, Karen; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Audrey E.; Vogt, Nicole P.] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Bizyaev, Dmitry] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Blake, Cullen H.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Blanton, Michael R.; Hogg, David W.; Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Blomqvist, Michael; Kirkby, David; Margala, Daniel] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Bochanski, John J.] Rider Univ, Lawrenceville, NJ 08648 USA. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. [Brandt, W. N.; Eracleous, Michael; Ak, Nurten Filiz; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Brown, Peter J.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Burden, Angela; Capozzi, Diego; Edmondson, Edward M.; Goddard, Daniel; Manera, Marc; Maraston, Claudia; Masters, Karen L.; Morice-Atkinson, Xan; Nichol, Robert C.; Percival, Will J.; Pieri, Matthew M.; Ross, Ashley J.; Thomas, Daniel; Zhao, Gong-Bo] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Busca, Nicolas G.; Rosell, Aurelio Carnero; Cunha, Katia; da Costa, Luiz N.; Ghezzi, Luan; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Souto, Diogo] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Busca, Nicolas G.; Rosell, Aurelio Carnero; Chiappini, Cristina; da Costa, Luiz N.; Dutra-Ferreira, Leticia; Girardi, Leo; Lorenzo-Oliveira, Diego; Maia, Marcio A. G.; Ogando, Ricardo L. C.; Porto de Mello, Gustavo F.; Rodrigues, Thaise S.; Santiago, Basilio; Sobreira, Flavia] Lab Interinstituc & Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Cai, Zheng; Cunha, Katia; Fan, Xiaohui; McGreer, Ian D.; Weiner, Benjamin J.] Steward Observ, Tucson, AZ 85721 USA. [Carr, Michael A.; Gunn, James E.; Knapp, Gillian R.; Lupton, Robert H.; Miyatake, Hironao; Pattarakijwanich, Petchara; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Chambers, K. C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Chaplin, William James; Elsworth, Yvonne] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William James; Elsworth, Yvonne; Hekker, Saskia; Huber, Daniel; Aguirre, V. Silva; Stello, Dennis] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark. [Chen, Yen-Chi] Carnegie Mellon Univ, Dept Stat, Bruce & Astrid McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Clerc, Nicolas; Dwelly, Tom; Georgakakis, A.; Grieb, Jan Niklas; Menzel, Marie-Luise; Merloni, Andrea; Nandra, Kirpal; Salazar-Albornoz, Salvador; Salvato, Mara; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Covey, Kevin] Lowell Observ, Flagstaff, AZ 86001 USA. [Covey, Kevin] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Cuesta, Antonio J.; Gontcho, Satya Gontcho A.; Miralda-Escude, Jordi; Perez-Rafols, Ignasi; Verde, Licia] Univ Barcelona, Inst Ciencies Cosmos, IEEC, E-08028 Barcelona, Spain. [Cuesta, Antonio J.; Foster, Jonathan; Padmanabhan, Nikhil] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Da Rio, Nicola; Ge, Jian; Grieves, Nolan; Liu, Jian; Tan, Jonathan C.; Thomas, Neil] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. [De Lee, Nathan] No Kentucky Univ, Dept Phys & Geol, Highland Hts, KY 41099 USA. [Delubac, Timothee; Kneib, Jean-Paul] EPFL, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland. [Dhital, Saurav] Embry Riddle Aeronaut Univ, Dept Phys Sci, Daytona Beach, FL 32114 USA. [Dutra-Ferreira, Leticia; Lorenzo-Oliveira, Diego; Porto de Mello, Gustavo F.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, Brazil. [Dutra-Ferreira, Leticia] Univ Fed Rio Grande do Norte, Dept Fis, BR-59072970 Natal, RN, Brazil. [Ealet, Anne; Escoffier, Stephanie] Aix Marseille Univ, Ctr Phys Particules Marseille, CNRS IN2P3, F-13288 Marseille, France. [Eisenstein, Daniel J.; Ghezzi, Luan; Green, Paul J.; McBride, Cameron K.; Morganson, Eric; Scott, Caroline; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Eracleous, Michael] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Ak, Nurten Filiz] Erciyes Univ, Dept Astron & Space Sci, Fac Sci, TR-38039 Kayseri, Turkey. [Finley, Hayley; Noterdaeme, Pasquier; Petitjean, Patrick] UPMC, Inst Astrophys Paris, CNRS, UMR7095, F-75014 Paris, France. [Finoguenov, Alexis] Univ Helsinki, Dept Phys, FI-00140 Helsinki, Finland. [Flaherty, Kevin] Wesleyan Univ, Van Vleck Observ, Dept Astron, Middletown, CT 06459 USA. [Fleming, Scott W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fleming, Scott W.] Comp Sci Corp, Baltimore, MD 21218 USA. [Frinchaboy, Peter M.; O'Connell, Julia E.; Thompson, Benjamin A.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Garcia, Rafael A.] Univ Paris Diderot, Lab AIM, Ctr Saclay, CEA DSM,CNRS,IRFU SAp, F-91191 Gif Sur Yvette, France. [Gillespie, Bruce A.; Lan, Ting-Wen; Menard, Brice; Neyrinck, Mark; Raddick, M. Jordan; Rahman, Mubdi; Thakar, Aniruddha R.; Zakamska, Nadia L.; Zasowski, Gail; Zhu, Guangtun] Johns Hopkins Univ, Ctr Astrophys Sci, Dept Phys & Astron, Baltimore, MD 21218 USA. [Girardi, Leo; Lucatello, Sara; Rodrigues, Thaise S.] INAF, Osservatorio Astron Padova, I-35122 Padua, Italy. [Grebel, Eva K.] Heidelberg Univ, Zentrum Astron, Astron Rech Inst, D-69120 Heidelberg, Germany. [Harding, Paul; Morrison, Heather L.; Zehavi, Idit] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Hekker, Saskia] Max Planck Inst Sonnensystemforsch, D-37077 Gottingen, Germany. [Honscheid, Klaus] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Honscheid, Klaus; Johnson, Jennifer A.; Ross, Ashley J.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Huber, Daniel; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Jiang, Linhua; Shen, Yue] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Kneib, Jean-Paul] Univ Provence, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Leauthaud, Alexie; Menard, Brice; Miyatake, Hironao; More, Surhud; Suzuki, Nao] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys Math Univ Kavli IPMU, WPI, Kashiwa, Chiba 2778583, Japan. [Lee, Khee-Gan; Martig, Marie; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lee, Young Sun] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon 305764, South Korea. [Lundgren, Britt; Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53703 USA. [Manera, Marc] UCL, London WC1E 6BT, England. [Martell, Sarah L.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Mathur, Savita] Space Sci Inst, Boulder, CO 80301 USA. [McGehee, Peregrine M.] CALTECH, IPAC, Pasadena, CA 91125 USA. [McMahon, Richard G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [McMahon, Richard G.] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. [Meszaros, Szabolcs] ELTE Gothard Astrophys Observ, H-9704 Szombathely, Hungary. [Miller, Adam A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Miller, Adam A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Miralda-Escude, Jordi; Verde, Licia] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain. [Mosser, Benoit] Univ Paris 07, Univ Paris 06, Observ Paris, LESIA,UMR 8109, F-92195 Meudon, France. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Nguyen, Duy Cuong] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Nidever, David L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48104 USA. [Olmstead, Matthew D.] Kings Coll, Dept Chem & Phys, Wilkes Barre, PA 18711 USA. [Padgett, Deborah L.] NASA GSFC, Greenbelt, MD USA. [Parejko, John K.] Yale Univ, Dept Phys, New Haven, CT USA. [Paris, Isabelle; Viel, Matteo] INAF, Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Park, Changbom] Korea Inst Adv Study, Sch Phys, Seoul 130722, South Korea. [Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Perez-Rafols, Ignasi] Univ Barcelona, Fac Fis, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Pieri, Matthew M.] Aix Marseille Univ, A MIDEX, CNRS, LAM UMR 7326, F-13388 Marseille 13, France. [Prada, Francisco; Rodriguez-Torres, Sergio] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Price-Whelan, Adrian M.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Protopapas, Pavlos] Harvard Univ, SEAS, Inst Appl Computat Sci, Cambridge, MA 02138 USA. [Reid, Beth A.; White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Robin, Annie C.] Univ Franche Comte, Inst Utinam, UMR CNRS 6213, OSU Theta, F-25010 Besancon, France. [Rockosi, Constance M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Rodrigues, Thaise S.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Rossi, Graziano] Sejong Univ, Dept Astron & Space Sci, Seoul 143747, South Korea. [Rykoff, Eli S.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Salazar-Albornoz, Salvador] Univ Sternwarte, D-81679 Munich, Germany. [Salvato, Mara] Cluster Excellence, D-85748 Garching, Germany. [Samushia, Lado] Kansas State Univ, Dept Phys, Manhattan, KS 66506 USA. [Samushia, Lado] Ilia State Univ, Natl Abastumani Astrophys Observ, GE-1060 Tbilisi, Rep of Georgia. [Santiago, Basilio] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Schiavon, Ricardo P.] Gemini Observ, Hilo, HI 96720 USA. [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Schultheis, Mathias] Univ Nice Sophia Antipolis, CNRS, Observ Cote dAzur, Lab Lagrange, F-06304 Nice 4, France. [Seo, Hee-Jong] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Serenelli, Aldo] CSIC IEEC, Inst Ciencias Espacio, Fac Ciencias, E-08193 Bellaterra, Spain. [Shetrone, Matthew] Univ Texas Austin, Hobby Eberly Telescope, McDonald Observatory, TX 79734 USA. [Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Slosar, Anze; Vazquez, Jose A.] Brookhaven Natl Lab, Upton, NY 11973 USA. [Smith, Verne V.] Natl Opt Astron Observ, Tucson, AZ USA. [Sobreira, Flavia] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Terrien, Ryan C.] Penn State Univ, Penn State Astrobiol Res Ctr, University Pk, PA 16802 USA. [Thomas, Daniel] South East Phys Network, SEPnet, Southampton, Hants, England. [Tojeiro, Rita] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Verde, Licia] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Viel, Matteo] Ist Nazl Fis Nucl, I-34127 Trieste, Italy. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Wisniewski, John P.] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [York, Donald G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Zhou, Xu; Zhou, Zhimin; Zou, Hu] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China. RP Wood-Vasey, WM (reprint author), Univ Pittsburgh, Dept Phys & Astron, PITT PACC, 3941 OHara St, Pittsburgh, PA 15260 USA. RI Ogando, Ricardo/A-1747-2010; White, Martin/I-3880-2015; Brandt, William/N-2844-2015; Meszaros, Szabolcs/N-2287-2014; Georgakakis, Antonis/K-4457-2013; Mao, Qingqing/E-2043-2016; Sobreira, Flavia/F-4168-2015; Jiang, Linhua/H-5485-2016; Croft, Rupert/N-8707-2014; EPFL, Physics/O-6514-2016; Carrera, Ricardo/K-8760-2014; OI Ogando, Ricardo/0000-0003-2120-1154; White, Martin/0000-0001-9912-5070; Brandt, William/0000-0002-0167-2453; Meszaros, Szabolcs/0000-0001-8237-5209; Mao, Qingqing/0000-0001-6001-6723; Sobreira, Flavia/0000-0002-7822-0658; Jiang, Linhua/0000-0003-4176-6486; Croft, Rupert/0000-0003-0697-2583; Carrera, Ricardo/0000-0001-6143-8151; Rahman, Mubdi/0000-0003-1842-6096; Escoffier, Stephanie/0000-0002-2847-7498; Covey, Kevin/0000-0001-6914-7797; Davenport, James/0000-0002-0637-835X; Georgakakis, Antonis/0000-0002-3514-2442; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769; Chambers, Kenneth /0000-0001-6965-7789; Pepper, Joshua/0000-0002-3827-8417; Beaton, Rachael/0000-0002-1691-8217; Shane, Neville/0000-0003-1024-7739; Kirkby, David/0000-0002-8828-5463; Viel, Matteo/0000-0002-2642-5707; Schmidt, Sarah/0000-0002-7224-7702; Zhu, Guangtun/0000-0002-7574-8078; Beutler, Florian/0000-0003-0467-5438; Finley, Hayley/0000-0002-1216-8914; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; Fleming, Scott/0000-0003-0556-027X; /0000-0002-1891-3794; Verde, Licia/0000-0003-2601-8770; Martig, Marie/0000-0001-5454-1492; McMahon, Richard/0000-0001-8447-8869; Hogg, David/0000-0003-2866-9403 NR 157 TC 340 Z9 341 U1 18 U2 53 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 JUL PY 2015 VL 219 IS 1 AR 12 DI 10.1088/0067-0049/219/1/12 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0RE UT WOS:000358858900012 ER PT J AU Bartelink, EJ Sholts, SB Milligan, CF Van Deest, TL Warmlander, SKTS AF Bartelink, Eric J. Sholts, Sabrina B. Milligan, Colleen F. Van Deest, Traci L. Warmlander, Sebastian K. T. S. TI A Case of Contested Cremains Analyzed Through Metric and Chemical Comparison SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; forensic anthropology; cremains; burned bone; X-ray diffraction; scanning electron microscopy ID ELECTRON-MICROSCOPE OBSERVATIONS; X-RAY-DIFFRACTION; ELEMENTAL ANALYSIS; BONE; CREMATION; IDENTIFICATION; SPECTROSCOPY AB Since the 1980s, cremation has become the fastest growing area of the U.S. funeral industry. At the same time, the number of litigations against funeral homes and cremation facilities has increased. Forensic anthropologists are often asked to determine whether the contents of an urn are actually cremated bone, and to address questions regarding the identity of the remains. This study uses both metric and chemical analyses for resolving a case of contested cremains. A cremains weight of 2021.8 g was predicted based on the decedent's reported stature and weight. However, the urn contents weighed 4173.5 g. The urn contents also contained material inconsistent with cremains (e.g., moist sediment, stones, ferrous metal). Analysis using XRD and SEM demonstrated that the urn contained thermally altered bone as well as inorganic material consistent with glass fiber cement. Although forensically challenging, cremains cases such as this one can be resolved using a multidisciplinary approach. C1 [Bartelink, Eric J.; Milligan, Colleen F.] Calif State Univ Chico, Human Identificat Lab, Dept Anthropol, Chico, CA 95929 USA. [Sholts, Sabrina B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Van Deest, Traci L.] Univ Florida, Dept Anthropol, CA Pound Human Identificat Lab, Gainesville, FL 32611 USA. [Warmlander, Sebastian K. T. S.] Stockholm Univ, Dept Biochem & Biophys, S-10691 Stockholm, Sweden. [Warmlander, Sebastian K. T. S.] Linkoping Univ, Div Commercial & Business Law, S-58183 Linkoping, Sweden. RP Warmlander, SKTS (reprint author), Stockholm Univ, Dept Biochem & Biophys, S-10691 Stockholm, Sweden. EM ebartelink@csuchico.edu; seb@dbb.su.se NR 27 TC 0 Z9 0 U1 2 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1198 EI 1556-4029 J9 J FORENSIC SCI JI J. Forensic Sci. PD JUL PY 2015 VL 60 IS 4 BP 1068 EP 1073 DI 10.1111/1556-4029.12734 PG 6 WC Medicine, Legal SC Legal Medicine GA CO6JL UT WOS:000359262900032 PM 25754694 ER PT J AU Solis, MA Metz, MA Scheffer, SJ Lewis, ML Kula, RR Springer, TL AF Solis, M. Alma Metz, M. A. Scheffer, S. J. Lewis, M. L. Kula, R. R. Springer, T. L. TI A New Cryptic Species of Diatraea (Lepidoptera: Crambidae: Crambinae) Feeding on Eastern Gama Grass and a Novel Host Association with a Braconid (Hymenoptera) in the United States SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE southern cornstalk borer; Pyraloidea; corn; sorghum ID PRIMERS; BORER; GAMAGRASS; GROTE AB A new species, Diatraea mitteri Solis, that had been residing cryptically as Diatraea crambidoides (Grote), feeding on eastern gama grass (Tripsacum dactyloides (L.) L., is described. D. crambidoides occurs in the southern United States and Mexico and is an economic pest of corn (Zea mays L.). It has been reported to also feed on sorghum (Sorghum bicolor (L.) Moench), johnsongrass (Sorghum halepense (L.) Persoon), and sugar cane (Saccharum officinarum L.). We confirm that D. crambidoides also feeds on eastern gama grass. Morphological and molecular characters support the status of D. mitteri as a new species. Parsimony analysis resulted in two clades corresponding to D. crambidoides and D. mitteri. We confirm the distribution of D. mitteri from Kansas, Oklahoma, and Texas, but its distribution could be as broad as the remaining range of eastern gama grass in the eastern United States. All the life stages are described and illustrated. A novel host association, Alabagrus imitatus Cresson (Hymenoptera: Braconidae), as a parasitoid of D. mitteri is reported. C1 [Solis, M. Alma; Metz, M. A.; Kula, R. R.] USDA ARS, Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Washington, DC 20560 USA. [Scheffer, S. J.; Lewis, M. L.] USDA ARS, Systemat Entomol Lab, Beltsville, MD 20705 USA. [Springer, T. L.] USDA ARS, Southern Plains Range Res Stn, Woodward, OK 73801 USA. RP Solis, MA (reprint author), USDA ARS, Smithsonian Inst, Natl Museum Nat Hist, Systemat Entomol Lab, Washington, DC 20560 USA. EM alma.solis@ars.usda.gov NR 28 TC 2 Z9 2 U1 3 U2 10 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0013-8746 EI 1938-2901 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD JUL PY 2015 VL 108 IS 4 BP 648 EP 659 DI 10.1093/aesa/sav049 PG 12 WC Entomology SC Entomology GA CN6IH UT WOS:000358537600023 ER PT J AU Chan, CK Psaltis, D Ozel, F Narayan, R Sadowski, A AF Chan, Chi-kwan Psaltis, Dimitrios Oezel, Feryal Narayan, Ramesh Sadowski, Aleksander TI THE POWER OF IMAGING: CONSTRAINING THE PLASMA PROPERTIES OF GRMHD SIMULATIONS USING EHT OBSERVATIONS OF SGR A (vol 799, 1, 2015) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Chan, Chi-kwan; Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Chan, Chi-kwan; Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Sadowski, Aleksander] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Chan, CK (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA. NR 1 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 JUL 1 PY 2015 VL 807 IS 1 AR 114 DI 10.1088/0004-637X/807/1/114 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200114 ER PT J AU Cheung, E Conroy, C Athanassoula, E Bell, EF Bosma, A Cardamone, CN Faber, SM Koo, DC Lintott, C Masters, KL Melvin, T Simmons, B Willett, KW AF Cheung, Edmond Conroy, Charlie Athanassoula, E. Bell, Eric F. Bosma, A. Cardamone, Carolin N. Faber, S. M. Koo, David C. Lintott, Chris Masters, Karen L. Melvin, Thomas Simmons, Brooke Willett, Kyle W. TI STELLAR POPULATIONS OF BARRED QUIESCENT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: stellar content; galaxies: structure ID DIGITAL SKY SURVEY; LINE-STRENGTH INDEXES; SPATIALLY-RESOLVED SPECTROSCOPY; STAR-FORMING GALAXIES; SPIRAL GALAXIES; DISC GALAXIES; SECULAR EVOLUTION; ABUNDANCE GRADIENTS; RADIAL MIGRATION; MORPHOLOGICAL EVOLUTION AB Selecting centrally quiescent galaxies from the Sloan Digital Sky Survey (SDSS) to create high signal-to-noise ratio (greater than or similar to 100 angstrom(-1)) stacked spectra with minimal emission-line contamination, we accurately and precisely model the central stellar populations of barred and unbarred quiescent disk galaxies. By splitting our sample by redshift, we can use the fixed size of the SDSS fiber to model the stellar populations at different radii within galaxies. At 0.02 < z < 0.04, the SDSS fiber radius corresponds to approximate to 1 kpc, which is the typical half-light radii of both classical bulges and disky pseudobulges. Assuming that the SDSS fiber primarily covers the bulges at these redshifts, our analysis shows that there are no significant differences in the stellar populations, i.e., stellar age, [Fe/H], [Mg/Fe], and [N/Fe], of the bulges of barred versus unbarred quiescent disk galaxies. Modeling the stellar populations at different redshift intervals from z = 0.020 to z = 0.085 at fixed stellar masses produces an estimate of the stellar population gradients out to about half the typical effective radius of our sample, assuming null evolution over this approximate to 1 Gyr epoch. We find that there are no noticeable differences in the slopes of the azimuthally averaged gradients of barred versus unbarred quiescent disk galaxies. These results suggest that bars are not a strong influence on the chemical evolution of quiescent disk galaxies. C1 [Cheung, Edmond; Faber, S. M.; Koo, David C.] Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. [Cheung, Edmond] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Athanassoula, E.; Bosma, A.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cardamone, Carolin N.] Wheelock Coll, Dept Sci, Boston, MA 02215 USA. [Faber, S. M.; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Lintott, Chris; Simmons, Brooke] Univ Oxford, Dept Phys, Oxford Astrophys, Oxford OX1 3RH, England. [Lintott, Chris] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Masters, Karen L.; Melvin, Thomas] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Willett, Kyle W.] Univ Minnesota, Sch Phys & Astron, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. RP Cheung, E (reprint author), Univ Tokyo, Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. EM ec2250@gmail.com OI Bell, Eric/0000-0002-5564-9873; Cheung, Edmond/0000-0001-8546-1428; Simmons, Brooke/0000-0001-5882-3323 FU NSF Grant [AST 08-08133, AST-1313280]; NASA grant [NNX13AI46G]; People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/under REA grant [PITN-GA-2011-289313]; CNES (Centre National d'Etudes Spatiales-France); PNCG (Programme National Cosmologie et Galaxies-France); Alfred P. Sloan Foundation; 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; Astrophysical Research Consortium FX Authors from UC Santa Cruz acknowledge financial support from the NSF Grant AST 08-08133. C.C. acknowledges funding from NASA grant NNX13AI46G and NSF grant AST-1313280. E.A. and A.B. acknowledge financial support to the DAGAL network from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme FP7/2007-2013/under REA grant agreement number PITN-GA-2011-289313, from the CNES (Centre National d'Etudes Spatiales-France), and from the PNCG (Programme National Cosmologie et Galaxies-France). 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 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. E.C. deeply thanks Genevieve J. Graves for sharing her stacking code. E.C. also thanks Jieun Choi and Kevin Bundy for useful discussions. We also thank the anonymous referee for a constructive report. The JavaScript Cosmology Calculator (Wright 2006) was used in the preparation of this paper. NR 84 TC 4 Z9 4 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 JUL 1 PY 2015 VL 807 IS 1 AR 36 DI 10.1088/0004-637X/807/1/36 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200036 ER PT J AU Dressing, CD Charbonneau, D AF Dressing, Courtney D. Charbonneau, David TI THE OCCURRENCE OF POTENTIALLY HABITABLE PLANETS ORBITING M DWARFS ESTIMATED FROM THE FULL KEPLER DATASET AND AN EMPIRICAL MEASUREMENT OF THE DETECTION SENSITIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; methods: data analysis; planetary systems; stars: low-mass; surveys; techniques: photometric ID MAIN-SEQUENCE STARS; EARTH-LIKE PLANETS; SOLAR-TYPE STARS; R-CIRCLE-PLUS; LIGHT CURVES; TERRESTRIAL PLANETS; CANDIDATE PLANETS; TRANSIT DETECTION; ERROR-CORRECTION; HOST-STARS AB We present an improved estimate of the occurrence rate of small planets orbiting small stars by searching the full four-year Kepler data set for transiting planets using our own planet detection pipeline and conducting transit injection and recovery simulations to empirically measure the search completeness of our pipeline. We identified 156 planet candidates, including one object that was not previously identified as a Kepler Object of Interest. We inspected all publicly available follow-up images, observing notes, and centroid analyses, and corrected for the likelihood of false positives. We evaluated the sensitivity of our detection pipeline on a star-by-star basis by injecting 2000 transit signals into the light curve of each target star. For periods shorter than 50 days, we find 0.56(-0.05)(+0.06) Earth-size planets (1-1.5 R-circle plus) and 0.46(-0.05)(+0.07) super-Earths (1.5-2 R-circle plus) per M dwarf. In total, we estimate a cumulative planet occurrence rate of 2.5 +/- 0.2 planets per M dwarf with radii 1-4 R-circle plus and periods shorter than 200 days. Within a conservatively defined habitable zone (HZ) based on the moist greenhouse inner limit and maximum greenhouse outer limit, we estimate an occurrence rate of 0.16(-0.07)(+0.17) Earth-size planets and 0.12(-0.05)(+0.10) super-Earths per M dwarf HZ. Adopting the broader insolation boundaries of the recent Venus and early Mars limits yields a higher estimate of 0.24(-0.08)(+0.18) Earth-size planets and 0.21(-0.06)(+0.11) super-Earths per M dwarf HZ. This suggests that the nearest potentially habitable non-transiting and transiting Earth-size planets are 2.6 +/- 0.4 pc and 10.6(-1.8)(+1.6) pc away, respectively. If we include super-Earths, these distances diminish to 2.1 +/- 0.2 pc and 8.6(-0.8)(+0.7) pc. C1 [Dressing, Courtney D.; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dressing, CD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cdressing@cfa.harvard.edu FU National Science Foundation Graduate Research Fellowship; NASA Kepler Mission Participating Scientist Program [NNX09AB53G, NNX12AC77G]; John Templeton Foundation; NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; National Aeronautics and Space Administration FX C.D. is supported by a National Science Foundation Graduate Research Fellowship. Support for this work was provided through the NASA Kepler Mission Participating Scientist Program grants NNX09AB53G and NNX12AC77G, which were awarded to D.C. This publication was made possible through the support of 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. We thank the anonymous referee for providing feedback that improved the quality of this paper and the Kepler team for providing the community with a fantastic collection of data. We are grateful to Jonathan Irwin for sharing a fast implementation of the transit model (Mandel & Agol 2002) and for providing valuable advice. We thank Jessie Christiansen for answering questions about the Kepler pipeline completeness and providing helpful suggestions. Funding for the Kepler mission is provided by the NASA Science Mission directorate. This publication made use of the Kepler Community Follow-Up Observing Program website (https://cfop.ipac.caltech.edu), the NASA Exoplanet Archive, and the Mikulski Archive for Space Telescopes (MAST). The NASA Exoplanet Archive is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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. NR 110 TC 89 Z9 90 U1 10 U2 18 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 JUL 1 PY 2015 VL 807 IS 1 AR 45 DI 10.1088/0004-637X/807/1/45 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200045 ER PT J AU Ferraz-Mello, S Dos Santos, MT Folonier, H Czismadia, S Do Nascimento, JD Patzold, M AF Ferraz-Mello, S. Dos Santos, M. Tadeu Folonier, H. Czismadia, Sz. Do Nascimento, J. -D., Jr. Paetzold, M. TI INTERPLAY OF TIDAL EVOLUTION AND STELLAR WIND BRAKING IN THE ROTATION OF STARS HOSTING MASSIVE CLOSE-IN PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; planet-star interactions; planetary systems; planets and satellites: dynamical evolution and stability; stars: rotation ID ANGULAR-MOMENTUM EVOLUTION; COROT SPACE MISSION; SUN-LIKE STARS; TRANSITING EXOPLANETS; HOT JUPITERS; SHORT-PERIOD; M-DWARFS; SYSTEMS; KEPLER; ORBIT AB This paper deals with the application of the creep tide theory (Ferraz-Mello) to the study of the rotation of stars hosting massive close-in planets. The stars have nearly the same tidal relaxation factors as gaseous planets and the evolution of their rotation is similar to that of close-in hot Jupiters: they tidally evolve toward a stationary solution. However, stellar rotation may also be affected by stellar wind braking. Thus, while the rotation of a quiet host star evolves toward a stationary attractor with a frequency (1+6e(2)) times the orbital mean motion of the companion, the continuous loss of angular momentum in an active star displaces the stationary solution toward slower values: active host stars with big close-in companions tend to have rotational periods longer than the orbital periods of their companions. The study of some hypothetical examples shows that, because of tidal evolution, the rules of gyrochronology cannot be used to estimate the age of one system with a large close-in companion, no matter if the star is quiet or active, if the current semimajor axis of the companion is smaller than 0.03-0.04 AU. Details on the evolution of the systems: CoRoT LRc06E21637, CoRoT-27, Kepler-75, CoRoT-2, CoRoT-18, CoRoT-14 and on hypothetical systems with planets of mass 1-4 M-Jup in orbit around a star similar to the Sun are given. C1 [Ferraz-Mello, S.; Dos Santos, M. Tadeu; Folonier, H.] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil. [Czismadia, Sz.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetenforsch, D-12489 Berlin, Germany. [Do Nascimento, J. -D., Jr.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Do Nascimento, J. -D., Jr.] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil. [Paetzold, M.] Univ Cologne, Rhein Inst Umweltforsch, D-50931 Cologne, Germany. RP Ferraz-Mello, S (reprint author), Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo, SP, Brazil. EM sylvio@iag.usp.br RI do Nascimento, Jose Dias/D-2416-2014; OI do Nascimento, Jose Dias/0000-0001-7804-2145; Ferraz-Mello, Sylvio/0000-0002-9603-2415 FU INCT Inespaco [FAPESP 2008/57866-1, CNPq 574004/2008-4]; [CNPq 306146/2010-0]; [FAPESP 2011/52096-6] FX The CoRoT space mission has been developed and operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA, Germany, and Spain. This investigation was supported by grants CNPq 306146/2010-0, FAPESP 2011/52096-6 and by INCT Inespaco procs. FAPESP 2008/57866-1 and CNPq 574004/2008-4. The help of Mr. E.S. Pereira in the calculation of some complementary examples is acknowledged. NR 53 TC 11 Z9 11 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 JUL 1 PY 2015 VL 807 IS 1 AR 78 DI 10.1088/0004-637X/807/1/78 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200078 ER PT J AU Gelfand, JD Slane, PO Temim, T AF Gelfand, Joseph D. Slane, Patrick O. Temim, Tea TI THE PROPERTIES OF THE PROGENITOR SUPERNOVA, PULSAR WIND, AND NEUTRON STAR INSIDE PWN G54.1+0.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (PWN G54.1+0.3); ISM: supernova remnants; pulsars: individual (PSR J1930+1852); X-rays: individual (PWN G54.1+0.3) ID RELATIVISTIC COLLISIONLESS SHOCKS; PAIR PRODUCTION MULTIPLICITIES; GALACTIC ABUNDANCE GRADIENT; REMNANT G54.1+0.3; NEBULA G54.1+0.3; CRAB-NEBULA; SPECTRAL EVOLUTION; ACCRETION SHOCK; RADIO-EMISSION; SIGMA-PROBLEM AB The evolution of a pulsar wind nebula (PWN) inside a supernova remnant (SNR) is sensitive to the properties of the central neutron star, pulsar wind, progenitor supernova, and interstellar medium. These properties are both difficult to measure directly and critical for understanding the formation of neutron stars and their interaction with the surrounding medium. In this paper, we determine these properties for PWN G54.1+0.3 by fitting its observed properties with a model for the dynamical and radiative evolution of a PWN inside an SNR. Our modeling suggests that the progenitor of G54.1+0.3 was an isolated similar to 15-20 M-circle dot star which exploded inside a massive star cluster, creating a neutron star initially spinning with a period of P-0 similar to 30-80 ms. We also find that greater than or similar to 99.9% of the pulsar's rotational energy is injected into the PWN as relativistic electrons and positrons whose energy spectrum is well characterized by a broken power law. Finally, we propose future observations which can both test the validity of this model and better determine the properties of this source-in particular, its distance and the initial spin period of the central pulsar. C1 [Gelfand, Joseph D.] NYU Abu Dhabi, New York, NY 10276 USA. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Temim, Tea] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Gelfand, Joseph D.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Temim, Tea] Oak Ridge Associated Univ, Oak Ridge, TN 37831 USA. RP Gelfand, JD (reprint author), NYU Abu Dhabi, POB 903, New York, NY 10276 USA. EM jg168@nyu.edu OI Gelfand, Joseph/0000-0003-4679-1058; Temim, Tea/0000-0001-7380-3144 FU NASA [RSA 1479542] FX Support for this work was provided by NASA through an award issued by JPL/Caltech (RSA 1479542). J.D.G. will like to thank Erin Sheldon for the IDL code used in the MCMC fits, Kaisey Mandel and David Hogg for useful discussions concerning MCMC fitting, Ester Aliu for information regarding the GeV spectrum, and Roger Chevalier, Vikram Dwarkadas, Daniel Patnaude, and Lorenzo Sironi for useful advice. NR 56 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 JUL 1 PY 2015 VL 807 IS 1 AR 30 DI 10.1088/0004-637X/807/1/30 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200030 ER PT J AU Hayashida, M Nalewajko, K Madejski, GM Sikora, M Itoh, R Ajello, M Blandford, RD Buson, S Chiang, J Fukazawa, Y Furniss, AK Urry, CM Hasan, I Harrison, FA Alexander, DM Balokovic, M Barret, D Boggs, SE Christensen, FE Craig, WW Forster, K Giommi, P Grefenstette, B Hailey, C Hornstrup, A Kitaguchi, T Koglin, JE Madsen, KK Mao, PH Miyasaka, H Mori, K Perri, M Pivovaroff, MJ Puccetti, S Rana, V Stern, D Tagliaferri, G Westergaard, NJ Zhang, WW Zoglauer, A Gurwell, MA Uemura, M Akitaya, H Kawabata, KS Kawaguchi, K Kanda, Y Moritani, Y Takaki, K Ui, T Yoshida, M Agarwal, A Gupta, AC AF Hayashida, M. Nalewajko, K. Madejski, G. M. Sikora, M. Itoh, R. Ajello, M. Blandford, R. D. Buson, S. Chiang, J. Fukazawa, Y. Furniss, A. K. Urry, C. M. Hasan, I. Harrison, F. A. Alexander, D. M. Balokovic, M. Barret, D. Boggs, S. E. Christensen, F. E. Craig, W. W. Forster, K. Giommi, P. Grefenstette, B. Hailey, C. Hornstrup, A. Kitaguchi, T. Koglin, J. E. Madsen, K. K. Mao, P. H. Miyasaka, H. Mori, K. Perri, M. Pivovaroff, M. J. Puccetti, S. Rana, V. Stern, D. Tagliaferri, G. Westergaard, N. J. Zhang, W. W. Zoglauer, A. Gurwell, M. A. Uemura, M. Akitaya, H. Kawabata, K. S. Kawaguchi, K. Kanda, Y. Moritani, Y. Takaki, K. Ui, T. Yoshida, M. Agarwal, A. Gupta, A. C. TI RAPID VARIABILITY OF BLAZAR 3C 279 DURING FLARING STATES IN 2013-2014 WITH JOINT FERMI-LAT, NuSTAR, SWIFT, AND GROUND-BASED MULTI-WAVELENGTH OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (3C 279); radiation mechanisms: non-thermal; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; EXTRAGALACTIC RADIO-SOURCES; ENERGY GAMMA-RADIATION; LUMINOUS BLAZARS; PKS 1510-089; MAGNETIC RECONNECTION; RELATIVISTIC JET; BRIGHT BLAZARS; QUASAR 3C-279 AB We report the results of a multiband observing campaign on the famous blazar 3C 279 conducted during a phase of increased activity from 2013 December to 2014 April, including first observations of it with NuSTAR. The gamma-ray emission of the source measured by Fermi-LAT showed multiple distinct flares reaching the highest flux level measured in this object since the beginning of the Fermi mission, with F(E > 100 MeV) of 10(-5) photons cm(-2) s(-1), and with a flux-doubling time scale as short as 2 hr. The gamma-ray spectrum during one of the flares was very hard, with an index of Gamma(gamma) = 1.7 +/- 0.1, which is rarely seen in flat-spectrum radio quasars. The lack of concurrent optical variability implies a very high Compton dominance parameter L-gamma/L-syn > 300. Two 1 day NuSTAR observations with accompanying Swift pointings were separated by 2 weeks, probing different levels of source activity. While the 0.5 - 70 keV X-ray spectrum obtained during the first pointing, and fitted jointly with Swift-XRT is well-described by a simple power law, the second joint observation showed an unusual spectral structure: the spectrum softens by Delta Gamma(X) similar or equal to 0.4 at similar to 4 keV. Modeling the broadband spectral energy distribution during this flare with the standard synchrotron plus inverse-Compton model requires: (1) the location of the gamma-ray emitting region is comparable with the broad-line region radius, (2) a very hard electron energy distribution index p similar or equal to 1, (3) total jet power significantly exceeding the accretion-disk luminosity L-j/L-d greater than or similar to 10, and (4) extremely low jet magnetization with L-B/L-j less than or similar to 10(-4). We also find that single-zone models that match the observed gamma-ray and optical spectra cannot satisfactorily explain the production of X-ray emission. C1 [Hayashida, M.] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. [Nalewajko, K.; Madejski, G. M.; Blandford, R. D.; Chiang, J.; Furniss, A. K.; Koglin, J. E.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Nalewajko, K.; Madejski, G. M.; Blandford, R. D.; Chiang, J.; Furniss, A. K.; Koglin, J. E.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Itoh, R.; Fukazawa, Y.; Kawaguchi, K.; Kanda, Y.; Takaki, K.; Ui, T.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Ajello, M.] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA. [Buson, S.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Buson, S.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Urry, C. M.; Hasan, I.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06520 USA. [Harrison, F. A.; Balokovic, M.; Forster, K.; Grefenstette, B.; Madsen, K. K.; Mao, P. H.; Miyasaka, H.; Rana, V.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Barret, D.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Barret, D.; Craig, W. W.] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Boggs, S. E.; Zoglauer, A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.; Hornstrup, A.; Westergaard, N. J.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, W. W.; Pivovaroff, M. J.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Giommi, P.; Perri, M.; Puccetti, S.] ASI Sci Data Ctr, D-52425 Rome, Italy. [Hailey, C.; Mori, K.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kitaguchi, T.] Hiroshima Univ, Grad Sch Sci, Core Res Energet Universe, Higashihiroshima, Hiroshima 7398526, Japan. [Perri, M.; Puccetti, S.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tagliaferri, G.] INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Uemura, M.; Akitaya, H.; Kawabata, K. S.; Moritani, Y.; Yoshida, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Agarwal, A.; Gupta, A. C.] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263002, India. RP Hayashida, M (reprint author), Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan. EM mahaya@icrr.u-tokyo.ac.jp; knalew@stanford.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Perri, Matteo/0000-0003-3613-4409; giommi, paolo/0000-0002-2265-5003; Puccetti, Simonetta/0000-0002-2734-7835; Rana, Vikram/0000-0003-1703-8796; Urry, Meg/0000-0002-0745-9792; Ajello, Marco/0000-0002-6584-1703 FU NASA [NNG08FD60C, NAS8-03060]; NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF3-140130]; NASA Headquarters under the NASA earth and Space Science Fellowship Program [NNX14AQ07H]; Smithsonian Institution; Academia Sinica FX This work was partially supported under the NASA contract no. NNG08FD60C, and made use of observations from the NuSTAR mission, a project led by California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software, and Calibration teams for support of 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). This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. 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.; K.N. was supported by NASA through Einstein Postdoctoral Fellowship grant number PF3-140130 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. M.B. acknowledges support from NASA Headquarters under the NASA earth and Space Science Fellowship Program, grant NNX14AQ07H. NR 81 TC 33 Z9 33 U1 0 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 JUL 1 PY 2015 VL 807 IS 1 AR 79 DI 10.1088/0004-637X/807/1/79 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200079 ER PT J AU Maeda, K Hattori, T Milisavljevic, D Folatelli, G Drout, MR Kuncarayakti, H Margutti, R Kamble, A Soderberg, A Tanaka, M Kawabata, M Kawabata, KS Yamanaka, M Nomoto, K Kim, JH Simon, JD Phillips, MM Parrent, J Nakaoka, T Moriya, TJ Suzuki, A Takaki, K Ishigaki, M Sakon, I Tajitsu, A Iye, M AF Maeda, K. Hattori, T. Milisavljevic, D. Folatelli, G. Drout, M. R. Kuncarayakti, H. Margutti, R. Kamble, A. Soderberg, A. Tanaka, M. Kawabata, M. Kawabata, K. S. Yamanaka, M. Nomoto, K. Kim, J. H. Simon, J. D. Phillips, M. M. Parrent, J. Nakaoka, T. Moriya, T. J. Suzuki, A. Takaki, K. Ishigaki, M. Sakon, I. Tajitsu, A. Iye, M. TI TYPE IIb SUPERNOVA 2013df ENTERING INTO AN INTERACTION PHASE: A LINK BETWEEN THE PROGENITOR AND THE MASS LOSS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: mass-loss; supernovae: individual (SN 1993J, SN 2011dh, SN 2013df) ID CORE-COLLAPSE SUPERNOVAE; X-RAY-EMISSION; SN 1993J; SUPERGIANT PROGENITOR; COMPACT PROGENITOR; BINARY COMPANION; STANDARD STARS; IA SUPERNOVAE; NEUTRON-STAR; LIGHT-CURVE AB We report the late-time evolution of Type IIb supernova (SN IIb) 2013df. SN 2013df showed a dramatic change in its spectral features at similar to 1 yr after the explosion. Early on it showed typical characteristics shared by SNe IIb/Ib/Ic dominated by metal emission lines, while later on it was dominated by broad and flat-topped Ha and He I emissions. The late-time spectra are strikingly similar to SN IIb 1993J, which is the only previous example clearly showing the same transition. This late-time evolution is fully explained by a change in the energy input from the Co-56 decay to the interaction between the SN ejecta and dense circumstellar matter (CSM). The mass-loss rate is derived to be similar to(5.4 +/- 3.2) x 10(-5) M(circle dot)yr(-1) (for the wind velocity of similar to 20 km s(-1)), similar to SN 1993J but larger than SN IIb 2011dh by an order of magnitude. The striking similarity between SNe IIb 2013df and 1993J in the (candidate) progenitors and the CSM environments. and the contrast in these natures to SN 2011dh. infer that there is a link between the natures of the progenitor and the mass loss: SNe IIb with a more extended progenitor have experienced a much stronger mass loss in the final centuries toward the explosion. It might indicate that SNe IIb from a more extended progenitor are the explosions during a strong binary interaction phase, while those from a less extended progenitor have a delay between the strong binary interaction and the explosion. C1 [Maeda, K.; Suzuki, A.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Maeda, K.; Folatelli, G.; Nomoto, K.; Ishigaki, M.] Univ Tokyo, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. [Hattori, T.; Kim, J. H.; Tajitsu, A.] Subaru Telescope, Natl Astron Observ Japan, Hilo, HI 96720 USA. [Milisavljevic, D.; Drout, M. R.; Margutti, R.; Kamble, A.; Soderberg, A.; Parrent, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Folatelli, G.] Consejo Nacl Invest Cient & Tecn, Inst Astrofis La Plata, La Plata, Buenos Aires, Argentina. [Kuncarayakti, H.] Millennium Inst Astrophys, Santiago, Chile. [Kuncarayakti, H.] Univ Chile, Dept Astron, Santiago, Chile. [Tanaka, M.; Iye, M.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Kawabata, M.; Kawabata, K. S.; Nakaoka, T.; Takaki, K.] Hiroshima Univ, Dept Phys Sci, Kagamiyama, Higashi Hiroshi 7398526, Japan. [Kawabata, K. S.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Yamanaka, M.] Konan Univ, Fac Sci & Engn, Dept Phys, Kobe, Hyogo 6588501, Japan. [Yamanaka, M.] Kyoto Univ, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan. [Simon, J. D.] Carnegie Inst Sci, Observ, Pasadena, CA 91101 USA. [Phillips, M. M.] Las Campanas Observ, Carnegie Observat, La Serena 601, Chile. [Moriya, T. J.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Sakon, I.] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. RP Maeda, K (reprint author), Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake cho, Kyoto 6068502, Japan. EM keiichi.maeda@kusastro.kyoto-u.ac.jp RI Kim, Ji Hoon/A-8989-2009; OI Kim, Ji Hoon/0000-0002-1418-3309; Margutti, Raffaella/0000-0003-4768-7586 FU JSPS [26800100, 15H02075, 15H00788, 23224004, 26400222]; WPI Initiative, MEXT, Japan; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC120009]; CONICYT through FONDECYT grant [3140563] FX The authors thank the staff at the Subaru Telescope for their excellent support in the observations. The authors thank Takaya Nozawa for his constructive comments on the manuscript. The work by K.M. is supported by the JSPS Grant-in-Aid for Scientific Research (No. 26800100) and by the WPI Initiative, MEXT, Japan. Support for H.K. is provided by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. H.K. acknowledges support by CONICYT through FONDECYT grant 3140563. The work by M.T. is supported by JSPS Grant-in-Aid for Scientific Research (15H02075, 15H00788). The work by K.N. is supported by the JSPS Grant-in-aid for Scientific Research (No. 23224004 and 26400222). NR 66 TC 8 Z9 8 U1 0 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 JUL 1 PY 2015 VL 807 IS 1 AR 35 DI 10.1088/0004-637X/807/1/35 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200035 ER PT J AU Reeves, KK McCauley, PI Tian, H AF Reeves, Katharine K. McCauley, Patrick I. Tian, Hui TI DIRECT OBSERVATIONS OF MAGNETIC RECONNECTION OUTFLOW AND CME TRIGGERING IN A SMALL ERUPTING SOLAR PROMINENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; Sun: activity; Sun: coronal mass ejections (CMEs); Sun: filaments, prominences ID CORONAL MASS EJECTIONS; X-RAY TELESCOPE; 2010 NOVEMBER 3; SUPRA-ARCADE DOWNFLOWS; FLUX ROPE; ACCELERATED ELECTRONS; EXTREME-ULTRAVIOLET; CONDUCTION FRONTS; CURRENT SHEETS; SLOW-RISE AB We examine a small prominence eruption that occurred on 2014 May 1 at 01: 35 UT and was observed by the Interface Region Imaging Spectrometer (IRIS) and the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory. Pre- and post-eruption images were taken by the X-ray Telescope (XRT) on Hinode. Pre-eruption, a dome-like structure exists above the prominence, as demarcated by coronal rain. As the eruption progresses, we find evidence for reconnection between the prominence magnetic field and the overlying field. Fast flows are seen in AIA and IRIS, indicating reconnection outflows. Plane-of-sky flows of 300 km s(-1) are observed in the AIA 171 A channel along a potentially reconnected field line. IRIS detects intermittent fast line of sight flows of 200 km s(-1) coincident with the AIA flows. Differential emission measure calculations show heating at the origin of the fast flows. Post-eruption XRT images show hot loops probably due to reconfiguration of magnetic fields during the eruption and subsequent heating of plasma in these loops. Although there is evidence for reconnection above the prominence during the eruption, high spatial resolution images from IRIS reveal potential reconnection sites below the prominence. A height-time analysis of the erupting prominence shows a slow initial rise with a velocity of 0.4 km s(-1) followed by a rapid acceleration with a final velocity of 250 km s(-1). Brightenings in IRIS during the transition between these two phases indicate the eruption trigger for the fast part of the eruption is likely a tethercutting mechanism rather than a break-out mechanism. C1 [Reeves, Katharine K.; McCauley, Patrick I.; Tian, Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reeves, KK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 58, Cambridge, MA 02138 USA. EM kreeves@cfa.harvard.edu RI McCauley, Patrick/P-7747-2015; OI McCauley, Patrick/0000-0002-1450-7350; Reeves, Katharine/0000-0002-6903-6832 FU Lockheed-Martin [8100002705, SP02H1701R]; NASA [NNM07AB07C, NNX12AI30G]; Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract FX The authors would like to thank the anonymous referee for thoughtful comments that improved this paper, and Patrick Antolin, Ed DeLuca, Wei Liu, Nick Murphy, and Xudong Sun for helpful discussions. This work is partially supported by contracts 8100002705 and SP02H1701R from Lockheed-Martin to SAO and contract NNM07AB07C from NASA to SAO. K.R. and P.M. also acknowledge support from NASA grant NNX12AI30G 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. 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 co-operation with ESA and NSC (Norway). This work has benefited from the use of NASA's Astrophysics Data System. NR 81 TC 7 Z9 7 U1 1 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 JUL 1 PY 2015 VL 807 IS 1 AR 7 DI 10.1088/0004-637X/807/1/7 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200007 ER PT J AU Roettenbacher, RM Monnier, JD Henry, GW Fekel, FC Williamson, MH Pourbaix, D Latham, DW Latham, CA Torres, G Baron, F Che, X Kraus, S Schaefer, GH Aarnio, AN Korhonen, H Harmon, RO ten Brummelaar, TA Sturmann, J Sturmann, L Turner, NH AF Roettenbacher, Rachael M. Monnier, John D. Henry, Gregory W. Fekel, Francis C. Williamson, Michael H. Pourbaix, Dimitri Latham, David W. Latham, Christian A. Torres, Guillermo Baron, Fabien Che, Xiao Kraus, Stefan Schaefer, Gail H. Aarnio, Alicia N. Korhonen, Heidi Harmon, Robert O. ten Brummelaar, Theo A. Sturmann, Judit Sturmann, Laszlo Turner, Nils H. TI DETECTING THE COMPANIONS AND ELLIPSOIDAL VARIATIONS OF RS CVn PRIMARIES. I. sigma GEMINORUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: activity; stars: imaging; stars: individual (sigma Geminorum); stars: variables: general ID SPECTROSCOPIC BINARIES; ACTIVE LONGITUDES; ASTROMETRIC BINARIES; VELOCITY VARIATION; MODEL ATMOSPHERES; LAMBDA-ANDROMEDAE; RADIAL-VELOCITIES; COOL GIANTS; CHARA ARRAY; II-PEGASI AB To measure the properties of both components of the RS Canum Venaticorum binary sigma Geminorum (sigma Gem), we directly detect the faint companion, measure the orbit, obtain model-independent masses and evolutionary histories, detect ellipsoidal variations of the primary caused by the gravity of the companion, and measure gravity darkening. We detect the companion with interferometric observations obtained with the Michigan InfraRed Combiner at Georgia State University's Center for High Angular Resolution Astronomy Array with a primary-to-secondary H-band flux ratio of 270 +/- 70. A radial velocity curve of the companion was obtained with spectra from the Tillinghast Reflector Echelle Spectrograph on the 1.5 m Tillinghast Reflector at Fred Lawrence Whipple Observatory. We additionally use new observations from the Tennessee State University Automated Spectroscopic and Photometric Telescopes ( AST and APT, respectively). From our orbit, we determine model-independent masses of the components (M-1 = 1.28 +/- 0.07 M-circle dot, M-2 = 0.73 +/- 0.03 M-circle dot), and estimate a system age of 5 -/+ 1 Gyr. An average of the 27 year APT light curve of s. Gem folded over the orbital period (P = 19.6027 +/- 0.0005 days) reveals a quasi-sinusoidal signature, which has previously been attributed to active longitudes 180 degrees apart on the surface of s Gem. With the component masses, diameters, and orbit, we find that the predicted light curve for ellipsoidal variations due to the primary star partially filling its Roche lobe potential matches well with the observed average light curve, offering a compelling alternative explanation to the active longitudes hypothesis. Measuring gravity darkening from the light curve gives beta < 0.1, a value slightly lower than that expected from recent theory. C1 [Roettenbacher, Rachael M.; Monnier, John D.; Baron, Fabien; Che, Xiao; Aarnio, Alicia N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Henry, Gregory W.; Fekel, Francis C.; Williamson, Michael H.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Pourbaix, Dimitri] Univ Libre Bruxelles, Inst Astron & Astrophys, FNRS, Brussels, Belgium. [Latham, David W.; Latham, Christian A.; Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kraus, Stefan] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Schaefer, Gail H.; ten Brummelaar, Theo A.; Sturmann, Judit; Sturmann, Laszlo; Turner, Nils H.] Georgia State Univ, Ctr High Angular Resolut Astron, Mt Wilson, CA 91023 USA. [Korhonen, Heidi] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Harmon, Robert O.] Ohio Wesleyan Univ, Dept Phys & Astron, Delaware, OH 43015 USA. RP Roettenbacher, RM (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. EM rmroett@umich.edu RI Korhonen, Heidi/E-3065-2016 OI Korhonen, Heidi/0000-0003-0529-1161 FU National Science Foundation through NSF [AST-0908253, AST-1211129]; Georgia State University through the College of Arts and Sciences; University of Michigan; NASA; Tennessee State University; State of Tennessee through its Centers of Excellence program; Rackham Graduate Student Research Grant from the University of Michigan; NSF [AST-1108963, AST-1311698]; STFC Rutherford Fellowship [ST/J004030/1]; NASA Harriet G. Jenkins Pre-Doctoral Fellowship FX We thank H.A. McAlister, J.A. Orosz, M. Reynolds, and M. Rieutord for their helpful comments and discussions. The authors also thank Lou Boyd of the Fairborn Observatory for the decades of crucial support he has given to our photometric program. The interferometric data in this paper were obtained at the CHARA Array, funded by the National Science Foundation through NSF grants AST-0908253 and AST-1211129, and by Georgia State University through the College of Arts and Sciences. The MIRC instrument at the CHARA Array was funded by the University of Michigan. The photometric data were supported by NASA, NSF, Tennessee State University, and the State of Tennessee through its Centers of Excellence program. R.M.R. would like to acknowledge support from the NASA Harriet G. Jenkins Pre-Doctoral Fellowship and a Rackham Graduate Student Research Grant from the University of Michigan. J.D.M. and R.M.R. acknowledge support from NSF grant AST-1108963. A.N.A. and J.D.M. acknowledge the support of NSF AST-1311698. S.K. acknowledges support from an STFC Rutherford Fellowship (ST/J004030/1). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the Jean-Marie Mariotti Center SearchCal service9 co-developped by FIZEAU and LAOG/IPAG, and of CDS Astronomical Databases SIMBAD and VIZIER.10 NR 65 TC 6 Z9 6 U1 0 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 JUL 1 PY 2015 VL 807 IS 1 AR 23 DI 10.1088/0004-637X/807/1/23 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200023 ER PT J AU Schwartz, P Jejcic, S Heinzel, P Anzer, U Jibben, PR AF Schwartz, P. Jejcic, S. Heinzel, P. Anzer, U. Jibben, P. R. TI PROMINENCE VISIBILITY IN HINODE/XRT IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: observational; Sun: corona; Sun: filaments, prominences; Sun: X-rays; gamma rays techniques: imaging spectroscopy ID X-RAY TELESCOPE; QUIESCENT PROMINENCE; ATOMIC DATABASE; MISSION; TRACE; ATMOSPHERES; ABSORPTION; CHIANTI; LINES; SOHO AB In this paper we study the soft X-ray. (SXR) signatures of one particular prominence. The X-ray observations used here were made by the Hinode/X-Ray Telescope instrument using two different filters. Both of them have a pronounced peak of the response function around 10 angstrom. One of them has a secondary smaller peak around 170 angstrom, which leads to a contamination of SXR images. The observed darkening in both of these filters has a very large vertical extension. The position and shape of the darkening correspond. nicely with the prominence structure seen in SDO/AIA images. First, we have investigated the possibility that the darkening is caused by X-ray absorption. However, detailed calculations of the optical thickness in this spectral range show clearly that this effect is completely negligible. Therefore, the alternative is the presence of an extended region with a large emissivity deficit, which can be caused by the presence of cool prominence plasmas within an otherwise hot corona. To reproduce the observed darkening, one needs a very large extension along the line. of. sight of the region amounting to around 105 km. We interpret this region as the prominence spine, which is also consistent with SDO/AIA observations in EUV. C1 [Schwartz, P.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Jejcic, S.] Univ Ljubljana, Fac Math & Phys, Ljubljana 1000, Slovenia. [Heinzel, P.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic. [Anzer, U.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Jibben, P. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schwartz, P (reprint author), Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. EM pschwartz@astro.sk RI Heinzel, Petr/G-9014-2014 FU Grant Agency of the Czech Republic [P209/12/0906]; Science Grant Agency [VEGA 2/0108/12]; Slovak Research and Development Agency [APVV-0816-11]; [RVO: 67985815] FX P.S. and P.H. acknowledge the support from grant P209/12/0906 of the Grant Agency of the Czech Republic. Work of P.S. and P.H. was supported by the project RVO: 67985815. Work of P.S. was also supported by the grant project VEGA 2/0108/12 of the Science Grant Agency. P.S. acknowledges support from the Slovak Research and Development Agency under the contract No. APVV-0816-11. S.J. and P.H. acknowledge the hospitality of the Astronomical Institute of the Slovak Academy of Sciences and University of Ljubljana during the course of this investigation. We are thankful to E.E. DeLuca for useful discussions concerning the XRT observations used in this work. The AIA data are courtesy of NASA/SDO and the AIA science team. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), and the University of Cambridge (UK). NR 32 TC 1 Z9 1 U1 0 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 JUL 1 PY 2015 VL 807 IS 1 AR 97 DI 10.1088/0004-637X/807/1/97 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200097 ER PT J AU Ting, YS Conroy, C Goodman, A AF Ting, Yuan-Sen Conroy, Charlie Goodman, Alyssa TI PROSPECTS FOR CHEMICALLY TAGGING STARS IN THE GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: abundances; Galaxy: disk; Galaxy: evolution; Galaxy: formation; ISM: abundances; stars: abundances ID HORIZONTAL-BRANCH STARS; INITIAL MASS FUNCTION; DWARF SPHEROIDAL GALAXY; MILKY-WAY; ELEMENTAL ABUNDANCE; FORMATION HISTORY; RADIAL MIGRATION; GALACTIC DISK; STELLAR POPULATIONS; SOLAR NEIGHBORHOOD AB It is now well-established that the elemental abundance patterns of stars hold key clues not only to their formation, but also to the assembly histories of galaxies. One of the most exciting possibilities is the use of stellar abundance patterns as "chemical tags" to identify stars that were born in the same molecular cloud. In this paper, we assess the prospects of chemical tagging as a function of several key underlying parameters. We show that in the fiducial case of 10(4) distinct cells in chemical space and 10(5)-10(6) stars in the survey, one can expect to detect similar to 10(2)-10(3) groups that are >= 5 sigma overdensities in the chemical space. However, we find that even very large overdensities in chemical space do not guarantee that the overdensity is due to a single set of stars from a common birth cloud. In fact, for our fiducial model parameters, the typical 5 sigma overdensity is comprised of stars from a wide range of clusters with the most dominant cluster contributing only 25% of the stars. The most important factors limiting the identification of disrupted clusters via chemical tagging are the number of chemical cells in the chemical space and the survey sampling rate of the underlying stellar population. Both of these factors can be improved through strategic observational plans. While recovering individual clusters through chemical tagging may prove challenging, we show, in agreement with previous work, that different CMFs imprint different degrees of clumpiness in chemical space. These differences provide the opportunity to statistically reconstruct the slope and high-mass cutoff of CMF and its evolution through cosmic time. C1 [Ting, Yuan-Sen; Conroy, Charlie; Goodman, Alyssa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ting, YS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Goodman, Alyssa/A-6007-2010; OI Goodman, Alyssa/0000-0003-1312-0477; Ting, Yuan-Sen/0000-0001-5082-9536 FU FAS Division of Science, Research Computing Group at Harvard University FX The authors thank Joss Bland-Hawthorn, Ken Freeman, Sanjib Sharma, Charlie Lada, and Eve Ostriker for helpful discussions, and Andrea Schruba and Peter Behroozi for sharing their data in electronic format. 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 98 TC 6 Z9 6 U1 1 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 JUL 1 PY 2015 VL 807 IS 1 AR 104 DI 10.1088/0004-637X/807/1/104 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200104 ER PT J AU Torres, G Claret, A Pavlovski, K Dotter, A AF Torres, Guillermo Claret, Antonio Pavlovski, Kresimir Dotter, Aaron TI CAPELLA (alpha AURIGAE) REVISITED: NEW BINARY ORBIT, PHYSICAL PROPERTIES, AND EVOLUTIONARY STATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; binaries: spectroscopic; stars: abundances; stars: evolution; stars: fundamental parameters; stars: individual (Capella) ID LOW-MASS STARS; RADIAL-VELOCITY MEASUREMENTS; STELLAR ASTROPHYSICS MESA; SPECTROSCOPIC SURVEY; RED GIANTS; CHROMOSPHERIC ACTIVITY; BOLOMETRIC CORRECTIONS; COMPONENT SPECTRA; MODEL ATMOSPHERE; ACCURATE MASSES AB Knowledge of the chemical composition and absolute masses of Capella are key to understanding the evolutionary state of this benchmark binary system comprising two giant stars. Previous efforts, including our own 2009 study, have largely failed to reach an acceptable agreement between the observations and current stellar evolution models, preventing us from assessing the status of the primary. Here we report a revision of the physical properties of the components incorporating recently published high-precision radial velocity measurements, and a new detailed chemical analysis providing abundances for more than 20 elements in both stars. We obtain highly precise (similar to 0.3%) masses of 2.5687 +/- 0.0074 M-circle dot and 2.4828 +/- 0.0067 M-circle dot, radii of 11.98 +/- 0.57 R-circle dot and 8.83 +/- 0.33 R-circle dot, effective temperatures of 4970 +/- 50 and 5730 +/- 60 K, and independently measured luminosities based on the orbital parallax (78.7 +/- 4.2 L-circle dot and 72.7 +/- 3.6 L-circle dot). We find an excellent match to stellar evolution models at the measured composition of [Fe/H] = -0.04 +/- 0.06. Three different sets of models place the primary star firmly at the end of the core helium-burning phase (clump), while the secondary is known to be evolving rapidly across the Hertzprung gap. The measured lithium abundance, the C/N ratio, and the C-12/C-13 isotopic carbon abundance ratio, which change rapidly in the giant phase, are broadly in agreement with expectations from models. Predictions from tidal theory for the spin rates, spin-orbit alignment, and other properties do not fare as well, requiring a 40-fold increase in the efficiency of the dissipation mechanisms in order to match the observations. C1 [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Claret, Antonio] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Pavlovski, Kresimir] Univ Zagreb, Fac Sci, Dept Phys, Zagreb 10000, Croatia. [Dotter, Aaron] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu; claret@iaa.es; pavlovski@phy.hr; aaron.dotter@gmail.com FU NSF [AST-1007992]; Smithsonian Institution Endowment funds; NASA FX We thank Brian Mason (U.S. Naval Observatory) for providing the historical positional measurements of the Capella HL system, and the anonymous referee for helpful comments. The work of G.T. was partially supported by NSF grant AST-1007992, and by Smithsonian Institution Endowment funds. The research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, of NASA's Astrophysics Data System Abstract Service, of the Washington Double Star Catalog maintained at the U.S. Naval Observatory, and 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 NASA and the NSF. NR 82 TC 5 Z9 5 U1 0 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 JUL 1 PY 2015 VL 807 IS 1 AR 26 DI 10.1088/0004-637X/807/1/26 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO1VX UT WOS:000358945200026 ER PT J AU Wells, M Pel, JW Glasse, A Wright, GS Aitink-Kroes, G Azzollini, R Beard, S Brandl, BR Gallie, A Geers, VC Glauser, AM Hastings, P Henning, T Jager, R Justtanont, K Kruizinga, B Lahuis, F Lee, D Martinez-Delgado, I Martinez-Galarza, JR Meijers, M Morrison, JE Muller, F Nakos, T O'Sullivan, B Oudenhuysen, A Parr-Burman, P Pauwels, E Rohloff, RR Schmalzl, E Sykes, J Thelen, MP van Dishoeck, EF Vandenbussche, B Venema, LB Visser, H Waters, LBFM Wright, D AF Wells, Martyn Pel, J. -W. Glasse, Alistair Wright, G. S. Aitink-Kroes, Gabby Azzollini, Ruyman Beard, Steven Brandl, B. R. Gallie, Angus Geers, V. C. Glauser, A. M. Hastings, Peter Henning, Th. Jager, Rieks Justtanont, K. Kruizinga, Bob Lahuis, Fred Lee, David Martinez-Delgado, I. Martinez-Galarza, J. R. Meijers, M. Morrison, Jane E. Mueller, Friedrich Nakos, Thodori O'Sullivan, Brian Oudenhuysen, Ad Parr-Burman, P. Pauwels, Evert Rohloff, R. -R. Schmalzl, Eva Sykes, Jon Thelen, M. P. van Dishoeck, E. F. Vandenbussche, Bart Venema, Lars B. Visser, Huib Waters, L. B. F. M. Wright, David TI The Mid-Infrared Instrument for the James Webb Space Telescope, VI: The Medium Resolution Spectrometer SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID THERMAL-EXPANSION MEASUREMENTS; OPTICAL MATERIALS; TEMPERATURE AB We describe the design and performance of the Medium Resolution Spectrometer (MRS) for the JWST-MIRI instrument. The MRS incorporates four coaxial spectral channels in a compact opto-mechanical layout that generates spectral images over fields of view up to 7.7 x 7.7 '' in extent and at spectral resolving powers ranging from 1300 to 3700. Each channel includes an all-reflective integral field unit (IFU): an "image slicer" that reformats the input field for presentation to a grating spectrometer. Two 1024 x 1024 focal plane detector arrays record the output spectral images with an instantaneous spectral coverage of approximately one third of the full wavelength range of each channel. The full 5-28.5 mu m spectrum is then obtained by making three exposures using gratings and pass-band-determining filters that are selected using just two three-position mechanisms. The expected on-orbit optical performance is presented, based on testing of the MIRI Flight Model and including spectral and spatial coverage and resolution. The point spread function of the reconstructed images is shown to be diffraction limited and the optical transmission is shown to be consistent with the design expectations. C1 [Wells, Martyn; Glasse, Alistair; Wright, G. S.; Beard, Steven; Gallie, Angus; Hastings, Peter; Lee, David; Parr-Burman, P.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Pel, J. -W.] Univ Groningen, Kapteyn Inst, NL-9700 Groningen, Netherlands. [Aitink-Kroes, Gabby; Jager, Rieks; Meijers, M.; Oudenhuysen, Ad; Pauwels, Evert] NOVA Opt IR Grp, NL-7990 AA Dwingeloo, Netherlands. [Azzollini, Ruyman; Geers, V. C.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Azzollini, Ruyman; Martinez-Delgado, I.] Ctr Astrobiol INTA CSIC, Dept Astrofis, Madrid 28850, Spain. [Brandl, B. R.; Lahuis, Fred; Martinez-Galarza, J. R.; Schmalzl, Eva; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Glauser, A. M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Henning, Th.; Mueller, Friedrich; Rohloff, R. -R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Justtanont, K.] Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden. [Kruizinga, Bob; Visser, Huib] TNO Opt, NL-2600 AD Delft, Netherlands. [Lahuis, Fred; Waters, L. B. F. M.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Martinez-Galarza, J. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morrison, Jane E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Nakos, Thodori] Sterrenkundig Observ UGent, B-9000 Ghent, Belgium. [O'Sullivan, Brian] Airbus Def & Space, Portsmouth PO3 5PU, Hants, England. [Pauwels, Evert; Venema, Lars B.] Pi Environm BV, NL-2221 AC Katwijk, Netherlands. [Sykes, Jon] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Thelen, M. P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Vandenbussche, Bart] Inst Astron KU Leuven, B-3001 Leuven, Belgium. [Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Wright, David] Stinger Ghaffarian Technol Inc, Greenbelt, MD 20770 USA. RP Wells, M (reprint author), Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. OI /0000-0003-1689-9201 NR 23 TC 14 Z9 13 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2015 VL 127 IS 953 BP 646 EP 664 DI 10.1086/682255 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CO0MY UT WOS:000358847000007 ER PT J AU Rothfels, CJ Li, FW Sigel, EM Huiet, L Larsson, A Burge, DO Ruhsam, M Deyholos, M Soltis, DE Stewart, CN Shaw, SW Pokorny, L Chen, T dePamphilis, C DeGironimo, L Chen, L Wei, XF Sun, X Korall, P Stevenson, DW Graham, SW Wong, GKS Pryer, KM AF Rothfels, Carl J. Li, Fay-Wei Sigel, Erin M. Huiet, Layne Larsson, Anders Burge, Dylan O. Ruhsam, Markus Deyholos, Michael Soltis, Douglas E. Stewart, C. Neal, Jr. Shaw, Shane W. Pokorny, Lisa Chen, Tao dePamphilis, Claude DeGironimo, Lisa Chen, Li Wei, Xiaofeng Sun, Xiao Korall, Petra Stevenson, Dennis W. Graham, Sean W. Wong, Gane K-S. Pryer, Kathleen M. TI The evolutionary history of ferns inferred from 25 low-copy nuclear genes SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE codon models; curated phylogenomics; divergence time dating; Equisetum; fern chronogram; incomplete lineage sorting; low-copy nuclear gene; model selection; monilophytes; transcriptome ID EUPOLYPOD II FERNS; BAYESIAN PHYLOGENETIC INFERENCE; RBCL NUCLEOTIDE-SEQUENCES; ADIANTUM-CAPILLUS-VENERIS; LAND PLANT PHYLOGENY; CHAIN MONTE-CARLO; RETICULATE EVOLUTION; MOLECULAR EVOLUTION; FLOWERING PLANTS; DRYOPTERIS DRYOPTERIDACEAE AB PREMISE OF THE STUDY: Understanding fern (monilophyte) phylogeny and its evolutionary timescale is critical for broad investigations of the evolution of land plants, and for providing the point of comparison necessary for studying the evolution of the fern sister group, seed plants. Molecular phylogenetic investigations have revolutionized our understanding of fern phylogeny, however, to date, these studies have relied almost exclusively on plastid data. METHODS: Here we take a curated phylogenomics approach to infer the first broad fern phylogeny from multiple nuclear loci, by combining broad taxon sampling (73 ferns and 12 outgroup species) with focused character sampling (25 loci comprising 35 877 bp), along with rigorous alignment, orthology inference and model selection. KEY RESULTS: Our phylogeny corroborates some earlier inferences and provides novel insights; in particular, we find strong support for Equisetales as sister to the rest of ferns, Marattiales as sister to leptosporangiate ferns, and Dennstaedtiaceae as sister to the eupolypods. Our divergence-time analyses reveal that divergences among the extant fern orders all occurred prior to similar to 200 MYA. Finally, our species-tree inferences are congruent with analyses of concatenated data, but generally with lower support. Those cases where species-tree support values are higher than expected involve relationships that have been supported by smaller plastid datasets, suggesting that deep coalescence may be reducing support from the concatenated nuclear data. CONCLUSIONS: Our study demonstrates the utility of a curated phylogenomics approach to inferring fern phylogeny, and highlights the need to consider underlying data characteristics, along with data quantity, in phylogenetic studies. C1 [Rothfels, Carl J.] Univ British Columbia, Dept Zool, Vancouver, BC V6J 3S7, Canada. [Rothfels, Carl J.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6J 3S7, Canada. [Li, Fay-Wei; Huiet, Layne; Pryer, Kathleen M.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Sigel, Erin M.] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA. [Larsson, Anders; Korall, Petra] Uppsala Univ, Evolutionary Biol Ctr, Dept Organismal Biol, Systemat Biol, SE-75236 Uppsala, Sweden. [Burge, Dylan O.] Calif Acad Sci, San Francisco, CA 94118 USA. [Ruhsam, Markus] Royal Bot Garden Edinburgh, Edinburgh EH3 5LR, Midlothian, Scotland. [Deyholos, Michael] Univ British Columbia, Dept Biol, Kelowna, BC V1V 1V7, Canada. [Soltis, Douglas E.] Univ Florida, Dept Biol, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Soltis, Douglas E.] Univ Florida, Genet Inst, Gainesville, FL 32611 USA. [Stewart, C. Neal, Jr.] Univ Tennessee, Dept Plant Sci, Knoxville, TN 37996 USA. [Pokorny, Lisa] CSIC, Real Jardin Bot, Dept Biodivers & Conservac, E-28014 Madrid, Spain. [Chen, Tao] Chinese Acad Sci, Shenzhen Fairy Lake Bot Garden, Shenzhen 518004, Guangdong, Peoples R China. [dePamphilis, Claude] Penn State Univ, Dept Biol, University Pk, PA 16802 USA. [DeGironimo, Lisa; Stevenson, Dennis W.] New York Bot Garden, Bronx, NY 10458 USA. [Chen, Li; Wei, Xiaofeng; Sun, Xiao] BGI Shenzhen, Beishan Ind Zone, Shenzhen 518083, Peoples R China. [Graham, Sean W.] Univ British Columbia, Dept Bot, Vancouver, BC V6J 3S7, Canada. [Graham, Sean W.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6J 3S7, Canada. [Wong, Gane K-S.] Univ Alberta, Dept Biol Sci, Edmonton, AB T6G 2E9, Canada. [Wong, Gane K-S.] Univ Alberta, Dept Med, Edmonton, AB T6G 2E1, Canada. RP Rothfels, CJ (reprint author), Univ Herbarium, Berkeley, CA 94720 USA. EM crothfels@yahoo.ca RI Graham, Sean/L-3944-2014; Wong, Gane Ka-Shu/G-5784-2013; Pokorny, Lisa/H-1233-2013; dePamphilis, Claude/P-6652-2016; OI Graham, Sean/0000-0001-8209-5231; Wong, Gane Ka-Shu/0000-0001-6108-5560; Larsson, Anders/0000-0002-2096-8102 FU National Science Foundation [OCI-1053575]; Natural Sciences and Engineering Research Council [Canada] (PGSD); National Science Foundation [U.S.A.] [DEB-1110767, DEB-1145614, DEB-1110775, DEB-1407158]; Swedish Research Council for Environment, Agricultural Sciences and Spatial Planning [2006-429, 2010-585]; Alberta Ministry of Innovation and Advanced Education; Natural Sciences and Engineering Research Council [Canada] (PDF); Alberta Innovates Technology Futures' Innovates Centers of Research Excellence program; Musea Ventures; BGI-Shenzhen FX The authors thank Mark Miller, Adam Bazinet, and David Swofford for assistance, and Associate Editor Aaron Liston and two anonymous reviewers for helpful comments on earlier versions of the manuscript. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by the National Science Foundation (OCI-1053575). This work was supported by the Natural Sciences and Engineering Research Council [Canada] (PGSD and PDF to C.J.R., Discovery Grant to S.W.G), the National Science Foundation [U.S.A.] (DEB-1110767 to K.M.P. and C.J.R., DEB-1145614 to K.M.P. and L.H., DEB-1110775 to K.M.P. and E.M.S., DEB-1407158 to K.M.P. and F-W.L.), and the Swedish Research Council for Environment, Agricultural Sciences and Spatial Planning (2006-429 and 2010-585 to P.K.). The 1000 Plants Project (1KP) initiative is funded by the Alberta Ministry of Innovation and Advanced Education, Alberta Innovates Technology Futures' Innovates Centers of Research Excellence program, Musea Ventures, and BGI-Shenzhen. NR 191 TC 22 Z9 22 U1 2 U2 47 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 JUL PY 2015 VL 102 IS 7 BP 1089 EP 1107 DI 10.3732/ajb.1500089 PG 19 WC Plant Sciences SC Plant Sciences GA CN2TW UT WOS:000358275800008 PM 26199366 ER PT J AU Cribbs, JD Hazari, Z Sonnert, G Sadler, PM AF Cribbs, Jennifer D. Hazari, Zahra Sonnert, Gerhard Sadler, Philip M. TI Establishing an Explanatory Model for Mathematics Identity SO CHILD DEVELOPMENT LA English DT Article ID SELF-EFFICACY; OUTCOME EXPECTATIONS; HIGH-SCHOOL; STUDENTS; GENDER; EXPERIENCES; MOTIVATION; BELIEFS; SCIENCE; ADOLESCENCE AB This article empirically tests a previously developed theoretical framework for mathematics identity based on students' beliefs. The study employs data from more than 9,000 college calculus students across the United States to build a robust structural equation model. While it is generally thought that students' beliefs about their own competence in mathematics directly impact their identity as a math person, findings indicate that students' self-perceptions related to competence and performance have an indirect effect on their mathematics identity, primarily by association with students' interest and external recognition in mathematics. Thus, the model indicates that students' competence and performance beliefs are not sufficient for their mathematics identity development, and it highlights the roles of interest and recognition. C1 [Cribbs, Jennifer D.] Western Kentucky Univ, Sch Teacher Educ, Bowling Green, KY 42101 USA. [Hazari, Zahra] Florida Int Univ, Dept Teaching & Learning, Dept Phys, Miami, FL 33199 USA. [Hazari, Zahra] Florida Int Univ, STEM Transformat Inst, Miami, FL 33199 USA. [Sonnert, Gerhard; Sadler, Philip M.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cribbs, JD (reprint author), Western Kentucky Univ, Sch Teacher Educ, Bowling Green, KY 42101 USA. EM jennifer.cribbs@wku.edu FU National Science Foundation [0813702] FX This research is part of the Factors Influencing College Success in Mathematics (FICSMath) project funded by the National Science Foundation (0813702). Without the contributions and support of many people, the FICSMath project would not have been possible. We thank the members of the FICSMath team: John Almarode, Devasmita Chakraverty, Jennifer Cribbs, Kate Dabney, Zahra Hazari, Heather Hill, Jaimie Miller, Matthew Moynihan, Jon Star, Robert Tai, Terry Tivnan, Annette Trenga, Carol Wade, and Charity Watson. We would also like to thank several mathematics educators who provided advice or counsel on this project: Sadie Bragg, David Bressoud, James S. Dietz, Solomon Garfunkel, Daniel Goroff, Ed Joyce, James Lewis, Karen Marrongelle, William McCallum, Ricardo Nemirovsky, and Bob Speiser. Last but not least, we are grateful to the many college calculus professors and their students who gave up a portion of a class to provide data. Any opinions, findings, and conclusions in this article are the authors' and do not necessarily reflect the views of the National Science Foundation. [Correction added on 06 April 2015, after first online publication: Updated NSF Grant Number and acknowledgements]. NR 60 TC 5 Z9 5 U1 1 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0009-3920 EI 1467-8624 J9 CHILD DEV JI Child Dev. PD JUL-AUG PY 2015 VL 86 IS 4 BP 1048 EP 1062 DI 10.1111/cdev.12363 PG 15 WC Psychology, Educational; Psychology, Developmental SC Psychology GA CN1LG UT WOS:000358180900005 ER PT J AU Zeng, Y Lin, Y Abundo, A Dudley, R AF Zeng, Yu Lin, Yvonne Abundo, Arianna Dudley, Robert TI Visual ecology of directed aerial descent in first-instar nymphs of the stick insect Extatosoma tiaratum SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Canopy; Gliding; Invertebrate; Vision ID CEPHALOTES-ATRATUS; EDGE-DETECTION; GLIDING ANTS; VISION; SENSITIVITY; EVOLUTION; ORIGINS; FORESTS; FLIGHT; COLOR AB Many wingless insects perform directed aerial descent (DAD) to return to vegetational structures after falling. Given the complex visual environment and spatial structures of tree canopies, those visual signals used as directional cues are not fully understood. Here, we address the role of visual contrast for DAD in newly hatched nymphs of the stick insect Extatosoma tiaratum under controlled laboratory conditions. Landing preferences of gliding E. tiaratum in various visual environments were studied. We used a single vertical stripe defined by variable contrast edges to test the use of contrast consistency and sharpness. We also used aggregate patterns to examine the effects of target size and the effectiveness of luminance contrast and chromatic contrast. E. tiaratum nymphs were attracted to single stripes with well-defined edges, and particularly favored narrow dark targets. The directionality and accuracy of landing were dependent on target size. Lastly, luminance contrasts were more effective in attracting landings than were chromatic contrasts. Visual contrasts are therefore used as spatial references for landing behavior in DAD. These behaviors may enable nymphs to quickly locate dark or shaded sides of vertically oriented vegetation in natural habitats. C1 [Zeng, Yu; Lin, Yvonne; Abundo, Arianna; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Zeng, Y (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM dreavoniz@berkeley.edu OI Zeng, Yu/0000-0002-2651-227X FU Undergraduate Research Apprentice Program (URAP) of UC Berkeley FX This work was partially funded by the Undergraduate Research Apprentice Program (URAP) of UC Berkeley to Y.L. and R.D. NR 30 TC 1 Z9 1 U1 4 U2 13 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 EI 1477-9145 J9 J EXP BIOL JI J. Exp. Biol. PD JUL PY 2015 VL 218 IS 14 BP 2305 EP 2314 DI 10.1242/jeb.109553 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA CN3CL UT WOS:000358301300025 PM 26026039 ER PT J AU Komatsu, M Fagan, TJ Mikouchi, T Petaev, MI Zolensky, ME AF Komatsu, Mutsumi Fagan, Timothy J. Mikouchi, Takashi Petaev, Michail I. Zolensky, Michael E. TI LIME silicates in amoeboid olivine aggregates in carbonaceous chondrites: Indicator of nebular and asteroidal processes SO METEORITICS & PLANETARY SCIENCE LA English DT Review ID AL-RICH INCLUSIONS; UNEQUILIBRATED ORDINARY CHONDRITES; OXYGEN ISOTOPIC COMPOSITIONS; EARLY SOLAR-SYSTEM; CV3 CHONDRITES; REFRACTORY INCLUSIONS; ALLENDE METEORITE; AQUEOUS ALTERATION; FAYALITIC OLIVINE; DARK INCLUSIONS AB MnO/FeO ratios in olivine from amoeboid olivine aggregates (AOAs) reflect conditions of nebular condensation and can be used in concert with matrix textures to compare metamorphic conditions in carbonaceous chondrites. LIME (low-iron, Mn-enriched) olivine was identified in AOAs from Y-81020 (CO3.05), Kaba (CV similar to 3.1), and in Y-86009 (CV3), Y-86751 (CV3), NWA 1152 (CR/CV3), but was not identified in AOAs from Efremovka (CV3.1-3.4) or Allende (CV>3.6). According to thermodynamic models of nebular condensation, LIME olivine is stable at lower temperatures than Mn-poor olivine and at low oxygen fugacities (dust enrichment <10x solar). Although this set of samples does not represent a single metamorphic sequence, the higher subtypes tend to have AOA olivine with lower Mn/Fe, suggesting that Mn/Fe decreases during parent body metamorphism. Y-81020 has the lowest subtype and most forsteritic AOA olivine (Fo(>95)) in our study, whereas Efremovka AOAs are slightly Fe-rich (Fo(>92)). AOA olivines from Kaba are mostly forsteritic, but rare Fe-rich olivine precipitated from an aqueous fluid. A combination of precipitation of Fe-rich olivine and diffusion of Fe into primary olivine grains resulted in iron-rich compositions (Fo(97-59)) in Allende AOAs. Variations from fine-grained, nonporous matrix toward higher porosity and coarser lath-like matrix olivine can be divided into six stages represented by (1) Y-81020, Efremovka, NWA 1152; (2) Y-86751 lithology B; (3) Y-86009; (4) Kaba; (5) Y-86751 lithology A; (6) Allende. These stages are inferred to represent general degree of metamorphism, although the specific roles of thermally driven grain growth and diffusion versus aqueous dissolution and precipitation remain uncertain. C1 [Komatsu, Mutsumi; Fagan, Timothy J.] Waseda Univ, Dept Earth Sci, Tokyo 1698050, Japan. [Komatsu, Mutsumi] Waseda Univ, Waseda Inst Adv Study, Tokyo 1698050, Japan. [Mikouchi, Takashi] Univ Tokyo, Dept Earth & Planetary Sci, Tokyo 1130033, Japan. [Petaev, Michail I.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Petaev, Michail I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zolensky, Michael E.] NASA Johnson Space Ctr, ARES, Houston, TX 77058 USA. RP Komatsu, M (reprint author), Waseda Univ, Dept Earth Sci, Tokyo 1698050, Japan. EM komatsu@aoni.waseda.jp FU Japan Society for the Promotion of Science [24740358]; Waseda University Grant for Special Research Projects [2013A-097]; NASA Cosmochemistry Program; LARS Program FX We thank the Japanese National Institute of Polar Research (NIPR) for sample allocation of Antarctic meteorites and Efremovka. We thank Naoji Sugiura for discussions on condensation of AOAs. Parts of this work have been presented previously at meetings, where we have benefited from discussions with Alexander N. Krot, Denton Ebel, Herbert Palme, and Munir Humayun, among many others. This work was supported by Grant-in-Aid for JSPS Fellows, JSPS Grant-in-Aid for Young Scientists (B) from Japan Society for the Promotion of Science (no. 24740358 to MK), and a Waseda University Grant for Special Research Projects (2013A-097 to MK). MEZ acknowledges support from the NASA Cosmochemistry and LARS Programs. We thank Mike Weisberg, Dominik Hezel, and an anonymous reviewer for insightful reviews, and Gretchen Benedix for editorial guidance. NR 105 TC 1 Z9 1 U1 1 U2 4 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 JUL PY 2015 VL 50 IS 7 BP 1271 EP 1294 DI 10.1111/maps.12460 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CN0TH UT WOS:000358126000008 ER PT J AU Paz, A Ibanez, R Lips, KR Crawford, AJ AF Paz, Andrea Ibanez, Roberto Lips, Karen R. Crawford, Andrew J. TI Testing the role of ecology and life history in structuring genetic variation across a landscape: a trait-based phylogeographic approach SO MOLECULAR ECOLOGY LA English DT Article DE dispersal ability; DNA barcoding; ecological niche modelling; hierarchical approximate Bayesian computation; landscape resistance; phylogeography ID AMERICAN BIOTIC INTERCHANGE; APPROXIMATE BAYESIAN COMPUTATION; SPECIES GEOGRAPHIC DISTRIBUTIONS; FRESH-WATER FISHES; POPULATION-STRUCTURE; STATISTICAL PHYLOGEOGRAPHY; RIVERINE BARRIERS; CENTRAL PANAMA; BODY-SIZE; DIVERSITY AB Hypotheses to explain phylogeographic structure traditionally invoke geographic features, but often fail to provide a general explanation for spatial patterns of genetic variation. Organisms' intrinsic characteristics might play more important roles than landscape features in determining phylogeographic structure. We developed a novel comparative approach to explore the role of ecological and life-history variables in determining spatial genetic variation and tested it on frog communities in Panama. We quantified spatial genetic variation within 31 anuran species based on mitochondrial DNA sequences, for which hierarchical approximate Bayesian computation analyses rejected simultaneous divergence over a common landscape. Regressing ecological variables, on genetic divergence allowed us to test the importance of individual variables revealing that body size, current landscape resistance, geographic range, biogeographic origin and reproductive mode were significant predictors of spatial genetic variation. Our results support the idea that phylogeographic structure represents the outcome of an interaction between organisms and their environment, and suggest a conceptual integration we refer to as trait-based phylogeography. C1 [Paz, Andrea; Crawford, Andrew J.] Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. [Ibanez, Roberto; Lips, Karen R.; Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Ibanez, Roberto; Crawford, Andrew J.] Circulo Herpetol Panama, Panama City, Panama. [Lips, Karen R.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. RP Paz, A (reprint author), Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. EM paz.andreita@gmail.com OI Lips, Karen/0000-0002-2719-1551; Paz, Andrea/0000-0001-6484-1210 FU National Geographic CRE grant [8133-06] FX Specimens were collected under Panama's Autoridad Nacional del Ambiente permit number SE/A-37-07 to R.I.D. Field work was funded by National Geographic CRE grant 8133-06 to A.J.C., K.R.L. and R.I.D. DNA sequence data were kindly obtained by A. C. Driskell at the Smithsonian Institution's Laboratories of Analytical Biology. We are grateful to C. Ortiz and J. Velasquez for help with ENM analyses. For valuable comments on this work, we are thankful to M. Hickerson, C. D. Cadena, N. R. Pinto, L. S. Barrientos, C. E. Guarnizo, L. F. Duenas and K. C. Wollenberg Valero. We thank T. Vines, L. Rissler and two anonymous reviewers for feedback via Axios Review and three anonymous reviewers from this journal for valuable feedback. NR 123 TC 6 Z9 6 U1 4 U2 42 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 JUL PY 2015 VL 24 IS 14 BP 3723 EP 3737 DI 10.1111/mec.13275 PG 15 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA CN1EX UT WOS:000358161300017 PM 26080899 ER PT J AU Bieryla, A Collins, K Beatty, TG Eastman, J Siverd, RJ Pepper, J Gaudi, BS Stassun, KG Canas, C Latham, DW Buchhave, LA Sanchis-Ojeda, R Winn, JN Jensen, ELN Kielkopf, JF McLeod, KK Gregorio, J Colon, KD Street, R Ross, R Penny, M Mellon, SN Oberst, TE Fulton, BJ Wang, J Berlind, P Calkins, ML Esquerdo, GA DePoy, DL Gould, A Marshall, J Pogge, R Trueblood, M Trueblood, P AF Bieryla, Allyson Collins, Karen Beatty, Thomas G. Eastman, Jason Siverd, Robert J. Pepper, Joshua Gaudi, B. Scott Stassun, Keivan G. Canas, Caleb Latham, David W. Buchhave, Lars A. Sanchis-Ojeda, Roberto Winn, Joshua N. Jensen, Eric L. N. Kielkopf, John F. McLeod, Kim K. Gregorio, Joao Colon, Knicole D. Street, Rachel Ross, Rachel Penny, Matthew Mellon, Samuel N. Oberst, Thomas E. Fulton, Benjamin J. Wang, Ji Berlind, Perry Calkins, Michael L. Esquerdo, Gilbert A. DePoy, Darren L. Gould, Andrew Marshall, Jennifer Pogge, Richard Trueblood, Mark Trueblood, Patricia TI KELT-7b: A HOT JUPITER TRANSITING A BRIGHT V=8.54 RAPIDLY ROTATING F-STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (KELT); techniques: photometric; techniques: spectroscopic ID SUN-LIKE STAR; IMAGE SUBTRACTION; GIANT PLANET; SYSTEM; ORBIT; PARAMETERS; ABUNDANCE; VELOCITY; MISSION; PERIOD AB We report the discovery of KELT-7b, a transiting hot Jupiter with a mass of 1.28 +/- 0.18 M-J, radius of 1.533(-0.047)(+0.046) R-J, and an orbital period of 2.7347749 +/- 0.0000039 days. The bright host star (HD 33643; KELT-7) is an F-star with V = 8.54, T-eff = 6789(-49)(+50) K, [Fe/H] = 0.139(-0.081)(+0.075), and log g = 4.149 +/- 0.019. It has a mass of 1.535(-0.054)(+0.066) M-circle dot, a radius of 1.732(-0.045)(+0.043) R-circle dot, and is the fifth most massive, fifth hottest, and the ninth brightest star known to host a transiting planet. It is also the brightest star around which Kilodegree Extremely Little Telescope (KELT) has discovered a transiting planet. Thus, KELT-7b is an ideal target for detailed characterization given its relatively low surface gravity, high equilibrium temperature, and bright host star. The rapid rotation of the star (73 +/- 0.5 km s(-1)) results in a Rossiter-McLaughlin effect with an unusually large amplitude of several hundred m s(-1). We find that the orbit normal of the planet is likely to be well-aligned with the stellar spin axis, with a projected spin-orbit alignment of lambda = 9 degrees.7 +/- 5 degrees.2. This is currently the second most rapidly rotating star to have a reflex signal (and thus mass determination) due to a planetary companion measured. C1 [Bieryla, Allyson; Eastman, Jason; Canas, Caleb; Latham, David W.; Buchhave, Lars A.; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Collins, Karen; Kielkopf, John F.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Beatty, Thomas G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16801 USA. [Eastman, Jason; Siverd, Robert J.; Street, Rachel; Ross, Rachel] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Pepper, Joshua; Colon, Knicole D.] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Gaudi, B. Scott; Penny, Matthew; Gould, Andrew; Pogge, Richard] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Sanchis-Ojeda, Roberto] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [McLeod, Kim K.] Wellesley Coll, Wellesley, MA 02481 USA. [Gregorio, Joao] Atalaia Grp, Portalegre, Portugal. [Gregorio, Joao] Crow Observ, Portalegre, Portugal. [Mellon, Samuel N.; Oberst, Thomas E.] Westminster Coll, New Wilmington, PA 16172 USA. [Fulton, Benjamin J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Wang, Ji] Yale Univ, New Haven, CT 06520 USA. [DePoy, Darren L.; Marshall, Jennifer] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Trueblood, Mark; Trueblood, Patricia] Winer Observ, Sonoita, AZ 85637 USA. RP Bieryla, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abieryla@cfa.harvard.edu OI Eastman, Jason/0000-0003-3773-5142; Jensen, Eric/0000-0002-4625-7333; Buchhave, Lars A./0000-0003-1605-5666; Pepper, Joshua/0000-0002-3827-8417; Latham, David/0000-0001-9911-7388; Stassun, Keivan/0000-0002-3481-9052 FU NASA Grant [NNG04GO70G]; Kepler mission [NNX13AB58A]; Smithsonian Astrophysical Observatory; National Science Foundation Graduate Research Fellowship [2014184874]; NASA through the Sagan Fellowship Program; Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics; National Science Foundation through PAARE Grant [AST-1358862]; NSF CAREER Grant [AST-1056524]; NASA Origins program [NNX11AG85G] FX Early work on KELT-North was supported by NASA Grant NNG04GO70G.; A.B. acknowledges partial support from the Kepler mission under Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory, D.W.L. PI.; B.J.F. acknowledges that this material is based on work supported by the National Science Foundation Graduate Research Fellowship under Grant No. 2014184874. 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. R.S.O. acknowledges that 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.; K.G.S. acknowledges support from the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics and the support of the National Science Foundation through PAARE Grant AST-1358862.; Work by B.S.G. and T.G.B. was partially supported by NSF CAREER Grant AST-1056524. Work by J.N.W. was supported by the NASA Origins program under grant NNX11AG85G. NR 74 TC 16 Z9 16 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 JUL PY 2015 VL 150 IS 1 AR 12 DI 10.1088/0004-6256/150/1/12 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5QU UT WOS:000357744400012 ER PT J AU Brahm, R Jordan, A Hartman, JD Bakos, GA Bayliss, D Penev, K Zhou, G Ciceri, S Rabus, M Espinoza, N Mancini, L De Val-Borro, M Bhatti, W Sato, B Tan, TG Csubry, Z Buchhave, L Henning, T Schmidt, B Suc, V Noyes, RW Papp, I Lazar, J Sari, P AF Brahm, R. Jordan, A. Hartman, J. D. Bakos, G. A. Bayliss, D. Penev, K. Zhou, G. Ciceri, S. Rabus, M. Espinoza, N. Mancini, L. De Val-Borro, M. Bhatti, W. Sato, B. Tan, T. G. Csubry, Z. Buchhave, L. Henning, T. Schmidt, B. Suc, V. Noyes, R. W. Papp, I. Lazar, J. Sari, P. TI HATS9-b AND HATS10-b: TWO COMPACT HOT JUPITERS IN FIELD 7 OF THE K2 MISSION SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HATS-9, GSC 6305-02502, HATS-10, GSC 6311-00085); techniques: photometric; techniques: spectroscopic ID KEPLER FIELD; PLANET-DETECTION; HATSOUTH SURVEY; GIANT PLANETS; BRIGHT STAR; STELLAR; SPECTROGRAPH; PHOTOMETRY; TRANSITS; MASS AB We report the discovery of two transiting extrasolar planets by the HATSouth survey. HATS-9b orbits an old (10.8 +/- 1.5 Gyr) V = 13.3 G dwarf star with a period P approximate to 1.9153 days. The host star has a mass of 1.03 M-circle dot, radius of 1.503 R-circle dot, and effective temperature 5366 +/- 70 K. The planetary companion has a mass of 0.837 M-J and radius of 1.065 R-J, yielding a mean density of 0.85 g cm(-3). HATS-10b orbits a V = 13.1 G dwarf star with a period P approximate to 3.3128 days. The host star has a mass of 1.1 M-circle dot, radius of 1.11 R-circle dot, and effective temperature 5880 +/- 120 K. The planetary companion has a mass of 0.53 M-J and radius of 0.97 R-J, yielding a mean density of 0.7 g cm-3. Both planets are compact in comparison with planets receiving similar irradiation from their host stars and lie in the nominal coordinates of Field 7 of K2, but only HATS-9b falls on working silicon. Future characterization of HATS-9b with the exquisite photometric precision of the Kepler telescope may provide measurements of its reflected light signature. C1 [Brahm, R.; Jordan, A.; Rabus, M.; Espinoza, N.; Suc, V.] Catholic Univ Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Brahm, R.; Jordan, A.; Espinoza, N.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Hartman, J. D.; Bakos, G. A.; Penev, K.; De Val-Borro, M.; Bhatti, W.; Csubry, Z.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bayliss, D.] Univ Geneva, Observ Astronom, CH-1290 Versoix, Switzerland. [Bayliss, D.; Zhou, G.] Australian Natl Univ, Canberra, ACT, Australia. [Ciceri, S.; Rabus, M.; Mancini, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Sato, B.; Schmidt, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Tokyo 1528551, Japan. [Tan, T. G.; Henning, T.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Buchhave, L.; Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Papp, I.; Lazar, J.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Brahm, R (reprint author), Catholic Univ Chile, Fac Fis, Inst Astrofis, Av Vicuna Mackenna 4860, Santiago 7820436, Chile. EM rbrahm@astro.puc.cl OI Jordan, Andres/0000-0002-5389-3944; Hartman, Joel/0000-0001-8732-6166; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Bakos, Gaspar/0000-0001-7204-6727; Buchhave, Lars A./0000-0003-1605-5666; Tan, Thiam-Guan/0000-0001-5603-6895 FU NSF MRI grant [NSF/AST-0723074]; NASA [NNX09AB29G/NNX12AH91H, NNX13AQ62G]; FONDECYT [1130857]; BASAL CATA [PFB-06]; "Millennium Institute of Astrophysics (MAS)" of the Millenium Science Initiative, Chilean Ministry of Economy [IC120009]; CONICYT-PCHA/Doctorado Nacional; "Millenium Institute of Astrophysics (MAS)" of the Millennium Science Initiative, Chilean Ministry of Economy [IC120009]; ARC Laureate Fellowship [FL0992131]; [NSF/AST-1108686] FX Development of the HATSouth project was funded by the NSF MRI grant NSF/AST-0723074, and operations have been supported by NASA grants NNX09AB29G/NNX12AH91H and internal Princeton funds. Follow-up observations have received 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. Work at the Australian National University is supported by ARC Laureate Fellowship Grant FL0992131. 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 Regis Lachaume for his technical assistance during the observations at the MPG 2.2 m Telescope. We thank Helmut Steinle and Jochen Greiner for supporting the GROND observations presented in this manuscript. We are grateful to P. Sackett for her help in the early phase of the HATSouth project. We thank Adam Burrows for useful comments regarding the evolutionary models of hot Jupiters. NR 59 TC 8 Z9 8 U1 1 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 JUL PY 2015 VL 150 IS 1 AR 33 DI 10.1088/0004-6256/150/1/33 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5QU UT WOS:000357744400033 ER PT J AU Evans, NR Berdnikov, L Lauer, J Morgan, D Nichols, J Gunther, HM Gorynya, N Rastorguev, A Moskalik, P AF Evans, Nancy Remage Berdnikov, Leonid Lauer, Jennifer Morgan, Douglas Nichols, Joy Guenther, H. Moritz Gorynya, Natalya Rastorguev, Alexey Moskalik, Pawel TI BINARY PROPERTIES FROM CEPHEID RADIAL VELOCITIES (CRaV) SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; stars: massive; stars: variables: Cepheids; techniques: radial velocities ID HUBBLE-SPACE-TELESCOPE; PERIOD-LUMINOSITY RELATION; SOLAR-TYPE STARS; GALACTIC CEPHEIDS; MASSIVE STARS; CORRELATION SPECTROMETER; CLASSICAL CEPHEIDS; NORTHERN CEPHEIDS; SOUTHERN CEPHEIDS; MAGELLANIC-CLOUD AB We have examined high accuracy radial velocities of Cepheids to determine the binary frequency. The data are largely from the CORAVEL spectrophotometer and the Moscow version, with a typical uncertainty of <= 1 km s(-1), and a time span from 1 to 20 years. A systemic velocity was obtained by removing the pulsation component using a high order Fourier series. From this data we have developed a list of stars showing no orbital velocity larger than +/- 1 km s(-1). The binary fraction was analyzed as a function of magnitude, and yields an apparent decrease in this fraction for fainter stars. We interpret this as incompleteness at fainter magnitudes, and derive the preferred binary fraction of 29% +/- 8% (20% +/- 6% per decade of orbital period) from the brightest 40 stars. A comparison of this fraction in this period range (1-20 years) implies a large fraction for the full period range. This is reasonable in that the high accuracy velocities are sensitive to the longer periods and smaller orbital velocity amplitudes in the period range sampled here. Thus the Cepheid velocity sample provides a sensitive detection in the period range between short period spectroscopic binaries and resolved companions. The recent identification of delta Cep as a binary with very low amplitude and high eccentricity underscores the fact that the binary fractions we derive are lower limits, to which other low amplitude systems will probably be added. The mass ratio (q) distribution derived from ultraviolet observations of the secondary is consistent with a flat distribution for the applicable period range (1-20 years). C1 [Evans, Nancy Remage] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Berdnikov, Leonid] Entoto Observ & Res Ctr, Astron & Astrophys Res Div, Addis Ababa, Ethiopia. [Berdnikov, Leonid] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Berdnikov, Leonid] Isaac Newton Inst Chile, Moscow Branch, Moscow 119992, Russia. [Lauer, Jennifer; Morgan, Douglas; Nichols, Joy; Guenther, H. Moritz] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Guenther, H. Moritz] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gorynya, Natalya] Russian Acad Sci, Inst Astron, Moscow V71, Russia. [Rastorguev, Alexey] Moscow MV Lomonosov State Univ, Sternberg State Astron Inst, Moscow, Russia. [Moskalik, Pawel] Copernicus Astron Ctr, Warsaw, Poland. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu RI Rastorguev, Alexey/P-7956-2015; OI Rastorguev, Alexey/0000-0003-3525-6869; Gunther, Hans Moritz/0000-0003-4243-2840 FU Chandra X-ray Center NASA Contract [NAS8-03060]; HST grant [GO-12215.01-A]; Russian Foundation for Basic Reserach grant [14-02-00472]; Russian Scientific Foundation [14-22-0041]; Polish NCN grant [DEC-2012/05/B/ST9/03932] FX We are grateful for comments from A. Tokivinin and B. Mason which resulted in an improved manuscript. It is a pleasure to thank Beth Sundheim and Bharath Kumaraswamy for work at the beginning of this project. We also thank Matthew Templeton for providing the program FTCLEAN used to generate the window functions, and for advice on its use. Comments from an anonymous referee improved the presentation of the paper. Support for this work was also provided from the Chandra X-ray Center NASA Contract NAS8-03060 and HST grant GO-12215.01-A. N.A.G. is grateful to Russian Foundation for Basic Reserach grant No. 14-02-00472 for the support of radial velocity measurements. A.S.R. is grateful to Russian Scientific Foundation grant No. 14-22-0041 for the support of data processing. P.M. acknowledges support from the Polish NCN grant no. DEC-2012/05/B/ST9/03932. Vizier and SIMBAD were used in the preparation of this study. NR 76 TC 10 Z9 10 U1 0 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 JUL PY 2015 VL 150 IS 1 AR 13 DI 10.1088/0004-6256/150/1/13 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5QU UT WOS:000357744400013 ER PT J AU Law, DR Yan, R Bershady, MA Bundy, K Cherinka, B Drory, N MacDonald, N Sanchez-Gallego, JR Wake, DA Weijmans, AM Blanton, MR Klaene, MA Moran, SM Sanchez, SF Zhang, K AF Law, David R. Yan, Renbin Bershady, Matthew A. Bundy, Kevin Cherinka, Brian Drory, Niv MacDonald, Nicholas Sanchez-Gallego, Jose R. Wake, David A. Weijmans, Anne-Marie Blanton, Michael R. Klaene, Mark A. Moran, Sean M. Sanchez, Sebastian F. Zhang, Kai TI OBSERVING STRATEGY FOR THE SDSS-IV/MaNGA IFU GALAXY SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article DE atmospheric effects; methods: observational; surveys; techniques: imaging spectroscopy ID OSCILLATION SPECTROSCOPIC SURVEY; INTEGRAL-FIELD SPECTROGRAPH; 2.5 M TELESCOPE; DIFFERENTIAL REFRACTION; PROTOTYPE OBSERVATIONS; SAURON PROJECT; CLASSIFICATION; OBJECTS; SYSTEM AB Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) is an integral-field spectroscopic survey that is one of three core programs in the fourth-generation Sloan Digital Sky Survey (SDSS-IV). MaNGA's 17 pluggable optical fiber-bundle integral field units (IFUs) will observe a sample of 10,000 nearby galaxies distributed throughout the SDSS imaging footprint (focusing particularly on the North Galactic Cap). In each pointing these IFUs are deployed across a 3(degrees) field; they yield spectral coverage 3600-10300 angstrom at a typical resolution R similar to 2000, and sample the sky with 2" diameter fiber apertures with a total bundle fill factor of 56%. Observing over such a large field and range of wavelengths is particularly challenging for obtaining uniform and integral spatial coverage and resolution at all wavelengths and across each entire fiber array. Data quality is affected by the IFU construction technique, chromatic and field differential refraction, the adopted dithering strategy, and many other effects. We use numerical simulations to constrain the hardware design and observing strategy for the survey with the aim of ensuring consistent data quality that meets the survey science requirements while permitting maximum observational flexibility. We find that MaNGA science goals are best achieved with IFUs composed of a regular hexagonal grid of optical fibers with rms displacement of 5 mu m or less from their nominal packing position; this goal is met by the MaNGA hardware, which achieves 3 mu m rms fiber placement. We further show that MaNGA observations are best obtained in sets of three 15 minute exposures dithered along the vertices of a 1.44 arcsec equilateral triangle; these sets form the minimum observational unit, and are repeated as needed to achieve a combined signal-to-noise ratio of 5 angstrom(-1) per fiber in the r-band continuum at a surface brightness of 23 AB arcsec(-2). In order to ensure uniform coverage and delivered image quality, we require that the exposures in a given set be obtained within a 60 minute interval of each other in hour angle, and that all exposures be obtained at airmass less than or similar to 1.2 (i.e., within 1-3 hr of transit depending on the declination of a given field). C1 [Law, David R.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Yan, Renbin; Sanchez-Gallego, Jose R.; Zhang, Kai] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Bershady, Matthew A.; Wake, David A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Bundy, Kevin] Univ Tokyo, Kavli Inst Phys & Math Universe, Todai Inst Adv Study, WPI, Kashiwa, Chiba 2778583, Japan. [Cherinka, Brian] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Drory, Niv] Univ Texas Austin, Dept Astron, McDonald Observ, Austin, TX 78712 USA. [MacDonald, Nicholas] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Wake, David A.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Weijmans, Anne-Marie] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Klaene, Mark A.] Apache Point Observ, Sunspot, NM 88349 USA. [Moran, Sean M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Sanchez, Sebastian F.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. RP Law, DR (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM dlaw@stsci.edu OI Yan, Renbin/0000-0003-1025-1711 FU Summer Undergraduate Research Program at the Dunlap Institute, University of Toronto; Leverhulme Trust; Alfred P. Sloan Foundation; Center for High-Performance Computing at the University of Utah; 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; 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 FX We thank Maryna Tsybulska for early contributions to this project, and acknowledge the Summer Undergraduate Research Program at the Dunlap Institute, University of Toronto for their support. A.W. acknowledges support of a Leverhulme Trust Early Career Fellowship. D.R.L. thanks the anonymous referee whose comments led to an improved version of the manuscript. 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 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, 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. NR 27 TC 20 Z9 20 U1 0 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 JUL PY 2015 VL 150 IS 1 AR 19 DI 10.1088/0004-6256/150/1/19 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5QU UT WOS:000357744400019 ER PT J AU Rodriguez, JE Pepper, J Stassun, KG Siverd, RJ Cargile, P Weintraub, DA Beatty, TG Gaudi, BS Mamajek, EE Sanchez, NN AF Rodriguez, Joseph E. Pepper, Joshua Stassun, Keivan G. Siverd, Robert J. Cargile, Phillip Weintraub, David A. Beatty, Thomas G. Gaudi, B. Scott Mamajek, Eric E. Sanchez, N. Nicole TI V409 TAU AS ANOTHER AA TAU: PHOTOMETRIC OBSERVATIONS OF STELLAR OCCULTATIONS BY THE CIRCUMSTELLAR DISK SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (V409 Tau, AA Tau); stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be ID MAIN-SEQUENCE STARS; HERBIG AE/BE STARS; 2-DIMENSIONAL RADIATIVE-TRANSFER; SPECTRAL ENERGY-DISTRIBUTIONS; UX ORI STARS; T-TAURI; MAGNETOSPHERIC ACCRETION; RW-AURIGAE; PROTOSTELLAR ENVELOPES; IMAGE SUBTRACTION AB AA Tau is a well studied young stellar object (YSO) that presents many of the photometric characteristics of a Classical T Tauri star (CTTS), including short-timescale stochastic variability attributed to spots and/or accretion as well as long-duration dimming events attributed to occultations by vertical features (e.g., warps) in its circumstellar disk. We present new photometric observations of AA Tau from the Kilodegree Extremely Little Telescope North (KELT-North) which reveal a deep, extended dimming event in 2011, which we show supports the interpretation by Bouvier et al. of an occultation by a high-density feature in the circumstellar disk located >8 AU from the star. We also present KELT-North observations of V409 Tau, a relatively unstudied YSO also in Taurus-Auriga, showing short timescale erratic variability, along with two separate long and deep dimming events, one from 2009 January through late 2010 October, and the other from 2012 March until at least 2013 September. We interpret both dimming events to have lasted more than 600 days, each with a depth of similar to 1.4 mag. From a spectral energy distribution analysis, we propose that V409 Tau is most likely surrounded by a circumstellar disk viewed nearly edge-on, and using Keplerian timescale arguments we interpret the deep dimmings of V409 Tau as occultations from one or more features within this disk greater than or similar to 10 AU from the star. In both AA Tau and V409 Tau, the usual CTTS short-timescale variations associated with accretion processes close to the stars continue during the occultations, further supporting the distant occulting material interpretation. Like AA Tau, V409 Tau serves as a laboratory for studying the detailed structure of the protoplanetary environments of T Tauri disks, specifically disk structures that may be signposts of planet formation at many AU out in the disk. We also provide a table of all currently known disk-occulting young stars as a convenient reference for future work on such objects. C1 [Rodriguez, Joseph E.; Pepper, Joshua; Stassun, Keivan G.; Siverd, Robert J.; Cargile, Phillip; Weintraub, David A.; Sanchez, N. Nicole] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Stassun, Keivan G.; Sanchez, N. Nicole] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Siverd, Robert J.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Cargile, Phillip] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beatty, Thomas G.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Beatty, Thomas G.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Gaudi, B. Scott] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Mamajek, Eric E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 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; Mamajek, Eric/0000-0003-2008-1488; Pepper, Joshua/0000-0002-3827-8417; Stassun, Keivan/0000-0002-3481-9052 FU National Aeronautics and Space Administration [NNG05GF22G]; U.S. National Science Foundation [AST-0909182, AST-1313422]; NASA [NNG04GO70G]; Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics; NSF CAREER Grant [AST-1056524]; NSF [AST-1313029]; National Science Foundation; CARMA partner universities FX We would like to thank Alice Quillen and the entire KELT team for their helpful discussions. We have used observational data from the ASAS photometric survey and we are thankful for the observations and data reduction performed. 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. 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. Work by B.S.G. and T.G.B. was partially supported by NSF CAREER Grant AST-1056524. This work has made use of NASA's Astrophysics Data System and the SIMBAD database operated at CDS, Strasbourg, France. E.E.M. acknowledges support from NSF award AST-1313029. This paper makes use of data from the first public release of the SuperWASP data (Butters et al. 2010) as provided by the SuperWASP consortium and services at 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. 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 California, Illinois, 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 79 TC 6 Z9 6 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 JUL PY 2015 VL 150 IS 1 AR 32 DI 10.1088/0004-6256/150/1/32 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM5QU UT WOS:000357744400032 ER PT J AU Geller, MJ Hwang, HS AF Geller, Margaret J. Hwang, Ho Seong TI HectoMAPping the Universe Karl Schwarzschild Award Lecture 2014 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article; Proceedings Paper CT 87th Annual International Scientific Meeting of the Astronomische Gesellschaft CY SEP 22-22, 2014 CL Bamberg, GERMANY DE cosmology: observations; large-scale structure; surveys ID DIGITAL SKY SURVEY; GALAXY REDSHIFT SURVEY; WEAK-LENSING MAPS; BARYON ACOUSTIC-OSCILLATIONS; STAR-FORMATION HISTORIES; ULTIMATE HALO MASS; SDSS-III; FIELD GALAXIES; ASSEMBLY GAMA; DATA RELEASE AB During the last three decades progress in mapping the Universe from an age of 400 000 years to the present has been stunning. Instrument/telescope combinations have naturally determined the sampling of various redshift ranges. Here we outline the impact of the Hectospec on the MMT on exploration of the Universe in the redshift range 0.2 less than or similar to z less than or similar to 0.8. We focus on dense redshift surveys, SHELS and HectoMAP. SHELS is a complete magnitude limited survey covering 8 square degrees. The HectoMAP survey combines a red-selected dense redshift survey and a weak lensing map covering 50 square degrees. Combining the dense redshift survey with a Subaru HyperSuprimeCam (HSC) weak lensing map will provide a powerful probe of the way galaxies trace the distribution of dark matter on a wide range of physical scales. ((c) 2015 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Geller, Margaret J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hwang, Ho Seong] Korea Inst Adv Study, Seoul 130722, South Korea. RP Geller, MJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu NR 53 TC 3 Z9 3 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA POSTFACH 101161, 69451 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD JUL PY 2015 VL 336 IS 5 BP 428 EP 436 DI 10.1002/asna.201512182 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM8ND UT WOS:000357957500002 ER PT J AU Helbig-Bonitz, M Ferger, SW Bohning-Gaese, K Tschapka, M Howell, K Kalko, EKV AF Helbig-Bonitz, Maria Ferger, Stefan W. Boehning-Gaese, Katrin Tschapka, Marco Howell, Kim Kalko, Elisabeth K. V. TI Bats are Not Birds - Different Responses to Human Land-use on a Tropical Mountain SO BIOTROPICA LA English DT Article DE Africa; agriculture; biodiversity conservation; community ecology; driving factors; Kilimanjaro; landscape management ID 2 CONTRASTING LANDSCAPES; SHADE CACAO PLANTATIONS; AGRICULTURAL INTENSIFICATION; INSECTIVOROUS BATS; BIODIVERSITY HOTSPOTS; SPECIES RICHNESS; HUMAN-POPULATION; ATLANTIC FOREST; CLIMATE-CHANGE; RAIN-FOREST AB Land-use intensification has consequences for biodiversity and ecosystem functioning, with various taxonomic groups differing widely in their sensitivity. As land-use intensification alters habitat structure and resource availability, both factors may contribute to explaining differences in animal species diversity. Within the local animal assemblages the flying vertebrates, bats and birds, provide important and partly complementary ecosystem functions. We tested how bats and birds respond to land-use intensification and compared abundance, species richness, and community composition across a land-use gradient including forest, traditional agroforests (home garden), coffee plantations and grasslands on Mount Kilimanjaro, Tanzania. Furthermore, we asked how sensitive different habitat and feeding guilds of bats and birds react to land-use intensification and the associated alterations in vegetation structure and food resource availability. In contrast to our expectations, land-use intensification had no negative effect on species richness and abundance of all birds and bats. However, some habitat and feeding guilds, in particular forest specialist and frugivorous birds, were highly sensitive to land-use intensification. Although the habitat guilds of both, birds and bats, depended on a certain degree of vegetation structure, total bat and bird abundance was mediated primarily by the availability of the respective food resources. Even though the highly structured southern slopes of Mount Kilimanjaro are able to maintain diverse bat and bird assemblages, the sensitivity of avian forest specialists against land-use intensification and the dependence of the bat and bird habitat guilds on a certain vegetation structure demonstrate that conservation plans should place special emphasis on these guilds. C1 [Helbig-Bonitz, Maria; Tschapka, Marco; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Ferger, Stefan W.; Boehning-Gaese, Katrin] Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany. [Ferger, Stefan W.; Boehning-Gaese, Katrin] Senckenberg Gesell Nat Forsch, D-60325 Frankfurt, Germany. [Boehning-Gaese, Katrin] Goethe Univ Frankfurt, Inst Ecol Evolut & Divers, D-60439 Frankfurt, Germany. [Tschapka, Marco; Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Howell, Kim] Univ Dar Es Salaam, Dept Zool & Wildlife Conservat, Dar Es Salaam, Tanzania. RP Helbig-Bonitz, M (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM maria.helbig@uni-ulm.de FU DFG Research Group 'KiLi' [KA-1241/1 7-1, Bo-1221/16-1] FX We thank all our collaborators from the KiLi-Project, especially G. Rutten, A. Ensslin, A. Hemp and M. Fischer for detailed information on tree density, T. Appelhans and T. Nauss for climate data as well as R. S. Mary for his commitment during fieldwork. We are very grateful for stimulating discussions with J. Fahr, K. Jung and S. Renner, as well as for support in acoustic data analysis by T. Bosch, N. Weber and V. Zeus. The work of M. H.