FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Ashton, G Davidson, I Ruiz, G AF Ashton, Gail Davidson, Ian Ruiz, Gregory TI Transient small boats as a long-distance coastal vector for dispersal of biofouling organisms SO ESTUARIES AND COASTS LA English DT Article DE Anthropogenic transport; Biofouling; Introduced; Latitudinal gradient; Nonindigenous species; Vector ID WESTERN NORTH-AMERICA; BALLAST WATER; MARINE ORGANISMS; INVASION; ALASKA; RISK; POPULATION; EXPANSION; TRANSPORT; PATTERNS AB Alaska is at the northern end of an apparent latitudinal trend of decreasing coastal marine introductions on the West Coast of North America. Historical propagule supply may have played a role in forming this trend, but few studies have evaluated propagule supply to northern latitudes. Here, we examined the role of small boat traffic as a mechanism of long-distance spread for nonindigenous species (NIS) into coastal Alaska. We used a combination of public records, marina surveys, and boater interviews to characterize vessel traffic patterns and boater behaviors. In-water SCUBA sampling of recently arrived transient boats provided data on extent, richness, composition, and biogeography of biofouling incursions to Alaska from outside of the state. We documented a striking seasonality and directionality of vessel traffic, and most vessels were on voyages of > 900 km. Most transient vessels sampled had few organisms, although one third had > 100 organisms on submerged surfaces. Several NIS were recorded, including two that are not known to be established in Alaska (Watersipora subtorquata and Amphibalanus improvisus). The seasonal northward pulse of vessels and their cumulative biofouling species represent an important incursion mechanism for species yet to establish at the northern edge of a marine bioinvasion front in the northeastern Pacific. The low numbers of NIS sampled in this study coincide with the low number of marine NIS known from Alaska, which suggests that an opportunity remains to promote awareness and management of the vector to limit NIS influx to the region. This may be particularly relevant for future scenarios of increased vessel traffic and ocean warming, which are likely to interact to increase establishment success of invaders from the south. C1 [Ashton, Gail] Smithsonian Environm Res Ctr, Marine Invas Lab, Tiburon, CA 94920 USA. [Davidson, Ian] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA. [Davidson, Ian] Smithsonian Environm Res Ctr, Portland, OR 97207 USA. [Ruiz, Gregory] Smithsonian Environm Res Ctr, Marine Invas Lab, Edgewater, MD 21037 USA. RP Ashton, G (reprint author), British Antarctic Survey, Madingley Rd, Cambridge CB3 0ET, England. EM gvashton@gmail.com OI Ruiz, Gregory/0000-0003-2499-441X; Davidson, Ian/0000-0002-8729-6048 FU Alaska Department of Fish and Game FX This research was funded by the Alaska Department of Fish and Game (project leader Tammy Davis). Gary Freitag, Barbara Morgan, Steve Corporon, Monaca Noble, and Trevor Ruiz provided local assistance in Ketchikan, and we also thank Dr Ernie Meloche for inspiration in the field. Other parties who offered assistance in the form of data, access, local knowledge, or personnel include Allen and Saunya Alloway at Wind and Water Charters and Scuba, Alaska Forestry Service, Ketchikan Customs and Border Protection, and Ketchikan Ports and Harbors. Taxonomic experts were Kristen Larson (tunicates), Jeff Cordell (mobile crustacea), Chris Brown (barnacles), and Linda McCann (bryozoans). The genetic analyses were completed by Jonathon Geller's laboratory. NR 46 TC 6 Z9 6 U1 7 U2 24 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 EI 1559-2731 J9 ESTUAR COAST JI Estuaries Coasts PD NOV PY 2014 VL 37 IS 6 BP 1572 EP 1581 DI 10.1007/s12237-014-9782-9 PG 10 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA AR6WY UT WOS:000343722700019 ER PT J AU Drake, BG AF Drake, Bert G. TI Rising sea level, temperature, and precipitation impact plant and ecosystem responses to elevated CO2 on a Chesapeake Bay wetland: review of a 28-year study SO GLOBAL CHANGE BIOLOGY LA English DT Review DE biomass production; ecosystem gas exchange; elevated CO2; evapotranspiration; net ecosystem production; nitrogen; photosynthesis; rising sea level; wetland ID OPEN-TOP CHAMBERS; ATMOSPHERIC CO2; CARBON-DIOXIDE; ESTUARINE MARSH; GAS-EXCHANGE; ACTIVATION STATE; SCIRPUS-OLNEYI; IN-SITU; PHOTOSYNTHESIS; NITROGEN AB An ongoing field study of the effects of elevated atmospheric CO2 on a brackish wetland on Chesapeake Bay, started in 1987, is unique as the longest continually running investigation of the effects of elevated CO2 on an ecosystem. Since the beginning of the study, atmospheric CO2 increased 18%, sea level rose 20cm, and growing season temperature varied with approximately the same range as predicted for global warming in the 21st century. This review looks back at this study for clues about how the effects of rising sea level, temperature, and precipitation interact with high atmospheric CO2 to alter the physiology of C3 and C4 photosynthetic species, carbon assimilation, evapotranspiration, plant and ecosystem nitrogen, and distribution of plant communities in this brackish wetland. Rising sea level caused a shift to higher elevations in the Scirpus olneyi C3 populations on the wetland, displacing the Spartina patens C4 populations. Elevated CO2 stimulated carbon assimilation in the Scirpus C3 species measured by increased shoot and root density and biomass, net ecosystem production, dissolved organic and inorganic carbon, and methane production. But elevated CO2 also decreased biomass of the grass, S.patens C4. The elevated CO2 treatment reduced tissue nitrogen concentration in shoots, roots, and total canopy nitrogen, which was associated with reduced ecosystem respiration. Net ecosystem production was mediated by precipitation through soil salinity: high salinity reduced the CO2 effect on net ecosystem production, which was zero in years of severe drought. The elevated CO2 stimulation of shoot density in the Scirpus C3 species was sustained throughout the 28years of the study. Results from this study suggest that rising CO2 can add substantial amounts of carbon to ecosystems through stimulation of carbon assimilation, increased root exudates to supply nitrogen fixation, reduced dark respiration, and improved water and nitrogen use efficiency. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Drake, BG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM drakeb@si.edu FU US Department of Energy [DE-FG05-85ER60374, DE-FG05-87ER13652, DE-FG02-95ER61993]; NSF-LTREB [DEB-0950080]; Department of Energy's Office of Biological and Environmental Research [DE-SC0008339] FX I wish to gratefully acknowledge the guidance of Dr Lee-Ann Hayek on statistical analyses and manuscript preparation and Dr Lu Meng for assistance with data records. I am grateful for the helpful suggestions of Drs James Bunce, Adam Langely, J. Patrick Megonigal, and two anonymous reviewers of an earlier version of this article. I also acknowledge the sustained support of the US Department of Energy through grants to the Smithsonian Institution that funded the CO2 program at the Smithsonian Environmental Research Center from 1985-1995 (DE-FG05-85ER60374), 1986-1988 (DE-FG05-87ER13652), and 1995-2009 (DE-FG02-95ER61993). The ongoing project is supported by the NSF-LTREB program (grant DEB-0950080) and the Department of Energy's Office of Biological and Environmental Research (grant DE-SC0008339). NR 59 TC 10 Z9 11 U1 20 U2 181 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 NOV PY 2014 VL 20 IS 11 BP 3329 EP 3343 DI 10.1111/gcb.12631 PG 15 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AR7MC UT WOS:000343762800004 PM 24820033 ER PT J AU Martin, AR Erickson, DL Kress, WJ Thomas, SC AF Martin, Adam R. Erickson, David L. Kress, W. John Thomas, Sean C. TI Wood nitrogen concentrations in tropical trees: phylogenetic patterns and ecological correlates SO NEW PHYTOLOGIST LA English DT Article DE functional traits; nitrogen (N); Panama; phylogeny; tropical forest; tropical tree; wood chemistry; wood economics ID RAIN-FOREST TREES; FUNCTIONAL TRAITS; WET FOREST; INTERSPECIFIC VARIATION; PHYSIOLOGICAL ECOLOGY; CARBOHYDRATE STORAGE; NEOTROPICAL FORESTS; ECONOMICS