-B. and S. W. F. was funded by the DFG Research Group 'KiLi' (KA-1241/1 7-1, Bo-1221/16-1). Research permission in Tanzania was given by COSTECH (2010-340-ER-NA-96-44, 2011-340-ER-96-44), TANAPA and TAWIRI (TNO/HQ/C.10/13/VOL.III). This study is a contribution of the DFG Research Group 'Kilimanjaro ecosystems under global change: Linking biodiversity, biotic interactions and biogeochemical ecosystem processes'. NR 70 TC 2 Z9 2 U1 6 U2 57 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD JUL PY 2015 VL 47 IS 4 BP 497 EP 508 DI 10.1111/btp.12221 PG 12 WC Ecology SC Environmental Sciences & Ecology GA CM8RW UT WOS:000357970700014 ER PT J AU Meyer, NFV Esser, HJ Moreno, R van Langevelde, F Liefting, Y Oller, DR Vogels, CBF Carver, AD Nielsen, CK Jansen, PA AF Meyer, Ninon F. V. Esser, Helen J. Moreno, Ricardo van Langevelde, Frank Liefting, Yorick Oller, David Ros Vogels, Chantal B. F. Carver, Andrew D. Nielsen, Clayton K. Jansen, Patrick A. TI An assessment of the terrestrial mammal communities in forests of Central Panama, using camera-trap surveys SO JOURNAL FOR NATURE CONSERVATION LA English DT Article DE Community surveys; Connectivity; Darien; Evenness; Fragmentation; Mesoamerican biological corridor; Species richness ID RAIN-FOREST; HABITAT FRAGMENTATION; CONSERVATION STATUS; NEOTROPICAL FOREST; ATLANTIC FOREST; TAYASSU-PECARI; ABUNDANCE; BIODIVERSITY; LANDSCAPE; DENSITY AB The Isthmus of Panama, part of the planet's third largest megadiversity hotspot, and connecting the faunas of North and South America, has lost more than half of its forest due to agriculture and economic development. It is unknown to what degree the remaining forest, which is fragmented and subject to poaching, still supports the wildlife diversity found in intact forests. Here, we use camera-trap surveys to assess whether forests in Central Panama, the narrowest and most disturbed portion of the Isthmus, still have intact communities of medium- and large-bodied terrestrial mammals. During 2005-2014, we collected camera-trap survey data from 15 national parks and forest fragments on both sides of the Panama Canal, and compared these to similar data from two sites in the intact Darien National Park in Eastern Panama, the nearest available reference. We found that most sites in Central Panama - including some of the national parks - had lower mammal species richness and evenness than the reference sites, and less structurally-complex mammal communities. Forests in Central Panama had little or no apex predators and large terrestrial frugivores, with the exception of two sites directly connected to the reference site. Our results indicate that the terrestrial mammal community in forests of Central Panama is currently degraded, even inside national parks. These data provide a baseline for evaluating the success of conservation efforts to prevent the Panamanian Isthmus to become a bottleneck for movement of animals. (C) 2015 Elsevier GmbH. All rights reserved. C1 [Meyer, Ninon F. V.; Esser, Helen J.; Moreno, Ricardo; Liefting, Yorick; Oller, David Ros; Vogels, Chantal B. F.; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Meyer, Ninon F. V.; Esser, Helen J.; van Langevelde, Frank; Liefting, Yorick; Oller, David Ros; Vogels, Chantal B. F.; Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Meyer, Ninon F. V.; Moreno, Ricardo] Yaguara Panama, Soc Panamena Biol, San Francisco, Panama. [Carver, Andrew D.; Nielsen, Clayton K.] So Illinois Univ, Dept Forestry, Carbondale, IL 62901 USA. [Carver, Andrew D.; Nielsen, Clayton K.] So Illinois Univ, Cooperat Wildlife Lab, Carbondale, IL 62901 USA. [Carver, Andrew D.] Asociac Panamer Conservac, Gamboa Resort 0265, Colon, Panama. RP Meyer, NFV (reprint author), Yaguara Panama Soc Panamena Biol, Calle 71,Chalet 50, Panama City, Panama. EM ninonmeyer@gmail.com RI Vogels, Chantal/N-1749-2015; OI Vogels, Chantal/0000-0003-0027-6480; Van Langevelde, Frank/0000-0001-8870-0797 FU Gorden and Betty Moore Foundation; Smithsonian Institution; Graduate school of production Ecology and Resource Conservation; Kaplan Award Program and Ancon Expedition Panam; Jaguar Conservation Fund of Panthera; APPC; GEMAS/Fondo Darien (USA embassy/TNC/Ministerio de economia y finanzas/ANAM/Fundes/Panamcham/Fundacion Natura) FX We thank the students of the University of Panama, the University of Wageningen and Van Hall Larenstein, the interns and fellows of STRI, the BCI game wardens, the policemen of Gamboa, and the Emberas of Pijibasal for field assistance; H. Rissanen, M. Roy and all local land owners for providing housing and access to forest fragments; the Ministerio de Ambiente de Panama, Smithsonian Tropical Research Institute (STRI), Primate Conservation Inc, and CREA for logistical support and permits; S. Valdez, M. Torres and C. Chang from the Sociedad Panamena de Biologia for the data of San Lorenzo; J. Willis for valuable information. The data of BCNM and Soberania were collected as part of the Tropical Ecology Assessment and Monitoring Network, a collaboration between Conservation International, the Missouri Botanical Garden, the Smithsonian Institution, and the Wildlife Conservation Society, and partially funded by these institutions, the Gorden and Betty Moore Foundation, and other donors. This study was partly funded by the Smithsonian Institution (Grand Challenges Award to PAJ), the Graduate school of production Ecology and Resource Conservation (PAJ and HJE), the Kaplan Award Program and Ancon Expedition Panam (RM), the Jaguar Conservation Fund of Panthera (CKN, RM, ADC), APPC, and GEMAS/Fondo Darien (USA embassy/TNC/Ministerio de economia y finanzas/ANAM/Fundes/Panamcham/Fundacion Natura) (RM). Finally, we thank two anonymous reviewers for comments on a previous version of the manuscript. NR 48 TC 2 Z9 4 U1 12 U2 63 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1617-1381 EI 1618-1093 J9 J NAT CONSERV JI J. Nat. Conserv. PD JUL PY 2015 VL 26 BP 28 EP 35 DI 10.1016/j.jnc.2015.04.003 PG 8 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CN0JP UT WOS:000358100200004 ER PT J AU Touchton, JM Wikelski, M AF Touchton, Janeene M. Wikelski, Martin TI Ecological opportunity leads to the emergence of an alternative behavioural phenotype in a tropical bird SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE alternative behavioural phenotypes; ant-following birds; behavioural diversification; competitive release; ecological opportunity; Hylophylax naevioides; individual differences; territorial breakdown ID CHARACTER DISPLACEMENT; RESOURCE POLYMORPHISM; ADAPTIVE RADIATIONS; EVOLUTION; PLASTICITY; POPULATION; ANTS; DIVERSIFICATION; COMPETITION; DISPERSAL AB 1. Loss of a dominant competitor can open ecological opportunities. Ecological opportunities are considered prerequisites for adaptive radiations. Nonetheless, initiation of diversification in response to ecological opportunity is seldom observed, so we know little about the stages by which behavioural variation either increases or coalesces into distinct phenotypes. 2. Here, a natural experiment showed that in a tropical island's guild of army ant-following birds, a new behavioural phenotype emerged in subordinate spotted antbirds (Hylophylax naevioides) after the socially dominant ocellated antbird (Phaenostictus mcleannani) died out. 3. Individuals with this behavioural phenotype are less territorial; instead, they roam in search of ant swarms where they feed in locations from which dominant competitors formerly excluded them. Roaming individuals fledge more young than territorial individuals. 4. We conclude that ecological opportunity arising from species loss may enhance the success of alternative behavioural phenotypes and can favour further intraspecific diversification in life-history traits in surviving species. C1 [Touchton, Janeene M.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Touchton, Janeene M.; Wikelski, Martin] Max Planck Inst Ornithol, D-78315 Radolfzell am Bodensee, Germany. [Touchton, Janeene M.] Smithsonian Trop Res Inst, Panama City, Panama. [Wikelski, Martin] Univ Konstanz, Dept Biol, D-78457 Constance, Germany. RP Touchton, JM (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, 106A Guyot Hall, Princeton, NJ 08544 USA. EM touchtonj@gmail.com FU Princeton University; Smithsonian Tropical Research Institute; Max Planck Institute for Ornithology at Radolfzell, Germany; Konstanz University, Germany FX We thank L. Caro, I. Diaz, H. Arias, M. Rodriguez, D. Garcia, D. Martinez, E. Hurme, M. Smith, J. Moxley, R. Zambrano and C. Ziegler for field assistance. M Hau, H. Horn, E. Leigh Jr., J. Tobias, MJ. West-Eberhard, C. Ziegler and four anonymous reviewers provided helpful discussion and clarification of the manuscript. This research was conducted under research permits by Autoridad Nacional del Ambiente (SE/A-61-09), Panama and The Smithsonian Tropical Research Institute's Animal Care and Use Committee (07-06-24-08). Logistical and financial support was provided by Princeton University, The Smithsonian Tropical Research Institute, The Max Planck Institute for Ornithology at Radolfzell, Germany, and Konstanz University, Germany. NR 57 TC 0 Z9 0 U1 5 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8790 EI 1365-2656 J9 J ANIM ECOL JI J. Anim. Ecol. PD JUL PY 2015 VL 84 IS 4 BP 1041 EP 1049 DI 10.1111/1365-2656.12341 PG 9 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA CM6QK UT WOS:000357813500016 PM 25640464 ER PT J AU Peterson, PM Romaschenko, K Arrieta, YH AF Peterson, Paul M. Romaschenko, Konstantin Herrera Arrieta, Yolanda TI Phylogeny and subgeneric classification of Bouteloua with a new species, B-herrera-arrietae (Poaceae: Chloridoideae: Cynodonteae: Boutelouinae) SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE Bouteloua; classification; DNA; ITS; phylogeny; plastid DNA sequences ID MOLECULAR PHYLOGENY; MEXICAN GRASSES; DNA-SEQUENCES; INCONGRUENCE; GRAMINEAE; NETWORKS; RECOVERY; COMPLEX; DIOECY; TREES AB Bouteloua (Poaceae: Chloridoideae: Cynodonteae; Boutelouiane) is an important genus of forage grasses containing 60 species found primarily in the Americas with a center of diversity in northern Mexico. A modern subgeneric classification is lacking. The goals of our study were to reconstruct the evolutionary history among the species of Bouteloua using molecular data with increased species sampling compared to previous studies. A phylogenetic analysis was conducted on 209 samples, of which 59 species (206 individuals) were in Bouteloua, using two plastid (rpl32-trnL spacer and rps16-trnK spacer) and nuclear ITS 1&2 (ribosomal internal transcribed spacer) sequences to infer evolutionary relationships and produce a subgeneric classification. Overall, ITS and plastid phylogenies rendered similar patterns. However, the ITS phylogeny lacked backbone structure, recovering only four internal clades out of nine found in the plastid phylogeny. The ITS network shows a radiative evolutionary pattern and indicates a number of incompatible splits, suggesting past hybridization between species of different sections. The maximum-likelihood tree from the combined plastid and ITS regions is well resolved and depicts a strongly supported monophyletic Bouteloua that includes ten strongly supported clades and one moderately supported clade. The molecular results support the recognition of 10 sections and two subsections within Bouteloua s.l.; three sections are new: Barbata, Hirsuta, and Trifida; four sections are new combinations: Buchloe, Cyclostachya, Opizia, and Triplathera; and two subsections are new: Eriopoda and Hirsuta. Based on our molecular results and the possession of unique morphological characters we describe a new species from Nuevo Leon, Boutelouaherrera-arrietae. C1 [Peterson, Paul M.; Romaschenko, Konstantin] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Romaschenko, Konstantin] Natl Acad Sci, MG Kholodny Inst Bot, UA-01601 Kiev, Ukraine. [Herrera Arrieta, Yolanda] Inst Politecn Nacl, CIIDIR Unidad Durango COFAA, Durango 34220, Mexico. RP Peterson, PM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM peterson@si.edu RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 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 for many extended discussions pertinent to the manuscript; Alice Tangerini for preparing the illustration; Laurence J. Dorr for checking the taxonomy section; and Neil Snow and Joseph K. Wipff for providing helpful comments on the manuscript. NR 75 TC 2 Z9 2 U1 4 U2 10 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 JUL PY 2015 VL 53 IS 4 BP 351 EP 366 DI 10.1111/jse.12159 PG 16 WC Plant Sciences SC Plant Sciences GA CM8NU UT WOS:000357959700008 ER PT J AU Vogler, RE Beltramino, AA Strong, EE Peso, JG Rumi, A AF Vogler, Roberto E. Beltramino, Ariel A. Strong, Ellen E. Peso, Juana G. Rumi, Alejandra TI A phylogeographical perspective on the ex situ conservation of Aylacostoma (Thiaridae, Gastropoda) from the High Parana River (Argentina-Paraguay) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE conservation genetics; endangered freshwater snails; evolutionarily significant units; haplotypes; molecular divergence ID FRESH-WATER; MAXIMUM-LIKELIHOOD; POPULATION-GROWTH; DNA POLYMORPHISM; SNAIL; MOLLUSKS; GENETICS; PHYLOGENIES; SOFTWARE; MODEL AB Aylacostoma Spix, 1827, contains species that are the subject of focused conservation efforts under the auspices of the 'Aylacostoma Project', the only ex situ conservation programme for freshwater gastropods in South America. Two species from the High Parana River (Argentina-Paraguay) are included in this programme (Aylacostoma chloroticum Hylton Scott, 1954 and Aylacostoma brunneum Vogler & Peso, 2014), as their habitats have disappeared as a consequence of the filling of the Yacyreta Reservoir in the 1990s. At present, A. chloroticum is restricted to only one known wild population in a small and fragile habitat, and wild populations of A. brunneum are presumed to have gone extinct. We used partial sequences of the cytochrome oxidase subunit I gene to provide the first phylogeographical perspective on these species from a limited dataset containing representatives of several wild populations that are successfully being bred in captivity. We found low genetic diversity and two haplotypes in A. chloroticum, and absence of variation with one haplotype in A. brunneum. The reservoir's entry zone was identified to be of great interest for conservation, and is where we suggest re-introductions and translocations should be targeted, to preserve the future evolutionary potential of the extant diversity. (C) 2015 The Linnean Society of London. C1 [Vogler, Roberto E.; Peso, Juana G.] Univ Nacl Misiones, Fac Ciencias Exactas Quim & Nat, Dept Biol, Posadas, Argentina. [Vogler, Roberto E.; Beltramino, Ariel A.; Rumi, Alejandra] Consejo Nacl Invest Cient & Tecn, RA-1033 Buenos Aires, DF, Argentina. [Beltramino, Ariel A.; Rumi, Alejandra] Univ Nacl La Plata, Fac Ciencias Nat & Museo, Div Zool Invertebrados, La Plata, Buenos Aires, Argentina. [Strong, Ellen E.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Vogler, RE (reprint author), Univ Nacl Misiones, Fac Ciencias Exactas Quim & Nat, Dept Biol, Rivadavia 2370,N3300LDX, Posadas, Argentina. EM robertovogler@fceqyn.unam.edu.ar OI Beltramino, Ariel/0000-0002-0052-6710; Vogler, Roberto/0000-0001-9660-552X FU Conservation, Research and Education Opportunities International (CREOI) FX We thank Conservation, Research and Education Opportunities International (CREOI) for partially funding this study. We are especially grateful to Maria Jose Molina for providing the pictures of living Aylacostoma specimens. NR 72 TC 1 Z9 1 U1 0 U2 5 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 JUL PY 2015 VL 174 IS 3 BP 487 EP 499 DI 10.1111/zoj.12250 PG 13 WC Zoology SC Zoology GA CM5SM UT WOS:000357748900005 ER PT J AU Comizzoli, P AF Comizzoli, Pierre TI Biobanking efforts and new advances in male fertility preservation for rare and endangered species SO ASIAN JOURNAL OF ANDROLOGY LA English DT Review DE conservation; cryobiology; endangered species; male fertility; spermatozoa ID ASSISTED REPRODUCTIVE TECHNOLOGIES; PANDA AILUROPODA-MELANOLEUCA; BLACK-FOOTED FERRET; ARTIFICIAL-INSEMINATION; ELEPHAS-MAXIMUS; SUCCESSFUL CRYOPRESERVATION; SPERM CRYOPRESERVATION; SPERMATOZOA; CONSERVATION; WILD AB Understanding and sustaining biodiversity is a multi-disciplinary science that benefits highly from the creation of organized and accessible collections of biomaterials (Genome Resource Banks). Large cryo-collections are invaluable tools for understanding, cataloging, and protecting the genetic diversity of the worlds unique animals and plants. Specifically, the systematic collection and preservation of semen from rare species has been developed significantly in recent decades with some biobanks now being actively used for endangered species management and propagation (including the introduction of species such as the black-footed ferret and the giant panda). Innovations emerging from the growing field of male fertility preservation for humans, livestock species, and laboratory animals are also becoming relevant to the protection and the propagation of valuable domestic and wild species. These new approaches extend beyond the "classical" methods associated with sperm freezing to include testicular tissue preservation combined with xenografting or in vitro culture, all of which have potential for rescuing vast amounts of unused germplasm. There also are other options under development that are predicted to have a high impact within the next decade (stem cell technologies, bio-stabilization of sperm cells at ambient temperatures, and the use of genomics tools). However, biobanking efforts and new fertility preservation strategies have to expand the way beyond mammalian species, which will offer knowledge and tools to better manage species that serve as valuable biomedical models or require assistance to reverse endangerment. C1 Vet Hosp, Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Comizzoli, P (reprint author), Vet Hosp, Natl Zool Pk, Smithsonian Conservat Biol Inst, POB 37012, Washington, DC 20013 USA. EM comizzolip@si.edu NR 64 TC 5 Z9 5 U1 6 U2 46 PU MEDKNOW PUBLICATIONS & MEDIA PVT LTD PI MUMBAI PA B-9, KANARA BUSINESS CENTRE, OFF LINK RD, GHAKTOPAR-E, MUMBAI, 400075, INDIA SN 1008-682X EI 1745-7262 J9 ASIAN J ANDROL JI Asian J. Androl. PD JUL PY 2015 VL 17 IS 4 BP 640 EP 645 DI 10.4103/1008-682X.153849 PG 6 WC Andrology; Urology & Nephrology SC Endocrinology & Metabolism; Urology & Nephrology GA CL9HR UT WOS:000357288800019 PM 25966625 ER PT J AU Currie, T Lisse, CM Kuchner, M Madhusudhan, N Kenyon, SJ Thalmann, C Carson, J Debes, J AF Currie, Thayne Lisse, Carey M. Kuchner, Marc Madhusudhan, Nikku Kenyon, Scott J. Thalmann, Christian Carson, Joseph Debes, John TI DIRECT IMAGING AND SPECTROSCOPY OF A YOUNG EXTRASOLAR KUIPER BELT IN THE NEAREST OB ASSOCIATION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: early-type; stars: individual (HD 115600) ID DEBRIS DISK; HR 4796A; EVOLUTIONARY MODELS; SCORPIUS-CENTAURUS; CIRCUMSTELLAR DISK; PLANET FORMATION; BURNING LIMIT; MAIN-SEQUENCE; STARS; SYSTEM AB We describe the discovery of a bright, young Kuiper belt-like debris disk around HD 115600, a similar to 1.4-1.5 M-circle dot, similar to 15 Myr old member of the Sco-Cen OB Association. Our H-band coronagraphy/integral field spectroscopy from the Gemini Planet Imager shows the ring has a (luminosity-scaled) semimajor axis of (similar to 22 AU) similar to 48 AU, similar to the current Kuiper belt. The disk appears to have neutral-scattering dust, is eccentric (e similar to 0.1-0.2), and could be sculpted by analogs to the outer solar system planets. Spectroscopy of the disk ansae reveal a slightly blue to gray disk color, consistent with major Kuiper belt chemical constituents, where water ice is a very plausible dominant constituent. Besides being the first object discovered with the next generation of extreme adaptive optics systems (i.e., SCExAO, GPI, SPHERE), HD 115600's debris ring and planetary system provide a key reference point for the early evolution of the solar system, the structure, and composition of the Kuiper belt and the interaction between debris disks and planets. C1 [Currie, Thayne] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Kuchner, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Madhusudhan, Nikku] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Thalmann, Christian] ETH, Zurich, Switzerland. [Carson, Joseph] Coll Charleston, Dept Phys & Astron, Charleston, SC 29401 USA. [Debes, John] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Currie, T (reprint author), Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, 650 N Aohoku Pl, Hilo, HI 96720 USA. RI Lisse, Carey/B-7772-2016 OI Kenyon, Scott/0000-0003-0214-609X; Lisse, Carey/0000-0002-9548-1526 FU GPI Early Science Time Allocation Committee; Gemini Director Markus Kissler-Patig FX We thank the anonymous referee, Wladimir Lyra, Eric Mamajek, and Mengshu Xu for helpful comments; Fredrik Rantakryo for executing these queue-mode observations; and the GPI Early Science Time Allocation Committee and Gemini Director Markus Kissler-Patig for supporting this program. NR 46 TC 14 Z9 14 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 JUL 1 PY 2015 VL 807 IS 1 AR L7 DI 10.1088/2041-8205/807/1/L7 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL8YY UT WOS:000357262100007 ER PT J AU Garraffo, C Drake, JJ Cohen, O AF Garraffo, Cecilia Drake, Jeremy J. Cohen, Ofer TI MAGNETIC COMPLEXITY AS AN EXPLANATION FOR BIMODAL ROTATION POPULATIONS AMONG YOUNG STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: evolution; stars: magnetic field; stars: rotation ID LOW-MASS STARS; SUN-LIKE STARS; ANGULAR-MOMENTUM; MAIN-SEQUENCE; SOLAR-TYPE; EVOLUTION; BRAKING; FIELDS; PLEIADES; VELOCITIES AB Observations of young open clusters have revealed a bimodal distribution of fast and slower rotation rates that has proven difficult to explain with predictive models of spin down that depend on rotation rates alone. The Metastable Dynamo Model proposed recently by Brown, employing a stochastic transition probability from slow to more rapid spin down regimes, appears to be more successful but lacks a physical basis for such duality. Using detailed 3D MHD wind models computed for idealized multipole magnetic fields, we show that surface magnetic field complexity can provide this basis. Both mass and angular momentum losses decline sharply with increasing field complexity. Combined with observation evidence for complex field morphologies in magnetically active stars, our results support a picture in which young, rapid rotators lose angular momentum in an inefficient way because of field complexity. During this slow spin-down phase, magnetic complexity is eroded, precipitating a rapid transition from weak to strong wind coupling. C1 [Garraffo, Cecilia; Drake, Jeremy J.; Cohen, Ofer] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Garraffo, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Cohen, Ofer/0000-0003-3721-0215 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?"; NASA [NAS8-03060]; NASA HEC Pleiades system [SMD-13-4526] FX 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?." J.J.D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center. Numerical simulations were performed on the NASA HEC Pleiades system under award SMD-13-4526. NR 28 TC 10 Z9 10 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 JUL 1 PY 2015 VL 807 IS 1 AR L6 DI 10.1088/2041-8205/807/1/L6 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL8YY UT WOS:000357262100006 ER PT J AU Graninger, D Oberg, KI Qi, CH Kastner, J AF Graninger, Dawn Oeberg, Karin I. Qi, Chunhua Kastner, Joel TI HNC IN PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; ISM: molecules; protoplanetary disks ID CO SNOW LINE; ROTATIONAL-EXCITATION; TW HYA; CHEMISTRY; HCN; EVOLUTION; N2H+; ABUNDANCE; MODELS; CLOUDS AB The distributions and abundances of small organics in protoplanetary disks are potentially powerful probes of disk physics and chemistry. HNC is a common probe of dense interstellar regions and the target of this study. We use the Submillimeter Array (SMA) to observe HNC 3-2 toward the protoplanetary disks around the T Tauri star TW Hya and the Herbig Ae star HD 163296. HNC is detected toward both disks, constituting the first spatially resolved observations of HNC in disks. We also present SMA observations of HCN 3-2 and IRAM 30 m observations of HCN and HNC 1-0 toward HD 163296. The disk-averaged HNC/HCN emission ratio is 0.1-0.2 toward both disks. Toward TW Hya, the HNC emission is confined to a ring. The varying HNC abundance in the TW Hya disk demonstrates that HNC chemistry is strongly linked to the disk physical structure. In particular, the inner rim of the HNC ring can be explained by efficient destruction of HNC at elevated temperatures, similar to what is observed in the ISM. However, to realize the full potential of HNC as a disk tracer requires a combination of high SNR spatially resolved observations of HNC and HCN and disk-specific HNC chemical modeling. C1 [Graninger, Dawn; Oeberg, Karin I.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kastner, Joel] Rochester Inst Technol, Sch Phys & Astron, Ctr Imaging Sci, Rochester, NY 14623 USA. [Kastner, Joel] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. RP Graninger, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dgraninger@cfa.harvard.edu OI Kastner, Joel/0000-0002-3138-8250 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Simons Collaboration on the Origins of Life Investigator award [321183]; Alfred P. Sloan Foundation; David and Lucile Packard Foundation; National Science Foundation [AST-1108950]; Smithsonian Institution; Academia Sinica FX This work has benefited from discussions with Sean Andrews, David Wilner, Ryan Loomis, and Eric Herbst and helpful comments from the anonymous referee. 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 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 had the opportunity to conduct observations from this mountain. The study is also based on observations with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). K.I.O. acknowledges funding from the Simons Collaboration on the Origins of Life Investigator award #321183, the Alfred P. Sloan Foundation, and the David and Lucile Packard Foundation. J.K.'s research on nearby, irradiated disks is supported by National Science Foundation grant AST-1108950 to RIT. NR 33 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 JUL 1 PY 2015 VL 807 IS 1 AR L15 DI 10.1088/2041-8205/807/1/L15 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL8YY UT WOS:000357262100015 ER PT J AU Yang, Y Li, ZY Sjouwerman, LO Wang, QD Gu, QS Kraft, RP Yuan, F AF Yang, Yang Li, Zhiyuan Sjouwerman, Lorant O. Wang, Q. Daniel Gu, Qiusheng Kraft, Ralph P. Yuan, Feng TI DETECTION OF A COMPACT NUCLEAR RADIO SOURCE IN THE LOCAL GROUP ELLIPTICAL GALAXY M32 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (M32); galaxies: nuclei; radio continuum: galaxies ID SUPERMASSIVE BLACK-HOLE; ACTIVE GALACTIC NUCLEI; SAGITTARIUS-A-ASTERISK; X-RAY; FUNDAMENTAL PLANE; ACCRETION; MASS; VARIABILITY; POPULATION; EVOLUTION AB The Local Group compact elliptical galaxy M32 hosts one of the nearest candidate supermassive black holes (SMBHs), which has a previously suggested X-ray counterpart. Based on sensitive observations taken with the Karl G. Jansky Very Large Array (VLA), we detect for the first time a compact radio source coincident with the nucleus of M32, which exhibits an integrated flux density of similar to 47.3. +/- 6.1 mu Jy at 6.6 GHz. We discuss several possibilities for the nature of this source, favoring an origin of the long-sought radio emission from the central SMBH, for which we also revisit the X-ray properties based on recently acquired Chandra and XMM-Newton data. Our VLA observations also discover radio emission from three previously known optical planetary nebulae in the inner region of M32. C1 [Yang, Yang; Li, Zhiyuan; Wang, Q. Daniel; Gu, Qiusheng] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Yang, Yang; Li, Zhiyuan; Gu, Qiusheng] Nanjing Univ, Key Lab Modern Astron & Astrophys, Nanjing 210093, Jiangsu, Peoples R China. [Yang, Yang; Li, Zhiyuan; Gu, Qiusheng] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China. [Sjouwerman, Lorant O.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kraft, Ralph P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yuan, Feng] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. RP Yang, Y (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. EM lizy@nju.edu.cn FU National Natural Science Foundation of China [11473010, 11133001]; Recruitment Program of Global Youth Experts FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. We thank M. Sarzi for valuable comments on the SAURON observations of PNe in M32. This work was partially supported by the National Natural Science Foundation of China (grants 11473010 and 11133001). Y.Y. is indebted to the hospitality of NRAO during her visit. Z.L. acknowledges support from the Recruitment Program of Global Youth Experts. NR 36 TC 3 Z9 3 U1 1 U2 3 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 JUL 1 PY 2015 VL 807 IS 1 AR L19 DI 10.1088/2041-8205/807/1/L19 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL8YY UT WOS:000357262100019 ER PT J AU Pasquini, SC Wright, SJ Santiago, LS AF Pasquini, Sarah C. Wright, S. Joseph Santiago, Louis S. TI Lianas always outperform tree seedlings regardless of soil nutrients: results from a long-term fertilization experiment SO ECOLOGY LA English DT Article DE Barro Colorado Nature Monument; Panama; chlorophyll fluorescence; fertilization; lianas; Neotropics; nitrogen; nutrient limitation; phosphorus; photosynthetic performance; plant architecture and morphology; potassium; tropical forest ID LOWLAND TROPICAL FOREST; RAIN-FOREST; CHLOROPHYLL FLUORESCENCE; ABOVEGROUND BIOMASS; GROWTH-RESPONSES; NATIONAL-PARK; LEAF; NITROGEN; PHOSPHORUS; PLANTS AB Lianas are a prominent growth form in tropical forests, and there is compelling evidence that they are increasing in abundance throughout the Neotropics. While recent evidence shows that soil resources limit tree growth even in deep shade, the degree to which soil resources limit lianas in forest understories, where they coexist with trees for decades, remains unknown. Regardless, the physiological underpinnings of soil resource limitation in deeply shaded tropical habitats remain largely unexplored for either trees or lianas. Theory predicts that lianas should be more limited by soil resources than trees because they occupy the quick-return end of the leaf economic spectrum, characterized by high rates of photosynthesis, high specific leaf area, short leaf life span, affinity to high-nutrient sites, and greater foliar nutrient concentrations. To address these issues, we asked whether soil resources (nitrogen, phosphorus, and potassium), alone or in combination, applied experimentally for more than a decade would cause significant changes in the morphology or physiology of tree and liana seedlings in a lowland tropical forest. We found evidence for the first time that phosphorus limits the photosynthetic performance of both trees and lianas in deeply shaded understory habitats. More importantly, lianas always showed significantly greater photosynthetic capacity, quenching, and saturating light levels compared to trees across all treatments. We found little evidence for nutrient x growth form interactions, indicating that lianas were not disproportionately favored in nutrient-rich habitats. Tree and liana seedlings differed markedly for six key morphological traits, demonstrating that architectural differences occurred very early in ontogeny prior to lianas finding a trellis (all seedlings were self-supporting). Overall, our results do not support nutrient loading as a mechanism of increasing liana abundance in the Neotropics. Rather, our finding that lianas always outperform trees, in terms of photosynthetic processes and under contrasting rates of resource supply of macronutrients, will allow lianas to increase in abundance if disturbance and tree turnover rates are increasing in Neotropical forests as has been suggested. C1 [Pasquini, Sarah C.; Santiago, Louis S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Wright, S. Joseph; Santiago, Louis S.] Smithsonian Trop Res Inst, Balboa, Panama. RP Pasquini, SC (reprint author), Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. EM sarah.pasquini@email.ucr.edu RI Santiago, Louis/E-3185-2016; Wright, Stuart/M-3311-2013 OI Santiago, Louis/0000-0001-5994-6122; Wright, Stuart/0000-0003-4260-5676 FU Department of Botany and Plant Sciences at the University of California, Riverside, a STRI Short-Term Fellowship; Smithsonian Scholarly Studies program FX We thank Omar Hernandez, Rufino Gonzalez, and David Brassfield (Smithsonian Tropical Research Institute) for help with plant identification, and Juan Carrion (Universidad de Panama) and Eric Griffin (University of Pittsburgh) for field assistance. We would also like to thank Steve Hovick (Ohio State University) and Jonathan Pruitt (University of Pittsburgh) for statistical advice, and Darrel Jenerette (University of California, Riverside), George Vourlitis (Cal State San Marcos), and Walter Carson (University of Pittsburgh) for comments on earlier drafts. We also thank Jack Putz and one anonymous reviewer for their helpful comments. Funding for this research was provided by the Department of Botany and Plant Sciences at the University of California, Riverside, a STRI Short-Term Fellowship to S. C. Pasquini, and by the Smithsonian Scholarly Studies program to S. J. Wright. NR 73 TC 5 Z9 6 U1 14 U2 43 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 JUL PY 2015 VL 96 IS 7 BP 1866 EP 1876 DI 10.1890/14-1660.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CM2QF UT WOS:000357525800014 PM 26378309 ER PT J AU Kurten, EL Wright, SJ Carson, WP AF Kurten, Erin L. Wright, S. Joseph Carson, Walter P. TI Hunting alters seedling functional trait composition in a Neotropical forest SO ECOLOGY LA English DT Article DE defaunation; dispersal; functional traits; hunting; Panama; poaching; seed predation; seedlings; tropical forest ID TROPICAL TREE COMMUNITY; RAIN-FOREST; RECRUITMENT; CONSEQUENCES; DISPERSAL; DIVERSITY; PREDATION; MAMMALS; PANAMA; HERBIVORES AB Defaunation alters trophic interactions between plants and vertebrates, which may disrupt trophic cascades, thereby favoring a subset of plant species and reducing diversity. If particular functional traits characterize the favored plant species, then defaunation may alter community-wide patterns of functional trait composition. Changes in plant functional traits occurring with defaunation may help identify the species interactions affected by defaunation and the potential for other cascading effects of defaunation. We tested the hypotheses that defaunation would (1) disrupt seed dispersal, thereby favoring species whose dispersal agents are not affected (e.g., small birds, bats, and abiotic agents), (2) reduce seed predation, thereby favoring larger-seeded species, and (3) reduce herbivory, thereby favoring species with lower leaf mass per area (LMA), leaf toughness, and wood density. We examined how these six traits responded to vertebrate defaunation caused by hunters or by experimental exclosures among more than 30000 woody seedlings in a lowland tropical moist forest. Exclosures reduced terrestrial frugivores, granivores, and herbivores, while hunters also reduced volant and arboreal frugivores and granivores. The comparison of exclosures and hunting allowed us to parse the impacts of arboreal and volant species (reduced by hunters only) and terrestrial species (reduced by both hunters and exclosures). The loss of terrestrial vertebrates alone had limited effects on plant trait composition. The additional loss of volant and arboreal vertebrates caused significant shifts in plant species composition towards communities with more species dispersed abiotically, including lianas and low wood-density tree species, and fewer species dispersed by large vertebrates. In contrast to previous studies, community seed mass did not decline significantly in hunted sites. Our exclosure results suggest this is because reducing seed predators disproportionately benefits large-seeded species, partially compensating for the reduction of seed dispersers at hunted sites. Our results demonstrate that decreased seed dispersal and seed predation are important determinants of seedling community compositional change as a consequence of defaunation. Defaunation may also negatively impact carbon storage in tropical forests, by favoring lianas and low wood density tree species. C1 [Kurten, Erin L.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. [Carson, Walter P.] Univ Pittsburgh, Dept Biol Sci, Pittsburgh, PA 15260 USA. RP Kurten, EL (reprint author), Stanford Univ, Dept Biol, 371 Serra Mall, Stanford, CA 94305 USA. EM erinkurten@gmail.com RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Smithsonian Tropical Research Institute; NSF [DEB-9527729, DEB-0212054, DEB-0808338]; Theresa Heinz Environmental Scholars program; STRI short-term fellowship program FX We extend our gratitude to the Autoridad Nacional del Ambiente (ANAM) for permitting us to conduct research within the Parque Nacional Soberania. D. Brassfield, D. Urena, and J. Balbuena conducted the seedling censuses in the hunting comparison. A competitive research grant from the Smithsonian Tropical Research Institute to S. J. Wright funded seedling censuses in hunted and protected forests. Comments from D. Ackerly, R. Dirzo, and two anonymous reviewers improved the manuscript. NSF grants DEB-9527729 and DEB-0212054 to WPC funded the exclosure experiment. NSF DEB-0808338, the Theresa Heinz Environmental Scholars program, and the STRI short-term fellowship program provided support to E. L. Kurten. NR 42 TC 7 Z9 7 U1 13 U2 86 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 JUL PY 2015 VL 96 IS 7 BP 1923 EP 1932 DI 10.1890/14-1735.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CM2QF UT WOS:000357525800019 PM 26378314 ER PT J AU Cooper, NW Sherry, TW Marra, PP AF Cooper, Nathan W. Sherry, Thomas W. Marra, Peter P. TI Experimental reduction of winter food decreases body condition and delays migration in a long-distance migratory bird SO ECOLOGY LA English DT Article DE American Redstart; body condition; fat storage; floater; food availability; migration timing; muscle loss; non-breeding season; pectoral muscle; Setophaga ruticilla; space use; trade-off ID GLOBAL CLIMATE-CHANGE; NONBREEDING-SEASON; MIGRANT BIRD; FAT STORAGE; HABITAT SEGREGATION; SPRING DEPARTURE; ARRIVAL DATE; ANNUAL CYCLE; SPACE USE; ABUNDANCE AB Many tropical habitats experience pronounced dry seasons, during which arthropod food availability declines, potentially limiting resident and migratory animal populations. In response to declines in food, individuals may attempt to alter their space use to enhance access to food resources, but may be socially constrained from doing so by con- and heterospecifics. If social constraints exist, food declines should result in decreased body condition. In migratory birds, correlational evidence suggests a link between body condition and migration timing. Poor body condition and delayed migration may, in turn, impact fitness in subsequent seasons via carry-over effects. To determine if winter food availability affects space use, inter- and intraspecific competition, body composition (i.e., mass, fat, and pectoral muscle), and migration timing, we experimentally decreased food availability on individual American Redstart (Setophaga ruticilla) territories in high-quality mangrove habitat. Redstarts on control territories experienced similar to 40% loss of food due to the seasonal nature of the environment. Redstarts on experimental territories experienced similar to 80% declines in food, which closely mimicked natural declines in nearby, low-quality, scrub habitat. Individuals on food-reduced territories did not expand their territories locally, but instead either became non-territorial floaters or remained on territory. Regardless of territorial status, food-reduced American Redstarts all deposited fat compared to control birds. Fat deposits provide insurance against the risk of starvation, but, for American Redstarts, came at the expense of maintaining pectoral muscle. Subsequently, food-reduced American Redstarts experienced, on average, a one-week delay in departure on spring migration, likely due to the loss of pectoral muscle. Thus, our results demonstrate experimentally, for the first time, that declines in winter food availability can result in a fat-muscle trade-off, which, in turn, delays departure on spring migration. Previous work has demonstrated that, for each day delayed after the first male arrival on the breeding grounds, American Redstarts experience an 11% decrease in the chance of successfully reproducing. Therefore, such delays in departure likely lead to fitness costs for migratory birds. Because tropical seasonal forests are expected to become drier in response to global climate change, Neotropical migratory bird populations may experience significant winter food limitation, further exacerbating population declines in the coming decades. C1 [Cooper, Nathan W.; Sherry, Thomas W.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Cooper, Nathan W.; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. RP Cooper, NW (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, Boggs 400, New Orleans, LA 70118 USA. EM nathanwands@gmail.com OI Cooper, Nathan/0000-0002-4667-1542 FU NSF LTREB; Smithsonian predoctoral fellowship FX Four anonymous reviewers provided many helpful comments that improved the manuscript. We thank the Petroleum Corporation of Jamaica and the Jamaican National Environmental Planning Agency for access to field sites and permits. We thank J. Hazlehurst for the American Redstart drawings in Fig. 1. We thank all field assistants for their hard work, and L. Smith and the Whitehouse Football Club for ongoing support. All research was supported by NSF LTREB grants to P. Marra and T. Sherry, and a Smithsonian predoctoral fellowship to N. W. Cooper. NR 62 TC 9 Z9 9 U1 8 U2 77 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUL PY 2015 VL 96 IS 7 BP 1933 EP 1942 DI 10.1890/14-1365.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CM2QF UT WOS:000357525800020 PM 26378315 ER PT J AU Lynn, DH Coats, DW AF Lynn, Denis H. Coats, D. Wayne TI In Memoriam: John O. Corliss (1922-2014) SO JOURNAL OF EUKARYOTIC MICROBIOLOGY LA English DT Biographical-Item ID CILIATED PROTOZOA; REVISED CLASSIFICATION; PHYLUM CILIOPHORA; PROTISTS; BIODIVERSITY; BIOSPHERE C1 [Lynn, Denis H.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. [Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lynn, DH (reprint author), Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. EM lynn@zoology.ubc.ca RI Lynn, Denis/F-4939-2010 OI Lynn, Denis/0000-0002-1554-7792 NR 26 TC 0 Z9 0 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1066-5234 EI 1550-7408 J9 J EUKARYOT MICROBIOL JI J. Eukaryot. Microbiol. PD JUL-AUG PY 2015 VL 62 IS 4 BP 562 EP 565 DI 10.1111/jeu.12212 PG 4 WC Microbiology SC Microbiology GA CL9WO UT WOS:000357329400012 PM 25809661 ER PT J AU Smuts, B Bauer, E Ward, C AF Smuts, Barbara Bauer, Erika Ward, Camille TI Rollovers during play: Complementary perspectives SO BEHAVIOURAL PROCESSES LA English DT Article DE Domestic dogs; Play fighting; Role reversals; Dominance; Tactical maneuvering ID DOMESTIC DOGS; SOCIAL PLAY; FAMILIARIS; RATS AB In this commentary, we compare and contrast Norman et al.s' findings on rollovers during dog play (Norman et al., 2015; the "target article") with our work on dog play fighting (Bauer and Smuts, 2007; Ward et al., 2008). We first review our major findings and then correct some errors in the target article's descriptions of our work. We then further explore the concept of "defensive" rollovers proposed in the target article. We conclude that a combination of the target article's approach and ours should inform future investigations of dog rollovers. (C) 2015 Elsevier B.V. All rights reserved. C1 [Smuts, Barbara; Bauer, Erika; Ward, Camille] Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. [Bauer, Erika] Natl Zoo Smithsonian Inst, Anim Behav Grp, Washington, DC USA. [Ward, Camille] About Dogs LLC, Ann Arbor, MI 48105 USA. RP Smuts, B (reprint author), Univ Michigan, Dept Psychol, Ann Arbor, MI 48109 USA. EM bsmuts@umich.edu NR 16 TC 0 Z9 0 U1 1 U2 11 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0376-6357 EI 1872-8308 J9 BEHAV PROCESS JI Behav. Processes PD JUL PY 2015 VL 116 BP 50 EP 52 DI 10.1016/j.beproc.2015.04.006 PG 3 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA CL5GC UT WOS:000356986800008 PM 25907148 ER PT J AU Singh, RP Shafeeque, CM Sharma, SK Pandey, NK Singh, R Mohan, J Kolluri, G Saxena, M Sharma, B Sastry, KVH Kataria, JM Azeez, PA AF Singh, Ram P. Shafeeque, Chathathayil M. Sharma, Sanjeev K. Pandey, Nitin K. Singh, Renu Mohan, Jag Kolluri, Gautham Saxena, Meeta Sharma, Bhaskar Sastry, Kochiganti V. H. Kataria, Jag M. Azeez, Parappurath A. TI Bisphenol a reduces fertilizing ability and motility by compromising mitochondrial function of sperm SO ENVIRONMENTAL TOXICOLOGY AND CHEMISTRY LA English DT Article DE Sperm viability; Flow cytometer; Mitochondrial membrane potential; Fertility ID SPERMATOZOA; EXPOSURE; CHICKEN AB Bisphenol A (BPA) acts as an endocrine disruptor, affects animal reproductive success in vivo and affects sperm functions in vitro at environmentally relevant concentrations, leading to reduction in sperm motility and fertilizing ability in fish. The effect of in vitro BPA on avian sperm functions has not been explored. The present study examined the effect of environmentally relevant concentrations of BPA (0mM, 0.18mM, 0.37mM, and 0.74mM) on sperm functions in chicken in vitro. Sperm were exposed to concentrations of BPA for 30 min and analyzed for motility, fertilizing ability, live sperm percentage, and mitochondrial membrane potential (m). Results showed that BPA at a concentration of 0.74 mM significantly decreased motility, fertilizing ability, live sperm count percentage, and sperm m. Sperm motility was positively correlated with fertility (r =0.73, p 0.01), live sperm percentage (r=0.64, p0.01), and high m (r=0.44, p0.01). A dose-dependent and time-dependent effect of BPA was observed on sperm motility at all BPA concentrations. However, sperm's fertilizing ability was unaffected in low BPA concentration (0.18mM and 0.37mM). A significantly higher percentage of moribund sperm was observed at 0.37mM and 0.74mM BPA compared with at 0.18mM BPA, in the negative control, and in the vehicle control. The present study confirms that environmentally relevant concentrations of BPA are capable of compromising sperm functions, leading to reduction in fertilizing ability of chicken sperm. Environ Toxicol Chem 2015;34:1617-1622. (c) 2015 SETAC C1 [Singh, Ram P.; Shafeeque, Chathathayil M.; Azeez, Parappurath A.] Salim Ali Ctr Ornithol & Nat Hist, Avian Physiol & Genet Div, Coimbatore, Tamil Nadu, India. [Singh, Ram P.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Sharma, Sanjeev K.; Pandey, Nitin K.; Mohan, Jag; Kolluri, Gautham; Sastry, Kochiganti V. H.; Kataria, Jag M.] Cent Avian Res Inst, Div Physiol & Reprod, Izatnagar, Uttar Pradesh, India. [Saxena, Meeta; Sharma, Bhaskar] Indian Vet Res Inst, Div Biochem, Izatnagar 243122, Uttar Pradesh, India. [Singh, Renu] Indian Vet Res Inst, Div Physiol & Climatol, Izatnagar 243122, Uttar Pradesh, India. RP Singh, RP (reprint author), Salim Ali Ctr Ornithol & Nat Hist, Avian Physiol & Genet Div, Coimbatore, Tamil Nadu, India. EM rampratapsingh81@gmail.com OI Sharma, Sanjeev Kumar/0000-0002-3273-0708 FU SERB, Department of Science and Technology, Government of India [SERB/FT/LS-147/2011] FX The present work was supported by SERB, Department of Science and Technology, Government of India (SERB/FT/LS-147/2011). There is no conflict of interest, and all the authors agree with the publication conditions of the journal. NR 19 TC 3 Z9 3 U1 6 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0730-7268 EI 1552-8618 J9 ENVIRON TOXICOL CHEM JI Environ. Toxicol. Chem. PD JUL PY 2015 VL 34 IS 7 BP 1617 EP 1622 DI 10.1002/etc.2957 PG 6 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA CL5QC UT WOS:000357013700024 PM 25728985 ER PT J AU Kawashima, T Thorington, RW Bohaska, PW Chen, YJ Sato, F AF Kawashima, Tomokazu Thorington, Richard W., Jr. Bohaska, Paula W. Chen, Yen-Jean Sato, Fumi TI Anatomy of Shoulder Girdle Muscle Modifications and Walking Adaptation in the Scaly Chinese Pangolin (Manis Pentadactyla Pentadactyla: Pholidota) Compared with the Partially Osteoderm-Clad Armadillos (Dasypodidae) SO ANATOMICAL RECORD-ADVANCES IN INTEGRATIVE ANATOMY AND EVOLUTIONARY BIOLOGY LA English DT Article DE pangolin; functional anatomy; imaging analysis; shoulder girdle muscles; armadillo; locomotion; evolutionary morphology ID CARDIAC NERVOUS-SYSTEM; NEW-WORLD MONKEYS; EVOLUTIONARY ANATOMY; FUNCTIONAL-ANATOMY; CHICK WINGS; MORPHOLOGY; INNERVATION; PRIMATES; FORELIMB; BRANCHES AB Because pangolins are unique mammals with a body and limbs almost entirely sheathed in hard keratinous overlapping scales and with digging and climbing abilities, the shoulder girdle muscles may differ significantly from those of other mammals including the partially osteoderm-clad armadillos. Therefore, we conducted a functional anatomical study of the shoulder girdle muscles in Chinese pangolins (Manis pentadactyla pentadactyla, Pholidota) and some armadillo species (Dasypodidae). Our CT scans revealed that the pangolin's overlapping scales are hard structures completely encasing the limbs. The armadillo's limbs, however, are covered with small relatively soft non-overlapping scales embedded in the skin, and articulate completely free of the hard osteodermal carapace. The attachments of some shoulder girdle muscles in the pangolin have moved from the surrounding edges of the scapula to the spine, and they, therefore, fully cover the scapula. In addition, some pangolin shoulder girdle muscles cross the shoulder joint to insert on the distal humerus, but this does not occur in armadillos. We cannot rule out the possibility that these muscle modifications represent adaptations for digging and/or climbing in pangolins. Our results and previous literature do not establish specific links between them and locomotive modes. However, we propose that the Chinese pangolin may use its derived muscular features when walking to move its armor-restricted forelimbs more effectively by swinging its head from side to side. Anat Rec, 298:1217-1236, 2015. (c) 2015 Wiley Periodicals, Inc. C1 [Kawashima, Tomokazu; Sato, Fumi] Toho Univ, Dept Anat, Sch Med, Tokyo 1438540, Japan. [Thorington, Richard W., Jr.; Bohaska, Paula W.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Chen, Yen-Jean] Natl Museum Nat Sci, Dept Zool, Div Bird & Mammal, Taichung, Taiwan. RP Kawashima, T (reprint author), Toho Univ, Dept Anat, Sch Med, Ota Ku, 5-21-16 Omori Nishi, Tokyo 1438540, Japan. EM tomokazu.kawashima@med.toho-u.ac.jp NR 59 TC 1 Z9 1 U1 12 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-8486 EI 1932-8494 J9 ANAT REC JI Anat. Rec. PD JUL PY 2015 VL 298 IS 7 BP 1217 EP 1236 DI 10.1002/ar.23170 PG 20 WC Anatomy & Morphology SC Anatomy & Morphology GA CL0JS UT WOS:000356629500001 PM 25950650 ER PT J AU Petaros, A Sholts, SB Slaus, M Bosnar, A Warmlander, SKTS AF Petaros, Anja Sholts, Sabrina B. Slaus, Mario Bosnar, Alan Warmlander, Sebastian K. T. S. TI Evaluating sexual dimorphism in the human mastoid process: A viewpoint on the methodology SO CLINICAL ANATOMY LA English DT Article DE forensic anthropology; mastoid process; osteology; sexual dimorphism; standardization ID DISCRIMINANT FUNCTION-ANALYSIS; LASER-SCANNING TECHNOLOGY; ANATOMIC POSITION; TEMPORAL BONE; LA-QUINA; TRAITS; CRANIA; TRIANGLE; SKULLS; AGE AB The mastoid process is one of the most sexually dimorphic features in the human skull, and is therefore often used to identify the sex of skeletons. Numerous techniques for assessing variation in the size and shape of the mastoid process have been proposed and implemented in osteological research, but its complex form still presents difficulties for consistent and effective analysis. In this article, we compare the different techniques and variables that have been used to define, measure, and visually score sexual dimorphism in the mastoid process. We argue that the current protocols fail to capture the full morphological range of this bony projection, and suggest ways of improving and standardizing them, regarding both traditional and 3D-based approaches. Clin. Anat. 28:593-601, 2015. (c) 2015 Wiley Periodicals, Inc. C1 [Petaros, Anja; Bosnar, Alan] Rijeka Univ, Sch Med, Dept Forens Med & Criminalist, Rijeka 51000, Croatia. [Sholts, Sabrina B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. [Slaus, Mario] Croatian Acad Sci & Arts, Anthropol Ctr, Zagreb, Croatia. [Warmlander, Sebastian K. T. S.] Stockholm Univ, Arrhenius Labs, Div Biophys, S-10691 Stockholm, Sweden. [Warmlander, Sebastian K. T. S.] Linkoping Univ, IEI, Div Commercial & Business Law, Linkoping, Sweden. [Warmlander, Sebastian K. T. S.] Univ Calif Los Angeles, UCLA Getty Conservat Programme, Cotsen Inst Archaeol, Los Angeles, CA USA. RP Petaros, A (reprint author), Rijeka Univ, Sch Med, Dept Forens Med & Criminalist, Brace Branchetta 20, Rijeka 51000, Croatia. EM anja.petaros@yahoo.com NR 68 TC 2 Z9 2 U1 1 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0897-3806 EI 1098-2353 J9 CLIN ANAT JI Clin. Anat. PD JUL PY 2015 VL 28 IS 5 BP 593 EP 601 DI 10.1002/ca.22545 PG 9 WC Anatomy & Morphology SC Anatomy & Morphology GA CL2WB UT WOS:000356806400009 PM 25865024 ER PT J AU Zhu, Y Comita, LS Hubbell, SP Ma, KP AF Zhu, Yan Comita, Liza S. Hubbell, Stephen P. Ma, Keping TI Conspecific and phylogenetic density-dependent survival differs across life stages in a tropical forest SO JOURNAL OF ECOLOGY LA English DT Article DE density dependence; determinants of plant community diversity and structure; Janzen-Connell hypothesis; neighbourhood analysis; phylogenetic relatedness; seedlings dynamics; species coexistence; tropical forest ID BORNEAN RAIN-FOREST; SEEDLING MORTALITY; HABITAT ASSOCIATIONS; SPECIES COEXISTENCE; NEOTROPICAL FOREST; SPATIAL-PATTERNS; ECOLOGICAL COMMUNITIES; LOCAL NEIGHBORHOOD; TRAIT EVOLUTION; TREE SEEDLINGS AB Ecologists have long recognized that plant performance is affected by the density and composition of neighbouring individuals. With the advent of highly resolved species-level phylogenies, it has become possible to test whether such density-dependent neighbourhood interactions are also phylogenetically dependent. Most studies of density dependence have focused on a single life stage; however, the relative importance of different neighbourhood interactions may shift over the lifetime of an individual. We examined effects of conspecific neighbour density, heterospecific neighbour density and average phylogenetic relatedness of heterospecific neighbours on the survival of seedlings, saplings, juveniles and adult trees of 29 focal tree species using long-term, spatially explicit forest dynamics data and a highly resolved DNA barcode phylogeny from the tropical forest of Barro Colorado Island (BCI), Panama. Our results show a decline in the strength of conspecific negative density dependence across life stages: strong negative conspecific neighbour effects at early life stages gave way to weak positive conspecific neighbour effects for adult trees. In contrast, the effect of heterospecific neighbour density on survival showed no clear trend with life stage. We found evidence of phylogenetic density dependence in the BCI forest, with a significant negative impact of neighbourhood relatedness on focal tree survival, but only for later life stages. In contrast to studies from other tropical forests, neighbourhood relatedness had a significant positive effect on seedling survival. Furthermore, we found that focal species varied much more widely in their sensitivity to conspecific neighbour density than in their reactions to heterospecific neighbour density or phylogenetic relatedness.Synthesis. Overall, our results demonstrate that both conspecific density dependence and phylogenetic density dependence influence tropical tree survival, but that their relative importance varies with life stage and among species. Our study highlights the need to incorporate multiple life stages and multiple species when assessing the factors contributing to individual survival and species coexistence for long-lived organisms. C1 [Zhu, Yan; Ma, Keping] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Comita, Liza S.] Yale Univ, Sch Forestry Environm Studies, New Haven, CT 06511 USA. [Comita, Liza S.] Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. [Comita, Liza S.; Hubbell, Stephen P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. RP Ma, KP (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, 20 Nanxincun, Beijing 100093, Peoples R China. EM kpma@ibcas.ac.cn FU CAS [KSCX2-EW-Z-5]; State Key Laboratory of Vegetation and Environmental Change [2011zyts12]; NSF-China [31200342, 31170401, 31011120470]; National Science Foundation [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, DEB-0075102, DEB-0710211, DEB-0823728, DEB-1242622, DEB-0640386]; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund; NSF Research Coordination Network [DEB 1046113] FX We thank Rolando Perez, Salomon Aguilar and Robin Foster for contributing their botanical expertise and Suzanne Lao for data management. We also thank Margaret Metz, Luxiang Lin and Xingxing Man for sharing R code. Lei Chen, Daniel Johnson, Michael Sovic, C. E. Timothy Paine and an anonymous referee provided helpful feedback on the manuscript. Y. Z. was financially supported by Key Innovation Project of CAS (KSCX2-EW-Z-5), State Key Laboratory of Vegetation and Environmental Change (2011zyts12) and the NSF-China (31200342; 31170401; 31011120470). Funding and logistical support for the BCI forest dynamics plot was provided by the National Science Foundation (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, DEB-0075102, DEB-0710211, DEB-0823728, DEB-1242622, DEB-0640386), 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 and numerous private individuals. Data collection was possible due to the hard work of over 100 people from 10 countries over the past three decades. Collaboration and manuscript preparation was facilitated by an NSF Research Coordination Network grant (DEB 1046113) to the Smithsonian Center for Tropical Forest Science, a global network of large-scale demographic tree plots. NR 76 TC 14 Z9 16 U1 19 U2 90 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 JUL PY 2015 VL 103 IS 4 BP 957 EP 966 DI 10.1111/1365-2745.12414 PG 10 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA CL0KC UT WOS:000356630600018 ER PT J AU Paine, CET Amissah, L Auge, H Baraloto, C Baruffol, M Bourland, N Bruelheide, H Dainou, K de Gouvenain, RC Doucet, JL Doust, S Fine, PVA Fortunel, C Haase, J Holl, KD Jactel, H Li, XF Kitajima, K Koricheva, J Martinez-Garza, C Messier, C Paquette, A Philipson, C Piotto, D Poorter, L Posada, JM Potvin, C Rainio, K Russo, SE Ruiz-Jaen, M Scherer-Lorenzen, M Webb, CO Wright, SJ Zahawi, RA Hector, A AF Paine, C. E. Timothy Amissah, Lucy Auge, Harald Baraloto, Christopher Baruffol, Martin Bourland, Nils Bruelheide, Helge Dainou, Kasso de Gouvenain, Roland C. Doucet, Jean-Louis Doust, Susan Fine, Paul V. A. Fortunel, Claire Haase, Josephine Holl, Karen D. Jactel, Herve Li, Xuefei Kitajima, Kaoru Koricheva, Julia Martinez-Garza, Cristina Messier, Christian Paquette, Alain Philipson, Christopher Piotto, Daniel Poorter, Lourens Posada, Juan M. Potvin, Catherine Rainio, Kalle Russo, Sabrina E. Ruiz-Jaen, Mariacarmen Scherer-Lorenzen, Michael Webb, Campbell O. Wright, S. Joseph Zahawi, Rakan A. Hector, Andy TI Globally, functional traits are weak predictors of juvenile tree growth, and we do not know why SO JOURNAL OF ECOLOGY LA English DT Article DE functional ecology; FunDivEurope; growth; hierarchical models; plant population and community dynamics; relative growth rate; size-standardized growth rate; TreeDivNet ID COMMUNITY ECOLOGY; PLANT TRAITS; DEMOGRAPHIC RATES; FORESTS; MODELS; LEAF; BIODIVERSITY; SIZE; TEMPERATURE; SENSITIVITY AB Plant functional traits, in particular specific leaf area (SLA), wood density and seed mass, are often good predictors of individual tree growth rates within communities. Individuals and species with high SLA, low wood density and small seeds tend to have faster growth rates. If community-level relationships between traits and growth have general predictive value, then similar relationships should also be observed in analyses that integrate across taxa, biogeographic regions and environments. Such global consistency would imply that traits could serve as valuable proxies for the complex suite of factors that determine growth rate, and, therefore, could underpin a new generation of robust dynamic vegetation models. Alternatively, growth rates may depend more strongly on the local environment or growth-trait relationships may vary along environmental gradients. We tested these alternative hypotheses using data on 27352 juvenile trees, representing 278 species from 27 sites on all forested continents, and extensive functional trait data, 38% of which were obtained at the same sites at which growth was assessed. Data on potential evapotranspiration (PET), which summarizes the joint ecological effects of temperature and precipitation, were obtained from a global data base. We estimated size-standardized relative height growth rates (SGR) for all species, then related them to functional traits and PET using mixed-effect models for the fastest growing species and for all species together. Both the mean and 95th percentile SGR were more strongly associated with functional traits than with PET. PET was unrelated to SGR at the global scale. SGR increased with increasing SLA and decreased with increasing wood density and seed mass, but these traits explained only 3.1% of the variation in SGR. SGR-trait relationships were consistently weak across families and biogeographic zones, and over a range of tree statures. Thus, the most widely studied functional traits in plant ecology were poor predictors of tree growth over large scales.Synthesis. We conclude that these functional traits alone may be unsuitable for predicting growth of trees over broad scales. Determining the functional traits that predict vital rates under specific environmental conditions may generate more insight than a monolithic global relationship can offer. C1 [Paine, C. E. Timothy] Univ Stirling, Biol & Environm Sci, Stirling FK9 4LA, Scotland. [Amissah, Lucy; Poorter, Lourens] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Amissah, Lucy] KNUST, Council Sci & Ind Res, Forestry Res Inst Ghana, Kumasi, Ghana. [Auge, Harald] Helmholtz Ctr Environm Res, UFZ, Dept Community Ecol, D-06120 Halle, Germany. [Auge, Harald; Bruelheide, Helge] German Ctr Integrat Biodivers Res iDiv, D-04103 Leipzig, Germany. [Baraloto, Christopher; Fortunel, Claire] INRA, UMR Ecol Forets Guyane, Kourou 97387, French Guiana. [Baraloto, Christopher; Kitajima, Kaoru] Florida Int Univ, Dept Biol Sci, Int Ctr Trop Bot, Miami, FL 33199 USA. [Baruffol, Martin] Univ Zurich, Inst Evolutionary Biol & Environm Studies, CH-8057 Zurich, Switzerland. [Bourland, Nils; Dainou, Kasso; Doucet, Jean-Louis] Univ Liege, Unit Forest & Nat Management, Lab Trop & Subtrop Forest Reg, Liege, Belgium. [Bruelheide, Helge] Univ Halle Wittenberg, Inst Biol Geobot & Bot Garden, D-06108 Halle, Germany. [de Gouvenain, Roland C.] Rhode Isl Coll, Dept Biol, Providence, RI 02908 USA. [Doust, Susan] Australian Antarctic Div, Kingston, Tas 7050, Australia. [Fine, Paul V. A.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Fortunel, Claire] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Haase, Josephine; Scherer-Lorenzen, Michael] Univ Freiburg, Geobot, Fac Biol, D-79104 Freiburg, Germany. [Haase, Josephine; Philipson, Christopher] ETH, Inst Terr Ecosyst, Ecosyst Management, CH-8092 Zurich, Switzerland. [Holl, Karen D.] Univ Calif Santa Cruz, Environm Studies Dept, Santa Cruz, CA 95064 USA. [Jactel, Herve] INRA, BIOGECO, UMR1202, F-33510 Cestas, France. [Jactel, Herve] Univ Bordeaux, UMR1202, BIOGECO, F-33400 Talence, France. [Kitajima, Kaoru; Potvin, Catherine; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Kitajima, Kaoru] Kyoto Univ, Forest Biomat Sci, Sakyo Ku, Kyoto, Japan. [Koricheva, Julia] Royal Holloway Univ London, Sch Biol Sci, Egham TW20 0EX, Surrey, England. [Martinez-Garza, Cristina] Univ Autonoma Estado Morelos, Ctr Invest Biodiversidad & Conservac, Cuernavaca 62209, Morelos, Mexico. [Messier, Christian; Paquette, Alain] Univ Quebec, Ctr Forest Res, Montreal, PQ H3C 3P8, Canada. [Messier, Christian] Univ Quebec, ISFORT, Montreal, PQ H3C 3P8, Canada. [Messier, Christian] Univ Quebec Outaouais, Montreal, PQ H3C 3P8, Canada. [Piotto, Daniel] Univ Fed Sul Bahia, BR-45613204 Ferradas Itabuna, BA, Brazil. [Posada, Juan M.] Univ Rosario, Fac Nat Sci & Math, Biol Program, Bogota 111221, Colombia. [Potvin, Catherine; Ruiz-Jaen, Mariacarmen] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Rainio, Kalle] Univ Turku, Dept Biol, Sect Ecol, FI-20014 Turku, Finland. [Russo, Sabrina E.] Univ Nebraska, Sch Biol Sci, Lincoln, NE 68588 USA. [Webb, Campbell O.] Arnold Arboretum Harvard Univ, Boston, MA 02131 USA. [Zahawi, Rakan A.] Org Trop Studies, Las Cruces Biol Stn, Apartado San Vito De Cot, Costa Rica. [Hector, Andy] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. RP Paine, CET (reprint author), Univ Stirling, Biol & Environm Sci, Stirling FK9 4LA, Scotland. EM c.e.t.paine@stir.ac.uk RI Posada, Juan/G-3616-2016; Rainio, Kalle/I-1495-2013; Auge, Harald/D-4802-2015; Wright, Stuart/M-3311-2013; Piotto, Daniel/F-9956-2012; Hector, Andrew/H-4199-2011; iDiv, Deutsches Zentrum/B-5164-2016; Koricheva, Julia /G-6754-2011; OI Posada, Juan/0000-0001-7794-9300; Rainio, Kalle/0000-0002-5859-0037; Auge, Harald/0000-0001-7432-8453; Wright, Stuart/0000-0003-4260-5676; Piotto, Daniel/0000-0002-6505-0098; Hector, Andrew/0000-0002-1309-7716; Koricheva, Julia /0000-0002-9033-0171; Fine, Paul/0000-0002-0550-5628 FU Swiss National Science [121967]; European Union [265171, 226299] FX We thank the multitudes involved in planting, measuring and maintenance of the study sites, and collecting growth and trait data. Jens Kattge, manager of the TRY global trait data base, and Kyle Dexter contributed additional trait data. Statistical advice from Marco Geraci, Sophia Ratcliffe, Nadja Ruger and Christian Wirth strengthened the analysis. This research was funded by Swiss National Science grant number 121967 to A.H. and by the European Union Seventh Framework Program (FP7/2007-2013) under grant agreements no 265171 (project FunDivEUROPE) and no 226299 (project BACCARA). NR 52 TC 13 Z9 14 U1 15 U2 104 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 JUL PY 2015 VL 103 IS 4 BP 978 EP 989 DI 10.1111/1365-2745.12401 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA CL0KC UT WOS:000356630600020 ER PT J AU Kraft, TS Wright, SJ Turner, I Lucas, PW Oufiero, CE Noor, MNS Sun, IF Dominy, NJ AF Kraft, Thomas S. Wright, S. Joseph Turner, Ian Lucas, Peter W. Oufiero, Christopher E. Noor, Md. Nur Supardi Sun, I-Fang Dominy, Nathaniel J. TI Seed size and the evolution of leaf defences SO JOURNAL OF ECOLOGY LA English DT Article DE fracture toughness; herbivory; plant development and life-history traits; seed dispersal; spatial aggregation ID LONG-TAILED MACAQUES; LOWLAND RAIN-FORESTS; PLANT DEFENSE; FRACTURE-TOUGHNESS; FUNCTIONAL TRAITS; TROPICAL FOREST; LIFE-SPAN; PHENOTYPIC PLASTICITY; RESOURCE AVAILABILITY; ONCOPELTUS-FASCIATUS AB Leaf defences vary widely among tree species, affecting rates of herbivory, survival and reproduction. Two contrasting hypotheses account for variation in leaf defences among species. The first predicts that a slow life history, which is characteristic of larger seeded species adapted to resource-limited environments, is associated with well-defended leaves. The second, apparency theory, predicts that elevated leaf defences are necessitated for species that are more detectable to herbivores. Here we use comparative methods and a global data set to test (i) the relationship between seed size and leaf defences and (ii) the relationship between clumping (spatial apparency) and leaf defences. We found that seed size was positively related to leaf fracture toughness, but not phenolics or tannin concentration and that spatial aggregation was unrelated to leaf defences.Synthesis. Our results suggest that larger seed size and increased leaf toughness are correlated as part of a trait syndrome associated with a slow, resource-limited life history, not clumped dispersion and increased spatial apparency. C1 [Kraft, Thomas S.; Dominy, Nathaniel J.] Dartmouth Coll, Class Life Sci Ctr 1978, Dept Biol Sci, Hanover, NH 03755 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Turner, Ian] Royal Bot Gardens Kew, Richmond TW9 3AB, Surrey, England. [Lucas, Peter W.] Kuwait Univ, Dept Biol Sci, Safat 13110, Kuwait. [Oufiero, Christopher E.] Towson Univ, Dept Biol Sci, Towson, MD 21252 USA. [Noor, Md. Nur Supardi] Forest Res Inst Malaysia, Div Forest Environm, Kuala Lumpur 52109, Malaysia. [Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien, Taiwan. [Dominy, Nathaniel J.] Dept Anthropol, Dartmouth Coll, Hanover, NH 03755 USA. RP Kraft, TS (reprint author), Dartmouth Coll, Class Life Sci Ctr 1978, Dept Biol Sci, Hanover, NH 03755 USA. EM thomas.s.kraft@dartmouth.edu RI Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Dominy, Nathaniel/0000-0001-5916-418X; Kraft, Thomas/0000-0002-0634-9233 FU Explorer's Club; National Geographic Society [6584-99, 7179-01]; National Institutes of Health [5F32GM064287]; Research Grants Council of Hong Kong [7241/97M]; Sigma Xi; Frank Levinson Fund; Smithsonian Tropical Research Institute; NSF [BCS-0923791]; National Evolutionary Synthesis Center (NSF) [EF-0905606] FX We are grateful to Y.C. Chan, C.A. Chapman, O. Calderon, R.T. Corlett, J.G. Fleagle, P.J. Grubb, V. Horlyck, H.F. Howe, J. Magnay and R.W. Wrangham for technical assistance and guidance. We thank R.S. Duncan for contributing unpublished data. Our research was approved by the Ugandan National Council for Science and Technology, the Ugandan Wildlife Authority, and the Makerere University Biological Field Station (Kibale); the Forest Research Institute of Malaysia (Pasoh); the National Parks Board of Singapore (permit no. NP/RP328A; Bukit Timah); and the Smithsonian Tropical Research Institute and the Autoridad Nacional del Ambiente (Panama). Funding was received from the Explorer's Club, the National Geographic Society (grant nos. 6584-99 and 7179-01), the National Institutes of Health (Ruth L. Kirschstein National Research Service Award no. 5F32GM064287), the Research Grants Council of Hong Kong (grant no. 7241/97M), Sigma Xi, the Frank Levinson Fund and the Smithsonian Tropical Research Institute (10-week Graduate Fellowship). For training in phylogenetic comparative methods, we thank C. Nunn and the AnthroTree Workshop which is supported by the NSF (BCS-0923791) and the National Evolutionary Synthesis Center (NSF grant EF-0905606). NR 119 TC 1 Z9 1 U1 6 U2 49 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 JUL PY 2015 VL 103 IS 4 BP 1057 EP 1068 DI 10.1111/1365-2745.12407 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA CL0KC UT WOS:000356630600027 ER PT J AU McNulty, KP Begun, DR Kelley, J Manthi, FK Mbua, EN AF McNulty, Kieran P. Begun, David R. Kelley, Jay Manthi, Fredrick K. Mbua, Emma N. TI A systematic revision of Proconsul with the description of a new genus of early Miocene hominoid SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Ekembo; Ugandapithecus; Fossil ape; Taxonomy; Tinderet; Rusinga ID KASWANGA PRIMATE SITE; RUSINGA-ISLAND; MIDDLE-MIOCENE; EAST-AFRICA; AFROPITHECUS-TURKANENSIS; LATE OLIGOCENE; WESTERN KENYA; CATARRHINES; MORPHOLOGY; UGANDA AB For more than 80 years, Proconsul has held a pivotal position in interpretations of catarrhine evolution and hominoid diversification in East Africa. The majority of what we 'know' about Proconsul, however, derives from abundant younger fossils found at the Kisingiri localities on Rusinga and Mfangano Islands rather than from the smaller samples found at Koru-the locality of the type species, Proconsul africanus-and other Tinderet deposits. One outcome of this is seen in recent attempts to expand the genus "Ugandapithecus" (considered here a junior subjective synonym of Proconsul), wherein much of the Tinderet sample was referred to that genus based primarily on differentiating it from the Kisingiri specimens rather than from the type species, P. africanus. This and other recent taxonomic revisions to Proconsul prompted us to undertake a systematic review of dentognathic specimens attributed to this taxon. Results of our study underscore and extend the substantive distinction of Tinderet and Ugandan Proconsul (i.e., Proconsul sensu stricto) from the Kisingiri fossils, the latter recognized here as a new genus. Specimens of the new genus are readily distinguished from Proconsul sensu stricto by morphology preserved in the P. africanus holotype, but also in [(1)s, lower incisors, upper and lower canines, and especially mandibular characteristics. A number of these differences are more advanced among Kisingiri specimens in the direction of crown hominoids. Proconsul sensu stricto is characterized by a suite of unique features that strongly unite the included species as a clade. There have been decades of contentious debate over the phylogenetic placement of Proconsul (sensu lato), due in part to there being a mixture of primitive and more advanced morphology within the single genus. By recognizing two distinct clades that, in large part, segregate these character states, we believe that better phylogenetic resolution can be achieved. (C) 2015 Elsevier Ltd. All rights reserved. C1 [McNulty, Kieran P.] Univ Minnesota, Hubert H Humphrey Ctr 395, Evolutionary Anthropol Lab, Minneapolis, MN 55455 USA. [Begun, David R.] Univ Toronto, Dept Anthropol, Toronto, ON M5S 2S2, Canada. [Kelley, Jay] Arizona State Univ, Inst Human Origins, Tempe, AZ 85287 USA. [Kelley, Jay] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Kelley, Jay] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Manthi, Fredrick K.; Mbua, Emma N.] Natl Museums Kenya, Dept Earth Sci, Nairobi 4065800100, Kenya. RP McNulty, KP (reprint author), Univ Minnesota, Hubert H Humphrey Ctr 395, Evolutionary Anthropol Lab, 301 19th Ave S, Minneapolis, MN 55455 USA. EM kmcnulty@umn.edu FU Wenner-Gren Foundation; Johns Hopkins School of Medicine; Leakey Foundation; National Science Foundation [0852609, 1241807]; McKnight Foundation; University of Minnesota; Lloyd A. Wilford Endowment; Leverhulme Foundation; Turkana Basin Institute; Institute of Human Origins, Arizona State University; Alexander Humboldt Stiftung; NSERC FX We thank many people and agencies that assisted with the development and completion of this project. This research was initiated as a result of funding from the Wenner-Gren Foundation and the Johns Hopkins School of Medicine to D.R. Begun in 1987-1989 and was renewed following research and travel generously funded by multiple Leakey Foundation grants to K. McNulty, National Science Foundation grants to K. McNulty (0852609, 1241807), the McKnight Foundation, the University of Minnesota, the Lloyd A. Wilford Endowment, the Leverhulme Foundation, and the Turkana Basin Institute. J. Kelley gratefully acknowledges support from the Institute of Human Origins, Arizona State University. D.R. Begun also wishes to acknowledge the Alexander Humboldt Stiftung and NSERC for funding support. We are grateful to the National Museums of Kenya, the Uganda Museum, the Natural History Museum, and to Rose Mwanja, Ezra Musiime, Tom Mukhuyu, Samuel Muteti, James Yatich, and Mary Muungu for access to and assistance with specimens in their care. Many people provided assistance, comments, criticisms, insights, and suggestions on various aspects of this work, and we especially thank Holly Dunsworth, Will Harcourt-Smith, Tom Lehmann, Dan Peppe, Nicole Garrett, Kirsten Jenkins, Rutger Jansma, Susy Cote, Isaiah Nengo, Andrew Hill, and Brenda Benefit. K. McNulty acknowledges the evolutionary anthropology faculty and students at Durham University for their helpful comments on an early version of this manuscript, and for their gracious hospitality. We are likewise grateful to the anonymous reviewers, associate editor, and editor whose comments strengthened the paper. This manuscript is publication #1 supporting Research on East African Catarrhine and Hominoid Evolution (REACHE). NR 88 TC 6 Z9 6 U1 8 U2 29 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD JUL PY 2015 VL 84 BP 42 EP 61 DI 10.1016/j.jhevol.2015.03.009 PG 20 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA CL5EG UT WOS:000356982000004 PM 25962549 ER PT J AU Duffy, JE Reynolds, PL Bostrom, C Coyer, JA Cusson, M Donadi, S Douglass, JG Eklof, JS Engelen, AH Eriksson, BK Fredriksen, S Gamfeldt, L Gustafsson, C Hoarau, G Hori, M Hovel, K Iken, K Lefcheck, JS Moksnes, PO Nakaoka, M O'Connor, MI Olsen, JL Richardson, JP Ruesink, JL Sotka, EE Thormar, J Whalen, MA Stachowicz, JJ AF Duffy, J. Emmett Reynolds, Pamela L. Bostroem, Christoffer Coyer, James A. Cusson, Mathieu Donadi, Serena Douglass, James G. Ekloef, Johan S. Engelen, Aschwin H. Eriksson, Britas Klemens Fredriksen, Stein Gamfeldt, Lars Gustafsson, Camilla Hoarau, Galice Hori, Masakazu Hovel, Kevin Iken, Katrin Lefcheck, Jonathan S. Moksnes, Per-Olav Nakaoka, Masahiro O'Connor, Mary I. Olsen, Jeanine L. Richardson, J. Paul Ruesink, Jennifer L. Sotka, Erik E. Thormar, Jonas Whalen, Matthew A. Stachowicz, John J. TI Biodiversity mediates top-down control in eelgrass ecosystems: a global comparative-experimental approach SO ECOLOGY LETTERS LA English DT Article DE Biodiversity-ecosystem functioning; bottom-up control; coordinated experiments; food webs; metabolic ecology; structural equation modelling; top-down control ID ZOSTERA-MARINA; TROPHIC INTERACTIONS; NUTRIENT ENRICHMENT; MICROSATELLITE LOCI; SEAGRASS ECOSYSTEM; FUNCTIONAL-ROLE; DIVERSITY; COMMUNITY; EUTROPHICATION; POPULATIONS AB Nutrient pollution and reduced grazing each can stimulate algal blooms as shown by numerous experiments. But because experiments rarely incorporate natural variation in environmental factors and biodiversity, conditions determining the relative strength of bottom-up and top-down forcing remain unresolved. We factorially added nutrients and reduced grazing at 15 sites across the range of the marine foundation species eelgrass (Zostera marina) to quantify how top-down and bottom-up control interact with natural gradients in biodiversity and environmental forcing. Experiments confirmed modest top-down control of algae, whereas fertilisation had no general effect. Unexpectedly, grazer and algal biomass were better predicted by cross-site variation in grazer and eelgrass diversity than by global environmental gradients. Moreover, these large-scale patterns corresponded strikingly with prior small-scale experiments. Our results link global and local evidence that biodiversity and top-down control strongly influence functioning of threatened seagrass ecosystems, and suggest that biodiversity is comparably important to global change stressors. C1 [Duffy, J. Emmett; Reynolds, Pamela L.; Lefcheck, Jonathan S.; Richardson, J. Paul] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Duffy, J. Emmett] Smithsonian Inst, Tennenbaum Marine Observ Network, Washington, DC 20013 USA. [Bostroem, Christoffer] Abo Akad Univ, Dept Biosci Environm & Marine Biol, FIN-20520 Turku, Finland. [Coyer, James A.] Cornell Univ, Shoals Marine Lab, Portsmouth, NH 03801 USA. [Cusson, Mathieu] Univ Quebec Chicoutimi, Dept Sci Fondamentales & Quebec Ocean, Chicoutimi, PQ G7H 2B1, Canada. [Donadi, Serena; Eriksson, Britas Klemens; Olsen, Jeanine L.] Univ Groningen, Ctr Ecol & Evolutionary Studies, NL-9747 AG Groningen, Netherlands. [Douglass, James G.] Florida Gulf Coast Univ, Ft Myers, FL 33965 USA. [Ekloef, Johan S.] Stockholm Univ, Dept Ecol Environm & Plant Sci, S-10691 Stockholm, Sweden. [Engelen, Aschwin H.] Univ Algarve, CCMAR, P-8005139 Faro, Portugal. [Fredriksen, Stein; Thormar, Jonas] Univ Oslo, Dept Biosci, N-0316 Oslo, Norway. [Gamfeldt, Lars; Moksnes, Per-Olav] Univ Gothenburg, Dept Biol & Environm Sci, SE-40530 Gothenburg, Sweden. [Gustafsson, Camilla] Univ Helsinki, Tvarminne Zool Stn, Hango 10900, Finland. [Hoarau, Galice] Univ Nordland, Fac Biosci & Aquaculture, N-8049 Bodo, Norway. [Hori, Masakazu] Fisheries Res Agcy, Hiroshima 7390452, Japan. [Hovel, Kevin] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Iken, Katrin] Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Fairbanks, AK 99775 USA. [Nakaoka, Masahiro] Hokkaido Univ, Field Sci Ctr Northern Biosphere, Akkeshi Marine Stn, Akkeshi, Hokkaido 0881113, Japan. [O'Connor, Mary I.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [O'Connor, Mary I.] Univ British Columbia, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. [Ruesink, Jennifer L.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Sotka, Erik E.] Coll Charleston, Grice Marine Lab, Charleston, SC 29412 USA. [Whalen, Matthew A.; Stachowicz, John J.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. RP Duffy, JE (reprint author), Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. EM duffye@si.edu RI O'Connor, Mary/F-2275-2010; Eriksson, Britas Klemens/D-8601-2015; Thormar, Jonas/F-3103-2010; Eklof, Johan/C-7722-2017; Engelen, Aschwin/M-3432-2013; OI Eriksson, Britas Klemens/0000-0003-4752-922X; Thormar, Jonas/0000-0002-7925-3822; Eklof, Johan/0000-0001-6936-0926; Engelen, Aschwin/0000-0002-9579-9606; Lefcheck, Jonathan/0000-0002-8787-1786 FU National Science Foundation [OCE-1031061] FX We thank the many staff, students, and volunteers who assisted with field and laboratory research; Jim Grace and Jarrett Byrnes for advice on structural equation modelling; Brad Cardinale and Jonathan Losos for comments that improved the MS; and the home institutions of all project partners, who provided invaluable in-kind support. Primary funding was provided by the National Science Foundation (OCE-1031061 to J.E.D.). NR 51 TC 22 Z9 22 U1 27 U2 159 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 JUL PY 2015 VL 18 IS 7 BP 696 EP 705 DI 10.1111/ele.12448 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CL0CJ UT WOS:000356606100011 PM 25983129 ER PT J AU Cheng, BS Bible, JM Chang, AL Ferner, MC Wasson, K Zabin, CJ Latta, M Deck, A Todgham, AE Grosholz, ED AF Cheng, Brian S. Bible, Jillian M. Chang, Andrew L. Ferner, Matthew C. Wasson, Kerstin Zabin, Chela J. Latta, Marilyn Deck, Anna Todgham, Anne E. Grosholz, Edwin D. TI Testing local and global stressor impacts on a coastal foundation species using an ecologically realistic framework SO GLOBAL CHANGE BIOLOGY LA English DT Article DE additive; climate change; diel-cycling hypoxia; latent; multiple stressors; Olympia oyster; Ostrea lurida; salinity; synergy; warming ID BENTHIC MARINE-INVERTEBRATES; CLIMATE-CHANGE; ENVIRONMENTAL-STRESS; OCEAN ACIDIFICATION; THERMAL TOLERANCE; DISSOLVED-OXYGEN; OLYMPIA OYSTER; TEMPERATURE; HYPOXIA; CALIFORNIA AB Despite the abundance of literature on organismal responses to multiple environmental stressors, most studies have not matched the timing of experimental manipulations with the temporal pattern of stressors in nature. We test the interactive effects of diel-cycling hypoxia with both warming and decreased salinities using ecologically realistic exposures. Surprisingly, we found no evidence of negative synergistic effects on Olympia oyster growth; rather, we found only additive and opposing effects of hypoxia (detrimental) and warming (beneficial). We suspect that diel-cycling provided a temporal refuge that allowed physiological compensation. We also tested for latent effects of warming and hypoxia to low-salinity tolerance using a seasonal delay between stressor events. However, we did not find a latent effect, rather a threshold survival response to low salinity that was independent of early life-history exposure to warming or hypoxia. The absence of synergism is likely the result of stressor treatments that mirror the natural timing of environmental stressors. We provide environmental context for laboratory experimental data by examining field time series environmental data from four North American west coast estuaries and find heterogeneous environmental signals that characterize each estuary, suggesting that the potential stressor exposure to oysters will drastically differ over moderate spatial scales. This heterogeneity implies that efforts to conserve and restore oysters will require an adaptive approach that incorporates knowledge of local conditions. We conclude that studies of multiple environmental stressors can be greatly improved by integrating ecologically realistic exposure and timing of stressors found in nature with organismal life-history traits. C1 [Cheng, Brian S.; Bible, Jillian M.; Grosholz, Edwin D.] Univ Calif Davis, Bodega Marine Lab, Davis, CA 95616 USA. [Cheng, Brian S.; Zabin, Chela J.; Grosholz, Edwin D.] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. [Bible, Jillian M.] Univ Calif Davis, Dept Ecol & Evolut, Davis, CA 95616 USA. [Chang, Andrew L.; Ferner, Matthew C.; Deck, Anna] San Francisco Bay Natl Estuarine Res Reserve, Tiburon, CA USA. [Wasson, Kerstin] Elkhorn Slough Natl Estuarine Res Reserve, Watsonville, CA USA. [Latta, Marilyn] Calif State Coastal Conservancy, Oakland, CA USA. [Todgham, Anne E.] Univ Calif Davis, Dept Anim Sci, Davis, CA 95616 USA. RP Cheng, BS (reprint author), Smithsonian Environm Res Ctr, POB 28,647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM bscheng@gmail.com RI Chang, Andrew/J-8058-2016; OI Chang, Andrew/0000-0002-7870-285X; Cheng, Brian/0000-0003-1679-8398 FU National Estuarine Research Reserve System Science Collaborative (NOAA) [NA09NOS4190153]; Bodega Marine Laboratory Graduate Fellowship; NSF GK-12 Fellowship (NSF) [0841297]; NERRS Graduate Research Fellowship FX We would like to thank C. Knight, C. Norton, D. Hooper, E. Seubert, N. Miller, and S. Boles for invaluable laboratory support. We would also like to thank the Bodega Marine Laboratory staff, J. Newman, K. Menard, D. Hall, and P. Smith. Thanks to D. Trockel for providing helpful coding script. We also thank E. Sanford, J. J. Stachowicz, N. A. Fangue, S.L. Williams, K. J. Kroeker, L.M. Komoroske, and two anonymous reviewers for helpful comments on earlier versions of the manuscript. Funding support was provided by the National Estuarine Research Reserve System Science Collaborative (NOAA Grant #NA09NOS4190153), Bodega Marine Laboratory Graduate Fellowship, NSF GK-12 Fellowship (NSF Grant # 0841297), and NERRS Graduate Research Fellowship (to BSC). NR 69 TC 10 Z9 10 U1 6 U2 46 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 JUL PY 2015 VL 21 IS 7 BP 2488 EP 2499 DI 10.1111/gcb.12895 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CK7OS UT WOS:000356422500004 ER PT J AU Williams, SM Chollett, I Roff, G Cortes, J Dryden, CS Mumby, PJ AF Williams, Stacey M. Chollett, Iliana Roff, George Cortes, Jorge Dryden, Charlie S. Mumby, Peter J. TI Hierarchical spatial patterns in Caribbean reef benthic assemblages SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Assembly rules; Caribbean; community attributes; corals; macroecology; octocorals; Orbicella reefs; species richness; sponges ID CORAL-REEF; BIOTIC HOMOGENIZATION; SPECIES-DIVERSITY; ECOLOGY; VARIANCE; RICHNESS; CONSERVATION; PERSPECTIVE; DISPERSAL; DECLINE AB AimCoral assemblages on Caribbean reefs have largely been considered to be biogeographically homogeneous at a regional scale. We reassess this in three taxa (corals, sponges and octocorals) using three community attributes with increasing levels of information (species richness, composition and relative abundance) across hierarchical spatial scales, and identify the key environmental drivers associated with this variation. LocationCaribbean Basin. MethodsWe assessed reefs along 546 transects positioned within the same forereef habitat (Orbicella reef) in 11 countries, using a consistent methodology and surveyors. Spatial variability in richness, composition and relative abundance was assessed at four hierarchical spatial scales - transects (metres), sites (kilometres), areas (tens of kilometres) and regions (hundreds of kilometres) - using permutational multivariate analysis of variance (PERMANOVA). The relevance of contemporary environmental factors in explaining the observed spatial patterns was also assessed using PERMANOVA. ResultsConsistent with previous studies, species richness of coral assemblages, commonly the focus of biogeographical studies, showed little variance at large spatial scales. In contrast, species composition and relative abundance showed significant variability at regional scales. Coral, sponge and octocoral assemblages each varied independently across spatial scales. Rugosity and wave exposure were key drivers of the composition and relative abundance of coral and octocoral assemblages. Main conclusionsCaribbean reef assemblages exhibit considerable biogeographical variability at broad spatial scales (hundreds of kilometres) when more responsive community attributes were used. However, the high degree of variability within sites (kilometres) highlights the relevance of local ecological drivers such as rugosity and wave exposure in structuring assemblages. The high levels of within-site variability that is not explained by environmental variables may suggest a previously unrealized contribution of anthropogenic disturbance operating at local scales throughout the region. C1 [Williams, Stacey M.; Cortes, Jorge] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 115012060, Costa Rica. [Williams, Stacey M.] ISER, Lajas, PR 00667 USA. [Chollett, Iliana; Mumby, Peter J.] Univ Exeter, Marine Spatial Ecol Lab, Exeter EX4 4PS, Devon, England. [Chollett, Iliana; Roff, George; Mumby, Peter J.] Univ Queensland, Marine Spatial Ecol Lab, Brisbane, Qld 4072, Australia. [Dryden, Charlie S.] Newcastle Univ, Sch Marine Sci & Technol, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. RP Chollett, I (reprint author), Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. EM iliana.chollett@gmail.com FU European Union [244161]; Pew [2008-000330-010]; Australian Research Council [FL0992179]; Fundacion de la Universidad de Costa Rica para la Investigacion (FUNDEVI); Universidad de Costa Rica through the Marine Science and Limnology Research Center (CIMAR) [808-B0-531] FX The research leading to these results has received funding from the European Union 7th Framework programme (P7/2007-2013) under grant agreement no. 244161, Pew (grant 2008-000330-010) and an Australian Research Council Laureate Fellowship (FL0992179) to P.J.M., and support from the Universidad de Costa Rica (project 808-B0-531) through the Marine Science and Limnology Research Center (CIMAR) and Fundacion de la Universidad de Costa Rica para la Investigacion (FUNDEVI) to J.C. We are very grateful to C. Sanchez and S. Newman for their constant support during fieldwork. We thank the fisheries departments, ministries of the environment and individuals who provided permission and assistance in the following countries: Antigua (S. Archibald), Barbados (L. Brewster), Belize (Fisheries: J. Azueta; Environmental Research Institute: L. Cho-Rickets; Reefs End Lodge: Saint), Bonaire (STINAPA Bonaire, R. de Leon, Dive Friends Bonaire), Curacao (CARMABI: M. Vermeij), Dominican Republic (Punta Cana Ecological Foundation: B. Hulefeld, J. Jhell; La Caleta Marine Park: R. Torres; Las Galeras and Superior Divers; Y. Rodriguez), Honduras (Roatan Marine Park: N. Bach; Utila Center of Marine Ecology: S. Box; Reef House Resort; Clearwater Paradise), Jamaica (Montego Bay Marine Park: B. Zane; Lady G' Diver), Panama (Smithsonian Tropical Research Institute), St Lucia (Soufriere Marine Management Area: T. Nelson; Fisheries: A. Joseph, S. Williams-Peter) and St Vincent and the Grenadines (Fisheries: Mr. Ryan, C. Isaacs; Tobago Cays Marine Park: O. Harvey; Kings Landing: M. James; G. Adams). We thank S. Kahng and H. Lasker for insight into identification and reproductive modes of octocorals, the Marine Spatial Ecology Lab, particularly J. Ortiz, C. Doropoulos and A. Harborne, for fruitful discussions on the overall topic, and the editors and referees for their insightful comments which greatly improved this manuscript. NR 55 TC 7 Z9 7 U1 1 U2 45 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 JUL PY 2015 VL 42 IS 7 BP 1327 EP 1335 DI 10.1111/jbi.12509 PG 9 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA CL1AL UT WOS:000356674300013 ER PT J AU Marini, KLD McKellar, AE Ratcliffe, LM Marra, PP Reudink, MW AF Marini, Kristen L. D. McKellar, Ann E. Ratcliffe, Laurene M. Marra, Peter P. Reudink, Matthew W. TI Age-related change in carotenoid-based plumage of the American Redstart (Setophaga ruticilla) SO JOURNAL OF ORNITHOLOGY LA English DT Article DE American Redstart; Colour change; Plumage colour; Carotenoid; Setophaga ruticilla ID SWALLOWS TACHYCINETA-BICOLOR; REPRODUCTIVE INVESTMENT; MIGRATORY SONGBIRD; FORAGING BEHAVIOR; HOUSE FINCHES; VITAMIN-A; COLOR; BIRDS; SIGNALS; EVOLUTION AB Plumage colouration serves a variety of functions for birds, including conspecific signalling, crypsis, and predator-prey interactions. Though much research has been conducted on colour changes in species with delayed plumage maturation, where birds do not exhibit definitive adult plumage until their second breeding season or later, relatively few studies have examined how plumage colour changes once definitive adult plumage has been attained. In this study on male and female American Redstarts (Setophaga ruticilla), which exhibit male delayed plumage maturation, we used reflectance spectrometry to evaluate carotenoid-based tail colour changes over 11 breeding seasons, examining both within-individual and population-level changes. At a population level, males in their first breeding season in definitive adult plumage had a feather hue that was more orange-shifted than birds in their second year in adult plumage, and marginally, but not significantly, more orange-shifted than birds in their third year in adult plumage. Within-individual analysis of males recaptured in subsequent seasons also revealed a shift away from orange towards a more yellow feather hue as individuals aged. Within individuals, red chroma was highest for males in their second year in adult plumage, but it showed no population-level effects. At the population level, female redstarts in their first breeding season displayed plumage with a higher red chroma and a lower brightness than birds in their second breeding season, potentially as a result of differences in the timing and conditions of moult (first-year bird tail feathers were grown in the nest). For adult males and females, there was no difference in plumage colouration between birds that returned to the study site compared to those that failed to return. Together, our results suggest that within-individual change rather than differential survival best explains our findings. We suggest that studies examining age-related colour changes are critical for understanding the evolution of complex signalling systems, such as that of American Redstarts. C1 [Marini, Kristen L. D.; Reudink, Matthew W.] Thompson Rivers Univ, Dept Biol Sci, Kamloops, BC, Canada. [McKellar, Ann E.] Environm Canada, Saskatoon, SK, Canada. [Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. RP Reudink, MW (reprint author), Thompson Rivers Univ, Dept Biol Sci, Kamloops, BC, Canada. EM mreudink@tru.ca OI Reudink, Matthew/0000-0001-8956-5849 FU National Science Foundation; Natural Sciences and Engineering Research Council; CUEF U-REAP FX We thank R. Norris, K. Langin, R. Germain, and numerous field assistants for help collecting feathers throughout this study. We thank N. Flood for helpful comments on earlier drafts of this manuscript. Funding for this project was provided by the National Science Foundation (PPM), Natural Sciences and Engineering Research Council Discovery Grants (MWR and LMR), and a CUEF U-REAP award (KLDM). NR 53 TC 0 Z9 0 U1 2 U2 14 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0021-8375 EI 1439-0361 J9 J ORNITHOL JI J. Ornithol. PD JUL PY 2015 VL 156 IS 3 BP 783 EP 793 DI 10.1007/s10336-015-1168-7 PG 11 WC Ornithology SC Zoology GA CK7WS UT WOS:000356447100022 ER PT J AU Morandi, A Sun, M Forman, W Jones, C AF Morandi, Andrea Sun, Ming Forman, William Jones, Christine TI The galaxy cluster outskirts probed by Chandra SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; cosmology: observations; large-scale structure of Universe; X-rays: galaxies: clusters ID X-RAY OBSERVATIONS; SUNYAEV-ZELDOVICH OBSERVATIONS; GAS MASS FRACTION; INTRACLUSTER MEDIUM; OUTER REGIONS; SURFACE BRIGHTNESS; BARYON FRACTIONS; ENTROPY PROFILES; VIRIAL RADIUS; ABELL 1835 AB We studied the physical properties of the intracluster medium (ICM) in the virialization region of a sample of 320 clusters (0.056 < z < 1.24, kT a parts per thousand(3) 3 keV) in the Chandra archive. With the emission measure profiles from this large sample, the typical gas density, gas slope and gas fraction can be constrained out to and beyond R-200. We observe a steepening of the density profiles beyond R-500 with beta similar to 0.68 at R-500 and beta similar to 1 at R-200 and beyond. By tracking the direction of the cosmic filaments approximately with the ICM eccentricity, we report that galaxy clusters deviate from spherical symmetry, with only small differences between relaxed and disturbed systems. We also did not find evolution of the gas density with redshift, confirming its self-similar evolution. The value of the baryon fraction reaches the cosmic value at R-200; however, systematics due to non-thermal pressure support and clumpiness might enhance the measured gas fraction, leading to an actual deficit of the baryon budget with respect to the primordial value. This study has important implications for understanding the ICM physics in the outskirts. C1 [Morandi, Andrea; Sun, Ming] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Forman, William; Jones, Christine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Morandi, A (reprint author), Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. EM andrea.morandi@uah.edu OI Morandi, Andrea/0000-0002-5575-3056; Forman, William/0000-0002-9478-1682 FU Chandra grants [GO2-13160A, GO2-13102A]; NASA [NNX14AI29G] FX We are indebted to Erwin Lau, Stefano Ettori, Mauro Roncarelli, Norbert Werner, Daisuke Nagai, Craig Sarazin, Ben Maughan, Dominique Eckert and Alexey Vikhlinin for valuable comments. We thank Terry Gaetz for the work and information on the ACIS stowed background. AM gratefully acknowledges the hospitality of the Harvard-Smithsonian Center for Astrophysics. AM and MS acknowledge support from Chandra grants GO2-13160A, GO2-13102A, and NASA grant NNX14AI29G. We thank the anonymous referee for the careful reading of the manuscript and suggestions, which improved the presentation of our work. NR 73 TC 9 Z9 9 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 JUL 1 PY 2015 VL 450 IS 3 BP 2261 EP 2278 DI 10.1093/mnras/stv660 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300003 ER PT J AU Vedantham, HK Koopmans, LVE de Bruyn, AG Wijnholds, SJ Brentjens, M Abdalla, FB Asad, KMB Bernardi, G Bus, S Chapman, E Ciardi, B Daiboo, S Fernandez, ER Ghosh, A Harker, G Jelic, V Jensen, H Kazemi, S Lambropoulos, P Martinez-Rubi, O Mellema, G Mevius, M Offringa, AR Pandey, VN Patil, AH Thomas, RM Veligatla, V Yatawatta, S Zaroubi, S Anderson, J Asgekar, A Bell, ME Bentum, MJ Best, P Bonafede, A Breitling, F Broderick, J Bruggen, M Butcher, HR Corstanje, A de Gasperin, F de Geus, E Deller, A Duscha, S Eisloffel, J Engels, D Falcke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hassall, TE Heald, G Hoeft, M Horandel, J Iacobelli, M Juette, E Kondratiev, VI Kuniyoshi, M Kuper, G Mann, G Markoff, S McFadden, R McKay-Bukowski, D McKean, JP Mulcahy, DD Munk, H Nelles, A Norden, MJ Orru, E Pandey-Pommier, M Pizzo, R Polatidis, AG Reich, W Renting, A Rottgering, H Schwarz, D Shulevski, A Smirnov, O Stappers, BW Steinmetz, M Swinbank, J Tagger, M Tang, Y Tasse, C ter Veen, S Thoudam, S Toribio, C Vocks, C Wise, MW Wucknitz, O Zarka, P AF Vedantham, H. K. Koopmans, L. V. E. de Bruyn, A. G. Wijnholds, S. J. Brentjens, M. Abdalla, F. B. Asad, K. M. B. Bernardi, G. Bus, S. Chapman, E. Ciardi, B. Daiboo, S. Fernandez, E. R. Ghosh, A. Harker, G. Jelic, V. Jensen, H. Kazemi, S. Lambropoulos, P. Martinez-Rubi, O. Mellema, G. Mevius, M. Offringa, A. R. Pandey, V. N. Patil, A. H. Thomas, R. M. Veligatla, V. Yatawatta, S. Zaroubi, S. Anderson, J. Asgekar, A. Bell, M. E. Bentum, M. J. Best, P. Bonafede, A. Breitling, F. Broderick, J. Bruggen, M. Butcher, H. R. Corstanje, A. de Gasperin, F. de Geus, E. Deller, A. Duscha, S. Eisloeffel, J. Engels, D. Falcke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hassall, T. E. Heald, G. Hoeft, M. Hoerandel, J. Iacobelli, M. Juette, E. Kondratiev, V. I. Kuniyoshi, M. Kuper, G. Mann, G. Markoff, S. McFadden, R. McKay-Bukowski, D. McKean, J. P. Mulcahy, D. D. Munk, H. Nelles, A. Norden, M. J. Orru, E. Pandey-Pommier, M. Pizzo, R. Polatidis, A. G. Reich, W. Renting, A. Roettgering, H. Schwarz, D. Shulevski, A. Smirnov, O. Stappers, B. W. Steinmetz, M. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. ter Veen, S. Thoudam, S. Toribio, C. Vocks, C. Wise, M. W. Wucknitz, O. Zarka, P. TI Lunar occultation of the diffuse radio sky: LOFAR measurements between 35 and 80 MHz SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: observational; techniques: interferometric; Moon; dark ages; reionization; first stars ID 21 CM; THERMAL RADIATION; DARK-AGES; SURFACE; MOON; REIONIZATION; SPECTRUM; UNIVERSE; SIGNAL; EPOCH AB We present radio observations of the Moon between 35 and 80 MHz to demonstrate a novel technique of interferometrically measuring large-scale diffuse emission extending far beyond the primary beam (global signal) for the first time. In particular, we show that (i) the Moon appears as a negative-flux source at frequencies 35 < nu < 80 MHz since it is 'colder' than the diffuse Galactic background it occults, (ii) using the (negative) flux of the lunar disc, we can reconstruct the spectrum of the diffuse Galactic emission with the lunar thermal emission as a reference, and (iii) that reflected RFI (radio-frequency interference) is concentrated at the centre of the lunar disc due to specular nature of reflection, and can be independently measured. Our RFI measurements show that (i) Moon-based Cosmic Dawn experiments must design for an Earth-isolation of better than 80 dB to achieve an RFI temperature < 1 mK, (ii) Moon-reflected RFI contributes to a dipole temperature less than 20 mK for Earth-based Cosmic Dawn experiments, (iii) man-made satellite-reflected RFI temperature exceeds 20 mK if the aggregate scattering cross-section of visible satellites exceeds 175 m(2) at 800 km height, or 15 m(2) at 400 km height. Currently, our diffuse background spectrum is limited by sidelobe confusion on short baselines (10-15 per cent level). Further refinement of our technique may yield constraints on the redshifted global 21 cm signal from Cosmic Dawn (40 > z > 12) and the Epoch of Reionization (12 > z > 5). C1 [Vedantham, H. K.; Koopmans, L. V. E.; de Bruyn, A. G.; Asad, K. M. B.; Bus, S.; Daiboo, S.; Fernandez, E. R.; Ghosh, A.; Jelic, V.; Kazemi, S.; Lambropoulos, P.; Martinez-Rubi, O.; Mevius, M.; Pandey, V. N.; Patil, A. H.; Thomas, R. M.; Veligatla, V.; Zaroubi, S.; McKean, J. P.; Shulevski, A.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [de Bruyn, A. G.; Wijnholds, S. J.; Brentjens, M.; Yatawatta, S.; Asgekar, A.; Bentum, M. J.; de Geus, E.; Deller, A.; Duscha, S.; Falcke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Heald, G.; Kondratiev, V. I.; Kuper, G.; McFadden, R.; McKean, J. P.; Munk, H.; Norden, M. J.; Orru, E.; Pizzo, R.; Polatidis, A. G.; Renting, A.; Tang, Y.; Toribio, C.; Wise, M. W.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Abdalla, F. B.; Chapman, E.; Harker, G.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Bernardi, G.; Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Bernardi, G.; Smirnov, O.] Rhodes Univ, Dept Phys & Elelctron, ZA-6140 Grahamstown, South Africa. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Jensen, H.; Mellema, G.] Stockholm Univ, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden. [Jensen, H.; Mellema, G.] Stockholm Univ, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden. [Offringa, A. R.; Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Anderson, J.] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Anderson, J.; Breitling, F.; Mann, G.; Steinmetz, M.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore 560048, Karnataka, India. [Bell, M. E.] CSIRO Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Bentum, M. J.] Univ Twente, NL-7522 NB Enschede, Netherlands. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Bruggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Broderick, J.; Hassall, T. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Corstanje, A.; Falcke, H.; Hoerandel, J.; Nelles, A.; ter Veen, S.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [de Geus, E.] SmarterVision BV, NL-9401 JX Assen, Netherlands. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Fender, R.] Univ Oxford, Astrophys, Oxford OX1 3RH, England. [Ferrari, C.] Univ Nice Sophia Antipolis, UMR7293, Lab Lagrange, CNRS,Observ Cote dAzur, F-06300 Nice, France. [Garrett, M. A.; Iacobelli, M.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmeier, J.; Tagger, M.] LPC2E CNRS, F-45071 Orleans 2, France. [Griessmeier, J.] Univ Orleans, OSUC, USR 704, Stn Radioastron Nancay,Observ Paris,CNRS INSU, F-18330 Nancay, France. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Kondratiev, V. I.] Lebedev Phys Inst, Astro Space Ctr, Moscow 117997, Russia. [Kuniyoshi, M.; Mulcahy, D. D.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Markoff, S.; Swinbank, J.; Wise, M. W.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [McKay-Bukowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bukowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Tasse, C.; Zarka, P.] Observ Paris, LESIA, UMR CNRS 8109, F-92195 Meudon, France. RP Vedantham, HK (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM harish@astro.rug.nl RI Harker, Geraint/C-4885-2012; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Jelic, Vibor/B-2938-2014; Yatawatta, Sarod/E-6037-2013; OI Shulevski, Aleksandar/0000-0002-1827-0469; Harker, Geraint/0000-0002-7894-4082; Kondratiev, Vladislav/0000-0001-8864-7471; Jelic, Vibor/0000-0002-6034-8610; Swinbank, John/0000-0001-9445-1846; Yatawatta, Sarod/0000-0001-5619-4017; de Gasperin, Francesco/0000-0003-4439-2627; Abdalla, Filipe/0000-0003-2063-4345; Deller, Adam/0000-0001-9434-3837 FU European Research Council under ERC-Starting Grant [FIRST-LIGHT - 258942]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX We thank Professor Frank Briggs for bringing to our notice an unnecessary approximation to equation (7) made in an earlier version of the manuscript. We thank the computer group at the Kapteyn Institute for providing the PYTHON modules that we used to render Fig. 4. HKV and LVEK acknowledge the financial support from the European Research Council under ERC-Starting Grant FIRST-LIGHT - 258942. CF acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. 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. NR 31 TC 7 Z9 7 U1 1 U2 11 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 JUL 1 PY 2015 VL 450 IS 3 BP 2291 EP 2305 DI 10.1093/mnras/stv746 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300005 ER PT J AU Cechura, J Vrtilek, SD Hadrava, P AF Cechura, J. Vrtilek, S. D. Hadrava, P. TI Interpreting the X-ray state transitions of Cygnus X-1(a similar to...) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; techniques: spectroscopic; circumstellar matter; stars: mass-loss ID DIFFUSE INTERSTELLAR BANDS; LONG-TERM VARIABILITY; BLACK-HOLE; DOPPLER TOMOGRAPHY; STELLAR WIND; X-1; MASS; ACCRETION; EMISSION; BINARIES AB We present a novel method for interpreting observations of high-mass X-ray binaries (HMXBs) based on a combination of spectroscopic data and numerical results from a radiation hydrodynamic model of stellar winds. We calculate synthetic Doppler tomograms of predicted emission in low/hard and high/soft X-ray states and compare them with Doppler tomograms produced using spectra of Cygnus X-1, a prototype of HMXBs. Emission from HMXBs is determined by local conditions within the circumstellar medium, namely density, temperature, and ionization state. These quantities depend strongly on the X-ray state of the systems. By increasing intensity of an X-ray emission produced by the compact companion in the HMXB model, we achieved a complete redistribution of the circumstellar medium in the vicinity of the modelled system. These changes (which simulate the transitions between two major spectral states) are also apparent in the synthetic Doppler tomograms which are in good agreement with the observations. C1 [Cechura, J.; Hadrava, P.] Acad Sci Czech Republic, Inst Astron, Prague 14100, Czech Republic. [Cechura, J.; Vrtilek, S. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cechura, J (reprint author), Acad Sci Czech Republic, Inst Astron, Bocni II 1401-1, Prague 14100, Czech Republic. EM cechura@astro.cas.cz; saku@cfa.harvard.edu; had@asu.cas.cz FU Czech Science Foundation - Albert Einstein Center for Gravitation and Astrophysics [GACR 14-37086G]; Smithsonian Institution Endowment Grant; [SVV-260089] FX We are grateful to C. S. Peris for helpful suggestions. We also thank an anonymous referee for constructive comments which greatly improved the quality of the paper. Observations by our colleges at Ondrejov and Xinlong observatories are highly appreciated. We gratefully acknowledge the use of the MOLLY and DOPPLER software written by T. R. Marsh and the MODMAP software written by D. Steeghs. This work was supported in part by the Czech Science Foundation (GACR 14-37086G) - Albert Einstein Center for Gravitation and Astrophysics, a grant SVV-260089, and a Smithsonian Institution Endowment Grant awarded to SDV. NR 43 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 JUL 1 PY 2015 VL 450 IS 3 BP 2410 EP 2422 DI 10.1093/mnras/stv756 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300014 ER PT J AU Carnerero, MI Raiteri, CM Villata, M Acosta-Pulido, JA D'Ammando, F Smith, PS Larionov, VM Agudo, I Arevalo, MJ Arkharov, AA Bach, U Bachev, R Benitez, E Blinov, DA Bozhilov, V Buemi, CS Bueno, AB Carosati, D Casadio, C Chen, WP Damljanovic, G Di Paola, A Efimova, NV Ehgamberdiev, SA Giroletti, M Gomez, JL Gonzalez-Morales, PA Grinon-Marin, AB Grishina, TS Gurwell, MA Hiriart, D Hsiao, HY Ibryamov, S Jorstad, SG Joshi, M Kopatskaya, EN Kurtanidze, OM Kurtanidze, SO Lahteenmaki, A Larionova, EG Larionova, LV Lazaro, C Leto, P Lin, CS Lin, HC Manilla-Robles, AI Marscher, AP McHardy, IM Metodieva, Y Mirzaqulov, DO Mokrushina, AA Molina, SN Morozova, DA Nikolashvili, MG Orienti, M Ovcharov, E Panwar, N Yabar, AP Gimenez, IP Ramakrishnan, V Richter, GM Rossini, M Sigua, LA Strigachev, A Taylor, B Tornikoski, M Trigilio, C Troitskaya, YV Troitsky, IS Umana, G Valcheva, A Velasco, S Vince, O Wehrle, AE Wiesemeyer, H AF Carnerero, M. I. Raiteri, C. M. Villata, M. Acosta-Pulido, J. A. D'Ammando, F. Smith, P. S. Larionov, V. M. Agudo, I. Arevalo, M. J. Arkharov, A. A. Bach, U. Bachev, R. Benitez, E. Blinov, D. A. Bozhilov, V. Buemi, C. S. Bueno, A. Bueno Carosati, D. Casadio, C. Chen, W. P. Damljanovic, G. Di Paola, A. Efimova, N. V. Ehgamberdiev, Sh. A. Giroletti, M. Gomez, J. L. Gonzalez-Morales, P. A. Grinon-Marin, A. B. Grishina, T. S. Gurwell, M. A. Hiriart, D. Hsiao, H. Y. Ibryamov, S. Jorstad, S. G. Joshi, M. Kopatskaya, E. N. Kurtanidze, O. M. Kurtanidze, S. O. Lahteenmaki, A. Larionova, E. G. Larionova, L. V. Lazaro, C. Leto, P. Lin, C. S. Lin, H. C. Manilla-Robles, A. I. Marscher, A. P. McHardy, I. M. Metodieva, Y. Mirzaqulov, D. O. Mokrushina, A. A. Molina, S. N. Morozova, D. A. Nikolashvili, M. G. Orienti, M. Ovcharov, E. Panwar, N. Pastor Yabar, A. Puerto Gimenez, I. Ramakrishnan, V. Richter, G. M. Rossini, M. Sigua, L. A. Strigachev, A. Taylor, B. Tornikoski, M. Trigilio, C. Troitskaya, Yu. V. Troitsky, I. S. Umana, G. Valcheva, A. Velasco, S. Vince, O. Wehrle, A. E. Wiesemeyer, H. TI Multiwavelength behaviour of the blazar OJ 248 from radio to gamma-rays(a similar to...) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: jets; quasars: general; quasars: individual: OJ 248 ID RAY LOUD BLAZARS; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; RAPID NONTHERMAL FLARES; BL-LACERTAE; 3C 454.3; GASP-WEBT; PKS 1510-089; NOVEMBER 1995; INNER JET AB We present an analysis of the multiwavelength behaviour of the blazar OJ 248 at z = 0.939 in the period 2006-2013. We use low-energy data (optical, near-infrared, and radio) obtained by 21 observatories participating in the Gamma-Ray Large Area Space Telescope (GLAST)-AGILE Support Program of the Whole Earth Blazar Telescope, as well as data from the Swift (optical-UV and X-rays) and Fermi (gamma-rays) satellites, to study flux and spectral variability and correlations among emissions in different bands. We take into account the effect of absorption by the Damped Lyman alpha intervening system at z = 0.525. Two major outbursts were observed in 2006-2007 and in 2012-2013 at optical and near-IR wavelengths, while in the high-frequency radio light curves prominent radio outbursts are visible peaking at the end of 2010 and beginning of 2013, revealing a complex radio-optical correlation. Cross-correlation analysis suggests a delay of the optical variations after the gamma-ray ones of about a month, which is a peculiar behaviour in blazars. We also analyse optical polarimetric and spectroscopic data. The average polarization percentage P is less than 3 per cent, but it reaches similar to 19 per cent during the early stage of the 2012-2013 outburst. A vague correlation of P with brightness is observed. There is no preferred electric vector polarization angle and during the outburst the linear polarization vector shows wide rotations in both directions, suggesting a complex behaviour/structure of the jet and possible turbulence. The analysis of 140 optical spectra acquired at the Steward Observatory reveals a strong Mg ii broad emission line with an essentially stable flux of 6.2 x 10(- 15) erg cm(- 2) s(- 1) and a full width at half-maximum of 2053 km s(- 1). C1 [Carnerero, M. I.; Raiteri, C. M.; Villata, M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Carnerero, M. I.; Acosta-Pulido, J. A.; Arevalo, M. J.; Bueno, A. Bueno; Gonzalez-Morales, P. A.; Grinon-Marin, A. B.; Lazaro, C.; Pastor Yabar, A.; Puerto Gimenez, I.; Velasco, S.] IAC, E-38205 Tenerife, Spain. [Carnerero, M. I.; Acosta-Pulido, J. A.; Arevalo, M. J.; Bueno, A. Bueno; Gonzalez-Morales, P. A.; Grinon-Marin, A. B.; Lazaro, C.; Pastor Yabar, A.; Puerto Gimenez, I.; Velasco, S.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [D'Ammando, F.; Rossini, M.] Univ Bologna, Dip Fis & Astron, I-40127 Bologna, Italy. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Larionov, V. M.; Blinov, D. A.; Grishina, T. S.; Jorstad, S. G.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Mokrushina, A. A.; Morozova, D. A.; Troitskaya, Yu. V.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Larionov, V. M.; Arkharov, A. A.; Efimova, N. V.; Mokrushina, A. A.] Pulkovo Observ, St Petersburg 196140, Russia. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, Santiago, Chile. [Agudo, I.; Casadio, C.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Bach, U.; Wiesemeyer, H.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Bachev, R.; Ibryamov, S.; Strigachev, A.] Bulgarian Acad Sci, Inst Astron, BU-1784 Sofia, Bulgaria. [Benitez, E.] Univ Nacl Autonoma Mexico, Astron Inst, Mexico City 04510, DF, Mexico. [Blinov, D. A.] Univ Crete, Phys Dept, GR-71003 Iraklion, Greece. [Bozhilov, V.; Ovcharov, E.; Valcheva, A.] Univ Sofia St Kliment Ohrisdski, Dept Astron, BG-1164 Sofia, Bulgaria. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain. [Carosati, D.] TNG Fdn Galileo Galilei, INAF, E-38712 La Palma, Spain. [Chen, W. P.; Hsiao, H. Y.; Lin, C. S.; Lin, H. C.; Panwar, N.] Natl Cent Univ, Grad Inst Astron, Zhongli 32001, Taiwan. [Damljanovic, G.; Vince, O.] Astron Observ, Belgrade 11060, Serbia. [Di Paola, A.] Osserv Astron Roma, INAF, I-00136 Rome, Italy. [Ehgamberdiev, Sh. A.; Mirzaqulov, D. O.] Ulugh Beg Astron Inst, Maidanak Observ, Tashkent 100052, Uzbekistan. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Jorstad, S. G.; Joshi, M.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia. [Kurtanidze, O. M.] Landessternwarte Heidelberg, ZAH, D-69117 Heidelberg, Germany. [Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan 422526, Russia. [Kurtanidze, O. M.] Guangzhou Univ, Ctr Astrophys, Guangzhou 510006, Guangdong, Peoples R China. [Lahteenmaki, A.; Ramakrishnan, V.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FI-02540 Kylmala, Finland. [Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, FI-00076 Aalto, Finland. [Manilla-Robles, A. I.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [McHardy, I. M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Metodieva, Y.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Richter, G. M.] Astrophys Inst Potsdam, D-14482 Potsdam, Germany. [Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA. [Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA. RP Carnerero, MI (reprint author), Osserv Astron Torino, INAF, Via Osservatorio 20, I-10025 Pino Torinese, Italy. EM maribel@oato.inaf.it; villata@oato.inaf.it RI Ramakrishnan, Venkatessh/C-8628-2017; Lahteenmaki, Anne/L-5987-2013; Larionov, Valeri/H-1349-2013; Troitskaya, Yuliya/N-2222-2015; Morozova, Daria/H-1298-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Blinov, Dmitry/G-9925-2013; Agudo, Ivan/G-1701-2015; Velasco, Sergio/K-3508-2016; Grishina, Tatiana/H-6873-2013 OI Ramakrishnan, Venkatessh/0000-0002-9248-086X; Larionova, Liudmila/0000-0002-0274-1481; Umana, Grazia/0000-0002-6972-8388; Villata, Massimo/0000-0003-1743-6946; Di Paola, Andrea/0000-0002-2189-8644; Leto, Paolo/0000-0003-4864-2806; Larionov, Valeri/0000-0002-4640-4356; Troitskaya, Yuliya/0000-0002-9907-9876; Morozova, Daria/0000-0002-9407-7804; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Blinov, Dmitry/0000-0003-0611-5784; Agudo, Ivan/0000-0002-3777-6182; Velasco, Sergio/0000-0002-4170-0789; Grishina, Tatiana/0000-0002-3953-6676 FU Russian RFBR [15-02-00949]; St. Petersburg University [6.38.335.2015]; Shota Rustaveli National Science Foundation [FR/638/6-320/12, 31/77]; CEIC (Andalucia) [P09-FQM-4784]; MINECO (Spain) grant; Smithsonian Institution; Academia Sinica; Fermi Guest Investigator grants [NNX08AW56G, NNX09AU10G]; NASA Fermi Guest Investigator grants [NNX11AQ03G, NNX13AO99G]; NSF; BU; Lowell Observatory; UK Science and Technology Facilities Council; Academy of Finland [212656, 210338, 121148]; UNAM-DGAPA-PAPIIT [IN111514]; Ministry of Education, Science and Technological Development of the Republic of Serbia [176011, 176021, 176004]; INAF [PRIN-INAF 2011] FX We thank the referee, Vasiliki Pavlidou, for useful comments and suggestions. This article is partly based on observations made with the telescopes IAC80 and TCS operated by the Instituto de Astrofisica de Canarias in the Spanish Observatorio del Teide on the island of Tenerife. Most of the observations were taken under the rutinary observation program. The IAC team acknowledges the support from the group of support astronomers and telescope operators of the Observatorio del Teide. St. Petersburg University team acknowledges support from Russian RFBR grant 15-02-00949 and St. Petersburg University research grant 6.38.335.2015. AZT-24 observations are made within an agreement between Pulkovo, Rome, and Teramo observatories. The Abastumani team acknowledges financial support of the project FR/638/6-320/12 by the Shota Rustaveli National Science Foundation under contract 31/77. This paper is partly based on observations carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by the MPIA and the IAA-CSIC. Acquisition and reduction of the MAPCAT and IRAM 30 m data is supported in part by MINECO (Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784. This paper is partly based on observations carried out at the IRAM 30 m Telescope, which is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The SMA 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 Steward Observatory spectropolarimetric monitoring project is supported by the Fermi Guest Investigator grants NNX08AW56G and NNX09AU10G. The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grants NNX11AQ03G and NNX13AO99G. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory. 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 funding from the UK Science and Technology Facilities Council. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). Partly based on observations with the Medicina and Noto telescopes operated by INAF - Istituto di Radioastronomia. EB acknowledge financial support from UNAM-DGAPA-PAPIIT through grant IN111514. GD and OV did the observations/investigations in line with Projects No. 176011 (Dynamics and Kinematics of Celestial Bodies and Systems), 176021 (Visible and Invisible Matter in Nearby Galaxies: Theory and Observations), and 176004 (Stellar Physics) which are supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia. The Torino team acknowledges financial support by INAF through contract PRIN-INAF 2011. NR 70 TC 6 Z9 6 U1 1 U2 9 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 JUL 1 PY 2015 VL 450 IS 3 BP 2677 EP 2691 DI 10.1093/mnras/stv823 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300034 ER PT J AU Bitsakis, T Dultzin, D Ciesla, L Krongold, Y Charmandaris, V Zezas, A AF Bitsakis, T. Dultzin, D. Ciesla, L. Krongold, Y. Charmandaris, V. Zezas, A. TI Studying the evolution of galaxies in compact groups over the past 3 Gyr - I. Nuclear activity SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: groups: general; galaxies: interactions; galaxies: nuclei; galaxies: Seyfert ID DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; ON-ORBIT PERFORMANCE; BRIGHT IRAS GALAXIES; DWARF SEYFERT NUCLEI; 6TH DATA RELEASE; GALACTIC NUCLEI; LINE REGIONS; NEARBY GALAXIES; HOST GALAXIES AB We present the first of a series of studies of the evolution of galaxies in compact groups over the past 3 Gyr. This article focuses on the evolution of nuclear activity and how it has been affected by the dense environment of the groups. Our analysis is based on the largest multiwavelength compact-group sample to date, containing complete ultraviolet-infrared (UV-IR) photometry for 1770 isolated groups (7417 galaxies). We classified the nuclear activity of the galaxies based on optical emission-line and mid-infrared (mid-IR) diagnostic methods, as well as using spectral energy distribution fitting. We observe a 15 per cent increase in the number of active galactic nucleus (AGN)-hosting late-type galaxies found in dynamically old groups over the past 3 Gyr, accompanied by a corresponding decrease in their circumnuclear star formation. Comparing our compact group results with those for local isolated field and interacting pair galaxies, we find no differences in the AGNs at the same redshift range. Based on both optical and mid-IR colour classifications, we report the absence of Seyfert 1 nuclei and attribute this to the low accretion rates caused by depletion of gas. We propose that the observed increase in low-ionization nuclear emission-line regions (LINERs) and Seyfert 2 nuclei (at low z) in early-type galaxies of dynamically young groups is due to the morphological transformation of lenticular galaxies into elliptical ones. Finally, we show that, at any given stellar mass, galaxies found in dynamically old groups are more likely to host an AGN. Our findings suggest that depletion of gas due to past star formation and tidal stripping is the major mechanism driving the evolution of nuclear activity in compact groups of galaxies. C1 [Bitsakis, T.; Dultzin, D.; Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Ciesla, L.; Charmandaris, V.; Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Charmandaris, V.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, GR-15236 Penteli, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, A.] FORTH, Iraklion 71003, Greece. RP Bitsakis, T (reprint author), Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, DF, Mexico. EM tbitsakis@astro.unam.mx RI Bitsakis, Theodoros/O-2766-2013; Charmandaris, Vassilis/A-7196-2008; Zezas, Andreas/C-7543-2011 OI Bitsakis, Theodoros/0000-0001-5787-8242; Charmandaris, Vassilis/0000-0002-2688-1956; Zezas, Andreas/0000-0001-8952-676X FU DGAPA-UNAM; PAIIT-UNAM [107313]; EU [PIRSES-GA-2012-316788] FX TB acknowledges support from DGAPA-UNAM postdoctoral fellowships. DD acknowledges support through grant 107313 from PAIIT-UNAM. VC acknowledges partial support from EU FP7 Grant PIRSES-GA-2012-316788. We also appreciate the very useful comments of the referee, which helped to improve this article. This research has made use of data products from Galaxy Evolution Explorer (GALEX), an ultraviolet space telescope operated by Caltech/NASA, Infrared Science Archive (IRSA/Caltech), a UCLA/JPL-Caltech/NASA joint project, and the Sloan Digital Sky Survey (SDSS). TB also thanks P. Bonfini, G. Maravelias, A. Maragkoudakis and A. Steiakaki for useful discussions and suggestions. NR 95 TC 5 Z9 5 U1 2 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 JUL 1 PY 2015 VL 450 IS 3 BP 3114 EP 3126 DI 10.1093/mnras/stv755 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LJ UT WOS:000356339300064 ER PT J AU Reef, R Winter, K Morales, J Adame, MF Reef, DL Lovelock, CE AF Reef, Ruth Winter, Klaus Morales, Jorge Adame, Maria Fernanda Reef, Dana L. Lovelock, Catherine E. TI The effect of atmospheric carbon dioxide concentrations on the performance of the mangrove Avicennia germinans over a range of salinities SO PHYSIOLOGIA PLANTARUM LA English DT Article ID RHIZOPHORA-MANGLE L; ELEVATED CO2; RESPONSES; PHOTOSYNTHESIS; GROWTH; GRADIENT; NITROGEN; AVAILABILITY; ENRICHMENT; TEMPERATE AB By increasing water use efficiency and carbon assimilation, increasing atmospheric CO2 concentrations could potentially improve plant productivity and growth at high salinities. To assess the effect of elevated CO2 on the salinity response of a woody halophyte, we grew seedlings of the mangrove Avicennia germinans under a combination of five salinity treatments [from 5 to 65 parts per thousand (ppt)] and three CO2 concentrations (280, 400 and 800ppm). We measured survivorship, growth rate, photosynthetic gas exchange, root architecture and foliar nutrient and ion concentrations. The salinity optima for growth shifted higher with increasing concentrations of CO2, from 0ppt at 280ppm to 35ppt at 800ppm. At optimal salinity conditions, carbon assimilation rates were significantly higher under elevated CO2 concentrations. However, at salinities above the salinity optima, salinity had an expected negative effect on mangrove growth and carbon assimilation, which was not alleviated by elevated CO2, despite a significant improvement in photosynthetic water use efficiency. This is likely due to non-stomatal limitations to growth at high salinities, as indicated by our measurements of foliar ion concentrations that show a displacement of K+ by Na+ at elevated salinities that is not affected by CO2. The observed shift in the optimal salinity for growth with increasing CO2 concentrations changes the fundamental niche of this species and could have significant effects on future mangrove distribution patterns and interspecific interactions. C1 [Reef, Ruth; Reef, Dana L.; Lovelock, Catherine E.] Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. [Winter, Klaus; Morales, Jorge] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Adame, Maria Fernanda] Griffith Univ, Australian Rivers Inst, Nathan, Qld 4111, Australia. RP Reef, R (reprint author), Univ Queensland, Sch Biol Sci, St Lucia, Qld 4072, Australia. EM r.reef@uq.edu.au RI Lovelock, Catherine/G-7370-2012 OI Lovelock, Catherine/0000-0002-2219-6855 FU Queensland-Smithsonian Fellowship; Australian Research Council [DE120101706] FX We would like to thank Dr Ken Krauss, Prof. Wayne Sousa, Dr Helene Muller-Landau and Dr Egbert Leigh for fruitful discussions and Dr Ivania Ceron, Jorge Aranda and Maya and Ethan Reef for assistance in the field. Dr Ben Turner and Dayana Agudo for mineral element and stable isotope analysis, Milton Garcia for microclimate measurements. This work has been funded by a 2012 Queensland-Smithsonian Fellowship to R. R. and by an Australian Research Council Discovery Early Career Research Award (DE120101706) to R. R. The mangrove propagules were collected under permit from ANAM, Panama (SC/P-21-12). NR 38 TC 3 Z9 3 U1 11 U2 46 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-9317 EI 1399-3054 J9 PHYSIOL PLANTARUM JI Physiol. Plant. PD JUL PY 2015 VL 154 IS 3 BP 358 EP 368 DI 10.1111/ppl.12289 PG 11 WC Plant Sciences SC Plant Sciences GA CL0ES UT WOS:000356613100003 PM 25263409 ER PT J AU Orosei, R Jordan, RL Morgan, DD Cartacci, M Cicchetti, A Duru, F Gurnett, DA Heggy, E Kirchner, DL Noschese, R Kofman, W Masdea, A Plaut, JJ Seu, R Watters, TR Picardi, G AF Orosei, R. Jordan, R. L. Morgan, D. D. Cartacci, M. Cicchetti, A. Duru, F. Gurnett, D. A. Heggy, E. Kirchner, D. L. Noschese, R. Kofman, W. Masdea, A. Plaut, J. J. Seu, R. Watters, T. R. Picardi, G. TI Mars Advanced Radar for Subsurface and Ionospheric Sounding (MARSIS) after nine years of operation: A summary SO PLANETARY AND SPACE SCIENCE LA English DT Article DE Mars Express; Mars; Ground Penetrating Radar (GPR); Ionosphere; Ice; Water ID ELECTRON-DENSITY PROFILES; MEDUSAE FOSSAE FORMATION; MARTIAN GEOLOGIC RECORD; EXPRESS; DEPOSITS; ICE; STRATIGRAPHY; REFLECTIVITY; FREQUENCY; SIGNALS AB Mars Express, the first European interplanetary mission, carries the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) to search for ice and water in the Martian subsurface. Developed by an Italian-US team, MARSIS transmits low-frequency, wide-band radio pulses penetrating below the surface and reflected by dielectric discontinuities linked to structural or compositional changes. MARSIS is also a topside ionosphere sounder, transmitting a burst of short, narrow-band pulses at different frequencies that are reflected by plasma with varying densities at different altitudes. The radar operates since July 2005, after the successful deployment of its 40 m antenna, acquiring data at altitudes lower than 1200 km. Subsurface sounding (SS) data are processed on board by stacking together a batch of echoes acquired at the same frequency. On ground, SS data are further processed by correlating the received echo with the transmitted waveform and compensating, de-focusing caused by the dispersive ionosphere. Ground processing of active ionospheric sounding (AIS) data consists in the reconstruction of the electron density profile as a function of altitude. MARSIS observed the internal structure of Planum Boreum outlining the Basal Unit, an icy deposit lying beneath the North Polar Layered Deposits thought to have formed in an epoch in which climate was markedly different from the current one. The total volume of ice in polar layered deposits could be estimated, and parts of the Southern residual ice cap were revealed to consist of approximate to 10 m of CO2 ice. Radar properties of the Vastitas Borealis Formation point to the presence of large quantities of ice buried beneath the surface. Observations of the ionosphere revealed the complex interplay between plasma, crustal magnetic field and solar wind, contributing to space weather studies at Mars. The presence of three-dimensional plasma structures in the ionosphere was revealed for the first time. MARSIS could successfully operate at Phobos, becoming the first instrument of its kind to observe an asteroid-like body. The main goal pursued by MARSIS, the search for liquid water beneath the surface, remains elusive. However, because of the many factors affecting detection and of the difficulties in identifying water in radar echoes, a definitive conclusion on its presence cannot yet be drawn. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Orosei, R.] Ist Nazl Astrofis, Ist Radioastron, I-40129 Bologna, Italy. [Jordan, R. L.; Heggy, E.; Plaut, J. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91009 USA. [Morgan, D. D.; Duru, F.; Gurnett, D. A.; Kirchner, D. L.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Cartacci, M.; Cicchetti, A.; Noschese, R.] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Kofman, W.] Inst Planetol & Astrophys Grenoble, F-38041 Grenoble 9, France. [Kofman, W.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland. [Masdea, A.; Seu, R.; Picardi, G.] Univ Roma La Sapienza, Dipartimento Ingn Informaz Elettron & Telecomunic, I-00184 Rome, Italy. [Watters, T. R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Orosei, R (reprint author), Ist Nazl Astrofis, Ist Radioastron, Via Piero Gobetti 101, I-40129 Bologna, Italy. EM roberto.orosei@inaf.it RI Kofman, Wlodek/C-4556-2008; OI CICCHETTI, ANDREA/0000-0002-9588-6531; Cartacci, Marco/0000-0001-9825-1817; Noschese, Raffaella/0000-0003-0502-0337 FU Italian Space Agency (ASI) [I/032/12/0] FX This work was supported by the Italian Space Agency (ASI) through Contract no. I/032/12/0. This research has made use of NASA's Astrophysics Data System. NR 90 TC 5 Z9 5 U1 1 U2 13 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD JUL PY 2015 VL 112 BP 98 EP 114 DI 10.1016/j.pss.2014.07.010 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK4MA UT WOS:000356196700009 ER PT J AU Fourie, NH Jolly, CJ Phillips-Conroy, JE Brown, JL Bernstein, RM AF Fourie, Nicolaas H. Jolly, Clifford J. Phillips-Conroy, Jane E. Brown, Janine L. Bernstein, Robin M. TI Variation of hair cortisol concentrations among wild populations of two baboon species (Papio anubis, P-hamadryas) and a population of their natural hybrids SO PRIMATES LA English DT Article DE Hair; Cortisol; Baboons; Hybrids; Behavior; Stress ID MULTILEVEL SOCIETY; SOCIAL SUPPORT; CEREBROSPINAL-FLUID; GREETING BEHAVIOR; RHESUS MACAQUES; STRESS-RESPONSE; CHACMA BABOONS; RECEPTOR GENE; PRIMATE; GLUCOCORTICOIDS AB Male olive (Papio anubis) and hamadryas (P. hamadryas) baboons have distinctive sociobehavioral and physical characteristics. In the Awash National Park, Ethiopia, a hybrid population at the contact zone between these two species, exhibits heterogeneous sociobehavioral and physical characteristics. The ambiguity of the hybrid social environment and disruption of parental stress genotypes may be sources of physiological stress for hybrids. We examined levels of chronic stress among males of the three populations and tested the prediction that chronic cortisol levels would be higher among the hybrids. Animals were captured, sampled, and released during the wet season, and a hair sample was taken for assay. Cortisol was extracted from 182 hair samples with methanol and quantified by ELISA. We included age, age class, rainfall variation, and species affiliation in models examining variation in hair cortisol levels. Species and age significantly contributed to models explaining variation in hair cortisol. Infant hypercortisolism was observed in all three groups, and a decline in cortisol through juvenile and adolescent stages, with a subsequent rise in adulthood. This rise occurred earliest in hamadryas, corroborating other evidence of the precocious development of hamadryas baboons. As expected, hybrids had significantly elevated hair cortisol compared with olive baboons and hamadryas, irrespective of age, except for very young animals. Infant hypercortisolism was also less pronounced among hybrids. Species differences and age-related differences in cortisol levels suggest a dysregulated cortisol phenotype in hybrids, and possibly reflect some form of hybrid disadvantage. More work will be required to disentangle the effects of genetic factors and the social environment. C1 [Fourie, Nicolaas H.] NINR, Biobehav Branch, Intramural Res Program, NIH, Bethesda, MD 20892 USA. [Jolly, Clifford J.] NYU, Dept Anthropol, New York, NY 10003 USA. [Phillips-Conroy, Jane E.] Washington Univ, Sch Med, Dept Anat & Neurobiol, St Louis, MO 63110 USA. [Phillips-Conroy, Jane E.] Washington Univ, Dept Anthropol, St Louis, MO 63130 USA. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Bernstein, Robin M.] Univ Colorado, Dept Anthropol, Boulder, CO 80309 USA. RP Fourie, NH (reprint author), NINR, Biobehav Branch, Intramural Res Program, NIH, Room 2N104,10 Ctr Dr, Bethesda, MD 20892 USA. EM fourienh@mail.nih.gov OI Fourie, Nicolaas/0000-0002-5167-8570 NR 102 TC 7 Z9 7 U1 1 U2 20 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 0032-8332 EI 1610-7365 J9 PRIMATES JI Primates PD JUL PY 2015 VL 56 IS 3 BP 259 EP 272 DI 10.1007/s10329-015-0469-z PG 14 WC Zoology SC Zoology GA CK9BU UT WOS:000356536000008 PM 25903227 ER PT J AU Chang, T Wu, CC Echim, M Lamy, H Vogelsberger, M Hernquist, L Sijacki, D AF Chang, Tom Wu, Cheng-chin Echim, Marius Lamy, Herve Vogelsberger, Mark Hernquist, Lars Sijacki, Debora TI Complexity Phenomena and ROMA of the Earth's Magnetospheric Cusp, Hydrodynamic Turbulence, and the Cosmic Web SO PURE AND APPLIED GEOPHYSICS LA English DT Article; Proceedings Paper CT 6th International Conference on Fractals and Dynamic Systems in Geoscience CY SEP 30-OCT 02, 2013 CL Perugia, ITALY DE Fractals; ROMA; magnetospheric cusp; fluid turbulence; cosmic gas ID COLD DARK-MATTER; MOVING-MESH; MULTIFRACTAL ANALYSIS; SPACE PLASMAS; DISTRIBUTIONS AB "Dynamic complexity" is a phenomenon observed for a nonlinearly interacting system within which multitudes of different sizes of large scale coherent structures emerge, resulting in a globally nonlinear stochastic behavior vastly different from that which could be surmised from the underlying equations of interaction. A characteristic of such nonlinear, complex phenomena is the appearance of intermittent fluctuating events with the mixing and distribution of correlated structures on all scales. We briefly review here a relatively recent method, ROMA (rank-ordered multifractal analysis), explicitly developed for analysis of the intricate details of the distribution and scaling of such types of intermittent structure. This method is then used for analysis of selected examples related to the dynamic plasmas of the cusp region of the Earth's magnetosphere, velocity fluctuations of classical hydrodynamic turbulence, and the distribution of the structures of the cosmic gas obtained by use of large-scale, moving mesh simulations. Differences and similarities of the analyzed results among these complex systems will be contrasted and highlighted. The first two examples have direct relevance to the Earth's environment (i.e., geoscience) and are summaries of previously reported findings. The third example, although involving phenomena with much larger spatiotemporal scales, with its highly compressible turbulent behavior and the unique simulation technique employed in generating the data, provides direct motivation for applying such analysis to studies of similar multifractal processes in extreme environments of near-Earth surroundings. These new results are both exciting and intriguing. C1 [Chang, Tom; Vogelsberger, Mark] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Wu, Cheng-chin] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90095 USA. [Echim, Marius; Lamy, Herve] Belgian Inst Space Aeron, B-1180 Brussels, Belgium. [Echim, Marius] Inst Space Sci, Bucharest 077125, Romania. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 OHA, England. RP Chang, T (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM tom.tschang@gmail.com FU US National Science Foundation; European Community [313038/STORM] FX This research is partially supported by the US National Science Foundation and the European Community's Seventh Framework Programme (FP7/2007-2013) under Grant agreement no. 313038/STORM. Tom Chang wishes to thank Dr. Diego Perigini for inviting him to present this combined review and report of new findings related to ROMA at the 6th International Conference on Fractals and Dynamic Systems in Geoscience in the spirit of providing cross-discipline fertilization/exchange of scientific techniques and ideas in modern fractal analysis. NR 35 TC 1 Z9 1 U1 0 U2 6 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0033-4553 EI 1420-9136 J9 PURE APPL GEOPHYS JI Pure Appl. Geophys. PD JUL PY 2015 VL 172 IS 7 BP 2025 EP 2043 DI 10.1007/s00024-014-0874-z PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA CK6FV UT WOS:000356324800019 ER PT J AU Stefanski, SF Shi, XY Hall, JS Hernandez, A Fenichel, EP AF Stefanski, Stephanie F. Shi, Xiangying Hall, Jefferson S. Hernandez, Andres Fenichel, Eli P. TI Teak-cattle production tradeoffs for Panama Canal Watershed small scale producers SO FOREST POLICY AND ECONOMICS LA English DT Article DE Tectona grandis; Yield projection; Faustmann model; Cattle ranching; Landowner compensation; Ecosystem services ID ECOSYSTEM SERVICES; HARVEST-AGE; COSTA-RICA; PLANTATIONS; GROWTH; FOREST; PAYMENTS; CARBON; MODEL AB Reforestation and forest conservation are important issues in the Panama Canal Watershed (PCW). Uncertainty remains about relative net benefits of profit-maximizing timber rotations compared to the net present value of incumbent land uses such as cattle ranching. The scientific and popular literatures have displayed enthusiasm for teak (Tectona grandis) and native species plantations. We estimate a realistic yield model for teak, an exotic tree species, based on growth data from actual small scale landholders who were incentivized to convert lands to teak plantations. We use a suite of well fit yield models to solve for the optimal Faustmann rotation and compute the net present value (NPV) of a teak plantation to a private land manager as a starting point for understanding land-use patterns. We compare the NPV from forestry to cattle and find that site characteristics, discount rates, and market prices are all important factors in influencing the land manager's decision to switch from cattle ranching to plantation forestry. We find that traditional cattle ranching is economically competitive, in terms of NPV, with and may often outperform teak plantations within the PCW. This result is robust to the teak yield model selected. (C) 2015 Elsevier B.V. All rights reserved. C1 [Stefanski, Stephanie F.; Shi, Xiangying; Fenichel, Eli P.] Yale Univ, Yale Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Stefanski, Stephanie F.] Duke Univ, Nicholas Sch Environm, Durham, NC 27708 USA. [Shi, Xiangying] Shan Shui Conservat Ctr, Beijing, Peoples R China. [Hall, Jefferson S.; Hernandez, Andres] Smithsonian Trop Res Inst, Panama City, Panama. RP Fenichel, EP (reprint author), Yale Univ, Sch Forestry & Environm Studies, 195 Prospect St, New Haven, CT 06511 USA. OI Fenichel, Eli/0000-0002-7649-8250 FU Faculty Research Grant through F.K. Weyerhaeuser Memorial Fund from NSF [EAR-1360369]; ForestGEO, forest component of the Smithsonian Institution Global Observatory (SIGEO) FX This study was funded by a Faculty Research Grant through the F.K. Weyerhaeuser Memorial Fund administered by the Center for Business and the Environment at Yale, from NSF award EAR-1360369 Collaborative Research: Planning and Land Management in Tropical Ecosystem; Complexities of land-use and hydrology coupling in the Panama Canal Watershed, and with support from ForestGEO, the forest component of the Smithsonian Institution Global Observatory (SIGEO). The project also forms part of the Agua Salud Project, a collaboration between the Smithsonian Tropical Research Institute, the Panama Canal Authority, and other institutions. We thank Estrella Yanguas for logistical support and Edwin Hernandez, Erick Agrazal, Guillermo Fernandez, Miguel Nunez, Carlos Diaz, Sam Somerville, and Anabel Rivas for help in data collection and entry. Evan Ray provided research assistance. Mark Ashton provided helpful insights during the research effort. Sun Joseph Chang provided helpful comments on an earlier version of this paper. NR 53 TC 0 Z9 0 U1 1 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1389-9341 EI 1872-7050 J9 FOREST POLICY ECON JI Forest Policy Econ. PD JUL PY 2015 VL 56 BP 48 EP 56 DI 10.1016/j.forpol.2015.04.001 PG 9 WC Forestry SC Forestry GA CK0IG UT WOS:000355888300006 ER PT J AU Erwin, DH AF Erwin, D. H. TI A public goods approach to major evolutionary innovations SO GEOBIOLOGY LA English DT Article ID NEOPROTEROZOIC SNOWBALL-EARTH; GENE REGULATORY NETWORKS; GREAT OXIDATION EVENT; ECOLOGICAL OPPORTUNITY; EUKARYOTIC EVOLUTION; ECOSYSTEM ENGINEERS; OCEAN; ORGANISMS; ANIMALS; HISTORY AB The history of life is marked by a small number of major transitions, whether viewed from a genetic, ecological, or geological perspective. Specialists from various disciplines have focused on the packaging of information to generate new evolutionary individuals, on the expansion of ecological opportunity, or the abiotic drivers of environmental change to which organisms respond as the major drivers of these episodes. But the critical issue for understanding these major evolutionary transitions (METs) lies in the interactions between environmental, ecologic, and genetic change. Here, I propose that public goods may serve as one currency of such interactions: biological products that are non-excludable and non-rivalrous. Such biological public goods may be involved in either the generation of new evolutionary variation, as with genetic sequences that are easily transferred between different microbial lineages, or in the construction of new ecological niches, as with the progressive oxygenation of the oceans and atmosphere. Attention to public goods emphasizes the processes by which organisms actively construct their own evolutionary opportunities. Such public goods may have facilitated some METs. C1 Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. RP Erwin, DH (reprint author), Smithsonian Inst, Dept Paleobiol, MRC 121, Washington, DC 20560 USA. EM erwind@si.edu FU NASA Astrobiology Institute FX This research was funded by a grant from the NASA Astrobiology Institute to the MIT node. I appreciate perceptive comments on an earlier draft from G. Budd, J. Mcinerny, and an anonymous reviewer. NR 87 TC 5 Z9 5 U1 5 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1472-4677 EI 1472-4669 J9 GEOBIOLOGY JI Geobiology PD JUL PY 2015 VL 13 IS 4 BP 308 EP 315 DI 10.1111/gbi.12137 PG 8 WC Biology; Environmental Sciences; Geosciences, Multidisciplinary SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Geology GA CK3AP UT WOS:000356087700002 PM 25867676 ER PT J AU Angelova, LV Berrie, BH de Ghetaldi, K Kerr, A Weiss, RG AF Angelova, Lora Vihrova Berrie, Barbara H. de Ghetaldi, Kristen Kerr, Amber Weiss, Richard G. TI Partially hydrolyzed poly(vinyl acetate)-borax-based gel-like materials for conservation of art: Characterization and applications SO STUDIES IN CONSERVATION LA English DT Article DE Gels; Cleaning; Conservation; Treatments; Polymers; Painting conservation; Materials; Hydrolyzed poly(vinyl acetate) ID AQUEOUS-SOLUTIONS; EASEL PAINTINGS; DISPERSIONS; FLUORESCEIN; SCIENCE; BORATE AB A versatile gel-like system for the treatment of art has been prepared from partially hydrolyzed poly(vinyl acetate), borax, and large fractions of ethanol, isopropyl alcohol, n-propyl alcohol, and acetone. Variables such as the concentrations of the two gelating components, the degree of hydrolysis and molecular weight of the polymer, and the type of liquid gelated were investigated to establish formulations of gels with physical and chemical properties that are best suited for specific applications. The gels were designed to have an elastic character that allows them to conform to the topography of complex surfaces and be removed with ease by being lifted from the surface. Results from fluorescence studies demonstrated that the solvent is constrained within the area of the gel, allowing for localized treatment. Polymer and boron residues were not detected after cleaning tests on acrylic and dammar test paint-outs, and on two oil paintings with degraded surface coatings. The efficacy of the cleaning systems was determined visually. Studies of the materials removed during treatments showed that the gels appear to act by softening the coating surface while typically a pass with a solvent-dampened swab after gel treatment removes the softened coating. Two case studies and notes on other applications of the gels are described; recipes and preparation procedures are included. C1 [Angelova, Lora Vihrova; Weiss, Richard G.] Georgetown Univ, Dept Chem, Washington, DC 20057 USA. [Berrie, Barbara H.] Natl Gallery Art, Conservat Div, Washington, DC 20565 USA. [de Ghetaldi, Kristen] Univ Delaware, Winterthur Museum, Art Conservat Dept, Newark, DE USA. [Kerr, Amber] Smithsonian Amer Art Museum, Lunder Conservat Ctr, Washington, DC USA. RP Angelova, LV (reprint author), Georgetown Univ, Dept Chem, Reiss Sci Bldg 240,37th & O St NW, Washington, DC 20057 USA. EM angelovalora@gmail.com FU U.S. National Science Foundation [CHE-1147353]; Clare Boothe Luce Fellowship FX The U.S. National Science Foundation is gratefully acknowledged for its support of this research through grant CHE-1147353 given to Georgetown University. Dr Angelova is grateful for support through a Clare Boothe Luce Fellowship. The Kuraray Co. Ltd. generously supplied the polymer samples. We appreciate the discussions, ideas, and cooperation from our collaborators at the University of Florence, Professors Piero Baglioni and Luigi Dei, and Dr. Emiliano Carretti. We thank Drs Christopher Maines, Suzanne Lomax, and Mathieu Thoury for help with instrumentation and analysis at the NGA; Brian Baade for preparation of the paint-outs simulating Henry Ossawa Tanner's methods; Tiarna Doherty at the Lunder Conservation Center; Samantha Springer and fellow conservators at the Cleveland Museum of Art; Ana Alba, Stephan Wilcox and conservators at the NGA; Gene Karraker at the Getty Museum; conservators at the Los Angeles County Museum of Art, the Tate Britain, and those working privately in the Los Angeles and London areas who attended our talks and workshops for their invaluable questions, suggestions, and willingness to test the xPVAc-borate gels. We also thank Drs Gerald O. Brown and Patricia M. Cotts of DuPont Chemical Solutions Enterprises for performing the GPC experiments. NR 39 TC 4 Z9 4 U1 3 U2 29 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 JUL PY 2015 VL 60 IS 4 BP 227 EP 244 DI 10.1179/2047058413Y.0000000112 PG 18 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA CK2UK UT WOS:000356068700002 ER PT J AU Hertel, F Maldonado, JE Sustaita, D AF Hertel, Fritz Maldonado, Jesus E. Sustaita, Diego TI Wing and hindlimb myology of vultures and raptors (Accipitriformes) in relation to locomotion and foraging SO ACTA ZOOLOGICA LA English DT Article DE Accipitridae; Cathartidae; hindlimbs; myology; raptors; vultures; wings ID PIGEON COLUMBA-LIVIA; FUNCTIONAL-MORPHOLOGY; EVOLUTIONARY HISTORY; COMPARATIVE ANATOMY; FALCONS FALCONIDAE; PELVIC APPENDAGE; KILLING BEHAVIOR; FLIGHT BEHAVIOR; GLIDING FLIGHT; AVIAN FLIGHT AB Herein, we compare functional muscle properties among convergent forms of large, obligate avian scavengers. We performed quantitative analyses of all the muscle masses and cross-sectional areas (CSA) of the wings and hindlimbs of five species from two families, Cathartidae (New World vultures; Cathartes aura and Vultur gryphus) and Accipitridae (Old World vultures and raptors; Gyps africanus, Aquila rapax, and Buteo lineatus). These species comprise two paraphyletic functional groups, raptors (Aquila and Buteo) and vultures (Gyps, Cathartes, and Vultur). Our ordination analyses based on all of the muscles of the wings, hindlimbs, and wing and hindlimb muscles combined produced patterns that appeared to be more related to phylogeny, with a hint of a functional signal in wing muscle CSA. However, when wing muscles were grouped according to their functional roles (upstroke, downstroke, and wing stabilization), the percentages of mass and CSA allocated to the upstroke and stabilizing muscles were 1.4-5% greater in the vultures than in the raptors. Conversely, when hindlimb muscles were grouped according to their roles in grasping and terrestrial locomotion, the percentages of mass and CSA allocated to grasping muscles were 5.9-14% greater in the raptors. Our results provide a baseline for future lines of inquiry aimed at understanding how muscle mass and CSA are affected differentially across locomotor modules, possibly in response to differential demands on wing and hindlimb function experienced by these disparate accipitriform clades. C1 [Hertel, Fritz] Calif State Univ Northridge, Dept Biol, Northridge, CA 91330 USA. [Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC USA. [Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Sustaita, Diego] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. RP Hertel, F (reprint author), Calif State Univ Northridge, Dept Biol, 18111 Nordhoff St, Northridge, CA 91330 USA. EM fritz.hertel@csun.edu NR 95 TC 1 Z9 1 U1 3 U2 22 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 JUL PY 2015 VL 96 IS 3 BP 283 EP 295 DI 10.1111/azo.12074 PG 13 WC Anatomy & Morphology; Zoology SC Anatomy & Morphology; Zoology GA CJ6SJ UT WOS:000355623600002 ER PT J AU Meijer, HJM Tocheri, MW Due, RA Sutikna, T Saptomo, EW James, HF AF Meijer, Hanneke J. M. Tocheri, Matthew W. Due, Rokus Awe Sutikna, Thomas Saptomo, E. Wahyu James, Helen F. TI Continental-style avian extinctions on an oceanic island SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Birds; Extinction; Flores; Islands; Late Pleistocene; Wallacea ID LIANG BUA FLORES; LATE PLEISTOCENE; PREHISTORIC EXTINCTIONS; INDONESIA; BIRDS; PATTERNS; PACIFIC; AVIFAUNA; BIODIVERSITY; BIOGEOGRAPHY AB The Indonesian islands have long been recognized for their rich and unique avifaunas, but little is known regarding how past processes and events have shaped current avian distributions. Here we compare the modern non-passerine avifauna of Flores with the Late Pleistocene non-passerine fossil assemblage from the cave site of Liang Bua to assess whether the Late Pleistocene assemblage differs from the modern avifauna. Randomized permutation tests failed to detect a statistically significant difference in body size distributions, but a significant difference in dietary guild was found, as the modem fauna lacks scavengers. The emerging pattern of avian extinctions on Flores is characterized by a low proportion of extinct species, a loss of large-bodied species, and apparently minor effects on avian community structure. This is in contrast to other oceanic islands, which experienced dramatic changes in avifauna after the arrival of modern humans. Flores' close proximity to other islands and landmasses likely allowed for population connectivity that buffered populations from extinction. Widespread species may also have been able to recolonize if local extirpations took place. The extinction of the large-bodied avian scavengers Leptoptilos robustus and Trigonoceps sp. on Flores is consistent with the pattern of human-caused extinctions on other oceanic islands. However, the loss of these two large scavenging species may be linked to the extinction of the pygmy proboscidean (Stegodon florensis insularis). Such a dependence of avian species on mammalian megafauna, leading to extinction by trophic cascade, is characteristic of continental Late Pleistocene extinctions. (C) 2015 Elsevier B.V. All rights reserved. C1 [Meijer, Hanneke J. M.; James, Helen F.] Smithsonian Inst, Div Birds, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Meijer, Hanneke J. M.; Tocheri, Matthew W.] Smithsonian Inst, Dept Anthropol, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20013 USA. [Meijer, Hanneke J. M.] Inst Catala Paleontol Miqual Crusafont, Barcelona 08193, Spain. [Tocheri, Matthew W.] Lakehead Univ, Dept Anthropol, Thunder Bay, ON P78 5Z5, Canada. [Due, Rokus Awe; Sutikna, Thomas; Saptomo, E. Wahyu] Natl Ctr Archaeol, Jakarta 12510, Indonesia. [Sutikna, Thomas] Univ Wollongong, Ctr Archaeol Sci, Wollongong, NSW, Australia. RP Meijer, HJM (reprint author), Senckenberg Forschungsinst & Nat Museum, Dept Ornithol, Senckenberganlage 25, D-60325 Frankfurt, Germany. EM Hanneke.Meijer@senckenberg.de RI Meijer, Hanneke/A-1912-2013; OI Meijer, Hanneke/0000-0001-7066-6869; Tocheri, Matthew/0000-0001-7600-8998 FU Smithsonian Institution Postdoctoral Fellowship; Smithsonian Scholarly Studies Grant Program; Beatriu de Pinos Postdoctoral Fellowship [BP-B-00174]; Spanish Ministerio de Economia y Competitividad [CGL2011-28681] FX We express our gratitude to T. Djubiantono, former Director of the National Research and Development Centre for Archaeology (ARKENAS) for permission to study the Liang Bua bird material. We thank Gene Hunt for assistance with the statistical analyses. David Steadman and an anonymous reviewer provided helpful comments on an earlier version of this manuscript. This research resulted from a Smithsonian Institution Postdoctoral Fellowship to HJMM, and was also supported by the Smithsonian Scholarly Studies Grant Program (to MWT), a Beatriu de Pinos Postdoctoral Fellowship (BP-B-00174 to HJMM) and the Spanish Ministerio de Economia y Competitividad (CGL2011-28681). NR 49 TC 2 Z9 2 U1 1 U2 9 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 JUL 1 PY 2015 VL 429 BP 163 EP 170 DI 10.1016/j.palaeo.2015.03.041 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA CJ3AF UT WOS:000355355100012 ER PT J AU Schulze, DJ Hearn, BC AF Schulze, Daniel J. Hearn, B. Carter, Jr. TI MANTLE XENOCRYSTS FROM THE MASONTOWN, PENNSYLVANIA KIMBERLITE: AN ORDINARY MANTLE WITH Si-ENRICHED SPINEL SO CANADIAN MINERALOGIST LA English DT Article DE spinel; Pennsylvania; upper mantle; Ca-ferrite; diamond; UHP; Grenville ID MINERAL INCLUSIONS; FAYETTE COUNTY; DIAMONDS; MEGACRYSTS; XENOLITHS; BENEATH AB A hypabyssal kimberlite dike in southwestern Pennsylvania (USA), emplaced through Proterozoic basement and Phanerozic cover, contains a xenocryst and xenolith assemblage typical of material sampled within the subcontinental lithosphere, including xenocrysts of Cr-rich pyrope, magnesiochromite, Cr-rich diopside, and peridotite xenoliths. Temperatures and depths of equilibration of the clinopyroxene (840 degrees C and 130 km to 1350 degrees C and 170 km) indicate some sampling in the field of diamond stability. Diamonds have not been reported, however, and the chemistry of the garnet (lherzolite, Cr-poor megacryst, and Group II eclogite) and spinel (<56.0 wt.% Cr2O3) are consistent with diamond absence and the off-craton tectonic setting of the kimberlite. An unusual feature of this suite is that, unlike most mantle xenolith/xenocryst spinel, some of those from Masontown have an unusually high silica content (to 0.59 wt.% SiO2). The significance of the high silica content is unclear, but may be related to an ultrahigh-pressure precursor chromite polymorph with a calcium ferrite structure, which can accommodate Si in solid solution. C1 [Schulze, Daniel J.] Univ Toronto, Dept Earth Sci, Mississauga, ON L5L 1C6, Canada. [Schulze, Daniel J.] Univ Toronto, Dept Chem & Phys Sci, Mississauga, ON L5L 1C6, Canada. [Hearn, B. Carter, Jr.] US Geol Survey, Reston, VA 22092 USA. [Hearn, B. Carter, Jr.] Smithsonian Inst, Washington, DC 20560 USA. RP Schulze, DJ (reprint author), Univ Toronto, Dept Earth Sci, Mississauga, ON L5L 1C6, Canada. EM daniel.schulze@utoronto.ca FU NSERC FX This paper is dedicated to the late Peter L. Roeder, who spent much of his professional career studying spinel-group minerals and who was a friend, and inspiration, to the senior author. We thank Patrick Anderson and Nic Schulze for assistance in the field, Claudio Cermignani, Martina Miklos, Alison Dias, Adrian Van Rythoven, and Yanan Liu for technical assistance, Thomas Stachel and Michael Patterson for formal reviews, Bob Martin for editorial and other suggestions, and Peter Roeder and James Brenan for helpful discussions and suggestions. This research was supported by NSERC. NR 26 TC 0 Z9 0 U1 1 U2 1 PU MINERALOGICAL ASSOC CANADA PI QUEBEC PA 490, RUE DE LA COURONNE, QUEBEC, QC G1K 9A9, CANADA SN 0008-4476 EI 1499-1276 J9 CAN MINERAL JI Can. Mineral. PD JUL PY 2015 VL 53 IS 4 BP 767 EP 773 DI 10.3749/canmin.1500056 PG 7 WC Mineralogy SC Mineralogy GA DP4ND UT WOS:000378471700011 ER PT J AU Irwin, RP Lewis, KW Howard, AD Grant, JA AF Irwin, Rossman P., III Lewis, Kevin W. Howard, Alan D. Grant, John A. TI Paleohydrology of Eberswalde crater, Mars SO GEOMORPHOLOGY LA English DT Article; Proceedings Paper CT 45th Annual Binghamton Geomorphology Symposium CY SEP 12-14, 2014 CL Knoxville, TN DE Mars; Lake; Hydrology; Eberswalde; Holden ID MARTIAN IMPACT CRATERS; ART. NO. 5025; MARGARITIFER SINUS; VALLEY NETWORKS; ALLUVIAL FANS; INTERIOR CHANNELS; FLUVIAL PROCESSES; EVOLUTION; ORIGIN; CLIMATE AB Eberswalde crater, Mars, contains a well-preserved fluvial distributary network in a likely deltaic setting. The meandering inverted paleochannels and closed drainage basin of this deposit support relatively well constrained estimates of channel-forming discharge (over an individual event flood timescale), runoff production (event and annual timescales), and longevity of deposition (geologic timescale) during the Late Hesperian to Early Amazonian Epochs. The width and meander dimensions of two inverted paleochannels reflect the channel-forming discharge from event floods (similar to 200 to 400 m(3)/s), the deposit surface indicates the level (-1400 to -1350 m) and surface area (410 to 810 km(2)) of the likely paleolake, and the topography and mapped extent of tributaries constrain the watershed area (5000 to 17,000 km2). Based on these results and terrestrial empirical constraints on evaporation and sediment concentration, we evaluated three hypothetical water sources: meltwater liberated by the nearby Holden crater impact (continuous deposition over similar to 10(1)-10(2) years), intermittent rainfall or snowmelt during finite periods controlled by orbital evolution (deposition over similar to 10(4)-10(6) years), and highly infrequent runoff or melting of accumulated snowpacks following distant impacts or secular changes in orbital parameters. Local impact-generated runoff and highly infrequent rainfall or snowmelt require unreasonably high and low rates of evaporation, respectively, to maintain the paleolake level. The local impact hypothesis alternatively depends on one flooding episode with very high concentrations of fluvial sediment that are inconsistent with morphologic considerations. Multiple primary impact craters in the area postdate Holden ejecta but were later dissected, indicating fluvial erosion long after the Holden impact Intermittent rainfall of similar to 1 cm/day and seasonal snowmelt are both consistent with our results over a deposition timescale totaling similar to 10(4)-10(6) years. Published by Elsevier B.V. C1 [Irwin, Rossman P., III; Grant, John A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, MRC 315, Washington, DC 20013 USA. [Lewis, Kevin W.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. RP Irwin, RP (reprint author), Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, MRC 315, 6th St,Independence Ave SW, Washington, DC 20013 USA. EM irwinr@si.edu; klewis@jhu.edu; ah6p@virginia.edu; grantj@si.edu NR 118 TC 4 Z9 4 U1 3 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD JUL 1 PY 2015 VL 240 SI SI BP 83 EP 101 DI 10.1016/j.geomorph.2014.10.012 PG 19 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CJ3AK UT WOS:000355355600008 ER PT J AU Matsubara, Y Howard, AD Burr, DM Williams, RME Dietrich, WE Moore, JM AF Matsubara, Yo Howard, Alan D. Burr, Devon M. Williams, Rebecca M. E. Dietrich, William E. Moore, Jeffery M. TI River meandering on Earth and Mars: A comparative study of Aeolis Dorsa meanders, Mars and possible terrestrial analogs of the Usuktuk River, AK, and the Quinn River, NV SO GEOMORPHOLOGY LA English DT Article; Proceedings Paper CT 45th Annual Binghamton Geomorphology Symposium CY SEP 12-14, 2014 CL Knoxville, TN DE Meandering rivers; Terrestrial analog; Aeolis Dorsa; Mud-dominated; Permafrost controlled ID MEDUSAE FOSSAE FORMATION; MARTIAN OUTFLOW CHANNELS; ARCTIC COASTAL-PLAIN; THAW LAKE BASINS; RIPARIAN VEGETATION; BONNEVILLE BASIN; GREAT-BASIN; FLOODPLAIN FORMATION; SEDIMENT TRANSPORT; WIDTH ADJUSTMENT AB The paleo-meanders in the Aeolis Dorsa (AD) region show that meandering channels can develop in the absence of vegetation. Three possible mechanisms other than vegetation could contribute to the bank cohesion required to promote meandering: permafrost, abundant mud, and chemical cementation. Banks at the meandering Quinn River show little vegetation cover. Almost all sediment samples collected from the Quinn River deposits contain at least 41% mud (silt/clay), which is much higher than for most meandering streams. Ion chromatography (IC) analysis and scanning electron microscope (SEM) images showed presence of salts in river waters and sediments which may induce fine sediment to flocculate and be deposited. We find that bank cohesion promoting meandering can be provided by silt/clay, the deposition of which may be induced by dissolved salts. The sinuous Usuktuk River in the continuous permafrost region near Barrow, Alaska exhibited no exposed permafrost on stream banks. Instead vegetation seemed to be the dominant control of bank erosion. We have not found evidence for ice control of bank cohesion in this or other terrestrial rivers of similar size and in meandering pattern to the Martian AD meanders. We conclude that bank cohesion in the AD meanders was probably provided by deposition of fine suspended sediment that was flocculated by dissolved salts. (C) 2014 Elsevier B.V. All rights reserved. C1 [Matsubara, Yo] Ctr Earth & Planetary Studies, Natl Air & Space Museum, Smithsonian Inst, Washington, DC 20013 USA. [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Burr, Devon M.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Dietrich, William E.] Univ Calif Berkeley, Dept Earth & Planetary Sci, Berkeley, CA 94720 USA. [Moore, Jeffery M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Matsubara, Y (reprint author), Ctr Earth & Planetary Studies, Natl Air & Space Museum, Smithsonian Inst, Independence Ave ,6th St SW,MRC 315,POB 37012, Washington, DC 20013 USA. EM matsubaray@si.edu OI Howard, Alan/0000-0002-5423-1600 NR 175 TC 5 Z9 5 U1 3 U2 30 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0169-555X EI 1872-695X J9 GEOMORPHOLOGY JI Geomorphology PD JUL 1 PY 2015 VL 240 SI SI BP 102 EP 120 DI 10.1016/j.geomorph.2014.08.031 PG 19 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA CJ3AK UT WOS:000355355600009 ER PT J AU Carrillo-Briceno, JD De Gracia, C Pimiento, C Aguilera, OA Kindlimann, R Santamarina, P Jaramillo, C AF Carrillo-Briceno, Jorge D. De Gracia, Carlos Pimiento, Catalina Aguilera, Orangel A. Kindlimann, Rene Santamarina, Patricio Jaramillo, Carlos TI A new Late Miocene chondrichthyan assemblage from the Chagres Formation, Panama SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Neogene; Tropical America; Panama Canal Basin; Sharks; Rays; Paleoecology ID SOUTH-AMERICA; ISISTIUS-BRASILIENSIS; GATUN FORMATION; WESTERN PANAMA; PACIFIC-OCEAN; NEOGENE; ATLANTIC; ISTHMUS; CLOSURE; SHARKS AB The ILate Miocene Chagres Formation from northern Panama contains the youngest outcrops of the Panama Canal Basin. Here we report two chondrichthyan assemblages that include 30 taxa from both the Rio Indio and Chagres Sandstone Members of the Chagres Formation. We report 18 new fossil records for Panama and four for tropical America, constituting the most diverse chondrichthyan association for the Cenozoic of Panama. We performed a paleobathymetry analysis based on the modern water depth preference of extant chondrichthyan taxa. The assemblage from the Rio Indio Member is characterized by taxa with neritic affinities, suggesting depths <100 m, whereas the assemblage from the Chagres Sandstone Member is dominated by taxa with oceanic affinities, suggesting 200-300 m water depths. The Chagres Sandstone Member could have accumulated at the edge of a platform-upper slope, bordered by a deep oceanic margin. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Carrillo-Briceno, Jorge D.; Kindlimann, Rene] Univ Zurich, Paleontol Inst & Museum, CH-8006 Zurich, Switzerland. [De Gracia, Carlos; Pimiento, Catalina; Jaramillo, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa 084303092, Ancon, Panama. [Pimiento, Catalina] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Pimiento, Catalina] Univ Florida, Gainesville, FL 32611 USA. [Aguilera, Orangel A.] Univ Fed Fluminense, Dept & Posgrad Biol Marinha & Ambientes Costeiros, Inst Biol, BR-24020141 Niteroi, RJ, Brazil. [Santamarina, Patricio] Museo Argentino Ciencias Nat Bernardino Rivadavia, Buenos Aires, DF, Argentina. RP De Gracia, C (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa 084303092, Ancon, Panama. EM jorge.carrillo@pim.uzh.ch; degraciac@gmail.com; pimientoc@ufl.edu; orangel.aguilera@gmail.com; santamarinape@gmail.com; jaramilloc@si.edu OI De Gracia, Carlos/0000-0003-0637-3302; Carrillo Briceno, Jorge Domingo/0000-0002-8652-7692 FU SENACYT [APY-NI10-016A]; Ricardo Perez S.A; STRI-Tupper Paleontological Fund; Swiss National Science Foundation [31003A-149605]; International Travel Grant for Vertebrate Paleontology from the University of Florida FX This project has been supported by a SENACYT APY-NI10-016A grant (National Secretary of Science and Technology of Panama), Ricardo Perez S.A, STRI-Tupper Paleontological Fund, Swiss National Science Foundation grant 31003A-149605 (to Marcelo Sanchez- Villagra), and the International Travel Grant for Vertebrate Paleontology from the University of Florida. Thanks to the Evolutionary Morphology and Palaeobiology group at the Palaeontological Institute and Museum at the University of Zurich, Switzerland, and the Programa de Pos-graduacao em Biologia Marinha e Ambientes Costeiros at the Universidade Federal Fluminense in Brazil for their valuable assistance and collaboration. We thank the Direccion de Recursos Minerales of Panama for collecting permits; Carlos Jaramillo's lab members at STRI; Austin Hendy and the paleontology team from the University of Florida; and friends from Panama for logistical support. Special thanks to Jorge Ceballos, Morgane Brosse, and Marc Leu for their help with the microscopic photography, Juan David Carrillo and Thodoris Argyriou for their valuable assistance with analysis and with review of the text, and Werner Schwarzhans and an anonymous reviewer who helped improving it. NR 131 TC 7 Z9 7 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD JUL PY 2015 VL 60 BP 56 EP 70 DI 10.1016/j.jsames.2015.02.001 PG 15 WC Geosciences, Multidisciplinary SC Geology GA CJ3BN UT WOS:000355358500005 ER PT J AU Bretfeld, M Doerner, JP Franklin, SB AF Bretfeld, Mario Doerner, James P. Franklin, Scott B. TI Radial growth response and vegetative sprouting of aspen following release from competition due to insect-induced conifer mortality SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Populus tremuloides; Mountain pine beetle; Dendrochronology; Clonal growth; Suckering; Release ID MOUNTAIN PINE-BEETLE; YELLOWSTONE-NATIONAL-PARK; POTENTIAL FIRE BEHAVIOR; FOREST DIE-OFF; POPULUS-TREMULOIDES; TREMBLING ASPEN; TREE MORTALITY; KNOWLEDGE GAPS; NORTH-AMERICA; COLORADO AB Eruptive bark beetle outbreaks such as the recent mountain pine beetle epidemic in western North America often result in substantial changes to species composition, abiotic factors, and a highly altered fuel complex. Little is known about the implications of these outbreaks to non-host species, such as aspen (Populus tremuloides Michx.), which may be beneficiaries due to release from competition. We investigated radial growth response in aspen following mountain pine beetle-induced conifer mortality in north-central Colorado through dendrochronological analysis using the percent growth change method based on 5-year and 10-year running medians, and we quantified. regeneration responses in these areas compared to areas where beetle activity was largely absent. We hypothesized that growth in mature aspen would increase, expressed through wider annual growth rings, while vegetative regeneration (i.e. resprouting from the parent root system) would not increase in forests affected by bark beetles. Results showed a clear radial growth release in mixed aspen-conifer stands that were subject to extensive conifer mortality but not in forests that remained largely unaffected by beetles. Comparison of extent of suckering showed no significant differences, supporting our hypotheses and suggesting that additional resources due to release from competition were allocated towards radial growth rather than initiation of sucker growth, potentially indicating a trade-off between maintenance of existing stems and regeneration. Results from this study provide the first account of radial release detection in aspen following beetle-induced conifer mortality and help predict aspen persistence and future stand composition in these forests. Additional research, with a higher sample size and more time between sampling and bark beetle disturbance is highly recommended to confirm our findings and optimize release detection methods in aspen. (C) 2015 Elsevier B.V. All rights reserved. C1 [Bretfeld, Mario; Franklin, Scott B.] Univ No Colorado, Sch Biol Sci, Greeley, CO 80639 USA. [Doerner, James P.] Univ No Colorado, Dept Geog & GIS, Greeley, CO 80639 USA. RP Bretfeld, M (reprint author), Smithsonian Trop Res Inst, Roosvelt Ave, Balboa, Ancon, Panama. EM m.bretfeld@gmail.com; james.doerner@unco.edu; scott.franklin@unco.edu FU Colorado Mountain Club FX The authors thank the Fraser Experimental Forest for facilitating access to sample areas and providing information. For field and laboratory assistance we thank Megan Heier, Daniel Beverly, John Hoke, and Larry Franklin. For helpful comments on the manuscript, we thank Robert M. Hubbard and Mitchell McGlaughlin, as well as two anonymous reviewers. Funding for this research was provided by the Colorado Mountain Club. NR 68 TC 2 Z9 2 U1 6 U2 29 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 JUL 1 PY 2015 VL 347 BP 96 EP 106 DI 10.1016/j.foreco.2015.03.006 PG 11 WC Forestry SC Forestry GA CI2LR UT WOS:000354579600009 ER PT J AU Tomasini, EP Dubois, CMF Little, NC Centeno, SA Maier, MS AF Tomasini, Eugenia P. Favier Dubois, Cristian M. Little, Nicole C. Centeno, Silvia A. Maier, Marta S. TI Identification of pyroxene minerals used as black pigments in painted human bones excavated in Northern Patagonia by Raman spectroscopy and XRD SO MICROCHEMICAL JOURNAL LA English DT Article DE Raman microspectroscopy; Micro-X-ray diffraction; Pyroxenes; Painted bones; Iron oxides ID MANGANESE OXIDES; ROCK ART; X-RAY; SPECTRA; MICROSPECTROSCOPY; MICROSCOPY; FRANCE; QUERCY AB The skeletal remains of seven individuals were excavated in a secondary burial context in the site of Cima de los Huesos, in the San Matias Gulf (Rio Negro, Argentina). AMS dating of two samples for this site to 1173 +/- 45 and 1225 +/- 47 years BP make it one of the earliest burials of its kind uncovered so far in the Patagonian region. Among the findings, the skeleton of a male painted with parallel lines alternating red and black colors was uncovered. SEM-EDS elemental analysis of microsamples removed from the red and the black pigments showed the presence of Mn and Fe as the main components, respectively. Raman microspectroscopy combined with micro-X-ray diffraction analysis showed that the red pigment contains hematite and that the black pigment is composed of members of the pyroxene mineral group, ferrosilite (FeSiO3) and enstatite (MgSiO3) along with kanoite (MnMgSi2O6). This is, to our knowledge, the first report on the use of pyroxenes as black pigments to decorate human remains or archeological artifacts in South America. No organic compounds that could have been used as binders for the paints were detected by FTIR-ATR. Contamination due to quartz and aluminosilicates, mainly microcline and albite, from the burial environment did not allow determining whether clay minerals were used in the paints as binders and/or extenders. The multitechnique approach used was crucial to overcome the limitations of the individual techniques to firmly identify Mn-containing black pigments. (C) 2015 Elsevier B.V. All rights reserved. C1 [Tomasini, Eugenia P.; Maier, Marta S.] Univ Buenos Aires, UMYMFOR CONICET, Buenos Aires, DF, Argentina. [Tomasini, Eugenia P.; Maier, Marta S.] Univ Buenos Aires, Fac Ciencias Exactas & Nat, Dept Quim Organ, Buenos Aires, DF, Argentina. [Favier Dubois, Cristian M.] INCUAPA CONICET, Olavarria, Argentina. [Favier Dubois, Cristian M.] UNCPBA, Fac Ciencias Sociales, Dept Arqueol, Olavarria, Argentina. [Little, Nicole C.] Museum Support Ctr, Museum Conservat Inst, Smithsonian Inst, Suitland, MD 20746 USA. [Centeno, Silvia A.] Metropolitan Museum Art, Dept Sci Res, New York, NY 10028 USA. RP Centeno, SA (reprint author), Metropolitan Museum Art, Dept Sci Res, 1000 Fifth Ave, New York, NY 10028 USA. EM eugeniatomasini@gmail.com; cfavier3@gmail.com; silvia.centeno@metmuseum.org; maier@qo.fcen.uba.ar RI Little, Nicole/L-6420-2015; OI Little, Nicole/0000-0002-9533-3187; Centeno, Silvia/0000-0002-8496-4426; Maier, Marta/0000-0002-9160-1826 FU Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET) [11220130100288CO]; Agenda Nacional de Promocion Cientifica y Tecnologica (ANPCyT); University of Buenos Aires, Argentina [008BA]; Fundacion Bunge y Born FX The authors are indebted to the Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET), Agenda Nacional de Promocion Cientifica y Tecnologica (ANPCyT), and the University of Buenos Aires (008BA), Argentina, for financial support. E.P.T. thanks CONICET (11220130100288CO) and Fundacion Bunge y Born for a Postdoctoral Fellowship; C.M.F.D., E.P.T. and M.S.M. are research members of CONICET. NR 33 TC 2 Z9 2 U1 3 U2 32 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0026-265X EI 1095-9149 J9 MICROCHEM J JI Microchem J. PD JUL PY 2015 VL 121 BP 157 EP 162 DI 10.1016/j.microc.2015.03.003 PG 6 WC Chemistry, Analytical SC Chemistry GA CI2PO UT WOS:000354589700019 ER PT J AU Jimenez, H Dumas, P Bigot, L Ferraris, J AF Jimenez, H. Dumas, P. Bigot, L. Ferraris, J. TI Harvesting effects on tropical invertebrate assemblages in New Caledonia SO FISHERIES RESEARCH LA English DT Article DE Marine benthos; Fishery; Coral reef; Seagrass; MPA ID COASTAL MARINE COMMUNITIES; SANDY BEACH POPULATIONS; NEW-SOUTH-WALES; MACROBENTHIC COMMUNITIES; CORAL-REEFS; HUMAN EXPLOITATION; BARNSTABLE-HARBOR; HUMAN DISTURBANCE; INTERTIDAL ZONE; HUMAN-EXCLUSION AB Despite the importance of invertebrate resources for Pacific coral reef islands, few studies have specifically addressed the effects of harvesting on invertebrate assemblages including targeted and non-targeted species. The impacts of recreational harvesting on reef and seagrass invertebrate assemblages in New Caledonia (South Pacific) are investigated by comparing communities in non-MPA and MPA areas. Sampling was done using a standard core method on seagrasses and by visual survey along belt transects on reefs. A total of 371 species were recorded, 174 on seagrasses and 254 on reefs, with 57 common species. Reef and seagrass invertebrate communities were very different in MPA and non-MPA areas. On both habitats, MPAs were identified as undisturbed areas while non-MPAs were defined as moderately disturbed with a predominance of small-sized and opportunistic species. Fishing not only affects target species but also non-target species through secondary effects. These results highlight the necessity of a community based approach for the conservation of resources in tropical poorly known environments. (C) 2015 Elsevier B.V. All rights reserved. C1 [Jimenez, H.; Dumas, P.] Inst Rech Dev, UMR ENTROPIE, Lab Excellence LabEx CORAIL, Noumea 98848, New Caledonia. [Bigot, L.] Univ La Reunion, UMR ENTROPIE, Lab Excellence LabEx CORAIL, F-97715 St Denis, France. [Ferraris, J.] Inst Rech Dev, UMR ENTROPIE, Lab Excellence LabEx CORAIL, Observ Oceanol Banyuls, F-66550 Banyuls Sur Mer, France. RP Jimenez, H (reprint author), Smithsonian Environm Res Ctr, 3150 Paradise Dr, Tiburon, CA 94920 USA. EM haizea.jimenez@gmail.com OI Dumas, Pascal/0000-0001-7369-8989 FU IRD research program; PAMPA research program; GAIUS research program; EAJ Basque Government FX The authors would like to thank J. Baly for his invaluable field and laboratory assistance. This work was made possible through joint financial support from IRD, PAMPA, GAIUS research programs and EAJ Basque Government funding for the PhD thesis of Haizea Jimenez. NR 75 TC 1 Z9 1 U1 6 U2 33 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0165-7836 EI 1872-6763 J9 FISH RES JI Fish Res. PD JUL PY 2015 VL 167 BP 75 EP 81 DI 10.1016/j.fishres.2015.02.001 PG 7 WC Fisheries SC Fisheries GA CH0VO UT WOS:000353740700009 ER PT J AU Mumby, HS Mar, KU Thitaram, C Courtiol, A Towiboon, P Min-Oo, Z Htut-Aung, Y Brown, JL Lummaa, V AF Mumby, Hannah S. Mar, Khyne U. Thitaram, Chatchote Courtiol, Alexandre Towiboon, Patcharapa Min-Oo, Zaw Htut-Aung, Ye Brown, Janine L. Lummaa, Virpi TI Stress and body condition are associated with climate and demography in Asian elephants SO CONSERVATION PHYSIOLOGY LA English DT Article DE Elephas maximus; faeces; glucocorticoids; hormone; seasonality; weight ID PHYSIOLOGICAL STRESS; AFRICAN ELEPHANTS; PLASMA-CORTICOSTERONE; POPULATION VIABILITY; ENZYME-IMMUNOASSAY; LOXODONTA-AFRICANA; SALIVARY CORTISOL; ZOO ELEPHANTS; MYANMAR BURMA; MAXIMUS AB Establishing links between ecological variation, physiological markers of stress and demography is crucial for understanding how and why changes in environmental conditions affect population dynamics, and may also play a key role for conservation efforts of endangered species. However, detailed longitudinal studies of long-lived species are rarely available. We test how two markers of stress and body condition vary through the year and are associated with climatic conditions and large-scale mortality and fertility variation in the world's largest semi-captive population of Asian elephants employed in the timber industry in Myanmar. Glucocorticoid metabolites (used as a proxy for stress levels in 75 elephants) and body weight (used as a proxy for condition in 116 elephants) were monitored monthly across a typical monsoon cycle and compared with birth and death patterns of the entire elephant population over half a century (n = 2350). Our results show seasonal variation in both markers of stress and condition. In addition, this variation is correlated with population-level demographic variables. Weight is inversely correlated with population mortality rates 1 month later, and glucocorticoid metabolites are negatively associated with birth rates. Weight shows a highly positive correlation with rainfall 1 month earlier. Determining the factors associated with demography may be key to species conservation by providing information about the correlates of mortality and fertility patterns. The unsustainability of the studied captive population has meant that wild elephants have been captured and tamed for work. By elucidating the correlates of demography in captive elephants, our results offer management solutions that could reduce the pressure on the wild elephant population in Myanmar. C1 [Mumby, Hannah S.; Mar, Khyne U.; Lummaa, Virpi] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Thitaram, Chatchote; Towiboon, Patcharapa] Chiang Mai Univ, Fac Vet Med, Chiang Mai 50100, Thailand. [Courtiol, Alexandre] Leibniz Inst Zoo & Wildlife Res, Dept Evolutionary Genet, D-10315 Berlin, Germany. [Min-Oo, Zaw] Myanma Timber Enterprise, Minist Environm Conservat & Forestry, Yangon, Myanmar. [Htut-Aung, Ye] Yezin Univ, Dept Vet Med, Naypyidaw, Myanmar. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. RP Mumby, HS (reprint author), Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. EM h.mumby@sheffield.ac.uk OI Courtiol, Alexandre/0000-0003-0637-2959 FU Leverhulme Trust; Natural Environment Research Council; Nando Peretti Foundation; Rufford Foundation; European Research Council FX V.L., H.S.M. and K.U.M. would like to thank the Leverhulme Trust, Natural Environment Research Council for funding the Myanmar Timber Elephant project. The project received additional support from the Nando Peretti Foundation (V.L.), The Rufford Foundation (K.U.M.) and European Research Council (V.L.). NR 70 TC 1 Z9 1 U1 9 U2 14 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 2051-1434 J9 CONSERV PHYSIOL JI Conserv. Physiol. PD JUN 30 PY 2015 VL 3 AR cov030 DI 10.1093/conphys/cov030 PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences; Physiology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Physiology GA DK8SJ UT WOS:000375198300001 PM 27293715 ER PT J AU Norden, N Angarita, HA Bongers, F Martinez-Ramos, M Granzow-de la Cerda, I Breugel, M Lebrija-Trejos, E Meave, JA Vandermeer, J Williamson, GB Finegan, B Mesquita, R Chazdon, RL AF Norden, Natalia Angarita, Hector A. Bongers, Frans Martinez-Ramos, Miguel Granzow-de la Cerda, Inigo van Breugel, Michiel Lebrija-Trejos, Edwin Meave, Jorge A. Vandermeer, John Williamson, G. Bruce Finegan, Bryan Mesquita, Rita Chazdon, Robin L. TI Successional dynamics in Neotropical forests are as uncertain as they are predictable SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE dynamical models; predictability; succession; tropical secondary forest; uncertainty ID TROPICAL RAIN-FORESTS; TREE COMMUNITIES; DIVERSITY; CHRONOSEQUENCES; DISTURBANCES; BIODIVERSITY; RATES AB Although forest succession has traditionally been approached as a deterministic process, successional trajectories of vegetation change vary widely, even among nearby stands with similar environmental conditions and disturbance histories. Here, we provide the first attempt, to our knowledge, to quantify predictability and uncertainty during succession based on the most extensive long-term datasets ever assembled for Neotropical forests. We develop a novel approach that integrates deterministic and stochastic components into different candidate models describing the dynamical interactions among three widely used and interrelated forest attributes-stem density, basal area, and species density. Within each of the seven study sites, successional trajectories were highly idiosyncratic, even when controlling for prior land use, environment, and initial conditions in these attributes. Plot factors were far more important than stand age in explaining successional trajectories. For each site, the best-fit model was able to capture the complete set of time series in certain attributes only when both the deterministic and stochastic components were set to similar magnitudes. Surprisingly, predictability of stem density, basal area, and species density did not show consistent trends across attributes, study sites, or land use history, and was independent of plot size and time series length. The model developed here represents the best approach, to date, for characterizing autogenic successional dynamics and demonstrates the low predictability of successional trajectories. These high levels of uncertainty suggest that the impacts of allogenic factors on rates of change during tropical forest succession are far more pervasive than previously thought, challenging the way ecologists view and investigate forest regeneration. C1 [Norden, Natalia] Fdn Cedrela, Bogota 111311, Colombia. [Norden, Natalia; Angarita, Hector A.] Pontificia Univ Javeriana, Dept Ecol & Territorio, Bogota 110231, Colombia. [Bongers, Frans] Wageningen Univ, Forest Ecol & Forest Management Grp, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Martinez-Ramos, Miguel] Univ Nacl Autonoma Mexico, Inst Invest Ecosistemas Sustentabilidad, Morelia 58190, Michoacan, Mexico. [Granzow-de la Cerda, Inigo] Univ Autonoma Barcelona, Dept Biol Anim Biol Vegetal & Ecol, E-08193 Bellaterra, Spain. [van Breugel, Michiel] Yale Natl Univ Singapore Coll, Singapore 138614, Singapore. [van Breugel, Michiel; Lebrija-Trejos, Edwin] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Lebrija-Trejos, Edwin] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Meave, Jorge A.] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Ecol Recursos Nat, Mexico City 04510, DF, Mexico. [Vandermeer, John] Univ Michigan, Dept Ecol & Evolut Biol, Ann Arbor, MI 48109 USA. [Williamson, G. Bruce] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70808 USA. [Finegan, Bryan] Trop Agr Ctr Res & Higher Educ, Prod & Conservat Forests Program, Apartado 937170, Turrialba, Costa Rica. [Mesquita, Rita] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, AM, Brazil. [Chazdon, Robin L.] Univ Connecticut, Dept Ecol & Evolut Biol, Storrs, CT 06269 USA. RP Norden, N (reprint author), Fdn Cedrela, Bogota 111311, Colombia. EM natnorden@gmail.com OI Meave, Jorge A./0000-0002-6241-8803; Chazdon, Robin/0000-0002-7349-5687 FU Panamanian Sistema Nacional de Investigadores, Secretaria Nacional de Ciencia, Tecnologia e Innovacion; National Science Foundation [DEB-1147434, DEB-1147429, DEB-0639393, DEB-9524061, DEB-0135350, DEB-0235761]; Andrew W. Mellon Foundation; University of Connecticut Research Foundation; Mexican Secretaria del Medio Ambiente y Recursos Naturales-Consejo Nacional de Ciencia y Tecnologia (CONACYT) [2002-C01-0597]; Secretaria de Educacion Publica (SEP)-CONACYT [CB-2005-01-51043]; CONACYT [2004-168169]; SEP-CONACYT [CB-2009-128136]; Universidad Nacional Autonoma de Mixico-Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica [IN216007, IN213714]; Dutch Netherlands Organization for Scientific Research-Netherlands Foundation for the Advancement of Tropical Research [W85-326] FX We are grateful to the dozens of field assistants and colleagues who participated in the extensive censuses and assisted with data management (T. V. Bentos, J. and H. Jamangape, M. Molina, J. Panigua, B. Paniagua, E. Salicetti, E. A. Perez-Garcia, J. Rodriguez-Velazquez, J. Romero, and I. E. Romero-Perez). We thank J. Chave, R. K. Colwell, A. Duque, S. Levin, A. Ramirez, S. Russo, and M. Uriarte for insightful comments. E.L.-T. acknowledges support by Panamanian Sistema Nacional de Investigadores, Secretaria Nacional de Ciencia, Tecnologia e Innovacion. The studies were financially supported by National Science Foundation Grants DEB-1147434, DEB-1147429, DEB-0639393, DEB-9524061, DEB-0135350, and DEB-0235761; grants from Andrew W. Mellon Foundation and University of Connecticut Research Foundation; Mexican Secretaria del Medio Ambiente y Recursos Naturales-Consejo Nacional de Ciencia y Tecnologia (CONACYT) 2002-C01-0597, Secretaria de Educacion Publica (SEP)-CONACYT CB-2005-01-51043, CONACYT 2004-168169, and SEP-CONACYT CB-2009-128136; Universidad Nacional Autonoma de Mixico-Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica IN216007 and IN213714; and Dutch Netherlands Organization for Scientific Research-Netherlands Foundation for the Advancement of Tropical Research W85-326. NR 40 TC 30 Z9 30 U1 18 U2 58 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 JUN 30 PY 2015 VL 112 IS 26 BP 8013 EP 8018 DI 10.1073/pnas.1500403112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL6LU UT WOS:000357079400047 PM 26080411 ER PT J AU Kartzinel, TR Chen, PA Coverdale, TC Erickson, DL Kress, WJ Kuzmina, ML Rubenstein, DI Wang, W Pringle, RM AF Kartzinel, Tyler R. Chen, Patricia A. Coverdale, Tyler C. Erickson, David L. Kress, W. John Kuzmina, Maria L. Rubenstein, Daniel I. Wang, Wei Pringle, Robert M. TI DNA metabarcoding illuminates dietary niche partitioning by African large herbivores SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE African savannas; body size; competition; coexistence; ungulates ID SAVANNA GRAZERS; ECOLOGY; DIVERSIFICATION; HETEROGENEITY; SERENGETI; RUMINANTS; ECOSYSTEM; MAMMALS; MODELS; SYSTEM AB Niche partitioning facilitates species coexistence in a world of limited resources, thereby enriching biodiversity. For decades, biologists have sought to understand how diverse assemblages of large mammalian herbivores (LMH) partition food resources. Several complementary mechanisms have been identified, including differential consumption of grasses versus nongrasses and spatiotemporal stratification in use of different parts of the same plant. However, the extent to which LMH partition food-plant species is largely unknown because comprehensive species-level identification is prohibitively difficult with traditional methods. We used DNA metabarcoding to quantify diet breadth, composition, and overlap for seven abundant LMH species (six wild, one domestic) in semiarid African savanna. These species ranged from almost-exclusive grazers to almost-exclusive browsers: Grass consumption inferred from mean sequence relative read abundance (RRA) ranged from >99% (plains zebra) to <1% (dik-dik). Grass RRA was highly correlated with isotopic estimates of % grass consumption, indicating that RRA conveys reliable quantitative information about consumption. Dietary overlap was greatest between species that were similar in body size and proportional grass consumption. Nonetheless, diet composition differed between all species-even pairs of grazers matched in size, digestive physiology, and location-and dietary similarity was sometimes greater across grazing and browsing guilds than within them. Such taxonomically fine-grained diet partitioning suggests that coarse trophic categorizations may generate misleading conclusions about competition and coexistence in LMH assemblages, and that LMH diversity may be more tightly linked to plant diversity than is currently recognized. C1 [Kartzinel, Tyler R.; Chen, Patricia A.; Coverdale, Tyler C.; Rubenstein, Daniel I.; Pringle, Robert M.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Erickson, David L.; Kress, W. John; Kuzmina, Maria L.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Rubenstein, Daniel I.; Pringle, Robert M.] Mpala Res Ctr, Nanyuki, Kenya. [Wang, Wei] Princeton Univ, Lewis Sigler Inst, Princeton, NJ 08544 USA. RP Kartzinel, TR (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. EM tylerk@princeton.edu; rpringle@princeton.edu FU Princeton Environmental Institute; US National Science Foundation [DEB1355122]; National Geographic Society [9291-13] FX B. von Holt, K. Fox-Dobbs, R. Kartzinel, R. Long, the Lewis Sigler Institute, M. Musili, H. Oyieke, and the KenBOL Project assisted with data collection and analysis. M. Brown, G. Charles, E. DeFranco, V. Ezenwa, A. Hassan, R. Hohbein, S. Kurukura, and M. Mohamed provided field support. I. Lopez produced silhouette images (Fig. 1). T. Young and three reviewers provided helpful comments. We thank the Government of Kenya for permission to conduct this research, which was supported by Grants to R.M.P. from the Princeton Environmental Institute, US National Science Foundation (DEB1355122), and National Geographic Society (9291-13). NR 57 TC 29 Z9 30 U1 24 U2 107 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 JUN 30 PY 2015 VL 112 IS 26 BP 8019 EP 8024 DI 10.1073/pnas.1503283112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL6LU UT WOS:000357079400048 PM 26034267 ER PT J AU Gutierrez, EE Maldonado, JE Radosavljevic, A Molinari, J Patterson, BD Martinez, JM Rutter, AR Hawkins, MTR Garcia, FJ Helgen, KM AF Gutierrez, Eliecer E. Maldonado, Jesus E. Radosavljevic, Aleksandar Molinari, Jesus Patterson, Bruce D. Martinez-C, Juan M. Rutter, Amy R. Hawkins, Melissa T. R. Garcia, Franger J. Helgen, Kristofer M. TI The Taxonomic Status of Mazama bricenii and the Significance of the Tachira Depression for Mammalian Endemism in the Cordillera de Merida, Venezuela SO PLOS ONE LA English DT Article ID ECOLOGICAL NICHE MODELS; SPECIES GEOGRAPHIC DISTRIBUTIONS; AMERICAN DEER; SAMPLING BIAS; BIOGEOGRAPHIC SIGNIFICANCE; MITOCHONDRIAL-DNA; GENUS CRYPTOTIS; CLIMATE-CHANGE; BROCKET DEER; CONSERVATION AB We studied the taxonomy and biogeography of Mazama bricenii, a brocket deer classified as Vulnerable by the IUCN, drawing on qualitative and quantitative morphology and sequences of the mitochondrial cytochrome-b gene. We used Ecological Niche Modeling (ENM) to evaluate the hypothesis that M. bricenii of the Venezuelan Cordillera de Merida (CM) might have become isolated from populations of its putative sister species, Mazama rufina, in the Colombian Cordillera Oriental (CO). This hypothesis assumes that warm, dry climatic conditions in the Tachira Depression were unsuitable for the species. Our analyses did not reveal morphological differences between specimens geographically attributable to M. bricenii and M. rufina, and phylogenetic analyses of molecular data recovered M. bricenii nested within the diversity of M. rufina. These results indicate that M. bricenii should be regarded as a junior synonym of M. rufina. ENM analyses revealed the existence of suitable climatic conditions for M. rufina in the Tachira Depression during the last glacial maximum and even at present, suggesting that gene flow between populations in the CO and CM may have occurred until at least the beginning of the current interglacial period and may continue today. Because this pattern might characterize other mammals currently considered endemic to the CM, we examined which of these species match two criteria that we propose herein to estimate if they can be regarded as endemic to the CM with confidence: (1) that morphological or molecular evidence exists indicating that the putative endemic taxon is distinctive from congeneric populations in the CO; and (2) that the putative endemic taxon is restricted to either cloud forest or paramo, or both. Only Aepeomys reigi, Cryptotis meridensis, and Nasuella meridensis matched both criteria; hence, additional research is necessary to assess the true taxonomic status and distribution of the remaining species thought to be CM endemics. C1 [Gutierrez, Eliecer E.; Maldonado, Jesus E.; Hawkins, Melissa T. R.; Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. [Gutierrez, Eliecer E.; Maldonado, Jesus E.; Hawkins, Melissa T. R.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC USA. [Radosavljevic, Aleksandar] Northwestern Univ, Plant Biol & Conservat, Evanston, IL USA. [Radosavljevic, Aleksandar] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Molinari, Jesus] Univ Los Andes, Fac Ciencias, Dept Biol, Merida 5101, Venezuela. [Patterson, Bruce D.] Field Museum Nat Hist, Integrat Res Ctr, Chicago, IL 60605 USA. [Martinez-C, Juan M.] Univ Antioquia, Grp Mastozool & Colecc Teriol, Inst Biol, Medellin, Colombia. [Rutter, Amy R.] Penn State Univ, Dept Ecosyst Sci & Management, University Pk, PA 16802 USA. [Hawkins, Melissa T. R.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Garcia, Franger J.] Univ Carabobo, Dept Biol, Lab Museo Zool, Valencia, Carabobo, Venezuela. RP Gutierrez, EE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20560 USA. EM GutierrezE@si.edu RI Gutierrez, Eliecer/D-5703-2014 OI Gutierrez, Eliecer/0000-0001-6790-8185 FU Peter Buck Postdoctoral Fellowship by National Museum of Natural History (NMNH), Smithsonian Institution; Small Grants Program by National Museum of Natural History (NMNH), Smithsonian Institution; Systematics Research Fund Program of the Systematics Association; Linnean Society of London; National Science Foundation (REU) through internship program Natural History Research Experiences, NMNH [EAR-1062692] FX Funding: This work was funded by a Peter Buck Postdoctoral Fellowship (to EEG) and funds from the Small Grants Program (to KMH, EEG, JEM), both provided by the National Museum of Natural History (NMNH), Smithsonian Institution; and by a grant from the Systematics Research Fund Program of the Systematics Association and Linnean Society of London (to JEM, EEG, KMH). The National Science Foundation (REU Site, EAR-1062692) provided funding through the internship program Natural History Research Experiences, NMNH (to ARR, advised by EEG and KMH). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 107 TC 3 Z9 4 U1 3 U2 4 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 JUN 29 PY 2015 VL 10 IS 6 AR e0129113 DI 10.1371/journal.pone.0129113 PG 24 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CN1BL UT WOS:000358150400016 PM 26121688 ER PT J AU Restano, M Plaut, JJ Campbell, BA Gim, Y Nunes, D Bernardini, F Egan, A Seu, R Phillips, RJ AF Restano, Marco Plaut, Jeffrey J. Campbell, Bruce A. Gim, Yonggyu Nunes, Daniel Bernardini, Fabrizio Egan, Anthony Seu, Roberto Phillips, Roger J. TI Effects of the passage of Comet C/2013 A1 (Siding Spring) observed by the Shallow Radar (SHARAD) on Mars Reconnaissance Orbiter SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE Comet Siding Spring; SHARAD ID IONS AB The close passage of Comet C/2013 A1 (Siding Spring) to Mars provided a unique opportunity to observe the interaction of cometary materials with the Martian ionosphere and atmosphere using the sounding radar SHARAD (SHAllow RADar) aboard Mars Reconnaissance Orbiter. In two nightside observations, acquired in the 10h following the closest approach, the SHARAD data reveal a significant increase of the total electron content (TEC). The observed TEC values are typical for daylight hours just after dawn or before sunset but are unprecedented this deep into the night. Results support two predictions indicating that cometary pickup O+ ions, or ions generated from the ablation of cometary dust, are responsible for the creation of an additional ion layer. C1 [Restano, Marco; Bernardini, Fabrizio; Seu, Roberto] Univ Roma La Sapienza, Dipartimento DIET, I-00185 Rome, Italy. [Plaut, Jeffrey J.; Gim, Yonggyu; Nunes, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Campbell, Bruce A.] Smithsonian Inst, Washington, DC 20560 USA. [Egan, Anthony] Southwest Res Inst, Space Operat Dept, Boulder, CO USA. [Phillips, Roger J.] Southwest Res Inst, Planetary Sci Directorate, Boulder, CO USA. RP Restano, M (reprint author), Univ Roma La Sapienza, Dipartimento DIET, Piazzale Aldo Moro 5, I-00185 Rome, Italy. EM marco.res@inwind.it FU ASI FX The Shallow Subsurface Radar (SHARAD) was provided by the Italian Space Agency (ASI), and its operations are led by the DIET Department, University of Rome "La Sapienza" under an ASI science contract. The Mars Reconnaissance Orbiter mission is managed by the Jet Propulsion Laboratory, California Institute of Technology, for the NASA Science Mission Directorate, Washington, DC. SHARAD data become available on the Geosciences Node of NASA's Planetary Data System (http://pds-geosciences.wustl.edu/) 6 months after the collection of the observations. NR 22 TC 9 Z9 9 U1 0 U2 9 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 JUN 28 PY 2015 VL 42 IS 12 BP 4663 EP 4669 DI 10.1002/2015GL064150 PG 7 WC Geosciences, Multidisciplinary SC Geology GA CM9CB UT WOS:000358002500001 ER PT J AU Bass, H AF Bass, Holly TI BASQUIAT AND THE BAYOU SO NEW YORK TIMES BOOK REVIEW LA English DT Book Review C1 [Bass, Holly] Kennedy Ctr, Washington, DC 20566 USA. [Bass, Holly] Smithsonian Inst, Washington, DC 20560 USA. RP Bass, H (reprint author), Kennedy Ctr, Washington, DC 20566 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU NEW YORK TIMES PI NEW YORK PA 620 8TH AVE, NEW YORK, NY 10018 USA SN 0028-7806 J9 NY TIMES BK REV JI N. Y. Times Book Rev. PD JUN 28 PY 2015 VL 120 IS 26 BP 27 EP 27 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CL3IC UT WOS:000356842600032 ER PT J AU Bass, H AF Bass, Holly TI JEAN-MICHEL BASQUIAT Now's the Time SO NEW YORK TIMES BOOK REVIEW LA English DT Book Review C1 [Bass, Holly] Kennedy Ctr, Washington, DC 20566 USA. [Bass, Holly] Smithsonian Inst, Washington, DC 20560 USA. RP Bass, H (reprint author), Kennedy Ctr, Washington, DC 20566 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU NEW YORK TIMES PI NEW YORK PA 620 8TH AVE, NEW YORK, NY 10018 USA SN 0028-7806 J9 NY TIMES BK REV JI N. Y. Times Book Rev. PD JUN 28 PY 2015 VL 120 IS 26 BP 27 EP 27 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CL3IC UT WOS:000356842600033 ER PT J AU Cacciali, P Scott, NJ AF Cacciali, Pier Scott, Norman J. TI Key to the Ophiodes (Squamata: Sauria: Diploglossidae) of Paraguay with the description of a new species SO ZOOTAXA LA English DT Article DE Ophiodes luciae sp nov.; Reptilia; South America; Worm Lizards ID REPRODUCTIVE-BIOLOGY; ANGUIDAE; BRAZIL AB Ophiodes is a South American genus of legless diploglossid lizards. Four species have been formally described: O. intermedius, O. vertebralis, O. striatus, and O. fragilis; three additional species were described but not officially named in an unpublished dissertation. These species are referred to as Ophiodes sp. "1", Ophiodes sp. "2", and Ophiodes sp. "3". We recognize five species of Ophiodes in Paraguay, one widespread (O. intermedius) and four known from only one or two localities (O. fragilis, O. striatus, O. sp. "3", and an undescribed species, described herein). The new species described represents the fifth Paraguayan species and the eighth member of the genus. It is distinguished by a combination of the following characters: a high number of middorsal scales between occipital and cloacal opening (>165), 29 scale rows around midbody, the posterior limbs 4 scales long, and vertical black bars on the face absent. C1 [Cacciali, Pier] Senckenberg Forschungsinst, D-60325 Frankfurt, Germany. [Cacciali, Pier] Natl Museum, D-60325 Frankfurt, Germany. [Cacciali, Pier] Inst Invest Biol Paraguay, Asuncion, Paraguay. [Scott, Norman J.] Smithsonian Inst, Museum Southwestern Biol, Creston, CA 93432 USA. [Scott, Norman J.] Los Angeles Cty Museum, Creston, CA 93432 USA. RP Cacciali, P (reprint author), Senckenberg Forschungsinst, Senckenberganlage 25, D-60325 Frankfurt, Germany. EM pier_cacciali@yahoo.com FU Consejo Nacional de Ciencia y Tecnologia (CONACYT-Paraguay) through the program PRONII FX We are grateful to the following curators, collections managers, and institutions for permission to examine specimens under their care: C. Meyers (American Museum of Natural History, New York, U.S.A; AMNH), C. McCarthy and B. Clarke (Natural History Museum, London, England, NHMUK), J. Cabot-Nieves and J. M. Carmona (Estacion Biologica de Donana, Seville, Spain, EBD), D. Kizirian and N. Camacho (Los Angeles County Museum, Los Angeles, U.S.A, LACM), M. Motte (Museo Nacional de Historia Natural del Paraguay, San Lorenzo, Paraguay, MNHNP), T. Giermakowski (Museum of Southwestern Biology, University of New Mexico (Albuquerque, U.S.A., MSB), E. Gavetti and N. Franzese (Museo di Zoologia della Universita di Torino, Turin, Italy, MZUT), A. Kluge (Museum of Zoology, University of Michigan, Ann Arbor, U.S.A., UMMZ), and R. McDiarmid and S. Gotte (National Museum of Natural History, Smithsonian Institution, Washington, D.C., U.S.A., USNM). We thank S. Carreira for bibliographic material and Nicolas Martinez for photographs of MNHNP specimens. Also to anonymous reviewers who provide valuable comments that improved the manuscript. PC acknowledge Consejo Nacional de Ciencia y Tecnologia (CONACYT-Paraguay) through the program PRONII for financial support. NR 21 TC 0 Z9 0 U1 0 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 JUN 26 PY 2015 VL 3980 IS 1 BP 42 EP 50 PG 9 WC Zoology SC Zoology GA CL5BP UT WOS:000356975100002 PM 26249937 ER PT J AU O'Shea, M Sanchez, C Kathriner, A Mecke, S Lopes Carvalho, V Varela Ribeiro, A Afranio Soares, Z Lemos De Araujo, L Kaiser, H AF O'Shea, Mark Sanchez, Caitlin Kathriner, Andrew Mecke, Sven Lopes Carvalho, Venancio Varela Ribeiro, Agivedo Afranio Soares, Zito Lemos De Araujo, Luis Kaiser, Hinrich TI Herpetological Diversity of Timor-Leste: Updates and a Review of Species Distributions SO ASIAN HERPETOLOGICAL RESEARCH LA English DT Article DE Timor-Leste; Kaloula; Cyrtodactylus; Eremiascincus; Stegonotus ID 1860 SQUAMATA GEKKONIDAE; 1ST REPORT; HEMIPHYLLODACTYLUS BLEEKER; PYTHON-RETICULATUS; MITOCHONDRIAL-DNA; MARINE SNAKES; BROOKII GRAY; BIBRON 1839; REPTILIA; SCINCIDAE AB We report the results of five herpetological surveys during 2011-2013 that included visits to all districts of Timor-Leste (Aileu, Ainaro, Baucau, Bobonaro, Dili, Covalima, Ermera, Lautem, Liquica, Manatuto, Manufahi, Viqueque) except the Oecusse exclave. Our fieldwork culminated in the discovery of one putative new frog species (genus Kaloula), at least five putative new lizard species (genera Cyrtodactylus, Cryptoblepharus, and Sphenomorphus), and two putative new snake species (genera Stegonotus and Indotyphlops). In addition, we present new distribution records of amphibians and reptiles for 11 of the country's 12 contiguous districts, along with additional natural history data. Results from our surveys increase the number of amphibian and reptiles known to occur in Timor-Leste from 22 species before our surveys began to over 60, including over 20 as yet undescribed species. C1 [O'Shea, Mark] Wolverhampton Univ, Fac Sci & Engn, Wolverhampton WV1 1LY, W Midlands, England. [O'Shea, Mark] West Midland Safari Pk, Bewdley DY12 LF, Worcs, England. [Sanchez, Caitlin; Kaiser, Hinrich] Victor Valley Coll, Dept Biol, Victorville, CA 92395 USA. [Kathriner, Andrew] Villanova Univ, Dept Biol, Villanova, PA 19085 USA. [Mecke, Sven] Univ Marburg, Dept Anim Evolut & Systemat, Fac Biol, D-35032 Marburg, Germany. [Kaiser, Hinrich] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Kaiser, H (reprint author), Victor Valley Coll, Victorville, CA 92395 USA. EM hinrich.kaiser@vvc.edu FU Title V Grant; Associated Student Body at Victor Valley College FX Our foremost thanks are for the unwavering, personal support we have received from Their Excellencies Xanana Gusmao, current Prime Minister and former President of Timor-Leste, and Jose Ramos-Horta, former President and former Prime Minister of Timor-Leste. Their interest in the survey work, in the educational opportunities this brings to Timorese citizens, and the welfare of wildlife in the country is deeply rooted in their understanding of nation-building and very gratifying for a team of scientists. This gratitude extends further, especially to Claudia AbateDebat, former Senior Advisor in the Prime Minister's Office, for her tireless efforts to allow us to meet the right people and for helping us comport ourselves with aplomb during important meetings, and to Manuel Mendes, Director of National Parks, for issuing the necessary permits and for his dedication to the conservation of Timor-Leste. Special thanks go to Damien Kingsbury, for his assistance with any matters requiring an historical or political perspective. We received able assistance in the field during Phases IV-VIII from Zach Brown, Kevin Burns, Melissa Carillo, Marissa Cox, Britta Doring, Joanna Flores, Scott Heacox, Stephanie Hughes, Naveen Jalota, Paul Landry, Aaren Marsh, Gloria Morales, Kyle Olsen, Jay Paris, Julia Pozo, Justin Rader, Claudia Rivas, Robert SeWell, David Taylor, and Franziska Wagner. Without them, many specimen records would have been missed. For their assistance with the logistics of travel we thank Paulo Aniceto (Rentlo Car Rental), Faridah Suhaimi (Air Timor), Gareth Turner (Air Timor), Ed Turner (Air Timor), Ian Groucott (Emirates), as well as the staff at Timor Lodge Hotel, particularly Kemal, Michelle, and Sheemon. A survey such as this requires an inordinate amount of specimen work covering many taxa in order to provide the most reliable identifications possible. We therefore gratefully acknowledge the assistance of the many individuals who were instrumental in facilitating loans, or permitting one or several of us to examine specimens under their care (for institutional abbreviations see Sabaj Perez, 2014): Jeremy Jacobs, Steve Gotte, Robert Wilson, Kenneth Tighe, George Zug, and Roy McDiarmid (USNM); Annemarie Ohler and Ivan Ineich (MNHN); Gunther Kohler and Linda Acker (SMF); Wolfgang Bohme and Andre Koch (ZFMK); Pim Arntzen, Ronald de Ruiter, and Esther Dondorp (RMNH); Patrick Campbell and Cohn McCarthy (BMNH); Jose Rosado, Joe Martinez, and James Hanken (MCZ); David Kizirian and David Dickey (AMNH); Karla Schneider (MLU); Rolf Beutel and Matthias Kruger (Phyletisches Museum, Jena, Germany); Fritz Geller-Grimm (MWNH); Raffael Winkler, Denis Vallan, and Urs Wuest (NHMB); Heinz Grillitsch, Silke Schweiger, and Georg Ga beta ner (NMW); Frank Tillack and Mark-Oliver Rodel (ZMB); Paul Doughty (WAM); Kelvin Lim (ZRC); Stefan Hertwig (NMBE); Raffael Ernst and Markus Auer (MTKD); Andreas Schmitz (MHNG); and Alexander Haas and Jakob Hallermann (ZMH). Financial assistance for equipment and supplies was partially provided by a Title V Grant to Victor Valley College. Partial financing of student travel was provided by the Associated Student Body at Victor Valley College, and by donations from Pamela MacKay and Melinda Fisher. This paper is Contribution No. 15 from the Tropical Research Initiative at Victor Valley College. NR 160 TC 4 Z9 4 U1 1 U2 5 PU SCIENCE PRESS PI BEIJING PA 16 DONGHUANGCHENGGEN NORTH ST, BEIJING 100717, PEOPLES R CHINA SN 2095-0357 J9 ASIAN HERPETOL RES JI Asian Herpetol. Res. PD JUN 25 PY 2015 VL 6 IS 2 BP 73 EP 131 PG 59 WC Zoology SC Zoology GA CM7AQ UT WOS:000357843200001 ER PT J AU Leray, M Meyer, CP Mills, SC AF Leray, Matthieu Meyer, Christopher P. Mills, Suzanne C. TI Metabarcoding dietary analysis of coral dwelling predatory fish demonstrates the minor contribution of coral mutualists to their highly partitioned, generalist diet SO PEERJ LA English DT Article DE Coral reefs; Food web; Interactions; Invertebrates; Mutualism; Exosymbionts; Pyrosequencing; COI ID FEEDING BUTTERFLYFISHES CHAETODONTIDAE; GREAT-BARRIER-REEF; MICROHABITAT UTILIZATION; HABITAT SPECIALIZATION; SECONDARY PREDATION; SPECIES-DIVERSITY; CLIMATE-CHANGE; INDO-PACIFIC; HOST CORALS; COMMUNITY AB Understanding the role of predators in food webs can be challenging in highly diverse predator/prey systems composed of small cryptic species. DNA based dietary analysis can supplement predator removal experiments and provide high resolution for prey identification. Here we use a metabarcoding approach to provide initial insights into the diet and functional role of coral-dwelling predatory fish feeding on small invertebrates. Fish were collected in Moorea (French Polynesia) where the BIOCODE project has generated DNA barcodes for numerous coral associated invertebrate species. Pyrosequencing data revealed a total of 292 Operational Taxonomic Units (OTU) in the gut contents of the arc-eye hawkfish (Paracirrhites arcatus), the flame hawkfish (Neocirrhites armatus) and the coral croucher (Caracanthus maculatus). One hundred forty-nine (51%) of them had species-level matches in reference libraries (>98% similarity) while 76 additional OTUs (26%) could be identified to higher taxonomic levels. Decapods that have a mutualistic relationship with Pocillopora and are typically dominant among coral branches, represent a minor contribution of the predators' diets. Instead, predators mainly consumed transient species including pelagic taxa such as copepods, chaetognaths and siphonophores suggesting non random feeding behavior. We also identified prey species known to have direct negative interactions with stony corals, such as Hapalocarcinus sp, a gall crab considered a coral parasite, as well as species of vermetid snails known for their deleterious effects on coral growth. Pocillopora DNA accounted for 20.8% and 20.1% of total number of sequences in the guts of the flame hawkfish and coral croucher but it was not detected in the guts of the arc-eye hawkfish. Comparison of diets among the three fishes demonstrates remarkable partitioning with nearly 80% of prey items consumed by only one predator. Overall, the taxonomic resolution provided by the metabarcoding approach highlights a highly complex interaction web and demonstrates that levels of trophic partitioning among coral reef fishes have likely been underestimated. Therefore, we strongly encourage further empirical approaches to dietary studies prior to making assumptions of trophic equivalency in food web reconstruction. C1 [Leray, Matthieu; Mills, Suzanne C.] CBETM Univ Perpignan, USR CRIOBE CNRS EPHE UPVD 3278, Perpignan, France. [Leray, Matthieu; Mills, Suzanne C.] Smithsonian Inst, Lab Excellence CORAIL, Washington, DC 20560 USA. [Leray, Matthieu; Meyer, Christopher P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Leray, M (reprint author), CBETM Univ Perpignan, USR CRIOBE CNRS EPHE UPVD 3278, Perpignan, France. EM leray.upmc@gmail.com RI Mills, Suzanne/K-5538-2012 FU Gordon and Betty Moore Foundation; France American Cultural Exchange program (FACE)/Partner University Fund (PUF); Smithsonian Institution fellowship program; Agence National de Recherche [ANR-11-JSV7-012-01] FX Funding was provided by the Gordon and Betty Moore Foundation, France American Cultural Exchange program (FACE)/Partner University Fund (PUF), the Smithsonian Institution fellowship program and the Agence National de Recherche, ANR-11-JSV7-012-01 Live and Let Die. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 89 TC 8 Z9 9 U1 12 U2 58 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD JUN 25 PY 2015 VL 3 AR e1047 DI 10.7717/peerj.1047 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL9TF UT WOS:000357320300004 PM 26137428 ER PT J AU Mendelson, JR Kinsey, CT Murphy, JB AF Mendelson, Joseph R., III Kinsey, Chase. T. Murphy, James. B. TI A review of the biology and literature of the Gulf Coast Toad (Incilius nebulifer), native to Mexico and the United States SO ZOOTAXA LA English DT Review DE Amphibia; Anura; Bufonidae; Inclius nebulifer; Gulf Coast Toad; Mexico; United States ID NORTH-AMERICAN TOADS; BUFO-VALLICEPS; GENUS BUFO; ANURAN AMPHIBIANS; SOUND PRODUCTION; BATRACHOCHYTRIUM-DENDROBATIDIS; DISTURBED ENVIRONMENT; REPRODUCTIVE ECOLOGY; BODY-TEMPERATURE; SEXUAL SELECTION AB The Gulf Coast Toad (Incilius nebulifer) is an abundant and widespread species within its range in the United States and Mexico, so it appears on many faunal checklists and is considered in diverse kinds of research. We review the basic biology, distribution, and published history of this species, identifying only those records and publications referable to I. nebulifer, to help researchers identify published works pertaining to I. nebulfer rather than I. valliceps, with which it formerly was considered to be conspecific. C1 [Mendelson, Joseph R., III] Zoo Atlanta, Atlanta, GA 30312 USA. [Mendelson, Joseph R., III] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Kinsey, Chase. T.] Auburn Univ, Sch Forestry & Wildlife, Auburn, AL 36849 USA. [Murphy, James. B.] Smithsonian Inst, Div Amphibians & Reptiles, Washington, DC 20013 USA. RP Mendelson, JR (reprint author), Zoo Atlanta, Atlanta, GA 30312 USA. EM jmendelson@zooatlanta.org NR 326 TC 0 Z9 0 U1 2 U2 8 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 JUN 24 PY 2015 VL 3974 IS 4 BP 517 EP 537 DI 10.11646/zootaxa.3974.4.4 PG 21 WC Zoology SC Zoology GA CL3BF UT WOS:000356823000004 PM 26249922 ER PT J AU Vazquez-Rodriguez, AI Hansel, CM Zhang, T Lamborg, CH Santelli, CM Webb, SM Brooks, SC AF Vazquez-Rodriguez, Adiari I. Hansel, Colleen M. Zhang, Tong Lamborg, Carl H. Santelli, Cara M. Webb, Samuel M. Brooks, Scott C. TI Microbial- and thiosulfate-mediated dissolution of mercury sulfide minerals and transformation to gaseous mercury SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE mercury; metacinnabar; sulfur chemosynthesis; Thiobacillus; thiosulfate; mercury sulfide dissolution; sulfur metabolism; sulfur oxidation ID BACTERIAL COMMUNITY STRUCTURE; DISSOLVED ORGANIC-MATTER; METACINNABAR BETA-HGS; OXIDATIVE DISSOLUTION; HYDROTHERMAL VENTS; SULFUR CYCLE; DIVERSITY; THIOBACILLUS; MOBILIZATION; REDUCTION AB Mercury (Hg) is a toxic heavy metal that poses significant environmental and human health risks. Soils and sediments, where Hg can exist as the Hg sulfide mineral metacinnabar (beta-HgS), represent major Hg reservoirs in aquatic environments. Metacinnabar has historically been considered a sink for Hg in all but severely acidic environments, and thus disregarded as a potential source of Hg back to aqueous or gaseous pools. Here, we conducted a combination of field and laboratory incubations to identify the potential for metacinnabar as a source of dissolved Hg within near neutral pH environments and the underpinning (a)biotic mechanisms at play. We show that the abundant and widespread sulfur-oxidizing bacteria of the genus Thiobacillus extensively colonized metacinnabar chips incubated within aerobic, near neutral pH creek sediments. Laboratory incubations of axenic Thiobacillus thioparus cultures led to the release of metacinnabar-hosted Hg(II) and subsequent volatilization to Hg(0). This dissolution and volatilization was greatly enhanced in the presence of thiosulfate, which served a dual role by enhancing HgS dissolution through Hg complexation and providing an additional metabolic substrate for Thiobacillus. These findings reveal a new coupled abiotic-biotic pathway for the transformation of metacinnabar-bound Hg(II) to Hg(0), while expanding the sulfide substrates available for neutrophilic chemosynthetic bacteria to Hg-laden sulfides. They also point to mineral-hosted Hg as an underappreciated source of gaseous elemental Hg to the environment. C1 [Vazquez-Rodriguez, Adiari I.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Hansel, Colleen M.; Zhang, Tong; Lamborg, Carl H.] Woods Hole Oceanog Inst, Dept Marine Chem & Geochem, Woods Hole, MA 02543 USA. [Santelli, Cara M.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Webb, Samuel M.] Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA USA. [Brooks, Scott C.] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN USA. RP Hansel, CM (reprint author), Woods Hole Oceanog Inst, 266 Woods Hole Rd,Mailstop 52, Woods Hole, MA 02543 USA. EM chansel@whoi.edu RI Brooks, Scott/B-9439-2012; Webb, Samuel/D-4778-2009; OI Brooks, Scott/0000-0002-8437-9788; Webb, Samuel/0000-0003-1188-0464; Santelli, Cara/0000-0001-8617-0008 FU National Science Foundation Graduate Research Fellowship [DGE-0644491]; U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-76SF00515] FX This work was supported by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-0644491 awarded to AV. The authors thank R. Perdigato-Henriques and W. D. Leavitt for assistance in processing field samples; C. S. Kim, C. J. Lentini, and J. P. Shine for helpful conversations regarding this study; G. Swarr for assistance with Tekran operation; and N. Lupoli and Z. Dong for assistance with the DMA-80.; Part of this research was conducted at the Stanford Synchrotron Radiation Lightsource. Use of the Stanford Synchrotron Radiation Lightsource, SLAC National Accelerator Laboratory, is supported by the U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences under Contract No. DE-AC02-76SF00515. NR 44 TC 0 Z9 0 U1 10 U2 35 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD JUN 23 PY 2015 VL 6 AR 596 DI 10.3389/fmicb.2015.00596 PG 11 WC Microbiology SC Microbiology GA CL7DP UT WOS:000357131600001 PM 26157421 ER PT J AU Sellers, AJ Ruiz, GM Leung, B Torchin, ME AF Sellers, Andrew J. Ruiz, Gregory M. Leung, Brian Torchin, Mark E. TI Regional Variation in Parasite Species Richness and Abundance in the Introduced Range of the Invasive Lionfish, Pterois volitans SO PLOS ONE LA English DT Article ID BIOTIC RESISTANCE; SPATIAL VARIATION; MARINE INVASIONS; GNATHIID ISOPOD; PLANT INVASIONS; UNITED-STATES; FISH; DYNAMICS; SCORPAENIDAE; COMMUNITIES AB Parasites can play an important role in biological invasions. While introduced species often lose parasites from their native range, they can also accumulate novel parasites in their new range. The accumulation of parasites by introduced species likely varies spatially, and more parasites may shift to new hosts where parasite diversity is high. Considering that parasitism and disease are generally more prevalent at lower latitudes, the accumulation of parasites by introduced hosts may be greater in tropical regions. The Indo-Pacific lionfish (Pterois volitans) has become widely distributed across the Western Atlantic. In this study, we compared parasitism across thirteen locations in four regions, spanning seventeen degrees of latitude in the lionfish's introduced range to examine potential spatial variation in parasitism. In addition, as an initial step to explore how indirect effects of parasitism might influence interactions between lionfish and ecologically similar native hosts, we also compared parasitism in lionfish and two co-occurring native fish species, the graysby grouper, Cephalopholis cruentata, and the lizardfish, Synodus intermedius, in the southernmost region, Panama. Our results show that accumulation of native parasites on lionfish varies across broad spatial scales, and that colonization by ectoparasites was highest in Panama, relative to the other study sites. Endoparasite richness and abundance, on the other hand, were highest in Belize where lionfish were infected by twice as many endoparasite species as lionfish in other regions. The prevalence of all but two parasite species infecting lionfish was below 25%, and we did not detect an association between parasite abundance and host condition, suggesting a limited direct effect of parasites on lionfish, even where parasitism was highest. Further, parasite species richness and abundance were significantly higher in both native fishes compared to lionfish, and parasite abundance was negatively associated with the condition index of the native grouper but not that of the lionfish or lizardfish. While two co-occurring native fishes were more heavily parasitized compared to lionfish in Panama any indirect benefits of differential parasitism requires further investigation. Future parasitological surveys of lionfish across the eastern coast of North America and the Lesser Antilles would further resolve geographic patterns of parasitism in invasive lionfish. C1 [Sellers, Andrew J.; Torchin, Mark E.] Smithsonian Trop Res Inst, Panama City, Panama. [Sellers, Andrew J.; Leung, Brian] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Sellers, AJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM sellersa@si.edu OI Ruiz, Gregory/0000-0003-2499-441X FU Smithsonian Institution's Marine Science Network Grant; McGill University's Biology Department and Neotropical Environments Option (NEO) Program; Panama's Secretaria Nacional de Ciencia y Tecnologia (SENACYT) FX This work was funded in part by a Smithsonian Institution's Marine Science Network Grant awarded to GM Ruiz and ME Torchin; and graduate research grants awarded to AJ Sellers by McGill University's Biology Department and Neotropical Environments Option (NEO) Program. AJ Sellers was awarded a graduate scholarship by Panama's Secretaria Nacional de Ciencia y Tecnologia (SENACYT). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 50 TC 4 Z9 4 U1 4 U2 37 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 JUN 22 PY 2015 VL 10 IS 6 AR e0131075 DI 10.1371/journal.pone.0131075 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL3FM UT WOS:000356835800143 PM 26098309 ER PT J AU Wagner, D Opresko, DM AF Wagner, Daniel Opresko, Dennis M. TI Description of a new species of Leiopathes (Antipatharia: Leiopathidae) from the Hawaiian Islands SO ZOOTAXA LA English DT Article DE Anthozoa; black coral; biogeography; cold-water coral; deep-sea; Leiopathes annosa sp nov. ID DEEP-WATER ANTIPATHARIANS; NORTH-ATLANTIC; SEA CORALS; BIODIVERSITY; SEAMOUNTS; HABITAT; BIOLOGY; SITES; OCEAN; BANK AB The Hawaiian antipatharian coral previously identified as Leiopathes glaberrima (Esper, 1792) and Leiopathes sp. is described using polyp morphology, skeletal spine morphology and in situ photographs, and assigned the new name of Leiopathes annosa sp. nov. The species is characterized by tall (1 m or more), fan-shaped colonies, with thick, sometimes overlapping branches, and tissues that are colored bright orange when alive. Skeletal spines are smooth, hemispherical, often times multi-lobed, and typically 75 mu m tall, but range between 30-225 mu m. Polyps are of variable size (0.88-3.35 mm) and arranged on all sides of the corallum on thicker branches, and uniserially on terminal branches. Leiopathes annosa sp. nov differs from all other nominal species of Leiopathes by having a generally flabellate corallum with thick branches and conspicuous skeletal spines that are multi-lobed and hemispherical. The biogeographical distribution of species within the monogeneric family Leiopathidae is presented and discussed. C1 [Wagner, Daniel] NOAA, Papahanaumokuakea Marine Natl Monument, Honolulu, HI 96822 USA. [Opresko, Dennis M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC USA. RP Wagner, D (reprint author), NOAA, Papahanaumokuakea Marine Natl Monument, Honolulu, HI 96822 USA. EM Daniel.Wagner@noaa.gov; dmopresko@hotmail.com FU NOAA's Deep-Sea Coral Research and Technology Program; NOAA's Office of National Marine Sanctuaries through the Papahanaumokuakea Marine National Monument FX Special thanks to Chris Kelley for collecting the holotype of L. annosa sp. nov., and to Mercer Brugler and two anonymous reviewers for providing insightful comments on an earlier version of this manuscript. We thank Stephen Cairns, Cheryl Bright, Geoff Keel and Bill Moser for help in accessing material at the USNM, and Holly Bolick for facilitating work with the BPBM collections. Additional thanks to Scott Whittacker and Tina Carvalho for providing assistance in performing the SEM analyses, to Chris Kelley and Deetsie Chave for extracting records from the HURL archives, and to Dan Luck for help in compiling the biogeographic records. This work was funded in part by NOAA's Deep-Sea Coral Research and Technology Program and by NOAA's Office of National Marine Sanctuaries through the Papahanaumokuakea Marine National Monument. The scientific results and conclusions, as well as any views or opinions expressed herein, are those of the authors and do not necessarily reflect the views of NOAA or the Department of Commerce. NR 56 TC 0 Z9 0 U1 1 U2 8 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 JUN 22 PY 2015 VL 3974 IS 2 BP 277 EP 289 PG 13 WC Zoology SC Zoology GA CL2ZO UT WOS:000356817800011 PM 26249904 ER PT J AU Wayth, RB Lenc, E Bell, ME Callingham, JR Dwarakanath, KS Franzen, TMO For, BQ Gaensler, B Hancock, P Hindson, L Hurley-Walker, N Jackson, CA Johnston-Hollitt, M Kapinska, AD McKinley, B Morgan, J Offringa, AR Procopio, P Staveley-Smith, L Wu, C Zheng, Q Trott, CM Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, A Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF Wayth, R. B. Lenc, E. Bell, M. E. Callingham, J. R. Dwarakanath, K. S. Franzen, T. M. O. For, B. -Q. Gaensler, B. Hancock, P. Hindson, L. Hurley-Walker, N. Jackson, C. A. Johnston-Hollitt, M. Kapinska, A. D. McKinley, B. Morgan, J. Offringa, A. R. Procopio, P. Staveley-Smith, L. Wu, C. Zheng, Q. Trott, C. M. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Kaplan, D. L. Kasper, J. C. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Rogers, A. E. E. Roshi, A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Tingay, S. J. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI GLEAM: The GaLactic and Extragalactic All-Sky MWA Survey SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE Galaxy: general; radio continuum: general; radio lines: general; surveys ID MURCHISON WIDEFIELD ARRAY; RADIO IMAGING SURVEY; WIDE-FIELD; SOUTHERN SKY; NEXT-GENERATION; SOURCE CATALOG; TELESCOPE; LOFAR; COSMOLOGY; IMAGER AB GLEAM, the GaLactic and Extragalactic All-sky MWA survey, is a survey of the entire radio sky south of declination +25 degrees at frequencies between 72 and 231 MHz, made with the MWA using a drift scan method that makes efficient use of the MWA's very large field-of-view. We present the observation details, imaging strategies, and theoretical sensitivity for GLEAM. The survey ran for two years, the first year using 40-kHz frequency resolution and 0.5-s time resolution; the second year using 10-kHz frequency resolution and 2 s time resolution. The resulting image resolution and sensitivity depends on observing frequency, sky pointing, and image weighting scheme. At 154 MHz, the image resolution is approximately 2.5 x 2.2/cos(delta + 26.7 degrees) arcmin with sensitivity to structures up to similar to 10 degrees in angular size. We provide tables to calculate the expected thermal noise for GLEAM mosaics depending on pointing and frequency and discuss limitations to achieving theoretical noise in Stokes I images. We discuss challenges, and their solutions, that arise for GLEAM including ionospheric effects on source positions and linearly polarised emission, and the instrumental polarisation effects inherent to the MWA's primary beam. C1 [Wayth, R. B.; Franzen, T. M. O.; Hancock, P.; Hurley-Walker, N.; Jackson, C. A.; Morgan, J.; Trott, C. M.; Emrich, D.; Lynch, M. J.; Ord, S. M.; Tingay, S. J.; Waterson, M.; Williams, A.] Curtin Univ, ICRAR, Bentley, WA 6102, Australia. [Wayth, R. B.; Lenc, E.; Bell, M. E.; Callingham, J. R.; Gaensler, B.; Hancock, P.; Jackson, C. A.; Kapinska, A. D.; McKinley, B.; Procopio, P.; Staveley-Smith, L.; Trott, C. M.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Webster, R. L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Lenc, E.; Callingham, J. R.] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia. [Bell, M. E.; Callingham, J. R.; Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Marsfield, NSW 2122, Australia. [Dwarakanath, K. S.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [For, B. -Q.; Kapinska, A. D.; Staveley-Smith, L.; Wu, C.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Gaensler, B.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Hindson, L.; Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [McKinley, B.; Procopio, P.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Offringa, A. R.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Bernardi, G.] SKA SA, ZA-7405 Pinelands, South Africa. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Cappallo, R. J.; Corey, B. E.; McWhirter, S. R.; Rogers, A. E. E.] MIT, Haystack Observ, Westford, MA 01886 USA. [Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hazelton, B. J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, A.] Natl Radio Astron Observ, Green Bank, WV USA. RP Wayth, RB (reprint author), Curtin Univ, ICRAR, Bentley, WA 6102, Australia. EM r.wayth@curtin.edu.au RI Kapinska, Anna/B-3999-2014; Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Dwarakanath, K /D-4876-2012; Staveley-Smith, Lister/A-1683-2011; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012 OI Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593; Callingham, Joseph/0000-0002-7167-1819; Hancock, Paul/0000-0002-4203-2946; Kapinska, Anna/0000-0002-5289-5729; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Staveley-Smith, Lister/0000-0002-8057-0294; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; FU US National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council [LE0775621, LE0882938]; US Air Force Office of Scientific Research [FA9550-0510247]; Centre for All-sky Astrophysics [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington from New Zealand Ministry of Economic Development and an IBM Shared University Research Grant [MED-E1799]; Australian Federal government via Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; Australian Government; Government of Western Australia; Western Australian State government; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University; University of Western Australia 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 MWA comes from the US National Science Foundation (grants AST-0457585, PHY-0835713, CAREER-0847753, and AST-0908884), the Australian Research Council (LIEF grants LE0775621 and LE0882938), the US Air Force Office of Scientific Research (grant FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by grant CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via grant MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. This work was supported by resources provided by the Pawsey Supercomputing Centre with funding from the Australian Government and the Government of Western Australia. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing, and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University, and The University of Western Australia, funded by the Western Australian State government. NR 50 TC 9 Z9 9 U1 1 U2 9 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 JUN 22 PY 2015 VL 32 AR e0251 DI 10.1017/pasa.2015.26 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2VH UT WOS:000356803800001 ER PT J AU Reilly, NJ Changala, PB Baraban, JH Kokkin, DL Stanton, JF McCarthy, MC AF Reilly, Neil J. Changala, P. Bryan Baraban, Joshua H. Kokkin, Damian L. Stanton, John F. McCarthy, Michael C. TI Communication: The ground electronic state of Si2C: Rovibrational level structure, quantum monodromy, and astrophysical implications SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID INDUCED-FLUORESCENCE SPECTROSCOPY; CHEMICAL-VAPOR-DEPOSITION; JET-COOLED SIC2; SILICON-CARBIDE; CARBON STARS; DISILICON CARBIDE; VIOLET OPACITY; LINE SURVEY; SPECTRUM; IRC+10216 AB We report the gas-phase optical detection of Si2C near 390 nm and the first experimental investigation of the rovibrational structure of its (1)A(1) ground electronic state using mass-resolved and fluorescence spectroscopy and variational calculations performed on a high-level ab initio potential. From this joint study, it is possible to assign all observed K-a = 1 vibrational levels up to 3800 cm(-1) with confidence, as well as a number of levels in the K-a = 0, 2, and 3 manifolds. Dixon-dip plots for the bending coordinate (nu(2)) allow an experimental determination of a barrier to linearity of 783(48) cm(-1) (2 sigma), in good agreement with theory (802(9) cm(-1)). The calculated (K-a, nu(2)) eigenvalue lattice shows an archetypal example of quantum monodromy (absence of a globally valid set of quantum numbers) that is reflected by the experimentally observed rovibrational levels. The present study provides a solid foundation for infrared and optical surveys of Si2C in astronomical objects, particularly in the photosphere of N- and J-type carbon stars where the isovalent SiC2 molecule is known to be abundant. (C) 2015 AIP Publishing LLC. C1 [Reilly, Neil J.; Kokkin, Damian L.; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Changala, P. Bryan] Univ Colorado, Natl Inst Stand & Technol, JILA, Boulder, CO 80309 USA. [Changala, P. Bryan] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Baraban, Joshua H.] Univ Colorado, Dept Chem, Boulder, CO 80309 USA. [Stanton, John F.] Univ Texas Austin, Dept Chem, Austin, TX 78712 USA. RP Reilly, NJ (reprint author), Marquette Univ, Dept Chem, Milwaukee, WI 53233 USA. FU NASA [NNX13AE59G]; NSF [DGE1144083]; Welch Foundation of Houston, Texas [F-1283]; US National Science Foundation [CHE-1361031] FX The work in Cambridge is supported by NASA Grant No. NNX13AE59G. P.B.C. is supported by a NSF Graduate Research Fellowship (Award No. DGE1144083). J.F.S. would like to thank the Welch Foundation of Houston, Texas (Grant No. F-1283) and the US National Science Foundation (Grant No. CHE-1361031). NR 68 TC 2 Z9 2 U1 0 U2 23 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 JUN 21 PY 2015 VL 142 IS 23 AR 231101 DI 10.1063/1.4922651 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CL0HU UT WOS:000356623000001 PM 26093543 ER PT J AU Esposito, P Israel, GL de Martino, D D'Avanzo, P Testa, V Sidoli, L Di Stefano, R Belfiore, A Mapelli, M Piranomonte, S Castillo, GAR Moretti, A D'Elia, V Verrecchia, F Campana, S Rea, N AF Esposito, P. Israel, G. L. de Martino, D. D'Avanzo, P. Testa, V. Sidoli, L. Di Stefano, R. Belfiore, A. Mapelli, M. Piranomonte, S. Castillo, G. A. Rodriguez Moretti, A. D'Elia, V. Verrecchia, F. Campana, S. Rea, N. TI Swift J201424.9+152930: discovery of a new deeply eclipsing binary with 491-s and 3.4-h modulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE novae, cataclysmic variables; white dwarfs; X-rays: binaries; X-rays: individual: Swift J201424.9+152930 ID X-RAY BINARIES; PHOTON IMAGING CAMERA; CATACLYSMIC VARIABLES; INTERMEDIATE POLAR; XMM-NEWTON; ULTRAVIOLET/OPTICAL TELESCOPE; DONOR STARS; WHITE-DWARF; EX-HYDRAE; CALIBRATION AB We report on the discovery of a new X-ray pulsator, Swift J201424.9+152930 (Sw J2014). Owing to its X-ray modulation at 491 s, it was discovered in a systematic search for coherent signals in the archival data of the Swift X-ray Telescope. To investigate the nature of Sw J2014, we performed multiwavelength follow-up observations with space-borne (Swift and XMM-Newton) and ground-based (the 1.5-m Loiano Telescope and the 3.6-m Telescopio Nazionale Galileo) instruments. The X-ray spectrum of Sw J2014 can be described by a hard and highly absorbed (N-H similar to 5 x 10(22) cm(-2)) power law (Gamma similar to 1). The optical observations made it possible to single out the optical counterpart to this source, which displays several variable emission lines and total eclipses lasting approximate to 20 min. Total eclipses of similar length were observed also in X-rays. The study of the eclipses, allowed us to infer a second periodicity of 3.44 h, which we interpret as the orbital period of a close binary system. We also found that the period has not significantly changed over a similar to 7 yr timespan. Based on the timing signatures of Sw J2014, and its optical and X-ray spectral properties, we suggest that it is a close binary hosting an accreting magnetic white dwarf. The system is therefore a cataclysmic variable of the intermediate polar type and one of the very few showing deep eclipses. C1 [Esposito, P.; Sidoli, L.; Belfiore, A.] INAF, Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy. [Esposito, P.; Di Stefano, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Israel, G. L.; Testa, V.; Piranomonte, S.; Castillo, G. A. Rodriguez; D'Elia, V.; Verrecchia, F.] INAF, Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [de Martino, D.] INAF, Osservatorio Astron Capodimonte, I-80131 Naples, Italy. [D'Avanzo, P.; Campana, S.] INAF, Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Mapelli, M.] INAF, Osservatorio Astron Padova, I-35122 Padua, Italy. [Moretti, A.] INAF, Osservatorio Astron Brera, I-20121 Milan, Italy. [D'Elia, V.; Verrecchia, F.] ASI Sci Data Ctr ASDC, I-00133 Rome, Italy. [Rea, N.] Univ Amsterdam, Anton Pannekoek Inst, NL-1090 GE Amsterdam, Netherlands. [Rea, N.] Inst Ciencies Espai CSIC IEEC, Fac Ciencies, E-08193 Barcelona, Spain. RP Esposito, P (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm Milano, Via E Bassini 15, I-20133 Milan, Italy. EM paoloesp@iasf-milano.inaf.it RI Rea, Nanda/I-2853-2015; OI de Martino, Domitilla/0000-0002-5069-4202; Esposito, Paolo/0000-0003-4849-5092; Rea, Nanda/0000-0003-2177-6388; Campana, Sergio/0000-0001-6278-1576; Piranomonte, Silvia/0000-0002-8875-5453; Verrecchia, Francesco/0000-0003-3455-5082; Mapelli, Michela/0000-0001-8799-2548; moretti, alberto/0000-0002-9770-0315; Rodriguez Castillo, Guillermo Andres/0000-0003-3952-7291; Israel, GianLuca/0000-0001-5480-6438; Sidoli, Lara/0000-0001-9705-2883; D'Elia, Valerio/0000-0002-7320-5862 FU ESA Member States; NASA; Fulbright Research Scholar grant; US Department of State; Italian Ministry of Education, University and Research (MIUR) [FIRB 2012 RBFR12PM1F]; INAF [PRIN-2011-1]; ASI/INAF [I/004/11/0, I/037/12/0]; SAO/CXC [GO3-14093X]; NSF [AST-1211843]; NASA [NNX12AE39G] FX This research is based on observations obtained with Swift and XMM-Newton. Swift is a NASA mission with participation of the Italian Space Agency and the UK Space Agency. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. We also made use of observations collected at the Astronomical Observatory of Bologna in Loiano and of TNG operated on the island of La Palma by the Fundacion Galileo Galilei of the INAF. The IRAF software package is distributed by the NOAO, which is operated by AURA, Inc., under cooperative agreement with the NSF. We thank the anonymous referee for valuable comments on the manuscript and constructive suggestions. PE acknowledges a Fulbright Research Scholar grant administered by the US - Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. (The Fulbright Scholar Program is sponsored by the US Department of State and administered by CIES, a division of IIE.) MM acknowledges financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F, and from INAF through grant PRIN-2011-1. This work was partially supported by the following contracts and grants: ASI/INAF I/004/11/0 and I/037/12/0, SAO/CXC GO3-14093X, NSF AST-1211843, and NASA NNX12AE39G. NR 63 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 JUN 21 PY 2015 VL 450 IS 2 BP 1705 EP 1715 DI 10.1093/mnras/stv724 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500043 ER PT J AU Kolokythas, K O'Sullivan, E Giacintucci, S Raychaudhury, S Ishwara-Chandra, CH Worrall, DM Birkinshaw, M AF Kolokythas, Konstantinos O'Sullivan, Ewan Giacintucci, Simona Raychaudhury, Somak Ishwara-Chandra, C. H. Worrall, Diana M. Birkinshaw, Mark TI New insights into the evolution of the FR I radio galaxy 3C 270 (NGC 4261) from VLA and GMRT radio observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: groups: general; galaxies: individual: (3C 270, NGC 4261); galaxies: jets; radio continuum: galaxies ID DEEP CHANDRA OBSERVATION; ACTIVE-GALACTIC-NUCLEUS; X-RAY OBSERVATIONS; PARTICLE-ACCELERATION; MAGNETIC-FIELD; FLUX DENSITIES; CENTIMETER WAVELENGTHS; MULTIFREQUENCY RADIO; INTERGALACTIC MEDIUM; RELATIVISTIC JETS AB We present the Giant Metrewave Radio Telescope 240 MHz observations of the nearby luminous Fanaroff-Riley type I radio source 3C 270, in the group-central elliptical NGC 4261. Combining these data with reprocessed Very Large Array 1.55 and 4.8 GHz observations, we produce spectral-index maps that reveal a constant spectral index along the jets and a gradual steepening from the ends of the jets through the lobes towards the nucleus. A Jaffe & Perola (JP) model fitted to the integrated spectrum of the source gives an asymptotic low-frequency index of alpha(inj) = 0.53(-0.02)(+0.01), while JP models fitted to the observed spectral index trend along the lobes allow us to estimate radiative ages of similar to 29 and similar to 37 Myr for the west and east lobes, respectively. Our age estimates are a factor of 2 lower than the 75-Myr upper limit derived from X-ray data. We find unlikely the scenario of an early supersonic phase in which the lobe expanded into the ISM at approximately Mach 6 (3500 km s(-1)), and suggest that either the source underwent multiple active galactic nuclei outbursts with possible large changes in jet power, or possibly that the source age that we find is due to a backflow that transports young electrons from the jet tips through the lobes towards the nucleus relatively quickly. We calculate that in the lobes the energy ratio of non-radiating to radiating particles is similar to 4-24 indicating significant gas entrainment. If the lobes are in pressure balance with their surroundings, the total energy required to heat the entrained material is 10(58) erg, similar to 40 per cent of the total enthalpy of the lobes. C1 [Kolokythas, Konstantinos; O'Sullivan, Ewan; Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [O'Sullivan, Ewan; Worrall, Diana M.; Birkinshaw, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Raychaudhury, Somak] Presidency Univ, Dept Phys, Kolkata 700073, India. [Ishwara-Chandra, C. H.] TIFR, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Worrall, Diana M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. RP Kolokythas, K (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. EM kkolok@star.sr.bham.ac.uk; eosullivan@cfa.harvard.edu; somak@presiuniv.ac.in OI O'Sullivan, Ewan/0000-0002-5671-6900 FU University of Birmingham; National Aeronautics and Space Administration (NASA) [AR3-14014X, NAS8-03060]; Astrophysical Data Analysis programme [NNX13AE71G]; NASA through Einstein Postdoctoral Fellowship [PF0-110071]; Chandra X-ray Center; EU/FP7 Marie Curie award of the IRSES grant CAFEGROUPS [247653] FX KK is supported by the University of Birmingham. EO acknowledges support for this work from the National Aeronautics and Space Administration (NASA) through Chandra award number AR3-14014X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060, and through the Astrophysical Data Analysis programme, award NNX13AE71G. SG acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center, which is operated by the SAO. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. Some of this research was supported by the EU/FP7 Marie Curie award of the IRSES grant CAFEGROUPS (247653). We thank T. Ponman and Andreas Zezas for useful discussions of NGC 4261 and formation history. We would like to thank the anonymous referee for insightful comments which helped to enhance this work. NR 82 TC 1 Z9 1 U1 0 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 JUN 21 PY 2015 VL 450 IS 2 BP 1732 EP 1744 DI 10.1093/mnras/stv665 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500046 ER PT J AU Russell, TD Miller-Jones, JCA Curran, PA Soria, R Altamirano, D Corbel, S Coriat, M Moin, A Russell, DM Sivakoff, GR Slaven-Blair, TJ Belloni, TM Fender, RP Heinz, S Jonker, PG Krimm, HA Kording, EG Maitra, D Markoff, S Middleton, M Migliari, S Remillard, RA Rupen, MP Sarazin, CL Tetarenko, AJ Torres, MAP Tudose, V Tzioumis, AK AF Russell, T. D. Miller-Jones, J. C. A. Curran, P. A. Soria, R. Altamirano, D. Corbel, S. Coriat, M. Moin, A. Russell, D. M. Sivakoff, G. R. Slaven-Blair, T. J. Belloni, T. M. Fender, R. P. Heinz, S. Jonker, P. G. Krimm, H. A. Koerding, E. G. Maitra, D. Markoff, S. Middleton, M. Migliari, S. Remillard, R. A. Rupen, M. P. Sarazin, C. L. Tetarenko, A. J. Torres, M. A. P. Tudose, V. Tzioumis, A. K. TI Radio monitoring of the hard state jets in the 2011 outburst of MAXI J1836-194 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE proper motions; stars: individual: MAXI J1836; 194; ISM: jets and outflows; radio continuum: stars; X-rays: binaries ID BLACK-HOLE CANDIDATE; X-RAY BINARIES; VLBA CALIBRATOR SURVEY; SPECTRAL ENERGY-DISTRIBUTION; COMPACT OBJECT FORMATION; ACTIVE GALACTIC NUCLEUS; BROAD-BAND SPECTRUM; GX 339-4; RELATIVISTIC JETS; INTERNAL SHOCKS AB MAXI J1836-194 is a Galactic black hole candidate X-ray binary that was discovered in 2011 when it went into outburst. In this paper, we present the full radio monitoring of this system during its 'failed' outburst, in which the source did not complete a full set of state changes, only transitioning as far as the hard intermediate state. Observations with the Karl G. Jansky Very Large Array (VLA) and Australia Telescope Compact Array (ATCA) show that the jet properties changed significantly during the outburst. The VLA observations detected linearly polarized emission at a level of similar to 1 per cent early in the outburst, increasing to similar to 3 per cent as the outburst peaked. High-resolution images with the Very Long Baseline Array (VLBA) show an similar to 15 mas jet along the position angle -21 +/- 2 degrees, in agreement with the electric vector position angle found from our polarization results (-21 +/- 4 degrees), implying that the magnetic field is perpendicular to the jet. Astrometric observations suggest that the system required an asymmetric natal kick to explain its observed space velocity. Comparing quasisimultaneous X-ray monitoring with the 5 GHz VLA observations from the 2011 outburst shows an unusually steep hard-state radio/X-ray correlation of L-R alpha L-X(1.8 +/- 0.2), where L-R and LX denote the radio and X-ray luminosities, respectively. With ATCA and Swift monitoring of the source during a period of re-brightening in 2012, we show that the system lay on the same steep correlation. Due to the low inclination of this system, we then investigate the possibility that the observed correlation may have been steepened by variable Doppler boosting. C1 [Russell, T. D.; Miller-Jones, J. C. A.; Curran, P. A.; Soria, R.; Slaven-Blair, T. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Altamirano, D.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Corbel, S.] Univ Paris Diderot, CNRS INSU, Lab AIM CEA IRFU, CEA DSM IRFU SAp, F-91191 Gif Sur Yvette, France. [Corbel, S.] Univ Orleans, CNRS INSU, Stn Radioastron Nancay, Observ Paris,USR 704,OSUC, F-18330 Nancay, France. [Coriat, M.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Moin, A.; Russell, D. M.] New York Univ Abu Dhabi, Abu Dhabi, U Arab Emirates. [Moin, A.] Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Sivakoff, G. R.; Tetarenko, A. J.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Belloni, T. M.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Fender, R. P.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.; Koerding, E. G.; Torres, M. A. P.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] USRA, Columbia, MD 21044 USA. [Maitra, D.] Wheaton Coll, Dept Phys & Astron, Norton, MA 02766 USA. [Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Middleton, M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Migliari, S.] Univ Barcelona, Dept Astron & Meteorol, E-08028 Barcelona, Spain. [Migliari, S.] Univ Barcelona, Inst Cosm Sci, E-08028 Barcelona, Spain. [Remillard, R. A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rupen, M. P.] Herzberg Astron & Astrophys, Natl Res Council, Penticton, BC V2A 6J9, Canada. [Rupen, M. P.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Tudose, V.] Inst Space Sci, RO-077125 Bucharest, Romania. [Tzioumis, A. K.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia. RP Russell, TD (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM thomas.russell@icrar.org RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011; Tudose, Valeriu/F-8976-2010; OI Miller-Jones, James/0000-0003-3124-2814; Sivakoff, Gregory/0000-0001-6682-916X; Russell, David/0000-0002-3500-631X; Russell, Thomas/0000-0001-6958-8891 FU Australian Research Council [DP 120102393]; Royal Society; French Research National Agency: CHAOS project [ANR-12-BS05-0009]; Uni-vEarthS Labex program of Sorbonne Paris Cite [ANR-10-LABX-0023, ANR-11-IDEX-0005-02]; NSERC Discovery Grant; INAF-PRIN [2012-6]; Spanish Ministerio de Economia y Competitividad; European Social Funds through a Ramon y Cajal Fellowship; Spanish Ministerio de Ciencia e Innovacion [AYA2013-47447-C03-1-P]; state government of Western Australia; Commonwealth of Australia FX We would like to thank the anonymous referee for their helpful comments and suggestions. We also thank Tom Maccarone for useful discussions. This research was supported under the Australian Research Council's Discovery Projects funding scheme (project number DP 120102393). DA acknowledges support from the Royal Society. SC acknowledges funding support from the French Research National Agency: CHAOS project ANR-12-BS05-0009 (http://www.chaos-project.fr) and financial support from the Uni-vEarthS Labex program of Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). GRS and AJT are supported by an NSERC Discovery Grant. TMB acknowledges support from INAF-PRIN 2012-6. SM acknowledges support by the Spanish Ministerio de Economia y Competitividad and European Social Funds through a Ramon y Cajal Fellowship and the Spanish Ministerio de Ciencia e Innovacion (SM; grant AYA2013-47447-C03-1-P). This research has made use of NASA's Astrophysics Data System. The International Centre for Radio Astronomy Research is a joint venture between Curtin University and the University of Western Australia, funded by the state government of Western Australia and the joint venture partners. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 118 TC 9 Z9 9 U1 0 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 JUN 21 PY 2015 VL 450 IS 2 BP 1745 EP 1759 DI 10.1093/mnras/stv723 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500047 ER PT J AU Pota, V Brodie, JP Bridges, T Strader, J Romanowsky, AJ Villaume, A Jennings, Z Faifer, FR Pastorello, N Forbes, DA Campbell, A Usher, C Foster, C Spitler, LR Caldwell, N Forte, JC Norris, MA Zepf, SE Beasley, MA Gebhardt, K Hanes, DA Sharples, RM Arnold, JA AF Pota, Vincenzo Brodie, Jean P. Bridges, Terry Strader, Jay Romanowsky, Aaron J. Villaume, Alexa Jennings, Zach Faifer, Favio R. Pastorello, Nicola Forbes, Duncan A. Campbell, Ainsley Usher, Christopher Foster, Caroline Spitler, Lee R. Caldwell, Nelson Forte, Juan C. Norris, Mark A. Zepf, Stephen E. Beasley, Michael A. Gebhardt, Karl Hanes, David A. Sharples, Ray M. Arnold, Jacob A. TI A SLUGGS and Gemini/GMOS combined study of the elliptical galaxy M60: wide-field photometry and kinematics of the globular cluster system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; galaxies: haloes; galaxies: kinematics and dynamics; galaxies: star clusters: individual: NGC 4649 ID HUBBLE-SPACE-TELESCOPE; ACS-VIRGO CLUSTER; CHANDRA MONITORING OBSERVATIONS; DATA REDUCTION PROCEDURES; SUPERMASSIVE BLACK-HOLE; DARK-MATTER CONTENT; DIGITAL-SKY-SURVEY; X-RAY BINARIES; NGC 4649; PLANETARY-NEBULAE AB We present new wide-field photometry and spectroscopy of the globular clusters (GCs) around NGC 4649 (M60), the third brightest galaxy in the Virgo cluster. Imaging of NGC 4649 was assembled from a recently obtained Hubble Space Telescope/Advanced Camera for Surveys mosaic, and new Subaru/Suprime-Cam and archival Canada-France-Hawaii Telescope/MegaCam data. About 1200 sources were followed up spectroscopically using combined observations from three multi-object spectrographs: Keck/Deep Imaging Multi-Object Spectrograph, Gemini/Gemini Multi-Object Spectrograph and Multiple Mirror Telescope/Hectospec. We confirm 431 unique GCs belonging to NGC 4649, a factor of 3.5 larger than previous data sets and with a factor of 3 improvement in velocity precision. We confirm significant GC colour bimodality and find that the red GCs are more centrally concentrated, while the blue GCs are more spatially extended. We infer negative GC colour gradients in the innermost 20 kpc and flat gradients out to large radii. Rotation is detected along the galaxy major axis for all tracers: blue GCs, red GCs, galaxy stars and planetary nebulae. We compare the observed properties of NGC 4649 with galaxy formation models. We find that formation via a major merger between two gas-poor galaxies, followed by satellite accretion, can consistently reproduce the observations of NGC 4649 at different radii. We find no strong evidence to support an interaction between NGC 4649 and the neighbouring spiral galaxy NGC 4647. We identify interesting GC kinematic features in our data, such as counter-rotating subgroups and bumpy kinematic profiles, which encode more clues about the formation history of NGC 4649. C1 [Pota, Vincenzo; Brodie, Jean P.; Romanowsky, Aaron J.; Villaume, Alexa; Jennings, Zach; Arnold, Jacob A.] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Bridges, Terry; Campbell, Ainsley; Hanes, David A.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Strader, Jay; Zepf, Stephen E.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Romanowsky, Aaron J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Faifer, Favio R.; Forte, Juan C.] Fac Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina. [Faifer, Favio R.] UNLP, CONICET, CCT La Plata, Inst Astrofis La Plata, La Plata, Buenos Aires, Argentina. [Pastorello, Nicola; Forbes, Duncan A.; Usher, Christopher] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Foster, Caroline; Spitler, Lee R.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Spitler, Lee R.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Norris, Mark A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Beasley, Michael A.] Univ La Laguna, E-38206 Tenerife, Canary Islands, Spain. [Beasley, Michael A.] Inst Astrofis Canarias, E-38200 Tenerife, Canary Islands, Spain. [Gebhardt, Karl] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Sharples, Ray M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Pota, V (reprint author), Univ Calif Observ, 1156 High St, Santa Cruz, CA 95064 USA. EM vincenzo.pota@gmail.com RI Sharples, Ray/N-7309-2013; OI Sharples, Ray/0000-0003-3449-8583; Foster, Caroline/0000-0003-0247-1204; Norris, Mark/0000-0002-7001-805X FU Natural Sciences and Engineering Research Council of Canada (NSERC); National Aeronautics and Space Administration; NSF [AST-1211995, AST-0071048]; ARC [DP130100388]; National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project under NASA [NCC5-626]; National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project under California Institute of Technology [NCC5-626]; W. M. Keck Foundation; National Science Foundation FX DAH acknowledges the support of research funding in the form of a Discovery Grant through the Natural Sciences and Engineering Research Council of Canada (NSERC). 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 work was supported by NSF grant AST-1211995. We thank the ARC for financial support via DP130100388.; 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. Some of the data presented herein were obtained at the W. M. Keck Observatory, operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration, and 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. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. Based in part on data collected at Subaru Telescope and obtained from the SMOKA (which is operated by the Astronomy Data Centre, National Astronomical Observatory of Japan), via a Gemini Observatory time exchange. The authors acknowledge the data analysis facilities provided by IRAF, which is distributed by the National Optical Astronomy Observatories and operated by AURA, Inc., under cooperative agreement with the National Science Foundation. We have used the data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Centre/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 161 TC 5 Z9 5 U1 1 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 JUN 21 PY 2015 VL 450 IS 2 BP 1962 EP 1983 DI 10.1093/mnras/stv677 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500064 ER PT J AU Churazov, E Vikhlinin, A Sunyaev, R AF Churazov, E. Vikhlinin, A. Sunyaev, R. TI (No) dimming of X-ray clusters beyond z similar to 1 at fixed mass: crude redshifts and masses from raw X-ray and SZ data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; distance scale; large-scale structure of Universe; X-rays: galaxies: clusters ID COSMOLOGY; GALAXIES; RADIATION; SAMPLE; LIMITS; SCALE AB Scaling relations in the Lambda cold dark matter cosmology predict that for a given mass the clusters formed at larger redshift are hotter, denser and therefore more luminous in X-rays than their local z similar to 0 counterparts. This effect overturns the decrease in the observable X-ray flux so that it does not decrease at z > 1, similar to the SZ signal. Provided that scaling relations remain valid at larger redshifts, X-ray surveys will not miss massive clusters at any redshift, no matter how far they are. At the same time, the difference in scaling with mass and distance of the observable SZ and X-ray signals from galaxy clusters at redshifts z less than or similar to 2 offers a possibility to crudely estimate the redshift and the mass of a cluster. This might be especially useful for pre-selection of massive high-redshift clusters and planning of optical follow-up for overlapping surveys in X-ray (e.g. by SRG/eRosita) and SZ (e.g. Planck, SPT and ACT). C1 [Churazov, E.; Sunyaev, R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.; Vikhlinin, A.; Sunyaev, R.] Space Res Inst IKI, Moscow 117997, Russia. [Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Churazov, E (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM churazov@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013 FU Russian Scientific Foundation [14-22-00271] FX We are grateful to the referee for a number of helpful comments and suggestions. We acknowledge partial support by grant No. 14-22-00271 from the Russian Scientific Foundation. NR 24 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 JUN 21 PY 2015 VL 450 IS 2 BP 1984 EP 1989 DI 10.1093/mnras/stv743 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500065 ER PT J AU Demory, BO Ehrenreich, D Queloz, D Seager, S Gilliland, R Chaplin, WJ Proffitt, C Gillon, M Gunther, MN Benneke, B Dumusque, X Lovis, C Pepe, F Segransan, D Triaud, A Udry, S AF Demory, Brice-Olivier Ehrenreich, David Queloz, Didier Seager, Sara Gilliland, Ronald Chaplin, William J. Proffitt, Charles Gillon, Michael Guenther, Maximilian N. Benneke, Bjoern Dumusque, Xavier Lovis, Christophe Pepe, Francesco Segransan, Damien Triaud, Amaury Udry, Stephane TI Hubble Space Telescope search for the transit of the Earth-mass exoplanet a Centauri B b SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: individual: alpha Centauri B ID ECLIPSING BINARIES; LIGHT-CURVE; HD 189733B; STAR; PLANETS; NOISE; ATMOSPHERES; PERIOD; MODEL; CYCLE AB Results from exoplanet surveys indicate that small planets (super-Earth size and below) are abundant in our Galaxy. However, little is known about their interiors and atmospheres. There is therefore a need to find small planets transiting bright stars, which would enable a detailed characterization of this population of objects. We present the results of a search for the transit of the Earth-mass exoplanet alpha Centauri B b with the Hubble Space Telescope (HST). We observed alpha Centauri B twice in 2013 and 2014 for a total of 40 h. We achieve a precision of 115 ppm per 6-s exposure time in a highly saturated regime, which is found to be consistent across HST orbits. We rule out the transiting nature of a Centauri B b with the orbital parameters published in the literature at 96.6 per cent confidence. We find in our data a single transit-like event that could be associated with another Earth-sized planet in the system, on a longer period orbit. Our programme demonstrates the ability of HST to obtain consistent, high-precision photometry of saturated stars over 26 h of continuous observations. C1 [Demory, Brice-Olivier; Queloz, Didier; Guenther, Maximilian N.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Ehrenreich, David; Lovis, Christophe; Pepe, Francesco; Segransan, Damien; Udry, Stephane] Univ Geneva, Astron Observ, CH-1290 Versoix, Switzerland. [Seager, Sara] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Gilliland, Ronald] Penn State Univ, Dept Astron, University Pk, PA 16802 USA. [Gilliland, Ronald] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Chaplin, William J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.] Aarhus Univ, Dept Phys & Astron, SAC, DK-8000 Aarhus C, Denmark. [Proffitt, Charles] Comp Sci Corp, Sci Programs, Baltimore, MD 21218 USA. [Proffitt, Charles] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gillon, Michael] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Benneke, Bjoern] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Dumusque, Xavier] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Triaud, Amaury] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Demory, BO (reprint author), Univ Cambridge, Cavendish Lab, Astrophys Grp, JJ Thomson Ave, Cambridge CB3 0HE, England. EM bod21@cam.ac.uk OI Gunther, Maximilian N./0000-0002-3164-9086; Demory, Brice-Olivier/0000-0002-9355-5165; Ehrenreich, David/0000-0001-9704-5405 FU NASA [NAS 5-26555]; NASA from the Space Telescope Science Institute [NAS 5-26555]; Swiss National Science Foundation (SNSF) [P300P2-147773]; [PID13180]; [13927] FX We are indebted to Shelly Meyett and Tricia Royle for their assistance in the planning and executing of these observations. We thank Tom Ayres for his help in preparing our phase 2 programme, as well as Adrian Barker, Samantha Thompson and Julien de Wit for discussions. We also thank the anonymous referee for a detailed and helpful review that improved the paper. We are grateful to STScI Director Matt Mountain for awarding Director's Discretionary Time for both programmes. Based on observations made with the NASA/ESA HST, 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. These observations are associated with programme PID13180 and 13927. Support for this programme 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. This work has been carried out within the frame of the National Center for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). DE, CL, FP, and SU acknowledge the financial support of the SNSF. AT is a Swiss National Science Foundation fellow under grant number P300P2-147773. NR 38 TC 11 Z9 11 U1 1 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 JUN 21 PY 2015 VL 450 IS 2 BP 2043 EP 2051 DI 10.1093/mnras/stv673 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500070 ER PT J AU Lorimer, DR Esposito, P Manchester, RN Possenti, A Lyne, AG McLaughlin, MA Kramer, M Hobbs, G Stairs, IH Burgay, M Eatough, RP Keith, MJ Faulkner, AJ D'Amico, N Camilo, F Corongiu, A Crawford, F AF Lorimer, D. R. Esposito, P. Manchester, R. N. Possenti, A. Lyne, A. G. McLaughlin, M. A. Kramer, M. Hobbs, G. Stairs, I. H. Burgay, M. Eatough, R. P. Keith, M. J. Faulkner, A. J. D'Amico, N. Camilo, F. Corongiu, A. Crawford, F. TI The Parkes multibeam pulsar survey - VII. Timing of four millisecond pulsars and the underlying spin-period distribution of the Galactic millisecond pulsar population SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; stars: neutron; pulsars: general ID RADIO PULSARS; INITIAL DISCOVERIES; BINARY; SEARCHES; SYSTEM; BIRTH AB We present timing observations of 4-ms pulsars discovered in the Parkes 20-cm multibeam pulsar survey of the Galactic plane. PSRs J1552-4937 and J1843-1448 are isolated objects with spin periods of 6.28 and 5.47 ms, respectively. PSR J1727-2946 is in a 40-d binary orbit and has a spin period of 27 ms. The 4.43-ms pulsar J1813-2621 is in a circular 8.16-d binary orbit around a low-mass companion star with a minimum companion mass of 0.2 M Combining these results with detections from five other Parkes multibeam surveys, gives a well-defined sample of 56 pulsars with spin periods below 20 ms. We develop a likelihood analysis to constrain the functional form which best describes the underlying distribution of spin periods for millisecond pulsars. The best results were obtained with a lognormal distribution. A gamma distribution is less favoured, but still compatible with the observations. Uniform, power-law and Gaussian distributions are found to be inconsistent with the data. Galactic millisecond pulsars being found by current surveys appear to be in agreement with a lognormal distribution which allows for the existence of pulsars with periods below 1.5 ms. C1 [Lorimer, D. R.; McLaughlin, M. A.] W Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA. [Esposito, P.; Crawford, F.] Ist Astrofis Spaziale & Fis Cosm Milano, INAF, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Manchester, R. N.; Hobbs, G.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Possenti, A.; Burgay, M.; D'Amico, N.; Corongiu, A.] INAF, Osservatorio Astron Cagliari, I-09047 Selargius, CA, Italy. [Lyne, A. G.; Keith, M. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Kramer, M.; Eatough, R. P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Stairs, I. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Faulkner, A. J.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [D'Amico, N.] Univ Cagliari, Dipartimento Fis, I-90042 Monserrato, CA, Italy. [Camilo, F.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Crawford, F.] Franklin & Marshall Coll, Dept Phys & Astron, Lancaster, PA 17604 USA. RP Lorimer, DR (reprint author), W Virginia Univ, Dept Phys & Astron, POB 6315, Morgantown, WV 26506 USA. EM Duncan.Lorimer@mail.wvu.edu OI Corongiu, Alessandro/0000-0002-5924-3141; Burgay, Marta/0000-0002-8265-4344; Esposito, Paolo/0000-0003-4849-5092 FU Commonwealth of Australia for operation as a National Facility; Royal Society; Oxford Astrophysics; US Department of State; NSERC Discovery Grant; National Science Foundation PIRE award [0968296] FX The Parkes radio telescope is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. DRL acknowledges support from the Royal Society as a University Research Fellow during the early phases of this project. DRL and MAM acknowledge support from Oxford Astrophysics while on sabbatical leave in 2013. PE acknowledges a Fulbright Research Scholar grant administered by the US-Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. The Fulbright Scholar Program is sponsored by the US Department of State and administered by CIES, a division of IIE. Pulsar Research at UBC is supported by an NSERC Discovery Grant. Current support to DRL and MAM is provided by the National Science Foundation PIRE award 0968296. DRL thanks Joris Verbiest for useful discussions and to Simon Johnston and the CSIRO staff for their hospitality during the final stages of this work. We thank the referee for useful comments on the originally submitted version of this paper. NR 51 TC 5 Z9 6 U1 0 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 JUN 21 PY 2015 VL 450 IS 2 BP 2185 EP 2194 DI 10.1093/mnras/stv804 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6LB UT WOS:000356338500082 ER PT J AU Ade, PAR Aikin, RW Barkats, D Benton, SJ Bischoff, CA Bock, JJ Bradford, KJ Brevik, JA Buder, I Bullock, E Dowell, CD Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Hasselfield, M Hildebrandt, SR Hilton, GC Hui, H Irwin, KD Kang, JH Karkare, KS Kaufman, JP Keating, BG Kefeli, S Kernasovskiy, SA Kovac, JM Kuo, CL Leitch, EM Lueker, M Megerian, KG Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Richter, S Schwarz, R Sheehy, CD Staniszewski, ZK Sudiwala, RV Teply, GP Thompson, K Tolan, JE Turner, AD Vieregg, AG Weber, AC Wong, CL Yoon, KW AF Ade, P. A. R. Aikin, R. W. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Bradford, K. J. Brevik, J. A. Buder, I. Bullock, E. Dowell, C. D. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Hui, H. Irwin, K. D. Kang, J. H. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kefeli, S. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leitch, E. M. Lueker, M. Megerian, K. G. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Richter, S. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Sudiwala, R. V. Teply, G. P. Thompson, K. Tolan, J. E. Turner, A. D. Vieregg, A. G. Weber, A. C. Wong, C. L. Yoon, K. W. CA BICEP2 Keck Array Collaborations TI BICEP2/KECK ARRAY. IV. OPTICAL CHARACTERIZATION AND PERFORMANCE OF THE BICEP2 AND KECK ARRAY EXPERIMENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; polarization ID GRAVITY-WAVES; POLARIZATION; POLARIMETER AB BICEP2. and the Keck Array. are polarization-sensitive microwave telescopes that observe the cosmic microwave background (CMB) from the South Pole at degree angular scales in search of a signature of inflation imprinted as B-mode polarization in the CMB. BICEP2. was deployed in late 2009, observed for three years until the end of 2012 at 150 GHz with 512 antenna-coupled transition edge sensor bolometers, and has reported a detection of B-mode polarization on degree angular scales. The Keck Array. was first deployed in late 2010 and will observe through 2016 with five receivers at several frequencies (95, 150, and 220 GHz). BICEP2. and the Keck Array. share a common optical design and employ the field-proven BICEP1. strategy of using small-aperture, cold, on-axis refractive optics, providing excellent control of systematics while maintaining a large field of view. This design allows for full characterization of far-field optical performance using microwave sources on the ground. Here we describe the optical design of both instruments and report a full characterization of the optical performance and beams of BICEP2. and the Keck Array. at 150 GHz. C1 [Ade, P. A. R.; Sudiwala, R. V.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Aikin, R. W.; Bock, J. J.; Brevik, J. A.; Filippini, J. P.; Golwala, S. R.; Hildebrandt, S. R.; Hui, H.; Kefeli, S.; Lueker, M.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Bischoff, C. A.; Bradford, K. J.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Dowell, C. D.; Hildebrandt, S. R.; Megerian, K. G.; Nguyen, H. T.; O'Brient, R.; Turner, A. D.; Weber, A. C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bullock, E.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Duband, L.] Univ Grenoble Alpes, CEA INAC SBT, F-38000 Grenoble, France. [Filippini, J. P.] Univ Illinois, Dept Phys, Urbana, IL 61820 USA. [Fliescher, S.; Pryke, C.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Halpern, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Hilton, G. C.; Irwin, K. D.] Natl Inst Stand & Technol, Boulder, CO 80305 USA. [Irwin, K. D.; Kang, J. H.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Thompson, K.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Irwin, K. D.; Kuo, C. L.; Ogburn, R. W.; Yoon, K. W.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Kaufman, J. P.; Keating, B. G.; Orlando, A.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Leitch, E. M.; Sheehy, C. D.; Vieregg, A. G.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Vieregg, A. G.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM avieregg@kicp.uchicago.edu OI Orlando, Angiola/0000-0001-8004-5054; Karkare, Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954 FU National Science Foundation (NSF) (Caltech/Harvard) [ANT-0742818, ANT-1044978]; National Science Foundation (NSF) (Chicago/Minnesota) [ANT-0742592, ANT-1110087]; NSF (Harvard) [ANT-1145172]; NSF (Minnesota) [ANT-1145143]; NSF (Stanford) [ANT-1145248]; W. M. Keck Foundation (Caltech); JPL Research and Technology Development Fund; NASA [06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at Caltech; Canada Foundation for Innovation; FAS Science Division Research Computing Group at Harvard; U.S. Department of Energy Office of Science; W. M. Keck Foundation FX BICEP2 was supported by the National Science Foundation (NSF) under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). The Keck Array. was supported by the NSF under grants ANT-1145172 (Harvard), ANT-1145143 (Minnesota), and ANT-1145248 (Stanford), and by the W. M. Keck Foundation (Caltech). The development of antenna-coupled detector technology was supported by the JPL Research and Technology Development Fund and grants 06-ARPA206-0040 and 10-SAT10-0017 from the NASA APRA and SAT programs. The development and testing of focal planes were supported by the Gordon and Betty Moore Foundation at Caltech. Readout electronics were supported by a Canada Foundation for Innovation grant to UBC. Computations presented in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard. The analysis effort at Stanford and SLAC was partially suported by the U.S. Department of Energy Office of Science. The receiver development was supported in part by a grant from the W. M. Keck Foundation. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. NR 29 TC 8 Z9 8 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 206 DI 10.1088/0004-637X/806/2/206 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500061 ER PT J AU Baxter, EJ Keisler, R Dodelson, S Aird, KA Allen, SW Ashby, MLN Bautz, M Bayliss, M Benson, BA Bleem, LE Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Chiu, I Cho, HM Clocchiatti, A Crawford, TM Crites, AT Desai, S Dietrich, JP de Haan, T Dobbs, MA Foley, RJ Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Harrington, NL Hennig, C Hoekstra, H Holder, GP Holzapfel, WL Hou, Z Hrubes, JD Jones, C Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Meyer, SS Millea, M Mocanu, LM Murray, SS Padin, S Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shirokoff, E Song, J Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, KT van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Baxter, E. J. Keisler, R. Dodelson, S. Aird, K. A. Allen, S. W. Ashby, M. L. N. Bautz, M. Bayliss, M. Benson, B. A. Bleem, L. E. 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. de Haan, T. Dobbs, M. A. Foley, R. J. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. L. Hennig, C. Hoekstra, H. Holder, G. P. Holzapfel, W. L. Hou, Z. Hrubes, J. D. Jones, C. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Meyer, S. S. Millea, M. Mocanu, L. M. Murray, S. S. Padin, S. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. T. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI A MEASUREMENT OF GRAVITATIONAL LENSING OF THE COSMIC MICROWAVE BACKGROUND BY GALAXY CLUSTERS USING DATA FROM THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; gravitational lensing: weak; galaxies: clusters: general ID LARGE-SCALE STRUCTURE; DARK-MATTER HALOES; 720 SQUARE DEGREES; SPT-SZ SURVEY; DENSITY PROFILES; STAR-FORMATION; DAMPING TAIL; X-RAYS; CMB; ROTATION AB Clusters of galaxies are expected to gravitationally lens the cosmic microwave background (CMB) and thereby generate a distinct signal in the CMB on arcminute scales. Measurements of this effect can be used to constrain the masses of galaxy clusters with CMB data alone. Here we present a measurement of lensing of the CMB by galaxy clusters using data from the South Pole Telescope (SPT). We develop a maximum likelihood approach to extract the CMB cluster lensing signal and validate the method on mock data. We quantify the effects on our analysis of several potential sources of systematic error and find that they generally act to reduce the best-fit cluster mass. It is estimated that this bias to lower cluster mass is roughly 0.85s in units of the statistical error bar, although this estimate should be viewed as an upper limit. We apply our maximum likelihood technique to 513 clusters selected via their Sunyaev-Zeldovich (SZ) signatures in SPT data, and rule out the null hypothesis of no lensing at 3.1s. The lensing-derived mass estimate for the full cluster sample is consistent with that inferred from the SZ flux: M-200,M-lens = 0.83(-0.37)(+0.38) M-200 (68% C. L., statistical error only). C1 [Baxter, E. J.] Univ Penn, Dept Phys & Astron, Ctr Particle Cosmol, Philadelphia, PA 19104 USA. [Baxter, E. J.; Dodelson, S.; Benson, B. A.; Carlstrom, J. E.; 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. [Baxter, E. J.; Keisler, R.; Dodelson, S.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Hou, Z.; Leitch, E. M.; Mantz, A.; Meyer, S. S.; Mocanu, L. M.; Padin, S.; Schaffer, K. K.; Shirokoff, E.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Keisler, R.; Allen, S. W.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Keisler, R.; Allen, S. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Keisler, R.; Bleem, L. E.; Carlstrom, J. E.; Hou, Z.; Meyer, S. S.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Dodelson, S.; Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Ashby, M. L. N.; Bayliss, M.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bayliss, M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Bocquet, S.; Chiu, I.; Desai, S.; Dietrich, J. P.; Hennig, C.; Liu, J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Brodwin, M.; Chiu, I.; Desai, S.; Dietrich, J. P.; Hennig, C.; Liu, J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Chang, C. L.; 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 & Astrosif, Santiago, Chile. [Crites, A. T.; Lueker, M.; Padin, S.; Williamson, R.] CALTECH, Pasadena, CA 91125 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [de Haan, T.; George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Dobbs, M. A.] Canadian Inst Adv Res, CIFAR Program Cosmol & Grav, Toronto, ON M5G 1Z8, Canada. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [George, E. M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, NL-2333 CA Leiden, Netherlands. [Knox, L.; Millea, M.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, 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. [Reichardt, C. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; 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, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Zenteno, A.] Natl Opt Astron Observ, Cerro Tololo Inter Amer Observ, La Serena, Chile. RP Baxter, EJ (reprint author), Univ Penn, Dept Phys & Astron, Ctr Particle Cosmol, Philadelphia, PA 19104 USA. RI Holzapfel, William/I-4836-2015; Williamson, Ross/H-1734-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; CRAWFORD, THOMAS/0000-0001-9000-5013; Dietrich, Jorg/0000-0002-8134-9591; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Forman, William/0000-0002-9478-1682; 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]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA Office of Space Science; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-1125897]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Alfred P. Sloan Research Fellowship; U.S. Department of Energy [DE-FG02-95ER40896]; Miller Research Fellowship; NSF [AST-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 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. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. 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. 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. M. Dobbs acknowledges support from an Alfred P. Sloan Research Fellowship. S. Dodelson is supported by the U.S. Department of Energy, including grant DE-FG02-95ER40896. T. de Haan is supported by a Miller Research Fellowship. Cluster studies at SAO are supported by NSF grant AST-1009649. NR 81 TC 9 Z9 9 U1 2 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 JUN 20 PY 2015 VL 806 IS 2 AR 247 DI 10.1088/0004-637X/806/2/247 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500102 ER PT J AU Bose, S Sutaria, F Kumar, B Duggal, C Misra, K Brown, PJ Singh, M Dwarkadas, V York, DG Chakraborti, S Chandola, HC Dahlstrom, J Ray, A Safonova, M AF Bose, Subhash Sutaria, Firoza Kumar, Brijesh Duggal, Chetna Misra, Kuntal Brown, Peter J. Singh, Mridweeka Dwarkadas, Vikram York, Donald G. Chakraborti, Sayan Chandola, H. C. Dahlstrom, Julie Ray, Alak Safonova, Margarita TI SN 2013ej: A TYPE IIL SUPERNOVA WITH WEAK SIGNS OF INTERACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 0628); supernovae: general; supernovae: individual (SN 2013ej) ID CORE-COLLAPSE SUPERNOVAE; EXPANDING PHOTOSPHERE METHOD; LIGHT CURVES; PLATEAU SUPERNOVAE; QUANTITATIVE SPECTROSCOPY; PHOTOMETRIC PROPERTIES; ANALYTIC SOLUTIONS; DUST FORMATION; IB SUPERNOVAE; NI-56 EJECTA AB We present optical photometric and spectroscopic observations of SN 2013ej. It is one of the brightest Type II supernovae (SNe II) exploded in a nearby (similar to 10 Mpc) galaxy, NGC 628. The light-curve characteristics are similar to SNe II, but with a relatively shorter (similar to 85 days) and steeper (similar to 1.7 mag (100 days)(-1) in V) plateau phase. The SN. shows a large drop of 2.4 mag in V-band brightness during the plateau-to-nebular transition. The absolute ultraviolet (UV) light curves are identical to SN 2012aw, showing a similar UV-plateau trend extending up to 85 days. The radioactive Ni-56 mass estimated from the tail luminosity is 0.02 M-circle dot, which is significantly lower than typical SNe IIP. The characteristics of spectral features and evolution of line velocities indicate that SN 2013ej is a Type II event. However, light-curve characteristics and some spectroscopic features provide strong support in classifying it as a Type IIL event. A detailed SYNOW modeling of spectra indicates the presence of some high-velocity components in H alpha and H beta profiles, implying a possible ejecta-circumstellar medium interaction. The nebular phase spectrum shows an unusual notch in the Ha emission, which may indicate bipolar distribution of Ni-56. Modeling of the bolometric light curve yields a progenitor mass of similar to 14 M-circle dot and a radius of similar to 450 R-circle dot, with a total explosion energy of similar to 2.3 x 10(51) erg. C1 [Bose, Subhash; Kumar, Brijesh; Misra, Kuntal; Singh, Mridweeka] Aryabhatta Res Inst Observ Sci, Naini Tal 263002, India. [Bose, Subhash; Chandola, H. C.] Kumaun Univ, Dept Phys, Ctr Adv Study, Naini Tal 263001, India. [Sutaria, Firoza; Duggal, Chetna; Safonova, Margarita] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Brown, Peter J.] Texas A&M Univ, Dept Phys & Astron, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Dwarkadas, Vikram] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, Donald G.] Univ Chicago, Ctr Astron & Astrophys, Chicago, IL 60637 USA. [York, Donald G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Chakraborti, Sayan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Dahlstrom, Julie] Carthage Coll, Kenosha, WI 53140 USA. [Ray, Alak] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. RP Bose, S (reprint author), Aryabhatta Res Inst Observ Sci, Naini Tal 263002, India. EM email@subhashbose.com FU NASA's Astrophysics Data Analysis Program [NNX13AF35G]; NASA through Chandra Award [GO2-13092B]; NASA [NAS8-03060] FX We are thankful to the observing staffs and technical assistants of the ARIES 1.0 and 1.3 m telescopes, and we also express our thanks to 2 m HCT telescope staffs for their kind cooperation in observation of SN 2013ej. We also express our thanks to Mr. Shashank Shekhar for his sincere efforts and cooperation during observations at the ARIES 1.3 m telescope. Authors gratefully acknowledge the services of the NASA ADS and NED databases, which are used to access data and references in this paper. SOUSA is supported by NASA's Astrophysics Data Analysis Program through grant NNX13AF35G. V.V.D.'s work on Type IIP SNe is supported by NASA through Chandra Award No. GO2-13092B issued by Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. We also thank the anonymous referee for detailed and insightful comments that helped significantly improve. the manuscript. NR 83 TC 11 Z9 11 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 160 DI 10.1088/0004-637X/806/2/160 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500015 ER PT J AU Czekala, I Andrews, SM Jensen, ELN Stassun, KG Torres, G Wilner, DJ AF Czekala, I. Andrews, S. M. Jensen, E. L. N. Stassun, K. G. Torres, G. Wilner, D. J. TI A DISK-BASED DYNAMICAL MASS ESTIMATE FOR THE YOUNG BINARY AK SCO SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: fundamental parameters; stars: individual (AK Sco); stars: pre-main sequence ID MAIN-SEQUENCE TRACKS; ECLIPSING BINARY; PROTOPLANETARY DISKS; EVOLUTIONARY TRACKS; STARS; SCORPII; SYSTEM; TEMPERATURES; CONSTRAINTS; CALIBRATION AB We present spatially and spectrally resolved Atacama Large Millimeter/submillimeter Array (ALMA) observations of gas and dust in the disk orbiting the pre-main sequence (pre-MS) binary AK Sco. By forward-modeling the disk velocity field traced by CO J = 2-1 line emission, we infer the mass of the central binary, M-* = 2.49 +/- 0.10 M-circle dot, a new dynamical measurement that is independent of stellar evolutionary models. Assuming the disk and binary are co-planar within similar to 2 degrees, this disk-based binary mass measurement is in excellent agreement with constraints from radial velocity monitoring of the combined stellar spectra. These ALMA results are also compared with the standard approach of estimating masses from the location of the binary in the Hertzsprung-Russell diagram, using several common pre-MS model grids. These models predict stellar masses that are marginally consistent with our dynamical measurement (at similar to 2 sigma), but are systematically high (by similar to 10%). These same models consistently predict an age of 18 +/- 1 Myr for AK Sco, in line with its membership in the Upper Centaurus-Lupus association but surprisingly old for it to still host a gas-rich disk. As ALMA accumulates comparable data for large samples of pre-MS stars, the methodology employed here to extract a dynamical mass from the disk rotation curve should prove extraordinarily useful for efforts to characterize the fundamental parameters of early stellar evolution. C1 [Czekala, I.; Andrews, S. M.; Torres, G.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jensen, E. L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Stassun, K. G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, K. G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. RP Czekala, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM iczekala@cfa.harvard.edu OI Jensen, Eric/0000-0002-4625-7333; Czekala, Ian/0000-0002-1483-8811; Stassun, Keivan/0000-0002-3481-9052 FU NSF Graduate Fellowship; Smithsonian Institution; NRAO Student Observing Support program FX The authors appreciate the helpful advice of Eric Stempels and Maxwell Moe; help with an eccentric disk model from Meredith Hughes, Sam Factor, and Eugene Chiang; and the technical support regarding our many ALMA calibration questions from Jennifer Donovan Meyer. The authors also thank the referree, Michal Simon, for his insightful and helpful comments. I.C. is supported by the NSF Graduate Fellowship and the Smithsonian Institution. S.A. acknowledges the very helpful support provided by the NRAO Student Observing Support program related to the early development of this project. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2012.1.00496.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. Figure 3 was generated with triangle.py (Foreman-Mackey et al. 2014). This research made extensive use of the Julia programming language (Bezanson et al. 2012) and Astropy (Astropy Collaboration 2013). NR 51 TC 13 Z9 13 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 JUN 20 PY 2015 VL 806 IS 2 AR 154 DI 10.1088/0004-637X/806/2/154 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500009 ER PT J AU Damjanov, I Geller, MJ Zahid, HJ Hwang, HS AF Damjanov, Ivana Geller, Margaret J. Zahid, H. Jabran Hwang, Ho Seong TI QUIESCENT COMPACT GALAXIES AT INTERMEDIATE REDSHIFT IN THE COSMOS FIELD. THE NUMBER DENSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: stellar content; galaxies: structure ID SIMILAR-TO 2; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; STAR-FORMING GALAXIES; SUPERDENSE MASSIVE GALAXIES; EXTRAGALACTIC LEGACY SURVEY; INSIDE-OUT GROWTH; VLT DEEP SURVEY; LESS-THAN 2 AB We investigate the evolution of compact galaxy number density over the redshift range 0.2 < z < 0.8. Our sample consists of galaxies with secure spectroscopic redshifts observed in the COSMOS field. With the large uncertainties, the compact galaxy number density trend with redshift is consistent with a constant value over the interval 0.2 < z < 0.8. Our number density estimates are similar to the estimates at z > 1 for equivalently selected compact samples. Small variations in the abundance of the COSMOS compact sources as a function of redshift correspond to known structures in the field. The constancy of the compact galaxy number density is robust and insensitive to the compactness threshold or the stellar mass range (for M-* > 10(10) M-circle dot). To maintain constant number density any size growth of high-redshift compact systems with decreasing redshift must be balanced by a formation of quiescent compact systems at z < 1. C1 [Damjanov, Ivana] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Geller, Margaret J.; Zahid, H. Jabran; Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hwang, Ho Seong] Korea Inst Adv Study, Sch Phys, Seoul 130722, South Korea. RP Damjanov, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Geller, Margaret/0000-0002-9146-4876 FU Harvard College Observatory Menzel Fellowship; Natural Sciences and Engineering Research Council of Canada Postdoctoral Fellowship (NSERC) [PDF-421224-2012]; Smithsonian Institution; Clay Fellowship FX We thank the referee for a careful reading of the manuscript and for suggesting the inclusion of Table 2. I.D. is supported by the Harvard College Observatory Menzel Fellowship and the Natural Sciences and Engineering Research Council of Canada Postdoctoral Fellowship (NSERC PDF-421224-2012). The Smithsonian Institution supports the research of M.J.G. H.J.Z. gratefully acknowledges the generous support of the Clay Fellowship. NR 77 TC 12 Z9 12 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 158 DI 10.1088/0004-637X/806/2/158 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500013 ER PT J AU Foreman-Mackey, D Montet, BT Hogg, DW Morton, TD Wang, D Scholkopf, B AF Foreman-Mackey, Daniel Montet, Benjamin T. Hogg, David W. Morton, Timothy D. Wang, Dun Schoelkopf, Bernhard TI A SYSTEMATIC SEARCH FOR TRANSITING PLANETS IN THE K2 DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; methods: data analysis; methods: statistical; planetary systems; stars: statistics ID ASTROPHYSICAL FALSE POSITIVES; LIGHT CURVES; ERROR-CORRECTION; KEPLER MISSION; CANDIDATES; ALGORITHM; EARTH; POPULATION; PHOTOMETRY; EXOPLANET AB Photometry of stars from the K2. extension of NASA's Kepler. mission is afflicted by systematic effects caused by small (few-pixel) drifts in the telescope pointing and other spacecraft issues. We present a method for searching K2. light curves for evidence of exoplanets by simultaneously fitting for these systematics and the transit signals of interest. This method is more computationally expensive than standard search algorithms but we demonstrate that it can be efficiently implemented and used to discover transit signals. We apply this method to the full Campaign 1 data set and report a list of 36 planet candidates transiting 31 stars, along with an analysis of the pipeline performance and detection efficiency based on artificial signal injections and recoveries. For all planet candidates, we present posterior distributions on the properties of each system based strictly on the transit observables. C1 [Foreman-Mackey, Daniel; Hogg, David W.; Wang, Dun] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Montet, Benjamin T.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hogg, David W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Hogg, David W.] NYU, Ctr Data Sci, New York, NY 10003 USA. [Morton, Timothy D.] Princeton Univ, Dept Astrophys, Princeton, NJ 08544 USA. [Schoelkopf, Bernhard] Max Planck Inst Intelligent Syst, D-72076 Tubingen, Germany. RP Foreman-Mackey, D (reprint author), NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. EM danfm@nyu.edu OI Montet, Benjamin/0000-0001-7516-8308; Hogg, David/0000-0003-2866-9403 FU National Science Foundation [IIS-1124794, DGE1144469]; National Aeronautics and Space Administration [NNX12AI50G]; Moore-Sloan Data Science Environment at NYU; NASA under the Exoplanet Exploration Program; NASA Science Mission directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G] FX It is a pleasure to thank Eric Agol (UW), Ruth Angus (Oxford), Tom Barclay (Ames), Zach Berta-Thompson (MIT), Daniel Bramich (QEERI, Qatar), Geza Kovacs (Konkoly Observatory), Laura Kreidberg (Chicago), Erik Petigura (Berkeley), Roberto Sanchis Ojeda (Berkeley), and Andrew Vanderburg (Harvard) for helpful contributions to the ideas and code presented here. We also thank the anonymous referee for comments that improved the manuscript. D. F. M., D. W. H., and D. W. were partially supported by the National Science Foundation (grant IIS-1124794), the National Aeronautics and Space Administration (grant NNX12AI50G), and the Moore-Sloan Data Science Environment at NYU. B. T. M. was supported by a National Science Foundation Graduate Research Fellowship (grant DGE1144469). This research made use of the NASA Astrophysics Data System and the NASA Exoplanet Archive. The Archive is operated by the California Institute of Technology, under contract with NASA under the Exoplanet Exploration Program. This paper includes data collected by the Kepler. mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. We are grateful to the entire Kepler team, past and present. Their tireless efforts were all essential to the tremendous success of the mission and the successes of K2, present and future. These data 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 is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. NR 45 TC 36 Z9 36 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 215 DI 10.1088/0004-637X/806/2/215 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500070 ER PT J AU Hahn, CH Blanton, MR Moustakas, J Coil, AL Cool, RJ Eisenstein, DJ Skibba, RA Wong, KC Zhu, GT AF Hahn, ChangHoon Blanton, Michael R. Moustakas, John Coil, Alison L. Cool, Richard J. Eisenstein, Daniel J. Skibba, Ramin A. Wong, Kenneth C. Zhu, Guangtun TI PRIMUS: EFFECTS OF GALAXY ENVIRONMENT ON THE QUIESCENT FRACTION EVOLUTION AT z < 0.8 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: groups: general; galaxies: star formation; galaxies: statistics ID DIGITAL-SKY-SURVEY; STAR-FORMATION HISTORY; STELLAR MASS FUNCTION; SIMILAR-TO 1; REDSHIFT SURVEY; SPECTROSCOPIC SAMPLE; LUMINOSITY FUNCTION; PHYSICAL-PROPERTIES; DENSITY RELATION; FIELD GALAXIES AB We investigate the effects of galaxy environment on the evolution of the quiescent fraction (f(Q)) from z = 0.8 to 0.0 using spectroscopic redshifts and multi-wavelength imaging data from the PRIsm MUlti-object Survey (PRIMUS) and the Sloan Digital Sky Survey (SDSS). Our stellar mass limited galaxy sample consists of similar to 14,000 PRIMUS galaxies within z - 0.2-0.8 and similar to 64,000 SDSS galaxies within z - 0.05-0.12. We classify the galaxies as quiescent or star-forming (SF) based on an evolving specific star formation cut, and as low or high density environments based on fixed cylindrical aperture environment measurements on a volume-limited environment defining population. For quiescent and SF galaxies in low or high density environments, we examine the evolution of their stellar mass function (SMF). Then using the SMFs we compute f(Q) (M-*). and quantify its evolution within our redshift range. We find that the quiescent fraction is higher at higher masses and in denser environments. The quiescent fraction rises with cosmic time for all masses and environments. At a fiducial mass of 10(10.5) M-circle dot, from z similar to 0.7 to 0.1, the quiescent fraction rises by 15% at the lowest environments and by 25% at the highest environments we measure. These results suggest that for a minority of galaxies their cessation of star formation is due to external influences on them. In other words, in the recent universe a substantial fraction of the galaxies that cease forming stars do so due to internal processes. C1 [Hahn, ChangHoon; Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Moustakas, John] Siena Coll, Dept Phys & Astron, Loudonville, NY 12211 USA. [Coil, Alison L.; Skibba, Ramin A.] Univ Calif, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Cool, Richard J.] Univ Arizona, MMT Observ, Tucson, AZ 85721 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wong, Kenneth C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Zhu, Guangtun] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Hahn, CH (reprint author), NYU, Dept Phys, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. EM chh327@nyu.edu OI Zhu, Guangtun/0000-0002-7574-8078; HAHN, CHANG HOON/0000-0003-1197-0902 FU NSF [AST-0607701, 0908246, 0908442, 0908354]; NASA [08-ADP08-0019]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; [NSF-AST-1109432]; [NSF-AST-0908354]; [NSF-AST-1211644] FX C.H. and M.B. were supported by NSF-AST-1109432 and NSF-AST-0908354. M.B. was also supported by NSF-AST-1211644. A.L.C. acknowledges support from NSF CAREER award. We acknowledge Katarina Kovac and Ying-Jie Peng for insightful discussions. We also thank Marla Geha for providing published quiescent fraction results in electronic format.; Funding for PRIMUS has been provided by NSF grants AST-0607701, 0908246, 0908442, 0908354, and NASA grant 08-ADP08-0019. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer, launched in April 2003, whose mission was developed in cooperation with the Centre National d'Etudes Spatiales of France and the Korean Ministry of Science and Technology. 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. NR 74 TC 5 Z9 5 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 JUN 20 PY 2015 VL 806 IS 2 AR 162 DI 10.1088/0004-637X/806/2/162 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500017 ER PT J AU Heinz, S Burton, M Braiding, C Brandt, WN Jonker, PG Sell, P Fender, RP Nowak, MA Schulz, NS AF Heinz, S. Burton, M. Braiding, C. Brandt, W. N. Jonker, P. G. Sell, P. Fender, R. P. Nowak, M. A. Schulz, N. S. TI LORD OF THE RINGS: A KINEMATIC DISTANCE TO CIRCINUS X-1 FROM A GIANT X-RAY LIGHT ECHO SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; stars: distances; stars: individual (Circinus X-1); stars: neutron; techniques: radial velocities; X-rays: binaries ID CO-TO-H-2 CONVERSION FACTOR; MOLECULAR CLOUDS; MILKY-WAY; STAR; BINARY; SCATTERING; DISTRIBUTIONS; HALOS; JETS; COMPANION AB Circinus X-1 exhibited a bright X-ray flare in late 2013. Follow-up observations with Chandra and XMM-Newton from 40 to 80 days after the flare reveal a bright X-ray light echo in the form of four well-defined rings with radii from 5 to 13 arcmin, growing in radius with time. The large fluence of the flare and the large column density of interstellar dust toward Circinus X-1 make this the largest and brightest set of rings from an X-ray light echo observed to date. By deconvolving the radial intensity profile of the echo with the MAXI X-ray light curve of the flare we reconstruct the dust distribution toward Circinus X-1 into four distinct dust concentrations. By comparing the peak in scattering intensity with the peak intensity in CO maps of molecular clouds from the Mopra Southern Galactic Plane CO Survey we identify the two innermost rings with clouds at radial velocity similar to-74 and similar to-81 km s(-1), respectively. We identify a prominent band of foreground photoelectric absorption with a lane of CO gas at similar to-32 km s(-1). From the association of the rings with individual CO clouds we determine the kinematic distance to Circinus X-1 to be DCirX-1 = 9.4(-1.0)(+0.8) kpc. This distance rules out earlier claims of a distance around 4 kpc, implies that Circinus X-1 is a frequent super-Eddington source, and places a lower limit of . 22 on the Lorentz factor and an upper limit of theta(jet) less than or similar to 3 degrees on the jet viewing angle. C1 [Heinz, S.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Burton, M.; Braiding, C.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sell, P.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Fender, R. P.] Univ Oxford, Dept Astron, Astrophys, Oxford OX1 3RH, England. [Nowak, M. A.; Schulz, N. S.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Heinz, S (reprint author), Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. EM heinzs@astro.wisc.edu RI Brandt, William/N-2844-2015; Sell, Paul/B-1283-2017; OI Brandt, William/0000-0002-0167-2453; Sell, Paul/0000-0003-1771-5531; Burton, Michael/0000-0001-7289-1998 FU National Aeronautics and Space Administration through Chandra Award [GO4-15049X]; Chandra X-ray Observatory Center; National Aeronautics Space Administration [NAS8-03060]; ESA Member States; USA (NASA); Commonwealth of Australia; Australian Research Council (ARC); UNSW, Sydney; Monash Universities; CSIRO FX We would like to thanks Snezana Stanimirovic, Bob Benjamin, Audra Hernandez, Min-Yong Lee, and Eugene Churazov for helpful discussions. We would also like to thank the CXC team for outstanding support in scheduling and analyzing the Chandra observations. 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, ChIPS, and Sherpa. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO4-15049X 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. XMM data used in this manuscript were obtained through generously scheduled Director's Discretionary Time. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). During the preparation of this manuscript, we made use of the XMM-ESAS package. We would like to thank the Swift scheduling team for help in planning and executing this program. The CO data was obtained using the Mopra radio telescope, a part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The University of New South Wales (UNSW) digital filter bank (the UNSW-MOPS) used for the observations with Mopra was provided with support from the Australian Research Council (ARC), UNSW, Sydney and Monash Universities, as well as the CSIRO. This research has made use of the MAXI data provided by RIKEN, JAXA and the MAXI team. We acknowledge the use of public data from the Swift data archive. NR 54 TC 6 Z9 6 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 265 DI 10.1088/0004-637X/806/2/265 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500120 ER PT J AU Keck, ML Brenneman, LW Ballantyne, DR Bauer, F Boggs, SE Christensen, FE Craig, WW Dauser, T Elvis, M Fabian, AC Fuerst, F Garcia, J Grefenstette, BW Hailey, CJ Harrison, FA Madejski, G Marinucci, A Matt, G Reynolds, CS Stern, D Walton, DJ Zoghbi, A AF Keck, M. L. Brenneman, L. W. Ballantyne, D. R. Bauer, F. Boggs, S. E. Christensen, F. E. Craig, W. W. Dauser, T. Elvis, M. Fabian, A. C. Fuerst, F. Garcia, J. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Madejski, G. Marinucci, A. Matt, G. Reynolds, C. S. Stern, D. Walton, D. J. Zoghbi, A. TI NUSTAR AND SUZAKU X-RAY SPECTROSCOPY OF NGC 4151: EVIDENCE FOR REFLECTION FROM THE INNER ACCRETION DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: individual (NGC 4151); galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-4151; BLACK-HOLE SPIN; BROAD-BAND SPECTRUM; NARROW-LINE REGION; DEEP CHANDRA ACIS; XMM-NEWTON; SWIFT J2127.4+5654; EMISSION-LINES; IRON LINES AB We present X-ray timing and spectral analyses of simultaneous 150 ks Nuclear Spectroscopic Telescope Array (NuSTAR) and Suzaku X-ray observations of the Seyfert 1.5 galaxy NGC 4151. We disentangle the continuum emission, absorption, and reflection properties of the active galactic nucleus (AGN) by applying inner accretion disk reflection and absorption-dominated models. With a time-averaged spectral analysis, we find strong evidence for relativistic reflection from the inner accretion disk. We find that relativistic emission arises from a highly ionized inner accretion disk with a steep emissivity profile, which suggests an intense, compact illuminating source. We find a preliminary, near-maximal black hole spin a > 0.9 accounting for statistical and systematic modeling errors. We find a relatively moderate reflection fraction with respect to predictions for the lamp post geometry, in which the illuminating corona is modeled as a point source. Through a time-resolved spectral analysis, we find that modest coronal and inner disk reflection (IDR) flux variation drives the spectral variability during the observations. We discuss various physical scenarios for the IDR model and we find that a compact corona is consistent with the observed features. C1 [Keck, M. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Keck, M. L.; Brenneman, L. W.; Elvis, M.; Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bauer, F.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Dauser, T.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Fuerst, F.; Grefenstette, B. W.; Harrison, F. A.; Walton, D. J.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Madejski, G.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Marinucci, A.; Matt, G.] Univ Rome Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Stern, D.; Walton, D. J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zoghbi, A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Keck, ML (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. EM keckm@bu.edu RI XRAY, SUZAKU/A-1808-2009; Boggs, Steven/E-4170-2015; Zoghbi, Abderahmen/A-8445-2017; OI Boggs, Steven/0000-0001-9567-4224; Zoghbi, Abderahmen/0000-0002-0572-9613; Ballantyne, David/0000-0001-8128-6976 FU NASA [NNG08FD60C, NNX13AE90G]; National Aeronautics and Space Administration; Italian Space Agency under ASI/INAF [I/037/12/0-011/13]; European Union [n.312789]; NASA-ADAP [NNX14AF86G, NNX14AF89G]; CONICYT-Chile (Basal-CATA) [PFB-06/2007]; CONICYT-Chile (FONDECYT) [1141218]; CONICYT-Chile (Anillo) [ACT1101]; ICM [IC120009] FX 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. This research made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). M.L.K. gratefully acknowledges support through NASA grant #NNX13AE90G. G.M. and A.M. acknowledge financial support from Italian Space Agency under grant ASI/INAF I/037/12/0-011/13 and from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n.312789. C.S.R. acknowledges support from the NASA-ADAP program under grants NNX14AF86G and NNX14AF89G. F.E.B. acknowledges support from CONICYT-Chile (Basal-CATA PFB-06/2007, FONDECYT 1141218, Anillo ACT1101) and ICM grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS. We thank Alan Marscher for helpful discussions. We thank the anonymous referee for comments, which have improved this manuscript. This research made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and Matplotlib (Hunter 2007). NR 87 TC 16 Z9 16 U1 1 U2 8 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 JUN 20 PY 2015 VL 806 IS 2 AR 149 DI 10.1088/0004-637X/806/2/149 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500004 ER PT J AU Matson, RA Gies, DR Guo, Z Quinn, SN Buchhave, LA Latham, DW Howell, SB Rowe, JF AF Matson, Rachel A. Gies, Douglas R. Guo, Zhao Quinn, Samuel N. Buchhave, Lars A. Latham, David W. Howell, Steve B. Rowe, Jason F. TI HST/COS DETECTION OF THE SPECTRUM OF THE SUBDWARF COMPANION OF KOI-81 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: evolution; stars: individual (KOI-81); subdwarfs ID MASS WHITE-DWARFS; TOMOGRAPHIC SEPARATION; ULTRAVIOLET DETECTION; COMPOSITE SPECTRA; COMPACT OBJECTS; MAIN-SEQUENCE; BINARY-SYSTEM; PHI-PERSEI; STARS; DISCOVERY AB KOI-81 is a totally eclipsing binary discovered by the Kepler mission that consists of a rapidly rotating B-type star and a small, hot companion. The system was forged through large-scale mass transfer that stripped the mass donor of its envelope and spun up the mass gainer star. We present an analysis of UV spectra of KOI-81 that were obtained with the Cosmic Origins Spectrograph on the Hubble Space Telescope that reveal for the first time the spectral features of the faint, hot companion. We present a double-lined spectroscopic orbit for the system that yields mass estimates of 2.92 M-circle dot and 0.19 M-circle dot for the B-star and hot subdwarf, respectively. We used a Doppler tomography algorithm to reconstruct the UV spectra of the components, and a comparison of the reconstructed and model spectra yields effective temperatures of 12 and 19-27 kK for the B-star and hot companion, respectively. The B-star is pulsating, and we identified a number of peaks in the Fourier transform of the light curve, including one that may indicate an equatorial rotation period of 11.5 hr. The B-star has an equatorial velocity that is 74% of the critical velocity where centrifugal and gravitational accelerations balance at the equator, and we fit the transit light curve by calculating a rotationally distorted model for the photosphere of the B-star. C1 [Matson, Rachel A.; Gies, Douglas R.; Guo, Zhao; Quinn, Samuel N.] Georgia State Univ, Ctr High Angular Resolut Astron, Atlanta, GA 30302 USA. [Matson, Rachel A.; Gies, Douglas R.; Guo, Zhao; Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Buchhave, Lars A.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howell, Steve B.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. RP Matson, RA (reprint author), Georgia State Univ, Ctr High Angular Resolut Astron, POB 5060, Atlanta, GA 30302 USA. EM rmatson@chara.gsu.edu; gies@chara.gsu.edu; guo@chara.gsu.edu; quinn@astro.gsu.edu; lbuchhave@cfa.harvard.edu; dlatham@cfa.harvard.edu; steve.b.howell@nasa.gov; Jason.Rowe@nasa.gov OI Buchhave, Lars A./0000-0003-1605-5666; Gies, Douglas/0000-0001-8537-3583; Latham, David/0000-0001-9911-7388 FU NASA through Space Telescope Science Institute [12288]; NASA [NAS 5-26555]; National Science Foundation [AST-1411654]; GSU ACI Fellowship; GSU College of Arts and Sciences; Research Program Enhancement fund of the Board of Regents of the University System of Georgia FX We are grateful to Charles Proffitt and Denise Taylor of STScI for their aid in planning the observations with HST. Support for program #12288 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. This material is also based upon work supported by the National Science Foundation under Grant No. AST-1411654. Institutional support has been provided from a GSU ACI Fellowship (RAM), the GSU College of Arts and Sciences, and the Research Program Enhancement fund of the Board of Regents of the University System of Georgia, administered through the GSU Office of the Vice President for Research and Economic Development. 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 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2015 VL 806 IS 2 AR 155 DI 10.1088/0004-637X/806/2/155 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500010 ER PT J AU Melnick, GJ Kaufman, MJ AF Melnick, Gary J. Kaufman, Michael J. TI O-2 EMISSION TOWARD ORION H-2 PEAK 1 AND THE ROLE OF FUV-ILLUMINATED C-SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual objects (Orion) ID RHO-OPHIUCHI CLOUD; MOLECULAR CLOUDS; THERMAL BALANCE; WATER MASER; EXCITATION; ABUNDANCE; WAVES; BAR; SATELLITE; ASTRONOMY AB Molecular oxygen (O-2) has been the target of ground-based and space-borne searches for decades. Of the thousands of lines of sight surveyed, only those toward Rho Ophiuchus and Orion H-2 Peak 1 have yielded detections of any statistical significance. The detection of the O-2 N-J = 3(3)-1(2) and 5(4)-3(4) lines at 487.249 GHz and 773.840 GHz, respectively, toward Rho Ophiuchus has been attributed to a short-lived peak in the time-dependent, cold-cloud O-2 abundance, while the detection of the O-2 NJ = 33-12, 54-34 lines, plus the 7(6)-5(6) line at 1120.715 GHz, toward Orion has been ascribed to time-dependent preshock physical and chemical evolution and low-velocity (12 km s(-1)) non-dissociative C-type shocks, both of which are fully shielded from far-ultraviolet (FUV) radiation, plus a postshock region that is exposed to an FUV field. We report a re-interpretation of the Orion O-2 detection based on new C-type shock models that fully incorporate the significant effects the presence of even a weak FUV field can have on the preshock gas, shock structure, and postshock chemistry. In particular, we show that a family of solutions exists, depending on the FUV intensity, that reproduces both the observed O-2 intensities and O-2 line ratios. The solution in closest agreement with the shock parameters inferred for H-2 Peak 1 from other gas tracers assumes a 23 km s(-1) shock impacting gas with a preshock density of 8 x 104 cm-3 and Go = 1, substantially different from that inferred for the fully. shielded shock case. As pointed out previously, the similarity between the LSR velocity of all three O-2 lines (approximate to 11 km s(-1)) and recently measured H2O 5(32)-4(41) maser emission at 620.701 GHz toward H-2 Peak 1 suggests that the O-2 emission arises behind the same shocks responsible for the maser emission, though the O-2 emission is almost certainly more extended than the localized high-density maser spots. Since maser emission arises along lines of sight of low-velocity gradient, indicating shock motion largely perpendicular to our line of sight, we note that this geometry can explain not only. the narrow (less than or similar to 3 km s(-1)) observed O-2 line widths despite their excitation behind a shock. but also why such O-2 detections are rare. C1 [Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kaufman, Michael J.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. RP Melnick, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NNX13AF16G] FX We wish to acknowledge helpful discussions with Paul Goldsmith. This work was supported by NASA through Astrophysics Data Analysis Program grant No. NNX13AF16G. NR 34 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 JUN 20 PY 2015 VL 806 IS 2 AR 227 DI 10.1088/0004-637X/806/2/227 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500082 ER PT J AU Metzger, BD Williams, PKG Berger, E AF Metzger, Brian D. Williams, P. K. G. Berger, Edo TI EXTRAGALACTIC SYNCHROTRON TRANSIENTS IN THE ERA OF WIDE-FIELD RADIO SURVEYS. I. DETECTION RATES AND LIGHT CURVE CHARACTERISTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; radio continuum: general; supernovae: general; surveys ID GAMMA-RAY BURSTS; ALLEN TELESCOPE ARRAY; STAR-FORMATION RATE; STELLAR TIDAL DISRUPTION; BINARY NEUTRON-STARS; MASSIVE BLACK-HOLE; MILLISECOND MAGNETAR; GRAVITATIONAL-WAVES; LUMINOSITY FUNCTION; EXTENDED EMISSION AB The impending era of wide-field radio surveys has the potential to revolutionize our understanding of astrophysical transients. Here we evaluate the prospects of a wide range of planned and hypothetical radio surveys using the properties and volumetric rates of known and hypothetical classes of extragalactic synchrotron radio transients (e.g., on-axis and off-axis gamma-ray bursts (GRBs), supernovae, tidal disruption events, compact object mergers). Utilizing these sources and physically motivated considerations we assess the allowed phase space of radio luminosity and peak timescale for extragalactic transients. We also include for the first time effects such as redshift evolution of the rates, K-corrections, and non-Euclidean luminosity distance, which affect the detection rates of the most sensitive surveys. The number of detected events is calculated by means of a Monte Carlo method, using the various survey properties (depth, cadence, area) and realistic detection criteria that include a cut on the minimum variability of the transients during the survey and an assessment of host galaxy contamination. We find that near-term GHz frequency surveys (ASKAP/VAST, Very Large Array Sky Survey) will detect few events: <= 30-50 on-and off-axis long GRBs (LGRBs) and off-axis tidal disruption events, and similar to 50-100 neutron star binary mergers if similar to 0.5% of the mergers result in a stable millisecond magnetar. Low-frequency surveys (e.g., LOFAR) are unlikely to detect any transients, while a hypothetical large-scale mm survey may detect similar to 40 on-axis LGRBs. On the other hand, we find that SKA1 surveys at similar to 0.1-1GHz have the potential to uncover thousands of transients, mainly on-axis and off-axis LGRBs, on-axis short GRBs, off-axis TDEs, and neutron star binary mergers with magnetar remnants. C1 [Metzger, Brian D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Williams, P. K. G.; Berger, Edo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Metzger, BD (reprint author), Columbia Univ, Columbia Astrophys Lab, Pupin Hall, New York, NY 10027 USA. EM bmetzger@phys.columbia.edu; pwilliams@cfa.harvard.edu; eberger@cfa.harvard.edu OI Williams, Peter/0000-0003-3734-3587 FU NASA [NNX14AQ68G]; NSF [AST-1410950]; Alfred P. Sloan Foundation FX This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System. B.D.M. acknowledges helpful conversations with Bradley Johnson, Dimitrios Giannios, Glenn Jones, Peter Mimica, and Ashley Zauderer. We thank Aleksey Generozov for technical assistance and Rodolfo Barniol-Duran for providing LLGRB light curve models. B.D.M. gratefully acknowledges support from NASA Fermi grant NNX14AQ68G, NSF grant AST-1410950, and the Alfred P. Sloan Foundation. NR 136 TC 19 Z9 19 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 JUN 20 PY 2015 VL 806 IS 2 AR 224 DI 10.1088/0004-637X/806/2/224 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500079 ER PT J AU Morganson, E Green, PJ Anderson, SF Ruan, JJ Myers, AD Eracleous, M Kelly, B Badenes, C Banados, E Blanton, MR Bershady, MA Borissova, J Brandt, WN Burgett, WS Chambers, K Draper, PW Davenport, JRA Flewelling, H Garnavich, P Hawley, SL Hodapp, KW Isler, JC Kaiser, N Kinemuchi, K Kudritzki, RP Metcalfe, N Morgan, JS Paris, I Parvizi, M Poleski, R Price, PA Salvato, M Shanks, T Schlafly, EF Schneider, DP Shen, Y Stassun, K Tonry, JT Walter, F Waters, CZ AF Morganson, Eric Green, Paul J. Anderson, Scott F. Ruan, John J. Myers, Adam D. Eracleous, Michael Kelly, Brandon Badenes, Carlos Banados, Eduardo Blanton, Michael R. Bershady, Matthew A. Borissova, Jura Brandt, William Nielsen Burgett, William S. Chambers, Kenneth Draper, Peter W. Davenport, James R. A. Flewelling, Heather Garnavich, Peter Hawley, Suzanne L. Hodapp, Klaus W. Isler, Jedidah C. Kaiser, Nick Kinemuchi, Karen Kudritzki, Rolf P. Metcalfe, Nigel Morgan, Jeffrey S. Paris, Isabelle Parvizi, Mahmoud Poleski, Radoslaw Price, Paul A. Salvato, Mara Shanks, Tom Schlafly, Eddie F. Schneider, Donald P. Shen, Yue Stassun, Keivan Tonry, John T. Walter, Fabian Waters, Chris Z. TI THE TIME DOMAIN SPECTROSCOPIC SURVEY: VARIABLE SELECTION AND ANTICIPATED RESULTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: supermassive black holes; stars: variables: general; surveys ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; MAIN-SEQUENCE STARS; SURVEY STRIPE 82; RR LYRAE STARS; DATA RELEASE; VARIABILITY SURVEY; SDSS-III; RADIAL-VELOCITY; CATACLYSMIC VARIABLES AB We present the selection algorithm and anticipated results for the Time Domain Spectroscopic Survey (TDSS). TDSS is an Sloan Digital Sky Survey (SDSS)-IV Extended Baryon Oscillation Spectroscopic Survey (eBOSS) subproject that will provide initial identification spectra of approximately 220,000 luminosity-variable objects (variable stars and active galactic nuclei across 7500 deg(2) selected from a combination of SDSS and multi-epoch Pan-STARRS1 photometry. TDSS will be the largest spectroscopic survey to explicitly target variable objects, avoiding pre-selection on the basis of colors or detailed modeling of specific variability characteristics. Kernel Density Estimate analysis of our target population performed on SDSS Stripe 82 data suggests our target sample will be 95% pure (meaning 95% of objects we select have genuine luminosity variability of a few magnitudes or more). Our final spectroscopic sample will contain roughly 135,000 quasars and 85,000 stellar variables, approximately 4000 of which will be RR Lyrae stars which may be used as outer Milky Way probes. The variability-selected quasar population has a smoother redshift distribution than a color-selected sample, and variability measurements similar to those we develop here may be used to make more uniform quasar samples in large surveys. The stellar variable targets are distributed fairly uniformly across color space, indicating that TDSS will obtain spectra for a wide variety of stellar variables including pulsating variables, stars with significant chromospheric activity, cataclysmic variables, and eclipsing binaries. TDSS will serve as a pathfinder mission to identify and characterize the multitude of variable objects that will be detected photometrically in even larger variability surveys such as Large Synoptic Survey Telescope. C1 [Morganson, Eric; Green, Paul J.; Isler, Jedidah C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Anderson, Scott F.; Ruan, John J.; Davenport, James R. A.; Hawley, Suzanne L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Eracleous, Michael; Brandt, William Nielsen; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Kelly, Brandon] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Badenes, Carlos] Univ Pittsburgh, Astrophys & Cosmol Ctr PITT PACC, Dept Phys & Astron & Pittsburgh Particle Phys, Pittsburgh, PA 15260 USA. [Banados, Eduardo; Schlafly, Eddie F.; Walter, Fabian] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Blanton, Michael R.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Bershady, Matthew A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Borissova, Jura] Univ Valparaiso, Inst Fis & Astron, Santiago, Chile. [Borissova, Jura] Millennium Inst Astrophys MAS, Santiago, Chile. [Burgett, William S.; Kaiser, Nick] GMTO Corp, Pasadena, CA 91101 USA. [Chambers, Kenneth; Flewelling, Heather; Hodapp, Klaus W.; Kudritzki, Rolf P.; Metcalfe, Nigel; Tonry, John T.; Waters, Chris Z.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Draper, Peter W.; Shanks, Tom] Univ Durham, Sci Labs, Dept Phys, Durham DH1 3LE, England. [Garnavich, Peter] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Isler, Jedidah C.] Syracuse Univ, Syracuse, NY 13244 USA. [Kinemuchi, Karen] Apache Point Observ, Sunspot, NM 88349 USA. [Paris, Isabelle] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Parvizi, Mahmoud; Stassun, Keivan] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Poleski, Radoslaw] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Price, Paul A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Salvato, Mara] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. [Shen, Yue] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Morganson, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM emorganson@cfa.harvard.edu RI Brandt, William/N-2844-2015; OI Brandt, William/0000-0002-0167-2453; Banados, Eduardo/0000-0002-2931-7824; Badenes, Carles/0000-0003-3494-343X; Davenport, James/0000-0002-0637-835X; Chambers, Kenneth /0000-0001-6965-7789; Schlafly, Edward Ford/0000-0002-3569-7421 FU Alfred P. Sloan Foundation; Center for High-Performance Computing at the University of Utah; Carnegie Institution for Science, Carnegie Mellon University; 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; 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; Yale University; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877] FX Funding for the SDSS-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 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, 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 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, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, 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). We thank Don York for many discussions, spanning a number of years, related to the combined SDSS and PS scientific potential, and we thank Tim Heckman for his support linking the two surveys through TDSS. We gratefully acknowledge help with candidate visual inspection provided by Jerica Green (SAO) and Caroline Scott (Imperial). NR 103 TC 13 Z9 13 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 JUN 20 PY 2015 VL 806 IS 2 AR 244 DI 10.1088/0004-637X/806/2/244 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500099 ER PT J AU Myers, PC AF Myers, Philip C. TI CHARACTERISTIC STRUCTURE OF STAR-FORMING CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; stars: formation ID PROBABILITY-DISTRIBUTION FUNCTIONS; TURBULENT MAGNETIZED CLOUDS; GIANT MOLECULAR CLOUD; INITIAL MASS FUNCTION; DENSITY DISTRIBUTION; DUST EXTINCTION; CORES; PROTOSTARS; FILAMENTS; HERSCHEL AB This paper presents a new method to diagnose the star-forming potential of a molecular cloud region from the probability density function of its column density (N-pdf). This method provides expressions for the column density and mass profiles of a symmetric filament having the same N-pdf as a filamentary region. The central concentration of this characteristic filament can distinguish regions and can quantify their fertility for star formation. Profiles are calculated for N-pdfs which are pure lognormal, pure power law, or a combination. In relation to models of singular polytropic cylinders, characteristic filaments can be unbound, bound, or collapsing depending on their central concentration. Such filamentary models of the dynamical state of N-pdf gas are more relevant to star-forming regions than are spherical collapse models. The star formation fertility of a bound or collapsing filament is quantified by its mean mass accretion rate when in radial free fall. For a given mass per length, the fertility increases with the filament mean column density and with its initial concentration. In selected regions the fertility of their characteristic filaments increases with the level of star formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmyers@cfa.harvard.edu NR 71 TC 3 Z9 3 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 226 DI 10.1088/0004-637X/806/2/226 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500081 ER PT J AU Samanta, T Banerjee, D Tian, H AF Samanta, Tanmoy Banerjee, Dipankar Tian, Hui TI QUASI-PERIODIC OSCILLATION OF A CORONAL BRIGHT POINT SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: magnetic fields; Sun: oscillations; Sun: transition region; Sun: UV radiation ID MAGNETIC-FIELD; SOLAR CORONA; TEMPORAL VARIATIONS; EXPLOSIVE EVENTS; ACTIVE-REGION; INTENSITY OSCILLATIONS; ACOUSTIC-OSCILLATIONS; SIGNATURE; SCALE; RECONNECTION AB Coronal bright points (BPs) are small-scale luminous features seen in the solar corona. Quasi-periodic brightenings are frequently observed in the BPs and are generally linked with underlying magnetic flux changes. We study the dynamics of a BP seen in the coronal hole using the Atmospheric Imaging Assembly images, the Helioseismic and Magnetic Imager magnetogram on board the Solar Dynamics Observatory, and spectroscopic data from the newly launched Interface Region Imaging Spectrograph (IRIS). The detailed analysis shows that the BP evolves throughout our observing period along with changes in underlying photospheric magnetic flux and shows periodic brightenings in different EUV and far-UV images. With the highest possible spectral and spatial resolution of IRIS, we attempted to identify the sources of these oscillations. IRIS sit-and-stare observation provided a unique opportunity to study the time evolution of one footpoint of the BP as the slit position crossed it. We noticed enhanced line profile asymmetry, enhanced line width, intensity enhancements, and large deviation from the average Doppler shift in the line profiles at specific instances, which indicate the presence of sudden flows along the line-of-sight direction. We propose that transition region explosive events originating from small-scale reconnections and the reconnection outflows are affecting the line profiles. The correlation between all these parameters is consistent with the repetitive reconnection scenario and could explain the quasi-periodic nature of the brightening. C1 [Samanta, Tanmoy; Banerjee, Dipankar] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Tian, Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Samanta, T (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. EM tsamanta@iiap.res.in; hui.tian@cfa.harvard.edu RI Banerjee, Dipankar/B-9129-2009 OI Banerjee, Dipankar/0000-0003-4653-6823 FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX; Lockheed-Martin [8100002705, SP02H1701R] FX We thank the IRIS team for providing the data in the public domain. 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. H. T. is supported by contracts 8100002705 and SP02H1701R from Lockheed-Martin to SAO. NR 49 TC 6 Z9 6 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 172 DI 10.1088/0004-637X/806/2/172 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500027 ER PT J AU Schmelz, JT Asgari-Targhi, M Christian, GM Dhaliwal, RS Pathak, S AF Schmelz, J. T. Asgari-Targhi, M. Christian, G. M. Dhaliwal, R. S. Pathak, S. TI HOT PLASMA FROM SOLAR ACTIVE REGION CORES: A TEST OF AC AND DC CORONAL HEATING MODELS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; Sun: UV radiation ID ALFVEN-WAVE TURBULENCE; X-RAY TELESCOPE; FIELD TEMPERATURE DISTRIBUTIONS; EUV IMAGING SPECTROMETER; MAGNETOHYDRODYNAMIC TURBULENCE; FOOTPOINT MOTIONS; TRANSITION-REGION; ATOMIC DATABASE; ENERGY-RELEASE; LOOPS AB Direct current (DC) models of solar coronal heating invoke magnetic reconnection to convert magnetic free energy into heat, whereas alternating current (AC) models invoke wave dissipation. In both cases the energy is supplied by photospheric footpoint motions. For a given footpoint velocity amplitude, DC models predict lower average heating rates but greater temperature variability when compared to AC models. Therefore, evidence of hot plasma (T > 5MK) in the cores of active regions could be one of the ways for current observations to distinguish between AC and DC models. We have analyzed data from the X-Ray Telescope (XRT) and the Atmospheric Imaging Assembly for 12 quiescent active region cores, all of which were observed in the XRT Be_thick channel. We did Differential Emission Measure (DEM) analysis and achieved good fits for each data set. We then artificially truncated the hot plasma of the DEM model at 5MK and examined the resulting fits to the data. For some regions in our sample, the XRT intensities continued to be well-matched by the DEM predictions, even without the hot plasma. This truncation, however, resulted in unacceptable fits for the other regions. This result indicates that the hot plasma is present in these regions, even if the precise DEM distribution cannot be determined with the data available. We conclude that reconnection may be heating the hot plasma component of these active regions. C1 [Schmelz, J. T.; Christian, G. M.; Dhaliwal, R. S.; Pathak, S.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Asgari-Targhi, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu FU NASA/SAO FX 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). The Atmospheric Imaging Assembly on the Solar Dynamics Observatory is part of NASA's Living with a Star program. CHIANTI is a collaborative project involving the NRL (USA), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). Solar physics research at the University of Memphis is supported by a Hinode subcontract from NASA/SAO. NR 75 TC 3 Z9 3 U1 1 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 JUN 20 PY 2015 VL 806 IS 2 AR 232 DI 10.1088/0004-637X/806/2/232 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500087 ER PT J AU Urata, Y Huang, KY Yamazaki, R Sakamoto, T AF Urata, Yuji Huang, Kuiyun Yamazaki, Ryo Sakamoto, Takanori TI EXTREMELY SOFT X-RAY FLASH AS THE INDICATOR OF OFF-AXIS ORPHAN GRB AFTERGLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: flare; gamma-ray burst: general; supernovae: general ID JET MODELS; BURSTS; SPECTRA; EMISSION; DESIGN; ENERGY; SWIFT; FIELD; PERFORMANCE; XRF-020903 AB We verified the off-axis jet model of X-ray flashes (XRFs) and examined a discovery of off-axis orphan gammaray burst (GRB) afterglows. The XRF sample was selected on the basis of the following three factors: (1) a constraint on the lower peak energy of the prompt spectrum E-obs(src), (2) redshift measurements, and (3) multicolor observations of an earlier (or brightening) phase. XRF 020903 was the only sample selected on the basis of these criteria. A complete optical multicolor afterglow light curve of XRF 020903 obtained from archived data and photometric results in the literature showed an achromatic brightening around 0.7 days. An off-axis jet model with a large observing angle (0.21 rad, which is twice the jet opening half-angle, theta(jet)) can naturally describe the achromatic brightening and the prompt X-ray spectral properties. This result indicates the existence of off-axis orphan GRB afterglow light curves. Events with a larger viewing angle (> similar to 2 theta(jet)) could be discovered using an 8 m class telescope with wide-field imagers such as the Subaru Hyper-Suprime-Cam and the Large Synoptic Survey Telescope. C1 [Urata, Yuji] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Huang, Kuiyun] Natl Taiwan Normal Univ, Dept Math & Sci, New Taipei City 24449, Taiwan. [Yamazaki, Ryo; Sakamoto, Takanori] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Yamazaki, Ryo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Urata, Y (reprint author), Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. EM urata@astro.ncu.edu.tw FU Ministry of Education, Science, Sports, and Culture (MEXT), Japan [15K05088, 25400234]; Ministry of Science and Technology of Taiwan [NSC 100-2112-M-008-007-MY3, MOST103-2112-M-008-021-(YU)]; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G] FX This work was supported in part by Grant-in-Aid for scientific research from the Ministry of Education, Science, Sports, and Culture (MEXT), Japan, No. 15K05088 (R.Y.) and No. 25400234 (T.S.). This work is partly supported by the Ministry of Science and Technology of Taiwan grants NSC 100-2112-M-008-007-MY3 and MOST103-2112-M-008-021-(YU). Subaru Suprime-Cam data were acquired through SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. 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, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. NR 63 TC 2 Z9 2 U1 0 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 JUN 20 PY 2015 VL 806 IS 2 AR 222 DI 10.1088/0004-637X/806/2/222 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500077 ER PT J AU Weisz, DR Johnson, LC Foreman-Mackey, D Dolphin, AE Beerman, LC Williams, BF Dalcanton, JJ Rix, HW Hogg, DW Fouesneau, M Johnson, BD Bell, EF Boyer, ML Gouliermis, D Guhathakurta, P Kalirai, JS Lewis, AR Seth, AC Skillman, ED AF Weisz, Daniel R. Johnson, L. Clifton Foreman-Mackey, Daniel Dolphin, Andrew E. Beerman, Lori C. Williams, Benjamin F. Dalcanton, Julianne J. Rix, Hans-Walter Hogg, David W. Fouesneau, Morgan Johnson, Benjamin D. Bell, Eric F. Boyer, Martha L. Gouliermis, Dimitrios Guhathakurta, Puragra Kalirai, Jason S. Lewis, Alexia R. Seth, Anil C. Skillman, Evan D. TI THE HIGH-MASS STELLAR INITIAL MASS FUNCTION IN M31 CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: star clusters: general; galaxies: star formation; Hertzsprung-Russell and C-M diagrams; Local Group; stars: luminosity function, mass function ID STAR-FORMATION HISTORY; YOUNG OPEN CLUSTERS; GALAXY NGC 4214; H II REGIONS; LUMINOSITY FUNCTION; LOCAL GROUP; CHEMICAL EVOLUTION; MAGELLANIC-CLOUD; DWARF GALAXIES; DISK GALAXIES AB We have undertaken the largest systematic study of the high-mass stellar initial mass function (IMF) to date using the optical color-magnitude diagrams (CMDs) of 85 resolved, young (4 Myr < t < 25 Myr), intermediate mass star clusters (10(3)-10(4) M-circle dot), observed as part of the Panchromatic Hubble Andromeda Treasury program. We fit each cluster's CMD to measure its mass function (MF) slope for stars greater than or similar to 2 M-circle dot. By modeling the ensemble of clusters, we find the distribution of MF slopes is best described by Gamma = +1.45(-0.06)(+0.03) with a very small intrinsic scatter and no drastic outliers. This model allows the MF slope to depend on cluster mass, size, and age, but the data imply no significant dependencies within this regime of cluster properties. The lack of an age dependence suggests that the MF slope has not significantly evolved over the first similar to 25 Myr and provides direct observational evidence that the measured MF represents the IMF. Taken together, this analysis-based on an unprecedented large sample of young clusters, homogeneously constructed CMDs, well-defined selection criteria, and consistent principled modeling-implies that the high-mass IMF slope in M31 clusters is universal. The IMF has a slope (Gamma = +1.45(-0.06)(+0.03); statistical uncertainties) that is slightly steeper than the canonical Kroupa (+1.30) and Salpeter (+1.35) values, and our measurement of it represents a factor of similar to 20 improvement in precision over the Kroupa IMF (+1.30 +/- 0.7). Using our inference model on select Milky Way (MW) and LMC high-mass IMF studies from the literature, we find Gamma(MW) similar to +1.15 +/- 0.1 and Gamma(LMC) similar to +1.3 +/- 0.1, both with intrinsic scatter of similar to 0.3-0.4 dex. Thus, while the high-mass IMF in the Local Group may be universal, systematics in the literature of IMF studies preclude any definitive conclusions; homogenous investigations of the high-mass IMF in the local universe are needed to overcome this limitation. Consequently, the present study represents the most robust measurement of the high-mass IMF slope to date. To facilitate practical use over the full stellar mass spectrum, we have grafted the M31 high-mass IMF slope onto widely used sub-solar mass Kroupa and Chabrier IMFs. The increased steepness in the M31 high-mass IMF slope implies that commonly used UV- and H alpha-based star formation rates should be increased by a factor of similar to 1.3-1.5 and the number of stars with masses >8 M-circle dot is similar to 25% fewer than expected for a Salpeter/Kroupa IMF. C1 [Weisz, Daniel R.; Johnson, L. Clifton; Beerman, Lori C.; Williams, Benjamin F.; Dalcanton, Julianne J.; Lewis, Alexia R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Foreman-Mackey, Daniel; Hogg, David W.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Dolphin, Andrew E.] Raytheon Co, Tucson, AZ 85756 USA. [Rix, Hans-Walter; Hogg, David W.; Fouesneau, Morgan; Gouliermis, Dimitrios] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Johnson, Benjamin D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Boyer, Martha L.; Kalirai, Jason S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gouliermis, Dimitrios] Heidelberg Univ, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Guhathakurta, Puragra] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Skillman, Evan D.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. RP Weisz, DR (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM dweisz@uw.edu OI Gouliermis, Dimitrios/0000-0002-2763-0075; Seth, Anil/0000-0003-0248-5470; Johnson, Lent/0000-0001-6421-0953; Weisz, Daniel/0000-0002-6442-6030; Hogg, David/0000-0003-2866-9403; Bell, Eric/0000-0002-5564-9873 FU NASA from the Space Telescope Science Institute [HST GO-12055]; NASA [NAS5-26555]; NASA through Hubble Fellowship [HST-HF-51331.01]; Space Telescope Science Institute; National Science Foundation [ACI-1053575, NSF PHY11-25915] FX The authors would like to thank the anonymous referee for a careful reading of the paper and insightful comments. D.R.W. also thanks Nate Bastian, Charlie Conroy, Rob Kennicutt, and John Saclo for their useful comments on this paper and discussions about the IMF and its history. Support for this work was provided by NASA through grant number HST GO-12055 from the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS5-26555. D.R.W. is supported by NASA through Hubble Fellowship grant HST-HF-51331.01 awarded by the Space Telescope Science Institute. D.R.W. also wishes to thank the MPIA and KITP for their generous hospitality during the writing of this paper. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1053575, was supported in part by the National Science Foundation under Grant No. NSF PHY11-25915, and made extensive use of NASA's Astrophysics Data System Bibliographic Services. In large part, analysis and plots presented in this paper utilized IPython and packages from NumPy, SciPy, and Matplotlib (Hunter 2007; Oliphant 2007; Perez & Granger 2007; Astropy Collaboration et al. 2013). NR 116 TC 11 Z9 11 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 JUN 20 PY 2015 VL 806 IS 2 AR 198 DI 10.1088/0004-637X/806/2/198 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7DA UT WOS:000357129500053 ER PT J AU Kopf, A Bicak, M Kottmann, R Schnetzer, J Kostadinov, I Lehmann, K Fernandez-Guerra, A Jeanthon, C Rahav, E Ullrich, M Wichels, A Gerdts, G Polymenakou, P Kotoulas, G Siam, R Abdallah, RZ Sonnenschein, EC Cariou, T O'Gara, F Jackson, S Orlic, S Steinke, M Busch, J Duarte, B Cacador, I Canning-Clode, J Bobrova, O Marteinsson, V Reynisson, E Loureiro, CM Luna, GM Quero, GM Loscher, CR Kremp, A DeLorenzo, ME Ovreas, L Tolman, J LaRoche, J Penna, A Frischer, M Davis, T Katherine, B Meyer, CP Ramos, S Magalhaes, C Jude-Lemeilleur, F Aguirre-Macedo, ML Wang, S Poulton, N Jones, S Collin, R Fuhrman, JA Conan, P Alonso, C Stambler, N Goodwin, K Yakimov, MM Baltar, F Bodrossy, L Van De Kamp, J Frampton, DMF Ostrowski, M Van Ruth, P Malthouse, P Claus, S Deneudt, K Mortelmans, J Pitois, S Wallom, D Salter, I Costa, R Schroeder, DC Kandil, MM Amaral, V Biancalana, F Santana, R Pedrotti, ML Yoshida, T Ogata, H Ingleton, T Munnik, K Rodriguez-Ezpeleta, N Berteaux-Lecellier, V Wecker, P Cancio, I Vaulot, D Bienhold, C Ghazal, H Chaouni, B Essayeh, S Ettamimi, S Zaid, E Boukhatem, N Bouali, A Chahboune, R Barrijal, S Timinouni, M El Otmani, F Bennani, M Mea, M Todorova, N Karamfilov, V ten Hoopen, P Cochrane, G L'Haridon, S Bizsel, KC Vezzi, A Lauro, FM Martin, P Jensen, RM Hinks, J Gebbels, S Rosselli, R De Pascale, F Schiavon, R dos Santos, A Villar, E Pesant, S Cataletto, B Malfatti, F Edirisinghe, R Silveira, JAH Barbier, M Turk, V Tinta, T Fuller, WJ Salihoglu, I Serakinci, N Ergoren, MC Bresnan, E Iriberri, J Nyhus, PAF Bente, E Karlsen, HE Golyshin, PN Gasol, JM Moncheva, S Dzhembekova, N Johnson, Z Sinigalliano, CD Gidley, ML Zingone, A Danovaro, R Tsiamis, G Clark, MS Costa, AC El Bour, M Martins, AM Collins, RE Ducluzeau, AL Martinez, J Costello, MJ Amaral-Zettler, LA Gilbert, JA Davies, N Field, D Glockner, FO AF Kopf, Anna Bicak, Mesude Kottmann, Renzo Schnetzer, Julia Kostadinov, Ivaylo Lehmann, Katja Fernandez-Guerra, Antonio Jeanthon, Christian Rahav, Eyal Ullrich, Matthias Wichels, Antje Gerdts, Gunnar Polymenakou, Paraskevi Kotoulas, Giorgos Siam, Rania Abdallah, Rehab Z. Sonnenschein, Eva C. Cariou, Thierry O'Gara, Fergal Jackson, Stephen Orlic, Sandi Steinke, Michael Busch, Julia Duarte, Bernardo Cacador, Isabel Canning-Clode, Joao Bobrova, Oleksandra Marteinsson, Viggo Reynisson, Eyjolfur Loureiro, Clara Magalhaes Luna, Gian Marco Quero, Grazia Marina Loescher, Carolin R. Kremp, Anke DeLorenzo, Marie E. Ovreas, Lise Tolman, Jennifer LaRoche, Julie Penna, Antonella Frischer, Marc Davis, Timothy Katherine, Barker Meyer, Christopher P. Ramos, Sandra Magalhaes, Catarina Jude-Lemeilleur, Florence Leopoldina Aguirre-Macedo, Ma Wang, Shiao Poulton, Nicole Jones, Scott Collin, Rachel Fuhrman, Jed A. Conan, Pascal Alonso, Cecilia Stambler, Noga Goodwin, Kelly Yakimov, Michael M. Baltar, Federico Bodrossy, Levente Van De Kamp, Jodie Frampton, Dion M. F. Ostrowski, Martin Van Ruth, Paul Malthouse, Paul Claus, Simon Deneudt, Klaas Mortelmans, Jonas Pitois, Sophie Wallom, David Salter, Ian Costa, Rodrigo Schroeder, Declan C. Kandil, Mahrous M. Amaral, Valentina Biancalana, Florencia Santana, Rafael Pedrotti, Maria Luiza Yoshida, Takashi Ogata, Hiroyuki Ingleton, Tim Munnik, Kate Rodriguez-Ezpeleta, Naiara Berteaux-Lecellier, Veronique Wecker, Patricia Cancio, Ibon Vaulot, Daniel Bienhold, Christina Ghazal, Hassan Chaouni, Bouchra Essayeh, Soumya Ettamimi, Sara Zaid, El Houcine Boukhatem, Noureddine Bouali, Abderrahim Chahboune, Rajaa Barrijal, Said Timinouni, Mohammed El Otmani, Fatima Bennani, Mohamed Mea, Marianna Todorova, Nadezhda Karamfilov, Ventzislav ten Hoopen, Petra Cochrane, Guy L'Haridon, Stephane Bizsel, Kemal Can Vezzi, Alessandro Lauro, Federico M. Martin, Patrick Jensen, Rachelle M. Hinks, Jamie Gebbels, Susan Rosselli, Riccardo De Pascale, Fabio Schiavon, Riccardo dos Santos, Antonina Villar, Emilie Pesant, Stephane Cataletto, Bruno Malfatti, Francesca Edirisinghe, Ranjith Silveira, Jorge A. Herrera Barbier, Michele Turk, Valentina Tinta, Tinkara Fuller, Wayne J. Salihoglu, Ilkay Serakinci, Nedime Ergoren, Mahmut Cerkez Bresnan, Eileen Iriberri, Juan Nyhus, Paul Anders Fronth Bente, Edvardsen Karlsen, Hans Erik Golyshin, Peter N. Gasol, Josep M. Moncheva, Snejana Dzhembekova, Nina Johnson, Zackary Sinigalliano, Christopher David Gidley, Maribeth Louise Zingone, Adriana Danovaro, Roberto Tsiamis, George Clark, Melody S. Costa, Ana Cristina El Bour, Monia Martins, Ana M. Collins, R. Eric Ducluzeau, Anne-Lise Martinez, Jonathan Costello, Mark J. Amaral-Zettler, Linda A. Gilbert, Jack A. Davies, Neil Field, Dawn Gloeckner, Frank Oliver TI The ocean sampling day consortium SO GIGASCIENCE LA English DT Editorial Material DE Ocean sampling day; OSD; Biodiversity; Genomics; Health Index; Bacteria; Microorganism; Metagenomics; Marine; Micro B3; Standards ID GLOBAL OCEAN AB Ocean Sampling Day was initiated by the EU-funded Micro B3 (Marine Microbial Biodiversity, Bioinformatics, Biotechnology) project to obtain a snapshot of the marine microbial biodiversity and function of the world's oceans. It is a simultaneous global mega-sequencing campaign aiming to generate the largest standardized microbial data set in a single day. This will be achievable only through the coordinated efforts of an Ocean Sampling Day Consortium, supportive partnerships and networks between sites. This commentary outlines the establishment, function and aims of the Consortium and describes our vision for a sustainable study of marine microbial communities and their embedded functional traits. C1 [Kopf, Anna; Kottmann, Renzo; Schnetzer, Julia; Fernandez-Guerra, Antonio; Bienhold, Christina; Gloeckner, Frank Oliver] Max Planck Inst Marine Microbiol, D-28359 Bremen, Germany. [Kopf, Anna; Schnetzer, Julia; Kostadinov, Ivaylo; Ullrich, Matthias; Mea, Marianna; Davies, Neil; Field, Dawn; Gloeckner, Frank Oliver] Jacobs Univ Bremen gGmbH, D-28759 Bremen, Germany. [Bicak, Mesude; Fernandez-Guerra, Antonio; Wallom, David; Field, Dawn] Univ Oxford, Oxford OX1 3QG, Oxon, England. [Lehmann, Katja] Ctr Ecol & Hydrol, Wallingford OX10 8BB, Oxon, England. [Jeanthon, Christian; Cariou, Thierry; Vaulot, Daniel] Univ Paris 06, CNRS, Stn Biol, F-29680 Roscoff, France. [Jeanthon, Christian; Cariou, Thierry; Vaulot, Daniel] Univ Paris 06, Sorbonne Univ, Stn Biol, F-29680 Roscoff, France. [Rahav, Eyal] Natl Inst Oceanog, Israel Oceanog & Limnol Res, IL-31080 Haifa, Israel. [Wichels, Antje; Gerdts, Gunnar] Biol Anstalt Helgoland, Alfred Wegener Inst, D-27498 Helgoland, Germany. [Polymenakou, Paraskevi; Kotoulas, Giorgos] Hellen Ctr Marine Res, Inst Marine Biol Biotechnol & Aquaculture, Iraklion 71500, Crete, Greece. [Siam, Rania; Abdallah, Rehab Z.] Amer Univ Cairo, Biol Dept, New Cairo 11835, Cairo Governora, Egypt. [Siam, Rania; Abdallah, Rehab Z.] Amer Univ Cairo, YJ Sci & Technol Res Ctr, New Cairo 11835, Cairo Governora, Egypt. [Sonnenschein, Eva C.; Jackson, Stephen] Tech Univ Denmark, Dept Syst Biol, DK-2800 Lyngby, Denmark. [O'Gara, Fergal] Natl Univ Ireland Univ Coll Cork, Cork, Ireland. [O'Gara, Fergal] Curtin Univ, Biomed Sci, Perth, WA 6845, Australia. [Villar, Emilie] Aix Marseille Univ, CNRS, UMR 7256, IGS, F-13288 Marseille, France. [Orlic, Sandi] Rudjer Boskovic Inst, Zagreb 10000, Croatia. [Steinke, Michael] Univ Essex, Sch Biol Sci, Colchester CO4 3SQ, Essex, England. [Busch, Julia] Carl von Ossietzky Univ Oldenburg, Inst Chem & Biol Marine Environm ICBM, D-26383 Wilhemshaven, Germany. [Duarte, Bernardo; Cacador, Isabel; Canning-Clode, Joao] Univ Lisbon, Fac Sci, Marine & Environm Sci Ctr, P-1749016 Lisbon, Portugal. [Canning-Clode, Joao] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Bobrova, Oleksandra] Odessa Natl II Mechnikov Univ, Dept Microbiol Virol & Biotechnol, UA-65082 Odessa, Ukraine. [Marteinsson, Viggo; Reynisson, Eyjolfur] Matis Ltd, IS-113 Reykjavik, Iceland. [Loureiro, Clara Magalhaes; Costa, Ana Cristina; Martins, Ana M.] Univ Acores, Dept Biol, InBio CIBIO, P-9501801 Ponta Delgada, Portugal. [Luna, Gian Marco; Quero, Grazia Marina] Inst Marine Sci CNR ISMAR, Natl Res Council, I-30122 Venice, Italy. [Loescher, Carolin R.] GEOMAR, Inst Microbiol, D-24118 Kiel, Germany. [Kremp, Anke] Finnish Environm Inst, Marine Res Ctr, Helsinki 00560, Finland. [DeLorenzo, Marie E.] NOAA, Natl Ocean Serv, NCCOS, Ctr Coastal Environm Hlth & Biomol Res, Charleston, SC 29412 USA. [Ovreas, Lise] Univ Bergen, Dept Biol, N-5020 Bergen, Norway. [Tolman, Jennifer; LaRoche, Julie] Dalhousie Univ, LaRoche Res Grp, Dept Biol, Halifax, NS B3H 4R2, Canada. [Penna, Antonella] Univ Urbino, Dept Biomol Sci, I-61121 Pesaro, Italy. [Frischer, Marc] Univ Georgia, Skidaway Inst Oceanog, Savannah, GA 31411 USA. [Davis, Timothy] NOAA, Great Lakes Environm Res Lab, Ann Arbor, MI 48108 USA. [Katherine, Barker; Meyer, Christopher P.