SPECTRUM; LIGHT REQUIREMENTS; NUTRIENT DYNAMICS AB In tropical and temperate trees, wood chemical traits are hypothesized to covary with species' life-history strategy along a wood economics spectrum' (WES), but evidence supporting these expected patterns remains scarce. Due to its role in nutrient storage, we hypothesize that wood nitrogen (N) concentration will covary along the WES, being higher in slow-growing species with high wood density (WD), and lower in fast-growing species with low WD. In order to test this hypothesis we quantified wood N concentrations in 59 Panamanian hardwood species, and used this dataset to examine ecological correlates and phylogenetic patterns of wood N. Wood N varied >14-fold among species between 0.04 and 0.59%; closely related species were more similar in wood N than expected by chance. Wood N was positively correlated with WD, and negatively correlated with log-transformed relative growth rates, although these relationships were relatively weak. We found evidence for co-evolution between wood N and both WD and log-transformed mortality rates. Our study provides evidence that wood N covaries with tree life-history parameters, and that these patterns consistently co-evolve in tropical hardwoods. These results provide some support for the hypothesized WES, and suggest that wood is an increasingly important N pool through tropical forest succession. C1 [Martin, Adam R.; Thomas, Sean C.] Univ Toronto, Fac Forestry, Toronto, ON M5S 3B3, Canada. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Thomas, SC (reprint author), Univ Toronto, Fac Forestry, Earth Sci Bldg,33 Willcocks St, Toronto, ON M5S 3B3, Canada. EM sc.thomas@utoronto.ca FU Hong Kong and Shanghai Banking Corporation Limited (HSBC) Climate Partnership; Natural Sciences and Engineering Research Council of Canada; Center for Tropical Forest Science; Smithsonian Tropical Research Institute FX The authors are grateful to Helene Muller-Landau for generous logistical support and Eric Manzane for invaluable assistance and botanical expertise in the field. Deborah Tam, John McCarron, Tony Ung and the late Bob Jefferies are thanked for their assistance in the lab. Julian Norghauer and three anonymous reviewers are thanked for providing important comments on early versions of the manuscript. Funding for this study was provided by the Hong Kong and Shanghai Banking Corporation Limited (HSBC) Climate Partnership, the Natural Sciences and Engineering Research Council of Canada, the Center for Tropical Forest Science, and the Smithsonian Tropical Research Institute. NR 77 TC 4 Z9 4 U1 2 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD NOV PY 2014 VL 204 IS 3 BP 484 EP 495 DI 10.1111/nph.12943 PG 12 WC Plant Sciences SC Plant Sciences GA AR9CM UT WOS:000343869000009 PM 25046797 ER PT J AU Selvans, MM Stock, JM Clayton, RW Cande, S Granot, R AF Selvans, M. M. Stock, J. M. Clayton, R. W. Cande, S. Granot, R. TI Deep crustal structure of the Adare and Northern Basins, Ross Sea, Antarctica, from sonobuoy data SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE West Antarctic Rift System; marine seismic data; crustal structure; sonobuoy; Adare Basin; Northern Basin ID SOUTHWEST INDIAN RIDGE; MARIE-BYRD-LAND; WEST ANTARCTICA; FRACTURE-ZONE; MOTION; PACIFIC; TRANSECT; VELOCITY; SVALBARD; MARGIN AB Extension associated with ultraslow seafloor spreading within the Adare Basin, in oceanic crust just north of the continental shelf in the Ross Sea, Antarctica, extended south into the Northern Basin. Magnetic and gravity anomaly data suggest continuity of crustal structure across the continental shelf break that separates the Adare and Northern Basins. We use sonobuoy refraction data and multi-channel seismic (MCS) reflection data collected during research cruise NBP0701, including 71 new sonobuoy records, to provide constraints on crustal structure in the Adare and Northern Basins. Adjacent 1D sonobuoy profiles along several MCS lines reveal deep crustal structure in the vicinity of the continental shelf break, and agree with additional sonobuoy data that document fast crustal velocities (6000-8000 m/s) at shallow depths (1-6 km below sea level) from the Adare Basin to the continental shelf, a structure consistent with that of other ultraslow-spread crust. Our determination of crustal structure in the Northern Basin only extends through sedimentary rock to the basement rock, and so cannot help to distinguish between different hypotheses for formation of the basin. (C) 2014 Elsevier B.V. All rights reserved. C1 [Selvans, M. M.; Stock, J. M.; Clayton, R. W.] CALTECH, Seismol Lab, Pasadena, CA 91125 USA. [Selvans, M. M.