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Ramos, Sandra; Magalhaes, Catarina] Univ Porto, Interdisciplinary Ctr Environm & Marine Res, CIIMAR, P-4050123 Oporto, Portugal. [Jude-Lemeilleur, Florence] CNRS, Stn Marine Arcachon, F-33120 Arcachon, France. [Jude-Lemeilleur, Florence] Univ Bordeaux, F-33120 Arcachon, France. [Leopoldina Aguirre-Macedo, Ma] Ctr Invest & Estudios Avanzados CINVESTAV, Unidad Merida, Yucatan 97310, Mexico. [Wang, Shiao; Silveira, Jorge A. Herrera] Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. [Poulton, Nicole] Bigelow Lab Ocean Sci, East Boothbay, ME 04544 USA. [Jones, Scott] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Collin, Rachel] Smithsonian Trop Res Inst, Balboa Ancon, Panama. [Fuhrman, Jed A.] Univ So Calif, Wrigley Inst Environm Studies, Los Angeles, CA 90089 USA. [Fuhrman, Jed A.] Univ So Calif, Dept Biol Sci, Los Angeles, CA 90089 USA. [Conan, Pascal; Salter, Ian] Univ Paris 06, Sorbonne Univ, CNRS, UMR7621,Lab Oceanog Microbienne,Observ Oceanol, F-66651 Banyuls Sur Mer, France. [Alonso, Cecilia; Amaral, Valentina; Santana, Rafael] Univ Republ, Ctr Univ Reg Este, Microbial Ecol Aquat Transit Syst Res Grp, Rocha, Uruguay. [Stambler, Noga] Bar Ilan Univ, Mina & Everard Goodman Fac Life Sci, IL-5290002 Ramat Gan, Israel. [Stambler, Noga] Interuniv Inst Marine Sci Eilat, IL-88103 Elat, Israel. [Stambler, Noga] NOAA, Atlantic Oceanog & Meteorol Lab, Ocean Chem & Ecosyst Div, Miami, FL 33149 USA. [Yakimov, Michael M.] CNR, IAMC, Inst Coastal Marine Environm, I-98122 Messina, Sicily, Italy. [Baltar, Federico] Univ Otago, Dept Marine Sci, Dunedin 9054, New Zealand. [Bodrossy, Levente; Van De Kamp, Jodie; Frampton, Dion M. F.] CSIRO Oceans & Atmosphere Flagship, Hobart, Tas 7000, Australia. [Ostrowski, Martin] Macquarie Univ, Dept Chem & Biomol Sci, Sydney, NSW 2109, Australia. [Van Ruth, Paul; Malthouse, Paul] South Australian Res & Dev Inst SARDI Aquat Sci, Henley Beach, SA 5022, Australia. [Claus, Simon; Deneudt, Klaas; Mortelmans, Jonas] Flanders Marine Inst, B-8400 Oostende, Belgium. [Pitois, Sophie] Ctr Environm Fisheries & Aquaculture Sci CEFAS, Lowestoft NR33 0HT, Suffolk, England. [Salter, Ian; Bienhold, Christina] Helmholtz Zentrum Polar & Meeresforsch, Alfred Wegener Inst, D-27570 Bremerhaven, Germany. [Costa, Rodrigo] Univ Algarve, Ctr Marine Sci, Microbial Ecol & Evolut Res Grp, P-8005139 Faro, Portugal. [Schroeder, Declan C.] Marine Biol Assoc UK, Plymouth, Devon, England. [Kandil, Mahrous M.] Univ Alexandria, Fac Agr, Soil & Water Sci Dept, Alexandria 21545, Egypt. [Pedrotti, Maria Luiza] Univ Paris 06, Univ Paris 04, CNRS, UMR 7093,LOV,Observ Oceanol, Paris, France. [Biancalana, Florencia] Argentine Inst Oceanog, Marine Biogeochem, RA-8000 Bahia Blanca, Buenos Aires, Argentina. [Yoshida, Takashi; Ogata, Hiroyuki] Kyoto Univ, Grad Sch Agr, Sakyo Ku, Kyoto 6068502, Japan. [dos Santos, Antonina] IPMA, Dept Sea & Marine Resources, P-1449006 Lisbon, Portugal. [Ingleton, Tim] New South Wales Off Environm & Heritage, Waters Wetlands & Coasts, Sydney, NSW, Australia. [Munnik, Kate] Lwandle Technol, Cape Town, South Africa. [Rodriguez-Ezpeleta, Naiara] AZTI, Marine Res Div, Sukarrieta 48395, Bizkaia, Spain. [Berteaux-Lecellier, Veronique; Wecker, Patricia] UPVD, EPHE, CNRS, CRIOBE,USR3278,LabEx Corail, F-98729 Papetoai Moorea, Fr Polynesia. [Ingleton, Tim] Univ Tasmania, Antarctic & Southern Ocean Studies, Hobart, Tas 7004, Australia. [Cancio, Ibon; Iriberri, Juan] Univ Basque Country, E-48080 Bilbao, Basque Country, Spain. [Davies, Neil] Univ Calif Berkeley, Gump South Pacific Res Stn, Moorea 98728, Fr Polynesia. [Ghazal, Hassan; Essayeh, Soumya; Chahboune, Rajaa] Univ Mohammed Premier, Polydisciplinary Fac Nador, Selouane, Nador, Morocco. [Ghazal, Hassan; Chaouni, Bouchra; Ettamimi, Sara; Boukhatem, Noureddine; Bouali, Abderrahim] Univ Mohammed Premier, Lab Genet & Biotechnol, Oujda, Morocco. [Gilbert, Jack A.] Zhejiang Univ, Coll Environm & Resource Sci, Hangzhou 310058, Zhejiang, Peoples R China. [Ettamimi, Sara] Univ Sidi Mohammed Ben Abdallah, Polydisciplinary Fac Taza, Fes, Morocco. [Chaouni, Bouchra; Zaid, El Houcine] Univ Mohammed Fifth Rabat, Fac Sci Rabat, Rabat, Morocco. [Chahboune, Rajaa; Barrijal, Said] Univ Abdelmalek Essaadi, Fac Sci & Tech Tanger, Tanger, Morocco. [Gilbert, Jack A.] Argonne Natl Lab, Biosci Div, Inst Genom & Syst Biol, Argonne, IL 60439 USA. [Timinouni, Mohammed; Bennani, Mohamed] Pasteur Inst Morocco, Casablanca 20100, Morocco. [El Otmani, Fatima] Chouaib Doukkali Univ, Fac Sci, Dept Biol, Microbiol Hlth & Environm Team, El Jadida, Morocco. [Gilbert, Jack A.] Univ Chicago, Chicago, IL 60637 USA. [Todorova, Nadezhda; Karamfilov, Ventzislav] Bulgarian Acad Sci, Inst Biodivers & Ecosyst Res IBER, BU-1113 Sofia, Bulgaria. [ten Hoopen, Petra; Cochrane, Guy] European Bioinformat Inst EMBL EBI, European Mol Biol Lab, Cambridge CB10 1SD, Cambs, England. [L'Haridon, Stephane] UBO, UEB, IUEM, F-29280 Plouzane, France. [Bizsel, Kemal Can] Dokuz Eylul Univ DEU, Inst Marine Sci & Technol IMST, I-35340 Izmir, Balcova, Turkey. [Vezzi, Alessandro; Rosselli, Riccardo; De Pascale, Fabio; Schiavon, Riccardo] Univ Padua, Dept Biol, I-35121 Padua, Italy. [Lauro, Federico M.; Hinks, Jamie] Singapore Ctr Environm Life Sci Engn, Singapore 637551, Singapore. [Martin, Patrick] Nanyang Technol Univ, Earth Observ Singapore, Singapore 639798, Singapore. [Jensen, Rachelle M.] Indigo V Expedit, Singapore 098497, Singapore. [Gebbels, Susan] Newcastle Univ, Sch Marine Sci & Technol, Dove Marine Lab, Cullercoats NE30 4PZ, Tyne & Wear, England. [Costello, Mark J.] Univ Auckland, Inst Marine Sci, Auckland 1142, New Zealand. [Pesant, Stephane] Univ Bremen, PANGAEA Data Publisher Earth & Environm Sci, MARUM Ctr Marine Environm Sci, D-28359 Bremen, Germany. [Cataletto, Bruno; Malfatti, Francesca] Natl Inst Oceanog & Expt Geophys, OGS, I-34151 Trieste, Italy. [Edirisinghe, Ranjith] Rajarata Univ Sri Lanka, Fac Sci Appl, Dept Phys Sci, Mihintale, Sri Lanka. [Amaral-Zettler, Linda A.; Gilbert, Jack A.] Marine Biol Lab, Woods Hole, MA 02543 USA. [Amaral-Zettler, Linda A.] Brown Univ, Dept Earth Environm & Planetary Sci, Providence, RI 02912 USA. [Barbier, Michele] Mediterranean Sci Commiss, Monaco 98000, Monaco. [Turk, Valentina; Tinta, Tinkara] Natl Inst Biol, Marine Biol Stn, Piran 6330, Slovenia. [Fuller, Wayne J.; Salihoglu, Ilkay; Serakinci, Nedime; Ergoren, Mahmut Cerkez] Near East Univ, Nicosia 99138, Northern Cyprus, Cyprus. [Martins, Ana M.] Univ Azores, Dept Oceanog & Fisheries, PT-9901862 Horta, Portugal. [Collins, R. Eric; Ducluzeau, Anne-Lise] Univ Alaska Fairbanks, Fairbanks, AK 99775 USA. [Martinez, Jonathan] Univ Hawaii Manoa, Kewalo Marine Lab, Honolulu, HI 96813 USA. [Bresnan, Eileen] Marine Scotland Marine Lab, Phytoplankton Ecol, Aberdeen AB11 9DB, Aberdeen, Scotland. [El Bour, Monia] Inst Natl Sci & Technol Mer INSTM, Salammbo 2025, Tunisia. [Nyhus, Paul Anders Fronth] Kind Blue Project ABS & Citizen Sci, N-0372 Oslo, Norway. [Bente, Edvardsen] Univ Oslo, Dept Biosci, Sect Aquat Biol & Toxicol, N-0316 Oslo, Norway. [Karlsen, Hans Erik] Marine Biol Res Stn, Drobak Field Stn, N-1440 Drobak, Norway. [Golyshin, Peter N.] Bangor Univ, Coll Nat Sci, Sch Biol Sci, Bangor LL57 2UW, Gwynedd, Wales. [Gasol, Josep M.] CSIC, Inst Ciencies Mar, Dept Biol Marina & Oceanog, E-08003 Barcelona, Catalunya, Spain. [Moncheva, Snejana; Dzhembekova, Nina] Fridtjof Nansen Inst Oceanol, Varna 9000, Bulgaria. [Johnson, Zackary] Duke Univ, Nicholas Sch Environm, Beaufort, NC 28516 USA. [Johnson, Zackary] Duke Univ, Dept Biol, Beaufort, NC 28516 USA. [Gidley, Maribeth Louise] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Cooperat Inst Marine & Atmospher Sci, Miami, FL 33149 USA. [Zingone, Adriana; Danovaro, Roberto] Stn Zool Anton Dohrn, I-80121 Naples, Italy. [Danovaro, Roberto] Polytech Univ Marche, Dept Life & Environm Sci, I-60131 Ancona, Italy. [Tsiamis, George] Univ Patras, Dept Environm & Nat Resources Management, Agrinion 30100, Greece. [Clark, Melody S.] NERC, British Antarctic Survey, Cambridge CB3 0ET, Cambs, England. RP Glockner, FO (reprint author), Max Planck Inst Marine Microbiol, Celsiusstr 1, D-28359 Bremen, Germany. EM fog@mpi-bremen.de RI van de Kamp, Jodie/E-9423-2015; Costa, Rodrigo/N-7274-2013; Ramos, Sandra/I-4359-2013; Magalhaes, Catarina/A-6836-2016; Aguirre-Macedo, Ma Leopoldina/A-2511-2008; Costa, Ana Cristina/L-8023-2013; Ovreas, Lise/H-8651-2016; dos Santos, Antonina/B-9055-2011; Frampton, Dion/D-3310-2012; Goodwin, Kelly/B-4985-2014; Sonnenschein, Eva/P-4539-2016; Quero, Grazia Marina/P-9602-2016; Bodrossy, Levente/Q-3745-2016; Zingone, Adriana/E-4518-2010; Sinigalliano, Christopher/A-8760-2014; gidley, maribeth/B-8335-2014; CONAN, Pascal/B-7646-2011; Iriberri, Juan/C-3819-2017; Rodriguez-Ezpeleta, Naiara/B-7138-2014; Martin, Patrick/F-6263-2017; Davies, Neil/E-5863-2012; OI Costa, Rodrigo/0000-0002-5932-4101; Ramos, Sandra/0000-0002-4065-7651; Magalhaes, Catarina/0000-0001-9576-2398; Aguirre-Macedo, Ma Leopoldina/0000-0002-3910-8305; Costa, Ana Cristina/0000-0002-0258-3460; dos Santos, Antonina/0000-0002-2238-9315; Goodwin, Kelly/0000-0001-9583-8073; Sonnenschein, Eva/0000-0001-6959-5100; Quero, Grazia Marina/0000-0002-2562-1255; Bodrossy, Levente/0000-0001-6940-452X; Zingone, Adriana/0000-0001-5946-6532; Sinigalliano, Christopher/0000-0002-9942-238X; gidley, maribeth/0000-0001-9583-8073; CONAN, Pascal/0000-0002-2879-9411; Iriberri, Juan/0000-0003-3787-6674; Rodriguez-Ezpeleta, Naiara/0000-0001-6735-6755; Martin, Patrick/0000-0001-8008-5558; Davies, Neil/0000-0001-8085-5014; Kostadinov, Ivaylo/0000-0003-4476-6764; Cochrane, Guy/0000-0001-7954-7057; Orlic, Sandi/0000-0002-6339-4145; Lauro, Federico/0000-0002-8373-1014; ten Hoopen, Petra/0000-0003-4242-4015; Baltar, Federico/0000-0001-8907-1494; Canning Clode, Joao/0000-0003-2143-6535; PESANT, Stephane/0000-0002-4936-5209; Golyshin, Peter/0000-0002-5433-0350; Duarte, Bernardo/0000-0003-1914-7435; Bienhold, Christina/0000-0003-2269-9468; Wallom, David/0000-0001-7527-3407; Loscher, Carolin/0000-0002-2044-6849; Vaulot, Daniel/0000-0002-0717-5685; Gasol, Josep M/0000-0001-5238-2387 NR 10 TC 16 Z9 16 U1 12 U2 51 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2047-217X J9 GIGASCIENCE JI GigaScience PD JUN 19 PY 2015 VL 4 AR 27 DI 10.1186/s13742-015-0066-5 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CX4JF UT WOS:000365665300001 PM 26097697 ER PT J AU Strandburg-Peshkin, A Farine, DR Couzin, ID Crofoot, MC AF Strandburg-Peshkin, Ariana Farine, Damien R. Couzin, Iain D. Crofoot, Margaret C. TI Shared decision-making drives collective movement in wild baboons SO SCIENCE LA English DT Article ID CHACMA BABOONS; ANIMAL GROUPS; LEADERSHIP; CONSENSUS; PRIMATE AB Conflicts of interest about where to go and what to do are a primary challenge of group living. However, it remains unclear how consensus is achieved in stable groups with stratified social relationships. Tracking wild baboons with a high-resolution global positioning system and analyzing their movements relative to one another reveals that a process of shared decision-making governs baboon movement. Rather than preferentially following dominant individuals, baboons are more likely to follow when multiple initiators agree. When conflicts arise over the direction of movement, baboons choose one direction over the other when the angle between them is large, but they compromise if it is not. These results are consistent with models of collective motion, suggesting that democratic collective action emerging from simple rules is widespread, even in complex, socially stratified societies. C1 [Strandburg-Peshkin, Ariana; Couzin, Iain D.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Farine, Damien R.; Crofoot, Margaret C.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.; Crofoot, Margaret C.] Smithsonian Trop Res Inst, Panama City, Panama. [Farine, Damien R.] Univ Oxford, Dept Zool, Edward Grey Inst Field Ornithol, Oxford, England. [Couzin, Iain D.] Max Planck Inst Ornithol, Dept Collect Behav, Constance, Germany. [Couzin, Iain D.] Univ Konstanz, Chair Biodivers & Collect Behav, Dept Biol, Constance, Germany. RP Strandburg-Peshkin, A (reprint author), Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. EM astrandb@princeton.edu; damien.farine@zoo.ox.ac.uk; mccrofoot@ucdavis.edu OI Farine, Damien/0000-0003-2208-7613; Couzin, Iain/0000-0001-8556-4558 FU NSF [EAGER-IOS-1250895, PHY-0848755, IOS-1355061, EAGER-IOS-1251585]; Max Planck Institute for Ornithology; Smithsonian Tropical Research Institute; Princeton University; NIH [T32HG003284]; Biotechnology and Biological Sciences Research Council [BB/L006081/1]; Office of Naval Research [N00014-09-1-1074, N00014-14-1-0635]; Army Research Office [W911NG-11-1-0385, W911NF-14-1-0431]; Human Frontier Science Program [RGP0065/2012] FX We thank the Kenya National Science and Technology Council, Kenyan Wildlife Service, and Mpala Research Centre for permission to conduct research. All procedures received Institutional Animal Care and Use Committee approval (2012.0601.2015). We thank M. Wikelski, E. Bermingham, D. Rubenstein, and M. Kinnaird for logistical support; R. Kays, S. Murray, M. Mutinda, R. Lessnau, S. Alavi, J. Nairobi, F. Kuemmeth, W. Heidrich, and I. Brugere for assistance; and T. Berger-Wolf, J. Silk, J. Fischer, B. Sheldon, L. Aplin, D. Pappano, M. Grobis, B. Rosenthal, A. Hein, B. Ziebart, L. Polansky, and J. Li for feedback. We acknowledge funding from NSF (grant EAGER-IOS-1250895), the Max Planck Institute for Ornithology, the Smithsonian Tropical Research Institute, and Princeton University. A. S.-P. and D.R.F. received additional support from NIH (grant T32HG003284), NSF (a Graduate Research Fellowship to A. S.-P.), and the Biotechnology and Biological Sciences Research Council (grant BB/L006081/1 to B. C. Sheldon). I.D.C. acknowledges support from NSF (grants PHY-0848755, IOS-1355061, and EAGER-IOS-1251585), the Office of Naval Research (grants N00014-09-1-1074 and N00014-14-1-0635), the Army Research Office (grants W911NG-11-1-0385 and W911NF-14-1-0431), and the Human Frontier Science Program (grant RGP0065/2012). Data are deposited at www.datarepository.movebank.org/(doi.org/10.5441/001/1.kn0816jn). NR 22 TC 44 Z9 44 U1 19 U2 84 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 JUN 19 PY 2015 VL 348 IS 6241 BP 1358 EP 1361 DI 10.1126/science.aaa5099 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK7XK UT WOS:000356449500050 PM 26089514 ER PT J AU Dillon, JS Neben, AR Hewitt, JN Tegmark, M Barry, N Beardsley, AP Bowman, JD Briggs, F Carroll, P de Oliveira-Costa, A Ewall-Wice, A Feng, L Greenhill, LJ Hazelton, BJ Hernquist, L Hurley-Walker, N Jacobs, DC Kim, HS Kittiwisit, P Lenc, E Line, J Loeb, A McKinley, B Mitchell, DA Morales, MF Offringa, AR Paul, S Pindor, B Pober, JC Procopio, P Riding, J Sethi, S Shankar, NU Subrahmanyan, R Sullivan, I Thyagarajan, N Tingay, SJ Trott, C Wayth, RB Webster, RL Wyithe, S Bernardi, G Cappallo, RJ Deshpande, AA Johnston-Hollitt, M Kaplan, DL Lonsdale, CJ McWhirter, SR Morgan, E Oberoi, D Ord, SM Prabu, T Srivani, KS Williams, A Williams, CL AF Dillon, Joshua S. Neben, Abraham R. Hewitt, Jacqueline N. Tegmark, Max Barry, N. Beardsley, A. P. Bowman, J. D. Briggs, F. Carroll, P. de Oliveira-Costa, A. Ewall-Wice, A. Feng, L. Greenhill, L. J. Hazelton, B. J. Hernquist, L. Hurley-Walker, N. Jacobs, D. C. Kim, H. S. Kittiwisit, P. Lenc, E. Line, J. Loeb, A. McKinley, B. Mitchell, D. A. Morales, M. F. Offringa, A. R. Paul, S. Pindor, B. Pober, J. C. Procopio, P. Riding, J. Sethi, S. Shankar, N. Udaya Subrahmanyan, R. Sullivan, I. Thyagarajan, Nithyanandan Tingay, S. J. Trott, C. Wayth, R. B. Webster, R. L. Wyithe, S. Bernardi, G. Cappallo, R. J. Deshpande, A. A. Johnston-Hollitt, M. Kaplan, D. L. Lonsdale, C. J. McWhirter, S. R. Morgan, E. Oberoi, D. Ord, S. M. Prabu, T. Srivani, K. S. Williams, A. Williams, C. L. TI Empirical covariance modeling for 21 cm power spectrum estimation: A method demonstration and new limits from early Murchison Widefield Array 128-tile data SO PHYSICAL REVIEW D LA English DT Article ID REIONIZATION OBSERVATORIES; COSMIC REIONIZATION; 21-CM FLUCTUATIONS; LOFAR OBSERVATIONS; BASE-LINE; EPOCH; EMISSION; FIELD; SENSITIVITY; COSMOLOGY AB The separation of the faint cosmological background signal from bright astrophysical foregrounds remains one of the most daunting challenges of mapping the high-redshift intergalactic medium with the redshifted 21 cm line of neutral hydrogen. Advances in mapping and modeling of diffuse and point source foregrounds have improved subtraction accuracy, but no subtraction scheme is perfect. Precisely quantifying the errors and error correlations due to missubtracted foregrounds allows for both the rigorous analysis of the 21 cm power spectrum and for the maximal isolation of the "EoR window" from foreground contamination. We present a method to infer the covariance of foreground residuals from the data itself in contrast to previous attempts at a priori modeling. We demonstrate our method by setting limits on the power spectrum using a 3 h integration from the 128-tile Murchison Widefield Array. Observing between 167 and 198 MHz, we find at 95% confidence a best limit of Delta(2)(k) < 3.7 x 10(4) mK(2) at comoving scale k = 0.18 h Mpc(-1) and at z = 6.8, consistent with existing limits. C1 [Dillon, Joshua S.; Neben, Abraham R.; Hewitt, Jacqueline N.; Tegmark, Max; de Oliveira-Costa, A.; Ewall-Wice, A.; Feng, L.; Williams, C. L.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Dillon, Joshua S.; Neben, Abraham R.; Hewitt, Jacqueline N.; Tegmark, Max; de Oliveira-Costa, A.; Ewall-Wice, A.; Feng, L.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst, Cambridge, MA 02139 USA. [Barry, N.; Beardsley, A. P.; Carroll, P.; Hazelton, B. J.; Morales, M. F.; Pober, J. C.; Sullivan, I.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Bowman, J. D.; Jacobs, D. C.; Kittiwisit, P.; Thyagarajan, Nithyanandan] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Briggs, F.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Briggs, F.; Kim, H. S.; Lenc, E.; Line, J.; McKinley, B.; Mitchell, D. A.; Offringa, A. R.; Pindor, B.; Procopio, P.; Riding, J.; Subrahmanyan, R.; Tingay, S. J.; Trott, C.; Wayth, R. B.; Webster, R. L.; Wyithe, S.; Ord, S. M.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT, Australia. [Hernquist, L.; Loeb, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hurley-Walker, N.; Ord, S. M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Kim, H. S.; Line, J.; McKinley, B.; Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.; Wyithe, S.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Mitchell, D. A.] CSIRO Astron & Space Sci CASS, Epping, NSW 1710, Australia. [Shankar, N. Udaya; Subrahmanyan, R.; Deshpande, A. A.; Srivani, K. S.; Williams, C. L.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Bernardi, G.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Bernardi, G.] SKA SA, ZA-7405 Cape Town, South Africa. [Cappallo, R. J.; Lonsdale, C. J.; McWhirter, S. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. RP Dillon, JS (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM jsdillon@mit.edu RI Wayth, Randall/B-2444-2013; Trott, Cathryn/B-5325-2013; Sethi, Shiv/D-4893-2012; Hurley-Walker, Natasha/B-9520-2013; Subrahmanyan, Ravi/D-4889-2012; M, Manjunath/N-4000-2014; Paul, Stephan/K-9237-2016; Deshpande, Avinash/D-4868-2012; Udayashankar , N/D-4901-2012; OI Lenc, Emil/0000-0002-9994-1593; Pober, Jonathan/0000-0002-3492-0433; Wayth, Randall/0000-0002-6995-4131; Trott, Cathryn/0000-0001-6324-1766; Hurley-Walker, Natasha/0000-0002-5119-4808; M, Manjunath/0000-0001-8710-0730; Paul, Stephan/0000-0002-8813-0437; /0000-0002-0086-7363 FU NSF [AST-0457585, AST-0821321, AST-1105835, AST-1410719, AST-1410484, AST-1411622, AST-1440343, AST-1401708]; MIT School of Science; Marble Astrophysics Fund; U.S. National Science Foundation [AST-0457585, PHY-0835713, CAREER-0847753, AST-0908884]; Australian Research Council (LIEF Grants) [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550- 0510247]; Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; Raman Research Institute; Australian National University; Victoria University of Wellington (New Zealand Ministry of Economic Development) [MED-E1799]; Victoria University of Wellington (IBM Shared University Research Grant); Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University; University of Western Australia - Western Australian State government FX We would like to thank Adrian Liu, Aaron Parsons, and Jeff Zheng for helpful discussions. We also acknowledge an anonymous referee whose insightful questions led to the refinement of method in order to a bias that occurs when a uv cell is used to estimate its own covariance and the ultimate form of Eq. (10). We would also like to thank Rennan Barkana for the theoretical power spectra in Fig. 9. This work was supported by NSF Grants No. AST-0457585, No. AST-0821321, No. AST-1105835, No. AST-1410719, No. AST-1410484, No. AST-1411622, and No. AST-1440343, by the MIT School of Science, by the Marble Astrophysics Fund, and by generous donations from Jonathan Rothberg and an anonymous donor. D. C. J. would like to acknowledge NSF support under Grant No. AST-1401708. 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 MWA comes from the U.S. National Science Foundation (Grants No. AST-0457585, No. PHY-0835713, No. CAREER-0847753, and No. AST-0908884), the Australian Research Council (LIEF Grants No. LE0775621 and No. LE0882938), the U.S. Air Force Office of Scientific Research (Grant No. FA9550-0510247), and the Centre for All-sky Astrophysics (an Australian Research Council Centre of Excellence funded by Grant No. CE110001020). Support is also provided by the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, and the Victoria University of Wellington (via Grant No. MED-E1799 from the New Zealand Ministry of Economic Development and an IBM Shared University Research Grant). The Australian Federal government provides additional support via the Commonwealth Scientific and Industrial Research Organisation (CSIRO), National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund, and Astronomy Australia Limited, under contract to Curtin University. We acknowledge the iVEC Petabyte Data Store, the Initiative in Innovative Computing, and the CUDA Center for Excellence sponsored by NVIDIA at Harvard University, and the International Centre for Radio Astronomy Research (ICRAR), a Joint Venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 69 TC 28 Z9 28 U1 1 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD JUN 19 PY 2015 VL 91 IS 12 AR 123011 DI 10.1103/PhysRevD.91.123011 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA CK8JB UT WOS:000356483200001 ER PT J AU Sohn, JC Powell, J AF Sohn, Jae-Cheon Powell, Jerry TI REVIEW OF EUCERATIA WALSINGHAM (LEPIDOPTERA, YPSOLOPHIDAE) WITH DESCRIPTION OF A NEW SPECIES SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Review DE Canada; Ditrysia; North America; USA; Yponomeutoidea AB The genus Euceratia is reviewed by the re-descriptions of two known species, E. castella and E. securella, and the description of a new species from California, E. intermedia n. sp. Euceratia is compared to other genera of Ypsolophidae. Diagnostic characters are provided for the three species of Euceratia and their distribution in the Nearctic Region is discussed. Imagoes and genitalia of all the species of Euceratia are illustrated. C1 [Sohn, Jae-Cheon] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Powell, Jerry] Univ Calif Berkeley, Essig Museum Entomol, Berkeley, CA 94720 USA. RP Sohn, JC (reprint author), Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, 10th & Constitut NW, Washington, DC 20560 USA. EM Sohnj@si.edu; powellj@berkeley.edu NR 16 TC 0 Z9 0 U1 0 U2 0 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD JUN 18 PY 2015 VL 69 IS 2 BP 131 EP 139 PG 9 WC Entomology SC Entomology GA CL0QX UT WOS:000356648400007 ER PT J AU Cabral, JS Petter, G Mendieta-Leiva, G Wagner, K Zotz, G Kreft, H AF Cabral, Juliano Sarmento Petter, Gunnar Mendieta-Leiva, Glenda Wagner, Katrin Zotz, Gerhard Kreft, Holger TI Branchfall as a Demographic Filter for Epiphyte Communities: Lessons from Forest Floor-Based Sampling SO PLOS ONE LA English DT Article ID NEOTROPICAL MONTANE FOREST; TROPICAL RAIN-FOREST; VASCULAR EPIPHYTES; ATLANTIC FOREST; VERTICAL STRATIFICATION; SPATIAL-DISTRIBUTION; SPECIES ASSEMBLAGES; POPULATION-DYNAMICS; FRENCH-GUIANA; INNER-CROWN AB Local variation in the abundance and richness of vascular epiphytes is often attributed to environmental characteristics such as substrate and microclimate. Less is known, however, about the impacts of tree and branch turnover on epiphyte communities. To address this issue, we surveyed branches and epiphytes found on the forest floor in 96 transects in two forests (Atlantic rainforest in Brazil and Caribbean rainforest in Panama). In the Brazilian forest, we additionally distinguished between edge and core study sites. We quantified branch abundance, epiphyte abundance, richness and proportion of adults to investigate the trends of these variables over branch diameter. Branches < 2 cm in diameter comprised > 90% of all branches on the forest floor. Abundance and richness of fallen epiphytes per transect were highest in the Brazilian core transects and lowest in the Panamanian transects. The majority of epiphytes on the floor (c. 65%) were found attached to branches. At all three study sites, branch abundance and branch diameter were negatively correlated, whereas epiphyte abundance and richness per branch, as well as the proportion of adults were positively correlated with branch diameter. The relationship between branch diameter and absolute epiphyte abundance or richness differed between study sites, which might be explained by differences in forest structure and dynamics. In the Panamanian forest, epiphytes had been previously inventoried, allowing an evaluation of our surveying method by comparing canopy and forest floor samplings. Individuals found on the forest floor corresponded to 13% of all individuals on branches < 10 cm in diameter (including crowns), with abundance, richness and composition trends on forest floor reflecting canopy trends. We argue that forest floor surveys provide useful floristic and, most notably, demographic information particularly on epiphytes occurring on the thinnest branches, which are least accessible. Here, branchfall acts as an important demographic filter structuring epiphyte communities. C1 [Cabral, Juliano Sarmento; Petter, Gunnar; Kreft, Holger] Univ Gottingen, Fac Forest Sci & Forest Ecol, Biodivers Macroecol & Conservat Biogeog Grp, D-37073 Gottingen, Germany. [Mendieta-Leiva, Glenda; Wagner, Katrin; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, Funct Ecol Plants, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Cabral, JS (reprint author), Univ Gottingen, Fac Forest Sci & Forest Ecol, Biodivers Macroecol & Conservat Biogeog Grp, D-37073 Gottingen, Germany. EM jsarmen@uni-goettingen.de OI Sarmento Cabral, Juliano/0000-0002-0116-220X; Mendieta-Leiva, Glenda/0000-0002-0156-4153 FU German Research Foundation (DFG) [SA-21331]; DFG Initiative of Excellence Free Floater Program at the University of Gottingen; DFG [Zo 94/5-1]; Smithsonian Tropical Research Institute FX J.S.C. acknowledges financial support by a German Research Foundation (DFG) grant (SA-21331). G.P. and H.K. were funded by the DFG Initiative of Excellence Free Floater Program at the University of Gottingen. G.Z., K.W. and G.M.L.'s work in Panama was supported by the DFG (Zo 94/5-1) and the Smithsonian Tropical Research Institute. NR 53 TC 5 Z9 5 U1 1 U2 12 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 JUN 17 PY 2015 VL 10 IS 6 AR e0128019 DI 10.1371/journal.pone.0128019 PG 19 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK9NS UT WOS:000356567400025 ER PT J AU Slik, JWF Arroyo-Rodriguez, V Aiba, S Alvarez-Loayza, P Alves, LF Ashton, P Balvanera, P Bastiang, ML Bellingham, PJ van den Berg, E Bernacci, L Bispo, PD Blanc, L Bohning-Gaese, K Boeckx, P Bongers, F Boyle, B Bradford, M Brearley, FQ Hockemba, MBN Bunyavejchewin, S Matos, DCL Castillo-Santiago, M Catharino, ELM Chai, SL Chen, YK Colwell, RK Robin, CL Clark, C Clark, DB Clark, DA Culmsee, H Damas, K Dattaraja, HS Dauby, G Davidar, P DeWalt, SJ Doucet, JL Duque, A Durigan, G Eichhorn, KAO Eisenlohr, PV Eler, E Ewango, C Farwig, N Feeley, KJ Ferreira, L Field, R de Oliveira, AT Fletcher, C Forshed, O Franco, G Fredriksson, G Gillespie, T Gillet, JF Amarnath, G Griffith, DM Grogan, J Gunatilleke, N Harris, D Harrison, R Hector, A Homeier, J Imai, N Itoh, A Jansen, PA Joly, CA de Jong, BHJ Kartawinata, K Kearsley, E Kelly, DL Kenfack, D Kessler, M Kitayama, K Kooyman, R Larney, E Laumonier, Y Laurance, S Laurance, WF Lawes, MJ do Amaral, IL Letche, SG Lindsell, J Lu, XH Mansor, A Marjokorpi, A Martin, EH Meilby, H Melo, FPL Metcalfe, DJ Medjibe, VP Metzger, JP Millet, J Mohandass, D Montero, JC Valeriano, MD Mugerwa, B Nagamasu, H Nilus, R Ochoa-Gaona, S Onrizal Page, N Parolin, P Parren, M Parthasarathy, N Paudel, E Permana, A Piedade, MTF Pitman, NCA Poorter, L Poulsen, AD Poulsen, J Powers, J Prasad, RC Puyravaud, JP Razafimahaimodiso, JC Reitsma, J dos Santos, JR Spironello, WR Romero-Saltos, H Rovero, F Rozak, AH Ruokolainen, K Rutishauser, E Saiter, F Saner, P Santos, BA Santos, F Sarker, SK Satdichanh, M Schmitt, CB Schongart, J Schulze, M Suganuma, MS Sheil, D Pinheiro, ED Sist, P Stevart, T Sukumar, R Sun, IF Sunderand, T Suresh, HS Suzuki, E Tabarelli, M Tang, JW Targhetta, N Theilade, I Thomas, DW Tchouto, P Hurtado, J Valencia, R van Valkenburg, JLCH Do, TV Vasquez, R Verbeeck, H Adekunle, V Vieira, SA Webb, CO Whitfeld, T Wich, SA Williams, J Wittmann, F Woll, H Yang, XB Yao, CYA Yap, SL Yoneda, T Zahawi, RA Zakaria, R Zang, RG de Assis, RL Luize, BG Venticinque, EM AF Slik, J. W. Ferry Arroyo-Rodriguez, Victor Aiba, Shin-Ichiro Alvarez-Loayza, Patricia Alves, Luciana F. Ashton, Peter Balvanera, Patricia Bastiang, Meredith L. Bellingham, Peter J. van den Berg, Eduardo Bernacci, Luis Bispo, Polyanna da Conceicao Blanc, Lilian Boehning-Gaese, Katrin Boeckx, Pascal Bongers, Frans Boyle, Brad Bradford, Matt Brearley, Francis Q. Hockemba, Mireille Breuer-Ndoundou Bunyavejchewin, Sarayudh Leal Matos, Darley Calderado Castillo-Santiago, Miguel Catharino, Eduardo L. M. Chai, Shauna-Lee Chen, Yukai Colwell, Robert K. Robin, Chazdon L. Clark, Connie Clark, David B. Clark, Deborah A. Culmsee, Heike Damas, Kipiro Dattaraja, Handanakere S. Dauby, Gilles Davidar, Priya DeWalt, Saara J. Doucet, Jean-Louis Duque, Alvaro Durigan, Giselda Eichhorn, Karl A. O. Eisenlohr, Pedro V. Eler, Eduardo Ewango, Corneille Farwig, Nina Feeley, Kenneth J. Ferreira, Leandro Field, Richard de Oliveira Filho, Ary T. Fletcher, Christine Forshed, Olle Franco, Geraldo Fredriksson, Gabriella Gillespie, Thomas Gillet, Jean-Francois Amarnath, Giriraj Griffith, Daniel M. Grogan, James Gunatilleke, Nimal Harris, David Harrison, Rhett Hector, Andy Homeier, Juergen Imai, Nobuo Itoh, Akira Jansen, Patrick A. Joly, Carlos A. de Jong, Bernardus H. J. Kartawinata, Kuswata Kearsley, Elizabeth Kelly, Daniel L. Kenfack, David Kessler, Michael Kitayama, Kanehiro Kooyman, Robert Larney, Eileen Laumonier, Yves Laurance, Susan Laurance, William F. Lawes, Michael J. do Amaral, Ieda Leao Letche, Susan G. Lindsell, Jeremy Lu, Xinghui Mansor, Asyraf Marjokorpi, Antti Martin, Emanuel H. Meilby, Henrik Melo, Felipe P. L. Metcalfe, Daniel J. Medjibe, Vincent P. Metzger, Jean Paul Millet, Jerome Mohandass, D. Montero, Juan C. Valeriano, Marcio de Morisson Mugerwa, Badru Nagamasu, Hidetoshi Nilus, Reuben Ochoa-Gaona, Susana Onrizal Page, Navendu Parolin, Pia Parren, Marc Parthasarathy, Narayanaswamy Paudel, Ekananda Permana, Andrea Piedade, Maria T. F. Pitman, Nigel C. A. Poorter, Lourens Poulsen, Axel D. Poulsen, John Powers, Jennifer Prasad, Rama C. Puyravaud, Jean-Philippe Razafimahaimodiso, Jean-Claude Reitsma, Jan dos Santos, Joao Roberto Spironello, Wilson Roberto Romero-Saltos, Hugo Rovero, Francesco Rozak, Andes Hamuraby Ruokolainen, Kalle Rutishauser, Ervan Saiter, Felipe Saner, Philippe Santos, Braulio A. Santos, Fernanda Sarker, Swapan K. Satdichanh, Manichanh Schmitt, Christine B. Schoengart, Jochen Schulze, Mark Suganuma, Marcio S. Sheil, Douglas Pinheiro, Eduardo da Silva Sist, Plinio Stevart, Tariq Sukumar, Raman Sun, I. -Fang Sunderand, Terry Suresh, H. S. Suzuki, Eizi Tabarelli, Marcelo Tang, Jangwei Targhetta, Natuelia Theilade, Ida Thomas, Duncan W. Tchouto, Peguy Hurtado, Johanna Valencia, Renato van Valkenburg, Johan L. C. H. Tran Van Do Vasquez, Rodolfo Verbeeck, Hans Adekunle, Victor Vieira, Simone A. Webb, Campbell O. Whitfeld, Timothy Wich, Serge A. Williams, John Wittmann, Florian Woell, Hannsjoerg Yang, Xiaobo Yao, C. Yves Adou Yap, Sandra L. Yoneda, Tsuyoshi Zahawi, Rakan A. Zakaria, Rahmad Zang, Runguo de Assis, Rafael L. Luize, Bruno Garcia Venticinque, Eduardo M. TI An estimate of the number of tropical tree species SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE diversity estimation; Fisher's log series; pantropical; spatial richness patterns; tropical tree species richness ID ABUNDANCE DISTRIBUTIONS; PLANT DIVERSITY; GLOBAL PATTERNS; RAIN-FORESTS; BIODIVERSITY; RICHNESS; COVERAGE; SAMPLE; AREA AB The high species richness of tropical forests has long been recognized, yet there remains substantial uncertainty regarding the actual number of tropical tree species. Using a pantropical tree inventory database from closed canopy forests, consisting of 657,630 trees belonging to 11,371 species, we use a fitted value of Fisher's alpha and an approximate pantropical stem total to estimate the minimum number of tropical forest tree species to fall between similar to 40,000 and similar to 53,000, i.e., at the high end of previous estimates. Contrary to common assumption, the Indo-Pacific region was found to be as species-rich as the Neotropics, with both regions having a minimum of similar to 19,000-25,000 tree species. Continental Africa is relatively depauperate with a minimum of similar to 4,500-6,000 tree species. Very few species are shared among the African, American, and the Indo-Pacific regions. We provide a methodological framework for estimating species richness in trees that may help refine species richness estimates of tree-dependent taxa. C1 [Slik, J. W. Ferry] Univ Brunei Darusallam, Fac Sci, Gadong, Brunei. [Arroyo-Rodriguez, Victor; Balvanera, Patricia] Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia, Michoacan, Mexico. [Aiba, Shin-Ichiro; Suzuki, Eizi; Yoneda, Tsuyoshi] Kagoshima Univ, Kagoshima 890, Japan. [Alvarez-Loayza, Patricia; Clark, Connie; Medjibe, Vincent P.; Pitman, Nigel C. A.; Poulsen, John] Duke Univ, Ctr Trop Conservat, Durham, NC USA. [Alves, Luciana F.; Bernacci, Luis] Inst Agron Campinas, Campinas, SP, Brazil. [Ashton, Peter] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Bastiang, Meredith L.] Smithsonian Natl Zool Pk, Washington, DC USA. [Bellingham, Peter J.] Landcare Res, Lincoln, New Zealand. [van den Berg, Eduardo] Univ Fed Lavras, Lavras, Brazil. [Bispo, Polyanna da Conceicao; Valeriano, Marcio de Morisson; dos Santos, Joao Roberto] Natl Inst Space Res INPE, Sao Jose Dos Campos, SP, Brazil. [Blanc, Lilian] Ctr Cooperat Int Rech Agronim Dev CIRAD, Belem, Para, Brazil. [Boehning-Gaese, Katrin] Gesell Naturforsch, Senckenberg, Biodivers & Climate Res Ctr BiK F, Frankfurt, Germany. [Boeckx, Pascal; Kearsley, Elizabeth; Verbeeck, Hans] Univ Ghent, B-9000 Ghent, Belgium. [Bongers, Frans; Jansen, Patrick A.; Parren, Marc; Poorter, Lourens] Wageningen Univ, NL-6700 AP Wageningen, Netherlands. [Boyle, Brad] Univ Arizona, Tucson, AZ USA. [Bradford, Matt] CSIRO, Land & Water Trop Forest Res Ctr, Atherton, Australia. [Brearley, Francis Q.] Manchester Metropolitan Univ, Manchester M15 6BH, Lancs, England. [Hockemba, Mireille Breuer-Ndoundou; Ewango, Corneille] Wildlife Conservat Soc, Congo Program, Nouabale Ndoki Park, Congo. [Bunyavejchewin, Sarayudh] Wildlife & Plant Conservat, Dept Natl Pk, Bangkok, Thailand. [Leal Matos, Darley Calderado; Ferreira, Leandro; Santos, Fernanda] Museu Paraense Emilio Goeldi, Belem, Para, Brazil. [Castillo-Santiago, Miguel; de Jong, Bernardus H. J.; Ochoa-Gaona, Susana] El Colegio Frontera ECOSUR, Chiapas, Mexico. [Catharino, Eduardo L. M.] Inst Bot Sao Paulo, Sao Paulo, Brazil. [Chai, Shauna-Lee] Alberta Innovates Technol Futures, Vegreville, AB, Canada. [Chen, Yukai] Hainan Normal Univ, Coll Life Sci, Haikou, Peoples R China. [Colwell, Robert K.; Robin, Chazdon L.] Univ Connecticut, Storrs, CT USA. [Colwell, Robert K.] Univ Colorado, Boulder, CO 80309 USA. [Clark, David B.; Clark, Deborah A.] Univ Missouri, St Louis, MO 63121 USA. [Culmsee, Heike; Homeier, Juergen] Univ Gottingen, D-37073 Gottingen, Germany. [Damas, Kipiro] PNG Forest Res Inst, Lae, Papua N Guinea. [Dattaraja, Handanakere S.; Page, Navendu; Sukumar, Raman; Suresh, H. S.] Indian Inst Sci, Bangalore 560012, Karnataka, India. [Dauby, Gilles] Univ Libre Bruxelles, Brussels, Belgium. [Davidar, Priya; Parthasarathy, Narayanaswamy] Pondicherry Univ, Pondicherry, India. [DeWalt, Saara J.] Clemson Univ, Clemson, SC USA. [Doucet, Jean-Louis; Gillet, Jean-Francois] Univ Liege, Gembloux Agro Bio Tech, Gembloux, Belgium. [Duque, Alvaro] Univ Nacl Colombia, Medellin, Colombia. [Durigan, Giselda; Franco, Geraldo] Inst Florestal Sao Paulo, Sao Paulo, Brazil. [Eichhorn, Karl A. O.] Eichhorn Ecol, Zeist, Netherlands. [Eisenlohr, Pedro V.] Univ Estado Mato Grosso, Caceres, Brazil. [Eler, Eduardo; do Amaral, Ieda Leao; Spironello, Wilson Roberto; de Assis, Rafael L.; Luize, Bruno Garcia] Inst Nacl de Pesquisas da Amazonia, Manaus, Amazonas, Brazil. [Farwig, Nina] Univ Marburg, Marburg, Germany. [Feeley, Kenneth J.] Florida Int Univ, Int Ctr Trop Bot, Miami, FL 33199 USA. [Field, Richard] Univ Nottingham, Nottingham NG7 2RD, England. [de Oliveira Filho, Ary T.] Univ Fed Minas Gerais, Inst Ciencias Biol, Belo Horizonte, MG, Brazil. [Fletcher, Christine] Forest Res Inst Malaysia, Kuala Lumpur, Malaysia. [Forshed, Olle] World Wildlife Fund WWF Sweden, Stockholm, Sweden. [Fredriksson, Gabriella] PanEco Sumatran Orangutan Conservat Program SOCP, Medan, North Sumatra, Indonesia. [Gillespie, Thomas] Univ Calif Los Angeles, Los Angeles, CA USA. [Amarnath, Giriraj] Int Water Management Inst, Colombo, Sri Lanka. [Griffith, Daniel M.] Univ Laica Eloy Alfaro Manabi, Manta, Ecuador. [Grogan, James] Mt Holyoke Coll, South Hadley, MA USA. [Gunatilleke, Nimal] Univ Peradeniya, Peradeniya, Sri Lanka. [Harris, David] Royal Bot Gardens Edinburgh, Edinburgh, Midlothian, Scotland. [Harrison, Rhett; Paudel, Ekananda; Satdichanh, Manichanh] Chinese Acad Sci, Kunming Inst Bot, Ctr Mt Ecosyst, Kunming, Peoples R China. [Harrison, Rhett] China & World Agroforestry Ctr ICRAF, East & Cent Asia Reg Off, Kunming, Peoples R China. [Hector, Andy] Univ Oxford, Oxford, England. [Imai, Nobuo] Kyoto Univ, Primate Res Inst, Inuyama, Aichi 484, Japan. [Itoh, Akira] Osaka City Univ, Osaka 558, Japan. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Panama City, Panama. [Joly, Carlos A.; Vieira, Simone A.] Univ Estadual Campinas, Campinas, Brazil. [Kartawinata, Kuswata] Indonesian Inst Sci LIPI, Herbarium Bogoriense, Biol Res Ctr, Cibinong, Indonesia. [Kelly, Daniel L.] Univ Dublin Trinity Coll, Dublin 2, Ireland. [Kenfack, David] Smithsonian Trop Res Inst, Washington, DC USA. [Kessler, Michael; Permana, Andrea; Saner, Philippe] Univ Zurich, Zurich, Switzerland. [Kitayama, Kanehiro; Nagamasu, Hidetoshi] Kyoto Univ, Kyoto, Japan. [Kooyman, Robert] Macquarie Univ, Sydney, NSW 2109, Australia. [Larney, Eileen; Razafimahaimodiso, Jean-Claude] Ctr ValBio, Ranomafana, Madagascar. [Laumonier, Yves; Sheil, Douglas; Sunderand, Terry] Ctr Int Forestry Res CIFOR, Bogor, Indonesia. [Laurance, Susan; Laurance, William F.] James Cook Univ, Cairns, Australia. [Lawes, Michael J.] Charles Darwin Univ, Res Inst Environm & Livelihoods, Darwin, NT 0909, Australia. [Letche, Susan G.] SUNY Coll Purchase, Purchase Coll, Purchase, NY 10577 USA. [Lindsell, Jeremy] RSPB, Sandy, Beds, England. [Lu, Xinghui; Zang, Runguo] Chinese Acad Forestry, Inst Forest Ecol Environm & Protect, Beijing, Peoples R China. [Mansor, Asyraf; Zakaria, Rahmad] Univ Sains Malaysia, Georgetown, Penang, Malaysia. [Marjokorpi, Antti] Stora Enso Oyj, Helsinki, Finland. [Martin, Emanuel H.] Udzungwa Ecol Monitoring Ctr, Mangula, Tanzania. [Martin, Emanuel H.] Sokoine Univ Agr, Morogoro, Tanzania. [Meilby, Henrik; Theilade, Ida] Univ Copenhagen, Copenhagen, Denmark. [Melo, Felipe P. L.; Tabarelli, Marcelo] Univ Fed Pernambuco, Recife, PE, Brazil. [Metcalfe, Daniel J.] CSIRO Land & Water, EcoSci Precinct, Acton, ACT, Australia. [Metzger, Jean Paul; Suganuma, Marcio S.] Univ Sao Paulo, Sao Paulo, Brazil. [Millet, Jerome] Natl Univ Laos, Viangchan, Laos. [Mohandass, D.; Tang, Jangwei] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Menglun, Peoples R China. [Montero, Juan C.] Univ Freiburg, Fac Environm & Nat Resources, D-79106 Freiburg, Germany. [Mugerwa, Badru] Inst Trop Forest Conservat, Kampala, Uganda. [Onrizal] Sabah Forestry Dept, Sandakan, Sabah, Malaysia. [Parolin, Pia] Univ Sumatera Utara, Medan, Sumatra, Indonesia. [Poulsen, Axel D.] Univ Hamburg, Hamburg, Germany. [Powers, Jennifer] Univ Oslo, Oslo, Norway. [Prasad, Rama C.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Puyravaud, Jean-Philippe] Int Inst Informat Technol, Hyderabad, Andhra Pradesh, India. [Reitsma, Jan] Sigur Nat Trust, Masinagudi, India. [Romero-Saltos, Hugo] Bur Waardenburg Bv, Culemborg, Netherlands. [Rovero, Francesco] Yachay Tech Univ, Dept Biol, Urcuqui, Ecuador. [Rozak, Andes Hamuraby] MUSE Museo Sci, Trento, Italy. [Ruokolainen, Kalle] Indonesian Inst Sci LIPI, Cibodas Bot Gardens, Cianjur, Indonesia. [Rutishauser, Ervan] Univ Turku, Turku, Finland. [Saiter, Felipe] Carboforexpert, Geneva, Switzerland. [Santos, Braulio A.] Inst Fed Espirito Santo, Santa Teresa, Brazil. [Sarker, Swapan K.] Univ Fed Paraiba, BR-58059900 Joao Pessoa, Paraiba, Brazil. [Schmitt, Christine B.] Shahjalal Univ Sci & Technol, Sylhet, Bangladesh. [Schoengart, Jochen; Targhetta, Natuelia] Univ Freiburg, Chair Landscape Management, D-79106 Freiburg, Germany. [Schulze, Mark] Inst Nacl de Pesquisas da Amazonia, Max Planck Project, Manaus, Amazonas, Brazil. [Sheil, Douglas; de Assis, Rafael L.] Oregon State Univ, Corvallis, OR 97331 USA. [Sheil, Douglas] Norwegian Univ Life Sci, As, Norway. [Pinheiro, Eduardo da Silva] Univ Fed Amazonas, Manaus, Amazonas, Brazil. [Sist, Plinio] CIRAD, Montpellier, France. [Stevart, Tariq; Vasquez, Rodolfo] Missouri Bot Garden, St Louis, MO 63166 USA. [Sun, I. -Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien, Taiwan. [Thomas, Duncan W.] Washington State Univ, Dept Biol, Vancouver, ON, Canada. [Tchouto, Peguy] Ecole Natl Eaux & Forets, Mbalmayo, Cameroon. [Hurtado, Johanna; Zahawi, Rakan A.] Org Trop Field Studies, La Selva, Costa Rica. [Valencia, Renato] Pontificia Univ Catolica Ecuador, Quito, Ecuador. [van Valkenburg, Johan L. C. H.] Nederlands Voedsel En Warenautoriteit, Wageningen, Netherlands. [Tran Van Do] Kyoto Univ, Ctr Southeast Asian Studies, Kyoto, Japan. [Adekunle, Victor] Fed Univ Technol Akure, Akure, Nigeria. [Webb, Campbell O.] Harvard Univ, Arnold Arboretum, Jamaica Plain, MA USA. [Whitfeld, Timothy] Brown Univ, Providence, RI 02912 USA. [Wich, Serge A.] Liverpool John Moores Univ, Liverpool L3 5UX, Merseyside, England. [Wich, Serge A.] Univ Amsterdam, Amsterdam, Netherlands. [Williams, John] Inst Politecn Nacl, Oaxaca, Mexico. [Wittmann, Florian] Max Planck Inst Chem, Biogeochem Dept, D-55128 Mainz, Germany. [Yang, Xiaobo] Hainan Univ, Haikou, Hainan, Peoples R China. [Yao, C. Yves Adou] Felix Houphouet Boigny Univ, Abidjan, Cote Ivoire. [Yap, Sandra L.] Univ Philippines, Inst Biol, Quezon City 1101, Philippines. [Venticinque, Eduardo M.] Univ Fed Rio Grande do Norte, BR-59072970 Natal, RN, Brazil. RP Slik, JWF (reprint author), Univ Brunei Darusallam, Fac Sci, Gadong, Brunei. EM ferryslik@hotmail.com RI Melo, Felipe/B-7720-2008; Alves, Luciana/E-1141-2012; Piedade, Maria Teresa/C-5372-2013; Culmsee, Heike/E-9360-2011; Kessler, Michael/A-3605-2009; Bradford, Matt/D-3389-2011; Vieira, Simone/H-1225-2011; Tabarelli, Marcelo/F-1088-2010; Homeier, Jurgen/G-1662-2011; Santos, Braulio/M-2582-2013; Metzger, Jean Paul/C-2514-2012; Laurance, Susan/G-6021-2011; Feeley, Kenneth/A-7631-2009; Research ID, CTBCC /O-3564-2014; James Cook University, TESS/B-8171-2012; Aiba, Shin-ichiro/A-3011-2010; de Jong, Ben/A-1996-2016; Hector, Andrew/H-4199-2011; Sheil, Douglas/A-3867-2015; M, Asyraf/A-6901-2011; van den Berg, Eduardo/L-9617-2014; Venticinque, Eduardo/G-8961-2015; Metcalfe, Daniel/G-3305-2010; Meilby, Henrik/E-1404-2015; Arroyo-Rodriguez, Victor/C-9255-2009; Eisenlohr, Pedro/F-8421-2012; Luize, Bruno/N-9838-2015; Schongart, Jochen/I-2659-2016; OI Metzger, Jean Paul /0000-0002-0087-5240; Wich, Serge/0000-0003-3954-5174; Schmitt, Christine B./0000-0002-8527-9682; Melo, Felipe/0000-0002-1271-3214; Alves, Luciana/0000-0002-8944-1851; Piedade, Maria Teresa/0000-0002-7320-0498; Culmsee, Heike/0000-0003-4577-6307; Vieira, Simone/0000-0002-0129-4181; Tabarelli, Marcelo/0000-0001-7573-7216; Homeier, Jurgen/0000-0001-5676-3267; Laurance, Susan/0000-0002-2831-2933; Aiba, Shin-ichiro/0000-0001-9852-7748; de Jong, Ben/0000-0002-3264-2759; Hector, Andrew/0000-0002-1309-7716; Sheil, Douglas/0000-0002-1166-6591; M, Asyraf/0000-0003-1255-7239; van den Berg, Eduardo/0000-0002-0843-6437; Metcalfe, Daniel/0000-0001-6853-7072; Meilby, Henrik/0000-0002-3770-3880; Eisenlohr, Pedro/0000-0002-5912-8370; Luize, Bruno/0000-0002-8384-8386; Harris, David/0000-0002-6801-2484; Letcher, Susan/0000-0002-9475-7674; Rutishauser, Ervan/0000-0003-1182-4032; Davidar, Priya/0000-0003-2463-6743; Theilade, Ida/0000-0003-3502-1277 FU Arnold Arboretum of Harvard University; Belgian Science Policy [SD/AR/01A]; Botanic Garden Meise; Brazilian Science Council; Conselho Nacional de Desenvovimento Cientifico e Tecnologico of Brazil [MAUA] [PRONEX-FAPEAM 1600/2006]; Conselho Nacional de Desenvovimento Cientifico e Tecnologico of Brazil [Universal] [479599/2008-4]; Conselho Nacional de Desenvovimento Cientifico e Tecnologico of Brazil [CNPq] [309458/2013-7]; British Ecological Society [4709/5747]; Coordination of Improvement of Higher Education Personnel, Brazil; DEFRA Darwin Initiative; Deland Award for student research, Arnold Arboretum; Department of Biotechnology-National Remote Sensing Agency, India; Department of National Parks, Wildlife and Plant Conservation, Thailand; El Consejo de Ciencia y Technologia Grant [33851-B]; Federal Ministry of Education and Research, Germany; Forest Department Sarawak, Malaysia; Fulbright Program; Fundacao de Amparo a Pesquisa de Minas Gerais, Brazil; German Agency for International Cooperation Projects [08.7860.3-001.00, 13.1432.7-001.00]; German Science Foundation [CRC 552, CU127/3-1, HO 3296/2-2, HO3296/4-1, RU 816]; Grant Agency of the Czech Republic Project [14-36098G]; Intitut National pour L'etude et la Recherche Agronomiques, Democratic Republic Congo; Instituto Nacional de Pesquisas de Amazonia/Max Planck Institute for Chemistry; Large-Scale Biosphere Atmosphere Experiment in Amazonia; Missouri Botanical Garden; Museo delle Scienze; National Institute for Environmental Studies, Japan; National Science Foundation (NSF) [DEB-0075334, DEB-0515678, LTEB1357177, LTREB/DEB1357112, NSF DEB-0424767, NSF DEB-0639393, NSF DEB-1147429, NSF DEB-1350125, NSF-DEB-1053237, NSF DEB-0841885]; NERC Human-Modified Tropical Forests Programme; Operation Wallacea; PAPIIT-DGAPA-UNAM, Mexico [IB-200812, IN-204215]; Pontificia Universidad Catolica del Ecuador; Rockefeller Foundation; Royal Forest Department of Thailand; Royal Society South-East Asia Rainforest Research Programme [RS243]; Rufford Small Grant Foundation; St. Louis Zoo; Sao Paulo Research Foundation [FAPESP 03/12595-7-COTEC/IF 41.065/2005-IBAMA/CGEN 093/2005]; Smithsonian Tropical Research Institute; Society of Systematic Biologists; Systematics Association; Swiss National Science Foundation; Tropenbos International; University of Minnesota; US Department of Agriculture Forest Service, International Institute of Tropical Forestry; USAID; World Wildlife Fund; Gordon and Betty Moore Foundation; Smithsonian Institution; National Science Foundation; John Merck Fund; John D. and Catherine T. MacArthur Foundation; Andrew W. Mellon Foundation; Frank Levinson Family Foundation; HSBC Climate Partnership; Bromley Charitable Trust; John Swire Sons Pty Ltd.; Small World Institute Fund FX We thank Michael Fine and one anonymous reviewer for useful comments, and David Newbery, Thorsten Wiegand, George Weiblen, Vojtech Novotny, Punchi Manage Saranga Amila Ruwan, Stuart Davies, Miriam van Heist, Terese Hart, Helen Murphy, Kazuki Miyamoto, Sylvester Tan, Edmund Tanner, Mauricio Alvarez, Ana Andrade, Phourin Chhang, George Chuyong, Indiana Coronado, Chang-Fu Hsieh, Shawn Lum, Jean-Remy Makana, Cao Min, Xiaoxue Mo, Meyner Nusalawo, Atila Oliveira, Lars Schmidt, Lee Sing Kong, Takuo Yamakura, and Nicole Zweifel for providing inventory data. Funding was provided by the Arnold Arboretum of Harvard University; Belgian Science Policy (SD/AR/01A); Botanic Garden Meise; Brazilian Science Council; Conselho Nacional de Desenvovimento Cientifico e Tecnologico of Brazil [MAUA (PRONEX-FAPEAM 1600/2006), Universal (479599/2008-4)/CNPq (309458/2013-7)]; British Ecological Society (4709/5747); Coordination of Improvement of Higher Education Personnel, Brazil; DEFRA Darwin Initiative; Deland Award for student research, Arnold Arboretum; Department of Biotechnology-National Remote Sensing Agency, India; Department of National Parks, Wildlife and Plant Conservation, Thailand; El Consejo de Ciencia y Technologia Grant 33851-B; Federal Ministry of Education and Research, Germany; Forest Department Sarawak, Malaysia; Fulbright Program; Fundacao de Amparo a Pesquisa de Minas Gerais, Brazil; German Agency for International Cooperation Projects 08.7860.3-001.00 and 13.1432.7-001.00; German Science Foundation Grants CRC 552 and CU127/3-1, HO 3296/2-2, HO3296/4-1, and RU 816; Grant Agency of the Czech Republic Project 14-36098G; Intitut National pour L'etude et la Recherche Agronomiques, Democratic Republic Congo; Instituto Nacional de Pesquisas de Amazonia/Max Planck Institute for Chemistry; Large-Scale Biosphere Atmosphere Experiment in Amazonia; Missouri Botanical Garden; Museo delle Scienze; National Institute for Environmental Studies, Japan; National Science Foundation (NSF) Grants DEB-0075334, DEB-0515678, LTEB1357177, LTREB/DEB1357112, NSF DEB-0424767, NSF DEB-0639393, NSF DEB-1147429, NSF DEB-1350125, NSF-DEB-1053237, and NSF DEB-0841885; NERC Human-Modified Tropical Forests Programme; Operation Wallacea; PAPIIT-DGAPA-UNAM IB-200812, IN-204215, Mexico; Pontificia Universidad Catolica del Ecuador; Rockefeller Foundation; Royal Forest Department of Thailand; Royal Society South-East Asia Rainforest Research Programme Project RS243; Rufford Small Grant Foundation; St. Louis Zoo; Sao Paulo Research Foundation Project FAPESP 03/12595-7-COTEC/IF 41.065/2005-IBAMA/CGEN 093/2005; Smithsonian Tropical Research Institute; Society of Systematic Biologists; Systematics Association; Swiss National Science Foundation; Tropenbos International; University of Minnesota; US Department of Agriculture Forest Service, International Institute of Tropical Forestry; USAID; and the World Wildlife Fund. Part of the data in this publication were provided by the Tropical Ecology Assessment and Monitoring (TEAM) Network, a collaboration between Conservation International, the Missouri Botanical Garden, the Smithsonian Institution, and the Wildlife Conservation Society, and partially funded by these institutions, the Gordon and Betty Moore Foundation, and other donors. The Center for Tropical Forest Science network has received major support from the Smithsonian Institution, particularly the Smithsonian Tropical Research Institute, the Arnold Arboretum of Harvard University, the National Science Foundation, the Rockefeller Foundation, the John Merck Fund, the John D.; and Catherine T. MacArthur Foundation, the Andrew W. Mellon Foundation, the Frank Levinson Family Foundation, the HSBC Climate Partnership, the Bromley Charitable Trust, John Swire & Sons Pty Ltd., and Small World Institute Fund. NR 40 TC 31 Z9 31 U1 13 U2 104 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 JUN 16 PY 2015 VL 112 IS 24 BP 7472 EP 7477 DI 10.1073/pnas.1423147112 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK5GS UT WOS:000356251800047 PM 26034279 ER PT J AU Zeder, MA AF Zeder, Melinda A. TI Reply to Mohlenhoff et al.: Human behavioral ecology needs a rethink that niche-construction theory can provide SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. EM zederm@si.edu NR 6 TC 2 Z9 2 U1 4 U2 22 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 JUN 16 PY 2015 VL 112 IS 24 BP E3094 EP E3094 DI 10.1073/pnas.1508096112 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK5GS UT WOS:000356251800004 PM 26034292 ER PT J AU Burnik Sturm, M Pukazhenthi, B Reed, D Ganbaatar, O Susnik, S Haymerle, A Voigt, CC Kaczensky, P AF Burnik Sturm, Martina Pukazhenthi, Budhan Reed, Dolores Ganbaatar, Oyunsaikhan Susnik, Stane Haymerle, Agnes Voigt, Christian C. Kaczensky, Petra TI A protocol to correct for intra- and interspecific variation in tail hair growth to align isotope signatures of segmentally cut tail hair to a common time line SO RAPID COMMUNICATIONS IN MASS SPECTROMETRY LA English DT Article ID STABLE-ISOTOPES; AFRICAN ELEPHANTS; DIET CHANGES; PATTERNS; VEGETATION; ANIMALS; ECOLOGY; HISTORY; HORSE; TERM AB RATIONALE: In recent years, segmental stable isotope analysis of hair has been a focus of research in animal dietary ecology and migration. To correctly assign tail hair segments to seasons or even Julian dates, information on tail hair growth rates is a key parameter, but is lacking for most species. METHODS: We (a) reviewed the literature on tail hair growth rates in mammals; b) made own measurements of three captive equid species; (c) measured delta H-2, delta C-13 and delta N-15 values in sequentially cut tail hairs of three sympatric, free-ranging equids from the Mongolian Gobi, using isotope ratio mass spectrometry (IRMS); and (d) collected environmental background data on seasonal variation by measuring delta H-2 values in precipitation by IRMS and by compiling pasture productivity measured by remote sensing via the normalized difference vegetation index (NDVI). RESULTS: Tail hair growth rates showed significant inter-and intra-specific variation making temporal alignment problematic. In the Mongolian Gobi, high seasonal variation of delta H-2 values in precipitation results in winter lows and summer highs of delta H-2 values of available water sources. In water-dependent equids, this seasonality is reflected in the isotope signatures of sequentially cut tails hairs. CONCLUSIONS: In regions which are subject to strong seasonal patterns we suggest identifying key isotopes which show strong seasonal variation in the environment and can be expected to be reflected in the animal tissue. The known interval between the maxima and minima of these isotope values can then be used to correctly temporally align the segmental stable isotope signature for each individual animal. (C) 2015 The Authors. Rapid Communications in Mass Spectrometry published by John Wiley & Sons Ltd. C1 [Burnik Sturm, Martina; Haymerle, Agnes; Kaczensky, Petra] Univ Vet Med, Res Inst Wildlife Ecol, Savoyenstr 1, A-1160 Vienna, Austria. [Pukazhenthi, Budhan; Reed, Dolores] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Ganbaatar, Oyunsaikhan] Natl Univ Mongolia, Sch Biol & Biotechnol, Great Gobi B Strictly Protected Area Adm, Ulaanbaatar, Mongol Peo Rep. [Ganbaatar, Oyunsaikhan] Natl Univ Mongolia, Sch Biol & Biotechnol, Dept Zool, Ulaanbaatar, Mongol Peo Rep. [Susnik, Stane] Inst Donkey Breeding & Res, Oslarija, Komen, Slovenia. [Voigt, Christian C.] Leibniz Inst Zoo & Wildlife Res IZW, Berlin, Germany. RP Burnik Sturm, M (reprint author), Univ Vet Med, Res Inst Wildlife Ecol, Savoyenstr 1, A-1160 Vienna, Austria. EM sturm.martina@gmail.com RI Burnik Sturm, Martina/D-2694-2016 OI Burnik Sturm, Martina/0000-0002-3198-1687 FU Austrian Science Foundation (FWF) [P24231] FX We wish to thank C. Walzer for capture and anesthesia of wild equids and Great Gobi B Strictly Protected Area staff N. Altansukh, B. Batsuuri, G. Nisekhkhuu, Ya. Amgalan, B. Chinbat, Z. Baast, N. Tumur, and L. Oinbayar for help with the capture of Przewalski's horses and/or tail hair sampling of domestic horses. Special thanks go to J. Theiner, the head of the micro-analytical chemistry lab at the Faculty of Chemistry, University Vienna, for kindly enabling sample preparation in his lab and to A. Burnik for his help with sample preparation. Sincere thanks also to K. Sorgel, A. Luckner and Y. Klaar for the stable isotope analyses at the IZW. This study was funded by the Austrian Science Foundation (FWF) project P24231. We wish to thank the anonymous reviewers for constructive comments and suggestions that helped to improve the manuscript. NR 35 TC 0 Z9 0 U1 1 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0951-4198 EI 1097-0231 J9 RAPID COMMUN MASS SP JI Rapid Commun. Mass Spectrom. PD JUN 15 PY 2015 VL 29 IS 11 BP 1047 EP 1054 DI 10.1002/rcm.7196 PG 8 WC Biochemical Research Methods; Chemistry, Analytical; Spectroscopy SC Biochemistry & Molecular Biology; Chemistry; Spectroscopy GA CI2HN UT WOS:000354566900008 PM 26044272 ER PT J AU Kays, R Crofoot, MC Jetz, W Wikelski, M AF Kays, Roland Crofoot, Margaret C. Jetz, Walter Wikelski, Martin TI Terrestrial animal tracking as an eye on life and planet SO SCIENCE LA English DT Review ID MIGRATORY PERFORMANCE; SATELLITE TRACKING; TELEMETRY SYSTEM; GPS COLLARS; RAIN-FOREST; MOVEMENT; POPULATION; DISPERSAL; DYNAMICS; SELECTION AB Moving animals connect our world, spreading pollen, seeds, nutrients, and parasites as they go about the their daily lives. Recent integration of high-resolution Global Positioning System and other sensors into miniaturized tracking tags has dramatically improved our ability to describe animal movement. This has created opportunities and challenges that parallel big data transformations in other fields and has rapidly advanced animal ecology and physiology. New analytical approaches, combined with remotely sensed or modeled environmental information, have opened up a host of new questions on the causes of movement and its consequences for individuals, populations, and ecosystems. Simultaneous tracking of multiple animals is leading to new insights on species interactions and, scaled up, may enable distributed monitoring of both animals and our changing environment. C1 [Kays, Roland] North Carolina Museum Nat Sci, Raleigh, NC 27601 USA. [Kays, Roland] N Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Kays, Roland; Crofoot, Margaret C.; Wikelski, Martin] Smithsonian Trop Res Inst, Balboa, Panama. [Crofoot, Margaret C.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Crofoot, Margaret C.; Wikelski, Martin] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Jetz, Walter] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Jetz, Walter] Imperial Coll London, Dept Life Sci, Ascot SL5 7PY, Berks, England. [Wikelski, Martin] Univ Konstanz, Dept Biol, Constance, Germany. RP Kays, R (reprint author), North Carolina Museum Nat Sci, Raleigh, NC 27601 USA. EM roland.kays@ncsu.edu FU NASA [NNX11AP72G]; NSF [EF 1232442, DBI 0756920, DBI 0960550, DBI-1262600, BCS 1440755, DEB 1026764, DEB-1441737, IOS 1250895] FX B. Carlson, J. Hody, K. Mertes, and J. Perrine read a previous draft and offered constructive comments. S. Dodge helped with data for Fig. 5. Work on this study was supported by NASA Biodiversity Grant NNX11AP72G and NSF grants EF 1232442, DBI 0756920, DBI 0960550, DBI-1262600, BCS 1440755, DEB 1026764, DEB-1441737, and IOS 1250895. The range map for Fig. 1 was provided by BirdLife International and NatureServe and the photograph by M. Kaatz. M. Berger and R. Weinzierl made the animation. Photographs are courtesy of D. Brown, R. Henrik, C. Markham, M. McGaw, K. Thorup, and N. Weber. NR 117 TC 68 Z9 69 U1 37 U2 83 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 JUN 12 PY 2015 VL 348 IS 6240 AR aaa2478 DI 10.1126/science.aaa2478 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CK2AK UT WOS:000356011500044 PM 26068858 ER PT J AU Sironi, L Petropoulou, M Giannios, D AF Sironi, Lorenzo Petropoulou, Maria Giannios, Dimitrios TI Relativistic jets shine through shocks or magnetic reconnection? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; magnetic reconnection; radiation mechanisms: non-thermal; shock waves; gamma-ray burst: general; galaxies: jets ID GAMMA-RAY BURSTS; EXTRAGALACTIC RADIO-SOURCES; INTRINSIC BRIGHTNESS TEMPERATURES; PAIR PLASMA RECONNECTION; BL-LAC OBJECTS; PARTICLE-ACCELERATION; COLLISIONLESS SHOCKS; SYNCHROTRON-RADIATION; NONTHERMAL PARTICLES; AFTERGLOW EMISSION AB Observations of gamma-ray-bursts and jets from active galactic nuclei reveal that the jet flow is characterized by a high radiative efficiency and that the dissipative mechanism must be a powerful accelerator of non-thermal particles. Shocks and magnetic reconnection have long been considered as possible candidates for powering the jet emission. Recent progress via fully-kinetic particle-in-cell simulations allows us to revisit this issue on firm physical grounds. We show that shock models are unlikely to account for the jet emission. In fact, when shocks are efficient at dissipating energy, they typically do not accelerate particles far beyond the thermal energy, and vice versa. In contrast, we show that magnetic reconnection can deposit more than 50 per cent of the dissipated energy into non-thermal leptons as long as the energy density of the magnetic field in the bulk flow is larger than the rest-mass energy density. The emitting region, i.e. the reconnection downstream, is characterized by a rough energy equipartition between magnetic fields and radiating particles, which naturally accounts for a commonly observed property of blazar jets. C1 [Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Petropoulou, Maria; Giannios, Dimitrios] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. RP Sironi, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lsironi@cfa.harvard.edu RI Petropoulou, Maria/L-6790-2016 OI Petropoulou, Maria/0000-0001-6640-0179 FU NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF1-120090, PF3-140113]; NASA [NAS8-03060, NNX13AP13G]; XSEDE [TG-AST120010] FX LS is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. MP is supported by NASA through Einstein Postdoctoral Fellowship grant number PF3-140113 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. DG acknowledges support from NASA grant NNX13AP13G. The simulations were performed on XSEDE resources under contract no. TG-AST120010, and on NASA High-End Computing (HEC) resources through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 84 TC 40 Z9 40 U1 4 U2 8 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 JUN 11 PY 2015 VL 450 IS 1 BP 183 EP 191 DI 10.1093/mnras/stv641 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6BA UT WOS:000356311600011 ER PT J AU Wilson, PA Sing, DK Nikolov, N des Etangs, AL Pont, F Fortney, JJ Ballester, GE Lopez-Morales, M Desert, JM Vidal-Madjar, A AF Wilson, P. A. Sing, D. K. Nikolov, N. des Etangs, A. Lecavelier Pont, F. Fortney, J. J. Ballester, G. E. Lopez-Morales, M. Desert, J. -M. Vidal-Madjar, A. TI GTC OSIRIS transiting exoplanet atmospheric survey: detection of potassium in HAT-P-1b from narrow-band spectrophotometry SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: individual: HAT-P-1b; planetary systems ID TRANSMISSION SPECTRAL SURVEY; RADIO OCCULTATION MEASUREMENTS; HD 209458B; GIANT PLANETS; SODIUM-ABSORPTION; TUNABLE IMAGER; LIGHT CURVES; JUPITER; HOT; SPECTROSCOPY AB We present the detection of potassium in the atmosphere of HAT-P-1b using optical transit narrow-band photometry. The results are obtained using the 10.4-m Gran Telescopio Canarias together with the OSIRIS instrument in tunable filter imaging mode. We observed four transits, two at continuum wavelengths outside the potassium feature, at 6792 and 8844 angstrom, and two probing the potassium feature in the line wing at 7582.0 angstrom and the line core at 7664.9 angstrom using a 12 angstrom filter width (R similar to 650). The planet-to-star radius ratios in the continuum are found to be R-pl/R-star = 0.1176 +/- 0.0013 at 6792 angstrom and R-pl/R-star = 0.1168 +/- 0.0022 at 8844 angstrom, significantly lower than the two observations in the potassium line: R-pl/R-star = 0.1248 +/- 0.0014 in the line wing at 7582.0 angstrom and R-pl/R-star = 0.1268 +/- 0.0012 in the line core at 7664.9 angstrom With a weighted mean of the observations outside the potassium feature R-pl/R-star = 0.1174 +/- 0.0010, the potassium is detected as an increase in the radius ratio of Delta R-pl/R-star = 0.0073 +/- 0.0017 at 7582.0 angstrom and Delta R-pl/R-star = 0.0094 +/- 0.0016 at 7664.9 angstrom (a significance of 4.3 sigma and 6.1 sigma, respectively). We hypothesize that the strong detection of potassium is caused by a large scaleheight, which can be explained by a high temperature at the base of the upper atmosphere. A lower mean molecular mass caused by the dissociation of molecular hydrogen into atomic hydrogen by the extreme ultraviolet flux from the host star may also partly explain the amplitude of our detection. C1 [Wilson, P. A.; des Etangs, A. Lecavelier; Vidal-Madjar, A.] CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Wilson, P. A.; des Etangs, A. Lecavelier; Vidal-Madjar, A.] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Wilson, P. A.; Sing, D. K.; Nikolov, N.; Pont, F.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ballester, G. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Desert, J. -M.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. RP Wilson, PA (reprint author), CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. EM pwilson@iap.fr RI Nikolov, Nikolay/H-6183-2015; OI Nikolov, Nikolay/0000-0002-6500-3574; Sing, David /0000-0001-6050-7645 FU STFC [ST/J0016/1]; European Research Council under the European Union [336792]; Space Telescope Science Institute [HST- GO-12473.01-A]; Halliday fellowship [ST/F011083/1]; French Agence Nationale de la Recherche (ANR) [ANR-12-BS05-0012] FX We thank the entire GTC staff and in particular Antonio Cabrera Lavers for their help with conducting these observations. This work is based on observations made with the 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 GTC is a joint initiative of Spain (led by the Instituto de Astrofisica de Canarias), the University of Florida and Mexico, including the Instituto de Astronomia de la Universidad Nacional Autonoma de Mexico (IA-UNAM) and Instituto Nacional de Astrofisica, Optica y Electronica (INAOE). PAW acknowledges support from STFC. The research leading to these results has received funding from the European Research Council under the European Unions Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement no. 336792. DKS, FP, and NN acknowledge support from STFC consolidated grant ST/J0016/1. GEB acknowledges support from Space Telescope Science Institute through grants HST- GO-12473.01-A. FP is grateful for the Halliday fellowship (ST/F011083/1). PAW and ALE acknowledge the support of the French Agence Nationale de la Recherche (ANR), under programme ANR-12-BS05-0012 'Exo-Atmos'. We would like to thank referee, Ron Gilliland, for his useful comments. NR 54 TC 10 Z9 10 U1 1 U2 6 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 JUN 11 PY 2015 VL 450 IS 1 BP 192 EP 200 DI 10.1093/mnras/stv642 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6BA UT WOS:000356311600012 ER PT J AU Kudritzki, RP Ho, IT Schruba, A Burkert, A Zahid, HJ Bresolin, F Dima, GI AF Kudritzki, Rolf-Peter Ho, I-Ting Schruba, Andreas Burkert, Andreas Zahid, H. Jabran Bresolin, Fabio Dima, Gabriel I. TI The chemical evolution of local star-forming galaxies: radial profiles of ISM metallicity, gas mass, and stellar mass and constraints on galactic accretion and winds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: evolution; galaxies: abundances; galaxies: evolution; galaxies: spiral ID MILKY-WAY DISK; ABUNDANCE GRADIENTS; SPIRAL GALAXIES; NEARBY GALAXIES; QUANTITATIVE SPECTROSCOPY; COSMOLOGICAL SIMULATIONS; GENERAL CONSTRAINTS; PHYSICAL-PROPERTIES; INTERSTELLAR-MEDIUM; FORMATION RATES AB The radially averaged metallicity distribution of the interstellar medium (ISM) and the young stellar population of a sample of 20 disc galaxies is investigated by means of an analytical chemical evolution model which assumes constant ratios of galactic wind mass-loss and accretion mass gain to star formation rate. Based on this model, the observed metallicities and their gradients can be described surprisingly well by the radially averaged distribution of the ratio of stellar mass to ISM gas mass. The comparison between observed and model-predicted metallicity is used to constrain the rate of mass-loss through galactic wind and accretion gain in units of the star formation rate. Three groups of galaxies are found: galaxies with either mostly winds and only weak accretion, or mostly accretion and only weak winds, and galaxies where winds are roughly balanced by accretion. The three groups are distinct in the properties of their gas discs. Galaxies with approximately equal rates of mass-loss and accretion gain have low metallicity, atomic-hydrogen-dominated gas discs with a flat spatial profile. The other two groups have gas discs dominated by molecular hydrogen out to 0.5 to 0.7 isophotal radii and show a radial exponential decline, which is on average steeper for the galaxies with small accretion rates. The rates of accretion (less than or similar to 1.0 x SFR) and outflow (less than or similar to 2.4 x SFR) are relatively low. The latter depend on the calibration of the zero-point of the metallicity determination from the use of H II region strong emission lines. C1 [Kudritzki, Rolf-Peter; Ho, I-Ting; Bresolin, Fabio; Dima, Gabriel I.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kudritzki, Rolf-Peter; Burkert, Andreas] Univ Observ Munich, D-81679 Munich, Germany. [Schruba, Andreas] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Zahid, H. Jabran] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kudritzki, RP (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM kud@ifa.hawaii.edu FU National Science Foundation [AST-1008798, AST-1108906]; Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence 'Origin and Structure of the Universe' FX RPK and FB acknowledge support by the National Science Foundation under grants AST-1008798 and AST-1108906 and by the Munich Institute for Astro- and Particle Physics (MIAPP) of the DFG cluster of excellence 'Origin and Structure of the Universe', where part of this work was carried out. We wish to thank our referee, Dr Yago Ascasibar, for his helpful and very constructive review. NR 79 TC 12 Z9 12 U1 0 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 JUN 11 PY 2015 VL 450 IS 1 BP 342 EP 359 DI 10.1093/mnras/stv522 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6BA UT WOS:000356311600026 ER PT J AU Sobral, D Stroe, A Dawson, WA Wittman, D Jee, MJ Rottgering, H van Weeren, RJ Brueggen, M AF Sobral, David Stroe, Andra Dawson, William A. Wittman, David Jee, M. James Rottgering, Huub van Weeren, Reinout J. Brueggen, Marcus TI MC2: boosted AGN and star formation activity in CIZA J2242.8+5301, a massive post-merger cluster at z=0.19 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual: CIZA J2242.8+5301; galaxies: evolution; intergalactic medium; cosmology: observations; large-scale structure of Universe ID MERGING GALAXY CLUSTER; SIMILAR-TO 1; ALPHA LUMINOSITY FUNCTION; HIGH-REDSHIFT GALAXIES; FORMING GALAXIES; METALLICITY RELATION; ENVIRONMENTAL DEPENDENCE; STELLAR MASS; FORMATION HISTORY; XMM-NEWTON AB Cluster mergers may play a fundamental role in the formation and evolution of cluster galaxies. Stroe et al. revealed unexpected overdensities of candidate H alpha emitters near the similar to 1-Mpc-wide shock fronts of the massive (similar to 2 x 10(15) M-circle dot) 'Sausage' merging cluster, CIZA J2242.8+5301. We used the Keck/Deep Imaging Multi-Object Spectrograph and the William Herschel Telescope/AutoFib2+WYFFOS to confirm 83 H alpha emitters in and around the merging cluster. We find that cluster star-forming galaxies in the hottest X-ray gas and/or in the cluster subcores (away from the shock fronts) show high [S II] 6716/[S II] 6761 and high [S II] 6716/H alpha, implying very low electron densities (<30 x lower than all other star-forming galaxies outside the cluster) and/or significant contribution from supernovae, respectively. All cluster star-forming galaxies near the cluster centre show evidence of significant outflows (blueshifted Na D similar to 200-300 km s(-1)), likely driven by supernovae. Strong outflows are also found for the cluster H alpha active galactic nucleus (AGN). H alpha star-forming galaxies in the merging cluster follow the z similar to 0 mass-metallicity relation, showing systematically higher metallicity (similar to 0.15-0.2 dex) than H alpha emitters outside the cluster (projected R > 2.5 Mpc). This suggests that the shock front may have triggered remaining metal-rich gas which galaxies were able to retain into forming stars. Our observations show that the merger of impressively massive (similar to 10(15) M-circle dot) clusters can provide the conditions for significant star formation and AGN activity, but, as we witness strong feedback by star-forming galaxies and AGN (and given how massive the merging cluster is), such sources will likely quench in a few 100 Myr. C1 [Sobral, David] Univ Lisbon, Dept Fis, Fac Ciencias, P-1749016 Lisbon, Portugal. [Sobral, David; Stroe, Andra; Dawson, William A.; Rottgering, Huub] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Dawson, William A.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Dawson, William A.; Wittman, David; Jee, M. James] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [van Weeren, Reinout J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brueggen, Marcus] Hamburger Sternwarte, D-21029 Hamburg, Germany. RP Sobral, D (reprint author), Univ Lisbon, Inst Astrofis & Ciencias Espaco, OAL, P-1349018 Lisbon, Portugal. EM sobral@strw.leidenuniv.nl; astroe@strw.leidenuniv.nl RI Sobral, David/C-7919-2014; OI Sobral, David/0000-0001-8823-4845; Wittman, David/0000-0002-0813-5888 FU Netherlands Organisation for Scientific research (NWO) [614.001.006]; FCT [IF/01154/2012/CP0189/CT0010, PEst-OE/FIS/UI2751/2014]; NASA - Chandra X-Ray Center [PF2-130104]; NASA [NAS8-03060]; US DOE [DE-AC52-07NA27344]; W.M. Keck Foundation; National Aeronautics and Space Administration FX We thank the referee for many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014. AS and HR acknowledge financial support from an NWO top subsidy (614.001.006). RJvW is supported by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. Part of this work performed under the auspices of the US DOE by LLNL under contract DE-AC52-07NA27344. 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. 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. NR 92 TC 11 Z9 11 U1 2 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 JUN 11 PY 2015 VL 450 IS 1 BP 630 EP 645 DI 10.1093/mnras/stv521 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK6BA UT WOS:000356311600046 ER PT J AU Alexander, KD Soderberg, AM Chomiuk, LB AF Alexander, Kate D. Soderberg, Alicia M. Chomiuk, Laura B. TI A NEW MODEL FOR THE RADIO EMISSION FROM SN 1994I AND AN ASSOCIATED SEARCH FOR RADIO TRANSIENTS IN M51 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M51); radio continuum: general; radio continuum: stars; supernovae: individual (SN 1994I) ID GAMMA-RAY BURST; REMNANT CASSIOPEIA-A; SUPERNOVA REMNANT; SPIRAL GALAXIES; IC SUPERNOVAE; EVOLUTION; EXPANSION; SPECTRA; STARS; DECELERATION AB We revisit the exquisite archival radio data for the Type Ic supernova SN 1994I and present a revised model for the supernova (SN) radio emission and a pilot study that aims to constrain the rate of C-band radio transients within the face-on host galaxy, M51 (NGC 5194). We find that the temporal and spectral evolution of the SN 1994I radio emission are well fit by a synchrotron self-absorption model and use this to estimate physical parameters. We compute a pre-explosion mass loss rate of M = 3.0 x 10(-5)M(circle dot) yr(-1) for the progenitor, consistent with those observed from galactic Wolf-Rayet stars. Our model makes different assumptions for the dynamical model for the shockwave interaction than the model previously published by Weiler et al., but our M. is consistent with theirs to within errors and assumptions. Drawing from a subset of the archival radio observations from the Very Large Array collected for the monitoring of SN 1994I, we conduct a pilot study to search for previously unidentified transients. Data were primarily taken at a frequency of 4.9 GHz and are logarithmic in cadence, enabling sensitivity to transients with variability timescales ranging from days to months. We find no new transient detections in 31 epochs of data, allowing us to place a 2 sigma upper limit of 17 deg(-2) for the source density of radio transients above 0.5 mJy (L greater than or similar to 4 x 10(25) erg s(-1) Hz(-1) at the distance of M51). This study highlights the feasibility of utilizing archival high-cadence radio studies of SN host galaxies to place constraints on the radio transient rate as a function of luminosity in the local universe. C1 [Alexander, Kate D.; Soderberg, Alicia M.; Chomiuk, Laura B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chomiuk, Laura B.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Alexander, KD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kalexander@cfa.harvard.edu OI Alexander, Kate/0000-0002-8297-2473 FU National Science Foundation Research Experiences for Undergraduates (REU); Department of Defense [0754568]; Smithsonian Institution FX Thanks to Jonathan McDowell and Marie Machacek for helpful comments on early drafts of this paper. This work is supported in part by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under Grant no. 0754568 and by the Smithsonian Institution. 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 SAOImage DS9, developed by Smithsonian Astrophysical Observatory. NR 53 TC 3 Z9 3 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 106 DI 10.1088/0004-637X/806/1/106 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300106 ER PT J AU Bowler, BP Shkolnik, EL Liu, MC Schlieder, JE Mann, AW Dupuy, TJ Hinkley, S Crepp, JR Johnson, JA Howard, AW Flagg, L Weinberger, AJ Aller, KM Allers, KN Best, WMJ Kotson, MC Montet, BT Herczeg, GJ Baranec, C Riddle, R Law, NM Nielsen, EL Wahhaj, Z Biller, BA Hayward, TL AF Bowler, Brendan P. Shkolnik, Evgenya L. Liu, Michael C. Schlieder, Joshua E. Mann, Andrew W. Dupuy, Trent J. Hinkley, Sasha Crepp, Justin R. Johnson, John Asher Howard, Andrew W. Flagg, Laura Weinberger, Alycia J. Aller, Kimberly M. Allers, Katelyn N. Best, William M. J. Kotson, Michael C. Montet, Benjamin T. Herczeg, Gregory J. Baranec, Christoph Riddle, Reed Law, Nicholas M. Nielsen, Eric L. Wahhaj, Zahed Biller, Beth A. Hayward, Thomas L. TI PLANETS AROUND LOW-MASS STARS (PALMS). V. AGE-DATING LOW-MASS COMPANIONS TO MEMBERS AND INTERLOPERS OF YOUNG MOVING GROUPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; brown dwarfs; stars: individual (2MASS J02155892, 0929121, 2MASS J15594729+4403595, HD 23514) ID TW-HYDRAE ASSOCIATION; DIGITAL SKY SURVEY; VERY-LOW MASS; BRIGHT SOURCE CATALOG; X-RAY SOURCES; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; CANDIDATE SUBSTELLAR COMPANION; SUPERNOVA FACTORY OBSERVATIONS; FINDING CAMPAIGN DISCOVERY; EXTRASOLAR GIANT PLANETS AB We present optical and near-infrared adaptive optics (AO) imaging and spectroscopy of 13 ultracool (>M6) companions to late-type stars (K7-M4.5), most of which have recently been identified as candidate members of nearby young moving groups (YMGs; 8-120 Myr) in the literature. Three of these are new companions identified in our AO imaging survey, and two others are confirmed to be comoving with their host stars for the first time. The inferred masses of the companions (similar to 10-100 M-Jup) are highly sensitive to the ages of the primary stars; therefore we critically examine the kinematic and spectroscopic properties of each system to distinguish bona fide YMG members from old field interlopers. The new M7 substellar companion 2MASS J02155892-0929121 C (40-60 M-Jup) shows. clear spectroscopic signs of low gravity and, hence, youth. The primary, possibly a member of the similar to 40 Myr Tuc-Hor moving group, is visually resolved into three components, making it a young low-mass quadruple system in a compact (less than or similar to 100 AU) configuration. In addition, LiI lambda 6708 absorption in the intermediate-gravity M7.5 companion 2MASS J15594729+4403595 B provides unambiguous evidence that it is young (less than or similar to 200 Myr) and resides below the hydrogen-burning limit. Three new close-separation (<1 '') companions (2MASS J06475229-2523304 B, PYC J11519+0731 B, and GJ 4378 Ab) orbit stars previously reported as candidate YMG members, but instead are likely old (greater than or similar to 1Gyr) tidally locked spectroscopic binaries without convincing kinematic associations with any known moving group. The high rate of false positives in the form of old active stars with YMG-like kinematics underscores the importance of radial velocity and parallax measurements to validate candidate young stars identified via proper motion and activity selection alone. Finally, we spectroscopically confirm the cool temperature and substellar nature of HD 23514 B, a recently discovered M8 benchmark brown dwarf orbiting the dustiest-known member of the Pleiades. C1 [Bowler, Brendan P.; Montet, Benjamin T.; Riddle, Reed] CALTECH, Pasadena, CA 91125 USA. [Shkolnik, Evgenya L.; Flagg, Laura] Lowell Observ, Flagstaff, AZ 86001 USA. [Liu, Michael C.; Howard, Andrew W.; Aller, Kimberly M.; Best, William M. J.; Kotson, Michael C.; Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Schlieder, Joshua E.] NASA, Ames Res Ctr, Postdoctoral Program Fellow, Moffett Field, CA 94035 USA. [Mann, Andrew W.; Dupuy, Trent J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hinkley, Sasha] Univ Exeter, Phys & Astron, Exeter EX4 4QL, Devon, England. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Johnson, John Asher; Montet, Benjamin T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Flagg, Laura] No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. [Weinberger, Alycia J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Allers, Katelyn N.] Bucknell Univ, Dept Phys & Astron, Lewisburg, PA 17837 USA. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Law, Nicholas M.] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Nielsen, Eric L.] Carl Sagan Ctr, SETI Inst, Mountain View, CA 94043 USA. [Nielsen, Eric L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA USA. [Wahhaj, Zahed] European So Observ, Santiago, Chile. [Biller, Beth A.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hayward, Thomas L.] Southern Operat Ctr AURA, Gemini Observ, La Serena, Chile. RP Bowler, BP (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM bpbowler@caltech.edu OI Montet, Benjamin/0000-0001-7516-8308; Nielsen, Eric/0000-0001-6975-9056; Herczeg, Gregory/0000-0002-7154-6065 FU NASA Grant [NNX11AC31G]; NSF Grant [AST09-09222]; National Science Foundation [AST-0906060, AST-0960343, AST-1207891]; Mt. Cuba Astronomical Foundation; Alfred P. Sloan Foundation; National Science Foundation Graduate Research Fellowship [DGE1144469]; National Aeronautics and Space Administration; National Science Foundation FX We thank the referee for their helpful suggestions and Niall Deacon for obtaining some of the IRTF observations presented here. M.C.L. has been supported by NASA Grant NNX11AC31G and NSF Grant AST09-09222. This paper is based on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: 2014B-0083; PI: Bowler), which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. This research is also based in part on observations obtained at the Gemini Observatory, which is operated by 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). The Robo-AO system was developed by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, and with the support of 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. Ongoing science operation support of Robo-AO is provided by the California Institute of Technology and the University of Hawai'i. C.B. acknowledges support from the Alfred P. Sloan Foundation. B.T.M. is supported by a National Science Foundation Graduate Research Fellowship under Grant DGE1144469. We utilized 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. NASA's Astrophysics Data System Bibliographic Services together with the VizieR catalog access tool and SIMBAD database operated at CDS, Strasbourg, France, were invaluable resources for this work. This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. Finally, mahalo nui loa to the kama'aina of Hawai'i for their support of Keck and the Maunakea observatories. We are grateful to conduct observations from this mountain. NR 203 TC 7 Z9 7 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 62 DI 10.1088/0004-637X/806/1/62 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300062 ER PT J AU Brodwin, M Greer, CH Leitch, EM Stanford, SA Gonzalez, AH Gettings, DP Abdulla, Z Carlstrom, JE Decker, B Eisenhardt, PR Lin, HW Mantz, AB Marrone, DP McDonald, M Stalder, B Stern, D Wylezalek, D AF Brodwin, M. Greer, C. H. Leitch, E. M. Stanford, S. A. Gonzalez, A. H. Gettings, D. P. Abdulla, Z. Carlstrom, J. E. Decker, B. Eisenhardt, P. R. Lin, H. W. Mantz, A. B. Marrone, D. P. McDonald, M. Stalder, B. Stern, D. Wylezalek, D. TI THE MASSIVE AND DISTANT CLUSTERS OF WISE SURVEY. III. SUNYAEV-ZEL'DOVICH MASSES OF GALAXY CLUSTERS AT z similar to 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: high-redshift; infrared: galaxies ID SOUTH-POLE TELESCOPE; 720 SQUARE DEGREES; X-RAY-PROPERTIES; SPECTROSCOPIC CONFIRMATION; STAR-FORMATION; COSMOLOGICAL IMPLICATIONS; SKY SURVEY; DISCOVERY; SAMPLE; CATALOG AB We present CARMA 30 GHz Sunyaev-Zel'dovich (SZ) observations of five high-redshift (z greater than or similar to 1), infrared-selected galaxy clusters discovered as part of the all-sky Massive and Distant Clusters of WISE Survey (MaDCoWS). The SZ decrements measured toward these clusters demonstrate that the MaDCoWS selection is discovering evolved, massive galaxy clusters with hot intracluster gas. Using the SZ scaling relation calibrated with South Pole Telescope clusters at similar masses and redshifts, we find these MaDCoWS clusters have masses in the range M-200 approximate to 2-6 x 10(14) M-circle dot. Three of these are among the most massive clusters found to date at z greater than or similar to 1, demonstrating that MaDCoWS is sensitive to the most massive clusters to at least z = 1.3. The added depth of the AllWISE data release will allow all-sky infrared cluster detection to z approximate to 1.5 and beyond. C1 [Brodwin, M.; Decker, B.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Greer, C. H.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85121 USA. [Leitch, E. M.; Abdulla, Z.; Carlstrom, J. E.; Mantz, A. B.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Leitch, E. M.; Abdulla, Z.; Carlstrom, J. E.; Mantz, A. B.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Gonzalez, A. H.; Gettings, D. P.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Eisenhardt, P. R.; Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Lin, H. W.; Stalder, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Wylezalek, D.] European So Observ, Garching, Germany. RP Brodwin, M (reprint author), Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. OI Marrone, Daniel/0000-0002-2367-1080 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 California; state of Illinois; state of Maryland; National Science Foundation; CARMA partner universities; NSF [AST-1140019]; National Aeronautics and Space Administration; NASA Astrophysics Data Analysis Program (ADAP) [NNX12AE15G]; NASA Keck PI Data Award; W. M. Keck Foundation; [PHY-0114422]; [GN-2013A-Q-44]; [GN-2013B-Q-8] FX We thank the anonymous referee for helpful comments that improved the paper. We thank L. Bleem for providing the code and data to produce Figure 4 and B. Benson for helpful conversations. 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 California, Illinois, 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; the work at Chicago was supported by NSF grant AST-1140019. Additional support was provided by PHY-0114422. 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. M.B., D.P.G., A.H.G., and S.A.S. acknowledge support for this research from the NASA Astrophysics Data Analysis Program (ADAP) through grant NNX12AE15G. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. 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. This work is based in part on data 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. Based in part on observations obtained 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), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Data were obtained in Program IDs GN-2013A-Q-44 and GN-2013B-Q-8. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. NR 52 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 JUN 10 PY 2015 VL 806 IS 1 AR 26 DI 10.1088/0004-637X/806/1/26 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300026 ER PT J AU Bromley, BC Kenyon, SJ AF Bromley, Benjamin C. Kenyon, Scott J. TI PLANET FORMATION AROUND BINARY STARS: TATOOINE MADE EASY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; planetary systems; planets and satellites: dynamical evolution and stability; planets and satellites: formation; protoplanetary disks; stars: individual (Kepler-16) ID TRANSITING CIRCUMBINARY PLANET; ECCENTRIC ASTROPHYSICAL DISCS; CIRCUMSTELLAR DUST DISKS; BODY-COAGULATION CODE; EARTH-LIKE PLANETS; PROTOPLANETARY DISKS; ACCRETION DISKS; DEBRIS DISKS; GIANT PLANETS; SOLAR NEBULA AB We examine characteristics of circumbinary orbits in the context of current planet formation scenarios. Analytical perturbation theory predicts the existence of nested circumbinary orbits that are generalizations of circular paths around a single star. These orbits have forced eccentric motion aligned with the binary as well as higher frequency oscillations, yet they do not cross, even in the presence of massive disks and perturbations from large planets. For this reason, dissipative gas and planetesimals can settle onto these "most circular" orbits, facilitating the growth of protoplanets. Outside a region close to the binary where orbits are generally unstable, circumbinary planets form in much the same way as their cousins around a single star. Here, we review the theory and confirm its predictions with a suite of representative simulations. We then consider the circumbinary planets discovered with NASA's Kepler satellite. These Neptune- and Jupiter-size planets, or their planetesimal precursors, may have migrated inward to reach their observed orbits, since their current positions are outside of unstable zones caused by overlapping resonances. In situ formation without migration seems less likely, only because the surface density of the protoplanetary disks must be implausibly high. Otherwise, the circumbinary environment is friendly to planet formation, and we expect that many earth-like "Tatooines" will join the growing census of circumbinary planets. C1 [Bromley, Benjamin C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bromley, BC (reprint author), Univ Utah, Dept Phys & Astron, 115 S 1400 E,Rm 201, Salt Lake City, UT 84112 USA. EM bromley@physics.utah.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA [NNX10AF35G, NNX11AM37G] FX We thank the referee for a timely and thoughtful report that helped us to hone our presentation. We also thank N. Georgakarakos, J. Pringle, R. Rafikov, P. Thebault, and A. Youdin for helpful comments on the manuscript. We gratefully acknowledge NASA for support through the Astrophysics Theory and Origins of Solar Systems programs (grant NNX10AF35G) and through the Outer Planets Program (grant NNX11AM37G). We also acknowledge NASA for a generous allocation of time on the "discover" supercomputing cluster. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. NR 169 TC 11 Z9 11 U1 1 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 JUN 10 PY 2015 VL 806 IS 1 AR 98 DI 10.1088/0004-637X/806/1/98 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300098 ER PT J AU Cohen, O Ma, Y Drake, JJ Glocer, A Garraffo, C Bell, JM Gombosi, TI AF Cohen, O. Ma, Y. Drake, J. J. Glocer, A. Garraffo, C. Bell, J. M. Gombosi, T. I. TI THE INTERACTION OF VENUS-LIKE, M-DWARF PLANETS WITH THE STELLAR WIND OF THEIR HOST STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); planets and satellites: atmospheres; planets and satellites: magnetic fields; planets and satellites: terrestrial planets ID RESISTIVE MHD SIMULATIONS; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; CLOSE-IN EXOPLANETS; MASS M-STARS; HABITABLE ZONES; HOT JUPITERS; GANYMEDES MAGNETOSPHERE; TERRESTRIAL EXOPLANETS; ATMOSPHERIC ESCAPE AB We study the interaction between the atmospheres of Venus-like, non-magnetized exoplanets orbiting an M-dwarf star, and the stellar wind using a multi-species MHD model. We focus our investigation on the effect of enhanced stellar wind and enhanced EUV flux as the planetary distance from the star decreases. Our simulations reveal different topologies of the planetary space environment for sub- and super-Alfvenic stellar wind conditions, which could lead to dynamic energy deposition into the atmosphere during the transition along the planetary orbit. We find that the stellar wind penetration for non-magnetized planets is very deep, up to a few hundreds of kilometers. We estimate a lower limit for the atmospheric mass-loss rate and find that it is insignificant over the lifetime of the planet. However, we predict that when accounting for atmospheric ion acceleration, a significant amount of the planetary atmosphere could be eroded over the course of a billion years. C1 [Cohen, O.; Drake, J. J.; Garraffo, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ma, Y.] Univ Calif Los Angeles, Inst Geophys & Planetary Phys, Los Angeles, CA 90024 USA. [Glocer, A.] NASA, GSFC, Greenbelt, MD 20771 USA. [Bell, J. M.] NIA, Ctr Planetary Atmospheres & Flight Sci, Hampton, VA 23666 USA. [Gombosi, T. I.] Univ Michigan, Ctr Space Environm Modeling, Ann Arbor, MI 48109 USA. RP Cohen, O (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Gombosi, Tamas/G-4238-2011; OI Gombosi, Tamas/0000-0001-9360-4951; Cohen, Ofer/0000-0003-3721-0215 FU Smithsonian Institution Consortium; Smithsonian Institute Competitive Grants Program for Science (CGPS) grant "Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?"; NASA Astrobiology Institute grant [NNX15AE05G]; NASA ESS; NASA ESTO-CT; NSF KDI; DoD MURI; NASA [NAS8-03060] FX We thank an anonymous referee for his/her useful comments. The work presented here was funded by the Smithsonian Institution Consortium for Unlocking the Mysteries of the Universe grant "Lessons from Mars: Are Habitable Atmospheres on Planets around M Dwarfs Viable?", by the Smithsonian Institute Competitive Grants Program for Science (CGPS) grant "Can Exoplanets Around Red Dwarfs Maintain Habitable Atmospheres?", and by NASA Astrobiology Institute grant NNX15AE05G. Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI. The simulations were performed on the Smithsonian Institute HYDRA cluster. J.J.D. was supported by NASA contract NAS8-03060 to the Chandra X-ray Center during the course of this research and thanks the Director, B. Wilkes, for continuing support and encouragement. NR 69 TC 7 Z9 7 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 41 DI 10.1088/0004-637X/806/1/41 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300041 ER PT J AU Grier, CJ Hall, PB Brandt, WN Trump, JR Shen, Y Vivek, M Ak, NF Chen, YG Dawson, KS Denney, KD Green, PJ Jiang, LH Kochanek, CS McGreer, ID Paris, I Peterson, BM Schneider, DP Tao, CL Wood-Vasey, WM Bizyaev, D Ge, J Kinemuchi, K Oravetz, D Pan, KK Simmons, A AF Grier, C. J. Hall, P. B. Brandt, W. N. Trump, J. R. Shen, Yue Vivek, M. Ak, N. Filiz Chen, Yuguang Dawson, K. S. Denney, K. D. Green, Paul J. Jiang, Linhua Kochanek, C. S. McGreer, Ian D. Paris, I. Peterson, B. M. Schneider, D. P. Tao, Charling Wood-Vasey, W. M. Bizyaev, Dmitry Ge, Jian Kinemuchi, Karen Oravetz, Daniel Pan, Kaike Simmons, Audrey TI THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: RAPID C (IV) BROAD ABSORPTION LINE VARIABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: kinematics and dynamics; galaxies: nuclei; quasars: absorption lines ID ACTIVE GALACTIC NUCLEI; X-RAY VARIABILITY; AGN FEEDBACK; DATA RELEASE; BLACK-HOLES; MULTIYEAR TIMESCALES; ASTRONOMICAL DATA; ATOMIC DATABASE; QUASAR FEEDBACK; TYPE-1 QUASARS AB We report the discovery of rapid variations of a high-velocity C (IV) broad absorption line trough in the quasar SDSS J141007.74+541203.3. This object was intensively observed in 2014 as a part of the Sloan Digital Sky Survey Reverberation Mapping Project, during which 32 epochs of spectroscopy were obtained with the Baryon Oscillation Spectroscopic Survey spectrograph. We observe significant (>4 sigma) variability in the equivalent width (EW) of the broad (similar to 4000 km s(-1) wide) C (IV) trough on rest-frame timescales as short as 1.20 days (similar to 29 hr), the shortest broad absorption line variability timescale yet reported. The EW varied by similar to 10% on these short timescales, and by about a factor of two over the duration of the campaign. We evaluate several potential causes of the variability, concluding that the most likely cause is a rapid response to changes in the incident ionizing continuum. If the outflow is at a radius where the recombination rate is higher than the ionization rate, the timescale of variability places a lower limit on the density of the absorbing gas of n(e) greater than or similar to 3.9 x 105 cm(-3). The broad absorption line variability characteristics of this quasar are consistent with those observed in previous studies of quasars, indicating that such short-term variability may in fact be common and thus can be used to learn about outflow characteristics and contributions to quasar/host-galaxy feedback scenarios. C1 [Grier, C. J.; Brandt, W. N.; Trump, J. R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Grier, C. J.; Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, Davey Lab 525, University Pk, PA 16802 USA. [Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Brandt, W. N.] Penn State Univ, Dept Phys, University Pk, PA 16802 USA. [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. [Shen, Yue; Jiang, Linhua] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Vivek, M.; Dawson, K. S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Ak, N. Filiz] Erciyes Univ, Dept Astron & Space Sci, Fac Sci, TR-38039 Kayseri, Turkey. [Chen, Yuguang] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. [Denney, K. D.; Kochanek, C. S.; Peterson, B. M.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Denney, K. D.; Kochanek, C. S.; Peterson, B. M.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Green, Paul J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McGreer, Ian D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Paris, I.] INAF, Osservatorio Astron Trieste, I-34131 Trieste, Italy. [Tao, Charling] Aix Marseille Univ, Ctr Phys Particules Marseille, CNRS, IN2P3, F-13288 Marseille 09, France. [Tao, Charling] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. [Bizyaev, Dmitry; Kinemuchi, Karen; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey] Apache Point Observ, Sunspot, NM USA. [Bizyaev, Dmitry; Kinemuchi, Karen; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey] New Mexico State Univ, Sunspot, NM USA. [Ge, Jian] Univ Florida, Dept Astron, Bryant Space Sci Ctr, Gainesville, FL 32611 USA. RP Grier, CJ (reprint author), Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM grier@psu.edu RI Brandt, William/N-2844-2015; Jiang, Linhua/H-5485-2016; OI Brandt, William/0000-0002-0167-2453; Jiang, Linhua/0000-0003-4176-6486; Grier, Catherine/0000-0001-9920-6057 FU NSF [AST-1108604, AST-1009756, AST-1008882]; V.M. Willaman Endowment; NSERC; NASA through Hubble Fellowship - Space Telescope Science Institute [51330, 51314]; NASA [NAS 5-26555]; NSF AAPF fellowship under NSF [AST-1302093]; 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 We thank A. Baskin for valuable discussions with regard to this work and also our anonymous referee for their helpful suggestions. We also thank Vahram Chavushyan for providing us with the original spectrum of this target taken in 1991. C.J.G. and W.N.B. acknowledge support from NSF grant AST-1108604 and the V.M. Willaman Endowment. P. B. H. is supported by NSERC. J.R.T. and Y.S. acknowledge support from NASA through Hubble Fellowship grants #51330 #51314, respectively, 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. KDD is supported by an NSF AAPF fellowship awarded under NSF grant AST-1302093. C.S.K. acknowledges the support of NSF grant AST-1009756. B.M.P. acknowledges support from NSF Grant AST-1008882 to The Ohio State University. 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 work has made use of the CHIANTI Atomic Database for Spectroscopic Diagnostics of Astrophysical Plasmas. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), and the University of Cambridge (UK). NR 75 TC 14 Z9 14 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 JUN 10 PY 2015 VL 806 IS 1 AR 111 DI 10.1088/0004-637X/806/1/111 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300111 ER PT J AU Guillochon, J Loeb, A AF Guillochon, James Loeb, Abraham TI THE FASTEST UNBOUND STARS IN THE UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gravitation ID MASSIVE BLACK-HOLE; HYPERVELOCITY BINARY STARS; DARK-MATTER HALOS; SGR A-ASTERISK; GALACTIC-CENTER; STELLAR-MASS; TIDAL INTERACTIONS; HOST GALAXIES; TEST PARTICLE; EJECTION AB The discovery of hypervelocity stars (HVSs) leaving our galaxy with speeds of nearly 10(3) km s(-1) has provided strong evidence of the existence of a massive compact object at the galaxy's center. HVSs ejected via the disruption of stellar binaries can occasionally yield a star with v(infinity) less than or similar to 10(4) km s(-1); here we show that this mechanism can be extended to massive black hole (MBH) mergers, where the secondary star is replaced by a MBH with mass M-2 greater than or similar to 10(5)M(circle dot). We find that stars that are originally bound to the secondary MBH are frequently ejected with v(infinity) > 10(4) km s(-1), and occasionally with velocities similar to 10(5) km s(-1) (one third the speed of light). For this reason we refer to stars ejected from these systems as "semi-relativistic" hypervelocity stars (SHSs). Bound to no galaxy, the velocities of these stars are so great that they can cross a significant fraction of the observable universe in the time since their ejection (several Gpc). We demonstrate that if a significant fraction of MBH mergers undergoes a phase in which their orbital eccentricity is greater than or similar to 0.5 and their periapse distance is tens of the primary's Schwarzschild radius, the space density of fast-moving (v(infinity) > 10(4) km s(-1)) SHSs may be as large as 10(3) Mpc(-3). Hundreds of SHSs will be giant stars that can be detected by future all-sky infrared surveys such as WFIRST or Euclid and proper motion surveys such as LSST, with spectroscopic follow-up being possible with the James Webb Space Telescope. C1 [Guillochon, James; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Guillochon, J (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM jguillochon@cfa.harvard.edu OI Guillochon, James/0000-0002-9809-8215 FU Einstein grant [PF3-140108]; NSF grant [AST-1312034, 1066293] FX We are thankful for fruitful discussions with F. Antonini, K. Batygin, A. Bogdan, W. Brown, C. Conroy, S. Genel, I. Ginsburg, P. Groot, M. Holman, S. Naoz, E. Ramirez-Ruiz, R. Sari, A. Sesana, D. Sijacki, J. Strader, and Y. Levin. We are especially grateful to M. C. Miller for extended discussions regarding the mechanism presented here, and to our referee, who provided a more direct derivation of the maximum speed for hypervelocity stars. This work was supported by the Einstein grant PF3-140108 (J.G.) and NSF grant AST-1312034 (A.L.). Much of this paper was written at the Aspen Center for Physics (NSF Grant #1066293), who we thank for their generous hospitality. NR 100 TC 5 Z9 5 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 124 DI 10.1088/0004-637X/806/1/124 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300124 ER PT J AU Haines, CP Pereira, MJ Smith, GP Egami, E Babul, A Finoguenov, A Ziparo, F McGee, SL Rawle, TD Okabe, N Moran, SM AF Haines, C. P. Pereira, M. J. Smith, G. P. Egami, E. Babul, A. Finoguenov, A. Ziparo, F. McGee, S. L. Rawle, T. D. Okabe, N. Moran, S. M. TI LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: evolution; galaxies: stellar content ID NEAR-INFRARED PROPERTIES; LOW-DENSITY ENVIRONMENTS; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; K-BAND PROPERTIES; VIRGO CLUSTER; SPIRAL GALAXIES; HALO MASS; STELLAR POPULATIONS; RADIAL-DISTRIBUTION AB We present a study of the spatial distribution and kinematics of star-forming galaxies in 30 massive clusters at 0.15 < z < 0.30, combining wide-field Spitzer 24 mu m and GALEX near-ultraviolet imaging with highly complete spectroscopy of cluster members. The fraction (f(SF)) of star-forming cluster galaxies rises steadily with cluster-centric radius, increasing fivefold by 2r(200), but remains well below field values even at 3r(200). This suppression of star formation at large radii cannot be reproduced by models in which star formation is quenched in infalling field galaxies only once they pass within r(200) of the cluster, but is consistent with some of them being first pre-processed within galaxy groups. Despite the increasing f(SF)-radius trend, the surface density of star-forming galaxies actually declines steadily with radius, falling similar to 15x from the core to 2r(200). This requires star formation to survive within recently accreted spirals for 2-3 Gyr to build up the apparent over-density of star-forming galaxies within clusters. The velocity dispersion profile of the star-forming galaxy population shows a sharp peak of 1.44 sigma(nu) at 0.3r(500), and is 10%-35% higher than that of the inactive cluster members at all cluster-centric radii, while their velocity distribution shows a flat, top-hat profile within r(500). All of these results are consistent with star-forming cluster galaxies being an infalling population, but one that must also survive similar to 0.5-2 Gyr beyond passing within r(200). By comparing the observed distribution of star-forming galaxies in the stacked caustic diagram with predictions from the Millennium simulation, we obtain a best-fit model in which star formation rates decline exponentially on quenching timescales of 1.73 +/- 0.25 Gyr upon accretion into the cluster. C1 [Haines, C. P.] Univ Chile, Dept Astron, Santiago, Chile. [Haines, C. P.; Pereira, M. J.; Egami, E.; Rawle, T. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Haines, C. P.; Smith, G. P.; Ziparo, F.; McGee, S. L.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Babul, A.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Finoguenov, A.] Univ Helsinki, Dept Phys, FI-0014 Helsinki, Finland. [Finoguenov, A.] Univ Maryland Baltimore Cty, Ctr Space Sci Technol, Baltimore, MD 21250 USA. [McGee, S. L.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Rawle, T. D.] ESA, European Space Astron Ctr, E-28691 Madrid, Spain. [Okabe, N.] ASIAA, Taipei 10617, Taiwan. [Moran, S. M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Okabe, N.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Okabe, N.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. RP Haines, CP (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM cphaines@das.uchile.cl OI Haines, Christopher/0000-0002-8814-8960 FU CONICYT Anillo project [ACT-1122]; Royal Society; Science and Technology Facilities Council; NASA [GO:40872]; National Science Foundation [AST-1211349] FX C.P.H. was funded by CONICYT Anillo project ACT-1122. G.P.S. acknowledges support from the Royal Society. F.Z. and G.P.S. acknowledge support from the Science and Technology Facilities Council. We acknowledge NASA funding for this project under the Spitzer program GO:40872. This work was supported in part by the National Science Foundation under grant No. AST-1211349. The Millennium simulation databases used in this paper and the web application providing online access to them were constructed as part of the activities of the German Astrophysical Virtual Observatory. NR 144 TC 23 Z9 23 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 101 DI 10.1088/0004-637X/806/1/101 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300101 ER PT J AU Huffenberger, KM Araujo, D Bischoff, C Buder, I Chinone, Y Cleary, K Kusaka, A Monsalve, R Naess, SK Newburgh, LB Reeves, R Ruud, TM Wehus, IK Zwart, JTL Dickinson, C Eriksen, HK Gaier, T Gundersen, JO Hasegawa, M Hazumi, M Miller, AD Radford, SJE Readhead, ACS Staggs, ST Tajima, O Thompson, KL AF Huffenberger, K. M. Araujo, D. Bischoff, C. Buder, I. Chinone, Y. Cleary, K. Kusaka, A. Monsalve, R. Naess, S. K. Newburgh, L. B. Reeves, R. Ruud, T. M. Wehus, I. K. Zwart, J. T. L. Dickinson, C. Eriksen, H. K. Gaier, T. Gundersen, J. O. Hasegawa, M. Hazumi, M. Miller, A. D. Radford, S. J. E. Readhead, A. C. S. Staggs, S. T. Tajima, O. Thompson, K. L. CA QUIET Collaboration TI THE Q/U IMAGING EXPERIMENT: POLARIZATION MEASUREMENTS OF RADIO SOURCES AT 43 AND 95 GHz SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; galaxies: active; galaxies: individual (Cen A, Pict A); methods: statistical; polarization ID ACTIVE GALACTIC NUCLEI; MICROWAVE BACKGROUND POLARIZATION; PROBE WMAP OBSERVATIONS; SCALE ROTATION MEASURES; HIGH-FREQUENCY; POINT SOURCES; EXTRAGALACTIC SOURCES; SOURCE CATALOG; FARADAYS FOG; BRIGHT AB We present polarization measurements of extragalactic radio sources observed during the cosmic microwave background polarization survey of the Q/U Imaging Experiment (QUIET), operating at 43 GHz (Q-band) and 95GHz (W-band). We examine sources selected at 20 GHz from the public, >40 mJy catalog of the Australia Telescope (AT20G) survey. There are similar to 480 such sources within QUIET's four low-foreground survey patches, including the nearby radio galaxies Centaurus A and Pictor A. The median error on our polarized flux density measurements is 30-40 mJy per Stokes parameter. At signal-to-noise ratio >3 significance, we detect linear polarization for seven sources in Q-band and six in W-band; only 1.3 +/- 1.1 detections per frequency band are expected by chance. For sources without a detection of polarized emission, we find that half of the sources have polarization amplitudes below 90 mJy (Q-band) and 106 mJy (W-band), at 95% confidence. Finally, we compare our polarization measurements to intensity and polarization measurements of the same sources from the literature. For the four sources with WMAP and Planck intensity measurements >1 Jy, the polarization fractions are above 1% in both QUIET bands. At high significance, we compute polarization fractions as much as 10%-20% for some sources, but the effects of source variability may cut that level in half for contemporaneous comparisons. Our results indicate that simple models-ones that scale a fixed polarization fraction with frequency-are inadequate to model the behavior of these sources and their contributions to polarization maps. C1 [Huffenberger, K. M.] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA. [Huffenberger, K. M.; Gundersen, J. O.] Univ Miami, Dept Phys, Coral Gables, FL 33146 USA. [Araujo, D.; Zwart, J. T. L.; Miller, A. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Araujo, D.; Zwart, J. T. L.; Miller, A. D.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Buder, I.; Tajima, O.] Univ Chicago, Kavli Inst Cosmol Phys, Dept Phys, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bischoff, C.; Buder, I.; Tajima, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bischoff, C.; Buder, I.] High Energy Accelerator Res Org KEK, Tsukuba, Ibaraki 3050801, Japan. [Chinone, Y.; Hasegawa, M.; Hazumi, M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Chinone, Y.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Kusaka, A.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Kusaka, A.] Princeton Univ, Joseph Henry Labs Phys, Princeton, NJ 08544 USA. [Kusaka, A.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Monsalve, R.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Naess, S. K.; Ruud, T. M.; Eriksen, H. K.] Univ Toronto, Dunlap Inst, Toronto, ON M5S 3H4, Canada. [Newburgh, L. B.] Univ Concepcion, Dept Astron, CePIA, Concepcion, Chile. [Reeves, R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wehus, I. K.; Gaier, T.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Zwart, J. T. L.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Dickinson, C.] Univ Oslo, Ctr Math Applicat, NO-0316 Oslo, Norway. [Thompson, K. L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Thompson, K. L.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. RP Huffenberger, KM (reprint author), Florida State Univ, Dept Phys, POB 3064350, Tallahassee, FL 32306 USA. EM huffenbe@physics.fsu.edu OI radford, simon/0000-0001-9113-1660; Huffenberger, Kevin/0000-0001-7109-0099; Bischoff, Colin/0000-0001-9185-6514; Zwart, Jonathan/0000-0002-4967-946X FU NSF [AST-0506648, PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, PHY-0551142]; KAKENHI [20244041, 20740158, 21111002]; PRODEX [C90284]; KIPAC Enterprise grant; Strategic Alliance for the Implementation of New Technologies (SAINT); Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Fermilab; Kavli Institute for Cosmological Physics; University of Chicago; JPL RTD program; ERC [307209] FX Bruce Winstein, who led the QUIET project, died in 2011, soon after observations concluded. The project's success owes a great debt to his intellectual and scientific leadership. Support for the QUIET instrument and operation was provided through the NSF cooperative agreement AST-0506648. Support was also provided by NSF awards PHY-0855887, PHY-0355328, AST-0448909, AST-1010016, and PHY-0551142; KAKENHI 20244041, 20740158, and 21111002; PRODEX C90284; a KIPAC Enterprise grant; and by the Strategic Alliance for the Implementation of New Technologies (SAINT). This research used resources of the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.; Some work was performed on the Joint Fermilab-KICP Supercomputing Cluster, supported by grants from Fermilab, the Kavli Institute for Cosmological Physics, and the University of Chicago. Some work was performed on the Abel Cluster, owned and maintained by the University of Oslo and NOTUR (the Norwegian High Performance Computing Consortium), and on the Central Computing System, owned and operated by the Computing Research Center at KEK. Portions of this work were performed at the Jet Propulsion Laboratory (JPL) and California Institute of Technology, operating under a contract with the National Aeronautics and Space Administration. The Q-band modules were developed using funding from the JPL R&TD program. We acknowledge the Northrop Grumman Corporation for collaboration in the development and fabrication of HEMT-based cryogenic temperature-compatible MMICs.; C.D. acknowledges an STFC Advanced Fellowship, an EU Marie-Curie IRG grant under the FP7 and an ERC Starting Grant (No. 307209). H. K. E. acknowledges an ERC Starting Grant under FP7. A. D. M. acknowledges a Sloan foundation fellowship. J. Z. gratefully acknowledges a South Africa National Research Foundation Square Kilometre Array Research Fellowship. NR 72 TC 1 Z9 1 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 112 DI 10.1088/0004-637X/806/1/112 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300112 ER PT J AU Kastner, JH Qi, CH Gorti, U Hily-Blant, P Oberg, K Forveille, T Andrews, S Wilner, D AF Kastner, Joel H. Qi, Chunhua Gorti, Uma Hily-Blant, Pierre Oberg, Karin Forveille, Thierry Andrews, Sean Wilner, David TI A RING OF C2H IN THE MOLECULAR DISK ORBITING TW Hya SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (TW Hya); stars: pre-main sequence ID PROTOPLANETARY DISKS; SUBMILLIMETER ARRAY; HYDRAE; LINE; CHEMISTRY; CO; EXCITATION; ACCRETION AB We have used the Submillimeter Array to image, at similar to 1.'' 