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20024 USA. [Cande, S.] Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Granot, R.] Ben Gurion Univ Negev, Dept Geol & Environm Sci, IL-84105 Beer Sheva, Israel. RP Selvans, MM (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, 4th St & Independence Ave SW,MRC 315, Washington, DC 20024 USA. EM selvansm@si.edu OI Stock, Joann Miriam/0000-0003-4816-7865 FU National Science Foundation [OPP04-40959, OPP-0440923, OPP-0944711] FX We thank F. Davey for helpful discussions of sonobuoy data analysis and interpretation, and K.S. Panter and an anonymous reviewer for suggestions that improved the figures in this manuscript. We also thank Captain Mike Watson, the crew, and the Raytheon Polar Services Corporation technical staff on board the Nathaniel B. Palmer. This study was supported by National Science Foundation grants OPP04-40959 (S. Cande) and OPP-0440923 and OPP-0944711 U. Stock and R. Clayton). NR 50 TC 1 Z9 1 U1 0 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X EI 1385-013X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD NOV 1 PY 2014 VL 405 BP 220 EP 230 DI 10.1016/j.epsl.2014.08.029 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AR5LF UT WOS:000343625500019 ER PT J AU Kipping, DM AF Kipping, David M. TI Bayesian priors for the eccentricity of transiting planets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; techniques: photometric; techniques: radial velocities; eclipses; planets and satellites: fundamental parameters ID RADIAL-VELOCITY SURVEYS; EXTRASOLAR PLANETS; HYPERGEOMETRIC FUNCTION; ORBITAL ECCENTRICITY; CANDIDATES; KEPLER; STARS; DETECTABILITY; EXOPLANETS; EFFICIENT AB Planets on eccentric orbits have a higher geometric probability of transiting their host star. By application of Bayes' theorem, we reverse this logic to showthat the eccentricity distribution of transiting planets is positively biased. Adopting the flexible Beta distribution as the underlying prior for eccentricity, we derive the marginalized transit probability as well as the a priori joint probability distribution of eccentricity and argument of periastron, given that a planet is known to transit. These results allow us to demonstrate that most planet occurrence rate calculations using Kepler data have overestimated the prevalence of planets by similar to 10 per cent. Indeed, the true occurrence of planets from transit surveys is fundamentally intractable without a prior assumption for the eccentricity distribution. Further more, we show that previously extracted eccentricity distributions using Kepler data are positively biased. In cases where one wishes to impose an informative eccentricity prior, we provide a recursive algorithm to apply inverse transform sampling of our joint prior probability distribution. Computer code of this algorithm, ECCSAMPLES, is provided to enable the community to sample directly from the prior (available here). C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu FU NASA Sagan Fellowship FX DMK is supported by the NASA Sagan Fellowship. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. NR 43 TC 15 Z9 15 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD NOV 1 PY 2014 VL 444 IS 3 BP 2263 EP 2269 DI 10.1093/mnras/stu1561 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR2FS UT WOS:000343399600025 ER PT J AU Lawler, SM Di Francesco, J Kennedy, GM Sibthorpe, B Booth, M Vandenbussche, B Matthews, BC Holland, WS Greaves, J Wilner, DJ Tuomi, M Blommaert, JADL de Vries, BL Dominik, C Fridlund, M Gear, W Heras, AM Ivison, R Olofsson, G AF Lawler, S. M. Di Francesco, J. Kennedy, G. M. Sibthorpe, B. Booth, M. Vandenbussche, B. Matthews, B. C. Holland, W. S. Greaves, J. Wilner, D. J. Tuomi, M. Blommaert, J. A. D. L. de Vries, B. L. Dominik, C. Fridlund, M. Gear, W. Heras, A. M. Ivison, R. Olofsson, G. TI The debris disc of solar analogue tau Ceti: Herschel observations and dynamical simulations of the proposed multiplanet system SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: dynamical evolution and stability; planet-disc; interactions; circumstellar matter; stars: individual: tau Ceti ID MAIN-SEQUENCE STARS; LOW-MASS PLANETS; ALL-SKY SURVEY; BETA-PICTORIS; HR 8799; SPIRE INSTRUMENT; DUST CONTENT; ALIGNMENT; EMISSION; ROTATION AB tau Ceti is a nearby, mature G-type star very similar to our Sun, with a massive Kuiper Belt analogue and possible multiplanet system that has been compared to our Solar system. We present Herschel Space Observatory images of the debris disc, finding the disc is resolved at 70 mu m and 160 mu m, and marginally resolved at 250 mu m. The Herschel images and infrared photometry from the literature are best modelled using a wide dust annulus with an inner edge between 1 and 10 au and an outer edge at similar to 55 au, inclined from face-on by 35 degrees +/- 10 degrees, and with no significant azimuthal structure. We model the proposed tightly packed planetary system of five super-Earths and find that the innermost dynamically stable disc orbits are consistent with the inner edge found by the observations. The photometric modelling, however, cannot rule out a disc inner edge as close to the star as 1 au, though larger distances produce a better fit to the data. Dynamical modelling shows that the five-planet system is stable with the addition of a Neptune or smaller mass planet on an orbit outside 5 au, where the radial velocity data analysis would not have detected a planet of this mass. C1 [Lawler, S. M.; Di Francesco, J.; Matthews, B. C.] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 2Y2, Canada. [Lawler, S. M.; Di Francesco, J.; Matthews, B. C.] Natl Res Council Canada, Herzberg Astron & Astrophys Program, Victoria, BC V9E 2E7, Canada. [Kennedy, G. M.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sibthorpe, B.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. [Booth, M.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago 7820436, Chile. [Vandenbussche, B.; Blommaert, J. A. D. L.] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium. [Holland, W. S.] Royal Observ Edinburgh, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Holland, W. S.] Univ Edinburgh, Royal Observ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Greaves, J.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tuomi, M.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Tuomi, M.] Univ Chile, Dept Astron, Santiago, Chile. [Blommaert, J. A. D. L.] Vrije Univ Brussel, Dept Phys & Astrophys, Astron & Astrophys Res Grp, B-1050 Brussels, Belgium. [Blommaert, J. A. D. L.] Flemish Inst Technol Res VITO, B-2400 Mol, Belgium. [de Vries, B. L.; Olofsson, G.] Stockholm Univ, AlbaNova Univ Ctr, Dept Astron, SE-10691 Stockholm, Sweden. [de Vries, B. L.] Stockholm Univ, Astrobiol Ctr, SE-10691 Stockholm, Sweden. [Dominik, C.] Univ Amsterdam, Anton Pannekoek Inst, NL-1098 XH Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Fridlund, M.] German Aerosp Ctr, Inst Planetary Res, D-12489 Berlin, Germany. [Fridlund, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Gear, W.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Heras, A. M.] ESA ESTEC, Sci & Robot Explorat Directorate, Sci Support Off, NL-2200 AG Noordwijk, Netherlands. [Ivison, R.] European So Observ, D-85748 Garching, Germany. [Ivison, R.