5 resolution, C2H N = 3 -> 2 emission from the circumstellar disk orbiting the nearby (D = 54 pc), similar to 8 Myr-old, similar to 0.8 M-circle dot classical T Tauri star TW Hya. The SMA imaging reveals that the C2H emission exhibits a ring-like morphology. Based on a model in which the C2H column density follows a truncated radial power-law distribution, we find that the inner edge of the ring lies at similar to 45 AU, and that the ring extends to at least similar to 120 AU. Comparison with previous (single-dish) observations of C2H N = 4 -> 3 emission indicates that the C2H molecules are subthermally excited and, hence, that the emission arises from the relatively warm (T greater than or similar to 40 K), tenuous (n << 10(7) cm(-3)) upper atmosphere of the disk. Based on these results and comparisons of the SMA C2H map with previous submillimeter and scattered-light imaging, we propose that the C2H emission most likely traces particularly efficient photo-destruction of small grains and/or photodesorption and photodissociation of hydrocarbons derived from grain ice mantles in the surface layers of the outer disk. The presence of a C2H ring in the TW Hya disk hence likely serves as a marker of dust grain processing and radial and vertical grain size segregation within the disk. C1 [Kastner, Joel H.] Rochester Inst Technol, Sch Phys & Astron, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Kastner, Joel H.] Rochester Inst Technol, Lab Multiwavelength Astrophys, Rochester, NY 14623 USA. [Qi, Chunhua; Oberg, Karin; Andrews, Sean; Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gorti, Uma] SETI Inst, Mountain View, CA 94043 USA. [Gorti, Uma] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hily-Blant, Pierre; Forveille, Thierry] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Hily-Blant, Pierre; Forveille, Thierry] CNRS, IPAG, F-38000 Grenoble, France. [Hily-Blant, Pierre] Inst Univ France, F-38000 Grenoble, France. RP Kastner, JH (reprint author), Rochester Inst Technol, Sch Phys & Astron, Chester F Carlson Ctr Imaging Sci, 54 Lomb Mem Dr, Rochester, NY 14623 USA. EM jhk@cis.rit.edu OI Kastner, Joel/0000-0002-3138-8250 FU Smithsonian Institution; Academia Sinica; National Science Foundation [AST-1108950]; NASA Origins of Solar Systems grant [NNX11AK63] FX 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. We gratefully acknowledge Alexander Faure for providing electron impact rates for C2H, and we thank the anonymous referee for helpful comments and suggestions. This research is supported by National Science Foundation grant AST-1108950 to RIT and NASA Origins of Solar Systems grant NNX11AK63 to SAO. NR 34 TC 9 Z9 9 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 JUN 10 PY 2015 VL 806 IS 1 AR 75 DI 10.1088/0004-637X/806/1/75 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300075 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, Scott J. Bromley, Benjamin C. TI FORMATION OF SUPER-EARTH MASS PLANETS AT 125-250 AU FROM A SOLAR-TYPE STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: formation; planets and satellites: general; stars: solar-type ID KUIPER-BELT OBJECTS; TRANS-NEPTUNIAN OBJECTS; N-BODY SIMULATION; PROTOPLANETARY DISK STRUCTURES; GAS GIANT PLANETS; ANALOG HD 107146; 2003 VB12 SEDNA; DEBRIS DISKS; SIZE DISTRIBUTION; FOMALHAUT B AB We investigate pathways for the formation of icy super-Earth mass planets orbiting at 125-250 AU around a 1 M-circle dot star. An extensive suite of coagulation calculations demonstrates that swarms of 1 cm-10 m planetesimals can form super-Earth mass planets on timescales of 1-3 Gyr. Collisional damping of 10(-2)-10(2) cm particles during oligarchic growth is a highlight of these simulations. In some situations, damping initiates a second runaway growth phase where 1000-3000 km protoplanets grow to super-Earth sizes. Our results establish the initial conditions and physical processes required for in situ formation of super-Earth planets at large distances from the host star. For nearby dusty disks in HD 107146, HD 202628, and HD 207129, ongoing super-Earth formation at 80-150 AU could produce gaps and other structures in the debris. In the solar system, forming a putative planet X at alpha less than or similar to 300 AU (alpha greater than or similar to 1000 AU) requires a modest (very massive) protosolar nebula. C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA Astrophysics Theory and Origins of Solar Systems programs [NNX10AF35G]; NASA Outer Planets Program [NNX11AM37G] FX We acknowledge generous allotments of computer time on the NASA "discover" cluster. We thank the referee, K. Ohtsuki, for a constructive and thorough review. Advice and comments from T. Currie and M. Geller also greatly improved our presentation. Portions of this project were supported by the NASA Astrophysics Theory and Origins of Solar Systems programs through grant NNX10AF35G and the NASA Outer Planets Program through grant NNX11AM37G. NR 170 TC 23 Z9 23 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 42 DI 10.1088/0004-637X/806/1/42 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300042 ER PT J AU Lau, ET Nagai, D Avestruz, C Nelson, K Vikhlinin, A AF Lau, Erwin T. Nagai, Daisuke Avestruz, Camille Nelson, Kaylea Vikhlinin, Alexey TI MASS ACCRETION AND ITS EFFECTS ON THE SELF-SIMILARITY OF GAS PROFILES IN THE OUTSKIRTS OF GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: clusters: general; galaxies: clusters: intracluster medium; methods: numerical ID DARK-MATTER HALOES; ADAPTIVE-MESH REFINEMENT; SMOOTHED-PARTICLE HYDRODYNAMICS; COSMOLOGICAL SHOCK-WAVES; LARGE-SCALE STRUCTURE; X-RAY LUMINOSITY; NONTHERMAL PRESSURE; INTRACLUSTER MEDIUM; FORMATION HISTORY; ANALYTICAL-MODEL AB Galaxy clusters exhibit remarkable self-similar behavior which allows us to establish simple scaling relationships between observable quantities and cluster masses, making galaxy clusters useful cosmological probes. Recent X-ray observations suggested that self-similarity may be broken in the outskirts of galaxy clusters. In this work, we analyze a mass-limited sample of massive galaxy clusters from the Omega500 cosmological hydrodynamic simulation to investigate the self-similarity of the diffuse X-ray emitting intracluster medium (ICM) in the outskirts of galaxy clusters. We find that the self-similarity of the outer ICM profiles is better preserved if they are normalized with respect to the mean density of the universe, while the inner profiles are more self-similar when normalized using the critical density. However, the outer ICM profiles as well as the location of accretion shock around clusters are sensitive to their mass accretion rate, which causes the apparent breaking of self-similarity in cluster outskirts. We also find that the collisional gas does not follow the distribution of collisionless dark matter (DM) perfectly in the infall regions of galaxy clusters, leading to 10% departures in the gas-to-DM density ratio from the cosmic mean value. Our results have a number implications for interpreting observations of galaxy clusters in X-ray and through the Sunyaev-Zel'dovich effect, and their applications to cosmology. C1 [Lau, Erwin T.; Nagai, Daisuke; Avestruz, Camille] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Lau, Erwin T.; Nagai, Daisuke; Avestruz, Camille; Nelson, Kaylea] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Nagai, Daisuke; Nelson, Kaylea] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lau, ET (reprint author), Yale Univ, Dept Phys, New Haven, CT 06520 USA. EM erwin.lau@yale.edu OI Avestruz, Camille/0000-0001-8868-0810 FU NSF [AST-1412768, 1009811]; NASA ATP grant [NNX11AE07G]; NASA Chandra grants [GO213004B, TM4-15007X]; Research Corporation; NSF Graduate Student Research Fellowship; Alan D. Bromley Fellowship from Yale University FX We thank Benedikt Diemer, Oleg Gnedin, Eiichiro Komatsu, Andrey Kravtsov, Avi Loeb, Xun Shi, Andrew Wetzel, and the anonymous referee for useful discussion and/or comments on the manuscript. This work was supported in part by NSF grants AST-1412768 & 1009811, NASA ATP grant NNX11AE07G, NASA Chandra grants GO213004B and TM4-15007X, the Research Corporation, and by the facilities and staff of the Yale University Faculty of Arts and Sciences High Performance Computing Center. CA acknowledges support from the NSF Graduate Student Research Fellowship and Alan D. Bromley Fellowship from Yale University. NR 74 TC 12 Z9 12 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 68 DI 10.1088/0004-637X/806/1/68 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300068 ER PT J AU Lee, SH Patnaude, DJ Raymond, JC Nagataki, S Slane, PO Ellison, DC AF Lee, Shiu-Hang Patnaude, Daniel J. Raymond, John C. Nagataki, Shigehiro Slane, Patrick O. Ellison, Donald C. TI MODELING BRIGHT gamma-RAY AND RADIO EMISSION AT FAST CLOUD SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; gamma rays: ISM; ISM: supernova remnants; shock waves ID SUPERNOVA REMNANT W44; LARGE-AREA TELESCOPE; FAST COLLISIONLESS SHOCKS; MOLECULAR CLOUDS; X-RAY; CYGNUS LOOP; COSMIC-RAYS; FERMI-LAT; SNR W44; IC 443 AB Recent observations by the Large Area Telescope on board the Fermi satellite have revealed bright gamma-ray emission from middle-aged supernova remnants (SNRs) inside our Galaxy. These remnants, which also possess bright nonthermal radio shells, are often found to be interacting directly with surrounding gas clouds. We explore the nonthermal emission mechanism at these dynamically evolved SNRs by constructing a hydrodynamical model. Two scenarios of particle acceleration, either a re-acceleration of Galactic cosmic rays or an efficient nonlinear diffusive shock acceleration (NLDSA) of particles injected from downstream, are considered. Using parameters inferred from observations, our models are contrasted with the observed spectra of SNR W44. For the re-acceleration case, we predict a significant enhancement of radio and GeV emission as the SNR undergoes a transition into the radiative phase. If sufficiently strong magnetic turbulence is present in the molecular cloud, the re-acceleration scenario can explain the observed broadband spectral properties. The NLDSA scenario also succeeds in explaining the gamma-ray spectrum but fails to reproduce the radio spectral index. Efficient NLDSA also results in a significant post-shock non-thermal pressure that limits the compression during cooling and prevents the formation of a prominent dense shell. Some other interesting differences between the two models in hydrodynamical behavior and resulting spectral features are illustrated. C1 [Lee, Shiu-Hang] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Patnaude, Daniel J.; Raymond, John C.; Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Lee, Shiu-Hang; Nagataki, Shigehiro] RIKEN, Astrophys Big Bang Lab, Wako, Saitama 3510198, Japan. [Lee, Shiu-Hang; Nagataki, Shigehiro] Interdisciplinary Theoret Sci Res Grp, Wako, Saitama 3510198, Japan. RP Lee, SH (reprint author), Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM slee@astro.isas.jaxa.jp; dpatnaude@cfa.harvard.edu; jraymond@cfa.harvard.edu; shigehiro.nagataki@riken.jp; slane@cfa.harvard.edu; don_ellison@ncsu.edu FU JAXA International Top Young Fellowship; NASA [NAS8-03060, NNX11AE03G]; Smithsonian Institution's Competitive Grants for Science Program; Japan Society for the Promotion of Science [23340069, 24.02022, 25.03786, 25610056]; [HST-GO-13436] FX The authors are grateful to the anonymous referee for offering helpful suggestions on improving the manuscript. S.L. and D.C.E. express deep thanks to Andrei Bykov who provided valuable comments on the manuscript during a collaboration meeting at ISSI, Bern. S.L. acknowledges support from the JAXA International Top Young Fellowship, and the warm hospitality of the Harvard-Smithsonian Center for Astrophysics where a major part of this study was carried out under the SAO Visiting Scientist Program. D.J.P. and P.O.S. acknowledge support from NASA contract NAS8-03060. D.J.P. also acknowledges support from the Smithsonian Institution's Competitive Grants for Science Program. J.C.R. acknowledges support from grant HST-GO-13436. S.N. acknowledges support from the Japan Society for the Promotion of Science (Nos. 23340069, 24.02022, 25.03786 and 25610056). D.C.E acknowledges support from NASA grant NNX11AE03G. NR 80 TC 5 Z9 5 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 71 DI 10.1088/0004-637X/806/1/71 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300071 ER PT J AU Lehmer, BD Tyler, JB Hornschemeier, AE Wik, DR Yukita, M Antoniou, V Boggs, S Christensen, FE Craig, WW Hailey, CJ Harrison, FA Maccarone, TJ Ptak, A Stern, D Zezas, A Zhang, WW AF Lehmer, B. D. Tyler, J. B. Hornschemeier, A. E. Wik, D. R. Yukita, M. Antoniou, V. Boggs, S. Christensen, F. E. Craig, W. W. Hailey, C. J. Harrison, F. A. Maccarone, T. J. Ptak, A. Stern, D. Zezas, A. Zhang, W. W. TI THE 0.3-30 keV SPECTRA OF POWERFUL STARBURST GALAXIES: NuSTAR AND CHANDRA OBSERVATIONS OF NGC 3256 AND NGC 3310 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 3256 and NGC 3310); galaxies: starburst; galaxies: star formation; X-rays: galaxies ID X-RAY-EMISSION; STAR-FORMING GALAXIES; LUMINOUS INFRARED GALAXIES; XMM-NEWTON OBSERVATIONS; INITIAL MASS FUNCTION; MERGER NGC-3256; FORMATION HISTORY; CLUSTER FORMATION; SPIRAL GALAXIES; LOW-METALLICITY AB We present nearly simultaneous Chandra and NuSTAR observations of two actively star-forming galaxies within 50 Mpc: NGC 3256 and NGC 3310. Both galaxies are significantly detected by both Chandra and NuSTAR, which together provide the first-ever spectra of these two galaxies spanning 0.3-30 keV. The X-ray emission from both galaxies is spatially resolved by Chandra; we find that hot gas dominates the E < 1-3 keV emission while ultraluminous X-ray sources (ULXs) provide majority contributions to the emission at E > 1-3 keV. The NuSTAR galaxy-wide spectra of both galaxies follow steep power-law distributions with Gamma approximate to 2.6 at E > 5-7 keV. Using new and archival Chandra data, we search for signatures of heavily obscured or low luminosity active galactic nuclei (AGNs). We find that both NGC 3256 and NGC 3310 have X-ray detected sources coincident with nuclear regions; however, the steep NuSTAR spectra of both galaxies restricts these sources to be either low luminosity AGNs (L2-10 keV/L-Edd less than or similar to 10(-5)) or non-AGNs in nature (e.g., ULXs or crowded X-ray sources that reach L2-10 keV similar to 10(40) erg s(-1) cannot be ruled out). Combining our constraints on the 0.3-30 keV spectra of NGC 3256 and NGC 3310 with equivalent measurements for nearby star-forming galaxies M83 and NGC 253, we analyze the star formation rate (SFR) normalized spectra of these starburst galaxies. The spectra of all four galaxies show sharply declining power-law slopes at energies above 3-6 keV primarily due to ULX populations. Our observations therefore constrain the average spectral shape of galaxy-wide populations of luminous accreting binaries (i.e., ULXs). Interestingly, despite a completely different galaxy sample selection, emphasizing here a range of SFRs and stellar masses, these properties are similar to those of super-Eddington accreting ULXs that have been studied individually in a targeted NuSTAR ULX program. We also find that NGC 3310 exhibits a factor of approximate to 3-10 elevation of X-ray emission over the other star-forming galaxies due to a corresponding overabundance of ULXs. We argue that the excess of ULXs in NGC 3310 is most likely explained by the relatively low metallicity of the young stellar population in this galaxy, a property that is expected to produce an excess of luminous X-ray binaries for a given SFR. C1 [Lehmer, B. D.; Wik, D. R.; Yukita, M.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Lehmer, B. D.; Tyler, J. B.; Hornschemeier, A. E.; Wik, D. R.; Yukita, M.; Ptak, A.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tyler, J. B.] Catholic Univ Amer, Dept Phys, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Antoniou, V.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boggs, S.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94720 USA. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Harrison, F. A.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Maccarone, T. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Crete, Greece. [Zezas, A.] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece. RP Lehmer, BD (reprint author), Johns Hopkins Univ, Homewood Campus, Baltimore, MD 21218 USA. RI Boggs, Steven/E-4170-2015; Yukita, Mihoko/E-4135-2017; Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Boggs, Steven/0000-0001-9567-4224; Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 FU Chandra X-ray Center grant [GO4-15086 Z]; NASA ADAP grant [NNX13AI48G]; European Research Council under the European Union's Seventh Framework Programme (FP)/ERC Grant [617001]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We thank the anonymous referee for helpful comments, which have improved the quality of this paper. We gratefully acknowledge financial support from Chandra X-ray Center grant GO4-15086 Z (B.D.L., J.B.T.) and NASA ADAP grant NNX13AI48G (B.D.L.). A. Z. acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 617001. 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. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (Italy) and the California Institute of Technology (USA). NR 88 TC 3 Z9 3 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 126 DI 10.1088/0004-637X/806/1/126 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300126 ER PT J AU Lena, D Robinson, A Storchi-Bergman, T Schnorr-Muller, A Seelig, T Riffel, RA Nagar, NM Couto, GS Shadler, L AF Lena, D. Robinson, A. Storchi-Bergman, T. Schnorr-Mueller, A. Seelig, T. Riffel, R. A. Nagar, N. M. Couto, G. S. Shadler, L. TI THE COMPLEX GAS KINEMATICS IN THE NUCLEUS OF THE SEYFERT 2 GALAXY NGC 1386: ROTATION, OUTFLOWS, AND INFLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; galaxies: individual (NGC 1386); galaxies: kinematics and dynamics; galaxies: nuclei; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; NARROW-LINE REGION; SUPERMASSIVE BLACK-HOLE; HOST GALAXIES; MULTIOBJECT SPECTROGRAPH; CIRCUMNUCLEAR DUST; GASEOUS KINEMATICS; CENTRAL KILOPARSEC; ELLIPTIC GALAXIES; STREAMING MOTIONS AB We present optical integral field spectroscopy of the circum-nuclear gas of the Seyfert 2 galaxy NGC 1386. The data cover the central 7 '' x 9 '' (530 x 680 pc) at a spatial resolution of 0.'' 9 (68 pc), and the spectral range 5700-70000 angstrom at a resolution 66 km s(-1). The line emission is dominated by a bright central component, with two lobes extending approximate to 3 '' north and south of the nucleus. We identify three main kinematic components. The first has low velocity dispersion ((sigma) over bar approximate to 90 km s(-1)), extends over the whole field of view, and has a velocity field consistent with gas rotating in the galaxy disk. We interpret the lobes as resulting from photoionization of disk gas in regions where the active galactic nucleus radiation cones intercept the disk. The second has higher velocity dispersion ((sigma) over bar approximate to 200 km s(-1)) and is observed in the inner 150 pc around the continuum peak. This component is double peaked, with redshifted and blueshifted components separated by approximate to 500 km s(-1). Together with previous Hubble Space Telescope imaging, these features suggest the presence of a bipolar outflow for which we estimate a mass outflow rate of M greater than or similar to 0.1 M-circle dot yr(-1). The third component is revealed by velocity residuals associated with enhanced velocity dispersion and suggests that outflow and/or rotation is occurring approximately in the equatorial plane of the torus. A second system of velocity residuals may indicate the presence of streaming motions along dusty spirals in the disk. C1 [Lena, D.; Robinson, A.; Seelig, T.; Shadler, L.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Storchi-Bergman, T.; Couto, G. S.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Schnorr-Mueller, A.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Schnorr-Mueller, A.] Minist Educ Brazil, CAPES Fdn, BR-70040020 Braslia, Brazil. [Riffel, R. A.] Univ Fed Santa Maria, BR-97105900 Santa Maria, RS, Brazil. [Nagar, N. M.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Storchi-Bergman, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lena, D (reprint author), Rochester Inst Technol, Sch Phys & Astron, 84 Lomb Mem Dr, Rochester, NY 14623 USA. EM dxl1840@g.rit.edu FU National Science Foundation [AST-1108786]; FAPERGS [2366-2551/14-0]; CNPq [470090/2013-8, 302683/2013-5] FX We thank the anonymous referee for insightful comments, which helped improve the manuscript. D.L. thanks M. Richmond and D. Merritt for helpful discussions, W. Steffen, and N. Koning for their assistance in the use of the program Shape, and acknowledges support from the National Science Foundation under grant no. AST-1108786. R.A.R. acknowledges support from FAPERGS (project No. 2366-2551/14-0) and CNPq (project No. 470090/2013-8 and 302683/2013-5). This work is based on observations obtained 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 Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil), and south-eastCYT (Argentina). We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr) and 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. NR 83 TC 9 Z9 9 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 84 DI 10.1088/0004-637X/806/1/84 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300084 ER PT J AU Roediger, E Kraft, RP Nulsen, PEJ Forman, WR Machacek, M Randall, S Jones, C Churazov, E Kokotanekova, R AF Roediger, E. Kraft, R. P. Nulsen, P. E. J. Forman, W. R. Machacek, M. Randall, S. Jones, C. Churazov, E. Kokotanekova, R. TI STRIPPED ELLIPTICAL GALAXIES AS PROBES OF ICM PHYSICS. I. TAILS, WAKES, AND FLOW PATTERNS IN AND AROUND STRIPPED ELLIPTICALS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Virgo); galaxies: individual (M89); hydrodynamics; methods: numerical; X-rays: galaxies; X-rays: galaxies: clusters ID KELVIN-HELMHOLTZ INSTABILITIES; LOW REYNOLDS NUMBERS; VIRGO CLUSTER; X-RAY; COLD FRONTS; DARK-MATTER; CHANDRA OBSERVATIONS; LENTICULAR GALAXIES; SAURON PROJECT; FORNAX CLUSTER AB Elliptical cluster galaxies are progressively stripped of their atmospheres due to their motion through the intracluster medium (ICM). Deep X-ray observations reveal the fine-structure of the galaxy's remnant atmosphere and its gas tail and wake. This fine-structure depends on dynamic conditions (galaxy potential, initial gas contents, orbit through the host cluster), orbital stage (early infall, pre-/post-pericenter passage), and ICM plasma properties (thermal conductivity, viscosity, magnetic field structure). We aim to disentangle dynamic and plasma effects in order to use stripped ellipticals as probes of ICM plasma properties. This first paper of a series investigates the hydrodynamics of progressive gas stripping by means of inviscid hydrodynamical simulations. We distinguish a long-lasting initial relaxation phase and a quasi-steady stripping phase. During quasi-steady stripping, the ICM flow around the remnant atmosphere resembles the flow around solid bodies, including a "deadwater" region in the near wake. Gas is stripped from the remnant atmosphere predominantly at its sides via Kelvin-Helmholtz instabilities. The downstream atmosphere is largely shielded from the ICM wind and thus shaped into a tail. Observationally, both this "remnant tail" and the stripped gas in the wake can appear as a "tail", but only in the wake can galactic gas mix with the ambient ICM. While the qualitative results are generic, the simulations presented here are tailored to the Virgo elliptical galaxy M89 (NGC 4552) for the most direct comparison to observations. Papers II and III of this series describe the effect of viscosity and compare to Chandra and XMM-Newton observations, respectively. C1 [Roediger, E.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Roediger, E.; Kraft, R. P.; Nulsen, P. E. J.; Forman, W. R.; Machacek, M.; Randall, S.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Churazov, E.] MPI Astrophys, D-85741 Garching, Germany. [Kokotanekova, R.] Univ Innsbruck, AstroMundus Master Programme, A-6020 Innsbruck, Austria. RP Roediger, E (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojensbergsweg 112, D-21029 Hamburg, Germany. EM eroediger@hs.uni-hamburg.de RI Churazov, Eugene/A-7783-2013; OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU Priority Programme Physics of the ISM of the DFG (German Research Foundation); John-Neumann Institut at the Forschungszentrum Julich [NIC 6006, 6970]; Smithsonian Astrophysical Observatory FX The FLASH code was in part developed by the DOE NNSA-ASC OASCR Flash center at the University of Chicago. E.R. acknowledges the support of the Priority Programme Physics of the ISM of the DFG (German Research Foundation), the supercomputing grants NIC 6006 and 6970 at the John-Neumann Institut at the Forschungszentrum Julich, a visiting scientist fellowship of the Smithsonian Astrophysical Observatory, and the hospitality of the Center for Astrophysics in Cambridge. We are grateful for helpful discussions with Marcus Bruggen and Dominique Eckert. We also thank the referee for helpful comments regarding the presentation of our results. This research has made use of the GOLDMine Database. NR 64 TC 10 Z9 10 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 JUN 10 PY 2015 VL 806 IS 1 AR 103 DI 10.1088/0004-637X/806/1/103 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300103 ER PT J AU Roediger, E Kraft, RP Nulsen, PEJ Forman, WR Machacek, M Randall, S Jones, C Churazov, E Kokotanekova, R AF Roediger, E. Kraft, R. P. Nulsen, P. E. J. Forman, W. R. Machacek, M. Randall, S. Jones, C. Churazov, E. Kokotanekova, R. TI STRIPPED ELLIPTICAL GALAXIES AS PROBES OF ICM PHYSICS. II. STIRRED, BUT MIXED? VISCOUS AND INVISCID GAS STRIPPING OF THE VIRGO ELLIPTICAL M89 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (Virgo); galaxies: individual (M89); hydrodynamics; instabilities; plasmas; X-rays: galaxies: clusters ID COLD FRONTS; MAGNETOHYDRODYNAMIC SIMULATIONS; CHANDRA OBSERVATIONS; INTERGALACTIC MEDIUM; MAGNETIC-FIELDS; FORNAX CLUSTER; INSTABILITIES; EVOLUTION; NGC-1404; BUBBLES AB Elliptical galaxies moving through the intracluster medium (ICM) are progressively stripped of their gaseous atmospheres. X-ray observations reveal the structure of galactic tails, wakes, and the interface between the galactic gas and the ICM. This fine-structure depends on dynamic conditions (galaxy potential, initial gas contents, orbit in the host cluster), orbital stage (early infall, pre-/post-pericenter passage), as well as on the still ill-constrained ICM plasma properties (thermal conductivity, viscosity, magnetic field structure). Paper I describes flow patterns and stages of inviscid gas stripping. Here we study the effect of a Spitzer-like temperature dependent viscosity corresponding to Reynolds numbers, Re, of 50-5000 with respect to the ICM flow around the remnant atmosphere. Global flow patterns are independent of viscosity in this Reynolds number range. Viscosity influences two aspects. In inviscid stripping, Kelvin-Helmholtz instabilities (KHIs) at the sides of the remnant atmosphere lead to observable horns or wings. Increasing viscosity suppresses KHIs of increasing length scale and thus observable horns and wings. Furthermore, in inviscid stripping, stripped galactic gas can mix with the ambient ICM in the galaxy's wake. This mixing is suppressed increasingly with increasing viscosity, such that viscously stripped galaxies have long X-ray bright, cool wakes. We provide mock X-ray images for different stripping stages and conditions. While these qualitative results are generic, we tailor our simulations to the Virgo galaxy M89 (NGC 4552), where Re approximate to 50 corresponds to a viscosity of 10% of the Spitzer level. Paper III compares new deep Chandra and archival XMM-Newton data to our simulations. C1 [Roediger, E.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Roediger, E.; Kraft, R. P.; Nulsen, P. E. J.; Forman, W. R.; Machacek, M.; Randall, S.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Churazov, E.] MPI Astrophys, D-85741 Garching, Germany. [Kokotanekova, R.] Univ Innsbruck, AstroMundus Master Programme, A-6020 Innsbruck, Austria. RP Roediger, E (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojensbergsweg 112, D-21029 Hamburg, Germany. EM eroediger@hs.uni-hamburg.de RI Churazov, Eugene/A-7783-2013; OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU Priority Programme Physics of the ISM of the DFG (German Research Foundation); John-Neumann Institut at the Forschungszentrum Julich [NIC 6006, 6970]; Smithsonian Astrophysical Observatory FX The FLASH code was in part developed by the DOE NNSA-ASC OASCR Flash center at the University of Chicago. E.R. acknowledges the support of the Priority Programme Physics of the ISM of the DFG (German Research Foundation), the supercomputing grants NIC 6006 and 6970 at the John-Neumann Institut at the Forschungszentrum Julich, a visiting scientist fellowship of the Smithsonian Astrophysical Observatory, and the hospitality of the Center for Astrophysics in Cambridge. We also thank the referee for helpful comments regarding the presentation of our results. NR 30 TC 8 Z9 8 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 JUN 10 PY 2015 VL 806 IS 1 AR 104 DI 10.1088/0004-637X/806/1/104 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300104 ER PT J AU Rugheimer, S Segura, A Kaltenegger, L Sasselov, D AF Rugheimer, S. Segura, A. Kaltenegger, L. Sasselov, D. TI UV SURFACE ENVIRONMENT OF EARTH-LIKE PLANETS ORBITING FGKM STARS THROUGH GEOLOGICAL EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; Earth; planets and satellites: surfaces; planets and satellites: terrestrial planets ID HABITABLE ZONE; ULTRAVIOLET-RADIATION; ARCHEAN ATMOSPHERE; M DWARF; NM; CANDIDATES; CHEMISTRY; LIGHT; INACTIVATION; REQUIREMENTS AB The UV environment of a host star affects the photochemistry in the atmosphere, and ultimately the surface UV environment for terrestrial planets and therefore the conditions for the origin and evolution of life. We model the surface UV radiation environment for Earth-sized planets orbiting FGKM stars in the circumstellar Habitable Zone for Earth through its geological evolution. We explore four different types of atmospheres corresponding to an early-Earth atmosphere at 3.9 Gyr ago and three atmospheres covering the rise of oxygen to present-day levels at 2.0 Gyr ago, 0.8 Gyr ago, and modern Earth. In addition to calculating the UV flux on the surface of the planet, we model the biologically effective irradiance, using DNA damage as a proxy for biological damage. We find that a pre-biotic Earth (3.9 Gyr ago) orbiting an F0V star receives 6 times the biologically effective radiation as around the early Sun and 3520 times the modern Earth-Sun levels. A pre-biotic Earth orbiting GJ 581 (M3.5 V) receives 300 times less biologically effective radiation, about 2 times modern Earth-Sun levels. The UV fluxes calculated here provide a grid of model UV environments during the evolution of an Earth-like planet orbiting a range of stars. These models can be used as inputs into photo-biological experiments and for pre-biotic chemistry and early life evolution experiments. C1 [Rugheimer, S.; Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Segura, A.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. [Rugheimer, S.; Kaltenegger, L.] Cornell Univ, Carl Sagan Inst, Ithaca, NY 14853 USA. RP Rugheimer, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM srugheimer@cfa.harvard.edu OI Rugheimer, Sarah/0000-0003-1620-7658 FU DFG [ENP KA 3142/1-1]; Simons Foundation [290357, 290360] FX We would like to thank Kevin France for discussions concerning the MUSCLES database and Sukrit Ranjan for discussions concerning DNA action specta. This work has made use of the MUSCLES M dwarf UV radiation field database. We would also like to acknowledge support from DFG funding ENP KA 3142/1-1 and the Simons Foundation (290357, Kaltenegger and 290360, Sasselov). NR 61 TC 6 Z9 6 U1 1 U2 17 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 JUN 10 PY 2015 VL 806 IS 1 AR 137 DI 10.1088/0004-637X/806/1/137 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300137 ER PT J AU Sand, DJ Crnojevic, D Bennet, P Willman, B Hargis, J Strader, J Olszewski, E Tollerud, EJ Simon, JD Caldwell, N Guhathakurta, P James, BL Koposov, S McLeod, B Morrell, N Peacock, M Salinas, R Seth, AC Stark, DP Toloba, E AF Sand, D. J. Crnojevic, D. Bennet, P. Willman, B. Hargis, J. Strader, J. Olszewski, E. Tollerud, E. J. Simon, J. D. Caldwell, N. Guhathakurta, P. James, B. L. Koposov, S. McLeod, B. Morrell, N. Peacock, M. Salinas, R. Seth, A. C. Stark, D. P. Toloba, E. TI A COMPREHENSIVE ARCHIVAL SEARCH FOR COUNTERPARTS TO ULTRA-COMPACT HIGH-VELOCITY CLOUDS: FIVE LOCAL VOLUME DWARF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: individual (ALFALFA-Dw1, GALFA-Dw1, GALFA-Dw2, GALFA-Dw3, GALFA-Dw4); radio lines: galaxies ID DIGITAL SKY SURVEY; MILKY-WAY SATELLITES; FAST ALPHA SURVEY; H I OBSERVATIONS; ALFALFA DISCOVERY; VIRGO CLUSTER; DATA RELEASE; DISTANCE DETERMINATIONS; STRUCTURAL-PROPERTIES; STAR-FORMATION AB We report five Local Volume dwarf galaxies (two of which are presented here for the first time) uncovered during a comprehensive archival search for optical counterparts to ultra-compact high-velocity clouds (UCHVCs). The UCHVC population of HI clouds are thought to be candidate gas-rich, low-mass halos at the edge of the Local Group and beyond, but no comprehensive search for stellar counterparts to these systems has been presented. Careful visual inspection of all publicly available optical and ultraviolet imaging at the position of the UCHVCs revealed six blue, diffuse counterparts with a morphology consistent with a faint dwarf galaxy beyond the Local Group. Optical spectroscopy of all six candidate dwarf counterparts show that five have an H alpha-derived velocity consistent with the coincident HI cloud, confirming their association; the sixth diffuse counterpart is likely a background object. The size and luminosity of the UCHVC dwarfs is consistent with other known Local Volume dwarf irregular galaxies. The gas fraction (M-HI/M-star) of the five dwarfs are generally consistent with that of dwarf irregular galaxies in the Local Volume, although ALFALFA-Dw1 (associated with ALFALFA UCHVC HVC274.68+74.70-123) has a very high M-HI/M-star similar to 40. Despite the heterogenous nature of our search, we demonstrate that the current dwarf companions to UCHVCs are at the edge of detectability due to their low surface brightness, and that deeper searches are likely to find more stellar systems. If more sensitive searches do not reveal further stellar counterparts to UCHVCs, then the dearth of such systems around the Local Group may be in conflict with Lambda CDM simulations. C1 [Sand, D. J.; Crnojevic, D.; Bennet, P.; Toloba, E.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Willman, B.; Hargis, J.] Haverford Coll, Dept Phys, Haverford, PA 19041 USA. [Strader, J.; Peacock, M.; Salinas, R.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Olszewski, E.; Stark, D. P.] Univ Arizona, Tucson, AZ 85721 USA. [Tollerud, E. J.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Simon, J. D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [James, B. L.; Koposov, S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Caldwell, N.; McLeod, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morrell, N.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Guhathakurta, P.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. [Seth, A. C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Sand, DJ (reprint author), Texas Tech Univ, Dept Phys, Box 41051, Lubbock, TX 79409 USA. EM david.sand@ttu.edu RI Koposov, Sergey/F-2754-2012; OI Koposov, Sergey/0000-0003-2644-135X; Tollerud, Erik/0000-0002-9599-310X; Salinas, Ricardo/0000-0002-1206-1930; Seth, Anil/0000-0003-0248-5470 FU NSF [AST-1412504, AST-1151462, AST-1010039, AST-1313006]; Space Telescope Science Institute under U.S. Government grant [NAG W-2166]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy Office of Science; Robert Martin Ayers Sciences Fund FX We warmly thank Maureen Conroy, John Roll, and Sean Moran for their prolonged efforts and help related to Magellan/Megacam. We thank Alison Marqusee, Chris Nagele, and Eric Smith for assistance obtaining ARC 3.5 m observations. We are also grateful to Elizabeth Adams for useful comments. D.J.S., J.D.S. and P.G. acknowledge support from NSF grant AST-1412504. B.W. and J.H. acknowledge support from NSF AST-1151462. P.G. acknowledges additional support from NSF grant AST-1010039. E.O. thanks the NSF for support through AST-1313006. The Digitized Sky Surveys were 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 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. 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/. Based in part on data collected at the Subaru Telescope and obtained from SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan. This research was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund. Observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). NR 78 TC 12 Z9 12 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 95 DI 10.1088/0004-637X/806/1/95 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300095 ER PT J AU Villaume, A Conroy, C Johnson, BD AF Villaume, Alexa Conroy, Charlie Johnson, Benjamin D. TI CIRCUMSTELLAR DUST AROUND AGB STARS AND IMPLICATIONS FOR INFRARED EMISSION FROM GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: stellar content; infrared: galaxies; stars: AGB and post-AGB ID ASYMPTOTIC GIANT BRANCH; LARGE-MAGELLANIC-CLOUD; SPECTRAL ENERGY-DISTRIBUTIONS; MASS-LOSS RETURN; OLD STELLAR POPULATIONS; SURFACE BRIGHTNESS FLUCTUATIONS; COLOR-MAGNITUDE DIAGRAMS; POST-STARBURST GALAXIES; EVOLVED STARS; TP-AGB AB Stellar population synthesis (SPS) models are used to infer many galactic properties including star formation histories, metallicities, and stellar and dust masses. However, most SPS models neglect the effect of circumstellar dust shells around evolved stars and it is unclear to what extent they impact the analysis of spectral energy distributions (SEDs). To overcome this shortcoming we have created a new set of circumstellar dust models, using the radiative transfer code DUSTY, for asymptotic giant branch (AGB) stars and incorporated them into the Flexible Stellar Population Synthesis code. The circumstellar dust models provide a good fit to individual AGB stars as well as the IR color-magnitude diagrams of the Large and Small Magellanic Clouds. IR luminosity functions from the Large and Small Magellanic Clouds are not well-fit by the 2008 Padova isochrones when coupled to our circumstellar dust models and so we adjusted the lifetimes of AGB stars in the models to provide a match to the data. We show, in agreement with previous work, that circumstellar dust from AGB stars can make a significant contribution to the IR (greater than or similar to 4 mu m) emission from galaxies that contain relatively little diffuse dust, including low-metallicity and/or non-star-forming galaxies. Our models provide a good fit to the mid-IR spectra of early-type galaxies. Circumstellar dust around AGB stars appears to have a small effect on the IR SEDs of metal-rich star-forming galaxies (i.e., when A(V) greater than or similar to 0.1). Stellar population models that include circumstellar dust will be needed to accurately interpret data from the James Webb Space Telescope and other IR facilities. C1 [Villaume, Alexa] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Conroy, Charlie; Johnson, Benjamin D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Villaume, A (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. EM avillaum@ucsc.edu OI Villaume, Alexa/0000-0003-1887-0621 FU NASA grant [NNX13AI46G] FX We would like to thank Martha Boyer, Martin Groenewegen, Dan Kelson, Ivo Labbe, Sundar Srinivasan, Benjamin Sargent, and Roberto Rampazzo for generously sharing their data, and Paul Martini, Dan Kelson, and Julianne Dalcanton for fruitful conversations on this topic. We also thank the anonymous referee for the thoughtful comments that improved the quality of this manuscript. This project was supported in part by NASA grant NNX13AI46G. NR 98 TC 13 Z9 13 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 82 DI 10.1088/0004-637X/806/1/82 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300082 ER PT J AU Whalen, TJ Hickox, RC Reines, AE Greene, JE Sivakoff, GR Johnson, KE Alexander, DM Goulding, AD AF Whalen, Thomas J. Hickox, Ryan C. Reines, Amy E. Greene, Jenny E. Sivakoff, Gregory R. Johnson, Kelsey E. Alexander, David M. Goulding, Andy D. TI VARIABLE HARD-X-RAY EMISSION FROM THE CANDIDATE ACCRETING BLACK HOLE IN DWARF GALAXY HENIZE 2-10 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: dwarf; galaxies: evolution; galaxies: individual (Henize 2-10); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; RADIO-EMISSION; NGC 4051; MASS; CHANDRA; VARIABILITY; SUPERNOVAE; SIGNATURES; SEYFERT; VLBI AB We present an analysis of the X-ray spectrum and long-term variability of the nearby dwarf starburst galaxy Henize 2-10. Recent observations suggest that this galaxy hosts an actively accreting black hole (BH) with mass. similar to 10(6) M-circle dot. The presence of an active galactic nucleus (AGN) in a low-mass starburst galaxy marks a new environment for AGNs, with implications for the processes by which "seed" BHs may form in the early universe. In this paper, we analyze four epochs of X-ray observations of Henize 2-10, to characterize the long-term behavior of its hard nuclear emission. We analyze observations with Chandra from 2001 and XMM-Newton from 2004 and 2011, as well as an earlier, less sensitive observation with ASCA from 1997. Based on a detailed analysis of the source and background, we find that the hard (2-10 keV) flux of the putative AGN has decreased by approximately an order of magnitude between the 2001 Chandra observation and exposures with XMM-Newton in 2004 and 2011. The observed variability confirms that the emission is due to a single source. It is unlikely that the variable flux is due to a supernova or ultraluminous X-ray source, based on the observed long-term behavior of the X-ray and radio emission, while the observed X-ray variability is consistent with the behavior of well-studied AGNs. C1 [Whalen, Thomas J.; Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Whalen, Thomas J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reines, Amy E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Greene, Jenny E.; Goulding, Andy D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Sivakoff, Gregory R.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Johnson, Kelsey E.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Whalen, TJ (reprint author), Dartmouth Coll, Dept Phys & Astron, 6127 Wilder Lab, Hanover, NH 03755 USA. EM ryan.c.hickox@dartmouth.edu RI Sivakoff, Gregory/G-9602-2011 OI Sivakoff, Gregory/0000-0001-6682-916X FU NASA [PF1-120086]; Hubble Fellowship Program; Dartmouth College Class of Faculty Fellowship; NSERC FX Support for A.E.R. was provided by NASA through the Einstein Fellowship Program, grant PF1-120086, and the Hubble Fellowship Program. R.C.H. acknowledges support from the Dartmouth College Class of 1962 Faculty Fellowship. G.R.S. acknowledges support from an NSERC Discovery Grant. This research has made use of data, software and/or web tools obtained from NASA's High Energy Astrophysics Science Archive Research Center (HEASARC), a service of Goddard Space Flight Center and the Smithsonian Astrophysical Observatory. NR 35 TC 5 Z9 5 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 37 DI 10.1088/0004-637X/806/1/37 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300037 ER PT J AU Wu, JF Orosz, JA McClintock, JE Steeghs, D Longa-Pena, P Callanan, PJ Gou, L Ho, LC Jonker, PG Reynolds, MT Torres, MAP AF Wu, Jianfeng Orosz, Jerome A. McClintock, Jeffrey E. Steeghs, Danny Longa-Pena, Penelope Callanan, Paul J. Gou, Lijun Ho, Luis C. Jonker, Peter G. Reynolds, Mark T. Torres, Manuel A. P. TI A DYNAMICAL STUDY OF THE BLACK HOLE X-RAY BINARY NOVA MUSCAE 1991 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; black hole physics; stars: black holes; X-rays: binaries ID ADVECTION-DOMINATED ACCRETION; INFRARED OBSERVATIONS; NEUTRON-STAR; MASS; A0620-00; ANNIHILATION; NOVA-MUSCAE-1991; SPECTROSCOPY; PARAMETERS; EMISSION AB We present a dynamical study of the Galactic black hole binary system Nova Muscae 1991 (GS/GRS 1124-683). We utilize 72 high-resolution Magellan Echellette spectra and 72 strictly simultaneous V-band photometric observations; the simultaneity is a unique and crucial feature of this dynamical study. The data were taken on two consecutive nights and cover the full 10.4 hr orbital cycle. The radial velocities of the secondary star are determined by cross-correlating the object spectra with the best-match template spectrum obtained using the same instrument configuration. Based on our independent analysis of five orders of the echellette spectrum, the semi-amplitude of the radial velocity of the secondary is measured to be K-2= 406.8 +/- 2.7 km s(-1), which is consistent with previous work, while the uncertainty is reduced by a factor of 3. The corresponding mass function is f(M)= 3.02 +/- 0.06M(circle dot). We have also obtained an accurate measurement of the rotational broadening of the stellar absorption lines (v sin i= 85.0 +/- 2.6 km s(-1)), and hence the mass ratio of the system q=0.079 +/- 0.007. Finally, we have measured the spectrum of the non-stellar component of emission that veils the spectrum of the secondary. In a future paper, we will use our veiling-corrected spectrum of the secondary and accurate values of K-2 and q to model multi-color light curves and determine the systemic inclination and the mass of the black hole. C1 [Wu, Jianfeng; McClintock, Jeffrey E.; Steeghs, Danny; Jonker, Peter G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Steeghs, Danny; Longa-Pena, Penelope] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Callanan, Paul J.] Natl Univ Ireland Univ Coll Cork, Dept Phys, Cork, Ireland. [Gou, Lijun] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Ho, Luis C.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Ho, Luis C.] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China. [Jonker, Peter G.; Torres, Manuel A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Torres, Manuel A. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Reynolds, Mark T.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. RP Wu, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jianfeng.wu@cfa.harvard.edu OI Wu, Jianfeng/0000-0001-7349-4695 FU NASA grant [NNX11AD08G]; Science and Technology Facilities Council [ST/L000733/1]; Chinese Academy of Sciences from the Strategic Priority Research Program [XDB09000000]; National Natural Science Foundation of China [11333005, 11473002]; National Astronomical Observatories of China [Y234031001] FX We thank the anonymous referee for a careful reading of the manuscript and helpful comments. We thank T. Marsh for developing and sharing the MOLLY spectral analysis software. J.E.M. acknowledges the support of NASA grant NNX11AD08G. D.S. acknowledges support from the Science and Technology Facilities Council, grant number ST/L000733/1. L.J.G. and L.C.H. acknowledge the support by the Chinese Academy of Sciences through grant No. XDB09000000 (Emergence of Cosmological Structures) from the Strategic Priority Research Program. L.J.G. acknowledges the support by National Natural Science Foundation of China (grant No. 11333005) and by National Astronomical Observatories of China (grant No. Y234031001). L.C.H. acknowledge the support by the National Natural Science Foundation of China through grant No. 11473002. NR 44 TC 4 Z9 4 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 92 DI 10.1088/0004-637X/806/1/92 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300092 ER PT J AU Zahid, HJ Damjanov, I Geller, MJ Chilingarian, I AF Zahid, H. Jabran Damjanov, Ivana Geller, Margaret J. Chilingarian, Igor TI QUIESCENT COMPACT GALAXIES AT INTERMEDIATE REDSHIFT IN THE COSMOS FIELD. II. THE FUNDAMENTAL PLANE OF MASSIVE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: structure ID SIMILAR-TO 2; DIGITAL SKY SURVEY; STELLAR POPULATION SYNTHESIS; HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; ELLIPTIC GALAXIES; SIZE EVOLUTION; NUMBER DENSITY; STAR-FORMATION; DISK GALAXIES AB We examine the relation between surface brightness, velocity dispersion, and size-the fundamental plane (FP)for quiescent galaxies at intermediate redshifts in the COSMOS field. The COSMOS sample consists of similar to 150 massive quiescent galaxies with an average velocity dispersion of. sigma similar to 250 km s(-1) and redshifts between 0.2 < z < 0.8. More than half of the galaxies in the sample are compact. The COSMOS galaxies exhibit a tight relation (similar to 0.1 dex scatter) between surface brightness, velocity dispersion, and size. At a fixed combination of velocity dispersion and size, the COSMOS galaxies are brighter than galaxies in the local universe. These surface brightness offsets are correlated with the rest-frame g - z color and D(n)4000 index; bluer galaxies and those with smaller D(n)4000 indices have larger offsets. Stellar population synthesis models indicate that the massive COSMOS galaxies are younger and therefore brighter than similarly massive quiescent galaxies in the local universe. Passive evolution alone brings the massive compact quiescent (MCQ) COSMOS galaxies onto the local FP at z = 0. Therefore, evolution in size or velocity dispersion for MCQ galaxies since z similar to 1 is constrained by the small scatter observed in the FP. We conclude that MCQ galaxies at z less than or similar to 1 are not a special class of objects but rather the tail of the mass and size distribution of the normal quiescent galaxy population. C1 [Zahid, H. Jabran; Geller, Margaret J.; Chilingarian, Igor] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Damjanov, Ivana] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chilingarian, Igor] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. RP Zahid, HJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM zahid@cfa.harvard.edu RI Chilingarian, Igor/N-5117-2016 OI Chilingarian, Igor/0000-0002-7924-3253 FU Clay Postdoctoral Fellowship; Harvard College Observatory Menzel Fellowship; Natural Sciences and Engineering Research Council of Canada [NSERC PDF-421224-2012]; Russian Science Foundation project [14-22-00041]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; NASA [NAS 5-26555]; 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 FX We thank the anonymous referee for a careful reading of the manuscript. H.J.Z. gratefully acknowledges the generous support of the Clay Postdoctoral Fellowship. I.D. is supported by the Harvard College Observatory Menzel Fellowship and the Natural Sciences and Engineering Research Council of Canada Postdoctoral Fellowship (NSERC PDF-421224-2012). I.C. acknowledges support from the Russian Science Foundation project #14-22-00041. This research has made use of NASA's Astrophysics Data System Bibliographic Services.; 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.; 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. NR 72 TC 5 Z9 5 U1 0 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 JUN 10 PY 2015 VL 806 IS 1 AR 122 DI 10.1088/0004-637X/806/1/122 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL2XF UT WOS:000356810300122 ER PT J AU Cernicharo, J McCarthy, MC Gottlieb, CA Agundez, M Prieto, LV Baraban, JH Changala, PB Guelin, M Kahane, C Martin-Drumel, MA Patel, NA Reilly, NJ Stanton, JF Quintana-Lacaci, G Thorwirth, S Young, KH AF Cernicharo, J. McCarthy, M. C. Gottlieb, C. A. Agundez, M. Prieto, L. Velilla Baraban, J. H. Changala, P. B. Guelin, M. Kahane, C. Martin-Drumel, M. A. Patel, N. A. Reilly, N. J. Stanton, J. F. Quintana-Lacaci, G. Thorwirth, S. Young, K. H. TI DISCOVERY OF SiCSi IN IRC+10216: A MISSING LINK BETWEEN GAS AND DUST CARRIERS OF Si-C BONDS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrochemistry; stars: AGB and post-AGB; stars: carbon; stars: individual (IRC, 10216) ID ASTRONOMICAL IDENTIFICATION; SUPERNOVA 1987A; SUBMILLIMETER; ANION AB We report the discovery in space of a disilicon species, SiCSi, from observations between 80 and 350 GHz with the IRAM 30 m radio telescope. Owing to the close coordination between laboratory experiments and astrophysics, 112 lines have now been detected in the carbon-rich star CW Leo. The derived frequencies yield improved rotational and centrifugal distortion constants up to sixth order. From the line profiles and interferometric maps with the Submillimeter Array, the bulk of the SiCSi emission arises from a region of 6. in radius. The derived abundance is comparable to that of SiC2. As expected from chemical equilibrium calculations, SiCSi and SiC2 are the most abundant species harboring a Si-C bond in the dust formation zone and certainly both play a key role in the formation of SiC dust grains. C1 [Cernicharo, J.; Agundez, M.; Prieto, L. Velilla; Quintana-Lacaci, G.] CSIC, ICMM, Grp Mol Astrophys, E-28049 Madrid, Spain. [McCarthy, M. C.; Gottlieb, C. A.; Martin-Drumel, M. A.; Patel, N. A.; Reilly, N. J.; Young, K. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, M. C.; Gottlieb, C. A.; Martin-Drumel, M. A.; Patel, N. A.; Young, K. H.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Baraban, J. H.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Changala, P. B.] Natl Inst Stand & Technol, JILA, Boulder, CO 80309 USA. [Changala, P. B.] Univ Colorado, Boulder, CO 80309 USA. [Changala, P. B.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Guelin, M.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Kahane, C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Kahane, C.] CNRS, IPAG, F-38000 Grenoble, France. [Reilly, N. J.] Marquette Univ, Dept Chem, Milwaukee, WI 53233 USA. [Stanton, J. F.] Univ Texas Austin, Dept Chem, Inst Theoret Chem, Austin, TX 78712 USA. [Thorwirth, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Cernicharo, J (reprint author), CSIC, ICMM, Grp Mol Astrophys, C Sor Juana Ines Cruz N3, E-28049 Madrid, Spain. RI Agundez, Marcelino/I-5369-2012; Thorwirth, Sven/C-6217-2011; OI Agundez, Marcelino/0000-0003-3248-3564; Thorwirth, Sven/0000-0001-8200-6710; Martin-Drumel, Marie-Aline/0000-0002-5460-4294; Velilla Prieto, Luis/0000-0001-8275-9341; Cernicharo, Jose/0000-0002-3518-2524; Quintana-Lacaci, Guillermo/0000-0002-5417-1943 FU spanish MINECO [AYA2009-07304, AYA2012-32032, CSD2009-00038]; ERC [ERC-2013-SyG]; NASA [NNX13AE59G]; NANOCOSMOS [610256] FX We thank spanish MINECO for funding under grants AYA2009-07304, AYA2012-32032, CSD2009-00038, and ERC under ERC-2013-SyG, G. A. 610256 NANOCOSMOS. The new laboratory measurements in Cambridge were supported by NASA grant NNX13AE59G. NR 37 TC 7 Z9 7 U1 2 U2 15 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 JUN 10 PY 2015 VL 806 IS 1 AR L3 DI 10.1088/2041-8205/806/1/L3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0LH UT WOS:000356633700003 ER PT J AU Fransson, C Larsson, J Migotto, K Pesce, D Challis, P Chevalier, RA France, K Kirshner, RP Leibundgut, B Lundqvist, P McCray, R Spyromilio, J Taddia, F Jerkstrand, A Mattila, S Smith, N Sollerman, J Wheeler, JC Crotts, A Garnavich, P Heng, K Lawrence, SS Panagia, N Pun, CSJ Sonneborn, G Sugerman, B AF Fransson, Claes Larsson, Josefin Migotto, Katia Pesce, Dominic Challis, Peter Chevalier, Roger A. France, Kevin Kirshner, Robert P. Leibundgut, Bruno Lundqvist, Peter McCray, Richard Spyromilio, Jason Taddia, Francesco Jerkstrand, Anders Mattila, Seppo Smith, Nathan Sollerman, Jesper Wheeler, J. Craig Crotts, Arlin Garnavich, Peter Heng, Kevin Lawrence, Stephen S. Panagia, Nino Pun, Chun S. J. Sonneborn, George Sugerman, Ben TI THE DESTRUCTION OF THE CIRCUMSTELLAR RING OF SN 1987A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE circumstellar matter; shock waves; supernovae: individual (SN 1987A) ID SUPERNOVA 1987A; RADIO REMNANT; SPECTROSCOPY; SIMULATIONS; EVOLUTION; SN-1987A; NEBULA; EJECTA; SHOCK AB We present imaging and spectroscopic observations with Hubble Space Telescope and Very Large Telescope of the ring of SN 1987A from 1994 to 2014. After an almost exponential increase of the shocked emission from the hotspots up to day similar to 8000 (similar to 2009), both this and the unshocked emission are now fading. From the radial positions of the hotspots we see an acceleration of these up to 500-1000 km s(-1), consistent with the highest spectroscopic shock velocities from the radiative shocks. In the most recent observations (2013 and 2014), we find several new hotspots outside the inner ring, excited by either X-rays from the shocks or by direct shock interaction. All of these observations indicate that the interaction with the supernova ejecta is now gradually dissolving the hotspots. We predict, based on the observed decay, that the inner ring will be destroyed by similar to 2025. C1 [Fransson, Claes; Migotto, Katia; Lundqvist, Peter; Taddia, Francesco; Sollerman, Jesper] AlbaNova Univ Ctr, Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [Larsson, Josefin] AlbaNova, KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, Josefin] AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Pesce, Dominic; Chevalier, Roger A.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Challis, Peter; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [France, Kevin] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [France, Kevin] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Leibundgut, Bruno; Spyromilio, Jason] European So Observ, D-85748 Garching, Germany. [McCray, Richard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jerkstrand, Anders] Queens Univ, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Mattila, Seppo] Turku Univ, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Mattila, Seppo] Turku Univ, Tuorla Observ, Dept Phys & Astron, FI-21500 Piikkio, Finland. [Smith, Nathan] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Crotts, Arlin] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Garnavich, Peter] Univ Notre Dame, Nieuwland Sci 25, Notre Dame, IN 46556 USA. [Heng, Kevin] Univ Bern, Ctr Space & Habitabil, CH-3012 Bern, Switzerland. [Lawrence, Stephen S.] Hofstra Univ, Dept Phys & Astron, Hempstead, NY 11549 USA. [Panagia, Nino] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Panagia, Nino] Osserv Astron Capodimonte, INAF NA, I-80131 Naples, Italy. [Panagia, Nino] Supernova Ltd, Virgin Gorda VG 1150, Virgin Islands, England. [Pun, Chun S. J.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Sonneborn, George] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Sugerman, Ben] Goucher Coll, Dept Phys & Astron, Baltimore, MD 21204 USA. RP Fransson, C (reprint author), AlbaNova Univ Ctr, Stockholm Univ, Oskar Klein Ctr, Dept Astron, SE-10691 Stockholm, Sweden. RI Jerkstrand, Anders/K-9648-2015; OI Jerkstrand, Anders/0000-0001-8005-4030; Sollerman, Jesper/0000-0003-1546-6615; Lundqvist, Peter/0000-0002-3664-8082; /0000-0003-0065-2933; Fransson, Claes/0000-0001-8532-3594; Heng, Kevin/0000-0003-1907-5910 FU Swedish Research Council; Swedish National Space Board, NASA [NNX12AF90G]; NSF [AST-1109801]; NASA through a grant from the Space Telescope Science Institute; ESO Programmes [080.D-0727, 082.D-0273, 086.D-0713, 088.D-0638, 090.D-645, 092.D0119, 094.D-0505] FX We are grateful to the referee for detailed comments. This work was supported by the Swedish Research Council and the Swedish National Space Board, NASA grant NNX12AF90G, NSF grant AST-1109801. Support for the HST observing program 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. Partially based on observations collected at the European Southern Observatory, Chile (ESO Programmes 080.D-0727, 082.D-0273, 086.D-0713, 088.D-0638, 090.D-645, 092.D0119, 094.D-0505). NR 23 TC 9 Z9 9 U1 1 U2 6 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 JUN 10 PY 2015 VL 806 IS 1 AR L19 DI 10.1088/2041-8205/806/1/L19 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0LH UT WOS:000356633700019 ER PT J AU Podigachoski, P Barthel, P Haas, M Leipski, C Wilkes, B AF Podigachoski, Pece Barthel, Peter Haas, Martin Leipski, Christian Wilkes, Belinda TI THE UNIFICATION OF POWERFUL QUASARS AND RADIO GALAXIES AND THEIR RELATION TO OTHER MASSIVE GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: formation; galaxies: high-redshift; galaxies: starburst; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT; UNIFIED SCHEMES; 3CR QUASARS; SPECTROSCOPY; EVOLUTION; EMISSION AB The unification model for powerful radio galaxies (RGs) and radio-loud quasars postulates that these objects are intrinsically the same but viewed along different angles. Herschel Space Observatory data permit the assessment of that model in the far-infrared spectral window. We analyze photometry from Spitzer and Herschel for the distant 3CR hosts, and find that RGs and quasars have different mid-infrared, but indistinguishable far-infrared colors. Both these properties, the former being orientation dependent and the latter orientation invariant, are in line with expectations from the unification model. Adding powerful radio-quiet active galaxies and typical massive starforming (SF) galaxies to the analysis, we demonstrate that infrared colors not only provide an orientation indicator, but can also distinguish active from SF galaxies. C1 [Podigachoski, Pece; Barthel, Peter] Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. [Haas, Martin] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Leipski, Christian] MPIA, D-69117 Heidelberg, Germany. [Wilkes, Belinda] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Podigachoski, P (reprint author), Univ Groningen, Kapteyn Astron Inst, NL-9747 AD Groningen, Netherlands. EM podigachoski@astro.rug.nl OI Podigachoski, Pece/0000-0003-3836-710X; Wilkes, Belinda/0000-0003-1809-2364 FU Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO); 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); NASA FX We thank the referee, Patrick Ogle, for a very constructive report which improved the manuscript. Data were taken from the Herschel Guaranteed Time project The Herschel Legacy of distant radio-loud AGN (PI: PB). P.P. acknowledges the Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO) for a PhD fellowship. The Herschel spacecraft was designed, built, tested, and launched under a contract to ESA managed by the Herschel/Planck Project team by an industrial consortium under the overall responsibility of the prime contractor Thales Alenia Space (Cannes), and including Astrium (Friedrichshafen) responsible for the payload module and for system testing at spacecraft level, Thales Alenia Space (Turin) responsible for the service module, and Astrium (Toulouse) responsible for the telescope, with in excess of a hundred subcontractors. 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). This work is partly based 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. NR 34 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 JUN 10 PY 2015 VL 806 IS 1 AR L11 DI 10.1088/2041-8205/806/1/L11 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0LH UT WOS:000356633700011 ER PT J AU Hallworth, MT Marra, PP AF Hallworth, Michael T. Marra, Peter P. TI Miniaturized GPS Tags Identify Non-breeding Territories of a Small Breeding Migratory Songbird SO SCIENTIFIC REPORTS LA English DT Article ID CONNECTIVITY; TRACKING; HABITAT; OVENBIRDS; BIRDS AB For the first time, we use a small archival global positioning system (GPS) tag to identify and characterize non-breeding territories, quantify migratory connectivity, and identify population boundaries of Ovenbirds (Seiurus aurocapilla), a small migratory songbird, captured at two widely separated breeding locations. We recovered 15 (31%) GPS tags with data and located the non-breeding territories of breeding Ovenbirds from Maryland and New Hampshire, USA (0.50 +/- 0.15 ha, mean +/- SE). All non-breeding territories had similar environmental attributes despite being distributed across parts of Florida, Cuba and Hispaniola. New Hampshire and Maryland breeding populations had non-overlapping non-breeding population boundaries that encompassed 114,803 and 169,233 km(2), respectively. Archival GPS tags provided unprecedented pinpoint locations and associated environmental information of tropical non-breeding territories. This technology is an important step forward in understanding seasonal interactions and ultimately population dynamics of populations throughout the annual cycle. C1 [Hallworth, Michael T.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC 20013 USA. RP Hallworth, MT (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, MRC 5503, Washington, DC 20013 USA. EM mhallwor@masonlive.gmu.edu FU Smithsonian Institution's Competitive Grants Program for Science; National Science Foundation FX We thank M. van den Tillaart and L. Meczarski of Lotek Wireless Inc. who provided technical support. We also thank D. L. Narango, C. S. Rushing and C. E. Studds for providing valuable comments on versions of this manuscript. This research was supported by grants from the Smithsonian Institution's Competitive Grants Program for Science and the National Science Foundation. NR 20 TC 10 Z9 11 U1 6 U2 31 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 JUN 9 PY 2015 VL 5 AR 11069 DI 10.1038/srep11069 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CT4AZ UT WOS:000362749500001 PM 26057892 ER PT J AU Falk, JJ ter Hofstede, HM Jones, PL Dixon, MM Faure, PA Kalko, EKV Page, RA AF Falk, Jay J. ter Hofstede, Hannah M. Jones, Patricia L. Dixon, Marjorie M. Faure, Paul A. Kalko, Elisabeth K. V. Page, Rachel A. TI Sensory-based niche partitioning in a multiple predator - multiple prey community SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE eavesdropping; gleaning bats; katydids; predator-prey diversity; sensory-based niche partitioning ID NEOTROPICAL KATYDIDS ORTHOPTERA; INSECTIVOROUS BATS; TRACHOPS-CIRRHOSUS; GLEANING BATS; NEOCONOCEPHALUS-ENSIGER; PHYLLOSTOMID BATS; ECHOLOCATING BATS; TETTIGONIIDAE; EVOLUTION; BEHAVIOR AB Many predators and parasites eavesdrop on the communication Signals of their prey. Eavesdropping is typically studied as dyadic predator-prey species interactions; yet in nature, most predators target multiple prey species and most prey must evade multiple predator species. The impact of predator communities on prey signal evolution is not well understood. Predators could converge in their preferences for conspicuous signal properties, generating competition among predators and natural selection on particular prey signal features. Alternatively, predator species could vary in their preferences for prey signal properties, resulting in sensory-based niche partitioning of prey resources. In the Neotropics, many substrate-gleaning bats use the mate-attraction songs of male katydids to locate them as prey. We studied mechanisms of niche partitioning in four substrate-gleaning bat species and found they are similar in morphology, echolocation signal design and prey-handling ability, but each species preferred different acoustic features of male song in 12 sympatric katydid species. This divergence in predator preference probably contributes to the coexistence of many substrate-gleaning bat species in the Neotropics, and the substantial diversity in the mate-attraction signals of katydids. Our results provide insight into how multiple eavesdropping predator species might influence prey signal evolution through sensory-based niche partitioning. C1 [Falk, Jay J.; Jones, Patricia L.] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14850 USA. [ter Hofstede, Hannah M.] Dartmouth Coll, Dept Biol Sci, Hanover, NH 03755 USA. [Jones, Patricia L.; Dixon, Marjorie M.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. [Faure, Paul A.] McMaster Univ, Dept Psychol Neurosci & Behav, Hamilton, ON L8S 4L8, Canada. [Kalko, Elisabeth K. V.] Univ Ulm, Dept Expt Ecol, D-89081 Ulm, Germany. [Falk, Jay J.; Jones, Patricia L.; Dixon, Marjorie M.; Kalko, Elisabeth K. V.; Page, Rachel A.] Smithsonian Trop Res Inst, Ancon, Panama. RP Falk, JJ (reprint author), Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14850 USA. EM jjf266@cornell.edu FU STRI; Natural Sciences and Engineering Research Council of Canada; NSF FX This research was supported by funding from the STRI (J.J.F., M.M.D., R.A.P. and H.M.tH.), Natural Sciences and Engineering Research Council of Canada (H.M.tH. and P.A.F) and an NSF Graduate Research Fellowship (P.L.J.). NR 52 TC 5 Z9 5 U1 3 U2 32 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 JUN 7 PY 2015 VL 282 IS 1808 AR 20150520 DI 10.1098/rspb.2015.0520 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CL6EQ UT WOS:000357060800002 PM 25994677 ER PT J AU Xu, X Liu, FX Cheng, RC Chen, J Xu, X Zhang, ZS Ono, H Pham, DS Norma-Rashid, Y Arnedo, MA Kuntner, M Li, DQ AF Xu, Xin Liu, Fengxiang Cheng, Ren-Chung Chen, Jian Xu, Xiang Zhang, Zhisheng Ono, Hirotsugu Dinh Sac Pham Norma-Rashid, Y. Arnedo, Miquel A. Kuntner, Matjaz Li, Daiqin TI Extant primitively segmented spiders have recently diversified from an ancient lineage SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE living fossils; genetic diversity; plesiomorphies; vicariance; dispersal; ancestral areas ID DISPERSAL-VICARIANCE ANALYSIS; DIVERGENCE TIME-ESTIMATION; EAST-CHINA-SEA; TECTONIC FRAMEWORK; YELLOW-SEA; ARANEAE; EVOLUTION; PHYLOGENY; PATTERNS; LIPHISTIIDAE AB Living fossils are lineages that have retained plesiomorphic traits through long time periods. It is expected that such lineages have both originated and diversified long ago. Such expectations have recently been challenged in some textbook examples of living fossils, notably in extant cycads and coelacanths. Using a phylogenetic approach, we tested the patterns of the origin and diversification of liphistiid spiders, a clade of spiders considered to be living fossils due to their retention of arachnid plesiomorphies and their exclusive grouping in Mesothelae, an ancient clade sister to all modern spiders. Facilitated by original sampling throughout their Asian range, we here provide the phylogenetic framework necessary for reconstructing liphistiid biogeographic history. All phylogenetic analyses support the monophyly of Liphistiidae and of eight genera. As the fossil evidence supports a Carboniferous Euramerican origin of Mesothelae, our dating analyses postulate a long eastward over-land dispersal towards the Asian origin of Liphistiidae during the Palaeogene (39-58 Ma). Contrary to expectations, diversification within extant liphistiid genera is relatively recent, in the Neogene and Late Palaeogene (4-24 Ma). While no over-water dispersal events are needed to explain their evolutionary history, the history of liphistiid spiders has the potential to play prominently in vicariant biogeographic studies. C1 [Xu, Xin; Liu, Fengxiang; Chen, Jian; Kuntner, Matjaz; Li, Daiqin] Hubei Univ, Coll Life Sci, CBEE, Wuhan, Peoples R China. [Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore. [Liu, Fengxiang; Kuntner, Matjaz] Biol Inst ZRC SAZU, Evolutionary Zool Lab, Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Xu, Xiang] Hunan Normal Univ, Coll Life Sci, Changsha, Hunan, Peoples R China. [Zhang, Zhisheng] Southwest Univ, Sch Life Sci, Minist Educ, Key Lab Ecoenvironm Gorges Reservoir Reg 3, Chongqing, Peoples R China. [Ono, Hirotsugu] Natl Museum Nat & Sci, Dept Zool, Tsukuba, Ibaraki 3050005, Japan. [Dinh Sac Pham] VAST, IEBR, Hanoi, Vietnam. [Norma-Rashid, Y.] Univ Malaya, Fac Sci, Inst Biol Sci, Kuala Lumpur 50603, Malaysia. [Arnedo, Miquel A.] Univ Barcelona, Dept Biol Anim, Inst Recerca Biodiversitat, E-08028 Barcelona, Spain. RP Kuntner, M (reprint author), Hubei Univ, Coll Life Sci, CBEE, Wuhan, Peoples R China. EM kuntner@gmail.com; dbslidq@nus.edu.sg RI Norma-Rashid, Y/B-8028-2010; Li, Daiqin/D-6922-2013; xu, xin/E-5012-2017 OI Norma-Rashid, Y/0000-0002-1450-1995; Li, Daiqin/0000-0001-8269-7734; xu, xin/0000-0001-5632-6622 FU NSFC [31272324]; Singapore Ministry of Education (AcRF Tier 1 grant) [R-154-000-591-112]; Slovenian Research Agency [P1-10236, MU-PROM/12-001] FX This work was supported in part by the NSFC (grant no. 31272324) and the Singapore Ministry of Education (AcRF Tier 1 grant no. R-154-000-591-112) grants to D.L., and by the Slovenian Research Agency grant nos. P1-10236 and MU-PROM/12-001 to M.K. NR 91 TC 3 Z9 3 U1 1 U2 19 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 JUN 7 PY 2015 VL 282 IS 1808 AR 20142486 DI 10.1098/rspb.2014.2486 PG 10 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA CL6EQ UT WOS:000357060800029 PM 25948684 ER PT J AU Calinger, K Calhoon, E Chang, HC Whitacre, J Wenzel, J Comita, L Queenborough, S AF Calinger, Kellen Calhoon, Elisabeth Chang, Hsiao-chi Whitacre, James Wenzel, John Comita, Liza Queenborough, Simon TI Historic Mining and Agriculture as Indicators of Occurrence and Abundance of Widespread Invasive Plant Species SO PLOS ONE LA English DT Article ID EASTERN UNITED-STATES; SOUTHERN NEW-ENGLAND; LAND-USE HISTORY; FOREST; MINE; ROADS; ASSOCIATIONS; LANDSCAPE; PATTERNS; NITROGEN AB Anthropogenic disturbances often change ecological communities and provide opportunities for non-native species invasion. Understanding the impacts of disturbances on species invasion is therefore crucial for invasive species management. We used generalized linear mixed effects models to explore the influence of land-use history and distance to roads on the occurrence and abundance of two invasive plant species (Rosa multiflora and Berberis thunbergii) in a 900-ha deciduous forest in the eastern U.S.A., the Powdermill Nature Reserve. Although much of the reserve has been continuously forested since at least 1939, aerial photos revealed a variety of land-uses since then including agriculture, mining, logging, and development. By 2008, both Rosa multiflora and Berberis thunbergii were widespread throughout the reserve (occurring in 24% and 13% of 4417 10-m diameter regularly-placed vegetation plots, respectively) with occurrence and abundance of each varying significantly with land-use history. Rosa multiflora was more likely to occur in historically farmed, mined, logged or developed plots than in plots that remained forested, (log odds of 1.8 to 3.0); Berberis thunbergii was more likely to occur in plots with agricultural, mining, or logging history than in plots without disturbance (log odds of 1.4 to 2.1). Mining, logging, and agriculture increased the probability that Rosa multiflora had >10% cover while only past agriculture was related to cover of Berberis thunbergii. Proximity to roads was positively correlated with the occurrence of Rosa multiflora (a 0.26 increase in the log odds for every 1-m closer) but not Berberis thunbergii, and roads had no impact on the abundance of either species. Our results indicated that a wide variety of disturbances may aid the introduction of invasive species into new habitats, while high-impact disturbances such as agriculture and mining increase the likelihood of high abundance post-introduction. C1 [Calinger, Kellen; Calhoon, Elisabeth; Chang, Hsiao-chi; Comita, Liza; Queenborough, Simon] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Whitacre, James; Wenzel, John] Carnegie Museum Nat Hist, Powdermill Nat Reserve, Rector, PA 15677 USA. [Comita, Liza] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Whitacre, James] Univ Illinois, Univ Lib, Urbana, IL 61801 USA. RP Calinger, K (reprint author), Ohio State Univ, Dept Evolut Ecol & Organismal Biol, 318 W 12th Ave, Columbus, OH 43210 USA. EM kcalinger@gmail.com OI Whitacre, James/0000-0003-3464-9337 FU Heinz Endowment FX The vegetation survey was made possible through a grant from the Heinz Endowment, http://www.heinz.org/. NR 40 TC 0 Z9 0 U1 7 U2 20 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 JUN 5 PY 2015 VL 10 IS 6 AR e0128161 DI 10.1371/journal.pone.0128161 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CJ7CR UT WOS:000355652200044 PM 26046534 ER PT J AU Touwaide, A Appetiti, E AF Touwaide, Alain Appetiti, Emanuela TI Food and medicines in the Mediterranean tradition. A systematic analysis of the earliest extant body of textual evidence SO JOURNAL OF ETHNOPHARMACOLOGY LA English DT Article DE Hippocrates; Antiquity; Hippocratic collection; Foodstuff; Materia medica; Mediterranean tradition AB Ethnopharmacological relevance: The relationship between food and medicines has long been investigated and is of crucial importance for the understanding of the development of ethnopharmacological knowledge through time. Hippocrates, considered the Father of Medicine, is credited with an aphorism equating food and medicine. No inquiry has been performed, however, into the collection of texts attributed to Hippocrates and, going beyond, into this statement, which is generally accepted without further examination. A clarification is much needed as the question of the relationship between food and medicines as potent substances are crucial to ethnopharmacology. Materials and methods: To verify the validity (if not the authenticity) of the theory on the identity of food and medicine attributed to Hippocrates, we digitized the whole collection of texts ascribed to Hippocrates in the original Greek language (the so-called Hippocratic Collection), which date back from the age of Hippocrates (late 5th century and 4th century BCE) to a more recent time (2nd century CE). On this basis, we extracted and databased all the information related to remedial therapy, that is, their materia medica (vegetable, animal and mineral) and their use(s). We identified both the plant species according to modern up-to-date taxonomy and the medical conditions as precisely as possible. We then screened these plants to discover what their uses were and, going backward in time, we examined (when possible) their native distribution, domestication, possible introduction (in the case of non-native species) and cultivation to determine whether these species had been known for a long time and might have been the object of long-term observation as both foodstuffs and medicines. Results: Tabulated data from the Hippocratic Collection revealed that 40% of the remedies in the Collection are made out of only 44 plants. Of this group, 33 species (=75% of the group) were also used for nutritional purposes in Antiquity. Domestication history of these species indicates that humans have long been in contact with them, something that the medical uses of these species confirm, as they are multiple and finely distinguished. A pilot analysis of archeological remains of medicines confirms that textual evidence corresponds to physical evidence, that is, to the practice of medicine. As a consequence, textual information can be accepted as reflecting actual practice. Conclusions: Although the pseudo-aphorism according to which food are medicines and medicines are food does not appear as such in the Hippocratic Collection, it aptly expresses a fundamental element of the Hippocratic approach to therapeutics, without being, however, a creation of neither Hippocrates nor his followers and the physicians who practiced a form of medicine in the way of Hippocrates. A vast majority of the core group of plant species used for the preparation of medicines were also consumed as foodstuff. Knowledge and use of these plants probably resulted from a long co-existence in the same environment and also from multiple experiences of trial and error over millennia, whose results accumulated over time and contributed to the formation of the Mediterranean medical tradition. (C) 2014 Elsevier Ireland Ltd. All rights reserved. C1 Inst Preservat Med Tradit, Washington, DC USA. Smithsonian Inst, Washington, DC 20013 USA. RP Touwaide, A (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM research@medicaltraditions.org NR 37 TC 2 Z9 2 U1 0 U2 3 PU ELSEVIER IRELAND LTD PI CLARE PA ELSEVIER HOUSE, BROOKVALE PLAZA, EAST PARK SHANNON, CO, CLARE, 00000, IRELAND SN 0378-8741 J9 J ETHNOPHARMACOL JI J. Ethnopharmacol. PD JUN 5 PY 2015 VL 167 SI SI BP 11 EP 29 DI 10.1016/j.jep.2014.10.035 PG 19 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA CI8UX UT WOS:000355048300004 PM 25446635 ER PT J AU Nguyen, TL Lee, H Matthews, DA McCarthy, MC Stanton, JF AF Thanh Lam Nguyen Lee, Hyunwoo Matthews, Devin A. McCarthy, Michael C. Stanton, John F. TI Stabilization of the Simplest Criegee Intermediate from the Reaction between Ozone and Ethylene: A High-Level Quantum Chemical and Kinetic Analysis of Ozonolysis SO JOURNAL OF PHYSICAL CHEMISTRY A LA English DT Article ID GAS-PHASE OZONOLYSIS; ACTIVE THERMOCHEMICAL TABLES; VOLATILE ORGANIC-COMPOUNDS; ATOMIC NATURAL ORBITALS; TRANSITION-STATE THEORY; REACTION-RATE CONSTANTS; GAUSSIAN-BASIS SETS; OLEFIN REACTIONS; POLYATOMIC-MOLECULES; INITIATED OXIDATION AB The fraction of the collisionally stabilized Criegee species CH2OO produced from the ozonolysis of ethylene is calculated using a two-dimensional (E, J)-grained master equation technique and semiclassical transition-state theory based on the potential energy surface obtained from high-accuracy quantum chemical calculations. Our calculated yield of 42 +/- 6% for the stabilized CH2OO agrees well, within experimental error, with available (indirect) experimental results. Inclusion of angular momentum in the master equation is found to play an essential role in bringing the theoretical results into agreement with the experiment. Additionally, yields of HO and HO2 radical products are predicted to be 13 +/- 6% and 17 +/- 6%, respectively. In the kinetic simulation, the HO radical product is produced mostly from the stepwise decomposition mechanism of primary ozonide rather than from dissociation of hot CH2OO. C1 [Thanh Lam Nguyen; Lee, Hyunwoo; Matthews, Devin A.; Stanton, John F.] Univ Texas Austin, Dept Chem, Austin, TX 78712 USA. [McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Stanton, JF (reprint author), Univ Texas Austin, Dept Chem, Mail Stop A5300, Austin, TX 78712 USA. EM jfstanton@mail.utexas.edu FU Robert A. Welch Foundation [F-1283]; U.S. Depaitment of Energy, Office of Basic Energy Sciences [DE-FG02-07ER15884]; National Science Foundation [CHE-1058063] FX J.F.S. and T.L.N. are supported by the Robert A. Welch Foundation (Grant F-1283). This material is based on work supported by the U.S. Depaitment of Energy, Office of Basic Energy Sciences under Award DE-FG02-07ER15884. M.C.M. is supported by National Science Foundation Grant CHE-1058063. NR 90 TC 8 Z9 8 U1 7 U2 53 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1089-5639 J9 J PHYS CHEM A JI J. Phys. Chem. A PD JUN 4 PY 2015 VL 119 IS 22 BP 5524 EP 5533 DI 10.1021/acs.jpca.5b02088 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA CK0KD UT WOS:000355893200002 PM 25945650 ER PT J AU McCarthy, MC Baraban, JH Changala, PB Stanton, JF Martin-Drumel, MA Thorwirth, S Gottlieb, CA Reilly, NJ AF McCarthy, Michael C. Baraban, Joshua H. Changala, P. Bryan Stanton, John F. Martin-Drumel, Marie-Aline Thorwirth, Sven Gottlieb, Carl A. Reilly, Neil J. TI Discovery of a Missing Link: Detection and Structure of the Elusive Disilicon Carbide Cluster SO JOURNAL OF PHYSICAL CHEMISTRY LETTERS LA English DT Article ID SILICON-CARBON CLUSTERS; AB-INITIO; ELECTRONIC STATES; SI2C; SPECTRUM; SIC2; SPECTROSCOPY; MOLECULES AB The rotational spectrum of the elusive but fundamentally important silicon carbide SiCSi has been detected using sensitive microwave techniques aided by high-level ab initio methods. Its equilibrium structure has been determined to very high precision using isotopic substitution and vibrational corrections calculated quantum-chemically: it is an isosceles triangle with a Si-C bond length of 1.693(1) angstrom, and an apex angle of 114.87(5)degrees. Now that all four SimCn clusters with m + n = 3 have been observed experimentally, their structure and chemical bonding can be rigorously compared. Because Si2C is so closely linked to other Si-bearing molecules that have been detected in the evolved carbon star IRC+10216, it is an extremely promising candidate for detection with radio telescopes. C1 [McCarthy, Michael C.; Martin-Drumel, Marie-Aline; Gottlieb, Carl A.; Reilly, Neil J.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCarthy, Michael C.; Martin-Drumel, Marie-Aline; Gottlieb, Carl A.; Reilly, Neil J.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Baraban, Joshua H.] Univ Colorado, Dept Chem & Biochem, Boulder, CO 80309 USA. [Changala, P. Bryan] Univ Colorado, NIST, JILA, Boulder, CO 80309 USA. [Changala, P. Bryan] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Stanton, John F.] Univ Texas Austin, Dept Chem, Inst Theoret Chem, Austin, TX 78712 USA. [Thorwirth, Sven] Univ Cologne, Phys Inst 1, D-50937 Cologne, Germany. RP McCarthy, MC (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM mmccarthy@cfa.harvard.edu RI Thorwirth, Sven/C-6217-2011; OI Thorwirth, Sven/0000-0001-8200-6710; Martin-Drumel, Marie-Aline/0000-0002-5460-4294 FU NASA [NNX13AE59G]; NSF [DGE1144083]; Welch Foundation of Houston, Texas [F-1283]; U.S. National Science Foundation [CHE-1361031]; Deutsche Forschungsgemeinschaft (DFG) [TH 1301/3-1, TH 1301/3-2] FX The work in Cambridge is supported by NASA Grant NNX13AE59G. P.B.C. is supported by an NSF Graduate Research Fellowship (Award No. DGE1144083). J.F.S. would like to thank the Welch Foundation of Houston, Texas (Grant F-1283), and the U.S. National Science Foundation (Grant CHE-1361031). S.T. gratefully acknowledges funding by the Deutsche Forschungsgemeinschaft (DFG) through grants TH 1301/3-1 and TH 1301/3-2. We thank E.S. Palmer and P. Antonucci for technical assistance, and D.L. Kokkin for assistance with early laboratory searches. NR 33 TC 5 Z9 5 U1 4 U2 19 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1948-7185 J9 J PHYS CHEM LETT JI J. Phys. Chem. Lett. PD JUN 4 PY 2015 VL 6 IS 11 BP 2107 EP 2111 DI 10.1021/acs.jpclett.5b00770 PG 5 WC Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Atomic, Molecular & Chemical SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA CK0KL UT WOS:000355894000020 PM 26266510 ER PT J AU Kenyon, SJ AF Kenyon, Scott J. TI ASTRONOMY Pluto leads the way in planet formation SO NATURE LA English DT Editorial Material ID CHARON; IMPACT; ORIGIN; HYDRA; NIX AB Images from the Hubble Space Telescope cast new light on the orbits, shapes and sizes of Pluto's small satellites. The analysis comes just before a planned reconnaissance by the first spacecraft to visit them. See Article p.45 C1 Smithsonian Astrophys Observ, Dept Solar Stellar & Planetary Phys, Cambridge, MA 02138 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, Dept Solar Stellar & Planetary Phys, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X NR 8 TC 0 Z9 1 U1 0 U2 11 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 JUN 4 PY 2015 VL 522 IS 7554 BP 40 EP 41 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CJ5QP UT WOS:000355543400023 PM 26040888 ER PT J AU Drake, EM Cypher, BL Ralls, K Perrine, JD White, R Coonan, TJ AF Drake, Elizabeth M. Cypher, Brian L. Ralls, Katherine Perrine, John D. White, Russell Coonan, Timothy J. TI HOME-RANGE SIZE AND HABITAT SELECTION BY MALE ISLAND FOXES (UROCYON LITTORALIS) IN A LOW-DENSITY POPULATION SO SOUTHWESTERN NATURALIST LA English DT Article ID MICROTUS-AGRESTIS; GPS TELEMETRY; FIELD VOLES; LONG-TERM; SPACE USE; COMPETITION; BEHAVIOR; ECOLOGY; TECHNOLOGIES; ORGANIZATION AB Island foxes (Urocyon littoralis) are listed as federally endangered on four of the six California Channel Islands to which they are endemic. The population on Santa Rosa Island declined by 99% during the 1990s due to golden eagle (Aguila chrysaetos) predation but is now recovering. This drastic population reduction provided an unprecedented opportunity to study home-range size and habitat use at very low levels of intraspecific competition. We used global positioning system (GPS) collars to track 14 adult male foxes from September 2009 through June 2010. On average, the collars operated for 16.5 wk, yielding 364 locations per fox. The 95% minimum convex polygon home ranges averaged 3.39 km(2), which is several times larger than reported in previous studies conducted at higher population densities. We used Euclidean distance analysis to assess habitat selection within 95% kernel density isopleth (KDI) home ranges and 50% KDI core areas. The foxes used most of the available vegetation types but exhibited significant selection for valley bottoms and for bare areas and grassland at night. Our results, together with previous studies on island foxes, suggest an inverse relationship between home-range size and population density as has been shown for many other species. However, the pattern is confounded by differences among study areas and methods. We therefore recommend that this study be repeated when the Santa Rosa Island population recovers to its historic density of 4 adult foxes/km(2) to better assess density-dependent changes in home-range size and habitat use. C1 [Drake, Elizabeth M.; Perrine, John D.] Calif Polytech State Univ San Luis Obispo, Dept Biol Sci, San Luis Obispo, CA 93401 USA. [Cypher, Brian L.] Calif State Univ Stanislaus, Endangered Species Recovery Program, Turlock, CA 95372 USA. [Ralls, Katherine] Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [White, Russell] Calif Polytech State Univ San Luis Obispo, Informat Serv, San Luis Obispo, CA 93401 USA. [Coonan, Timothy J.] Natl Pk Serv, Ventura, CA 93001 USA. RP Drake, EM (reprint author), Calif Polytech State Univ San Luis Obispo, Dept Biol Sci, San Luis Obispo, CA 93401 USA. EM bcypher@esrp.csustan.edu OI White, Russell/0000-0002-2141-3862 FU California Department of Fish and Game; National Park Service; Smithsonian Institution FX Funding for this project was provided by the California Department of Fish and Game through the Endangered Species Act (Section-6) Grant-in-Aid Program, the National Park Service, and the Smithsonian Institution through a restricted endowment grant. J. Benson and three anonymous reviewers gave comments that significantly improved the manuscript. We thank R. Rudolph, D. Rodriguez, A. Guglielmino, and D. Sphar for assistance with geographic information system, botany, and field efforts. We thank B. Hudgens and the U.S. Navy for providing data from San Clemente Island and J. King for data from Catalina Island. J. Maldonado translated our abstract into Spanish. This study was conducted under U.S. Fish and Wildlife Service Recovery Permit TE08627-0. NR 51 TC 0 Z9 0 U1 9 U2 16 PU SOUTHWESTERN ASSOC NATURALISTS PI SAN MARCOS PA SOUTHWEST TEXAS STATE UNIV, DEPT BIOLOGY, 601 UNIVERSITY DR, SAN MARCOS, TX 78666 USA SN 0038-4909 EI 1943-6262 J9 SOUTHWEST NAT JI Southw. Natural. PD JUN-SEP PY 2015 VL 60 IS 2-3 BP 247 EP 255 DI 10.1894/SWNAT-D-14-00021.1 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA DE8NR UT WOS:000370893300015 ER PT J AU Crouch, TD AF Crouch, Tom D. TI Birdmen: The Wright Brothers, Glenn Curtiss, and the Battle to Control the Skies SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 [Crouch, Tom D.] Smithsonian Inst, Natl Air & Space Museum, Aeronaut, Washington, DC 20560 USA. RP Crouch, TD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Aeronaut, 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 SUM PY 2015 VL 89 IS 2 BP 339 EP 343 PG 5 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA CZ8QJ UT WOS:000367363900008 ER PT J AU Crouch, TD AF Crouch, Tom D. TI The Wright Company: From Invention to Industry SO BUSINESS HISTORY REVIEW LA English DT Book Review C1 [Crouch, Tom D.] Smithsonian Inst, Natl Air & Space Museum, Aeronaut, Washington, DC 20560 USA. RP Crouch, TD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Aeronaut, 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 SUM PY 2015 VL 89 IS 2 BP 339 EP 343 PG 5 WC Business; History Of Social Sciences SC Business & Economics; Social Sciences - Other Topics GA CZ8QJ UT WOS:000367363900007 ER PT J AU Miller, AJ Novy, A Glover, J Kellogg, EA Maul, JE Raven, P Jackson, PW AF Miller, A. J. Novy, A. Glover, J. Kellogg, E. A. Maul, J. E. Raven, P. Jackson, P. Wyse TI Expanding the role of botanical gardens in the future of food SO NATURE PLANTS LA English DT Editorial Material C1 [Miller, A. J.] St Louis Univ, Dept Biol, St Louis, MO 63103 USA. [Miller, A. J.; Raven, P.; Jackson, P. Wyse] Missouri Bot Garden, St Louis, MO 63110 USA. [Novy, A.] US Bot Garden, Washington, DC 20024 USA. [Novy, A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Glover, J.] US Agcy Int Dev, Washington, DC 20004 USA. [Kellogg, E. A.] Donald Danforth Plant Sci Ctr, St Louis, MO 63132 USA. [Maul, J. E.] USDA ARS, Sustainable Agr Syst Lab, Beltsville, MD 20705 USA. [Jackson, P. Wyse] Washington Univ, Dept Biol, St Louis, MO 63130 USA. RP Miller, AJ (reprint author), St Louis Univ, Dept Biol, St Louis, MO 63103 USA. EM amille75@slu.edu; anovy@aoc.gov RI Kellogg, Elizabeth/M-2845-2013 OI Kellogg, Elizabeth/0000-0003-1671-7447 NR 14 TC 0 Z9 0 U1 2 U2 10 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2055-026X EI 2055-0278 J9 NAT PLANTS JI Nat. Plants PD JUN 1 PY 2015 VL 1 IS 6 AR 15078 DI 10.1038/NPLANTS.2015.78 PG 4 WC Plant Sciences SC Plant Sciences GA CV6TI UT WOS:000364403300001 PM 27250013 ER PT J AU Elliott, GD Lee, PC Paramore, E Van Vorst, M Comizzoli, P AF Elliott, Gloria D. Lee, Pei-Chih Paramore, Elisha Van Vorst, Matthew Comizzoli, Pierre TI Resilience of Oocyte Germinal Vesicles to Microwave-Assisted Drying in the Domestic Cat Model SO BIOPRESERVATION AND BIOBANKING LA English DT Article ID MAMMALIAN-CELLS; IN-VITRO; PRESERVATION; TREHALOSE; INTEGRITY; CHROMATIN; CRYOPRESERVATION; FERTILIZATION; STABILIZATION; INACTIVATION AB The ability to compact and inject the cat germinal vesicle (GV) into a recipient cytoplast allows exploration of a new fertility preservation strategy that avoids whole oocyte freezing. The objective of the present study was to understand the impact of water loss and storage time on GV DNA integrity. Immature cat oocytes were exposed to 1.5M trehalose for 10min before microwave-assisted dehydration for 0, 5, 10, 15, 20, 25, 30, or 40min. Oocytes then were rehydrated to assess chromatin configuration and the incidence of DNA fragmentation (TUNEL assay). The moisture content progressively decreased (p<0.05) from 1.7 to 0.1gH(2)O/gDW over the first 30min, but did not decrease further (p>0.05) after 40min. Chromatin configuration was unaffected (p>0.05) over time. The percentage of GVs with DNA fragmentation was unaltered (p>0.05) from 0 to 30min of treatment (range, 6.1%-12%), but increased (p<0.05) to 32.5% after 40min. Next, the influence of storage at two different supra-zero temperatures after 30min of drying was investigated. Oocyte-loaded, microwave-treated filters were individually sealed in Dri-Shield moisture barrier bags and stored at 4 degrees C or ambient temperature for 0 to 8 weeks. Moisture contents gradually decreased (p<0.05) from 0.12 to 0.10gH(2)O/gDW after 8 weeks of storage at 4 degrees C or ambient temperature. The percentage of GVs with DNA fragmentation more than doubled (p<0.05) from 0 (14.3%) to 2 days (30.0%-33.0%), but remained stable (p>0.05) thereafter (1 through 4 weeks, 25.0%-35.0%). Collective results demonstrate the feasibility of using microwave processing to dehydrate the mammalian GV to a moisture content that is nonlethal and enables nonfrozen storage, an alternative approach for preserving the maternal genome at cool or ambient temperature. C1 [Elliott, Gloria D.; Paramore, Elisha; Van Vorst, Matthew] Univ N Carolina, Dept Mech Engn & Engn Sci, Charlotte, NC 28223 USA. [Lee, Pei-Chih; Comizzoli, Pierre] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. RP Elliott, GD (reprint author), Univ N Carolina, Dept Mech Engn & Engn Sci, 9201 Univ City Blvd, Charlotte, NC 28223 USA. EM gdelliot@uncc.edu FU National Center for Research Resources, National Institutes of Health (NIH) [R01 RR026064]; Office of Research Infrastructure Programs/Office of the Director [R01 OD010948]; National Institute of General Medical Sciences [R01 GM101796] FX This work was supported in part by National Center for Research Resources (R01 RR026064), a component of the National Institutes of Health (NIH), and currently supported by the Office of Research Infrastructure Programs/Office of the Director (R01 OD010948), as well as by the National Institute of General Medical Sciences (R01 GM101796). NR 34 TC 3 Z9 3 U1 3 U2 6 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1947-5535 EI 1947-5543 J9 BIOPRESERV BIOBANK JI Biopreserv. Biobank. PD JUN 1 PY 2015 VL 13 IS 3 BP 164 EP 171 DI 10.1089/bio.2014.0078 PG 8 WC Cell Biology; Chemistry, Applied; Medical Laboratory Technology SC Cell Biology; Chemistry; Medical Laboratory Technology GA CV0KQ UT WOS:000363940000003 PM 26035005 ER PT J AU Bresciano, JC Salvador, CA Paz-y-Mino, C Parody-Merino, AM Bosch, J Woodhams, DC AF Bresciano, J. C. Salvador, C. A. Paz-y-Mino, C. Parody-Merino, A. M. Bosch, J. Woodhams, D. C. TI Variation in the Presence of Anti-Batrachochytrium dendrobatidis Bacteria of Amphibians Across Life Stages and Elevations in Ecuador SO ECOHEALTH LA English DT Article DE Andes; antifungal bacteria; biogeography; chytridiomycosis; life-history; microbiota ID SALAMANDER PLETHODON-CINEREUS; TIME TAQMAN PCR; CUTANEOUS BACTERIA; POPULATION DECLINES; SPECIES-DIVERSITY; RANA-MUSCOSA; CHYTRIDIOMYCOSIS; DISEASE; FROGS; INFECTION AB Amphibian populations are decreasing worldwide due to a variety of factors. In South America, the chytrid fungus Batrachochytrium dendrobatidis (Bd) is linked to many population declines. The pathogenic effect of Bd on amphibians can be inhibited by specific bacteria present on host skin. This symbiotic association allows some amphibians to resist the development of the disease chytridiomycosis. Here, we aimed (1) to determine for the first time if specific anti-Bd bacteria are present on amphibians in the Andes of Ecuador, (2) to monitor anti-Bd bacteria across developmental stages in a focal amphibian, the Andean marsupial tree frog, Gastrotheca riobambae, that deposits larvae in aquatic habitats, and (3) to compare the Bd presence associated with host assemblages including 10 species at sites ranging in biogeography from Amazonian rainforest (450 masl) to Andes montane rainforest (3200 masl). We sampled and identified skin-associated bacteria of frogs in the field using swabs and a novel methodology of aerobic counting plates, and a combination of morphological, biochemical, and molecular identification techniques. The following anti-Bd bacteria were identified and found to be shared among several hosts at high-elevation sites where Bd was present at a prevalence of 32.5%: Janthinobacterium lividum, Pseudomonas fluorescens, and Serratia sp. Bd were detected in Gastrotheca spp. and not detected in the lowlands (sites below 1000 masl). In G. riobambae, recognized Bd-resistant bacteria start to be present at the metamorphic stage. Overall bacterial abundance was significantly higher post-metamorphosis and on species sampled at lower elevations. Further metagenomic studies are needed to evaluate the roles of host identity, life-history stage, and biogeography of the microbiota and their function in disease resistance. C1 [Bresciano, J. C.; Parody-Merino, A. M.] Univ Int Menendez Pelayo Spain, Seville, Spain. [Salvador, C. A.; Paz-y-Mino, C.] Univ Amer UDLA, Fac Ciencias Salud, Inst Invest Biomed, Quito, Ecuador. [Salvador, C. A.] Univ Tecn Norte, Ctr Univ Invest Cient & Tecnol, Ibarra, Ecuador. [Bosch, J.] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. [Woodhams, D. C.] Univ Massachusetts, Dept Biol, Boston, MA 02125 USA. [Woodhams, D. C.] Smithsonian Trop Res Inst, Panama City, Panama. RP Bresciano, JC (reprint author), Univ Int Menendez Pelayo Spain, Calle Arjona 10 Escalera 6 Piso 4 Puerta 4, Seville, Spain. EM jorgebresciano@gmail.com OI Bosch, Jaime/0000-0002-0099-7934 FU Universidad de las Americas (Quito, Ecuador); Banco Santander and Fundacion General CSIC; Universidad Inodamerica (Quito, Ecuador); CSIC-Spain FX We would like to thank Universidad de las Americas (Quito, Ecuador), and Banco Santander and Fundacion General CSIC for partial funding, and Universidad Inodamerica (Quito, Ecuador) for support in Ecuador. JCB and AMP-M were funded by master scholarships from CSIC-Spain. JCB would like to mention special thanks to Georgina Bresciano and Veronica Maino for invaluable support. NR 63 TC 0 Z9 0 U1 10 U2 17 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1612-9202 EI 1612-9210 J9 ECOHEALTH JI EcoHealth PD JUN PY 2015 VL 12 IS 2 BP 310 EP 319 DI 10.1007/s10393-015-1010-y PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA CS0JZ UT WOS:000361746600014 PM 25669915 ER PT J AU Kinney, JR AF Kinney, Jeremy R. TI The Bombers and the Bombed: Allied Air War over Europe, 1940-1945 SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 [Kinney, Jeremy R.] Smithsonian Natl Air & Space Museum, Washington, DC 20560 USA. RP Kinney, JR (reprint author), Smithsonian Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0021-8723 EI 1945-2314 J9 J AM HIST JI J. Am. Hist. PD JUN PY 2015 VL 102 IS 1 BP 285 EP 286 DI 10.1093/jahist/jav237 PG 2 WC History SC History GA CR5LU UT WOS:000361384900108 ER PT J AU Crouch, TD AF Crouch, Tom D. TI No Requiem for the Space Age: The Apollo Moon Landings and American Culture SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 [Crouch, Tom D.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Crouch, TD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0021-8723 EI 1945-2314 J9 J AM HIST JI J. Am. Hist. PD JUN PY 2015 VL 102 IS 1 BP 299 EP 300 DI 10.1093/jahist/jav204 PG 4 WC History SC History GA CR5LU UT WOS:000361384900125 ER PT J AU Kaeppler, AL AF Kaeppler, Adrienne L. TI TWO HAWAIIAN DANCERS AND THEIR DAUGHTERS SO JOURNAL OF THE POLYNESIAN SOCIETY LA English DT Article DE Hawaiian dance; hula; biography Mary Kawena Pukui; biography Kau'i Zuttermeister; Bishop Museum; Second World War AB Two Hawaiian women, born around the turn of the 19th century into the 20th, became students, performers and finally acknowledged repositories of hula and its associated knowledge. They passed on their expertise and knowledge in many ways to many others, and especially to one daughter each, who has passed it on yet again. This narrative of aspects of these women's lives focusses on their learning and teaching, and contributes to a deeper understanding of the hula tradition in Hawai'i and the significant role of women in maintaining and enhancing it. C1 [Kaeppler, Adrienne L.] Smithsonian Inst, Washington, DC 20506 USA. RP Kaeppler, AL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, 10th & Constitut Ave NW, Washington, DC 20506 USA. EM kaepplea@si.edu NR 10 TC 0 Z9 0 U1 0 U2 0 PU POLYNESIAN SOC INC PI AUCKLAND PA C/O MAORI STUDIES, UNIV AUCKLAND, PRIVATE BAG, AUCKLAND 92019, NEW ZEALAND SN 0032-4000 EI 2230-5955 J9 J POLYNESIAN SOC JI J. Polyn. Soc. PD JUN PY 2015 VL 124 IS 2 BP 189 EP 207 PG 19 WC Anthropology SC Anthropology GA CR3ZK UT WOS:000361271400003 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 Eleusininae with a new genus, Micrachne (Poaceae: Chloridoideae: Cynodonteae) SO TAXON LA English DT Article DE Brachyachne; Chloris; Cynodon; Diplachne; Enteropogon; ITS; Leptochloa; Micrachne; plastid DNA sequences; Stapfochloa; systematics; Tetrapogon ID GRASS SUBFAMILY CHLORIDOIDEAE; SUBGENERIC CLASSIFICATION; CHLORIDEAE; SEQUENCES; SYSTEMATICS; INFERENCE; MRBAYES; TREES; SW AB The subtribe Eleusininae (Poaceae: Chloridoideae: Cynodonteae) is a diverse group containing about 212 species in 31 genera found primarily in low latitudes in Africa, Asia, Australia, and the Americas, and the classification among these genera and species is poorly understood. Therefore, we investigated the following 28 Eleusininae genera: Acrachne, Afrotrichloris, Apochiton, Astrebla, Austrochloris, Brachyachne, Chloris, Chrysochloa, Coelachyrum, Cynodon, Daknopholis, Dinebra, Diplachne, Disakisperma, Eleusine, Enteropogon, Eustachys, Harpochloa, Leptochloa, Lepturus, Lintonia, Microchloa, Ochthochloa, Oxychloris, Saugetia, Schoenefeldia, Stapfochloa, and Tetrapogon. The goals of our study were to reconstruct the evolutionary history of the subtribe Eleusininae using molecular data with increased species sampling compared to earlier studies. A phylogenetic analysis was conducted on 402 samples, of which 148 species (342 individuals) were in the Eleusininae, using four plastid (rpl32-trnL spacer, ndhA intron, rps16-trnK spacer, rps16 intron) and nuclear ITS 1 & 2 (ribosomal internal transcribed spacer) sequences to infer evolutionary relationships and revise the classification. We found strong support for the following Eleusininae lineages: Acrachne, Apochiton, Astrebla, Austrochloris, Chloris, Chrysochloa, Cynodon, Daknopholis, Dinebra, Diplachne, Disakisperma, Eleusine, Enteropogon, Eustachys, Leptochloa, Lepturus, Micrachne gen. nov., Stapfochloa, and Tetrapogon, and moderate support for Harpochloa and Microchloa. Four species of Brachyachne, including the type, are imbedded within Cynodon; Oxychloris scariosa (monotypic) is sister to Harpochloa-Microchloa; Coelachyrum is polyphyletic since C. lagopoides, Apochiton burttii, and C. poiflorum form a grade, with the latter species sister to Eleusine; Schoenefeldia appears paraphyletic since Afrotrichloris martinii and Schoenefeldia transiens together are sister to Schoenefeldia gracilis; Saugetia fasciculata, Enteropogon brandegeei, and E. chlorideus are embedded within Tetrapogon; Lintonia nutans and Ochthochloa compressa are embedded in Chloris; and Enteropogon mollis and Chloris exilis are embedded in Leptochloa. Our plastid and ITS analyses show rearrangement of lineages within Acrachne and Chloris, indicating possible hybridization events or evidence for multiple origins. The molecular results support recognition of a new genus, Micrachne with five species and emendation of Stapfochloa with six species. We provide 22 new combinations, Chloris flagellifera, Ch. nutans, Cynodon ambiguus, C. prostratus, Diplachne divaricatissima, Leptochloa anisopoda, L. exilis, Micrachne fulva, M. obtusiflora, M. patentiflora, M. pilosa, M. simonii, Stapfochloa berroi, S. canterae, S. ciliata, S. elata, S. parvispicula, Tetrapogon brandegeei, T. chlorideus, T. fasciculatus, T. pleistachyus, and T. roxburghiana; a new name, Cynodon simonii; and lectotypify Eleusine flagillifera. C1 [Peterson, Paul M.; Romaschenko, Konstantin] Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. [Romaschenko, Konstantin] Natl Acad Sci, MG Kholodny Inst Bot, UA-01601 Kiev, Ukraine. [Arrieta, Yolanda Herrera] CIIDIR Unidad Durango COFAA, Inst Politecn Nacl, Durango 34220, Mexico. RP Peterson, PM (reprint author), Natl Museum Nat Hist, Dept Bot, Smithsonian Inst, Washington, DC 20013 USA. EM peterson@si.edu RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 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, and the Laboratory of Analytical Biology; and the United States Department of Agriculture, all for financial support. We would also like to acknowledge Gabriel Johnson for help in the laboratory; Robert J. Soreng and Jeffery M. Saarela for accompanying the first author on numerous field expeditions; Maria Vorontsova for finding type images at K; Robert J. Soreng for many extended discussions pertinent to the manuscript; Jeffery M. Saarela and Neil Snow for providing helpful comments on the manuscript; and Franz Stadler for critical review during production. NR 64 TC 2 Z9 3 U1 6 U2 16 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 JUN PY 2015 VL 64 IS 3 BP 445 EP 467 PG 23 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA CR0ZZ UT WOS:000361053700003 ER PT J AU Erisman, F AF Erisman, Fred TI Ruth Nichols, Sky Girl, and the Aerial Frontier SO WESTERN AMERICAN LITERATURE LA English DT Article C1 [Erisman, Fred] Texas Christian Univ, Literature Emeritus, Ft Worth, TX 76129 USA. [Erisman, Fred] Smithsonian Inst, Natl Air & Space Museum, Aerosp Hist, Washington, DC 20560 USA. RP Erisman, F (reprint author), Texas Christian Univ, Literature Emeritus, Ft Worth, TX 76129 USA. NR 27 TC 0 Z9 0 U1 0 U2 0 PU UTAH STATE UNIV PI LOGAN PA WESTERN LIT ASSOC UMC 32, LOGAN, UT 84322 USA SN 0043-3462 EI 1948-7142 J9 WESTERN AM LIT JI West. Amer. Lit. PD SUM PY 2015 VL 50 IS 2 BP 119 EP 134 PG 16 WC Literature, American SC Literature GA CP4YD UT WOS:000359887600003 ER PT J AU Erlandson, JM Ainis, AF Braje, TJ Jew, NP Mcvey, M Rick, TC Vellanoweth, RL Watts, J AF Erlandson, Jon M. Ainis, Amira F. Braje, Todd J. Jew, Nicholas P. Mcvey, Marlene Rick, Torben C. Vellanoweth, Rene L. Watts, Jack TI 12,000 Years of Human Predation on Black Turban Snails (Chlorostoma funebralis) on Alta California's Northern Channel Islands SO CALIFORNIA ARCHAEOLOGY LA English DT Article ID SAN-MIGUEL ISLAND; TEGULA-FUNEBRALIS; HUMAN IMPACTS; SOUTH-AFRICA; MARITIME TECHNOLOGIES; DAISY CAVE; STONE-AGE; SHELLFISH; EXPLOITATION; CHRONOLOGY AB Examining the ecology and archaeology of black turban snails (Chlorostoma [Tegula] funebralis), found along North America's Pacific Coast from British Columbia to Baja California, we present evidence for 12,000 years of human predation in Northern Channel Island shell middens. Often viewed as evidence for Late Holocene economic intensification along the southern California Coast, we identified black turban middens dated to the terminal Pleistocene, as well as the early, middle, and late Holocene. Despite their small size and lower ranking as a prey species, humans harvested black turban snails because of their abundance, aggregation, and accessibility during daily tidal cycles. Examining 19 discrete archaeological components (with a total MNI of similar to 7,800) from San Miguel and Santa Rosa islands, we used a Shell Weight/MNI Index to document fluctuations in the mean size of black turban shells through time, identifying patterns attributed to a combination of environmental and demographic changes, including variation in the intensity of human predation. C1 [Erlandson, Jon M.; Mcvey, Marlene; Watts, Jack] 1224 Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Ainis, Amira F.; Jew, Nicholas P.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Vellanoweth, Rene L.] Calif State Univ Los Angeles, Dept Anthropol, Los Angeles, CA 90032 USA. RP Erlandson, JM (reprint author), 1224 Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. EM jerland@uoregon.edu; aainis@uoregon.edu; tbraje@mail.sdsu.edu; njew@uoregon.edu; mmcvey@uoregon.edu; rickt@si.edu; rvellan@calstatela.edu; jack.watts@gmail.com NR 102 TC 0 Z9 0 U1 1 U2 6 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1947-461X EI 1947-4628 J9 CALIF ARCHAOL JI Calif. Archaeol. PD JUN PY 2015 VL 7 IS 1 BP 59 EP 91 PG 33 WC Archaeology SC Archaeology GA CO4UY UT WOS:000359157400003 ER PT J AU Ambrose, LM Devine, JB Whayne, J AF Ambrose, Linda M. Devine, Jenny Barker Whayne, Jeannie TI Revisiting Rural Women's History SO AGRICULTURAL HISTORY LA English DT Article C1 [Ambrose, Linda M.] Laurentian Univ, Hist, Sudbury, ON P3E 2C6, Canada. [Devine, Jenny Barker] Illinois Coll, Hist, Jacksonville, IL USA. [Whayne, Jeannie] Univ Arkansas, Hist, Fayetteville, AR 72701 USA. [Whayne, Jeannie] Smithsonian Inst, Washington, DC 20560 USA. [Whayne, Jeannie] Univ Virginia, Carter Woodson Inst, Charlottesville, VA 22903 USA. [Whayne, Jeannie] Org Amer Historians, Bloomington, IN USA. RP Ambrose, LM (reprint author), Laurentian Univ, Hist, Sudbury, ON P3E 2C6, Canada. NR 4 TC 0 Z9 0 U1 0 U2 0 PU AGRICULTURAL HISTORY SOCIETY PI LITTLE ROCK PA UALR, DEPT HISTORY, 2801 S UNIVERSITY AVE, LITTLE ROCK, AR 72324-1099 USA SN 0002-1482 EI 1533-8290 J9 AGR HIST JI Agric. Hist. PD SUM PY 2015 VL 89 IS 3 BP 380 EP 387 DI 10.3098/ah.2015.089.3.380 PG 8 WC Agriculture, Multidisciplinary; History; History & Philosophy Of Science SC Agriculture; History; History & Philosophy of Science GA CN2RF UT WOS:000358268900004 ER PT J AU Sohn, JC Park, KT Cho, S AF Sohn, Jae-Cheon Park, Kyu-Tek Cho, Soowon TI A taxonomic review of Schoenobiinae (Lepidoptera: Crambidae) from Korea SO JOURNAL OF ASIA-PACIFIC ENTOMOLOGY LA English DT Review DE Catagela; Fauna; New record; Patissa; Pyraloidea AB The Korean species of Schoenobiinae are reviewed. A total of four genera and 10 species are recognized. Among these, three species: Schoenobius sasakii Inoue, Scirpophaga excerptalis (Walker), and Scirpophaga gotoi Lewvanich, are reported for the first time from Korea, and Scirpophaga praelata (Scopoli) is reported for the first time from South Korea. In addition, the occurrence of Scirpophaga xanthopygata Schawerda in Korea is reconfirmed. Diagnoses and photos of adults and genitalia are given for the species available for this study. A key to the Korean species of Schoenobiinae is also provided. (C) 2014 Korean Society of Applied Entomology, Taiwan Entomological Society and Malaysian Plant Protection Society. Published by Elsevier B.V. All rights reserved. C1 [Sohn, Jae-Cheon] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Park, Kyu-Tek] Korean Acad Sci & Technol, Songnam 463808, Gyunggi Prov, South Korea. [Cho, Soowon] Chungbuk Natl Univ, Dept Plant Med, Cheongju 362763, Chungbuk Prov, South Korea. RP Cho, S (reprint author), Chungbuk Natl Univ, Dept Plant Med, Cheongju 362763, Chungbuk Prov, South Korea. EM chosoowon@gmail.com FU National Institute of Biological Resources (NIBR) - Ministry of Environment (MOE) of the Republic of Korea (NIBR) [2014] FX This work was supported by a grant from the National Institute of Biological Resources (NIBR), funded by the Ministry of Environment (MOE) of the Republic of Korea (NIBR No. 2014). NR 62 TC 0 Z9 0 U1 1 U2 3 PU KOREAN SOC APPLIED ENTOMOLOGY PI SUWON PA NATL INST AGRICULTURAL SCIENCE & TECHNOLOGY, DIVISION ENTOMOLOGY, RDA, 249 SEODUN-DONG, SUWON, 441-707, SOUTH KOREA SN 1226-8615 EI 1876-7990 J9 J ASIA-PAC ENTOMOL JI J. Asia-Pac. Entomol. PD JUN PY 2015 VL 18 IS 2 BP 131 EP 137 DI 10.1016/j.aspen.2014.12.007 PG 7 WC Entomology SC Entomology GA CN6RL UT WOS:000358561800004 ER PT J AU McCauley, PI Su, YN Schanche, N Evans, KE Su, C McKillop, S Reeves, KK AF McCauley, P. I. Su, Y. N. Schanche, N. Evans, K. E. Su, C. McKillop, S. Reeves, K. K. TI Prominence and Filament Eruptions Observed by the Solar Dynamics Observatory: Statistical Properties, Kinematics, and Online Catalog SO SOLAR PHYSICS LA English DT Article DE Prominences, dynamics; Coronal mass ejections, low corona signatures; Corona, structures ID CORONAL MASS EJECTIONS; POLAR-CROWN PROMINENCE; UNSTABLE FLUX ROPES; QUIESCENT PROMINENCES; MAGNETIC-FIELD; SLOW-RISE; HYDROMAGNETIC INTERIOR; MICROWAVE OBSERVATIONS; CRITICAL HEIGHT; EMERGING FLUX AB We present a statistical study of prominence and filament eruptions observed by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). Several properties are recorded for 904 events that were culled from the Heliophysics Event Knowledgebase (HEK) and incorporated into an online catalog for general use. These characteristics include the filament and eruption type, eruption symmetry and direction, apparent twisting and writhing motions, and the presence of vertical threads and coronal cavities. Associated flares and white-light coronal mass ejections (CME) are also recorded. Total rates are given for each property along with how they differ among filament types. We also examine the kinematics of 106 limb events to characterize the distinct slow- and fast-rise phases often exhibited by filament eruptions. The average fast-rise onset height, slow-rise duration, slow-rise velocity, maximum field-of-view (FOV) velocity, and maximum FOV acceleration are 83 Mm, 4.4 hours, 2.1 km s(-1), 106 km s(-1), and 111 m s(-2), respectively. All parameters exhibit lognormal probability distributions similar to that of CME speeds. A positive correlation between latitude and fast-rise onset height is found, which we attribute to a corresponding negative correlation in the average vertical magnetic field gradient, or decay index, estimated from potential field source surface (PFSS) extrapolations. We also find the decay index at the fast-rise onset point to be 1.1 on average, consistent with the critical instability threshold theorized for straight current channels. Finally, we explore relationships between the derived kinematics properties and apparent twisting motions. We find that events with evident twist have significantly faster CME speeds and significantly lower fast-rise onset heights, suggesting relationships between these values and flux rope helicity. C1 [McCauley, P. I.; Su, Y. N.; Schanche, N.; Evans, K. E.; McKillop, S.; Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Su, Y. N.; Su, C.] Chinese Acad Sci, Key Lab Dark Matter & Space Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Evans, K. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Su, C.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. RP McCauley, PI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmccauley@cfa.harvard.edu; ynsu@pmo.ac.cn RI McCauley, Patrick/P-7747-2015 OI McCauley, Patrick/0000-0002-1450-7350 FU National Aeronautics and Space Administration (NASA) [NNX12AI30G]; National Science Foundation (NSF) [AGS1263241]; Lockheed-Martin Solar and Astrophysics Laboratory (LMSAL) [SP02H1701R]; National Science Foundation of China (NSFC) [11333009, 11173062, 11473071, J1210039]; Youth Fund of Jiangsu [BK20141043] FX Support for this work was provided by the National Aeronautics and Space Administration (NASA) through grant NNX12AI30G to the Smithsonian Astrophysical Observatory (SAO), by the National Science Foundation (NSF) through grant AGS1263241 for the solar physics Research Experiences for Undergraduates (REU) program at SAO, and by the Lockheed-Martin Solar and Astrophysics Laboratory (LMSAL) through contract SP02H1701R to SAO for support of the AIA. Additional support was provided by the National Science Foundation of China (NSFC) through grants No. 11333009, 11173062, 11473071, and J1210039, along with the Youth Fund of Jiangsu through grant No. BK20141043. The SDO is a NASA satellite, and the AIA instrument team is led by LMSAL. We gratefully acknowledge the anonymous referee for their constructive comments. P.I.M. thanks Sarah Gibson for her FORWARD tutorial, which facilitated our decay index analyses. We also thank the observers who contributed filament eruptions to the HEK: Anna Malanushenko, Nariaki Nitta, Wei Liu, Karel Schrijver, Mark Cheung, Ryan Timmons, Thomas Berger, Marc DeRosa, Ralph Seguin, Paul Higgins, Juan Martinez-Skyora, Alberto Sainz-Dalda, Gregory Slater, and Neil Hurlburt. NR 119 TC 14 Z9 14 U1 11 U2 19 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUN PY 2015 VL 290 IS 6 BP 1703 EP 1740 DI 10.1007/s11207-015-0699-7 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM9YX UT WOS:000358068200011 ER PT J AU Aleksi, J Ansoldi, S Antonelli, LA Antoranz, P Babic, A Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Bernardini, E Biasuzzi, B Biland, A Blanch, O Boller, A Bonnefoy, S Bonnoli, G Borracci, F Bretz, T Carmona, E Carosi, A Colin, P Colombo, E Contreras, JL Cortina, J Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G De Lotto, B Wilhelmi, ED Mendez, CD Prester, DD Dorner, D Doro, M Einecke, S Eisenacher, D Elsaesser, D Fonseca, MV Font, L Frantzen, K Fruck, C Galindo, D Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Godinovic, N Munoz, AG Gozzini, SR Hadasch, D Hanabata, Y Hayashida, M Herrera, J Hildebrand, D Hose, J Hrupec, D Hughes, G Idec, W Kadenius, V Kellermann, H Knoetig, ML Kodani, K Konno, Y Krause, J Kubo, H Kushida, J La Barbera, A Lelas, D Lewandowska, N Lindfors, E Lombardi, S Lopez, M Lopez-Coto, R Lopez-Oramas, A Lorenz, E Lozano, I Makariev, M Mallot, K Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Miranda, JM Mirzoyan, R Moralejo, A Munar-Adrover, P Nakajima, D Niedzwiecki, A Nilsson, K Nishijima, K Noda, K Orito, R Overkemping, A Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Persic, M Moroni, PGP Prandini, E Puljak, I Reinthal, R Rhode, W Ribo, M Rico, J Garcia, JR Rugamer, S Saito, T Saito, K Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Sun, S Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Spanier, F Stamatescu, V Stamerra, A Steinbring, T Steinke, B Storz, J Strzys, M Takalo, L Takami, H Tavecchio, F Temnikov, P Terzic, T Tescaro, D Teshima, M Thaele, J Tibolla, O Torres, DF Toyama, T Treves, A Uellenbeck, M Vogler, P Zanin, R Archambault, S Archer, A Beilicke, M Benbow, W Berger, K Bird, R Biteau, J Buckley, JH Bugaev, V Cerruti, M Chen, X Ciupik, L Collins-Hughes, E Cui, W Eisch, JD Falcone, A Feng, Q Finley, JP Fortin, P Fortson, L Furniss, A Galante, N Gillanders, GH Griffin, S Gyuk, G Hakansson, N Holder, J Johnson, CA Kaaret, P Kar, P Kertzman, M Kieda, D Lang, MJ McArthur, S McCann, A Meagher, K Millis, J Moriarty, P Ong, RA Otte, AN Perkins, JS Pichel, A Pohl, M Popkow, A Prokoph, H Pueschel, E Ragan, K Reyes, LC Reynolds, PT Richards, GT Roache, E Rovero, AC Sembroski, GH Shahinyan, K Staszak, D Telezhinsky, I Tucci, JV Tyler, J Varlotta, A Wakely, SP Welsing, R Wilhelm, A Williams, DA Buson, S Finke, J Villata, M Raiteri, C Aller, HD Aller, MF Cesarini, A Chen, WP Gurwell, MA Jorstad, SG Kimeridze, GN Koptelova, E Kurtanidze, OM Kurtanidze, SO Lahteenmaki, A Larionov, VM Larionova, EG Lin, HC McBreen, B Moody, JW Morozova, DA Marscher, AP Max-Moerbeck, W Nikolashvili, MG Perri, M Readhead, ACS Richards, JL Ros, JA Sadun, AC Sakamoto, T Sigua, LA Smith, PS Tornikoski, M Troitsky, IS Wehrle, AE Jordan, B AF Aleksi, J. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Bangale, P. de Almeida, U. Barres Barrio, J. A. Gonzalez, J. Becerra Bednarek, W. Bernardini, E. Biasuzzi, B. Biland, A. Blanch, O. Boller, A. Bonnefoy, S. Bonnoli, G. Borracci, F. Bretz, T. Carmona, E. Carosi, A. Colin, P. Colombo, E. Contreras, J. L. Cortina, J. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. De Lotto, B. Wilhelmi, E. de Ona Mendez, C. Delgado Prester, D. Dominis Dorner, D. Doro, M. Einecke, S. Eisenacher, D. Elsaesser, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Galindo, D. Lopez, R. J. Garcia Garczarczyk, M. Terrats, D. Garrido Gaug, M. Godinovic, N. Munoz, A. Gonzalez Gozzini, S. R. Hadasch, D. Hanabata, Y. Hayashida, M. Herrera, J. Hildebrand, D. Hose, J. Hrupec, D. Hughes, G. Idec, W. Kadenius, V. Kellermann, H. Knoetig, M. L. Kodani, K. Konno, Y. Krause, J. Kubo, H. Kushida, J. La Barbera, A. Lelas, D. Lewandowska, N. Lindfors, E. Lombardi, S. Lopez, M. Lopez-Coto, R. Lopez-Oramas, A. Lorenz, E. Lozano, I. Makariev, M. Mallot, K. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Miranda, J. M. Mirzoyan, R. Moralejo, A. Munar-Adrover, P. Nakajima, D. Niedzwiecki, A. Nilsson, K. Nishijima, K. Noda, K. Orito, R. Overkemping, A. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Persic, M. Moroni, P. G. Prada Prandini, E. Puljak, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Garcia, J. Rodriguez Rugamer, S. Saito, T. Saito, K. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Sun, S. Shore, S. N. Sillanpaa, A. Sitarek, J. Snidaric, I. Sobczynska, D. Spanier, F. Stamatescu, V. Stamerra, A. Steinbring, T. Steinke, B. Storz, J. Strzys, M. Takalo, L. Takami, H. Tavecchio, F. Temnikov, P. Terzic, T. Tescaro, D. Teshima, M. Thaele, J. Tibolla, O. Torres, D. F. Toyama, T. Treves, A. Uellenbeck, M. Vogler, P. Zanin, R. Archambault, S. Archer, A. Beilicke, M. Benbow, W. Berger, K. Bird, R. Biteau, J. Buckley, J. H. Bugaev, V. Cerruti, M. Chen, X. Ciupik, L. Collins-Hughes, E. Cui, W. Eisch, J. D. Falcone, A. Feng, Q. Finley, J. P. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gillanders, G. H. Griffin, S. Gyuk, G. Hakansson, N. Holder, J. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Kieda, D. Lang, M. J. McArthur, S. McCann, A. Meagher, K. Millis, J. Moriarty, P. Ong, R. A. Otte, A. N. Perkins, J. S. Pichel, A. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Ragan, K. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. Rovero, A. C. Sembroski, G. H. Shahinyan, K. Staszak, D. Telezhinsky, I. Tucci, J. V. Tyler, J. Varlotta, A. Wakely, S. P. Welsing, R. Wilhelm, A. Williams, D. A. Buson, S. Finke, J. Villata, M. Raiteri, C. Aller, H. D. Aller, M. F. Cesarini, A. Chen, W. P. Gurwell, M. A. Jorstad, S. G. Kimeridze, G. N. Koptelova, E. Kurtanidze, O. M. Kurtanidze, S. O. Lahteenmaki, A. Larionov, V. M. Larionova, E. G. Lin, H. C. McBreen, B. Moody, J. W. Morozova, D. A. Marscher, A. P. Max-Moerbeck, W. Nikolashvili, M. G. Perri, M. Readhead, A. C. S. Richards, J. L. Ros, J. A. Sadun, A. C. Sakamoto, T. Sigua, L. A. Smith, P. S. Tornikoski, M. Troitsky, I. S. Wehrle, A. E. Jordan, B. CA MAGIC Collaboration VERITAS Collaboration TI Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanisms: non-thermal; galaxies: active; BL Lacertae objects: individual: Mrk 421; gamma rays: galaxies ID LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; GAMMA-RAY OUTBURST; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; ATMOSPHERIC CHERENKOV TELESCOPES; EXTRAGALACTIC BACKGROUND LIGHT; SPECTRAL ENERGY-DISTRIBUTION; SELF-COMPTON MODEL; X-RAY; TEV BLAZARS AB Context. Because of its proximity, Mrk 421 is one of the best sources on which to study the nature of BL Lac objects. Its proximity allows us to characterize its broadband spectral energy distribution (SED). Aims. The goal is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk 421. These mechanisms may also apply to more distant blazars that cannot be studied with the same level of detail. Methods. A flare occurring in March 2010 was observed for 13 consecutive days (from MJD 55 265 to MJD 55 277) with unprecedented wavelength coverage from radio to very high energy (VHE; E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, Fermi-LAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We modeled the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigated the physical parameters, and evaluated whether the observed broadband SED variability can be associated with variations in the relativistic particle population. Results. The activity of Mrk 421 initially was high and then slowly decreased during the 13-day period. The flux variability was remarkable at the X-ray and VHE bands, but it was minor or not significant at the other bands. The variability in optical polarization was also minor. These observations revealed an almost linear correlation between the X-ray flux at the 2-10 keV band and the VHE gamma-ray flux above 200 GeV, consistent with the gamma-rays being produced by inverse-Compton scattering in the Klein-Nishina regime in the framework of SSC models. The one-zone SSC model can describe the SED of each day for the 13 consecutive days reasonably well, which once more shows the success of this standard theoretical scenario to describe the SEDs of VHE BL Lacs such as Mrk 421. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission, while the other smaller zone, which is spatially separated from the first, contributes to the daily variable emission occurring at X-rays and VHE gamma-rays. The second blob is assumed to have a smaller volume and a narrow electron energy distribution with 3 x 10(4) < gamma < 6 x 10(5), where. is the Lorentz factor of the electrons. Such a two-zone scenario would naturally lead to the correlated variability at the X-ray and VHE bands without variability at the optical/UV band, as well as to shorter timescales for the variability at the X-ray and VHE bands with respect to the variability at the other bands. Conclusions. Both the one-zone and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly with the underlying particle population. This shows that the particle acceleration and cooling mechanism that produces the radiating particles might be the main mechanism responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement with the observed SED at the narrow peaks of the low-and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by varying the parameters related to the emitting region itself (delta, B and R), in addition to the parameters related to the particle population. C1 [Aleksi, J.; Blanch, O.; Cortina, J.; Munoz, A. Gonzalez; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Rico, J.; Sitarek, J.; Stamatescu, V.] Campus UAB, IFAE, Bellaterra 08193, Spain. [Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy. [Ansoldi, S.; Biasuzzi, B.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Ist Nazl Fis Nucl, I-33100 Udine, Italy. [Antonelli, L. A.; Bonnoli, G.; Carosi, A.; Covino, S.; La Barbera, A.; Lombardi, S.; Maraschi, L.; Stamerra, A.; Tavecchio, F.] INAF Natl Inst Astrophys, I-00136 Rome, Italy. [Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] Univ Siena, I-53100 Siena, Italy. [Antoranz, P.; Da Vela, P.; Miranda, J. M.; Paoletti, R.] INFN Pisa, I-53100 Siena, Italy. [Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Rijeka, Rudjer Boskovic Inst, Croatian MAGIC Consortium, Zagreb 10000, Croatia. [Babic, A.; Prester, D. Dominis; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Terzic, T.] Univ Split, Zagreb 10000, Croatia. [Bangale, P.; de Almeida, U. Barres; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hose, J.; Kellermann, H.; Krause, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Noda, K.; Paneque, D.; Garcia, J. Rodriguez; Schweizer, T.; Sun, S.; Steinke, B.; Strzys, M.; Teshima, M.; Toyama, T.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Barrio, J. A.; Bonnefoy, S.; Contreras, J. L.; Fonseca, M. V.; Lopez, M.; Lozano, I.; Satalecka, K.; Scapin, V.] Univ Complutense, Madrid 28040, Spain. [Gonzalez, J. Becerra; Colombo, E.; Lopez, R. J. Garcia; Herrera, J.; Tescaro, D.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Bednarek, W.; Idec, W.; Niedzwiecki, A.; Sobczynska, D.] Univ Lodz, PL-90236 Lodz, Poland. [Bernardini, E.; De Caneva, G.; Garczarczyk, M.; Gozzini, S. R.; Hughes, G.; Mallot, K.; Chen, X.; Pohl, M.; Prokoph, H.; Telezhinsky, I.; Welsing, R.; Wilhelm, A.] DESY, D-15738 Zeuthen, Germany. [Biland, A.; Boller, A.; Hildebrand, D.; Knoetig, M. L.; Prandini, E.; Vogler, P.] ETH, CH-8093 Zurich, Switzerland. [Bretz, T.; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Rugamer, S.; Spanier, F.; Steinbring, T.; Storz, J.; Tibolla, O.] Univ Wurzburg, D-97074 Wurzburg, Germany. [Carmona, E.; Mendez, C. Delgado] CIEMAT, E-28040 Madrid, Spain. [Wilhelmi, E. de Ona; Hadasch, D.] Inst Space Sci, Barcelona 08193, Spain. [Doro, M.; Mariotti, M.; Paiano, S.; Scalzotto, V.; Schultz, C.; Buson, S.] Univ Padua, I-35131 Padua, Italy. [Doro, M.; Mariotti, M.; Paiano, S.; Scalzotto, V.; Schultz, C.; Buson, S.] Ist Nazl Fis Nucl, I-35131 Padua, Italy. [Einecke, S.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.; Uellenbeck, M.] Tech Univ Dortmund, D-44221 Dortmund, Germany. [Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, Dept Fis, Unitat Fis Radiac, Bellaterra 08193, Spain. [Font, L.; Terrats, D. Garrido; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain. [Galindo, D.; Marcote, B.; Munar-Adrover, P.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain. [Hanabata, Y.; Hayashida, M.; Kodani, K.; Konno, Y.; Kubo, H.; Kushida, J.; Nakajima, D.; Nishijima, K.; Orito, R.; Saito, T.; Saito, K.; Takami, H.] Kyoto Univ, Div Phys & Astron, Japanese MAGIC Consortium, Kashiwa, Chiba 2778582, Japan. [Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, SF-20500 Turku, Finland. [Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, Oulu 90014, Finland. [Makariev, M.; Maneva, G.; Temnikov, P.] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria. [Moroni, P. G. Prada; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy. [Moroni, P. G. Prada; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy. [Torres, D. F.] ICREA, Barcelona 08193, Spain. [Torres, D. F.] Inst Space Sci, Barcelona 08193, Spain. [Treves, A.] Univ Insubria, I-22100 Como, Italy. [Treves, A.] INFN Milano Bicocca, I-22100 Como, Italy. [Gonzalez, J. Becerra; Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Gonzalez, J. Becerra; Perkins, J. S.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Gonzalez, J. Becerra; Perkins, J. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Archambault, S.; Griffin, S.; Ragan, K.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Cerruti, M.; Fortin, P.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Collins-Hughes, E.; Pueschel, E.; McBreen, B.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Biteau, J.; Furniss, A.; Johnson, C. A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Chen, X.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Ciupik, L.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Tucci, J. V.; Varlotta, A.; Richards, J. L.] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA. [Eisch, J. D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Falcone, A.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Fortson, L.; Shahinyan, K.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Gillanders, G. H.; Lang, M. J.; Moriarty, P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kar, P.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [McArthur, S.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Meagher, K.; Otte, A. N.; Richards, G. T.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Pichel, A.; Rovero, A. C.] Inst Astron & Fis Espacio, RA-1428 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 Appl Phys & Instrumentat, Cork, Ireland. [Finke, J.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Villata, M.; Raiteri, C.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Cesarini, A.] Univ Trent, Dept Phys, I-38050 Trento, Italy. [Chen, W. P.; Koptelova, E.; Lin, H. C.] Natl Cent Univ, Grad Inst Astron, Jhongli 32054, Taiwan. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jorstad, S. G.; Marscher, A. P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, S. G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Koptelova, E.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kimeridze, G. N.; Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Kurtanidze, O. M.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. [Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Lahteenmaki, A.] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland. [Larionov, V. M.; Larionova, E. G.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Peetersburg 198504, Russia. [Larionov, V. M.] Pulkovo Observ, St Petersburg 198504, Russia. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Moody, J. W.] Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. [Max-Moerbeck, W.; Readhead, A. C. S.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Perri, M.] ASI Sci Data Ctr, I-00133 Rome, Italy. [Ros, J. A.] Agrp Astron Sabadell, Sabadell Barcelona 08206, Spain. [Sadun, A. C.] Univ Colorado Denver, Dept Phys, Denver, CO 80217 USA. [Sakamoto, T.] Aoyama Gakuin Univ, Coll Sci & Engn, Dept Math & Phys, Sagamihara, Kanagawa 2525258, Japan. [Smith, P. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. RP Paneque, D (reprint author), Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. EM dpaneque@mpp.mpg.de; sysun@mpp.mpg.de; takami@post.kek.jp RI Fonseca Gonzalez, Maria Victoria/I-2004-2015; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Delgado, Carlos/K-7587-2014; Barrio, Juan/L-3227-2014; Martinez Rodriguez, Manel/C-2539-2017; Cortina, Juan/C-2783-2017; Lahteenmaki, Anne/L-5987-2013; Larionov, Valeri/H-1349-2013; Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Lopez Moya, Marcos/L-2304-2014; Morozova, Daria/H-1298-2013; Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; GAug, Markus/L-2340-2014; Miranda, Jose Miguel/F-2913-2013; Stamatescu, Victor/C-9945-2016 OI Bonnoli, Giacomo/0000-0003-2464-9077; Antonelli, Lucio Angelo/0000-0002-5037-9034; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Bird, Ralph/0000-0002-4596-8563; Doro, Michele/0000-0001-9104-3214; Covino, Stefano/0000-0001-9078-5507; de Ona Wilhelmi, Emma/0000-0002-5401-0744; LA BARBERA, ANTONINO/0000-0002-5880-8913; Cesarini, Andrea/0000-0002-8611-8610; Villata, Massimo/0000-0003-1743-6946; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; De Lotto, Barbara/0000-0003-3624-4480; Perri, Matteo/0000-0003-3613-4409; Persic, Massimo/0000-0003-1853-4900; Raiteri, Claudia Maria/0000-0003-1784-2784; Temnikov, Petar/0000-0002-9559-3384; Torres, Diego/0000-0002-1522-9065; Delgado, Carlos/0000-0002-7014-4101; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Pueschel, Elisa/0000-0002-0529-1973; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; Larionov, Valeri/0000-0002-4640-4356; Font, Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Lopez Moya, Marcos/0000-0002-8791-7908; Morozova, Daria/0000-0002-9407-7804; Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; GAug, Markus/0000-0001-8442-7877; Miranda, Jose Miguel/0000-0002-1472-9690; Stamatescu, Victor/0000-0001-9030-7513 FU German BMBF; German MPG; Italian INFN; Italian INAF; Swiss National Fund SNF; ERDF under the Spanish MINECO; Japanese JSPS; Japanese MEXT; Centro de Excelencia Severo Ochoa project of the Spanish Consolider-Ingenio programme [SEV-2012-0234]; CPAN project of the Spanish Consolider-Ingenio programme [CSD2007-00042]; MultiDark project of the Spanish Consolider-Ingenio programme [CSD2009-00064]; Academy of Finland [268740, 212656, 210338, 121148]; Croatian Science Foundation (HrZZ) Project [09/176]; University of Rijeka [13.12.1.3.02]; DFG Collaborative Research Centers [SFB823/C4, SFB876/C3]; Polish MNiSzW [745/N-HESS-MAGIC/2010/0]; US Department of Energy Office of Science; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK; NASA [NNX11AQ03G, NNX08AW31G, NNX11A043G]; Academia Sinica; NSF [AST-0808050, AST-1109911]; Russian RFBR [12-02-00452]; St. Petersburg University [6.0.163.2010, 6.38.71.2012]; Georgian National Science Foundation [GNSF/ST07/4-180]; Shota Rustaveli National Science Foundation [FR/577/6-320/13] FX The authors thank the anonymous referee for providing a very detailed and constructive list of remarks that helped us to improve the manuscript. The MAGIC collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO, and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Centro de Excelencia Severo Ochoa SEV-2012-0234, CPAN CSD2007-00042, and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0. The VERITAS collaboration acknowledges supports from the grants from the US Department of Energy Office of Science, the US National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748) and by STFC in the UK. 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 Fermi-LAT collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France. The research at Boston University was funded in part by NASA Fermi Guest Investigator grant NNX11AQ03G. 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 program is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). This work was partly supported by Russian RFBR grant 12-02-00452 and St. Petersburg University research grants 6.0.163.2010, 6.38.71.2012. The Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST07/4-180 and by the Shota Rustaveli National Science Foundation through the grant FR/577/6-320/13.; We acknowledge the use of public data from the Swift and RXTE data archive. NR 98 TC 11 Z9 11 U1 4 U2 26 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 JUN PY 2015 VL 578 AR A22 DI 10.1051/0004-6361/201424811 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600034 ER PT J AU Benisty, M Juhasz, A Boccaletti, A Avenhaus, H Milli, J Thalmann, C Dominik, C Pinilla, P Buenzli, E Pohl, A Beuzit, JL Birnstiel, T de Boer, J Bonnefoy, M Chauvin, G Christiaens, V Garufi, A Grady, C Henning, T Huelamo, N Isella, A Langlois, M Menard, F Mouillet, D Olofsson, J Pantin, E Pinte, C Pueyo, L AF Benisty, M. Juhasz, A. Boccaletti, A. Avenhaus, H. Milli, J. Thalmann, C. Dominik, C. Pinilla, P. Buenzli, E. Pohl, A. Beuzit, J. -L. Birnstiel, T. de Boer, J. Bonnefoy, M. Chauvin, G. Christiaens, V. Garufi, A. Grady, C. Henning, T. Huelamo, N. Isella, A. Langlois, M. Menard, F. Mouillet, D. Olofsson, J. Pantin, E. Pinte, C. Pueyo, L. TI Asymmetric features in the protoplanetary disk MWC 758 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: high angular resolution; protoplanetary disks ID HD 142527; IMAGING POLARIMETRY; TRANSITIONAL DISKS; DUST FILTRATION; SPIRAL ARMS; GAP EDGES; PLANET; EVOLUTION; VLT/NACO; MWC-758 AB Context. The study of dynamical processes in protoplanetary disks is essential to understand planet formation. In this context, transition disks are prime targets because they are at an advanced stage of disk clearing and may harbor direct signatures of disk evolution. Aims. We aim to derive new constraints on the structure of the transition disk MWC 758, to detect non-axisymmetric features and understand their origin. Methods. We obtained infrared polarized intensity observations of the protoplanetary disk MWC 758 with VLT/SPHERE at 1.04 mu m to resolve scattered light at a smaller inner working angle (0.093 '') and a higher angular resolution (0.027 '') than previously achieved. Results. We observe polarized scattered light within 0.53 '' (148 au) down to the inner working angle (26 au) and detect distinct non-axisymmetric features but no fully depleted cavity. The two small-scale spiral features that were previously detected with HiCIAO are resolved more clearly, and new features are identified, including two that are located at previously inaccessible radii close to the star. We present a model based on the spiral density wave theory with two planetary companions in circular orbits. The best model requires a high disk aspect ratio (H/r similar to 0.20 at the planet locations) to account for the large pitch angles which implies a very warm disk. Conclusions. Our observations reveal the complex morphology of the disk MWC 758. To understand the origin of the detected features, the combination of high-resolution observations in the submillimeter with ALMA and detailed modeling is needed. C1 [Benisty, M.; Beuzit, J. -L.; Bonnefoy, M.; Chauvin, G.; Menard, F.; Mouillet, D.; Pinte, C.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Benisty, M.; Beuzit, J. -L.; Bonnefoy, M.; Chauvin, G.; Menard, F.; Mouillet, D.; Pinte, C.] CNRS, IPAG, F-38000 Grenoble, France. [Juhasz, A.] Inst Astron, Cambridge CB3 OHA, England. [Boccaletti, A.] Univ Paris 07, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Avenhaus, H.; Christiaens, V.] Univ Chile, Dept Astron, Santiago, Chile. [Milli, J.; de Boer, J.] ESO, Santiago, Chile. [Thalmann, C.; Garufi, A.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Dominik, C.] Sterrenkundig Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Pinilla, P.; de Boer, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Buenzli, E.; Pohl, A.; Henning, T.; Olofsson, J.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Pohl, A.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Grady, C.] Eureka Sci, Greenbelt, MD 20771 USA. [Grady, C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Huelamo, N.] Ctr Astrobiol INTA CSIC, Villanueva De La Canada 28691, Spain. [Isella, A.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Langlois, M.] Univ Lyon 1, CNRS, Ecole Normale Super Lyon, Observ Lyon,Ctr Rech Astrophys Lyon,UMR 5574, F-69230 St Genis Laval, France. [Menard, F.; Pinte, C.] Univ Chile, CNRS INSU, UMI FCA, France UMI 3386, Santiago, Chile. [Menard, F.; Pinte, C.] Univ Chile, Dept Astron, Santiago, Chile. [Pantin, E.] Univ Paris Diderot, CNRS, CEA DSM, Lab AIM,IRFU SAp, F-91191 Gif Sur Yvette, France. [Pueyo, L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Benisty, M (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. EM Myriam.Benisty@obs.ujf-grenoble.fr RI Huelamo, Nuria/C-3042-2017; OI Huelamo, Nuria/0000-0002-2711-8143; Buenzli, Esther/0000-0003-3306-1486; Birnstiel, Tilman/0000-0002-1899-8783 FU "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France; NASA Origins of Solar Systems program [NNG13PB64P]; NASA Origins of Solar Systems [NNX12AJ04G] FX We acknowledge the SVT team at ESO HQ for their help during the preparation of the OBs and the VLT team for conducting the observations. We thank C. P. Dullemond, G. Lesur, M. Min, and M. Tauras for fruitful discussions, and the referee for providing useful comments. M.B. acknowledges financial support from "Programme National de Physique Stellaire" (PNPS) of CNRS/INSU, France. C.G. was supported under the NASA Origins of Solar Systems program on NNG13PB64P. T.B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. NR 41 TC 46 Z9 46 U1 1 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR L6 DI 10.1051/0004-6361/201526011 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600007 ER PT J AU Borsa, F Scandariato, G Rainer, M Bignamini, A Maggio, A Poretti, E Lanza, AF Di Mauro, MP Benatti, S Biazzo, K Bonomo, AS Damasso, M Esposito, M Gratton, R Affer, L Barbieri, M Boccato, C Claudi, RU Cosentino, R Covino, E Desidera, S Fiorenzano, AFM Gandolfi, D Harutyunyan, A Maldonado, J Micela, G Molaro, P Molinari, E Pagano, I Pillitteri, I Piotto, G Shkolnik, E Silvotti, R Smareglia, R Southworth, J Sozzetti, A Stelzer, B AF Borsa, F. Scandariato, G. Rainer, M. Bignamini, A. Maggio, A. Poretti, E. Lanza, A. F. Di Mauro, M. P. Benatti, S. Biazzo, K. Bonomo, A. S. Damasso, M. Esposito, M. Gratton, R. Affer, L. Barbieri, M. Boccato, C. Claudi, R. U. Cosentino, R. Covino, E. Desidera, S. Fiorenzano, A. F. M. Gandolfi, D. Harutyunyan, A. Maldonado, J. Micela, G. Molaro, P. Molinari, E. Pagano, I. Pillitteri, I. Piotto, G. Shkolnik, E. Silvotti, R. Smareglia, R. Southworth, J. Sozzetti, A. Stelzer, B. TI The GAPS programme with HARPS-N at TNG VII. Putting exoplanets in the stellar context: magnetic activity and asteroseismology of tau Bootis A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: tau Boo; planetary systems; asteroseismology; techniques: spectroscopic; stars: activity ID SOLAR-LIKE OSCILLATIONS; CLOSE-IN PLANETS; LATE-TYPE STARS; SUN-LIKE STARS; CA II H; DIFFERENTIAL ROTATION; RADIAL-VELOCITY; HOT JUPITERS; HOST STARS; CHROMOSPHERIC ACTIVITY AB Aims. We observed the tau Boo system with the HARPS-N spectrograph to test a new observational strategy aimed at jointly studying asteroseismology, the planetary orbit, and star-planet magnetic interaction. Methods. We collected high-cadence observations on 11 nearly consecutive nights and for each night averaged the raw FITS files using a dedicated software. In this way we obtained spectra with a high signal-to-noise ratio, used to study the variation of the Ca II H&K lines and to have radial velocity values free from stellar oscillations, without losing the oscillations information. We developed a dedicated software to build a new custom mask that we used to refine the radial velocity determination with the HARPS-N pipeline and perform the spectroscopic analysis. Results. We updated the planetary ephemeris and showed the acceleration caused by the stellar binary companion. Our results on the stellar activity variation suggest the presence of a high-latitude plage during the time span of our observations. The correlation between the chromospheric activity and the planetary orbital phase remains unclear. Solar-like oscillations are detected in the radial velocity time series: we estimated asteroseismic quantities and found that they agree well with theoretical predictions. Our stellar model yields an age of 0.9 +/- 0.5 Gyr for tau Boo and further constrains the value of the stellar mass to 1.38 +/- 0.05 M-circle dot. C1 [Borsa, F.; Rainer, M.; Poretti, E.] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Scandariato, G.; Lanza, A. F.; Biazzo, K.; Cosentino, R.; Gandolfi, D.; Pagano, I.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Bignamini, A.; Molaro, P.; Smareglia, R.] Osserv Astron Trieste, INAF, I-34143 Trieste, Italy. [Maggio, A.; Affer, L.; Maldonado, J.; Micela, G.; Pillitteri, I.; Stelzer, B.] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. [Di Mauro, M. P.] IAPS, INAF, I-00133 Rome, Italy. [Benatti, S.; Gratton, R.; Boccato, C.; Claudi, R. U.; Desidera, S.; Piotto, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Bonomo, A. S.; Damasso, M.; Silvotti, R.; Sozzetti, A.] Osservatorio Astrofis Torino, INAF, I-10025 Pino Torinese, Italy. [Esposito, M.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Esposito, M.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Barbieri, M.] Univ Atacama, Dept Phys, Copayapu 485, Copiapo, Chile. [Cosentino, R.; Fiorenzano, A. F. M.; Harutyunyan, A.; Molinari, E.] INAF, Fdn Galileo Galilei, Brena Baja 38712, TF, Spain. [Covino, E.] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy. [Gandolfi, D.] Heidelberg Univ, Zentrum Astron, Landessternwarte Konigstuhl, D-69117 Heidelberg, Germany. [Molinari, E.] IASF, INAF, I-20133 Milan, Italy. [Pillitteri, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Piotto, G.] Univ Padua, Dip Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Shkolnik, E.] Lowell Observ, Flagstaff, AZ 86001 USA. [Southworth, J.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Borsa, F (reprint author), Osserv Astron Brera, INAF, Via E Bianchi 46, I-23807 Merate, LC, Italy. EM francesco.borsa@brera.inaf.it RI Maggio, Antonio/P-5700-2015; Pagano, Isabella/I-6934-2015; Pillitteri, Ignazio/L-1549-2016 OI Maggio, Antonio/0000-0001-5154-6108; Pagano, Isabella/0000-0001-9573-4928; Pillitteri, Ignazio/0000-0003-4948-6550 FU INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research FX The GAPS project acknowledges support from INAF through the "Progetti Premiali" funding scheme of the Italian Ministry of Education, University, and Research. We thank the referee G. Walker for interesting and useful comments that helped improve the clarity of the paper. NR 87 TC 9 Z9 9 U1 0 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 JUN PY 2015 VL 578 AR A64 DI 10.1051/0004-6361/201525741 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600076 ER PT J AU Hsiao, EY Burns, CR Contreras, C Hoflich, P Sand, D Marion, GH Phillips, MM Stritzinger, M Gonzalez-Gaitan, S Mason, RE Folatelli, G Parent, E Gall, C Amanullah, R Anupama, GC Arcavi, I Banerjee, DPK Beletsky, Y Blanc, GA Bloom, JS Brown, PJ Campillay, A Cao, Y De Cia, A Diamond, T Freedman, WL Gonzalez, C Goobar, A Holmbo, S Howell, DA Johansson, J Kasliwal, MM Kirshner, RP Krisciunas, K Kulkarni, SR Maguire, K Milne, PA Morrell, N Nugent, PE Ofek, EO Osip, D Palunas, P Perley, DA Persson, SE Piro, AL Rabus, M Roth, M Schiefelbein, JM Srivastav, S Sullivan, M Suntzeff, NB Surace, J Wozniak, PR Yaron, O AF Hsiao, E. Y. Burns, C. R. Contreras, C. Hoeflich, P. Sand, D. Marion, G. H. Phillips, M. M. Stritzinger, M. Gonzalez-Gaitan, S. Mason, R. E. Folatelli, G. Parent, E. Gall, C. Amanullah, R. Anupama, G. C. Arcavi, I. Banerjee, D. P. K. Beletsky, Y. Blanc, G. A. Bloom, J. S. Brown, P. J. Campillay, A. Cao, Y. De Cia, A. Diamond, T. Freedman, W. L. Gonzalez, C. Goobar, A. Holmbo, S. Howell, D. A. Johansson, J. Kasliwal, M. M. Kirshner, R. P. Krisciunas, K. Kulkarni, S. R. Maguire, K. Milne, P. A. Morrell, N. Nugent, P. E. Ofek, E. O. Osip, D. Palunas, P. Perley, D. A. Persson, S. E. Piro, A. L. Rabus, M. Roth, M. Schiefelbein, J. M. Srivastav, S. Sullivan, M. Suntzeff, N. B. Surace, J. Wozniak, P. R. Yaron, O. TI Strong near-infrared carbon in the Type Ia supernova iPTF13ebh SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: general; supernovae: general; supernovae: individual: iPTF13ebh ID PHOTOMETRY DATA RELEASE; HUBBLE-SPACE-TELESCOPE; HIGH-VELOCITY FEATURES; TIME OPTICAL-SPECTRA; WHITE-DWARF STAR; LIGHT CURVES; SN 2014J; MAXIMUM-LIGHT; THERMONUCLEAR SUPERNOVAE; FACTORY OBSERVATIONS AB We present near-infrared (NIR) time-series spectroscopy, as well as complementary ultraviolet (UV), optical, and NIR data, of the Type Ia supernova (SN Ia) iPTF13ebh, which was discovered within two days from the estimated time of explosion. The first NIR spectrum was taken merely 2 : 3 days after explosion and may be the earliest NIR spectrum yet obtained of a SN Ia. The most striking features in the spectrum are several NIR C I lines, and the C I lambda 1.0693 mu m line is the strongest ever observed in a SN Ia. Interestingly, no strong optical C II counterparts were found, even though the optical spectroscopic time series began early and is densely cadenced. Except at the very early epochs, within a few days from the time of explosion, we show that the strong NIR C I compared to the weaker optical C II appears to be general in SNe Ia. iPTF13ebh is a fast decliner with Delta m(15)(B) = 1.79 +/- 0.01, and its absolute magnitude obeys the linear part of the width-luminosity relation. It is therefore categorized as a "transitional" event, on the fast-declining end of normal SNe Ia as opposed to subluminous/91bg-like objects. iPTF13ebh shows NIR spectroscopic properties that are distinct from both the normal and subluminous/91bg-like classes, bridging the observed characteristics of the two classes. These NIR observations suggest that composition and density of the inner core are similar to that of 91bg-like events, and that it has a deep-reaching carbon burning layer that is not observed in more slowly declining SNe Ia. There is also a substantial difference between the explosion times inferred from the early-time light curve and the velocity evolution of the Si II lambda 0.6355 mu m line, implying a long dark phase of similar to 4 days. C1 [Hsiao, E. Y.; Contreras, C.; Stritzinger, M.; Gall, C.; Holmbo, S.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Hsiao, E. Y.; Contreras, C.; Phillips, M. M.; Beletsky, Y.; Campillay, A.; Gonzalez, C.; Morrell, N.; Osip, D.; Palunas, P.; Roth, M.] Campanas Observ, Carnegie Observ, Colina El Pino, Chile. [Burns, C. R.; Blanc, G. A.; Freedman, W. L.; Kasliwal, M. M.; Persson, S. E.; Piro, A. L.] Carnegie Observ, Pasadena, CA 91101 USA. [Hoeflich, P.; Diamond, T.] Florida State Univ, Tallahassee, FL 32306 USA. [Sand, D.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Marion, G. H.] Univ Texas Austin, Austin, TX 78712 USA. [Marion, G. H.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gonzalez-Gaitan, S.] Millennium Inst Astrophys, Santiago, Chile. [Gonzalez-Gaitan, S.; Blanc, G. A.] Univ Chile, Dept Astron, Santiago, Chile. [Mason, R. E.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Folatelli, G.] CCT CONICET UNLP, IALP, La Plata, Buenos Aires, Argentina. [Folatelli, G.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Parent, E.] Bishops Univ, Dept Phys, Sherbrooke, PQ J1M 1Z7, Canada. [Gall, C.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Amanullah, R.; Goobar, A.; Johansson, J.] Stockholm Univ, Dept Phys, Oskar Klein Ctr, Albanova Univ Ctr, S-10691 Stockholm, Sweden. [Anupama, G. C.; Srivastav, S.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Arcavi, I.; Howell, D. A.] Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Arcavi, I.; Howell, D. A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Banerjee, D. P. K.] Phys Res Lab, Astron & Astrophys Div, Ahmadabad 380009, Gujarat, India. [Bloom, J. S.; Nugent, P. E.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Brown, P. J.; Krisciunas, K.; Schiefelbein, J. M.; Suntzeff, N. B.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Cao, Y.; Kulkarni, S. R.; Perley, D. A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Nugent, P. E.] Lawrence Berkeley Natl Lab, Computat Res Div, Computat Cosmol Ctr, Berkeley, CA 94611 USA. [Maguire, K.] European Southern Observ Astron Res Southern Hemi, D-85748 Garching, Germany. [Milne, P. A.] Univ Arizona, Steward Observ, Tucson, AZ 85719 USA. [De Cia, A.; Ofek, E. O.; Yaron, O.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Rabus, M.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago, Region Metropol, Chile. [Sullivan, M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Surace, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Wozniak, P. R.] Los Alamos Natl Lab, Space & Remote Sensing, Los Alamos, NM 87545 USA. RP Hsiao, EY (reprint author), Aarhus Univ, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark. EM hsiao@phys.au.dk RI Gall, Christa/P-7630-2016; OI Gall, Christa/0000-0002-8526-3963; Wozniak, Przemyslaw/0000-0002-9919-3310; Sullivan, Mark/0000-0001-9053-4820; stritzinger, maximilian/0000-0002-5571-1833 FU National Science Foundation [AST-1008343]; Danish Agency for Science and Technology and Innovation; CONICYT through FONDECYT [3130680]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC12009]; Danish National Research Foundation; US Department of Energy; Gemini Observatory [GN-2013B-Q-76]; Office of Science of the US Department of Energy [DE-AC02-05CH11231]; National Aeronautics and Space Administration FX This paper is based upon work supported by the National Science Foundation under Grant No. AST-1008343. M.S., E.Y.H., C.C, and C.G. acknowledge the generous support provided by the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant. S.G. acknowledges support from CONICYT through FONDECYT grant 3130680 and from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. The Dark Cosmology Centre is funded by the Danish National Research Foundation. LANL participation in iPTF is supported by the US Department of Energy as part of the Laboratory Directed Research and Development program. The bulk of the data presented here was obtained with the 1 m Swope, 2.5 m du Pont, and the 6.5 m Magellan Telescopes at the Las Campanas Observatory. This work also relies on data obtained at the Gemini Observatory, under the long-term program GN-2013B-Q-76. The Gemini Observatory 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), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The authors would like to recognize the very significant cultural role and reverence that the summit of Mauna Kea has within the indigenous community of Hawaii. We are grateful for our opportunity to conduct observations from this mountain. We have also made use of the Nordic Optical Telescope, which is 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 William Herschel Telescope and its override programme 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 research used resources from the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. We have also 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. NR 136 TC 9 Z9 9 U1 0 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A9 DI 10.1051/0004-6361/201425297 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600021 ER PT J AU Luna, GJM Raymond, JC Brickhouse, NS Mauche, CW Suleimanov, V AF Luna, G. J. M. Raymond, J. C. Brickhouse, N. S. Mauche, C. W. Suleimanov, V. TI Testing the cooling flow model in the intermediate polar EX Hydrae SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE novae, cataclysmic variables; radiation mechanisms: general; X-rays: individuals: EX Hydrae ID X-RAY-EMISSION; MAGNETIC CATACLYSMIC VARIABLES; WHITE-DWARF MASSES; HEAT-CONDUCTION; THERMAL CONDUCTION; ACCRETION COLUMN; GALAXY CLUSTERS; SPECTRAL MODEL; SPECTROSCOPY; CHANDRA AB We use the best available X-ray data from the intermediate polar EX Hydrae to study the cooling-flow model often applied to interpret the X-ray spectra of these accreting magnetic white dwarf binaries. First, we resolve a long-standing discrepancy between the X-ray and optical determinations of the mass of the white dwarf in EX Hya by applying new models of the inner disk truncation radius. Our fits to the X-ray spectrum now agree with the white dwarf mass of 0.79 M-circle dot determined using dynamical methods through spectroscopic observations of the secondary. We use a simple isobaric cooling flow model to derive the emission line fluxes, emission measure distribution, and H-like to He-like line ratios for comparison with the 496 ks Chandra High Energy Transmission Grating observation of EX Hydrae. We find that the H/He ratios are not well reproduced by this simple isobaric cooling flow model and show that while H-like line fluxes can be accurately predicted, fluxes of lower-Z He-like lines are significantly underestimated. This discrepancy suggests that an extra heating mechanism plays an important role at the base of the accretion column, where cooler ions form. We thus explored more complex cooling models, including the change of gravitational potential with height in the accretion column and a magnetic dipole geometry. None of these modifications to the standard cooling flow model are able to reproduce the observed line ratios. While a cooling flow model with subsolar (0.1 circle dot) abundances is able to reproduce the line ratios by reducing the cooling rate at temperatures lower than similar to 10(7.3) K, the predicted line-to-continuum ratios are much lower than observed. We discuss and discard mechanisms, such as photoionization, departures from constant pressure, resonant scattering, different electron-ion temperatures, and Compton cooling. Thermal conduction transfers energy from the region above 10(7) K, where the H-like lines are mostly formed, to the cooler regions where the He-like ions of the lower-Z elements are formed, hence in principle it could help resolve the problem. However, simple models indicate that the energy is deposited below 10(6) K, which is too cool to increase the emission of the He-like lines we observe. We conclude that some other effect, such as thermally unstable cooling, modifies the temperature distribution. C1 [Luna, G. J. M.] IAFE CONICET UBA, Buenos Aires, DF, Argentina. [Luna, G. J. M.; Raymond, J. C.; Brickhouse, N. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mauche, C. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Suleimanov, V.] Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany. [Suleimanov, V.] Kazan Volga Reg Fed Univ, Kazan 420008, Russia. RP Luna, GJM (reprint author), IAFE CONICET UBA, CC 67,Suc 28 C1428ZAA CABA, Buenos Aires, DF, Argentina. EM gjmluna@iafe.uba.ar OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA [GO7-8026X]; CONICET/Argentina [PICT 2011/269, PIP D-4598/2012]; US Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344]; German Research Foundation (DFG) [WE 1312/48-1] FX We thanks Vinay Kashyap, Randall K. Smith, and Adam Foster. G.J.M.L. acknowledge support from: NASA to the Smithsonian Astrophysical Observatory (SAO) under Chandra GO7-8026X; grants PICT 2011/269 (Agencia) and PIP D-4598/2012 (CONICET/Argentina). C.W.M.'s contribution to this work was performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. V.S. was supported by German Research Foundation (DFG) grant WE 1312/48-1. NR 55 TC 1 Z9 1 U1 0 U2 1 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 JUN PY 2015 VL 578 AR A15 DI 10.1051/0004-6361/201525755 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600027 ER PT J AU Matuszak, M Karska, A Kristensen, LE Herczeg, GJ Tychoniec, L van Kempen, TA Fuente, A AF Matuszak, M. Karska, A. Kristensen, L. E. Herczeg, G. J. Tychoniec, L. van Kempen, T. A. Fuente, A. TI Far-infrared CO and H2O emission in intermediate-mass protostars SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: protostars; ISM: jets and outflows; ISM: molecules ID STAR-FORMING REGIONS; HERSCHEL-PACS SPECTROSCOPY; YOUNG STELLAR OBJECTS; KEY PROGRAM; EVOLUTIONARY SIGNATURES; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; WATER; GAS; LINES AB Context. Intermediate-mass young stellar objects (YSOs) provide a link to understanding how feedback from shocks and UV radiation scales from low-to high-mass star forming regions. Aims. Our aim is to analyze excitation of CO and H2O in deeply embedded intermediate-mass YSOs and compare it with similar studies on low-mass and high-mass YSOs. Methods. Herschel/PACS spectral maps are analyzed for six YSOs with bolometric luminosities of L-bol similar to 10(2)-10(3) L-circle dot. The maps cover spatial scales of similar to 10(4) AU in several CO and H2O lines located in the similar to 55-210 mu m range. Results. Rotational diagrams of CO show two temperature components at T-rot similar to 320 K and T-rot similar to 700-800 K, comparable to lowand high-mass protostars probed at similar spatial scales. The diagrams for H2O show a single component at T-rot similar to 130 K, as seen in low-mass protostars, and about 100 K lower than in high-mass protostars. Since the uncertainties in T-rot are on the same order as the difference between the intermediate and high-mass protostars, we cannot conclude whether the change in rotational temperature occurs at a specific luminosity or whether the change is more gradual from low-to high-mass YSOs. Conclusions. Molecular excitation in intermediate-mass protostars is comparable to the central 10(3) AU of low-mass protostars and consistent within the uncertainties with the high-mass protostars probed at 3 x 10(3) AU scales, suggesting similar shock conditions in all those sources. C1 [Matuszak, M.; Karska, A.; Tychoniec, L.] Adam Mickiewicz Univ, Astron Observ, PL-60268 Poznan, Poland. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Herczeg, G. J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [van Kempen, T. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Fuente, A.] OAN IGN, Alcala De Henares 28803, Spain. RP Matuszak, M (reprint author), Adam Mickiewicz Univ, Astron Observ, Sloneczna 36, PL-60268 Poznan, Poland. EM agata.karska@gmail.com RI Fuente, Asuncion/G-1468-2016; Kristensen, Lars/F-4774-2011; Karska, Agata/O-5311-2016; OI Fuente, Asuncion/0000-0001-6317-6343; Kristensen, Lars/0000-0003-1159-3721; Karska, Agata/0000-0001-8913-925X; Tychoniec, Lukasz/0000-0002-9470-2358 FU Polish National Science Center [2013/11/N/ST9/00400]; Polish NCN [Dec-2013/08/M/ST9/00664] FX The authors would like to thank the referee for the valuable comments which helped to improve the manuscript. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. A.K. acknowledges support from the Polish National Science Center grant 2013/11/N/ST9/00400. Research conducted within the scope of the HECOLS International Associated Laboratory, supported in part by the Polish NCN grant Dec-2013/08/M/ST9/00664. NR 30 TC 0 Z9 0 U1 0 U2 1 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A20 DI 10.1051/0004-6361/201526021 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600032 ER PT J AU Maxted, PFL Hutcheon, RJ Torres, G Lacy, CHS Southworth, J Smalley, B Pavlovski, K Marschall, LA Clausen, JV AF Maxted, P. F. L. Hutcheon, R. J. Torres, G. Lacy, C. H. S. Southworth, J. Smalley, B. Pavlovski, K. Marschall, L. A. Clausen, J. V. TI Precise mass and radius measurements for the components of the bright solar-type eclipsing binary star V1094 Tauri SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: eclipsing; stars: solar-type; stars: fundamental parameters; stars: individual: V1094 Tau ID LINED SPECTROSCOPIC BINARIES; LIMB-DARKENING COEFFICIENTS; MODEL ATMOSPHERES; F-TYPE; STROMGREN PHOTOMETRY; STELLAR; METALLICITY; CALIBRATIONS; EXTRACTION; ISOCHRONES AB Context. V1094 Tau is a bright eclipsing binary star with an orbital period close to nine days that contains two stars similar to the Sun. Aims. Our aim is to test models of Sun-like stars using precise and accurate mass and radius measurements for both stars in V1094 Tau. Methods. We present new spectroscopy of V1094 Tau, which we use to estimate the effective temperatures of both stars and to refine their spectroscopic orbits. We also present new, high-quality photometry covering both eclipses of V1094 Tau in the Stromgren uvby system and in the Johnson V-band. Results. The masses, radii, and effective temperatures of the stars in V1094 Tau are found to be MA = 1.0965 +/- 0.0040 M +/-, RA = 1.4109 +/- 0.0058 R-circle dot, T-eff,T- A = 5850 +/- 100 K, M-B = 1.0120 +/- 0.0028 M-circle dot, R-B = 1.1063 +/- 0.0066 R-circle dot, and T-eff,T- B = 5700 +/- 100 K. An analysis of the times of mid-eclipse and the radial velocity data reveals apsidal motion with a period of 14 500 +/- 3700 years. Conclusions. The observed masses, radii, and effective temperatures are consistent with stellar models for an age approximate to 6Gyr if the stars are assumed to have a metallicity similar to the Sun. This estimate is in reasonable agreement with our estimate of the metallicity derived using Stromgren photometry and treating the binary as a single star ([Fe/H] = -0.09 +/- 0.11). The rotation velocities of the stars suggest that V1094 Tau is close to the limit at which tidal interactions between the stars force them to rotate pseudosynchronously with the orbital motion. C1 [Maxted, P. F. L.; Hutcheon, R. J.; Southworth, J.; Smalley, B.] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lacy, C. H. S.] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. [Pavlovski, K.] Univ Zagreb, Dept Phys, Zagreb 10000, Croatia. [Marschall, L. A.] Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA. [Clausen, J. V.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. RP Maxted, PFL (reprint author), Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England. EM p.maxted@keele.ac.uk; richard.hutcheon@btinternet.com; gtorres@cfa.harvard.edu FU NSF [AST-1007992] FX We thank the referee for their careful consideration of our manuscript and their constructive comments that have helped to improve the paper. Thanks to Dr. A. W. Neely for the maintenance and operation of the NFO and for preliminary processing and distribution of the images. G.T. acknowledges partial support from NSF grant AST-1007992. J.V.C. participated fully in the data collection and analysis up to the time of his death, but bears no responsibility for the final text of this paper. NR 46 TC 2 Z9 2 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2015 VL 578 AR A25 DI 10.1051/0004-6361/201525873 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600037 ER PT J AU Ness, JU Beardmore, AP Osborne, JP Kuulkers, E Henze, M Piro, AL Drake, JJ Dobrotka, A Schwarz, G Starrfield, S Kretschmar, P Hirsch, M Wilms, J AF Ness, J-U Beardmore, A. P. Osborne, J. P. Kuulkers, E. Henze, M. Piro, A. L. Drake, J. J. Dobrotka, A. Schwarz, G. Starrfield, S. Kretschmar, P. Hirsch, M. Wilms, J. TI Short-period X-ray oscillations in super-soft novae and persistent super-soft sources SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE novae, cataclysmic variables; stars: oscillations; white dwarfs; X-rays: stars ID LARGE-MAGELLANIC-CLOUD; PHOTON IMAGING CAMERA; XMM-NEWTON; RS-OPHIUCHI; CATACLYSMIC VARIABLES; 2006 OUTBURST; GRATING SPECTROMETER; CLASSICAL NOVAE; SOURCE CAL-83; WHITE-DWARFS AB Context. Transient short-period (< 100 s) oscillations have been found in the X-ray light curves of three novae during their super-soft source (SSS) phase and in one persistent SSS. Aims. We pursue an observational approach to determine possible driving mechanisms and relations to fundamental system parameters such as the white dwarf mass. Methods. We performed a systematic search for short-period oscillations in all available XMM-Newton and Chandra X-ray light curves of persistent SSS and novae during their SSS phase. To study time evolution, we divided each light curve into short time-segments and computed power spectra. We then constructed a dynamic power spectrum from which we identified transient periodic signals even when only present for a short time. We base our confidence levels on simulations of false-alarm probability for the chosen oversampling rate of 16, corrected for multiple testing based on the number of time segments. From all time segments of each system, we computed fractions of time when periodic signals were detected. Results. In addition to the previously known systems with short-period oscillations, RSOph (35 s), KTEri (35 s), V339 Del (54 s), and Cal 83 (67 s), we found one additional system, LMC 2009a (33 s), and also confirm the 35 s period from Chandra data of KT Eri. The oscillation amplitudes are of about < 15% of the respective count rates and vary without any clear dependence on the X-ray count rate. The fractions of the time when the respective periods were detected at 2s significance (duty cycle) are 11.3%, 38.8%, 16.9%, 49.2%, and 18.7% for LMC2009a, RSOph, KT Eri, V339 Del, and Cal 83, respectively. The respective highest duty cycles found in a single observation are 38.1%, 74.5%, 61.4%, 67.8%, and 61.8%. Conclusions. Since fast rotation periods of the white dwarfs as origin of these transient oscillations are speculative, we concentrate on pulsation mechanisms. We present initial considerations predicting the oscillation period to scale linearly with the white dwarf radius (and thus mass), weakly with the pressure at the base, and luminosity. Estimates of the size of the white dwarf could be useful for determining whether these systems are more massive than typical white dwarfs, and thus whether they are growing from accretion over time. Signs of such mass growth may have implications for whether some of these systems are attractive as Type Ia supernova progenitors. C1 [Ness, J-U; Kuulkers, E.; Henze, M.; Kretschmar, P.] ESAC, ESA, Sci Operat Dept, Sci Operat Div, Villanueva De La Canada, Madrid, Spain. [Beardmore, A. P.; Osborne, J. P.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Piro, A. L.] CALTECH, Theoret Astrophys, Pasadena, CA 91125 USA. [Piro, A. L.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dobrotka, A.] Slovak Univ Technol Bratislava, Adv Technol Res Inst, Trnava 91724, Slovakia. [Schwarz, G.] Amer Astron Soc, Washington, DC 20009 USA. [Starrfield, S.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Hirsch, M.; Wilms, J.] Remeis Sternwarte, D-96049 Bamberg, Germany. [Hirsch, M.; Wilms, J.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. RP Ness, JU (reprint author), ESAC, ESA, Sci Operat Dept, Sci Operat Div, Villanueva De La Canada, Madrid, Spain. EM juness@sciops.esa.int RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Kretschmar, Peter/0000-0001-9840-2048; Henze, Martin/0000-0001-9985-3406 FU UK Space Agency; ESA; NSF [AST-1205732, PHY-1151197, PHY-1404569]; Sherman Fairchild Foundation; Slovak grant VEGA [1/0511/13]; NSF; NASA FX A. P. Beardmore and J. P. Osborne acknowledge support from the UK Space Agency. M. H. acknowledges support from an ESA fellowship. A. L. Piro is supported through NSF grants AST-1205732, PHY-1151197, PHY-1404569, and the Sherman Fairchild Foundation. A. Dobrotka was supported by the Slovak grant VEGA 1/0511/13. S. Starrfield gratefully acknowledges partial support from NSF and NASA grants to ASU. NR 60 TC 3 Z9 3 U1 0 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 JUN PY 2015 VL 578 AR A39 DI 10.1051/0004-6361/201425178 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CM2IF UT WOS:000357502600051 ER PT J AU Feitosa, RM Lattke, JE Schultz, TR AF Feitosa, Rodrigo M. Lattke, John E. Schultz, Ted R. TI Special Issue on Taxonomy, morphology, and phylogeny of ants SO SOCIOBIOLOGY LA English DT Editorial Material C1 [Feitosa, Rodrigo M.] Univ Fed Parana, BR-80060000 Curitiba, Parana, Brazil. [Lattke, John E.] Univ Nacl Loja, Loja, Ecuador. [Schultz, Ted R.] Smithsonian Inst, Washington, DC 20560 USA. RP Feitosa, RM (reprint author), Univ Fed Parana, BR-80060000 Curitiba, Parana, Brazil. RI Lattke, John/K-2934-2015 OI Lattke, John/0000-0002-6793-3003 NR 0 TC 0 Z9 0 U1 2 U2 4 PU UNIV ESTADUAL FEIRA SANTANA PI FEIRA DE SANTANA PA AV TRANSORDESTINA S N NOVO HORIZONTE, FEIRA DE SANTANA, BAHAI CEP44036-900, BRAZIL SN 0361-6525 J9 SOCIOBIOLOGY JI Sociobiology PD JUN PY 2015 VL 62 IS 2 BP 131 EP 131 PG 1 WC Entomology SC Entomology GA CM4RW UT WOS:000357673400001 ER PT J AU LaPolla, JS Greenwalt, DE AF LaPolla, J. S. Greenwalt, D. E. TI Fossil Ants (Hymenoptera: Formicidae) of the Middle Eocene Kishenehn Formation SO SOCIOBIOLOGY LA English DT Article DE Cenozoic; Coal Creek Member; Extinct; Crematogaster; Montana AB A broad range of interesting fossil insects have been discovered recently in Kishenehn Formation shale (middle Eocene, ca. 46 myo) in northwestern Montana, among them a diversity of ant species. Two hundred forty-nine ant fossils were examined in this study, with 152 them assignable at least to subfamily. Here, twelve fossil ant species are formally described. These include a new genus of Dolichoderinae (Ktunaxia, gen. nov.), and the oldest known species from two extant genera: Crematogaster (C. aurora, sp. nov.) and Pseudomyrmex (P. saxulum, sp. nov.). The Eocene is of particular interest for understanding ant evolution because it is during this period that many present-day speciose and ecologically dominant clades of ants apparently emerged. In order to understand the evolution of ants, and in particular their march to the terrestrial dominance observed in modern times, it is critical to understand the tempo of ant diversity during the Eocene. The Kishenehn provides another window into Eocene ant diversity; its relevance to some of the other major Eocene ant fossil deposits is discussed. C1 [LaPolla, J. S.] Towson Univ, Towson, MD USA. [Greenwalt, D. E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP LaPolla, JS (reprint author), Towson Univ, Dept Biol Sci, 8000 York Rd, Towson, MD 21252 USA. EM jlapolla@towson.edu FU National Science Foundation [DEB-0743542]; Evolution of Terrestrial Ecosystems Consortium of the USNM [329] FX As ant rock fossils can be particularly difficult to interpret, we benefited from the thoughtful discussion and opinions of the following people: Bonnie Blaimer, Barry Bolton, Brendon Boudinot, Vincent Perrichot, Ted Schultz, Jeffrey Sosa-Calvo, James Trager, and Phil Ward. We would also like to thank Ted Schultz and two anonymous reviewers whose suggestions significantly improved the manuscript. Of course we remain solely responsible for any errors that inevitably remain. This study was supported in part by the National Science Foundation under grant DEB-0743542 to JSL. This is contribution number 329 of the Evolution of Terrestrial Ecosystems Consortium of the USNM. NR 25 TC 1 Z9 2 U1 0 U2 3 PU UNIV ESTADUAL FEIRA SANTANA PI FEIRA DE SANTANA PA AV TRANSORDESTINA S N NOVO HORIZONTE, FEIRA DE SANTANA, BAHAI CEP44036-900, BRAZIL SN 0361-6525 J9 SOCIOBIOLOGY JI Sociobiology PD JUN PY 2015 VL 62 IS 2 BP 163 EP 174 PG 12 WC Entomology SC Entomology GA CM4RW UT WOS:000357673400003 ER PT J AU Sosa-Calvo, J Jesovnik, A Okonski, E Schultz, TR AF Sosa-Calvo, J. Jesovnik, A. Okonski, E. Schultz, T. R. TI Locating, collecting, and maintaining colonies of fungus-farming ants (Hymenoptera: Formicidae: Myrmicinae: Attini) SO SOCIOBIOLOGY LA English DT Article DE Formicidae; Attini; fungus-farming ants; natural history; nest architecture; live culture ID ATTA-CEPHALOTES L; GROWING ANTS; NEST ARCHITECTURE; TRACHYMYRMEX-SEPTENTRIONALIS; EMERY HYMENOPTERA; NATURAL-HISTORY; GENUS; SYMBIOSIS; AGRICULTURE; BIOLOGY AB The purpose of this paper is to describe methods developed by generations of attinologists for locating, collecting, and maintaining in the laboratory live colonies of fungus-farming ants. Our goal is to accelerate the study of the poorly known and increasingly threatened non-leaf-cutting species of this fascinating and biologically important group because leaf-cutting ants have historically received the majority of scientific attention. We describe standardized measurement and data collection protocols in three sections: (i) locating fungus-farming ants in the field; (ii) collecting whole colonies of fungus-farming ants; and (iii) maintaining living colonies of fungus-farming ants in the laboratory. We provide lists of necessary equipment and materials, including information on where they can be acquired. C1 [Sosa-Calvo, J.; Jesovnik, A.; Okonski, E.; Schultz, T. R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Sosa-Calvo, J.; Jesovnik, A.] Univ Maryland, Dept Entomol, Maryland Ctr Systemat Entomol, College Pk, MD 20742 USA. [Sosa-Calvo, J.] Univ Rochester, Dept Biol, Rochester, NY 14627 USA. RP Sosa-Calvo, J (reprint author), Univ Rochester, Dept Biol, Rochester, NY 14627 USA. EM jsosacalvo@gmail.com FU Max and Vera Britton Environmental Science Award (Cosmos Club Foundation); Peter Buck Pre-doctoral Fellowships (NMNH-SI); Explorers Club Washington Group Exploration and Field Research Grant; Cosmos Scholar Award (Cosmos Club Foundation); Smithsonian National Museum of Natural History (NMNH) Small Grants Program award; Smithsonian Institution Competitive Grants Program for Science award; National Science Foundation grant [DEB 0949689] FX We are indebted to past and present attinologists, who made this work possible. This paper was supported, in part, by a Max and Vera Britton Environmental Science Award (Cosmos Club Foundation) to JSC; Peter Buck Pre-doctoral Fellowships (NMNH-SI) to JSC and AJ; an Explorers Club Washington Group Exploration and Field Research Grant and a Cosmos Scholar Award (Cosmos Club Foundation) to AJ; a Smithsonian National Museum of Natural History (NMNH) Small Grants Program award to TRS and JSC; a Smithsonian Institution Competitive Grants Program for Science award to TRS; and National Science Foundation grant DEB 0949689 to TRS. This manuscript was greatly improved thanks to comments from Michael Lloyd, Bonnie Blaimer, and three anonymous reviewers. NR 98 TC 0 Z9 0 U1 1 U2 9 PU UNIV ESTADUAL FEIRA SANTANA PI FEIRA DE SANTANA PA AV TRANSORDESTINA S N NOVO HORIZONTE, FEIRA DE SANTANA, BAHAI CEP44036-900, BRAZIL SN 0361-6525 J9 SOCIOBIOLOGY JI Sociobiology PD JUN PY 2015 VL 62 IS 2 BP 300 EP 320 PG 21 WC Entomology SC Entomology GA CM4RW UT WOS:000357673400016 ER PT J AU Balaguera-Reina, SA Venegas-Anaya, M Densmore, LD AF Balaguera-Reina, Sergio A. Venegas-Anaya, Miryam Densmore, Llewellyn D., III TI The Biology and Conservation Status of the American Crocodile in Colombia SO JOURNAL OF HERPETOLOGY LA English DT Article AB Along with the Orinoco and Cuban Crocodiles (Crocodylus intermedius and Crocodylus rhombifer), the American Crocodile (Crocodylus acutus) is among the most threatened crocodylian species in the Americas. Although this species is distributed widely, its IUCN "threat category" in several countries is "of concern." We review the literature dealing with the biology and conservation status of C. acutus in Colombia and assess its Extent of Occurrence (EoO) and its EoO-Habitat Status. We propose a way to estimate the effective area of optimal habitable occurrence on the basis of the EoO (EoO-Effective Habitable Area). We found that only 37% of the national territories have been sampled in ecological studies during the last decade. The relatively few reports of abundance values and the lack of long-term projects that can produce accurate estimates of population sizes make it difficult to establish the conservation status of this species in Colombia. Our analyses indicate that the EoO-Habitat Status has a higher proportion of disturbed landscapes, as well as agricultural areas, than natural forests and protected areas. We considered that EoO-Effective Habitable Area is a good parameter to estimate the amount of suitable habitat and status of optimal habitat because it does not overestimate the actual areas that crocodiles inhabit. Spatial information gaps, combined with the absence of knowledge about the population ecology and habitat reduction are indeed the principal threats to the American Crocodile in Colombia. C1 [Balaguera-Reina, Sergio A.; Venegas-Anaya, Miryam; Densmore, Llewellyn D., III] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. [Venegas-Anaya, Miryam] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Balaguera-Reina, SA (reprint author), Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. EM sergio.balaguera-reina@ttu.edu NR 39 TC 2 Z9 3 U1 8 U2 32 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 JUN PY 2015 VL 49 IS 2 BP 200 EP 206 DI 10.1670/13-065 PG 7 WC Zoology SC Zoology GA CM0IA UT WOS:000357360400006 ER PT J AU Breitburg, DL Salisbury, J Bernhard, JM Cai, WJ Dupont, S Doney, SC Kroeker, KJ Levin, LA Long, WC Milke, LM Miller, SH Phelan, B Passow, U Seibel, BA Todgham, AE Tarrant, AM AF Breitburg, Denise L. Salisbury, Joseph Bernhard, Joan M. Cai, Wei-Jun Dupont, Sam Doney, Scott C. Kroeker, Kristy J. Levin, Lisa A. Long, W. Christopher Milke, Lisa M. Miller, Seth H. Phelan, Beth Passow, Uta Seibel, Brad A. Todgham, Anne E. Tarrant, Ann M. TI And on Top of All That... Coping with Ocean Acidification in the Midst of Many Stressors SO OCEANOGRAPHY LA English DT Article ID PREDATOR-PREY INTERACTIONS; SEA-URCHIN LARVAE; CLIMATE-CHANGE; MULTIPLE STRESSORS; MARINE ECOSYSTEM; COASTAL WATERS; CORAL-REEFS; IMPACTS; OXYGEN; PH AB Oceanic and coastal waters are acidifying due to processes dominated in the open ocean by increasing atmospheric CO2 and dominated in estuaries and some coastal waters by nutrient-fueled respiration. The patterns and severity of acidification, as well as its effects, are modified by the host of stressors related to human activities that also influence these habitats. Temperature, deoxygenation, and changes in food webs are particularly important co-stressors because they are pervasive, and both their causes and effects are often mechanistically linked to acidification. Development of a theoretical underpinning to multiple stressor research that considers physiological, ecological, and evolutionary perspectives is needed because testing all combinations of stressors and stressor intensities experimentally is impossible. Nevertheless, use of a wide variety of research approaches is a logical and promising strategy for improving understanding of acidification and its effects. Future research that focuses on spatial and temporal patterns of stressor interactions and on identifying mechanisms by which multiple stressors affect individuals, populations, and ecosystems is critical. It is also necessary to incorporate consideration of multiple stressors into management, mitigation, and adaptation to acidification and to increase public and policy recognition of the importance of addressing acidification in the context of the suite of other stressors with which it potentially interacts. C1 [Breitburg, Denise L.; Miller, Seth H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Salisbury, Joseph] Univ New Hampshire, Ocean Proc Anal Lab, Durham, NH 03824 USA. [Bernhard, Joan M.] Woods Hole Oceanog Inst WHOI, Dept Geol & Geophys, Woods Hole, MA USA. [Cai, Wei-Jun] Univ Delaware, Sch Marine Sci & Policy, Newark, DE USA. [Dupont, Sam] Univ Gothenburg, Dept Biol & Environm Sci, Fiskebackski, Sweden. [Doney, Scott C.] WHOI, Marine Chem & Geochem Dept, Woods Hole, MA USA. [Kroeker, Kristy J.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Levin, Lisa A.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. [Long, W. Christopher] NOAA, NMFS, Kodiak, AK USA. [Milke, Lisa M.] NOAA, NMFS, Milford, CT USA. [Phelan, Beth] NOAA, NMFS, Highlands, NJ USA. [Passow, Uta] Univ Calif Santa Barbara, Inst Marine Sci, Santa Barbara, CA 93106 USA. [Seibel, Brad A.] Univ Rhode Isl, Dept Biol Sci, Kingston, RI 02881 USA. [Todgham, Anne E.] Univ Calif Davis, Dept Anim Sci, Davis, CA 95616 USA. [Tarrant, Ann M.] WHOI, Dept Biol, Woods Hole, MA USA. RP Breitburg, DL (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM breitburgd@si.edu RI Doney, Scott/F-9247-2010; Long, William/C-7074-2009; Cai, Wei-Jun/C-1361-2013 OI Doney, Scott/0000-0002-3683-2437; Long, William/0000-0002-7095-1245; Cai, Wei-Jun/0000-0003-3606-8325 FU NOAA-CSCOR [NA10NOS4780138]; NASA [NNX14AL8]; NSF [OCE-1219948, OCE-927445, OCE-1041062, EF-1041070, EF-0424599, OCE-1041038, EF-1316113, ANT-1142122, OCE-1316040]; NOAA Ocean Acidification Program Office; Swedish Research Council VR; Swedish Research Council Formas FX We would like to thank the organizers of the 2013 Ocean Acidification principal investigators meeting for bringing the authors together to focus on this important issue, and S.R. Cooley and the other editors of this volume for their help and support throughout the writing process. A. Maas provided data plotted in Figure 2a. DLB thanks K. Cottingham for sharing ideas on multiple stressors, and I. Fang and H. Soulen for collecting data plotted in Fig. 2b. Funding for research on acidification and multiple stressors was provided by NOAA-CSCOR NA10NOS4780138 to DLB, NASA NNX14AL8 to JS, NSF OCE-1219948 to JMB, NSF OCE-927445 and OCE-1041062 to LAL, NSF EF-1041070 to W-JC, a Linnaeus grant from the Swedish Research Councils VR and Formas to SD, NSF EF-0424599 to SCD, NSF OCE-1041038 to UP, NSF EF-1316113 to BAS, NSF ANT-1142122 to AET, NSF OCE-1316040 to AMT, and the NOAA Ocean Acidification Program Office to BP, LMM, and WCL. The findings and conclusions in the paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service, NOAA. NR 95 TC 28 Z9 28 U1 12 U2 124 PU OCEANOGRAPHY SOC PI ROCKVILLE PA P.O. BOX 1931, ROCKVILLE, MD USA SN 1042-8275 J9 OCEANOGRAPHY JI Oceanography PD JUN PY 2015 VL 28 IS 2 SI SI BP 48 EP 61 DI 10.5670/oceanog.2015.31 PG 14 WC Oceanography SC Oceanography GA CL8NP UT WOS:000357231700009 ER PT J AU Leavelle, KM Powell, LL Powell, GVN Forsyth, A AF Leavelle, Karen M. Powell, Luke L. Powell, George V. N. Forsyth, Adrian TI A Radio-telemetry Study of Home Range and Habitat Use of the Endangered Yellow-billed Cotinga (Carpodectes antoniae) in Costa Rica SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE Carpodectes antoniae; habitat use; home range; mangroves; migration; Yellow-billed Cotinga ID LOCATION; BIRDS AB The Yellow-billed Cotinga (Carpodectes antoniae) is one of Central America's rarest and most endangered species. A regional endemic to Panama and Costa Rica, between 250 and 999 individuals appear to now survive mainly within Pacific coastal mangroves and adjacent lowland forest within the Terraba-Sierpe National Wetlands and the Osa Peninsula of Costa Rica, an Alliance for Zero Extinction Site. We used radio telemetry to determine seasonal movements and habitat use and requirements of three Yellow-billed Cotingas at the Rincon River and mangrove estuary on the Osa Peninsula. During the breeding months from approximately December to June, radio-tagged cotingas used mangroves primarily for courtship display, insect feeding, protection from inclement weather, and night roosts. They used lowland forest for feeding on fruit and insects and for infrequent courtship display. Birds fed on fruits from 23 lowland forest tree species throughout the year. Although the female ranged farther than the males during the non-breeding season, no bird showed evidence of migratory behavior. They did not wander from the Rincon mangroves during the non-breeding months from July to November, and they roosted in the same mangrove plot each night. The juxtaposition of mangroves and lowland forest rich in fruit trees may be critical to the survival of the species. C1 [Leavelle, Karen M.; Forsyth, Adrian] Osa Conservat, Washington, DC 20005 USA. [Powell, Luke L.] Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. RP Leavelle, KM (reprint author), Osa Birds Res & Conservat, 873 Bright Star St, Thousand Oaks, CA 91360 USA. EM karenleavelle@osabirds.org FU American Bird Conservancy; Mohammed bin Zayed Species Conservation Fund; Wisconsin Natural Resources Foundation; Osa Conservation FX Funding and support for this project was provided by the American Bird Conservancy, the Mohammed bin Zayed Species Conservation Fund, the Wisconsin Natural Resources Foundation, and Osa Conservation. We would like to thank the reviewers of this manuscript and their valuable comments. We thank Daniel Lebbin and Andrew Rothman from the American Bird Conservancy for their support for this project, and to Elizabeth Jones and Abraham Gallo for their expertise and guidance. Thank you to Lic. Wendy Barrantes-Ramirez of MINAE for permitting and support, and Luis Vargas in assisting with capture and tagging. Thanks to field personnel Manuel Sanchez, Courtney Thomas, Christina Boldero and Kenneth Gonzalez, and to El Chontal and ADEPAS for lodging. We also thank Reinaldo Aguilar for plant identification, and Joni Ellis of Optics for the Tropics for all optics donations. NR 21 TC 0 Z9 0 U1 1 U2 20 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 JUN PY 2015 VL 127 IS 2 BP 302 EP 309 PG 8 WC Ornithology SC Zoology GA CM5KN UT WOS:000357726800016 ER PT J AU Lemaitre, R AF Lemaitre, Rafael TI A new species of the hermit crab genus Michelopagurus McLaughlin, 1997 (Crustacea: Decapoda: Paguridae) from Moorea, French Polynesia SO ZOOSYSTEMA LA English DT Article DE Crustacea; Decapoda Paguridae; Michelopagurus; hermit crab; Moorea; French Polynesia; new species AB A new species of the family Paguridae Latreille, 1802, Michelopagurus tangaloa n. sp., is described from deep waters (485-1145 m) off the coast of Moorea, French Polynesia, South Pacific. This new species is the fifth known in the genus Michelopagurus McLaughlin, 1997, and the third from the Indo-West Pacific; the other two species are distributed in the Atlantic Ocean. All five species are rarely collected and most are known from a few type specimens. The new species most closely resembles its Indonesian congener M. chacei McLaughlin, 1997 but can be differentiated by having an acutely triangular rostrum terminating in a small spine, instead of the broadly rounded, terminally unarmed rostrum in M. chacei. Other subtle differences are: corneas reduced, not dilated or wider than distal width of peduncle in M. tangaloa n. sp., whereas corneas are weakly dilated and wider than distal width of peduncle in M. chacei; right cheliped dorsal surface of palm lacking spines, and carpi at most with weak dorsomesial distal row of small blunt spines in M. tangaloa n. sp., whereas the dorsal surface of the palm has a row of distinct spines, and carpus with dorsolateral and dorsomesial rows of distinct spines in M. chacei. A key to assist in the identification of all species of the genus is provided. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM lemaitrr@si.edu NR 12 TC 0 Z9 0 U1 0 U2 3 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 JUN PY 2015 VL 37 IS 2 BP 363 EP 370 DI 10.5252/z2015n2a5 PG 8 WC Zoology SC Zoology GA CM1EE UT WOS:000357422700005 ER PT J AU Bridges, NT Spagnuolo, MG de Silva, SL Zimbelman, JR Neely, EM AF Bridges, N. T. Spagnuolo, M. G. de Silva, S. L. Zimbelman, J. R. Neely, E. M. TI Formation of gravel-mantled megaripples on Earth and Mars: Insights from the Argentinean Puna and wind tunnel experiments SO AEOLIAN RESEARCH LA English DT Article DE Ripples; Megaripples; Puna; Mars; Wind tunnel; Threshold ID TRANSVERSE AEOLIAN RIDGES; SALTATION THRESHOLD; MERIDIANI-PLANUM; RIPPLES; MODEL AB Pumice and lithic clasts from gravel-mantled megaripples in the Argentinean Puna, an analog to Martian large ripples and Transverse Aeolian Ridges (TARs), were put in a boundary layer wind tunnel to derive threshold speeds for various stages of motion of the component clasts and observe incipient bedform development. Combined with results from a field meteorological station, it is found that the gravel components can initially only move under gusty conditions, with the impact of saltating pumice and sand lowering threshold. Pumices can saltate without the impact of sand, implying that they are both an impelling force for other pumices and lithics, and are the most likely clast constituent to undergo transport. Accumulation into bedforms in the tunnel occurs when clasts self organize, with larger, more immobile particles holding others in place, a process that is accentuated in the field on local topographic highs of the undulating ignimbrite bedrock surface. In such an arrangement, pumices and especially lithics remain largely stable, with vibration the dominant mode of motion. This results in sand and silt entrapment and growth of the bedform through infiltration and uplift of the gravel. Resulting bedforms are gravel-mantled ripple-like forms cored with fine grained sediment. The Martian aeolian environment is similar to the Puna in terms of having grains of variable size, infrequent wind gusts, and saltating sand, implying that some TARs on the planet may have formed in a similar way. (C) 2015 Elsevier B.V. All rights reserved. C1 [Bridges, N. T.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Spagnuolo, M. G.; de Silva, S. L.; Neely, E. M.] Oregon State Univ, Corvallis, OR 97331 USA. [Zimbelman, J. R.] Smithsonian Inst, CEPS NASM, Washington, DC 20013 USA. [Neely, E. M.] Portland State Univ, Dept Geol, Portland, OR 97201 USA. RP Bridges, NT (reprint author), UBA CONICET Ciudad Bs, IDEAN, As, Argentina. RI Bridges, Nathan/D-6341-2016; de Silva, Shanaka/A-4630-2011 OI de Silva, Shanaka/0000-0002-0310-5516 FU NASA's Mars Fundamental Research Program [NNX10AP79G] FX We are indebted to several individuals whose assistance made this project possible. D. Ball, C. Bradbury and A. Zink assisted in the setup, running, and documentation of the wind tunnel experiments. Discussions with R. Sullivan on the wind tunnel and fieldwork were illuminating. Support for this project was provided by grant NNX10AP79G (Principal Investigator de Silva) from NASA's Mars Fundamental Research Program. NR 36 TC 4 Z9 4 U1 2 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1875-9637 EI 2212-1684 J9 AEOLIAN RES JI Aeolian Res. PD JUN PY 2015 VL 17 BP 49 EP 60 DI 10.1016/j.aeolia.2015.01.007 PG 12 WC Geography, Physical SC Physical Geography GA CL7IW UT WOS:000357146700004 ER PT J AU Ashby, MLN Willner, SP Fazio, GG Dunlop, JS Egami, E Faber, SM Ferguson, HC Grogin, NA Hora, JL Huang, JS Koekemoer, AM Labbe, I Wang, Z AF Ashby, M. L. N. Willner, S. P. Fazio, G. G. Dunlop, J. S. Egami, E. Faber, S. M. Ferguson, H. C. Grogin, N. A. Hora, J. L. Huang, J-S. Koekemoer, A. M. Labbe, I. Wang, Z. TI S-CANDELS: THE SPITZER-COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC SURVEY. SURVEY DESIGN, PHOTOMETRY, AND DEEP IRAC SOURCE COUNTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: high-redshift; infrared: galaxies; surveys ID EXTENDED GROTH STRIP; SPACE-TELESCOPE OBSERVATIONS; LYMAN-BREAK GALAXIES; STAR-FORMATION RATES; ARRAY CAMERA IRAC; GOODS-SOUTH FIELD; LEGACY SURVEY; LUMINOSITY FUNCTIONS; CLUSTERING PROPERTIES; EVOLUTION SURVEY AB The Spitzer-Cosmic Assembly Deep Near-infrared Extragalactic Legacy Survey (S-CANDELS; PI G. Fazio) is a Cycle 8 Exploration Program designed to detect galaxies at very high redshifts (z > 5). To mitigate the effects of cosmic variance and also to take advantage of deep coextensive coverage in multiple bands by the Hubble Space Telescope (HST) Multi-cycle Treasury Program CANDELS, S-CANDELS was carried out within five widely separated extragalactic fields: the UKIDSS Ultra-deep Survey, the Extended Chandra Deep Field South, COSMOS, the HST Deep Field North, and the Extended Groth Strip. S-CANDELS builds upon the existing coverage of these fields from the Spitzer Extended Deep Survey (SEDS), a Cycle 6 Exploration Program, by increasing the integration time from SEDS' 12 hr to a total of 50 hr but within a smaller area, 0.16 deg(2). The additional depth significantly increases the survey completeness at faint magnitudes. This paper describes the S-CANDELS survey design, processing, and publicly available data products. We present Infrared Array Camera (IRAC) dual-band 3.6 + 4.5 mu m catalogs reaching to a depth of 26.5 AB mag. Deep IRAC counts for the roughly 135,000 galaxies detected by S-CANDELS are consistent with models based on known galaxy populations. The increase in depth beyond earlier Spitzer/IRAC surveys does not reveal a significant additional contribution from discrete sources to the diffuse Cosmic Infrared Background (CIB). Thus it remains true that only roughly half of the estimated CIB flux from COBE/DIRBE is resolved. C1 [Ashby, M. L. N.; Willner, S. P.; Fazio, G. G.; Hora, J. L.; Huang, J-S.; Wang, Z.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunlop, J. S.] Univ Edinburgh, Royal Observ, Scottish Univ Phys Alliance, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Egami, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Faber, S. M.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Faber, S. M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ferguson, H. C.; Grogin, N. A.; Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Labbe, I.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Ashby, MLN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mashby@cfa.harvard.edu OI Koekemoer, Anton/0000-0002-6610-2048 FU National Aeronautics and Space Administration (NASA); NASA by JPL/Caltech [1439337, 1439801]; HST [GO-12060.05-A]; European Research Council; Royal Society FX The authors are grateful to E. Diolaiti for helpful advice on the optimal use of StarFinder. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through contract numbers 1439337 and 1439801 issued by JPL/Caltech, and by HST grant GO-12060.05-A. J. S. D. acknowledges the support of the European Research Council via an Advanced Grant, and the support of the Royal Society via a Wolfson Research Merit Award. 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. NR 75 TC 22 Z9 22 U1 1 U2 1 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 JUN PY 2015 VL 218 IS 2 AR 33 DI 10.1088/0067-0049/218/2/33 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7AO UT WOS:000357122200019 ER PT J AU Kriek, M Shapley, AE Reddy, NA Siana, B Coil, AL Mobasher, B Freeman, WR de Groot, L Price, SH Sanders, R Shivaei, I Brammer, GB Momcheva, IG Skelton, RE van Dokkum, PG Whitaker, KE Aird, J Azadi, M Kassis, M Bullock, JS Conroy, C Dave, R Keres, D Krumholz, M AF Kriek, Mariska Shapley, Alice E. Reddy, Naveen A. Siana, Brian Coil, Alison L. Mobasher, Bahram Freeman, William R. de Groot, Laura Price, Sedona H. Sanders, Ryan Shivaei, Irene Brammer, Gabriel B. Momcheva, Ivelina G. Skelton, Rosalind E. van Dokkum, Pieter G. Whitaker, Katherine E. Aird, James Azadi, Mojegan Kassis, Marc Bullock, James S. Conroy, Charlie Dave, Romeel Keres, Dusan Krumholz, Mark TI THE MOSFIRE DEEP EVOLUTION FIELD (MOSDEF) SURVEY: REST-FRAME OPTICAL SPECTROSCOPY FOR similar to 1500 H-SELECTED GALAXIES AT 1.37 <= z <= 3.8 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: high-redshift; surveys ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC LEGACY SURVEY; MASS-METALLICITY RELATION; POST-STARBURST GALAXIES; HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; MEDIUM-BAND SURVEY; QUIESCENT GALAXIES AB In this paper we present the MOSFIRE Deep Evolution Field (MOSDEF) survey. The MOSDEF survey aims to obtain moderate-resolution (R = 3000-3650) rest-frame optical spectra (similar to 3700-7000 angstrom) for similar to 1500 galaxies at 1.37 <= z <= 3.80 in three well-studied CANDELS fields: AEGIS, COSMOS, and GOODS-N. Targets are selected in three redshift intervals: 1.37 <= z <= 1.70, 2.09 <= z <= 2.61, and 2.95 <= z <= 3.80, down to fixed H-AB (F160W) magnitudes of 24.0, 24.5, and 25.0, respectively, using the photometric and spectroscopic catalogs from the 3D-HST survey. We target both strong nebular emission lines (e.g., [O II] lambda lambda 3727, 3730, H beta, [O III] lambda lambda 4960, 5008, Ha, [N II] lambda lambda 6550, 6585, and [S II] lambda lambda 6718, 6733) and stellar continuum and absorption features (e.g., Balmer lines, Ca-II H and K, Mgb, 4000 angstrom break). Here we present an overview of our survey, the observational strategy, the data reduction and analysis, and the sample characteristics based on spectra obtained during the first 24 nights. To date, we have completed 21 masks, obtaining spectra for 591 galaxies. For similar to 80% of the targets we derive a robust redshift from either emission or absorption lines. In addition, we confirm 55 additional galaxies, which were serendipitously detected. The MOSDEF galaxy sample includes unobscured star-forming, dusty star-forming, and quiescent galaxies and spans a wide range in stellar mass (similar to 10(9)-10(11.5) M-circle dot) and star formation rate (similar to 10(0)-10(3) M-circle dot yr(-1)). The spectroscopically confirmed sample is roughly representative of an H-band limited galaxy sample at these redshifts. With its large sample size, broad diversity in galaxy properties, and wealth of available ancillary data, MOSDEF will transform our understanding of the stellar, gaseous, metal, dust, and black hole content of galaxies during the time when the universe was most active. C1 [Kriek, Mariska; Price, Sedona H.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Shapley, Alice E.; Sanders, Ryan] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Reddy, Naveen A.; Siana, Brian; Mobasher, Bahram; Freeman, William R.; de Groot, Laura; Shivaei, Irene] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Coil, Alison L.; Keres, Dusan] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Brammer, Gabriel B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Momcheva, Ivelina G.; van Dokkum, Pieter G.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Skelton, Rosalind E.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Whitaker, Katherine E.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Aird, James] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Kassis, Marc] WM Keck Observ, Kamuela, HI 96743 USA. [Bullock, James S.] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Conroy, Charlie; Krumholz, Mark] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Dave, Romeel] Univ Western Cape, ZA-7535 Cape Town, South Africa. RP Kriek, M (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Bullock, James/K-1928-2015; Skelton, Rosalind/S-1845-2016 OI Bullock, James/0000-0003-4298-5082; Skelton, Rosalind/0000-0001-7393-3336 FU NSF AAG [AST-1312780, 1312547, 1312764, 1313171]; NASA through the Space Telescope Science Institute [AR-13907]; Committee Faculty Research Grant; Hellmann Fellowship; Alfred P. Sloan Research Fellowship; NSF CAREER [AST-1055081]; W.M. Keck Foundation; NASA/ESA Hubble Space Telescope [12177, 12328, 12060-12064, 12440-12445, 13056]; NASA [NAS 5-26555] FX We thank the MOSFIRE instrument team for building this powerful instrument and for taking data for us during their commissioning runs. M. Kriek acknowledges valuable discussions with N. Konidaris about the reduction of MOSFIRE data and with M. Franx regarding the noise properties of the data. We thank the referee for a constructive report. This work would not have been possible without the 3D-HST collaboration, who provided to us the spectroscopic and photometric catalogs used to select our targets and to derive stellar population parameters. We are grateful to I. McLean, K. Kulas, and G. Mace for taking observations for us in 2013 May and June. We acknowledge support from an NSF AAG collaborative grant AST-1312780, 1312547, 1312764, and 1313171, and archival grant AR-13907, provided by NASA through a grant from the Space Telescope Science Institute. M. Kriek acknowledges support from a Committee Faculty Research Grant and a Hellmann Fellowship. N.A.R. is supported by an Alfred P. Sloan Research Fellowship. A.L.C. acknowledges funding from NSF CAREER grant AST-1055081. The data presented in this paper 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. This work is also based on observations made with the NASA/ESA Hubble Space Telescope (programs 12177, 12328, 12060-12064, 12440-12445, 13056), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 97 TC 45 Z9 45 U1 1 U2 4 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 JUN PY 2015 VL 218 IS 2 AR 15 DI 10.1088/00647-0049/218/2/15 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7AO UT WOS:000357122200001 ER PT J AU Swift, JJ Montet, BT Vanderburg, A Morton, T Muirhead, PS Johnson, JA AF Swift, Jonathan J. Montet, Benjamin T. Vanderburg, Andrew Morton, Timothy Muirhead, Philip S. Johnson, John Asher TI CHARACTERIZING THE COOL KOIs. VIII. PARAMETERS OF THE PLANETS ORBITING KEPLER'S COOLEST DWARFS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE methods: statistical; planets and satellites: general; stars: late-type; stars: low-mass ID TRANSIT TIMING OBSERVATIONS; FINITE INTEGRATION TIME; K-BAND SPECTRA; 1ST 4 MONTHS; LIGHT CURVES; SOLAR NEIGHBORHOOD; LOW-MASS; ERROR-CORRECTION; NEARBY STARS; SUPER-EARTHS AB The coolest dwarf stars targeted by the Kepler Mission constitute a relatively small but scientifically valuable subset of the Kepler target stars, and provide a high-fidelity, nearby sample of transiting planetary systems. Using archival Kepler data spanning the entire primary mission, we perform a uniform analysis to extract, confirm, and characterize the transit signals discovered by the Kepler pipeline toward M-type dwarf stars. We recover all but two of the signals reported in a recent listing from the Exoplanet Archive resulting in 163 planet candidates associated with a sample of 104 low-mass stars. We fitted the observed light curves to transit models using a Markov Chain Monte Carlo method and we have made the posterior samples publicly available to facilitate further studies. We fitted empirical transit times to individual transit signals with significantly non-linear ephemerides for accurate recovery of transit parameters and precise measuring of transit timing variations. We also provide the physical parameters for the stellar sample, including new measurements of stellar rotation, allowing the conversion of transit parameters into planet radii and orbital parameters. C1 [Swift, Jonathan J.; Montet, Benjamin T.] CALTECH, Pasadena, CA 91125 USA. [Montet, Benjamin T.; Vanderburg, Andrew; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Morton, Timothy] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Muirhead, Philip S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. RP Swift, JJ (reprint author), CALTECH, 1200 East Calif Blvd, Pasadena, CA 91125 USA. RI Muirhead, Philip/H-2273-2014 OI Muirhead, Philip/0000-0002-0638-8822 FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate; National Science Foundation [DGE 1144152, DGE 1144469] FX J.J.S. would like to thank Jason Eastman, David Kipping, Ellen Price, and Natalie Batalha for their helpful input regarding various aspects of this work. All of the data presented in this paper were obtained from the 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. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. A.V. and B.T.M. are supported by the National Science Foundation Graduate Research Fellowship, grant No. DGE 1144152 and DGE 1144469, respectively. NR 84 TC 8 Z9 8 U1 0 U2 0 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 JUN PY 2015 VL 218 IS 2 AR 26 DI 10.1088/0067-0049/218/2/26 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL7AO UT WOS:000357122200012 ER PT J AU Blakeslee, AMH Keogh, CL Fowler, AE Griffen, BD AF Blakeslee, April M. H. Keogh, Carolyn L. Fowler, Amy E. Griffen, Blaine D. TI Assessing the Effects of Trematode Infection on Invasive Green Crabs in Eastern North America SO PLOS ONE LA English DT Article ID MICROPHALLUS-SIMILIS JAGERSKIOLD; HETEROSACCUS-DOLLFUSI BOSCHMA; CHARYBDIS-LONGICOLLIS LEENE; ENEMY RELEASE HYPOTHESIS; CARCINUS-MAENAS L.; SHORE CRAB; PREY SELECTION; HEMIGRAPSUS-SANGUINEUS; METACERCARIAE DIGENEA; TROPHIC TRANSMISSION AB A common signature of marine invasions worldwide is a significant loss of parasites (= parasite escape) in non-native host populations, which may confer a release from some of the harmful effects of parasitism (e.g., castration, energy extraction, immune activation, behavioral manipulation) and possibly enhance the success of non-indigenous species. In eastern North America, the notorious invader Carcinus maenas (European green crab) has escaped more than two-thirds its native parasite load. However, one of its parasites, a trematode (Microphallus similis), can be highly prevalent in the non-native region; yet little is known about its potential impacts. We employed a series of laboratory experiments to determine whether and how M. similis infection intensity influences C. maenas, focusing on physiological assays of body mass index, energy storage, and immune activation, as well as behavioral analyses of foraging, shelter utilization, and conspicuousness. We found little evidence for enduring physiological or behavioral impacts four weeks after experimental infection, with the exception of mussel handling time which positively correlated with cyst intensity. However, we did find evidence for a short-term effect of M. similis infection during early stages of infection (soon after cercarial penetration) via a significant drop in circulating immune cells, and a significant increase in the crabs' righting response time. Considering M. similis is the only common parasite infecting C. maenas in eastern North America, our results for minimal lasting effects of the trematode on the crab's physiology and behavior may help explain the crab's continued prominence as a strong predator and competitor in the region. C1 [Blakeslee, April M. H.] Long Isl Univ, Brookville, NY 11548 USA. [Blakeslee, April M. H.; Fowler, Amy E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Keogh, Carolyn L.] Univ Georgia, Athens, GA 30602 USA. [Fowler, Amy E.] Marine Resources Res Inst, South Carolina Dept Nat Resources, Charleston, SC 29422 USA. [Griffen, Blaine D.] Univ S Carolina, Dept Biol Sci, Columbia, SC 29208 USA. [Griffen, Blaine D.] Univ S Carolina, Marine Sci Program, Columbia, SC 29208 USA. RP Blakeslee, AMH (reprint author), Long Isl Univ, 720 Northern Blvd, Brookville, NY 11548 USA. EM april.blakeslee@liu.edu FU Research Opportunity Award; National Science Foundation award (NSF) [OCE-1129166] FX This work was supported by a Research Opportunity Award to AMHB and BDG as a supplemental to BDG's National Science Foundation award (NSF #OCE-1129166). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 93 TC 1 Z9 1 U1 5 U2 36 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 JUN 1 PY 2015 VL 10 IS 6 AR e0128674 DI 10.1371/journal.pone.0128674 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA CL0KF UT WOS:000356630900182 PM 26030816 ER PT J AU Broderick, AE Narayan, R Kormendy, J Perlman, ES Rieke, MJ Doeleman, SS AF Broderick, Avery E. Narayan, Ramesh Kormendy, John Perlman, Eric S. Rieke, Marcia J. Doeleman, Sheperd S. TI THE EVENT HORIZON OF M87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: individual (M87); gravitation; radio continuum: galaxies; infrared: galaxies; ultraviolet: galaxies ID SUPERMASSIVE BLACK-HOLE; HUBBLE-SPACE-TELESCOPE; ADVECTION-DOMINATED ACCRETION; SAGITTARIUS A-ASTERISK; ACTIVE GALACTIC NUCLEI; RADIO GALAXIES; MAGNETOHYDRODYNAMIC SIMULATIONS; ELECTROMAGNETIC EXTRACTION; GASEOUS ATMOSPHERE; RELATIVISTIC JETS AB The 6 x 10(9) M-circle dot supermassive black hole at the center of the giant elliptical galaxy M87 powers a relativistic jet. Observations at millimeter wavelengths with the Event Horizon Telescope have localized the emission from the base of this jet to angular scales comparable to the putative black hole horizon. The jet might be powered directly by an accretion disk or by electromagnetic extraction of the rotational energy of the black hole. However, even the latter mechanism requires a confining thick accretion disk to maintain the required magnetic flux near the black hole. Therefore, regardless of the jet mechanism, the observed jet power in M87 implies a certain minimum mass accretion rate. If the central compact object in M87 were not a black hole but had a surface, this accretion would result in considerable thermal near-infrared and optical emission from the surface. Current flux limits on the nucleus of M87 strongly constrain any such surface emission. This rules out the presence of a surface and thereby provides indirect evidence for an event horizon. C1 [Broderick, Avery E.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Broderick, Avery E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Narayan, Ramesh; Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kormendy, John] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kormendy, John] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kormendy, John] Univ Sternwarte, D-81679 Munich, Germany. [Perlman, Eric S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Rieke, Marcia J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Doeleman, Sheperd S.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Broderick, AE (reprint author), Perimeter Inst Theoret Phys, 31 Caroline St North, Waterloo, ON N2L 2Y5, Canada. EM kormendy@astro.as.utexas.edu; eperlman@fit.edu OI Perlman, Eric/0000-0002-3099-1664 FU US National Science Foundation; Gordon and Betty Moore Foundation [GBMF3561]; NASA [NAS 5-26555, NNX14AB47G]; Perimeter Institute for Theoretical Physics; Natural Sciences and Engineering Research Council of Canada; NSF [AST1312651]; University of Texas; Max-Planck-Institut fur Extraterrestrsiche Physik (MPE), Garching-by-Munich, Germany FX Based on observations made with the Event Horizon Telescope and the NASA/ESA Hubble Space Telescope. The Event Horizon Telescope is supported through grants from the US National Science Foundation, by the Gordon and Betty Moore Foundation (GBMF3561), and through generous equipment donations from the Xilinx Corporation and the HGST company. The NASA/ESA Hubble Space Telescope observations were obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555. These observations are associated with program numbers 1105, 1228, 1517, 3242, 6775, 7171, 8140, 9454, 9493, 9705, 9829, 10133, 10617, 10910, and 11216. A. E.B. receives financial support from Perimeter Institute for Theoretical Physics and the Natural Sciences and Engineering Research Council of Canada through a Discovery Grant. R.N. received partial supported from the NSF via grant AST1312651 and NASA via grant NNX14AB47G. R.N. also thanks the Perimeter Institute for hospitality while some of this work was carried out. The authors are grateful to Sera Markoff and Brian McNamara for helpful conversations. This work would not have been practical without extensive use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory and the California Institute of Technology under contract with NASA. We also made extensive use of NASA's Astrophysics Data System bibliographic services. J.K.'s work was supported in Texas by the Curtis T. Vaughan, Jr. Centennial Chair in Astronomy and in Germany by a Faculty Research Assignment from the University of Texas and by the Max-Planck-Institut fur Extraterrestrsiche Physik (MPE), Garching-by-Munich, Germany. J.K. warmly thanks Director Ralf Bender and the staffs of the MPE and the Universitats-Sternwarte, Ludwig-Maximilians-Universitat, Munich for their hospitality and support during the 2014 visit when most of his work on this paper was done. NR 79 TC 10 Z9 10 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 179 DI 10.1088/004-637X/805/2/179 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400094 ER PT J AU Burkhart, B Lazarian, A Balsara, D Meyer, C Cho, J AF Burkhart, Blakesley Lazarian, A. Balsara, D. Meyer, C. Cho, J. TI ALFVENIC TURBULENCE BEYOND THE AMBIPOLAR DIFFUSION SCALE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); turbulence; waves ID COMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCE; ANISOTROPIC THERMAL CONDUCTION; MOLECULAR ION SPECTRA; MAGNETIC-FIELD; INTERSTELLAR-MEDIUM; STAR-FORMATION; ISOTHERMAL MAGNETOHYDRODYNAMICS; VELOCITY ANISOTROPY; SUPERNOVA-REMNANTS; RIEMANN SOLVER AB We investigate the nature of the Alfvenic turbulence cascade in two-fluid magnetohydrodynamic (MHD) simulations in order to determine if turbulence is damped once the ion and neutral species become decoupled at a critical scale called the ambipolar diffusion scale (L-AD). Using mode decomposition to separate the three classical MHD modes, we study the second-order structure functions of the Alfven mode velocity field of both neutrals and ions in the reference frame of the local magnetic field. On scales greater than L-AD we confirm that two-fluid turbulence strongly resembles single-fluid MHD turbulence. Our simulations show that the behavior of two-fluid turbulence becomes more complex on scales less than L-AD. We find that Alfvenic turbulence can exist past L-AD when the turbulence is globally super-Alfvenic, with the ions and neutrals forming separate cascades once decoupling has taken place. When turbulence is globally sub-Alfvenic and hence strongly anisotropic, with a large separation between the parallel and perpendicular decoupling scales, turbulence is damped at L-AD. We also find that the power spectrum of the kinetic energy in the damped regime is consistent with a k(-4) scaling (in agreement with the predictions of Lazarian et al.). C1 [Burkhart, Blakesley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burkhart, Blakesley; Lazarian, A.] Univ Wisconsin, Dept Astron, Madison, WI 53711 USA. [Balsara, D.; Meyer, C.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Cho, J.] Chungnam Natl Univ, Dept Astron & Space Sci, Taejon, South Korea. RP Burkhart, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA Einstein Fellowship; Center for Magnetic Self-Organization in Astrophysical and Laboratory Plasmas; Physics Graduate Program/UFRN, at Natal; NSF [AST 1212096, NSF-AST-1009091, NSF-ACI-1307369, NSF-DMS-1361197]; NASA grants from the Fermi program; NASA-NNX [12A088G]; National R & D Program through the National Research Foundation of Korea (NRF) - Ministry of Education [2011-0012081] FX B.B. acknowledges support from the NASA Einstein Fellowship. A.L. and B.B. thank the Center for Magnetic Self-Organization in Astrophysical and Laboratory Plasmas for financial support and acknowledge financial support from the Physics Graduate Program/UFRN, at Natal, for hospitality. A. L. is supported by the NSF grant AST 1212096. D.S.B. acknowledges support via NSF grants NSF-AST-1009091, NSF-ACI-1307369, and NSF-DMS-1361197. D.S.B. also acknowledges support via NASA grants from the Fermi program as well as NASA-NNX 12A088G. Several simulations were performed on a cluster at UND that is run by the Center for Research Computing. Computer support for NSF's XSEDE computing resources is also acknowledged. J.C.'s work is supported by the National R & D Program through the National Research Foundation of Korea (NRF), funded by the Ministry of Education (No. 2011-0012081) NR 61 TC 6 Z9 6 U1 1 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 JUN 1 PY 2015 VL 805 IS 2 AR 118 DI 10.1088/0004-637X/805/2/118 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400033 ER PT J AU Chakraborti, S Soderberg, A Chomiuk, L Kamble, A Yadav, N Ray, A Hurley, K Margutti, R Milisavljevic, D Bietenholz, M Brunthaler, A Pignata, G Pian, E Mazzali, P Fransson, C Bartel, N Hamuy, M Levesque, E MacFadyen, A Dittmann, J Krauss, M Briggs, MS Connaughton, V Yamaoka, K Takahashi, T Ohno, M Fukazawa, Y Tashiro, M Terada, Y Murakami, T Goldsten, J Barthelmy, S Gehrels, N Cummings, J Krimm, H Palmer, D Golenetskii, S Aptekar, R Frederiks, D Svinkin, D Cline, T Mitrofanov, IG Golovin, D Litvak, ML Sanin, AB Boynton, W Fellows, C Harshman, K Enos, H von Kienlin, A Rau, A Zhang, X Savchenko, V AF Chakraborti, Sayan Soderberg, Alicia Chomiuk, Laura Kamble, Atish Yadav, Naveen Ray, Alak Hurley, Kevin Margutti, Raffaella Milisavljevic, Dan Bietenholz, Michael Brunthaler, Andreas Pignata, Giuliano Pian, Elena Mazzali, Paolo Fransson, Claes Bartel, Norbert Hamuy, Mario Levesque, Emily MacFadyen, Andrew Dittmann, Jason Krauss, Miriam Briggs, M. S. Connaughton, V. Yamaoka, K. Takahashi, T. Ohno, M. Fukazawa, Y. Tashiro, M. Terada, Y. Murakami, T. Goldsten, J. Barthelmy, S. Gehrels, N. Cummings, J. Krimm, H. Palmer, D. Golenetskii, S. Aptekar, R. Frederiks, D. Svinkin, D. Cline, T. Mitrofanov, I. G. Golovin, D. Litvak, M. L. Sanin, A. B. Boynton, W. Fellows, C. Harshman, K. Enos, H. von Kienlin, A. Rau, A. Zhang, X. Savchenko, V. TI A MISSING-LINK IN THE SUPERNOVA-GRB CONNECTION: THE CASE OF SN 2012ap SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; radiation mechanisms: non-thermal; shock waves; supernovae: individual (SN 2012ap); techniques: interferometric ID GAMMA-RAY BURSTS; RELATIVISTIC BLAST WAVES; 25 APRIL 1998; EMISSION; MODEL; SYNCHROTRON AB Gamma-ray bursts (GRBs) are characterized by ultra-relativistic outflows, while supernovae are generally characterized by non-relativistic ejecta. GRB afterglows decelerate rapidly, usually within days, because their low-mass ejecta rapidly sweep up a comparatively larger mass of circumstellar material. However, supernovae with heavy ejecta can be in nearly free expansion for centuries. Supernovae were thought to have non-relativistic outflows except for a few relativistic ones accompanied by GRBs. This clear division was blurred by SN 2009bb, the first supernova with a relativistic outflow without an observed GRB. However, the ejecta from SN 2009bb was baryon loaded and in nearly free expansion for a year, unlike GRBs. We report the first supernova discovered without a GRB but with rapidly decelerating mildly relativistic ejecta, SN 2012ap. We discovered a bright and rapidly evolving radio counterpart driven by the circumstellar interaction of the relativistic ejecta. However, we did not find any coincident GRB with an isotropic fluence of more than one-sixth of the fluence from GRB 980425. This shows for the first time that central engines in SNe Ic, even without an observed GRB, can produce both relativistic and rapidly decelerating outflows like GRBs. C1 [Chakraborti, Sayan; Soderberg, Alicia; Kamble, Atish; Margutti, Raffaella; Milisavljevic, Dan; Dittmann, Jason] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Chakraborti, Sayan] Harvard Univ, Cambridge, MA 02138 USA. [Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Yadav, Naveen; Ray, Alak] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Hurley, Kevin] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Bietenholz, Michael] York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada. [Brunthaler, Andreas] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdrop, South Africa. [Brunthaler, Andreas] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Pian, Elena] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Mazzali, Paolo] Liverpool John Moores Univ, Liverpool L3 5UX, Merseyside, England. [Mazzali, Paolo] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Fransson, Claes] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Hamuy, Mario] Univ Chile, Dept Astron, Santiago, Chile. [Levesque, Emily] Univ Colorado, C327A, Boulder, CO 80309 USA. [MacFadyen, Andrew] NYU, New York, NY 10003 USA. [Krauss, Miriam] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Briggs, M. S.; Connaughton, V.] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35899 USA. [Yamaoka, K.] Nagoya Univ, Grad Sch Sci, Nagoya, Aichi 4648602, Japan. [Takahashi, T.] ISAS JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Ohno, M.; Fukazawa, Y.] Hiroshima Univ, Higashihiroshima, Hiroshima 7398526, Japan. [Tashiro, M.; Terada, Y.] Saitama Univ, Sakura Ku, Saitama, Saitama 3388570, Japan. [Murakami, T.] Kanazawa Univ, Kanazawa, Ishikawa 9201192, Japan. [Goldsten, J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Barthelmy, S.; Gehrels, N.; Cummings, J.; Krimm, H.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Cummings, J.] UMBC, Dept Phys, Baltimore, MD 21250 USA. [Krimm, H.] Univ Space Res Assoc, Columbia, MD 20144 USA. [Palmer, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Golenetskii, S.; Aptekar, R.; Frederiks, D.; Svinkin, D.] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia. [Cline, T.] NASA, Goddard Space Flight Ctr, Emeritus, Greenbelt, MD 20771 USA. [Mitrofanov, I. G.; Golovin, D.; Litvak, M. L.; Sanin, A. B.] Space Res Inst, Moscow 117997, Russia. [Boynton, W.; Fellows, C.; Harshman, K.; Enos, H.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [von Kienlin, A.; Rau, A.; Zhang, X.] MPE, D-85748 Garching, Germany. [Savchenko, V.] Observ Paris, F-75205 Paris 13, France. RP Chakraborti, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM schakraborti@fas.harvard.edu RI Hamuy, Mario/G-7541-2016; OI Frederiks, Dmitry/0000-0002-1153-6340; MacFadyen, Andrew/0000-0002-0106-9013; Margutti, Raffaella/0000-0003-4768-7586; Pian, Elena/0000-0001-8646-4858 FU Science and Technology Facilities Council [ST/L00061X/1] NR 36 TC 6 Z9 6 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 187 DI 10.1088/0004-637X/805/2/187 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400102 ER PT J AU Dawson, WA Jee, MJ Stroe, A Ng, YK Golovich, N Wittman, D Sobral, D Bruggen, M Rottgering, HJA van Weeren, RJ AF Dawson, William A. Jee, M. James Stroe, Andra Ng, Y. Karen Golovich, Nathan Wittman, David Sobral, David Brueggen, M. Roettgering, H. J. A. van Weeren, R. J. TI MC2: GALAXY IMAGING AND REDSHIFT ANALYSIS OF THE MERGING CLUSTER CIZA J2242.8+5301 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (CISA); galaxies: distances and redshifts ID HUBBLE-SPACE-TELESCOPE; DARK-MATTER; STAR-FORMATION; RICH CLUSTERS; LUMINOSITY FUNCTION; MASS-DISTRIBUTION; DATA REDUCTION; RADIO RELICS; BOW SHOCK; CD-GALAXY AB X- ray and radio observations of CIZA J2242.8+ 5301 suggest that it is a major cluster merger. Despite being well studied in the X- ray and radio, little has been presented on the cluster structure and dynamics inferred from its galaxy population. We carried out a deep ( i < 25) broadband imaging survey of the system with Subaru SuprimeCam ( g and i bands) and the Canada- France- Hawaii Telescope ( r band), as well as a comprehensive spectroscopic survey of the cluster area ( 505 redshifts) using Keck DEep Imaging Multi- Object Spectrograph. We use these data to perform a comprehensive galaxy/ redshift analysis of the system, which is the first step to a proper understanding of the geometry and dynamics of the merger, as well as using the merger to constrain self- interacting dark matter. We find that the system is dominated by two subclusters of comparable richness with a projected separation of 6'.9(-0.5)(+0.7) ( 1.3(-0.10)(+0.13) Mpc). We find that the north and south subclusters have similar redshifts of z approximate to 0.188 with a relative line- of- sight ( LOS) velocity difference of 69 +/- 190 km s(-1). We also find that north and south subclusters have velocity dispersions of 1160(-90)(+100) and 1080(-70)(+100) km s(-1), respectively. These correspond to masses of 16.1(-3.3)(+4.6) x 10(14) and 13.0(-2.5)(+4.0) x 10(14) M-circle dot, respectively. While velocity dispersion measurements of merging clusters can be biased, we believe the bias in this system to be minor due to the large projected separation and nearly plane- of- sky merger configuration. We also find that the cDs of the north and south subclusters are very near their subcluster centers, in both projection ( 55 and 85 kpc, respectively) and normalized LOS velocity (|Delta nu|/sigma(nu) = 0.43. +/- 0.13 and 0.21 +/- 0.12 for the north and south, respectively). CIZA J2242.8+ 5301 is a relatively clean dissociative cluster merger with near 1: 1 mass ratio, which makes it an ideal merger for studying mergerassociated physical phenomena. C1 [Dawson, William A.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Jee, M. James; Golovich, Nathan; Wittman, David] Univ Calif Davis, Davis, CA 95616 USA. [Stroe, Andra; Sobral, David; Roettgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Sobral, David] Univ Lisbon, OAL, Inst Astrofis & Ciencias Espacao, PT-1349018 Tapada Da Ajuda, Portugal. [Sobral, David] Univ Lisbon, Ctr Astron & Astrophys, P-1349018 Lisbon, Portugal. [Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dawson, WA (reprint author), Lawrence Livermore Natl Lab, 7000 East Ave, Livermore, CA 94550 USA. EM dawson29@llnl.gov RI Sobral, David/C-7919-2014; OI Sobral, David/0000-0001-8823-4845; Wittman, David/0000-0002-0813-5888; van Weeren, Reinout/0000-0002-0587-1660 FU NWO; Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant [IF/01154/2012/CP0189/CT0010]; FCT [PEst-OE/FIS/UI2751/2014]; NASA through the Einstein Postdoctoral grant by the Chandra X-ray Center [PF2-130104, NAS8-03060]; Deutsche Forschungsgemeinschaft [FOR 1254, SFB 676]; U.S. DOE by LLNL [DE-AC52-07NA27344]; W. M. Keck Foundation; NSF [AST-0071048]; CARA (Keck Observatory); UCO/Lick Observatory; NSF Facilities and Infrastructure grant [ARI92-14621]; Center for Particle Astrophysics; [HST-GO-13343.01-A] FX We would like to thank the broader membership of the MC2 for their continual development of the science motivating this work, and which has been instrumental in the acquisition of the data used in this paper. We would like to thank Anja von der Linden for the initial recommendation to rotate the Subaru SuprimeCam instrument 90 degrees between exposures to better probe instrument systematics. Slight modifications to this strategy enabled us to reduce the effects of stellar bleeds and nearly double the number of detected objects. We would like to thank Cristbal Sifon Andalaft and the referee for suggestions regarding additional substructure tests. We would also like to thank the referee for suggesting added discussion of the subcluster-BCG offsets. We also would like to thank Michael Schneider for valuable feedback regarding the presentation of the current work. M.J.J., D.W., and W.D. acknowledge support from HST-GO-13343.01-A. A.S. acknowledges financial support from NWO. D.S. acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), and from FCT grant PEst-OE/FIS/UI2751/2014. R.W. is supported by NASA through the Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. M.B. acknowledges support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft. M.B. acknowledges funding from the Deutsche Forschungsgemeinschaft under SFB 676. Part of this work was performed under the auspices of the U.S. DOE by LLNL under Contract DE-AC52-07NA27344. This research has made use of NASA's Astrophysics Data System. The William Herschel Telescope and Isaac Newton Telescope 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. 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. Funding for the DEEP2/DEIMOS pipelines has been provided by NSF grant AST-0071048. The DEIMOS spectrograph was funded by grants from CARA (Keck Observatory) and UCO/Lick Observatory, an NSF Facilities and Infrastructure grant (ARI92-14621), the Center for Particle Astrophysics, and gifts from Sun Microsystems and the Quantum Corporation. NR 61 TC 7 Z9 7 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 JUN 1 PY 2015 VL 805 IS 2 AR 143 DI 10.1088/0004-637X/805/2/143 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400058 ER PT J AU Ellsworth-Bowers, TP Glenn, J Riley, A Rosolowsky, E Ginsburg, A Evans, NJ Bally, J Battersby, C Shirley, YL Merello, M AF Ellsworth-Bowers, Timothy P. Glenn, Jason Riley, Allyssa Rosolowsky, Erik Ginsburg, Adam Evans, Neal J., II Bally, John Battersby, Cara Shirley, Yancy L. Merello, Manuel TI THE BOLOCAM GALACTIC PLANE SURVEY. XIII. PHYSICAL PROPERTIES AND MASS FUNCTIONS OF DENSE MOLECULAR CLOUD STRUCTURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: structure; ISM: clouds; submillimeter: ISM; stars: formation ID STAR-FORMING REGIONS; DUST CONTINUUM SOURCES; C2D LEGACY CLOUDS; MILKY-WAY; NEARBY GALAXIES; DARK CLOUDS; CO SURVEY; HI-GAL; SUPERSONIC TURBULENCE; INTERSTELLAR-MEDIUM AB We use the distance probability density function formalism of Ellsworth-Bowers et al. to derive physical properties for the collection of 1,710 Bolocam Galactic Plane Survey (BGPS) version 2 sources with well-constrained distance estimates. To account for Malmquist bias, we estimate that the present sample of BGPS sources is 90% complete above 400 M-circle dot and 50% complete above 70 M-circle dot. The mass distributions for the entire sample and astrophysically motivated subsets are generally fitted well by a lognormal function, with approximately power-law distributions at high mass. Power-law behavior emerges more clearly when the sample population is narrowed in heliocentric distance (power-law index alpha = 2.0 +/- 0.1 for sources nearer than 6.5 kpc and alpha = 1.9 +/- 0.1 for objects between 2 and 10 kpc). The high-mass power-law indices are generally 1.85 <= alpha <= 2.05 for various subsamples of sources, intermediate between that of giant molecular clouds and the stellar initial mass function. The fit to the entire sample yields a high-mass power-law (alpha) over cap = 1.94(-0.10)(+0.34). Physical properties of BGPS sources are consistent with large molecular cloud clumps or small molecular clouds, but the fractal nature of the dense interstellar medium makes it difficult to map observational categories to the dominant physical processes driving the observed structure. The face-on map of the Galactic disk's mass surface density based on BGPS dense molecular cloud structures reveals the high-mass star-forming regions W43, W49, and W51 to be prominent mass concentrations in the first quadrant. Furthermore, we present a 0.25 kpc resolution map of the dense gas mass fraction across the Galactic disk that peaks around 5%. C1 [Ellsworth-Bowers, Timothy P.; Glenn, Jason; Riley, Allyssa; Bally, John] Univ Colorado, CASA, Boulder, CO 80309 USA. [Rosolowsky, Erik] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Ginsburg, Adam] European So Observ, D-85748 Garching, Germany. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Battersby, Cara] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Merello, Manuel] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. RP Ellsworth-Bowers, TP (reprint author), Univ Colorado, CASA, UCB 389, Boulder, CO 80309 USA. EM timothy.ellsworthbowers@colorado.edu OI Ginsburg, Adam/0000-0001-6431-9633; Rosolowsky, Erik/0000-0002-5204-2259 FU National Science Foundation [AST-1008577]; NSF [AST-0708403, AST-0540882, AST-0838261, AST-1109116]; NSERC of Canada FX The authors thank A. Clauset for providing implementations of the power-law fitting methods used. This work was supported by the National Science Foundation through NSF grant AST-1008577. The BGPS project was supported in part by NSF grant AST-0708403, and was performed at the Caltech Submillimeter Observatory (CSO), supported by NSF grants AST-0540882 and AST-0838261. The CSO was operated by Caltech under contract from the NSF. E.R. is supported by a Discovery Grant from NSERC of Canada. N.J.E. is supported by NSF grant AST-1109116. NR 90 TC 3 Z9 3 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 157 DI 10.1088/0004-637X/805/2/157 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400072 ER PT J AU Hagino, K Stawarz, L Siemiginowska, A Cheung, CC Koziel-Wierzbowska, D Szostek, A Madejski, G Harris, DE Simionescu, A Takahashi, T AF Hagino, K. Stawarz, L. Siemiginowska, A. Cheung, C. C. Koziel-Wierzbowska, D. Szostek, A. Madejski, G. Harris, D. E. Simionescu, A. Takahashi, T. TI ON THE MERGING CLUSTER ABELL 578 AND ITS CENTRAL RADIO GALAXY 4C+67.13 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: individual (Abell 578); galaxies: individual (4C+67.13); galaxies: jets; intergalactic medium; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SUPERMASSIVE BLACK-HOLES; CENTIMETER VLA SURVEY; BRIGHTEST CLUSTER; XMM-NEWTON; JET POWER; ACCRETION MODES; HOST GALAXIES AB Here we analyze radio, optical, and X-ray data for the peculiar cluster Abell 578. This cluster is not fully relaxed and consists of two merging sub-systems. The brightest cluster galaxy (BCG), CGPG 0719.8+6704, is a pair of interacting ellipticals with projected separation similar to 10 kpc, the brighter of which hosts the radio source 4C+67.13. The Fanaroff-Riley type-II radio morphology of 4C+67.13 is unusual for central radio galaxies in local Abell clusters. Our new optical spectroscopy revealed that both nuclei of the CGPG 0719.8+6704 pair are active, albeit at low accretion rates corresponding to the Eddington ratio similar to 10(-4) (for the estimated black hole masses of similar to 3x10(8) M-circle dot and similar to 10(9) M.). The gathered X-ray (Chandra) data allowed us to confirm and to quantify robustly the previously noted elongation of the gaseous atmosphere in the dominant sub-cluster, as well as a large spatial offset (similar to 60 kpc projected) between the position of the BCG and the cluster center inferred from the modeling of the X-ray surface brightness distribution. Detailed analysis of the brightness profiles and temperature revealed also that the cluster gas in the vicinity of 4C+67.13 is compressed (by a factor of about similar to 1.4) and heated (from similar or equal to 2.0 keV up to 2.7 keV), consistent with the presence of a weak shock (Mach number similar to 1.3) driven by the expanding jet cocoon. This would then require the jet kinetic power of the order of similar to 10(45) erg s(-1), implying either a very high efficiency of the jet production for the current accretion rate, or a highly modulated jet/accretion activity in the system. C1 [Hagino, K.; Stawarz, L.; Simionescu, A.; Takahashi, T.] Inst Space & Astronaut Sci JAXA, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Hagino, K.; Takahashi, T.] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Stawarz, L.; Koziel-Wierzbowska, D.; Szostek, A.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Siemiginowska, A.; Harris, D. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Madejski, G.] Stanford Univ, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Dept Phys, Stanford, CA 94305 USA. [Madejski, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. RP Hagino, K (reprint author), Inst Space & Astronaut Sci JAXA, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM hagino@astro.isas.jaxa.jp OI , kouichi/0000-0003-4235-5304 FU Japan Society for the Promotion of Science (JSPS) Research Fellowship; Polish NSC [DEC-2012/04/A/ST9/00083]; NASA [NAS8-03060, DPR S-15633]; Chandra grant [GO0-11144X] FX K. H. is supported by the Japan Society for the Promotion of Science (JSPS) Research Fellowship for Young Scientists. L. S. was supported by Polish NSC grant DEC-2012/04/A/ST9/00083. Support for A. S. was provided by NASA contract NAS8-03060. Work by C. C. C. at NRL is supported in part by NASA DPR S-15633 Y. A. Sz. and G. M. were supported by Chandra grant GO0-11144X. The authors thank the anonymous referee for her/his constructive comments which helped to improve the paper. NR 79 TC 1 Z9 1 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 101 DI 10.1088/0004-637X/805/2/101 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400016 ER PT J AU Johnson, MD Gwinn, CR AF Johnson, Michael D. Gwinn, Carl R. TI THEORY AND SIMULATIONS OF REFRACTIVE SUBSTRUCTURE IN RESOLVED SCATTER-ROADENED IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: structure; Galaxy: nucleus; radio continuum: ISM; scattering; techniques: interferometric ID INTERSTELLAR-MEDIUM; BLACK-HOLE; BROADENED IMAGE; INTERPLANETARY SCINTILLATIONS; PULSAR SCINTILLATION; SCALE STRUCTURE; GALACTIC-CENTER; INNER SCALE; A-ASTERISK; TURBULENCE AB At radio wavelengths, scattering in the interstellar medium distorts the appearance of astronomical sources. Averaged over a scattering ensemble, the result is a blurred image of the source. However, Narayan & Goodman and Goodman & Narayan showed that for an incomplete average, scattering introduces refractive substructure in the image of a point source that is both persistent and wideband. We show that this substructure is quenched but not smoothed by an extended source. As a result, when the scatter-broadening is comparable to or exceeds the unscattered source size, the scattering can introduce spurious compact features into images. In addition, we derive efficient strategies to numerically compute realistic scattered images, and we present characteristic examples from simulations. Our results show that refractive substructure is an important consideration for ongoing missions at the highest angular resolutions, and we discuss specific implications for RadioAstron and the Event Horizon Telescope. C1 [Johnson, Michael D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gwinn, Carl R.