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Lawler, SM (reprint author), Univ Victoria, Dept Phys & Astron, STN CSC, POB 1700, Victoria, BC V8W 2Y2, Canada. EM lawler@uvic.ca RI Ivison, R./G-4450-2011 OI Ivison, R./0000-0001-5118-1313 FU European Union through ERC [279973]; FONDECYT Postdoctral Fellowship [3140479] FX The authors thank an anonymous referee for providing helpful comments on this paper. SML and BCM acknowledge an NSERC Discovery Accelerator Supplement which funded this work. This work was also supported by the European Union through ERC grant number 279973 (GMK). MB acknowledges support from a FONDECYT Postdoctral Fellowship, project no. 3140479. NR 60 TC 4 Z9 4 U1 0 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 NOV 1 PY 2014 VL 444 IS 3 BP 2665 EP 2675 DI 10.1093/mnras/stu1641 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR2FS UT WOS:000343399600052 ER PT J AU Duncan, K Conselice, CJ Mortlock, A Hartley, WG Guo, Y Ferguson, HC Dave, R Lu, Y Ownsworth, J Ashby, MLN Dekel, A Dickinson, M Faber, S Giavalisco, M Grogin, N Kocevski, D Koekemoer, A Somerville, RS White, CE AF Duncan, K. Conselice, C. J. Mortlock, A. Hartley, W. G. Guo, Y. Ferguson, H. C. Dave, R. Lu, Y. Ownsworth, J. Ashby, M. L. N. Dekel, A. Dickinson, M. Faber, S. Giavalisco, M. Grogin, N. Kocevski, D. Koekemoer, A. Somerville, R. S. White, C. E. TI The mass evolution of the first galaxies: stellar mass functions and star formation rates at 4 < z < 7 in the CANDELS GOODS-South field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: luminosity function; mass function ID ULTRA-DEEP FIELD; LYMAN-BREAK GALAXIES; HIGH-REDSHIFT GALAXIES; EXTRAGALACTIC LEGACY SURVEY; EARLY RELEASE SCIENCE; ULTRAVIOLET LUMINOSITY DENSITY; SPECTRAL ENERGY-DISTRIBUTIONS; ACTIVE GALACTIC NUCLEI; BROAD-BAND PHOTOMETRY; LY-ALPHA EMITTERS AB We measure new estimates for the galaxy stellar mass function and star formation rates for samples of galaxies at z similar to 4, 5, 6 and 7 using data in the CANDELS GOODS South field. The deep near-infrared observations allow us to construct the stellar mass function at z >= 6 directly for the first time. We estimate stellar masses for our sample by fitting the observed spectral energy distributions with synthetic stellar populations, including nebular line and continuum emission. The observed UV luminosity functions for the samples are consistent with previous observations; however, we find that the observed M-UV-M-* relation has a shallow slope more consistent with a constant mass-to-light ratio and a normalization which evolves with redshift. Our stellar mass functions have steep low-mass slopes (alpha approximate to -1.9), steeper than previously observed at these redshifts and closer to that of theUVluminosity function. Integrating our new mass functions, we find the observed stellar mass density evolves from log(10)rho(*) =(+0.58)(-0.89) at z similar to 7 to 7.36 +/- 0.06 M-circle dot Mpc(-3) at z similar to 4. Finally, combining the measured UV continuum slopes (beta) with their rest-frame UV luminosities, we calculate dust-corrected star formation rates (SFR) for our sample. We find the specific SFR for a fixed stellar mass increases with redshift whilst the global SFR density falls rapidly over this period. Our new SFR density estimates are higher than previously observed at this redshift. C1 [Duncan, K.; Conselice, C. J.; Mortlock, A.; Hartley, W. G.; Ownsworth, J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Mortlock, A.] Univ Edinburgh, Inst Astron, SUPA, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Hartley, W. G.] Swiss Fed Inst Technol, Dept Phys, CH-8093 Zurich, Switzerland. [Guo, Y.; Faber, S.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Guo, Y.; Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Ferguson, H. C.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dave, R.] Univ Western Cape, ZA-7535 Cape Town, South Africa. [Lu, Y.; Grogin, N.] Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94309 USA. [Ashby, M. L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dekel, A.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Kocevski, D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Somerville, R. S.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [White, C. E.