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Johnson, MD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mjohnson@cfa.harvard.edu FU U.S. National Science Foundation [AST-1008865]; Gordon and Betty Moore Foundation [GBMF-3561] FX We gratefully acknowledge helpful conversations with Ramesh Narayan, Vincent Fish, and Yuri Kovalev. We thank the referee for identifying the connection with geometrical optics. We thank the U.S. National Science Foundation (AST-1008865); M.J. thanks the Gordon and Betty Moore Foundation (#GBMF-3561) for financial support for this work. NR 45 TC 23 Z9 22 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 JUN 1 PY 2015 VL 805 IS 2 AR 180 DI 10.1088/0004-637X/805/2/180 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400095 ER PT J AU Krishnan, V Ellingsen, SP Reid, MJ Brunthaler, A Sanna, A McCallum, J Reynolds, C Bignall, HE Phillips, CJ Dodson, R Rioja, M Caswell, JL Chen, X Dawson, JR Fujisawa, K Goedhart, S Green, JA Hachisuka, K Honma, M Menten, K Shen, ZQ Voronkov, MA Walsh, AJ Xu, Y Zhang, B Zheng, XW AF Krishnan, V. Ellingsen, S. P. Reid, M. J. Brunthaler, A. Sanna, A. McCallum, J. Reynolds, C. Bignall, H. E. Phillips, C. J. Dodson, R. Rioja, M. Caswell, J. L. Chen, X. Dawson, J. R. Fujisawa, K. Goedhart, S. Green, J. A. Hachisuka, K. Honma, M. Menten, K. Shen, Z. Q. Voronkov, M. A. Walsh, A. J. Xu, Y. Zhang, B. Zheng, X. W. TI FIRST PARALLAX MEASUREMENTS TOWARD A 6.7 GHz METHANOL MASER WITH THE AUSTRALIAN LONG BASELINE ARRAY-DISTANCE TO G 339.884-1.259 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: kinematics and dynamics; masers; stars: formation ID STAR-FORMING REGIONS; H-II REGIONS; PERSEUS SPIRAL ARM; OUTER ROTATION CURVE; TRIGONOMETRIC PARALLAXES; MILKY-WAY; GALACTIC LONGITUDES; VLBI ASTROMETRY; HIGH-RESOLUTION; MASSIVE STARS AB We have conducted the first parallax and proper motion measurements of 6.7 GHz methanol maser emission using the Australian Long Baseline Array. The parallax of G 339.884-1.259 measured from five epochs of observations is 0.48 +/- 0.08 mas, corresponding to a distance of 2.1(-0.3)(+0.4) kpc, placing it in the Scutum spiral arm. This is consistent (within the combined uncertainty) with the kinematic distance estimate for this source at 2.5 +/- 0.5 kpc using the latest Solar and Galactic rotation parameters. We find from the Lyman continuum photon flux that the embedded core of the young star is of spectral type B1, demonstrating that luminous 6.7 GHz methanol masers can be associated with high-mass stars toward the lower end of the mass range. C1 [Krishnan, V.; Ellingsen, S. P.; McCallum, J.] Univ Tasmania, Sch Phys Sci, Hobart, Tas 7001, Australia. [Krishnan, V.; Phillips, C. J.; Caswell, J. L.; Dawson, J. R.; Green, J. A.; Voronkov, M. A.] CSIRO, Australia Telescope Natl Fac, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brunthaler, A.; Sanna, A.; Menten, K.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reynolds, C.; Bignall, H. E.; Walsh, A. J.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Dodson, R.; Rioja, M.] Univ Western Australia M468, Int Ctr Radio Astron Res, Crawley, WA 09, Australia. [Rioja, M.] Observ Astron Nacl IGN, E-28014 Madrid, Spain. [Chen, X.; Hachisuka, K.; Shen, Z. Q.; Zhang, B.] Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Dawson, J. R.] Macquarie Univ, Dept Phys & Astron, MQ Res Ctr Astron Astrophys & Astrophoton, N Ryde, NSW 2109, Australia. [Fujisawa, K.; Hachisuka, K.] Yamaguchi Univ, Fac Sci, Dept Phys, Yamaguchi 7538512, Japan. [Goedhart, S.] Hartebeesthoek Radio Astron Observ, ZA-1740 Krugersdorp, South Africa. [Green, J. A.] Jodrell Bank Observ, SKA Org, Macclesfield SK11 9DL, Cheshire, England. [Honma, M.] Natl Astron Observ Japan, Mizusawa VLBI Observ, Mitaka, Tokyo 1818588, Japan. [Honma, M.] Grad Univ Adv Study, Dept Astronom Sci, Mitaka, Tokyo 1818588, Japan. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Goedhart, S.] SKA South Africa, ZA-7405 Pinelands, South Africa. RP Krishnan, V (reprint author), Univ Tasmania, Sch Phys Sci, Private Bag 37, Hobart, Tas 7001, Australia. EM Vasaant.Krishnan@utas.edu.au RI Ellingsen, Simon/J-7754-2014; Walsh, Andrew/B-5627-2013 OI Ellingsen, Simon/0000-0002-1363-5457; Walsh, Andrew/0000-0001-9506-0855 FU Deutscher Akademischer Austauschdienst (DAAD); National Natural Science Foundation of China [11133008]; Sigma Xi FX Funding assistance was provided in part by Sigma Xi Grants-in-Aid of research, the Deutscher Akademischer Austauschdienst (DAAD), and National Natural Science Foundation of China (Grant No. 11133008). The authors would like to thank the referee for their detailed analysis and comments in reviewing this paper. NR 85 TC 5 Z9 5 U1 2 U2 7 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 JUN 1 PY 2015 VL 805 IS 2 AR 129 DI 10.1088/0004-637X/805/2/129 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400044 ER PT J AU Lee, CF Hirano, N Zhang, QZ Shang, H Ho, PTP Mizuno, Y AF Lee, Chin-Fei Hirano, Naomi Zhang, Qizhou Shang, Hsien Ho, Paul T. P. Mizuno, Yosuke TI JET MOTION, INTERNAL WORKING SURFACES, AND NESTED SHELLS IN THE PROTOSTELLAR SYSTEM HH 212 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (HH 212); ISM: jets and outflows; stars: formation ID MAGNETOHYDRODYNAMIC MODELS; HYDRODYNAMIC SIMULATIONS; PULSED JETS; SIO SHOCKS; OUTFLOWS; DRIVEN; HH-212; HH212; WIND; DISK AB HH 212 is a nearby (400 pc) highly collimated protostellar jet powered by a Class 0 source in Orion. We have mapped the inner 80 '' (similar to 0.16 pc) of the jet in SiO (J = 8 - 7) and CO (J = 3 - 2) simultaneously at similar to 0 ''.5 resolution with the Atacama Millimeter/Submillimeter Array (SMA) at unprecedented sensitivity. The jet consists of a chain of knots and. bow shocks with. sinuous structures in between. Compared to what we saw. in our previous observations with the SMA, the jet. appears to be more continuous, especially in the northern part. Some of the knots are now observed to be associated with small bow shocks, with their bow wings curving back to the jet axis, as seen in pulsed jet simulations. Two of the knots are reasonably resolved, showing kinematics consistent with sideways ejection, possibly tracing the internal working surfaces formed by a temporal variation in the jet velocity. In addition, nested shells are seen in CO around the jet axis connecting to the knots and bow shocks, driven by them. The proper motion of the jet is estimated to be similar to 115 +/- 50 km s(-1), comparing with our previous observations. The jet has a small semi-periodical wiggle. with a period of similar to 93 yr. The amplitude of the wiggle first increases with the distance from the central source and then stays roughly constant. One possible origin of the wiggle could be the kink instability in a magnetized jet. C1 [Lee, Chin-Fei; Hirano, Naomi; Shang, Hsien; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Zhang, Qizhou; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mizuno, Yosuke] Goethe Univ, Inst Theoret Phys, D-60438 Frankfurt, Germany. RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM cflee@asiaa.sinica.edu.tw RI Mizuno, Yosuke/D-5656-2017; OI Mizuno, Yosuke/0000-0002-8131-6730; Zhang, Qizhou/0000-0003-2384-6589 FU National Science Council of Taiwan [NSC 101-2119-M-001-002-MY3]; Academia Sinica (Career Development Award) FX We thank the anonymous referee for insightful comments. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00647. S. ALMA is a partnership of the ESO (representing its member states), NSF (USA), and NINS (Japan). together with the NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by the ESO, AUI/NRAO, and NAOJ. These data were made available to C.-F.L. as part of his ALMA proposal 2011.0.00122. S (PI: Chin-Fei Lee), which requested observations duplicating those of proposal 2011.0.00647. S. C.-F.L. acknowledges grants from the National Science Council of Taiwan (NSC 101-2119-M-001-002-MY3) and the Academia Sinica (Career Development Award). NR 35 TC 9 Z9 9 U1 2 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 JUN 1 PY 2015 VL 805 IS 2 AR 186 DI 10.1088/0004-637X/805/2/186 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400101 ER PT J AU Lu, X Zhang, QZ Wang, K Gu, QS AF Lu, Xing Zhang, Qizhou Wang, Ke Gu, Qiusheng TI INITIAL FRAGMENTATION IN THE INFRARED DARK CLOUD G28.53-0.25 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; stars: formation ID MASSIVE STAR-FORMATION; SUBMILLIMETER ARRAY OBSERVATIONS; WATER MASER SURVEY; MAGNETIC-FIELDS; FORMING REGIONS; HIERARCHICAL FRAGMENTATION; PROTOSTELLAR CANDIDATES; MOLECULAR OUTFLOWS; CO OUTFLOWS; MILKY-WAY AB To study the fragmentation and gravitational collapse of dense cores in infrared dark clouds (IRDCs), we have obtained submillimeter continuum and spectral line data as well as multiple inversion transitions of NH3 and H2O maser data of four massive clumps in IRDC G28.53-0.25. Combining single-dish and interferometer NH3 data, we derive a. rotation temperature of G28.53. We identity 12 dense cores at a 0.1 pc scale based on submillimeter continuum, and obtain their physical properties using NH3 and continuum data. By comparing the Jeans masses of cores with the core masses, we find that turbulent pressure is important for supporting the gas when 1 pc scale clumps fragment into 0.1 pc scale cores. All cores have a virial parameter that is smaller than 1 if we assume an inverse squared radial density profile, suggesting they are gravitationally bound, and the three most promising starforming cores have a virial parameter that is smaller than 1 even when taking the magnetic field into account. We also associate the cores with star formation activities revealed by outflows, masers, or infrared sources. Unlike what previous studies have suggested, MM1 turns out to harbor a few star-forming cores and is likely a progenitor of a high-mass star cluster. MM5 is intermediate while MM7/8 are quiescent in terms of star formation, but they also harbor gravitationally bound dense cores and have the potential for. forming stars, as in MM1. C1 [Lu, Xing; Gu, Qiusheng] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Lu, Xing; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lu, Xing; Gu, Qiusheng] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210093, Peoples R China. [Lu, Xing; Gu, Qiusheng] Collaborat Innovat Ctr Modern Astron & Space Expl, Nanjing 210093, Jiangsu, Peoples R China. [Wang, Ke] European So Observ, D-85748 Garching, Germany. RP Lu, X (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. EM xlu@cfa.harvard.edu OI Wang, Ke/0000-0002-7237-3856; Zhang, Qizhou/0000-0003-2384-6589 FU National Natural Science Foundation of China [11328301, 11273015, 11133001]; National Basic Research Program (973 program) [2013CB834905]; Smithsonian Predoctoral Fellowship; ESO fellowship FX This work was supported by the National Natural Science Foundation of China under grants 11328301, 11273015, and 11133001, and the National Basic Research Program (973 program No. 2013CB834905). X.L. acknowledges the support of a Smithsonian Predoctoral Fellowship. K.W. acknowledges support from the ESO fellowship. NR 57 TC 1 Z9 1 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 171 DI 10.1088/0004-637X/805/2/171 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400086 ER PT J AU Luo, B Brandt, WN Hall, PB Wu, JF Anderson, SF Garmire, GP Gibson, RR Plotkin, RM Richards, GT Schneider, DP Shemmer, O Shen, Y AF Luo, B. Brandt, W. N. Hall, P. B. Wu, Jianfeng Anderson, S. F. Garmire, G. P. Gibson, R. R. Plotkin, R. M. Richards, G. T. Schneider, D. P. Shemmer, O. Shen, Yue TI X-RAY INSIGHTS INTO THE NATURE OF PHL 1811 ANALOGS AND WEAK EMISSION-LINE QUASARS: UNIFICATION WITH A GEOMETRICALLY THICK ACCRETION DISK? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars: emission lines; X-rays: galaxies ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; BROAD ABSORPTION-LINE; BLACK-HOLE GROWTH; SPECTRAL ENERGY-DISTRIBUTIONS; SURVEY COMMISSIONING DATA; RADIO-QUIET QUASARS; 7TH DATA RELEASE; HIGH-REDSHIFT; EDDINGTON RATIO AB We present an X-ray and multiwavelength study of 33 weak emission-line quasars (WLQs) and 18 quasars that are analogs of the extreme WLQ, PHL 1811, at z approximate to 0.5-2.9. New Chandra 1.5-9.5 ks exploratory observations were obtained for 32 objects while the others have archival X-ray observations. Significant fractions of these luminous type 1 quasars are distinctly X-ray weak compared to typical quasars, including 16 (48%) of the WLQs and 17 (94%) of the PHL 1811 analogs with average X-ray weakness factors of 17 and 39, respectively. We measure a relatively hard (Gamma = 1.16(-0.32)(+0.37)) effective power-law photon index for a stack of the X-ray weak subsample, suggesting X-ray absorption, and spectral analysis of one PHL 1811 analog, J1521+5202, also indicates significant intrinsic X-ray absorption. We compare composite Sloan Digital Sky Survey spectra for the X-ray weak and X-ray normal populations and find several optical-UV tracers of X-ray weakness, e.g., Fe II rest-frame equivalent width (REW) and relative color. We describe how orientation effects under our previously proposed "shielding-gas" scenario can likely unify the X-ray weak and X-ray normal populations. We suggest that the shielding gas may naturally be understood as a geometrically thick inner accretion disk that shields the broad line region from the ionizing continuum. If WLQs and PHL 1811 analogs have very high Eddington ratios, the inner disk could be significantly puffed up (e.g., a slim disk). Shielding of the broad emission-line region by a geometrically thick disk may have a significant role in setting the broad distributions of C IV REW and blueshift for quasars more generally. C1 [Luo, B.; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luo, B.; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Davey Lab 104, Dept Phys, University Pk, PA 16802 USA. [Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Wu, Jianfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Anderson, S. F.; Gibson, R. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Garmire, G. P.] Huntingdon Inst Xray Astron LLC, Huntingdon, PA 16652 USA. [Plotkin, R. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Richards, G. T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA. [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. RP Luo, B (reprint author), Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. RI Brandt, William/N-2844-2015; OI Brandt, William/0000-0002-0167-2453; Shemmer, Ohad/0000-0003-4327-1460; Luo, Bin/0000-0002-9036-0063; Plotkin, Richard/0000-0002-7092-0326 FU Chandra X-ray Center [GO3-14100X]; NASA ADP [NNX10AC99G]; ACIS [SV4-74018]; V.M. Willaman Endowment; NSERC; Smithsonian Astrophysica Observatory [SV2-82024]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; Participating Institutions; Smithsonian Astrophysical observatory [SV2-82024] FX We thank M. Eracleous, Y.-F. Jiang, K. Korista, H. Netzer, A. E. Scott, and J. M. Wang for helpful discussions. We thank the referee for carefully reviewing the manuscript and providing helpful comments. We acknowledge financial support from Chandra X-ray Center grant GO3-14100X (B.L., W.N.B.), NASA ADP grant NNX10AC99G (B.L., W.N.B.), ACIS team contract SV4-74018 (B.L., W.N.B.), the V.M. Willaman Endowment (B.L., W.N.B.), NSERC (P.B.H.), and Smithsonian Astrophysica Observatory contract SV2-82024 (G.P.G.). 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 Guaranteed Time Observations (GTO) included here were selected by the ACIS Instrument Principal Investigator, Gordon P. Garmire, of the Huntingdon Institute for X-ray Astronomy, LLC, which is under contract to the Smithsonian Astrophysical observatory, contract SV2-82024. NR 131 TC 19 Z9 19 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 122 DI 10.1088/0004-637X/805/2/122 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400037 ER PT J AU Margutti, R Guidorzi, C Lazzati, D Milisavljevic, D Kamble, A Laskar, T Parrent, J Gehrels, NC Soderberg, AM AF Margutti, R. Guidorzi, C. Lazzati, D. Milisavljevic, D. Kamble, A. Laskar, T. Parrent, J. Gehrels, N. C. Soderberg, A. M. TI DUST IN THE WIND: THE ROLE OF RECENT MASS LOSS IN LONG GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRBs 060218, 100316D, 980425, 130925A); supernovae: general ID GRB 130925A; RADIO OBSERVATIONS; SCATTERING MODEL; SUPERNOVAE; AFTERGLOW; EVOLUTION; STARS; TELESCOPE; ENVIRONMENT; EXPLOSIONS AB We study the late-time (t > 0.5 days) X-ray afterglows of nearby (z < 0.5) long gamma-ray bursts (GRBs) with Swift and identify a population of explosions with slowly decaying, super-soft (photon index Gamma(x) > 3) X-ray emission that is inconsistent with forward shock synchrotron radiation associated with the afterglow. These explosions also show larger-than-average intrinsic absorption (NHx,i > 6 x 10(21) cm(-2)) and prompt gamma-ray emission with extremely long duration (T-90 > 1000 s). The chance association of these three rare properties (i.e., large NHx,i, super-soft Gamma(x), and extreme duration) in the same class of explosions is statistically unlikely. We associate these properties with the turbulent mass-loss history of the progenitor star that enriched and shaped the circumburst medium. We identify a natural connection between NHx,i, Gamma(x), and T-90 in these sources by suggesting that the late-time super-soft X-rays originate from radiation reprocessed by material lost to the environment by the stellar progenitor before exploding (either in the form of a dust echo or as reprocessed radiation from a long-lived GRB remnant), and that the interaction of the explosion's shock/jet with the complex medium is the source of the extremely long prompt emission. However, current observations do not allow us to exclude the possibility that super-soft X-ray emitters originate from peculiar stellar progenitors with large radii that only form in very dusty environments. C1 [Margutti, R.; Milisavljevic, D.; Kamble, A.; Laskar, T.; Parrent, J.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Guidorzi, C.] Univ Ferrara, Dept Phys & Earth Sci, I-44122 Ferrara, Italy. [Lazzati, D.] Oregon State Univ, Dept Phys, Corvallis, OR 97331 USA. [Gehrels, N. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Lazzati, Davide/0000-0002-9190-662X; Margutti, Raffaella/0000-0003-4768-7586 FU NSF [1066293]; David and Lucile Packard Foundation Fellowship for Science and Engineering award FX We thank the referee for helpful comments that improved the quality of our work. R.M. is grateful to the Aspen Center for Physics and the NSF Grant #1066293 for hospitality during the completion of this work and for providing a stimulating environment that inspired this project. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. NR 62 TC 8 Z9 8 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 159 DI 10.1088/0004-637X/805/2/159 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400074 ER PT J AU Murphy, NA Lukin, VS AF Murphy, Nicholas A. Lukin, Vyacheslav S. TI ASYMMETRIC MAGNETIC RECONNECTION IN WEAKLY IONIZED CHROMOSPHERIC PLASMAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; methods: numerical; plasmas; Sun: chromosphere ID 2-FLUID SIMULATIONS; SOLAR CHROMOSPHERE; PENUMBRAL MICROJETS; AMBIPOLAR DIFFUSION; ELLERMAN BOMBS; CURRENT LOOPS; IONIZATION; ATMOSPHERE; DRIVEN; FLARE AB Realistic models of magnetic reconnection in the solar chromosphere must take into account that the plasma is partially ionized and that plasma conditions within any two magnetic flux bundles undergoing reconnection may not be the same. Asymmetric reconnection in the chromosphere may occur when newly emerged flux interacts with pre-existing, overlying flux. We present 2.5D simulations of asymmetric reconnection in weakly ionized, reacting plasmas where the magnetic field strengths, ion and neutral densities, and temperatures are different in each upstream region. The plasma and neutral components are evolved separately to allow non-equilibrium ionization. As in previous simulations of chromospheric reconnection, the current sheet thins to the scale of the neutral-ion mean free path and the ion and neutral outflows are strongly coupled. However, the ion and neutral inflows are asymmetrically decoupled. In cases with magnetic asymmetry, a net flow of neutrals through the current sheet from the weak-field (high-density) upstream region into the strong-field upstream region results from a neutral pressure gradient. Consequently, neutrals dragged along with the outflow are more likely to originate from the weak-field region. The Hall effect leads to the development of a characteristic quadrupole magnetic field modified by asymmetry, but the X-point geometry expected during Hall reconnection does not occur. All simulations show the development of plasmoids after an initial laminar phase. C1 [Murphy, Nicholas A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lukin, Vyacheslav S.] Natl Sci Fdn, Arlington, VA 22230 USA. [Lukin, Vyacheslav S.] US Naval Res Lab, Washington, DC USA. RP Murphy, NA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM namurphy@cfa.harvard.edu OI Murphy, Nicholas/0000-0001-6628-8033 FU NASA [NNX12AB25G, NNX15AF43G, NNX11AB61G, NNM07AB07C]; NSF SHINE [AGS-1156076, AGS-1358342]; LMSAL [8100002705]; NASA LWS; Solar and Heliospheric Physics programs; National Science Foundation FX The authors thank H. Ji, J. Leake, J. Lin, L. Ni, N. Nishizuka, J. Raymond, K. Reeves, C. Shen, H. Tian, and E. Zweibel for useful discussions and an anonymous referee for useful comments that helped to improve this paper. N.A.M. acknowledges support from NASA grants NNX12AB25G, NNX15AF43G, and NNX11AB61G; NSF SHINE grants AGS-1156076 and AGS-1358342; contract 8100002705 from LMSAL; and NASA contract NNM07AB07C to the Smithsonian Astrophysical Observatory (SAO). V.S.L. acknowledges support from the NASA LWS and Solar and Heliospheric Physics programs, as well as the National Science Foundation. Resources supporting this work were provided by the NASA High-End Computing Program through the NASA Advanced Supercomputing Division at Ames Research Center. We thank J. Sattelberger formerly from SAO and J. Chang from NASA for technical support. This work has benefited from the use of NASA's Astrophysics Data System. NR 90 TC 4 Z9 4 U1 1 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 JUN 1 PY 2015 VL 805 IS 2 AR 134 DI 10.1088/0004-637X/805/2/134 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400049 ER PT J AU Plotkin, RM Shemmer, O Trakhtenbrot, B Anderson, SF Brandt, WN Fan, XH Gallo, E Lira, P Luo, B Richards, GT Schneider, DP Strauss, MA Wu, JF AF Plotkin, Richard M. Shemmer, Ohad Trakhtenbrot, Benny Anderson, Scott F. Brandt, W. N. Fan, Xiaohui Gallo, Elena Lira, Paulina Luo, Bin Richards, Gordon T. Schneider, Donald P. Strauss, Michael A. Wu, Jianfeng TI DETECTION OF REST-FRAME OPTICAL LINES FROM X-SHOOTER SPECTROSCOPY OF WEAK EMISSION-LINE QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; quasars: emission lines ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; BL-LACERTAE OBJECTS; SPECTRAL ENERGY-DISTRIBUTION; NEAR-INFRARED SPECTROSCOPY; SURVEY COMMISSIONING DATA; RADIO-QUIET QUASARS; BLACK-HOLE GROWTH; PHL 1811 ANALOGS; DATA RELEASE 7 AB Over the past 15 yr, examples of exotic radio-quiet quasars with intrinsically weak or absent broad emission line regions (BELRs) have emerged from large-scale spectroscopic sky surveys. Here, we present spectroscopy of seven such weak emission line quasars (WLQs) at moderate redshifts (z = 1.4-1.7) using the X-shooter spectrograph, which provides simultaneous optical and near-infrared spectroscopy covering the rest-frame ultraviolet (UV) through optical. These new observations effectively double the number of WLQs with spectroscopy in the optical rest-frame, and they allow us to compare the strengths of (weak) high-ionization emission lines (e.g., C IV) to low-ionization lines (e.g., Mg II, H beta, H alpha) in individual objects. We detect broad Ha and Ha emission in all objects, and these lines are generally toward the weaker end of the distribution expected for typical quasars (e.g., H beta has rest-frame equivalent widths ranging from 15-40 angstrom). However, these low-ionization lines are not exceptionally weak, as is the case for high-ionization lines in WLQs. The X-shooter spectra also display relatively strong optical Fe II emission, H beta FWHM less than or similar to 4000 km s(-1), and significant C IV blueshifts (approximate to 1000-5500 km s(-1)) relative to the systemic redshift; two spectra also show elevated UV Fe II emission, and an outflowing component to their (weak) Mg II emission lines. These properties suggest that WLQs are exotic versions of "wind-dominated" quasars. Their BELRs either have unusual high-ionization components, or their BELRs are in an atypical photoionization state because of an unusually soft continuum. C1 [Plotkin, Richard M.; Gallo, Elena] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Shemmer, Ohad] Univ N Texas, Dept Phys, Denton, TX 76203 USA. [Trakhtenbrot, Benny] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [Anderson, Scott F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Brandt, W. N.; Luo, Bin; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, Bin; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brandt, W. N.] Penn State Univ, Dept Phys, Davey Lab 104, University Pk, PA 16802 USA. [Fan, Xiaohui] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Lira, Paulina] Univ Chile, Dept Astron, Santiago, Chile. [Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Wu, Jianfeng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Plotkin, RM (reprint author), Univ Michigan, Dept Astron, 1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM rplotkin@umich.edu RI Brandt, William/N-2844-2015; Lira, Paulina/G-8536-2016; OI Brandt, William/0000-0002-0167-2453; Shemmer, Ohad/0000-0003-4327-1460; Luo, Bin/0000-0002-9036-0063; Plotkin, Richard/0000-0002-7092-0326; Trakhtenbrot, Benny/0000-0002-3683-7297 FU NASA ADP [NNX10AC99G]; Chandra X-ray Center [GO3-14100X]; NSF [AST 11-07862]; National Aeronautics and Space Administration FX We thank the anonymous referee for constructive comments that improved this paper. We thank Lucas Ellebroek and Hughes Sana for advice on reducing the X-shooter spectra. W.N.B. and B.L. acknowledge support from NASA ADP grant NNX10AC99G, and Chandra X-ray Center grant GO3-14100X. XF acknowledges support from NSF grant AST 11-07862. 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 also made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 93 TC 15 Z9 15 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 123 DI 10.1088/0004-637X/805/2/123 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400038 ER PT J AU Randall, SW Nulsen, PEJ Jones, C Forman, WR Bulbul, E Clarke, TE Kraft, R Blanton, EL David, L Werner, N Sun, M Donahue, M Giacintucci, S Simionescu, A AF Randall, S. W. Nulsen, P. E. J. Jones, C. Forman, W. R. Bulbul, E. Clarke, T. E. Kraft, R. Blanton, E. L. David, L. Werner, N. Sun, M. Donahue, M. Giacintucci, S. Simionescu, A. TI A VERY DEEP CHANDRA OBSERVATION OF THE GALAXY GROUP NGC 5813: AGN SHOCKS, FEEDBACK, AND OUTBURST HISTORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: groups: individual (NGC 5813); galaxies: individual (NGC 5813); X-rays: galaxies ID X-RAY SPECTROSCOPY; GALACTIC NUCLEUS FEEDBACK; ELLIPTIC GALAXIES; PERSEUS CLUSTER; GAS MOTIONS; HIGH-RESOLUTION; COOLING FLOW; COLD FRONTS; INTRACLUSTER MEDIUM; RADIO-LOBE AB We present results from a very deep (650 ks) Chandra X-ray observation of the galaxy group NGC 5813, the deepest Chandra observation of a galaxy group to date. This system uniquely shows three pairs of collinear cavities, with each pair associated with an unambiguous active galactic nucleus (AGN) outburst shock front. The implied mean kinetic power is roughly the same for each outburst, demonstrating that the average AGN kinetic luminosity can remain stable over long timescales (similar to 50 Myr). The two older outbursts have larger, roughly equal total energies as compared with the youngest outburst, implying that the youngest outburst is ongoing. We find that the gas radiative cooling rate and mean shock heating rate are well balanced at each shock front, suggesting that shock heating alone is sufficient to offset cooling and establish AGN/intracluster medium (ICM) feedback within at least the central 30 kpc. This heating takes place roughly isotropically and most strongly at small radii, as is required for feedback to operate. We suggest that shock heating may play a significant role in AGN feedback at smaller radii in other systems, where weak shocks are more difficult to detect. We find non-zero shock front widths that are too large to be explained by particle diffusion. Instead, all measured widths are consistent with shock broadening due to propagation through a turbulent ICM with a mean turbulent speed of similar to 70 km s(-1). Finally, we place lower limits on the temperature of any volume-filling thermal gas within the cavities that would balance the internal cavity pressure with the external ICM. C1 [Randall, S. W.; Nulsen, P. E. J.; Jones, C.; Forman, W. R.; Bulbul, E.; Kraft, R.; David, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clarke, T. E.] Naval Res Lab, Washington, DC 20375 USA. [Blanton, E. L.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Blanton, E. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Werner, N.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Sun, M.] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Simionescu, A.] Japan Aerosp Explorat Agcy, Sagamihara, Kanagawa 2298510, Japan. RP Randall, SW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM srandall@cfa.harvard.edu OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution; Chandra X-ray observatory grant [GO1-12104X]; 6.1 Base funding FX Support for this work was partially provided by the Chandra X-ray Center through NASA contract NAS8-03060, the Smithsonian Institution, and by Chandra X-ray observatory grant GO1-12104X. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. We thank A. Foster, R. Smith, H. Russell, and C. Sarazin for useful discussions. NR 68 TC 14 Z9 15 U1 0 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 JUN 1 PY 2015 VL 805 IS 2 AR 112 DI 10.1088/0004-637X/805/2/112 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400027 ER PT J AU Raymond, JC Edgar, RJ Ghavamian, P Blair, WP AF Raymond, John C. Edgar, Richard J. Ghavamian, Parviz Blair, William P. TI CARBON, HELIUM, AND PROTON KINETIC TEMPERATURES IN A CYGNUS LOOP SHOCK WAVE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Cygnus Loop); ISM: supernova remnants; shock waves; ultraviolet: ISM ID FAST COLLISIONLESS SHOCKS; SUPERNOVA REMNANT; NONRADIATIVE SHOCKS; OPTICAL-EMISSION; SOLAR CORONA; COSMIC-RAYS; SN 1006; EQUILIBRATION; SN-1006; GAS AB Observations of SN 1006 have shown that ions and electrons in the plasma behind fast supernova remnant shock waves are far from equilibrium, with the electron temperature much lower than the proton temperature and ion temperatures approximately proportional to ion mass. In the similar to 360 km s(-1) shock waves of the Cygnus Loop, on the other hand, electron and ion temperatures are roughly equal, and there is evidence that the oxygen kinetic temperature is not far from the proton temperature. In this paper, we report observations of the He II lambda 1640 line and the C IV lambda 1550 doublet in a 360 km s(-1) shock in the Cygnus Loop. While the best-fit kinetic temperatures are somewhat higher than the proton temperature, the temperatures of He and C are consistent with the proton temperature and the upper limits are 0.5 and 0.3 times the mass-proportional temperatures, implying efficient thermal equilibration in this collisionless shock. The equilibration of helium and hydrogen affects the conversion between proton temperatures determined from H alpha line profiles and shock speeds, and the efficient equilibration found here reduces the shock speed estimates and the distance estimate to the Cygnus Loop of Medina et al. to about 800 pc. C1 [Raymond, John C.; Edgar, Richard J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ghavamian, Parviz] Towson Univ, Dept Phys Astron & Geosci, Towson, MD 21252 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu OI Blair, William/0000-0003-2379-6518 FU NASA [NAS8-03060]; [HST-GO-12885]; [HST-GO-13436] FX The authors thank the referee for requesting an additional plot, which revealed a numerical error in the average temperatures, and for other useful suggestions. This work was performed under grants HST-GO-12885 and HST-GO-13436 to the Smithsonian Astrophysical Observatory. R.J.E. was supported by NASA contract NAS8-03060. J.R. and P.G. thank Lorentz Center Workshop on Particle Acceleration from the Solar System to Cosmology for useful discussions. NR 45 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 JUN 1 PY 2015 VL 805 IS 2 AR 152 DI 10.1088/0004-637X/805/2/152 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400067 ER PT J AU Tobin, JJ Looney, LW Wilner, DJ Kwon, W Chandler, CJ Bourke, TL Loinard, L Chiang, HF Schnee, S Chen, XP AF Tobin, John J. Looney, Leslie W. Wilner, David J. Kwon, Woojin Chandler, Claire J. Bourke, Tyler L. Loinard, Laurent Chiang, Hsin-Fang Schnee, Scott Chen, Xuepeng TI A SUB-ARCSECOND SURVEY TOWARD CLASS 0 PROTOSTARS IN PERSEUS: SEARCHING FOR SIGNATURES OF PROTOSTELLAR DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: formation; stars: protostars; techniques: interferometric ID SPITZER C2D SURVEY; MAGNETIC BRAKING CATASTROPHE; STAR-FORMING REGIONS; 1ST HYDROSTATIC CORE; NEARBY DENSE CORES; CIRCUMSTELLAR DISKS; CONTINUUM OBSERVATIONS; YOUNGEST PROTOSTARS; KEPLERIAN DISK; BINARY-SYSTEMS AB We present a 1.3 mm dust continuum survey toward nine Class 0 protostars and two Class I protostars in the Perseus molecular cloud, using CARMA with a resolution of similar to 0 ''.3 (70 AU). This sample approximately doubles the number of Class 0 protostars observed with spatial resolutions <100 AU at millimeter wavelengths, enabling the presence of large protostellar disks and proto-binary systems to be probed. We have detected flattened structures with radii > 100 AU around two sources (L1448 IRS2 and Per-emb-14), and these sources may be strong disk candidates. Marginally resolved structures within 30 degrees of perpendicular to the outflow are found toward three protostars (L1448 IRS3C, IRAS 03282+3035, L1448C) and are considered disk candidates. Two others (L1448 IRS3B, IRAS 03292+3039) have complex resolved structures, possibly indicative of massive, fragmenting inner envelopes or disks; L1448 IRS3B also has evidence for a companion separated by 0 ''.9 (similar to 210 AU). The candidate first hydrostatic core L1451-MMS is marginally resolved on 1 '' scales and the Class 0 protostar IC 348-MMS and does not have strong indications of resolved structure at any scale. The strong disk candidate sources were followed up with (CO)-O-18 (J = 2 -> 1) observations; we detect velocity gradients that are consistent with the expected rotation axis, but without enough sensitivity to determine if it is Keplerian. We compare the observed visibility amplitudes to radiative transfer models of protostellar envelopes and disks. The visibility amplitude ratios show that a compact component (possibly a disk) is necessary for five of nine Class 0 sources. An envelope-only scenario cannot be ruled out for the other four Class 0 sources. We conclude that there is evidence for the formation of large disks in the Class 0 phase, but Class 0 disks likely have a range of radii and masses that depend on the initial conditions of their parent cores. C1 [Tobin, John J.; Schnee, Scott] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Tobin, John J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Looney, Leslie W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Wilner, David J.; Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kwon, Woojin] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Chandler, Claire J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Bourke, Tyler L.] Jodrell Bank, Macclesfield, Cheshire, England. [Loinard, Laurent] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Chiang, Hsin-Fang] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Chiang, Hsin-Fang] Univ Hawaii Manoa, NASA Astrobiol Inst, Hilo, HI 96720 USA. [Chen, Xuepeng] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. RP Tobin, JJ (reprint author), Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. EM tobin@strw.leidenuniv.nl OI Loinard, Laurent/0000-0002-5635-3345 FU NASA through Hubble Fellowship - Space Telescope Science Institute [HST-HF-51300.01 A]; Netherlands Organisation for Scientific Research (NWO) [639.041.439]; European Union A-ERC [291141]; DGAPA; UNAM; CONACyT (Mexico); NASA [NAS 5-26555]; state of Illinois; state of California; state of Maryland; James S. McDonnell Foundation; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; University of Chicago; Associates of the California Institute of Technology; National Science Foundation; Smithsonian Institution; Academia Sinica FX We wish to thank the anonymous referee for helpful comments that have improved the clarity of this paper. We also wish to thank Mike Dunham and Jes Jorgensen for useful discussions. J.J.T. acknowledges support provided by NASA through Hubble Fellowship grant #HST-HF-51300.01 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. This work is supported by grant 639.041.439 from the Netherlands Organisation for Scientific Research (NWO). This work is supported by the European Union A-ERC grant 291141 CHEMPLAN. L.L. acknowledges the support of DGAPA, UNAM, CONACyT (Mexico), for financial support. Support for CARMA construction was derived from the states of Illinois, California, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, 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. The SMA 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 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. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 93 TC 18 Z9 19 U1 1 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 JUN 1 PY 2015 VL 805 IS 2 AR 125 DI 10.1088/0004-637X/805/2/125 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL1PG UT WOS:000356715400040 ER PT J AU Hanisch, RJ Berriman, GB Lazio, TJW Bunn, SE Evans, J McGlynn, TA Plante, R AF Hanisch, R. J. Berriman, G. B. Lazio, T. J. W. Bunn, S. Emery Evans, J. McGlynn, T. A. Plante, R. TI The Virtual Astronomical Observatory: Re-engineering access to astronomical data SO ASTRONOMY AND COMPUTING LA English DT Article DE Catalogs; Surveys; Virtual observatory tools; Data discovery; Data access; Applications ID TOOL; VO; SOFTWARE; SYSTEM; IRIS AB The US Virtual Astronomical Observatory was a software infrastructure and development project designed both to begin the establishment of an operational Virtual Observatory (VU) and to provide the US coordination with the international VU effort. The concept of the VU is to provide the means by which an astronomer is able to discover, access, and process data seamlessly, regardless of its physical location. This paper describes the origins of the VAO, including the predecessor efforts within the US National Virtual Observatory, and summarizes its main accomplishments. These accomplishments include the development of both scripting toolkits that allow scientists to incorporate VU data directly into their reduction and analysis environments and high-level science applications for data discovery, integration, analysis, and catalog cross-comparison. Working with the international community, and based on the experience from the software development, the VAO was a major contributor to international standards within the International Virtual Observatory Alliance. The VAO also demonstrated how an operational virtual observatory could be deployed, providing a robust operational environment in which VU services worldwide were routinely checked for aliveness and compliance with international standards. Finally, the VAO engaged in community outreach, developing a comprehensive web site with on-line tutorials, announcements, links to both US and internationally developed tools and services, and exhibits and hands-on training at annual meetings of the American Astronomical Society and through summer schools and community days. All digital products of the VAO Project, including software, documentation, and tutorials, are stored in a repository for community access. The enduring legacy of the VAO is an increasing expectation that new telescopes and facilities incorporate VU capabilities during the design of their data management systems. Published by Elsevier B.V. C1 [Hanisch, R. J.] Virtual Astron Observ, Washington, DC 20036 USA. [Hanisch, R. J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Berriman, G. B.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Lazio, T. J. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bunn, S. Emery] CALTECH, Ctr Adv Comp Res, Pasadena, CA 91125 USA. [Evans, J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [McGlynn, T. A.] NASA, Goddard Space Flight Ctr, High Energy Astrophys Sci Arch Res Ctr, Greenbelt, MD 20771 USA. [Plante, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. RP Lazio, TJW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.hanisch@nist.gov; gbb@ipac.caltech.edu; joseph.lazio@jpl.nasa.gov; janet@cfa.harvard.edu; thomas.a.mcglynn@nasa.gov; rplante@illinois.edu FU National Science Foundation [AST-0834235]; NASA [NNX13AC07G]; NASA/HEASARC; National Aeronautics & Space Administration (NASA) FX The VAO program would not have been possible without the financial support of the National Science Foundation (AST-0834235) and NASA (NNX13AC07G to STScI/MAST), and it was supported NASA/HEASARC. Funding at IPAC has been provided by a grant from the National Aeronautics & Space Administration (NASA) to the Jet Propulsion Laboratory, operated by the California Institute of Technology under contract to NASA. We appreciate the wise guidance of the Board of Directors of the VAO, LLC, and the VAO Science Council, and we are grateful for feedback from the astronomical community that helped us improve our science tools and infrastructure. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 47 TC 3 Z9 3 U1 1 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2213-1337 EI 2213-1345 J9 ASTRON COMPUT JI Astron. Comput. PD JUN PY 2015 VL 11 SI SI BP 190 EP 209 DI 10.1016/j.ascom.2015.03.007 PN B PG 20 WC Astronomy & Astrophysics; Computer Science, Interdisciplinary Applications SC Astronomy & Astrophysics; Computer Science GA CK9FV UT WOS:000356546900015 ER PT J AU Bowler, BP Andrews, SM Kraus, AL Ireland, MJ Herczeg, G Ricci, L Carpenter, J Brown, ME AF Bowler, Brendan P. Andrews, Sean M. Kraus, Adam L. Ireland, Michael J. Herczeg, Gregory Ricci, Luca Carpenter, John Brown, Michael E. TI AN ALMA CONSTRAINT ON THE GSC 6214-210 B CIRCUM-SUBSTELLAR ACCRETION DISK MASS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; brown dwarfs; stars: individual (GSC 6214-210) ID SCORPIUS OB ASSOCIATION; GIANT PLANET FORMATION; SUN-LIKE STAR; CIRCUMPLANETARY DISKS; WIDE ORBITS; CIRCUMSTELLAR DISKS; HR 8799; COMPANIONS; EVOLUTION; SYSTEMS AB We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of GSC 6214-210 A and B, a solar-mass member of the 5-10 Myr Upper Scorpius association with a 15 +/- 2 M-Jup companion orbiting at approximate to 330 AU (2 ''.2). Previous photometry and spectroscopy spanning 0.3-5 mu m revealed optical and thermal excess as well as strong H alpha and Pa beta emission originating from a circum-substellar accretion disk around GSC 6214-210 B, making it the lowest-mass companion with unambiguous evidence of a subdisk. Despite ALMA's unprecedented sensitivity and angular resolution, neither component was detected in our 880 mu m (341 GHz) continuum observations down to a 3 sigma limit of 0.22 mJy/beam. The corresponding constraints on the dust mass and total mass are <0.15M(circle plus) and <0.05 M-Jup, respectively, or <0.003% and <0.3% of the mass of GSC 6214-210 B itself assuming a 100:1 gas-to-dust ratio and characteristic dust temperature of 10-20 K. If the host star possesses a putative circum-stellar disk then at most it is a meager 0.0015% of the primary mass, implying that giant planet formation has certainly ceased in this system. Considering these limits and its current accretion rate, GSC 6214210 B appears to be at the end stages of assembly and is not expected to gain any appreciable mass over the next few megayears. C1 [Bowler, Brendan P.; Carpenter, John; Brown, Michael E.] CALTECH, Pasadena, CA 91125 USA. [Andrews, Sean M.; Ricci, Luca] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kraus, Adam L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Ireland, Michael J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Herczeg, Gregory] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Bowler, BP (reprint author), CALTECH, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM bpbowler@caltech.edu OI Ireland, Michael/0000-0002-6194-043X; Herczeg, Gregory/0000-0002-7154-6065 FU National Aeronautics and Space Administration; National Science Foundation FX We are grateful to the referee for helpful comments, Jonathan Swift for productive discussions about pursuing this idea, and Vanessa Bailey for providing zero point flux densities for MMT and LBT filters. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00487.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 utilized 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 the National Aeronautics and Space Administration and the National Science Foundation. NASA's Astrophysics Data System Bibliographic Services together with the VizieR catalog access tool and SIMBAD database operated at CDS, Strasbourg, France, were invaluable resources for this work. NR 47 TC 5 Z9 5 U1 1 U2 3 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 JUN 1 PY 2015 VL 805 IS 2 AR L17 DI 10.1088/2041-8205/805/2/L17 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CL0IY UT WOS:000356626900007 ER PT J AU Pafilis, E Frankild, SP Schnetzer, J Fanini, L Faulwetter, S Pavloudi, C Vasileiadou, K Leary, P Hammock, J Schulz, K Parr, CS Arvanitidis, C Jensen, LJ AF Pafilis, Evangelos Frankild, Sune P. Schnetzer, Julia Fanini, Lucia Faulwetter, Sarah Pavloudi, Christina Vasileiadou, Katerina Leary, Patrick Hammock, Jennifer Schulz, Katja Parr, Cynthia Sims Arvanitidis, Christos Jensen, Lars Juhl TI ENVIRONMENTS and EOL: identification of Environment Ontology terms in text and the annotation of the Encyclopedia of Life SO BIOINFORMATICS LA English DT Article; Proceedings Paper CT 11th ISCB-Student-Council Symposium held in conjunction with the 23rd Annual International Conference on Intelligent Systems for Molecular Biology (ISMB) / 14th European Conference on Computational Biology (ECCB) CY JUL 10-14, 2015 CL Dublin, IRELAND SP Int Soc Computat Biol, Student Council AB The association of organisms to their environments is a key issue in exploring biodiversity patterns. This knowledge has traditionally been scattered, but textual descriptions of taxa and their habitats are now being consolidated in centralized resources. However, structured annotations are needed to facilitate large-scale analyses. Therefore, we developed ENVIRONMENTS, a fast dictionary-based tagger capable of identifying Environment Ontology (ENVO) terms in text. We evaluate the accuracy of the tagger on a new manually curated corpus of 600 Encyclopedia of Life (EOL) species pages. We use the tagger to associate taxa with environments by tagging EOL text content monthly, and integrate the results into the EOL to disseminate them to a broad audience of users. C1 [Pafilis, Evangelos; Fanini, Lucia; Faulwetter, Sarah; Pavloudi, Christina; Vasileiadou, Katerina; Arvanitidis, Christos] Hellen Ctr Marine Res, Inst Marine Biol Biotechnol & Aquaculture, Iraklion, Greece. [Frankild, Sune P.; Jensen, Lars Juhl] Univ Copenhagen, Dis Syst Biol Program, Novo Nordisk Fdn Ctr Prot Res, Fac Hlth & Med Sci, Copenhagen, Denmark. [Schnetzer, Julia] Max Planck Inst Marine Microbiol, Bremen, Germany. [Schnetzer, Julia] Jacobs Univ gGmbH, Sch Sci & Engn, Bremen, Germany. [Leary, Patrick] Marine Biol Lab, Woods Hole, MA 02543 USA. [Hammock, Jennifer; Schulz, Katja; Parr, Cynthia Sims] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Pafilis, E (reprint author), Hellen Ctr Marine Res, Inst Marine Biol Biotechnol & Aquaculture, Iraklion, Greece. EM pafilis@hcmr.gr; lars.juhl.jensen@cpr.ku.dk OI Fanini, Lucia/0000-0003-2301-2576; Faulwetter, Sarah/0000-0003-4892-4440 FU Encyclopedia Of Life Rubenstein Fellows Program [CRDF EOL-33066-13/E33066]; LifeWatchGreece Research Infrastructure [384676-94/GSRT/ NSRF(CE)]; Novo Nordisk Foundation Center for Protein Research [NNF14CC0001] FX The Encyclopedia Of Life Rubenstein Fellows Program [CRDF EOL-33066-13/E33066], the LifeWatchGreece Research Infrastructure [384676-94/GSRT/ NSRF(C&E)] and the Novo Nordisk Foundation Center for Protein Research [NNF14CC0001]. NR 8 TC 9 Z9 9 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1367-4803 EI 1460-2059 J9 BIOINFORMATICS JI Bioinformatics PD JUN 1 PY 2015 VL 31 IS 11 BP 1872 EP 1874 PG 3 WC Biochemical Research Methods; Biotechnology & Applied Microbiology; Computer Science, Interdisciplinary Applications; Mathematical & Computational Biology; Statistics & Probability SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Computer Science; Mathematical & Computational Biology; Mathematics GA CL0IL UT WOS:000356625300032 PM 25619994 ER PT J AU Dines, JP Mesnick, SL Ralls, K May-Collado, L Agnarsson, I Dean, MD AF Dines, James P. Mesnick, Sarah L. Ralls, Katherine May-Collado, Laura Agnarsson, Ingi Dean, Matthew D. TI A trade-off between precopulatory and postcopulatory trait investment in male cetaceans SO EVOLUTION LA English DT Review DE Morphological evolution; reproductive strategies; sexual selection; trade-offs ID SPERM COMPETITION GAMES; SEXUAL SIZE DIMORPHISM; ALTERNATIVE MATING TACTICS; MALE REPRODUCTIVE SUCCESS; TESTES SIZE; NATURAL-SELECTION; STENELLA-LONGIROSTRIS; HUMPBACK WHALES; BEAKED-WHALE; HOUSE MICE AB Mating with multiple partners is common across species, and understanding how individual males secure fertilization in the face of competition remains a fundamental goal of evolutionary biology. Game theory stipulates that males have a fixed budget for reproduction that can lead to a trade-off between investment in precopulatory traits such as body size, armaments, and ornaments, and postcopulatory traits such as testis size and spermatogenic efficiency. Recent theoretical and empirical studies have shown that if males can monopolize access to multiple females, they will invest disproportionately in precopulatory traits and less in postcopulatory traits. Using phylogenetically controlled comparative methods, we demonstrate that across 58 cetacean species with the most prominent sexual dimorphism in size, shape, teeth, tusks, and singing invest significantly less in relative testes mass. In support of theoretical predictions, these species tend to show evidence of male contests, suggesting there is opportunity for winners to monopolize access to multiple females. Our approach provides a robust dataset with which to make predictions about male mating strategies for the many cetacean species for which adequate behavioral observations do not exist. C1 [Dines, James P.] Nat Hist Museum Los Angeles Cty, Mammal, Los Angeles, CA 90007 USA. [Dines, James P.] Univ So Calif, Integrat & Evolutionary Biol, Los Angeles, CA 90089 USA. [Mesnick, Sarah L.] Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Southwest Fisheries Sci Ctr, Marine Mammal & Turtle Div, La Jolla, CA 92037 USA. [Ralls, Katherine] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [May-Collado, Laura; Agnarsson, Ingi] Univ Vermont, Dept Biol, Burlington, VT 05405 USA. [Dean, Matthew D.] Univ So Calif, Mol & Computat Biol, Los Angeles, CA 90089 USA. RP Dines, JP (reprint author), Nat Hist Museum Los Angeles Cty, Mammal, 900 Exposition Blvd, Los Angeles, CA 90007 USA. EM jdines@nhm.org; sarah.mesnick@noaa.gov OI Dines, James/0000-0002-3104-2540 FU USC; National Institutes of Health [1R01GM098536]; William Cheney, Jr. Memorial Fund for Mammalogy FX M. McGowen provided electronic copies of cetacean phylogenies. A. Allen, C. Chan, J. Wong, and D. Losey provided expert assistance in ferreting out obscure data sources and maintaining the database. P. Ralph offered statistical advice. R. Baird, P. Best, R. L. Brownell, Jr., R. Connor, J. Durban, C. George, J. Ford, J. Learmonth, J. Mead, L. Moller, R. Pitman, A. Sirovic, R. Wells, and P. Willis generously shared data and provided valuable discussion and insights. J. Conner, M. Alfaro, P. Clapham, W. Perrin, R. Pitman, and four anonymous reviewers provided valuable comments on the manuscript. B. Jarrett provided the artwork for Figure 1. This work was supported by USC startup funds (MDD), National Institutes of Health grant #1R01GM098536 (MDD), and the William Cheney, Jr. Memorial Fund for Mammalogy (JPD). NR 136 TC 11 Z9 11 U1 11 U2 62 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 JUN PY 2015 VL 69 IS 6 BP 1560 EP 1572 DI 10.1111/evo.12676 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CL1AU UT WOS:000356675400015 PM 25929734 ER PT J AU Schook, MW Wildt, DE Raghanti, MA Wolfe, BA Dennis, PM AF Schook, Mandi W. Wildt, David E. Raghanti, Mary Ann Wolfe, Barbara A. Dennis, Patricia M. TI Increased inflammation and decreased insulin sensitivity indicate metabolic disturbances in zoo-managed compared to free-ranging black rhinoceros (Diceros bicornis) SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Black rhinoceros; Hemochromatosis; Glucose; Inflammation; Insulin; Iron overload ID NECROSIS-FACTOR-ALPHA; SERUM-AMYLOID-A; BODY IRON STORES; RISK-FACTORS; THOROUGHBRED GELDINGS; QUANTITATIVE METHODS; POTENTIAL LINK; BLOOD-GLUCOSE; CHECK INDEX; TNF-ALPHA AB Black rhinoceros (rhinos) living in zoos express a host of unusual disease syndromes that are associated with increased morbidity and mortality, including hemolytic anemia, rhabdomyolysis, hepatopathy and ulcerative skin disease, hypophosphatemia and iron overload. We hypothesized that iron overload is a consequence and indicator of disturbances related to inflammation and insulin/glucose metabolism. The objectives of this study were to: (1) generate the first baseline information on biomarkers of inflammation (tumor necrosis factor alpha [TNF alpha], serum amyloid A [SAA]), insulin sensitivity (insulin, glucose and proxy calculations of insulin sensitivity), phosphate and iron stores (ferritin) using banked serum from free-ranging black rhinos; and (2) then compare serum biomarkers between zoo-managed (n = 86 individuals) and free-ranging (n = 120) animals. Enzyme immunoassays were validated for serum and then biomarker levels analyzed using mixed models while controlling for sex, age and year of sample collection. Concentrations of TNF alpha, SAA, insulin and insulin-to glucose ratio were higher (P < 0.05) in black rhinos managed in ex situ conditions compared to free-living counterparts. Findings indicate that the captive environment is contributing to increased inflammation and decreased insulin sensitivity in this endangered species. (C) 2015 Elsevier Inc. All rights reserved. C1 [Schook, Mandi W.; Wildt, David E.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Schook, Mandi W.; Wolfe, Barbara A.] The Wilds, Cumberland, OH 43732 USA. [Schook, Mandi W.; Raghanti, Mary Ann; Dennis, Patricia M.] Cleveland Metropk Zoo, Cleveland, OH 44109 USA. [Raghanti, Mary Ann] Kent State Univ, Kent, OH 44242 USA. [Wolfe, Barbara A.] Columbus Zoo & Aquarium, Powell, OH 43065 USA. [Wolfe, Barbara A.; Dennis, Patricia M.] Ohio State Univ, Dept Vet Prevent Med, Columbus, OH 43210 USA. RP Schook, MW (reprint author), Cleveland Metropk Zoo, 4200 Wildlife Way, Cleveland, OH 44109 USA. EM mws@clevelandmetroparks.com; wildtd@si.edu; mraghant@kent.edu; Barbara.Wolfe@cvm.osu.edu; pmd@clevelandmetroparks.com RI Dennis, Patricia/A-2081-2015 FU Morris Animal Foundation [D08ZO-028]; Philip D. Reed, Jr. Fellowship; Conservation Centers for Species Survival (C2S2); Cleveland Metroparks Zoo FX The authors thank zoological institutions contributing samples for analysis: Disney's Animal Kingdom, Denver Zoo, St. Louis Zoo, Columbus Zoo, Cleveland Metroparks Zoo, White Oak Conservation Center, Fossil Rim Wildlife Center, Milwaukee County Zoo, Miami Metro Zoo, Sedgwick County Zoo, Fort Worth Zoo, Great Plains Zoo and Brookfield Zoo. We also thank South African National Parks for access to serum, housing and laboratory space and Scott Larsen for generous access to serum samples from the University of California, Davis's free-ranging black rhino cryo-repository. We also thank Chris Peterson and Lindsey Long for assistance with sample analysis and Karen Grace-Martin of The Analysis Factor for statistical consulting. Funding for this project was provided by a grant from the Morris Animal Foundation (grant #D08ZO-028). This project also was partially supported by a Philip D. Reed, Jr. Fellowship (to M.S.), the Conservation Centers for Species Survival (C2S2) and core support from the Cleveland Metroparks Zoo. NR 114 TC 1 Z9 1 U1 7 U2 32 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 EI 1095-6840 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD JUN-JUL PY 2015 VL 217 BP 10 EP 19 DI 10.1016/j.ygcen.2015.05.003 PG 10 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA CK7FQ UT WOS:000356398600002 PM 25980685 ER PT J AU Ubelaker, DH AF Ubelaker, Douglas H. TI Transformation by Fire: The Archaeology of Cremation in Cultural Context SO JOURNAL OF ANTHROPOLOGICAL RESEARCH LA English DT Book Review C1 [Ubelaker, Douglas H.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 1 U2 2 PU UNIV NEW MEXICO, DEPT ANTHROPOL PI ALBUQUERQUE PA MSC01 1040, ANTHROPOLOGY 1, UNIV NEW MEXICO, ALBUQUERQUE, NM 87131 USA SN 0091-7710 EI 2153-3806 J9 J ANTHROPOL RES JI J. Anthropol. Res. PD SUM PY 2015 VL 71 IS 2 BP 289 EP 290 PG 2 WC Anthropology SC Anthropology GA CK6DK UT WOS:000356318500027 ER PT J AU Young, HS Dirzo, R McCauley, DJ Agwanda, B Cattaneo, L Dittmarjj, K Eckerlin, RP Fleischer, RC Helgen, LE Hintz, A Montinieri, J Zhao, S Helgen, KM AF Young, Hillary S. Dirzo, Rodolfo McCauley, Douglas J. Agwanda, Bernard Cattaneo, Lia Dittmarjj, Katharina Eckerlin, Ralph P. Fleischer, Robert C. Helgen, Lauren E. Hintz, Ashley Montinieri, John Zhao, Serena Helgen, Kristofer M. TI DRIVERS OF INTENSITY AND PREVALENCE OF FLEA PARASITISM ON SMALL MAMMALS IN EAST AFRICAN SAVANNA ECOSYSTEMS SO JOURNAL OF PARASITOLOGY LA English DT Article ID SEXUAL SIZE DIMORPHISM; DISEASE RISK; BIASED PARASITISM; INFECTIOUS-DISEASE; SPECIES-DIVERSITY; PATHOGEN TRANSMISSION; MAXIMUM-LIKELIHOOD; GROUND-SQUIRRELS; AIR-TEMPERATURE; HOST DIVERSITY AB The relative importance of environmental factors and host factors in explaining variation in prevalence and intensity of flea parasitism in small mammal communities is poorly established. We examined these relationships in an East African savanna landscape, considering multiple host levels: across individuals within a local population, across populations within species, and across species within a landscape. We sampled fleas from 2,672 small mammals of 27 species. This included a total of 8,283 fleas, with 5 genera and 12 species identified. Across individual hosts within a site, both rodent body mass and season affected total intensity of flea infestation, although the explanatory power of these factors was generally modest (<10%). Across host populations in the landscape, we found consistently positive effects of host density and negative effects of vegetation cover on the intensity of flea infestation. Other factors explored (host diversity, annual rainfall, anthropogenic disturbance, and soil properties) tended to have lower and less consistent explanatory power. Across host species in the landscape, we found that host body mass was strongly positively correlated with both prevalence and intensity of flea parasitism, while average robustness of a host species to disturbance was not correlated with flea parasitism. Cumulatively, these results provide insight into the intricate roles of both host and environmental factors in explaining complex patterns of flea parasitism across landscape mosaics. C1 [Young, Hillary S.; McCauley, Douglas J.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Young, Hillary S.; Dirzo, Rodolfo] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Young, Hillary S.; Cattaneo, Lia; Helgen, Lauren E.; Hintz, Ashley; Zhao, Serena; Helgen, Kristofer M.] Natl Museum Nat Hist, Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. [Agwanda, Bernard; Hintz, Ashley; Zhao, Serena; Helgen, Kristofer M.] Natl Museums Kenya, Mammal Sect, Nairobi, Kenya. [Dittmarjj, Katharina] SUNY Buffalo, Dept Biol Sci, Buffalo, NY 14260 USA. [Eckerlin, Ralph P.] No Virginia Community Coll, Div Nat Sci, Annandale, VA 22003 USA. [Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Montinieri, John] Ctr Dis Control & Prevent, Natl Ctr Infect Dis, Div Vector Borne Infect Dis, Ft Collins, CO 80521 USA. RP Young, HS (reprint author), Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. EM hillary.young@lifesci.ucsb.edu FU James Smithson Fund of the Smithsonian Institution; National Geographic Society [4691-91, 8846-10, 9106-12]; National Science Foundation [DEB-09-09670]; Smithsonian Barcode Network; Stanford's Woods Institute for the Environment; Smithsonian Institution Women's Committee [SWC 22, 44] FX We thank Jack Silanje, Peter Lokeny, Everlyn Ndinda, Stephen Nyaga, Anne Adelson, Benjamin Boyce, Cara Brook, Jacy Hyde, Lacey Hughey, Jennifer Guyton, and Pasha Feinberg for their assistance throughout this project. We also thank the Kenyan government, Kenya Wildlife Service, National Museums Kenya, Mpala Research Centre, Ol Jogi Ranch, Ol Pejeta Ranch, Segera Ranch, Ol Maisor Ranch, and the Lekiji, Il Motiok, Koija, Lododo, Narok, Il Polei, Thome, Marura, and Kimugandura communities for their assistance in facilitating this research. Financial support for this project came from the James Smithson Fund of the Smithsonian Institution, the National Geographic Society (grants 4691-91, 8846-10, 9106-12), National Science Foundation (DEB-09-09670), Smithsonian Barcode Network, Stanford's Woods Institute for the Environment, and Smithsonian Institution Women's Committee (SWC 22 and 44). All small mammal trapping and sampling was conducted in accordance with institutional animal care and use permits (Smithsonian Institution IACUC permit 2009-04) and the guidelines of the American Society of Mammalogists for the use of wild mammals in research. We thank S. Miller, A. Bergman, A. Driskell, D. Lunde, and J. Ososky for assistance at the Smithsonian Institution. NR 87 TC 2 Z9 2 U1 3 U2 11 PU AMER SOC PARASITOLOGISTS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-3395 EI 1937-2345 J9 J PARASITOL JI J. Parasitol. PD JUN PY 2015 VL 101 IS 3 BP 327 EP 335 DI 10.1645/14-684.1 PG 9 WC Parasitology SC Parasitology GA CK9DA UT WOS:000356539600009 PM 25634599 ER PT J AU Liberti, J Sapountzis, P Hansen, LH Sorensen, SJ Adams, RMM Boomsma, JJ AF Liberti, Joanito Sapountzis, Panagiotis Hansen, Lars H. Sorensen, Soren J. Adams, Rachelle M. M. Boomsma, Jacobus J. TI Bacterial symbiont sharing in Megalomyrmex social parasites and their fungus-growing ant hosts SO MOLECULAR ECOLOGY LA English DT Article DE 16S rRNA pyrosequencing; Acinetobacter; Bartonellaceae; Entomoplasmatales; social parasites; symbiosis ID FOREL HYMENOPTERA-FORMICIDAE; LEAF-CUTTING ANTS; INTERSPECIFIC TRANSMISSION; MICROBIAL COMMUNITIES; MAXIMUM-LIKELIHOOD; GUT MICROBIOTA; BUMBLE BEES; HONEY-BEE; GENE; WOLBACHIA AB Bacterial symbionts are important fitness determinants of insects. Some hosts have independently acquired taxonomically related microbes to meet similar challenges, but whether distantly related hosts that live in tight symbiosis can maintain similar microbial communities has not been investigated. Varying degrees of nest sharing between Megalomyrmex social parasites (Solenopsidini) and their fungus-growing ant hosts (Attini) from the genera Cyphomyrmex, Trachymyrmex and Sericomyrmex allowed us to address this question, as both ant lineages rely on the same fungal diet, interact in varying intensities and are distantly related. We used tag-encoded FLX 454 pyrosequencing and diagnostic PCR to map bacterial symbiont diversity across the Megalomyrmex phylogenetic tree, which also contains free-living generalist predators. We show that social parasites and hosts share a subset of bacterial symbionts, primarily consisting of Entomoplasmatales, Bartonellaceae, Acinetobacter, Wolbachia and Pseudonocardia and that Entomoplasmatales and Bartonellaceae can co-infect specifically associated combinations of hosts and social parasites with identical 16S rRNA genotypes. We reconstructed in more detail the population-level infection dynamics for Entomoplasmatales and Bartonellaceae in Megalomyrmex symmetochus guest ants and their Sericomyrmex amabilis hosts. We further assessed the stability of the bacterial communities through a diet manipulation experiment and evaluated possible transmission modes in shared nests such as consumption of the same fungus garden food, eating of host brood by social parasites, trophallaxis and grooming interactions between the ants, or parallel acquisition from the same nest environment. Our results imply that cohabiting ant social parasites and hosts may obtain functional benefits from bacterial symbiont transfer even when they are not closely related. C1 [Liberti, Joanito; Sapountzis, Panagiotis; Adams, Rachelle M. M.; Boomsma, Jacobus J.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Hansen, Lars H.; Sorensen, Soren J.] Univ Copenhagen, Dept Biol, Mol Microbial Ecol Grp, DK-2100 Copenhagen, Denmark. [Adams, Rachelle M. M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Adams, RMM (reprint author), Univ Copenhagen, Dept Biol, Ctr Social Evolut, Univ Pk 15, DK-2100 Copenhagen, Denmark. EM rmmadams@gmail.com; jjboomsma@bio.ku.dk RI Sorensen, Soren/J-5015-2014; Boomsma, Jacobus/M-2785-2014; OI Sorensen, Soren/0000-0001-6227-9906; Boomsma, Jacobus/0000-0002-3598-1609; Sapountzis, Panagiotis/0000-0001-6286-3918; Liberti, Joanito/0000-0002-4158-2591 FU Marie Curie International Incoming Fellowship [237266]; Danish National Research Foundation [DNRF57]; ERC [323085] FX We thank the Smithsonian Tropical Research Institute for providing facilities to work in Panama and the Autoridad Nacional del Ambiente y el Mar for issuing sampling and export permits. Sebastian Gottfried assisted in the field sampling and helped with the laboratory work in Panama. Gaspar Bruner and Hermogenes Fernandez-Marin provided part of the ant and fungal samples. Michael Poulsen, Pepijn W. Kooij, Saria Otani and Morten Schiott gave valuable suggestions for data analyses. Waleed A. Al-Soud and Karin P. Vestberg assisted with the sequencing runs and Ana Jesovnik with the nomenclature of the S. cf. diego/zacapanus samples. David Nash and Gosta Nachman helped with statistical analyses, Bjorn Hermansen with creating maps of the sampling sites, Luigi Pontieri with editing some of the figures, Rozlyn E. Haley with the ant drawings and Andreas Schramm, E. Allen Herre and William T. Wcislo with insightful comments and discussion. This work was funded by a Marie Curie International Incoming Fellowship (237266) to R.M.M.A., a grant from the Danish National Research Foundation (DNRF57) to J.J.B. and an ERC Advanced Grant (323085) to J.J.B. NR 94 TC 4 Z9 4 U1 4 U2 31 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 JUN PY 2015 VL 24 IS 12 BP 3151 EP 3169 DI 10.1111/mec.13216 PG 19 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA CL0FI UT WOS:000356615200018 PM 25907143 ER PT J AU Iglesias-Marzoa, R Lopez-Morales, M Jesus Arevalo Morales, M AF Iglesias-Marzoa, Ramon Lopez-Morales, Mercedes Arevalo Morales, Maria Jesus TI The rvfit Code: A Detailed Adaptive Simulated Annealing Code for Fitting Binaries and Exoplanets Radial Velocities SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EARTH-SIZED PLANET; EXTRASOLAR PLANETS; ECLIPSING BINARY; MONTE-CARLO; OPTIMIZATION; ORBITS; TRANSITS; CURVES; STARS AB The fitting of radial velocity curves is a frequent procedure in binary star and exoplanet research. In the majority of cases, the fitting routines need to be fed with a set of initial parameter values and priors from which to begin the computations and their results can be affected by local minima. We present a new code, the rvfit code, for fitting radial velocities of stellar binaries and exoplanets using an adaptive simulated annealing (ASA) global minimization method, which quickly converges to a global solution minimum without the need to provide preliminary parameter values. We show the performance of the code using both synthetic and real datasets: double-lined binaries, single-lined binaries, and exoplanet systems. In all examples, the Keplerian orbital parameters fitted by the rvfit code and their computed uncertainties are compared with literature solutions. Finally, we provide the source code, with a working example and a detailed description of how to use it. C1 [Iglesias-Marzoa, Ramon; Arevalo Morales, Maria Jesus] Univ La Laguna, Dept Astrophys, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Iglesias-Marzoa, Ramon] Spain Ctr Estudios Fis Cosmos Aragon, E-44001 Teruel, Spain. [Lopez-Morales, Mercedes] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arevalo Morales, Maria Jesus] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. RP Iglesias-Marzoa, R (reprint author), Univ La Laguna, Dept Astrophys, E-38205 San Cristobal la Laguna, Tenerife, Spain. EM riglesias@cefca.es FU Spanish Secretary of State for R\D\i (MICINN) [AYA2012-39346-C02-02] FX This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. We are grateful to Guillermo Torres for his fast reply on the data about LV Her. This research has been supported by the Spanish Secretary of State for R\&D\&i (MICINN) under the grant AYA2012-39346-C02-02. We thank the anonymous referee for a number of useful comments and suggestions. NR 52 TC 4 Z9 4 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2015 VL 127 IS 952 BP 567 EP 582 DI 10.1086/682056 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CK8TV UT WOS:000356512300007 ER PT J AU Evans, BS Ryder, TB Reitsma, R Hurlbert, AH Marra, PP AF Evans, Brian S. Ryder, Thomas B. Reitsma, Robert Hurlbert, Allen H. Marra, Peter P. TI Characterizing avian survival along a rural-to-urban land use gradient SO ECOLOGY LA English DT Article DE avian demography; birds; citizen science; land use gradients; mark-recapture; Neighborhood Nestwatch; resource availability; survival; top-down vs. bottom-up processes; urbanization; Washington, DC, USA ID ADULT SEX-RATIOS; URBANIZATION GRADIENT; ECOLOGICAL TRAPS; NESTING BIRDS; UNITED-STATES; LANDSCAPE; HABITAT; POPULATIONS; SURVIVORSHIP; PRODUCTIVITY AB Many avian species persist in human-dominated landscapes; however, little is known about the demographic consequences of urbanization in these populations. Given that urban habitats introduce novel benefits (e.g., anthropogenic resources) and pressures (e.g., mortality risks), conflicting mechanisms have been hypothesized to drive the dynamics of urban bird populations. Top-down processes such as predation predict reduced survivorship in suburban and urban habitats, whereas bottom-up processes, such as increased resource availability, predict peak survival in suburban habitats. In this study, we use mark-recapture data of seven focal species encountered between 2000 and 2012 to test hypotheses about the processes that regulate avian survival along an urbanization gradient in greater Washington, D.C., USA. American Robin, Gray Catbird, Northern Cardinal, and Song Sparrow exhibited peak survival at intermediate and upper portions of the rural-to-urban gradient; this pattern supports the hypothesis that bottom-up processes (e.g., resource availability) can drive patterns of avian survival in some species. In contrast, Carolina Chickadee showed no response and Carolina and House Wren showed a slightly negative response to urban land cover. These contrasting results underscore the need for comparative studies documenting the mechanisms that drive demography and how those factors differentially affect urban adapted and urban avoiding species. C1 [Evans, Brian S.; Hurlbert, Allen H.] Univ N Carolina, Curriculum Environm & Ecol, Chapel Hill, NC 27599 USA. [Evans, Brian S.; Ryder, Thomas B.; Reitsma, Robert; Marra, Peter P.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Hurlbert, Allen H.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. RP Evans, BS (reprint author), Univ N Carolina, Curriculum Environm & Ecol, Chapel Hill, NC 27599 USA. EM bsevans.unc@gmail.com FU Mills Corporation; Wallace Genetic Foundation; Susan and Frank Mars; Youth Access Grants; National Science Foundation [ESI-0540185] FX The Mills Corporation, Wallace Genetic Foundation, Susan and Frank Mars, Youth Access Grants, and the National Science Foundation (ESI-0540185) provided financial support for this study. We are grateful for the many talented field assistants for their contributions over the course of this project, as well as S. Cole, N. Diggs, A. M. Kilpatrick, and K. Sullivan for their invaluable training and support. Thanks to J. Sauer and two anonymous reviewers for substantive feedback that greatly improved the manuscript. Finally, we thank all of the Neighborhood Nestwatch participants for their kindness and commitment to this project. NR 62 TC 6 Z9 6 U1 12 U2 117 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUN PY 2015 VL 96 IS 6 BP 1631 EP 1640 DI 10.1890/14-0171.1 PG 10 WC Ecology SC Environmental Sciences & Ecology GA CK2DV UT WOS:000356021700018 ER PT J AU Hostetler, JA Chandler, RB AF Hostetler, Jeffrey A. Chandler, Richard B. TI Improved state-space models for inference about spatial and temporal variation in abundance from count data SO ECOLOGY LA English DT Article DE abundance; Dail and Madsen model; density dependence; detectability; Gompertz model; immigration; North American Breeding Bird Survey; population dynamics; Ricker model; state-space model; zero-inflated distribution ID BREEDING BIRD SURVEY; POPULATION-DYNAMICS; DENSITY-DEPENDENCE; METAPOPULATION DYNAMICS; BIOLOGICAL POPULATIONS; HIERARCHICAL-MODELS; SAMPLING-VARIANCE; OBSERVATION ERROR; PROCESS NOISE; POINT COUNTS AB Models of population dynamics are frequently used for purposes such as testing hypotheses about density dependence and predicting species' responses to future environmental change or conservation actions. Fitting models of population dynamics to field data is challenging because most data sets are characterized by observation error, which can inflate estimates of process variation if ignored. Recently, state-space models have been developed to deal with this problem by directly modeling both the observation error and the ecological process of interest. Conventional state-space models, however, have several important limitations: (1) they assume that random effects are Gaussian distributed, which implies that abundance can be negative and that false positive observation errors are equally likely as false negative errors; (2) they do not admit spatial variation in population dynamics; and (3) some of the parameters of the model are not estimable. We demonstrate how each of these problems can be resolved using a class of hierarchical models proposed by Dail and Madsen (2011) that attributes observation error to imperfect detection. We expand this class of models to accommodate classical growth models (e.g., exponential and Ricker-logistic), zero-inflation, and random effects. We also present methods for forecasting population size under future environmental conditions. Implementation of these ideas is possible using either frequentist or Bayesian methods, as demonstrated by accompanying R and JAGS code. Results of a simulation study suggest that bias is negligible and coverage nominal in most cases for the proposed model extensions. An analysis of data from the North American Breeding Bird Survey highlights how these methods can be readily applied to existing data, but it also suggests that precision will be low when direct information about detection probability (such as is collected using distance sampling or replicated counts) is lacking. C1 [Hostetler, Jeffrey A.] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Chandler, Richard B.] USGS Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. RP Hostetler, JA (reprint author), Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, St Petersburg, FL 33701 USA. EM jeffrey.hostetler@myfwc.com RI Hostetler, Jeffrey/A-3345-2011; Chandler, Richard/F-9702-2016 OI Hostetler, Jeffrey/0000-0003-3669-1758; FU U.S. National Park Service; Smithsonian Institution; USGS's Breeding Bird Survey program FX We thank J. Andrew Royle, T. Scott Sillett, and John Sauer for helpful suggestions on our analysis. We gratefully acknowledge the U.S. National Park Service, the Smithsonian Institution, and USGS's Breeding Bird Survey program for funding support. We thank Keith Pardieck and David Ziolkowski for help with data acquisition. We are grateful for the numerous helpful suggestions for manuscript revision provided by J. Andrew Royle, T. Scott Sillett, and anonymous referees. NR 49 TC 7 Z9 8 U1 8 U2 73 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUN PY 2015 VL 96 IS 6 BP 1713 EP 1723 DI 10.1890/14-1487.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA CK2DV UT WOS:000356021700026 ER PT J AU Franklin, AD Crosier, AE Vansandt, LM Mattson, E Xiao, ZG AF Franklin, Ashley D. Crosier, Adrienne E. Vansandt, Lindsey M. Mattson, Elliot Xiao, Zhengguo TI INDUCTION OF CYTOKINE PRODUCTION IN CHEETAH (ACINONYX JUBATUS) PERIPHERAL BLOOD MONONUCLEAR CELLS AND VALIDATION OF FELINE-SPECIFIC CYTOKINE ASSAYS FOR ANALYSIS OF CHEETAH SERUM SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Acinonyx jubatus; cheetah; cytokines; inflammation; lipopolysaccharide; peripheral blood mononuclear cells ID HEPATOCYTE-STIMULATING FACTOR; MULTIPLE FORMS; IFN-GAMMA; DISEASES AB Peripheral blood mononuclear cells (PBMCs) were isolated from the whole blood of cheetahs (Acinonyx jubatus; n = 3) and stimulated with lipopolysaccharides (LPS) to induce the production of proinflammatory cytokines TNF-alpha, IL-1 beta, and IL-6 for establishment of cross-reactivity between these cheetah cytokines and feline-specific cytokine antibodies provided in commercially available Feline DuoSet (R) ELISA kits (R&D Systems, Inc., Minneapolis, Minnesota 55413, USA). This study found that feline-specific cytokine antibodies bind specifically to cheetah proinflammatory cytokines TNF-alpha, IL-1 beta, and IL-6 from cell culture supernatants. The assays also revealed that cheetah PBMCs produce a measurable, cell concentration-dependent increase in proinflammatory cytokine production after LPS stimulation. To enable the use of these kits, which are designed for cell culture supernatants for analyzing cytokine concentrations in cheetah serum, percent recovery and parallelism of feline cytokine standards in cheetah serum were also evaluated. Cytokine concentrations in cheetah serum were approximated based on the use of domestic cat standards in the absence of cheetah standard material. In all cases (for cytokines TNF-alpha, IL-1 beta, and IL-6), percent recovery increased as the serum sample dilution increased, though percent recovery varied between cytokines at a given dilution factor. A 1 : 2 dilution of serum resulted in approximately 45, 82, and 7% recovery of TNF-alpha, IL-1 beta, and IL-6 standards, respectively. Adequate parallelism was observed across a large range of cytokine concentrations for TNF-alpha and IL-1 beta; however, a significant departure from parallelism was observed between the IL-6 standard and the serum samples (P = 0.004). Therefore, based on our results, the Feline DuoSet ELISA (R&D Systems, Inc.) kits are valid assays for the measurement of TNF-alpha and IL-1 beta in cheetah serum but should not be used for accurate measurement of IL-6. C1 [Franklin, Ashley D.; Crosier, Adrienne E.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Franklin, Ashley D.; Vansandt, Lindsey M.; Mattson, Elliot; Xiao, Zhengguo] Univ Maryland, Anim & Avian Sci Dept, College Pk, MD 20742 USA. RP Franklin, AD (reprint author), Point Defiance Zoo & Aquarium, Dept Zool, 5400 North Pearl St, Tacoma, WA 98407 USA. EM ashley.franklin@pdza.org RI Franklin, Ashley/J-3069-2015 OI Franklin, Ashley/0000-0002-0818-5156 FU Emanuel J. Friedman Philanthropies FX The authors would like to thank the Smithsonian Conservation Biology Institute for providing access to cheetah whole blood samples. Funding for this project was provided by Emanuel J. Friedman Philanthropies. There is no conflict of interest between the authors and R&D Systems, Inc. NR 13 TC 0 Z9 0 U1 3 U2 16 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 JUN PY 2015 VL 46 IS 2 BP 306 EP 313 PG 8 WC Veterinary Sciences SC Veterinary Sciences GA CK2DU UT WOS:000356021600018 PM 26056884 ER PT J AU Marrow, JC Woc-Colburn, M Hayek, LAC Marker, L Murray, S AF Marrow, Judilee C. Woc-Colburn, Margarita Hayek, Lee-Ann C. Marker, Laurie Murray, Suzan TI COMPARISON OF TWO alpha(2)-ADRENERGIC AGONISTS ON URINE CONTAMINATION OF SEMEN COLLECTED BY ELECTROEJACULATION IN CAPTIVE AND SEMI-FREE-RANGING CHEETAH (ACINONYX JUBATUS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Acinonyx jubatus; alpha(2)-adrenergic agonist; cheetah; electroejaculation; semen; urine contamination ID SPERM; MEDETOMIDINE; XYLAZINE; QUALITY; BLADDER; FLOW AB Alpha(2)-adrenergic agonists are used to immobilize many veterinary species, but use has been infrequently linked to urine contamination of semen collected via electroejaculation. The objective of the study was to compare the alpha(2)-agonists medetomidine and dexmedetomidine on urine contamination of semen in anesthetized cheetahs (Acinonyx jubatus) during electroejaculation procedures. From 2009-2012, a retrospective medical record review revealed 21 anesthesia events in 12 adult male cheetahs. Animals were immobilized with combinations of Telazol(R) (2.33 +/- 0.43 mg/kg) and ketamine (2.38 +/- 1 mg/kg); Telazol (1.17 +/- 0.14 mg/kg), ketamine (1.17 +/- 0.14 mg/kg), and medetomidine (0.012 +/- 0.0017 mg/kg); or Telazol (1.59 +/- 0.1 mg/kg), ketamine (1.59 +/- 0.1 mg/kg) and dexmedetomidine (0.01 +/- 0.001 mg/kg). Semen was successfully collected in all animals; four animals anesthetized with medetomidine had urine contamination (P = 0.037). Medetomidine may contribute to urine contamination; however, further investigation is needed to determine significance in cheetahs. C1 [Marrow, Judilee C.; Woc-Colburn, Margarita; Murray, Suzan] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Wildlife Hlth Sci, Washington, DC 20008 USA. [Hayek, Lee-Ann C.] Smithsonian Inst, Washington, DC 20013 USA. [Marker, Laurie] Cheetah Conservat Fund, Otjiwarongo, Namibia. RP Marrow, JC (reprint author), Binder Pk Zoo, 7400 Div Dr, Battle Creek, MI 49014 USA. EM judileemarrowdvm@gmail.com NR 12 TC 0 Z9 0 U1 4 U2 10 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 JUN PY 2015 VL 46 IS 2 BP 417 EP 420 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA CK2DU UT WOS:000356021600042 PM 26056908 ER PT J AU Pimiento, C Balk, MA AF Pimiento, Catalina Balk, Meghan A. TI Body-size trends of the extinct giant shark Carcharocles megalodon: a deep-time perspective on marine apex predators SO PALEOBIOLOGY LA English DT Article ID FOSSIL RECORD; RANDOM-WALKS; WHITE SHARK; EVOLUTION; STASIS; SELECTION; DISTRIBUTIONS; PATTERNS; MODELS; PANAMA AB The extinct shark Carcharocles megalodon is one of the largest marine apex predators ever to exist. Nonetheless, little is known about its body-size variations through time and space. Here, we studied the body-size trends of C. megalodon through its temporal and geographic range to better understand its ecology and evolution. Given that this species was the last of the megatooth lineage, a group of species that shows a purported size increase through time, we hypothesized that C. megalodon also displayed this trend, increasing in size over time and reaching its largest size prior to extinction. We found that C. megalodon body-size distribution was left-skewed (suggesting a long-term selective pressure favoring larger individuals), and presented significant geographic variation (possibly as a result of the heterogeneous ecological constraints of this cosmopolitan species) over geologic time. Finally, we found that stasis was the general mode of size evolution of C. megalodon (i.e., no net changes over time), contrasting with the trends of the megatooth lineage and our hypothesis. Given that C. megalodon is a relatively long-lived species with a widely distributed fossil record, we further used this study system to provide a deep-time perspective to the understanding of the body-size trends of marine apex predators. For instance, our results suggest that (1) a selective pressure in predatory sharks for consuming a broader range of prey may favor larger individuals and produce left-skewed distributions on a geologic time scale; (2) body-size variations in cosmopolitan apex marine predators may depend on their interactions with geographically discrete communities; and (3) the inherent characteristics of shark species can produce stable sizes over geologic time, regardless of the size trends of their lineages. C1 [Pimiento, Catalina] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Pimiento, Catalina] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Pimiento, Catalina] Smithsonian Trop Res Inst, Balboa, Panama. [Balk, Meghan A.] Univ New Mexico, Albuquerque, NM 87131 USA. RP Pimiento, C (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM pimientoc@ufl.edu FU National Science Foundation [EAR 0418042, PIRE 0966884]; University of New Mexico from the National Institute of Biomedical Imaging and Bioengineering [T32EB009414] FX This project was funded by the National Science Foundation EAR 0418042, PIRE 0966884 (OISE, DRL, EAR). M. A. Balk was supported by the Program in Interdisciplinary Biological and Biomedical Sciences through the University of New Mexico award number T32EB009414 from the National Institute of Biomedical Imaging and Bioengineering. We thank B. MacFadden for his advice and encouragement, but mostly for providing us with the conceptual foundation to pursue this work. We also thank C. Jaramillo for his support and guidance; G. Morgan, D. Ward, B. Silliman, and J. Griffin for insight; and F. Smith, G. Hunt, J. Velez-Juarbe, and P. Shirk for revising earlier versions of this manuscript. Special thanks to the FLMNH, NMNH, MNH, LACM, UCMP, SDNHM, MACN, UNLP, UNMSM, and USNM for allowing us access to their collections and databases; the Field Museum of Natural History, the North Carolina Museum of Natural Sciences, the Museum national d'Histoire naturelle, the Royal Belgian Institute of Natural Sciences, the Museum fur Naturkunde, and the Museo de Nacional de Ciencias Naturales de Madrid for assistance with lists of specimens; to P. Hietz and O. Rodriguez for assistance accessing the collections in the Museum of Natural History, Vienna, Austria; and to D. I. Hastie and E. Fitzgerald for assistance accessing the collections in the Museum Victoria, Australia. Finally, we are grateful for the constructive comments made by M. Gottfried and P. Novack-Gottshall, which substantially improved the original version of the manuscript. The content of this paper is the sole responsibility of the authors and does not necessarily represent the official views of the National Institute of Biomedical Imaging and Bioengineering or the National Institutes of Health. This is University of Florida Contribution to Paleobiology number 674. NR 58 TC 3 Z9 3 U1 15 U2 38 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 JUN PY 2015 VL 41 IS 3 BP 479 EP 490 DI 10.1017/pab.2015.16 PG 12 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA CK3EJ UT WOS:000356099100008 PM 26321775 ER PT J AU Galimany, E Baeta, M Durfort, M Lleonart, J Ramon, M AF Galimany, Eve Baeta, Marc Durfort, Merce Lleonart, Jordi Ramon, Montserrat TI Reproduction and size at first maturity in a Mediterranean exploited Callista chione bivalve bed SO SCIENTIA MARINA LA English DT Article DE gonads; first maturity; hermaphroditism; Veneridae; commercial mollusks ID COD GADUS-MORHUA; RUDITAPES-PHILIPPINARUM; MOLLUSCA-BIVALVIA; GAMETOGENIC CYCLE; SEXUAL-MATURITY; HALIOTIS-IRIS; MANILA CLAM; NEW-ZEALAND; NORTH-WEST; VENERIDAE AB The smooth clam Callista chione is an Atlantic-Mediterranean species that is commercially exploited in several European countries. Several aspects of its reproduction were studied in a coastal location of the northwestern Mediterranean as a tool for sustainable fisheries management. Gonadal development was classified into 6 different stages, ranging from immature to degradation of the remaining sexual structures. Results showed that C. chione was able to reproduce throughout the year but a main spawning period occurred in spring. First records of hermaphrodites were found for this species. The mature spermatozoa measured 4.70 +/- 0.66 mu m (without the flagellum), including a very short acrosome of 0.75 +/- 0.09 mu m. The mid-piece of the spermatozoa had a mitochondrial sheath composed of five mitochondria. Ripe oocytes ranged from 60 to 80 mu m in length. Size at first maturity (SL50) was estimated for the first time in a Mediterranean population, showing values of 30.26 mm in 2005-2006 but only 21.45 mm in 2014. C1 [Galimany, Eve; Ramon, Montserrat] Inst Espanol Oceanog, Ctr Oceanog Balears, Palma de Mallorca 07015, Spain. [Galimany, Eve; Baeta, Marc; Lleonart, Jordi; Ramon, Montserrat] CSIC, Inst Ciencias Mar, E-08003 Barcelona, Spain. [Durfort, Merce] Univ Barcelona, Fac Biol, Dept Biol Cellular, E-08028 Barcelona, Spain. RP Galimany, E (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM mramon@icm.csic.es FU Department d'Agricultura, Ramaderia i Pesca (Generalitat de Catalunya); Direccion General de Costas (Ministerio de Agricultura, Alimentacion y Medio Ambiente) FX This article is a result of the research project "Avaluacio de l'estat del banc natural de petxina lluenta del Maresme" (Evaluation of the condition of the smooth clam bed in the Maresme) funded by the Department d'Agricultura, Ramaderia i Pesca (Generalitat de Catalunya) and the Direccion General de Costas (Ministerio de Agricultura, Alimentacion y Medio Ambiente). We are grateful to the fisherman Mauricio Pulido for allowing us to board his boat Nautes. The histological process of the samples was performed by Dr. Francesc Padros, from the Servei de Diagnostic Patologic en Peixos, Faculty of Veterinary, UAB. The authors also thank "Puertos del Estado" (Ministerio de Fomento) for the environmental water temperature data. The co-author Dr. Montserrat Ramon is part of a Consolidated Research Group (reference 2014 SGR 1383) of the Generalitat de Catalunya. NR 46 TC 1 Z9 1 U1 1 U2 8 PU INST CIENCIAS MAR BARCELONA PI BARCELONA PA PG MARITIM DE LA BARCELONETA, 37-49, 08003 BARCELONA, SPAIN SN 0214-8358 EI 1886-8134 J9 SCI MAR JI Sci. Mar. PD JUN PY 2015 VL 79 IS 2 BP 233 EP 242 DI 10.3989/scimar.04155.13A PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA CK3UZ UT WOS:000356143000008 ER PT J AU Fayle, TM Turner, EC Basset, Y Ewers, RM Reynolds, G Novotny, V AF Fayle, Tom M. Turner, Edgar C. Basset, Yves Ewers, Robert M. Reynolds, Glen Novotny, Vojtech TI Whole-ecosystem experimental manipulations of tropical forests SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review DE climate change; forest fragmentation; forest restoration; logging; nutrients; species interactions ID AMAZONIAN RAIN-FOREST; LITTER MANIPULATION; INSECT HERBIVORES; THROUGHFALL EXCLUSION; SPECIES RICHNESS; PUERTO-RICO; WET FOREST; FOOD WEBS; SCALE; CONSERVATION AB Tropical forests are highly diverse systems involving extraordinary numbers of interactions between species, with each species responding in a different way to the abiotic environment. Understanding how these systems function and predicting how they respond to anthropogenic global change is extremely challenging. We argue for the necessity of 'whole-ecosystem' experimental manipulations, in which the entire ecosystem is targeted, either to reveal the functioning of the system in its natural state or to understand responses to anthropogenic impacts. We survey the current range of whole-ecosystem manipulations, which include those targeting weather and climate, nutrients, biotic interactions, human impacts, and habitat restoration. Finally we describe the unique challenges and opportunities presented by such projects and suggest directions for future experiments. C1 [Fayle, Tom M.; Basset, Yves; Novotny, Vojtech] Univ South Bohemia, Acad Sci Czech Republ, Ctr Biol, Inst Entomol, Ceske Budejovice 37005, Czech Republic. [Fayle, Tom M.; Basset, Yves; Novotny, Vojtech] Univ South Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Fayle, Tom M.; Ewers, Robert M.] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, Ascot SL5 7PY, Berks, England. [Fayle, Tom M.] Univ Malaysia Sabah, Inst Trop Biol & Conservat, Kota Kinabalu, Sabah, Malaysia. [Turner, Edgar C.] Univ Museum Zool, Insect Ecol Grp, Cambridge CB2 3EJ, England. [Basset, Yves] Smithsonian Trop Res Inst, Panama City, Panama. [Reynolds, Glen] Danum Valley Field Ctr, Royal Soc SE Asia Rainforest Res Programme, Lahad Datu 91112, Sabah, Malaysia. RP Fayle, TM (reprint author), Univ South Bohemia, Acad Sci Czech Republ, Ctr Biol, Inst Entomol, Branisovska 31, Ceske Budejovice 37005, Czech Republic. EM tmfayle@gmail.com RI Fayle, Tom/A-2721-2009; Basset, Yves/B-6642-2014; Novotny, Vojtech/G-9434-2014 OI Fayle, Tom/0000-0002-1667-1189; Novotny, Vojtech/0000-0001-7918-8023 FU Australian Research Council [DP140101541]; European Social Fund [CZ.1.07/2.3.00120.0064]; state budget of the Czech Republic; Sistema Nacional de Investigacion of Panama; PT SMART Research Institute; Isaac Newton Trust, Cambridge; European Research Council [281986] FX This review was initiated during a symposium on 'The effects of large scale manipulations of tropical forests on arthropod assemblages' at the INTECOL 2013 congress, London 18-23 August 2013. T.M.F. is funded by the Australian Research Council (DP140101541), T.M.F. and R.M.E. by Yayasan Sime Darby, TMF and Y.B. by the project Biodiversity of Forest Ecosystems (CZ.1.07/2.3.00120.0064) co-financed by the European Social Fund and the state budget of the Czech Republic, and T.M.F. Y.B. and V.N. by the Czech Science Foundation (GACR 14-32302S, 14-36098G, 14-04258S respectively). Y.B. is also supported by the Sistema Nacional de Investigacion of Panama. E.C.T. is supported by funds from PT SMART Research Institute and the Isaac Newton Trust, Cambridge. R.M.E. is supported by European Research Council Project number 281986. We are grateful to Maureen Fayle, Andrew Hector, Jan Leps, Scott Miller, Kalsum M. Yusah, Paul Craze, and two anonymous reviewers for advice during the drafting of the manuscript, and Jennifer Balch for additional information regarding her burning experiments. NR 98 TC 7 Z9 7 U1 8 U2 79 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 JUN PY 2015 VL 30 IS 6 BP 334 EP 346 DI 10.1016/j.tree.2015.03.010 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA CK4JO UT WOS:000356190300010 PM 25896491 ER PT J AU Urashima, T Inamori, H Fukuda, K Saito, T Messer, M Oftedal, OT AF Urashima, Tadasu Inamori, Hiroaki Fukuda, Kenji Saito, Tadao Messer, Michael Oftedal, Olav T. TI 4-O-Acetyl-sialic acid (Neu4,5Ac(2)) in acidic milk oligosaccharides of the platypus (Ornithorhynchus anatinus) and its evolutionary significance SO GLYCOBIOLOGY LA English DT Article DE evolution; milk oligosaccharides; monotreme; platypus; sialic acid ID TACHYGLOSSUS-ACULEATUS-SETOSUS; CHEMICAL-CHARACTERIZATION; MAMMARY-GLAND; ECHIDNA MILK; COLOSTRUM; LACTOSE; GALACTOSIDASE; MARSUPIALS; PROTECTION; DIARRHEA AB Monotremes (echidnas and platypus) retain an ancestral form of reproduction: egg-laying followed by secretion of milk onto skin and hair in a mammary patch, in the absence of nipples. Offspring are highly immature at hatching and depend on oligosaccharide-rich milk for many months. The primary saccharide in long-beaked echidna milk is an acidic trisaccharide Neu4,5Ac(2)(alpha 2-3)Gal(beta 1-4)Glc (4-O-acetyl 3'-sialyllactose), but acidic oligosaccharides have not been characterized in platypus milk. In this study, acidic oligosaccharides purified from the carbohydrate fraction of platypus milk were characterized by matrix-assisted laser desorption/ionization time-of-flight mass spectrometry and H-1-nuclear magnetic resonance spectroscopy. All identified structures, except Neu5Ac(alpha 2-3)Gal(beta 1-4)Glc (3'-sialyllactose) contained Neu4,5Ac(2) (4-O-acetyl-sialic acid). These include the trisaccharide 4-O-acetyl 3'-sialyllactose, the pentasaccharide Neu4,5Ac(2)(alpha 2-3)Gal(beta 1-4)GlcNAc(beta 1-3)Gal(beta 1-4)Glc (4-O-acetyl-3'-sialyllacto-N-tetraose d) and the hexasaccharide Neu4,5Ac(2)(alpha 2-3)Gal(beta 1-4)[Fuc(alpha 1-3)]GlcNAc(beta 1-3)Gal(beta 1-4)Glc (4-O-acetyl-3'-sialyllacto-N-fucopentaose III). At least seven different octa- to deca-oligosaccharides each contained a lacto-N-neohexaose core (LNnH) and one or two Neu4,5Ac(2) and one to three fucose residues. We conclude that platypus milk contains a diverse (a parts per thousand yen20) array of neutral and acidic oligosaccharides based primarily on lactose, lacto-N-neotetraose (LNnT) and LNnH structural cores and shares with echidna milk the unique feature that all identified acidic oligosaccharides (other than 3'-sialyllactose) contain the 4-O-acetyl-sialic acid moiety. We propose that 4-O-acetylation of sialic acid moieties protects acidic milk oligosaccharides secreted onto integumental surfaces from bacterial hydrolysis via steric interference with bacterial sialidases. This may be of evolutionary significance since taxa ancestral to monotremes and other mammals are thought to have secreted milk, or a milk-like fluid containing oligosaccharides, onto skin surfaces. C1 [Urashima, Tadasu; Inamori, Hiroaki; Fukuda, Kenji] Obihiro Univ Agr & Vet Med, Grad Sch Anim & Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Sendai, Miyagi 9818555, Japan. [Messer, Michael] Univ Sydney, Sch Mol Biosci, Sydney, NSW 2006, Australia. [Oftedal, Olav T.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Oftedal, OT (reprint author), Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM oftedalo@si.edu FU Yotsuba Milk Products Co., Hokkaido, Japan FX We acknowledge financial support for laboratory research from the Yotsuba Milk Products Co., Hokkaido, Japan. NR 68 TC 4 Z9 4 U1 5 U2 29 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0959-6658 EI 1460-2423 J9 GLYCOBIOLOGY JI Glycobiology PD JUN PY 2015 VL 25 IS 6 BP 683 EP 697 DI 10.1093/glycob/cwv010 PG 15 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA CJ7IM UT WOS:000355668400009 PM 25601457 ER PT J AU Soon, W Legates, DR AF Soon, Willie Legates, David R. TI Response to the comment on: "Soon, W., and Legates, DR, solar irradiance modulation of equator-to-pole (Arctic) temperature gradients: empirical evidence for climate variation on multi-decadal timescales. Journal of Atmospheric and solar-terrestrial physics, 93, (2013) 45-56" by F. Meunier and A. H. Reis SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Editorial Material DE Sun-climate connection AB We thank Meunier and Reis (hereafter as MR) for their comments on our paper. We, however, do not see the relevance of their alternative interpretation to our original results and believe this reflects their confusion regarding our conclusions rather than a discussion on physical mechanisms. (C) 2015 Elsevier Ltd. All rights reserved. C1 [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Legates, David R.] Univ Delaware, Coll Earth Ocean & Environm, Newark, DE 19716 USA. RP Soon, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM wsoon@cfa.harvard.edu NR 9 TC 0 Z9 0 U1 2 U2 6 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD JUN PY 2015 VL 128 BP 92 EP 93 DI 10.1016/j.jastp.2015.01.013 PG 2 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA CJ7YY UT WOS:000355717500010 ER PT J AU Bernal, XE de Silva, P AF Bernal, Ximena E. de Silva, Priyanka TI Cues used in host-seeking behavior by frog-biting midges (Corethrella spp. Coquillet) SO JOURNAL OF VECTOR ECOLOGY LA English DT Article DE Carbon dioxide; eavesdropping; host-emitted cues; vectors ID CARBON-DIOXIDE; AEDES-ALBOPICTUS; DEFENSIVE BEHAVIOR; LACTIC-ACID; DIPTERA; MOSQUITO; 1-OCTEN-3-OL; ATTRACTANTS; CULICIDAE; AEGYPTI AB We investigated the role of carbon dioxide and host temperature in host attraction in frog-biting midges (Corethrella spp). In these midges, females are known to use frog calls to localize their host, but the role of other host-emitted cues has yet not been investigated. We hypothesized that carbon dioxide acts as a supplemental cue to frog calls. To test this hypothesis, we determined the responses of the midges to carbon dioxide, frog calls, and both cues. A significantly lower number of midges are attracted to carbon dioxide and silent traps than to traps broadcasting frog calls. Adding carbon dioxide to the calls does not increase the attractiveness to the midges. Instead, carbon dioxide can have deterrent effects on frog-biting midges. Temperature of calling frogs is not a cue potentially available to the midges. Contrary to our hypothesis, there was no supplemental effect of carbon dioxide when presented in conjunction to calls. Midge host-seeking behavior strongly depends on the mating calls emitted by their anuran host. Overall, non-acoustic cues such as host body temperature and carbon dioxide are not important in long-distance host location by frog-biting midges. C1 [Bernal, Ximena E.] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Bernal, Ximena E.] Smithsonian Trop Res Inst, Balboa, Panama. [de Silva, Priyanka] Univ Peradeniya, Dept Zool, Fac Sci, Peradeniya, Sri Lanka. RP Bernal, XE (reprint author), Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. EM xbernal@purdue.edu FU NSF IOS [1258039/1433990] FX We are grateful to Joel Tenney from ICA TriNova LLC, who kindly provided the modified, low-emission rate device, and to Bianca Rendon who provided valuable help in the field. Two anonymous reviewers provided valuable comments that improved the quality of the manuscript. We are also thankful to the Smithsonian Tropical Research institute for their logistic support. The Autoridad Nacional del Ambiente (ANAM) provided the required permits to collect and export specimens (No. SC/A-20-12, SE/A-64-13, SE/A-52-14). This work was partially funded by NSF grant IOS#1258039/1433990 to XEB. NR 45 TC 3 Z9 4 U1 1 U2 5 PU SOC VECTOR ECOLOGY PI CORONA PA 1966 COMPTON AVE, CORONA, CA 92881 USA SN 1081-1710 EI 1948-7134 J9 J VECTOR ECOL JI J. Vector Ecol. PD JUN PY 2015 VL 40 IS 1 BP 122 EP 128 DI 10.1111/jvec.12140 PG 7 WC Entomology SC Entomology GA CJ9VN UT WOS:000355851400015 PM 26047192 ER PT J AU Barnard, R Garcia, MR Murray, SS AF Barnard, R. Garcia, M. R. Murray, S. S. TI Chandra, XMM-Newton and HST observations of a transient in M31 with a possible asymmetric, precessing disc SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE X-rays: binaries; X-rays: general ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; SPECTRAL TRANSITIONS; CENTRAL REGION; LIGHT CURVES; STARS; DISCOVERY; GALAXIES; BO-158; PERIOD AB The transient X-ray source CXOM31 004205.77+411330.43 exhibited several outbursts during our long-term monitoring campaign of approximately monthly observations of the M31 centre with Chandra. However, the decay profile appears to be unlike those observed from Galactic transients. We followed up the 2011 outburst with two similar to B band HST/ACS observations, one in outburst and the other in quiescence, and used difference imaging to search for a counterpart; this would be dominated by reprocessed X-ray emission from the disc. We found a counterpart with B = 28.21 +/- 0.16. An XMM-Newton observation from a previous outburst yielded a spectrum that is well described by an absorbed power law with absorption equivalent to similar to 2.6 x 10(21) H atom cm(-2) and photon index similar to 1.8; the highest quality Chandra spectrum yielded only similar to 130 counts, and best fits consistent with the XMM-Newton results. We calculated an absolute V magnitude of +1.9 during outburst for a typical disc spectrum. An empirical relation between the ratio of X-ray to optical flux and orbital period suggests a period less than or similar to 4 h for a black hole accretor. Such a short period is expected to yield an asymmetric, precessing disc, and we propose that the observed decay light curve is due to modulation of the mass transfer rate due to the disc precession. C1 [Barnard, R.; Garcia, M. R.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rbarnard@cfa.harvard.edu FU ESA member states; US (NASA); Chandra grant [GO3-14096X]; HST [GO-13111.05-A]; NASA through a grant from the Space Telescope Science Institute [13111]; Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]; NASA [NAS8-03060] FX This research has made use of data obtained from the Chandra satellite, and software provided by the Chandra X-Ray Center (CXC). We thank Z. Li for creating the merged Chandra image used to register the X-ray image. We also include analysis of public archival data from XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the US (NASA). RB was funded by the Chandra grant GO3-14096X, along with the HST grant GO-13111.05-A. Support for program #13111 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. MRG and SSM are partially supported by NASA contract NAS8-03060. NR 27 TC 0 Z9 0 U1 0 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 JUN 1 PY 2015 VL 449 IS 4 BP 3426 EP 3431 DI 10.1093/mnras/stv551 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000008 ER PT J AU Smith, RJ Lucey, JR Conroy, C AF Smith, Russell J. Lucey, John R. Conroy, Charlie TI The SINFONI Nearby Elliptical Lens Locator Survey: discovery of two new low-redshift strong lenses and implications for the initial mass function in giant early-type galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing: strong; stars: luminosity function, mass function; galaxies: elliptical and lenticular, cD; galaxies: stellar content ID DIGITAL SKY SURVEY; TO-LIGHT RATIO; GRAVITATIONAL LENSES; FUNDAMENTAL PLANE; DATA RELEASE; SYSTEMATIC VARIATION; POPULATION SYNTHESIS; ATLAS(3D) PROJECT; CLUSTER GALAXIES; HALO RESPONSE AB We present results from a blind survey to identify strong gravitational lenses among the population of low-redshift early-type galaxies. The SINFONI Nearby Elliptical Lens Locator Survey (SNELLS) uses integral-field infrared spectroscopy to search for lensed emission line sources behind massive lens candidates at z < 0.055. From 27 galaxies observed, we have recovered one previously known lens (ESO 325-G004) at z = 0.034, and discovered two new systems, at z = 0.031 and 0.052. All three lens galaxies have high velocity dispersions (sigma > 300 km s(-1)) and alpha-element abundances ([Mg/Fe] > 0.3). From the lensing configurations we derive total J-band mass-to-light ratios of 1.8 +/- 0.1, 2.1 +/- 0.1 and 1.9 +/- 0.2 within the similar to 2 kpc Einstein radius. Correcting for estimated dark matter contributions, and comparing to stellar population models with a Milky Way (Kroupa) initial mass function (IMF), we determine the 'mass excess factor', alpha. Assuming the lens galaxies have 'old' stellar populations (10 +/- 1 Gyr), the average IMF mass factor is = 1.10 +/- 0.08 +/- 0.10, where the first error is random and the second is systematic. If we instead fit the stellar populations from 6dF optical survey spectra, all three galaxies are consistent with being old, but the age errors are 3-4 Gyr, due to limited signal-to-noise ratio. The IMF constraints are therefore looser in this case, with = 1.23(-0.13)(+0.16) +/- 0.10. Our results are thus consistent with a Kroupa IMF (alpha = 1.00) on average, and strongly reject very heavy IMFs with alpha greater than or similar to 2. A Salpeter IMF (alpha = 1.55) is inconsistent at the 3.5 sigma level if the galaxies are old, but cannot be excluded using age constraints derived from the currently available optical spectra. C1 [Smith, Russell J.; Lucey, John R.] Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Smith, RJ (reprint author), Univ Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England. EM russell.smith@durham.ac.uk FU STFC Durham Astronomy Consolidated Grant [ST/L00075X/1]; National Aeronautics and Space Administration; National Science Foundation; ESO [093.B-0193, 293.B-5026] FX RJS was supported by the STFC Durham Astronomy Consolidated Grant 2014-2017 (ST/L00075X/1). We are grateful to Matthieu Schaller, Richard Bower and the EAGLE consortium for help in deriving estimates of the projected dark matter masses in massive galaxies, and to Ian Smail for useful discussions during development of the project. We thank an anonymous referee for helpful comments and suggestions. 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 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. The data used in this work are available through the ESO science archive under programme IDs 093.B-0193 and 293.B-5026, and through databases for 2MASS (www.ipac.caltech.edu/2mass) and the 6dF Galaxy Survey (www.6dfgs.net). NR 79 TC 25 Z9 25 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 JUN 1 PY 2015 VL 449 IS 4 BP 3441 EP 3457 DI 10.1093/mnras/stv518 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000010 ER PT J AU Davis, TA Rowlands, K Allison, JR Shabala, SS Ting, YS Lagos, CDP Kaviraj, S Bourne, N Dunne, L Eales, S Ivison, RJ Maddox, S Smith, DJB Smith, MWL Temi, P AF Davis, Timothy A. Rowlands, Kate Allison, James R. Shabala, Stanislav S. Ting, Yuan-Sen Lagos, Claudia del P. Kaviraj, Sugata Bourne, Nathan Dunne, Loretta Eales, Steve Ivison, Rob. J. Maddox, Steve Smith, Daniel J. B. Smith, Matthew W. L. Temi, Pasquale TI Molecular and atomic gas in dust lane early-type galaxies - I. Low star formation efficiencies in minor merger remnants SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: molecules; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: interactions; galaxies: ISM ID CO-TO-H-2 CONVERSION FACTOR; SCIENCE DEMONSTRATION PHASE; MASS-METALLICITY RELATION; DIGITAL-SKY-SURVEY; ATLAS(3D) PROJECT; HERSCHEL-ATLAS; FORMING GALAXIES; ELLIPTIC GALAXIES; SAURON PROJECT; COLD GAS AB In this work we present IRAM 30-m telescope observations of a sample of bulge-dominated galaxies with large dust lanes, which have had a recent minor merger. We find these galaxies are very gas rich, with H-2 masses between 4 x 10(8) and 2 x 10(10) M-circle dot. We use these molecular gas masses, combined with atomic gas masses from an accompanying paper, to calculate gas-to-dust and gas-to-stellar-mass ratios. The gas-to-dust ratios of our sample objects vary widely (between approximate to 50 and 750), suggesting many objects have low gas-phase metallicities, and thus that the gas has been accreted through a recent merger with a lower mass companion. We calculate the implied minor companion masses and gas fractions, finding a median predicted stellar mass ratio of approximate to 40:1. The minor companion likely had masses between approximate to 10(7) and 10(10) M-circle dot. The implied merger mass ratios are consistent with the expectation for low-redshift gas-rich mergers from simulations. We then go on to present evidence that (no matter which star formation rate indicator is used) our sample objects have very low star formation efficiencies (star formation rate per unit gas mass), lower even than the early-type galaxies from ATLAS(3D) which already show a suppression. This suggests that minor mergers can actually suppress star formation activity. We discuss mechanisms that could cause such a suppression, include dynamical effects induced by the minor merger. C1 [Davis, Timothy A.; Lagos, Claudia del P.; Ivison, Rob. J.] European So Observ, D-85748 Garching, Germany. [Davis, Timothy A.; Kaviraj, Sugata; Smith, Daniel J. B.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL1 9AB, Herts, England. [Rowlands, Kate] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Allison, James R.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Shabala, Stanislav S.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Ting, Yuan-Sen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lagos, Claudia del P.] Univ Western Australia, Int Ctr Radio Astron ICRAR, Crawley, WA 6009, Australia. [Bourne, Nathan; Dunne, Loretta] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Dunne, Loretta; Maddox, Steve] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Eales, Steve; Smith, Matthew W. L.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Temi, Pasquale] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. RP Davis, TA (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM t.davis4@herts.ac.uk RI Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Smith, Daniel/0000-0001-9708-253X; Lagos, Claudia/0000-0003-3021-8564; Davis, Timothy/0000-0003-4932-9379; Maddox, Stephen/0000-0001-5549-195X; Ting, Yuan-Sen/0000-0001-5082-9536 FU Science and Technology Facilities Council Ernest Rutherford Fellowship; European Research Council Starting Grant SEDmorph; Australian Research Council [DE130101399]; European Research Council Advanced grant COSMICISM; European Community [229517, 283393]; INSU/CNRS (France); MPG (Germany); IGN (Spain); STFC (UK); ARC (Australia); AAO; National Aeronautics and Space Administration FX TAD acknowledges support from a Science and Technology Facilities Council Ernest Rutherford Fellowship, and thanks Maarten Baes, Gianfranco De Zotti, Ivan Oteo Gomez, Michal Michalowski and Catherine Vlahakis for comments which improved the paper. KR acknowledges support from the European Research Council Starting Grant SEDmorph (PI: V. Wild). SSS thanks the Australian Research Council for an Early Career Fellowship (DE130101399). LD, RJI and SM acknowledge support from the European Research Council Advanced grant COSMICISM. The research leading to these results has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517 and No. 283393 (RadioNet3). This paper is based on observations carried out with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).; The H-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS website is http://www.h-atlas.org/. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programs including GALEX MIS, VST KIDS, VISTA VIKING, WISE, H-ATLAS, GMRT and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO and the participating institutions. The GAMA website is http://www.gama-survey.org/. This publication makes use of data products from the WISE, 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. NR 92 TC 10 Z9 10 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 JUN 1 PY 2015 VL 449 IS 4 BP 3503 EP 3516 DI 10.1093/mnras/stv597 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000014 ER PT J AU Sidoli, L La Palombara, N Esposito, P Tiengo, A Mereghetti, S AF Sidoli, L. La Palombara, N. Esposito, P. Tiengo, A. Mereghetti, S. TI Spectral properties of the soft excess pulsar RX J0059.2-7138 during its 2013 outburst SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: neutron; X-rays: binaries; X-rays: individual: (RX J0059.2-7138) ID SMALL-MAGELLANIC-CLOUD; PHOTON IMAGING CAMERA; BE/X-RAY BINARIES; XMM-NEWTON SURVEY; X-RAY; TRANSIENT PULSAR; NEUTRON-STARS; MAGNETIC-FIELDS; CROSS-SECTIONS; ABSORPTION AB We report on an X-ray observation of the Be X-ray binary pulsar RX J0059.2-7138, performed by XMM-Newton in 2014 March. The 19 ks long observation was carried out about three months after the discovery of the latest outburst from this Small Magellanic Cloud transient, when the source luminosity was L-X similar to 10(38) erg s(-1). A spin period of P-spin = 2.762 383(5) s was derived, corresponding to an average spin-up of. (P) over dot(spin) = -(1.27 +/- 0.01) x 10(-12) s s(-1) from the only previous period measurement, obtained more than 20 years earlier. The time-averaged continuum spectrum (0.2-12 keV) consisted of a hard power-law (photon index similar to 0.44) with an exponential cut-off at a phase-dependent energy (similar to 20-50 keV) plus a significant soft excess below similar to 0.5 keV. In addition, several features were observed in the spectrum: an emission line at 6.6 keV from highly ionized iron, a broad feature at 0.9-1 keV likely due to a blend of Fe L-shell lines, and narrow emission and absorption lines consistent with transitions in highly ionized oxygen, nitrogen and iron visible in the high-resolution RGS data (0.4-2.1 keV). Given the different ionization stages of the narrow-line components, indicative of photoionization from the luminous X-ray pulsar, we argue that the soft excess in RX J0059.2-7138 is produced by reprocessing of the pulsar emission in the inner regions of the accretion disc. C1 [Sidoli, L.; La Palombara, N.; Esposito, P.; Tiengo, A.; Mereghetti, S.] INAF, Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Esposito, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tiengo, A.] IUSS, I-27100 Pavia, Italy. [Tiengo, A.] INFN, Sez Pavia, I-27100 Pavia, Italy. RP Sidoli, L (reprint author), INAF, Ist Astrofis Spaziale & Fis Cosm, Via E Bassini 15, I-20133 Milan, Italy. EM sidoli@iasf-milano.inaf.it OI La Palombara, Nicola/0000-0001-7015-6359; Tiengo, Andrea/0000-0002-6038-1090; Sidoli, Lara/0000-0001-9705-2883; MEREGHETTI, SANDRO/0000-0003-3259-7801; Esposito, Paolo/0000-0003-4849-5092 FU ESA Member States; USA (NASA); Fulbright Research Scholar grant; [ASI-INAF I/037/12/0] FX This work is based on data from observations with XMM-Newton. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). LS thanks A. Pollock and A. Gimenez-Garcia for interesting discussions. PE acknowledges a Fulbright Research Scholar grant administered by the US-Italy Fulbright Commission and is grateful to the Harvard-Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. We acknowledge financial contribution from the agreement ASI-INAF I/037/12/0. NR 30 TC 2 Z9 2 U1 0 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 JUN 1 PY 2015 VL 449 IS 4 BP 3710 EP 3718 DI 10.1093/mnras/stv580 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA CJ2VE UT WOS:000355342000033 ER EF