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Duncan, K (reprint author), Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. EM ppxkd@nottingham.ac.uk OI Duncan, Kenneth/0000-0001-6889-8388; Koekemoer, Anton/0000-0002-6610-2048 FU CANDELS Multi- Cycle Treasury Program with the NASA/ESA HST; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA; ERC FX We thank the anonymous referee for their thorough review and help in greatly improving the paper. This work is based on observations taken by the CANDELS Multi- Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA. AM acknowledges funding via an ERC consolidator grant (PI: McLure). We would also like to acknowledge funding from the Science and Technology Facilities Council (STFC) and the Leverhulme Trust. NR 138 TC 66 Z9 66 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 NOV 1 PY 2014 VL 444 IS 3 BP 2960 EP 2984 DI 10.1093/mnras/stu1622 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR2FS UT WOS:000343399600072 ER PT J AU Zavala-Norzagaray, AA Ley-Quinonez, CP Espinosa-Carreon, TL Canizalez-Roman, A Hart, CE Aguirre, AA AF Zavala-Norzagaray, A. A. Ley-Quinonez, C. P. Espinosa-Carreon, T. L. Canizalez-Roman, A. Hart, C. E. Aguirre, A. A. TI Trace Elements in Blood of Sea Turtles Lepidochelys olivacea in the Gulf of California, Mexico SO BULLETIN OF ENVIRONMENTAL CONTAMINATION AND TOXICOLOGY LA English DT Article DE Heavy metals; Cadmium; Sea turtle Lepidochelys olivacea; Gulf of California, Mexico ID HEAVY-METAL ACCUMULATION; CHELONIA-MYDAS; BAJA-CALIFORNIA; CARETTA-CARETTA; MARINE TURTLES; MEDITERRANEAN SEA; ADRIATIC SEA; TISSUES; CADMIUM; GROWTH AB This study determined the concentrations of heavy metals in blood collected from Pacific Ridley sea turtles (Lepidochelys olivacea) inhabiting the coast of Guasave, Mexico, in the Gulf of California. The highest reported metal concentration in blood was Zn, followed by Se. Of nonessential toxic metals, As was reported in higher percentage compared to Cd. The concentrations of metals detected were present as follows: Zn > Se > Mn > As > Ni > Cd > Cu. Cd concentration in blood is higher in our population in comparison with other populations of L. olivacea, and even higher in other species of sea turtles. Our study reinforces the usefulness of blood for the monitoring of the levels of contaminating elements, and is easily accessible and nonlethal for sea turtles. C1 [Zavala-Norzagaray, A. A.; Espinosa-Carreon, T. L.] Inst Politecn Nacl, CIIDIR SINALOA, Guasave, Sinaloa, Mexico. [Zavala-Norzagaray, A. A.; Canizalez-Roman, A.] Univ Autonoma Sinaloa, Fac Ciencias Quim Biol, Programa Doctorado Biotecnol, Culiacan, Sinaloa, Mexico. [Zavala-Norzagaray, A. A.; Hart, C. E.] Grp Tortuguero Calif AC, La Paz, BCS, Mexico. [Ley-Quinonez, C. P.] Serv Salud Sinaloa, Lab Estatal Salud Publ, Culiacan, Mexico. [Canizalez-Roman, A.] Univ Autonoma Sinaloa, Fac Med, Culiacan, Sinaloa, Mexico. [Hart, C. E.] Univ Guadalajara, Ctr Univ Costa, Puerto Vallarta, Mexico. [Hart, C. E.] Red Tortuguera AC, Tepic, Nayarit, Mexico. [Aguirre, A. A.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Aguirre, A. A.] Smithsonian Mason Sch Conservat, Front Royal, VA USA. RP Zavala-Norzagaray, AA (reprint author), Inst Politecn Nacl, CIIDIR SINALOA, Guasave, Sinaloa, Mexico. EM anorzaga@ipn.mx FU IPN-CIIDIR SIN-ALOA; GRUPO TORTUGUERO; Universidad Autonoma de Sinaloa; EcoHealth Alliance; [IPN-SIP:20100363] FX This work was supported by IPN-CIIDIR SIN-ALOA, GRUPO TORTUGUERO, Universidad Autonoma de Sinaloa and EcoHealth Alliance (formerly known as Wildlife Trust). The first author acknowledges the participation of Rodolfo Ayon, Gaspar Angulo, Renato Leal and Carlos Romero. This research was performed under Mexican regulations and laws under permit provided by SEMARNAT (Secretaria de Medio Ambiente y Recursos Naturales) No. of permission SGPA/DGVS/03481/09. Partial funding was provided by Project IPN-SIP:20100363. NR 43 TC 3 Z9 3 U1 3 U2 31 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-4861 EI 1432-0800 J9 B ENVIRON CONTAM TOX JI Bull. Environ. Contam. Toxicol. PD NOV PY 2014 VL 93 IS 5 BP 536 EP 541 DI 10.1007/s00128-014-1320-8 PG 6 WC Environmental Sciences; Toxicology SC Environmental Sciences & Ecology; Toxicology GA AQ8AO UT WOS:000343043000006 PM 24957795 ER PT J AU Aylward, FO Suen, G Biedermann, PHW Adams, AS Scott, JJ Malfatti, SA del Rio, TG Tringe, SG Poulsen, M Raffa, KF Klepzig, KD Currie, CR AF Aylward, Frank O. Suen, Garret Biedermann, Peter H. W. Adams, Aaron S. Scott, Jarrod J. Malfatti, Stephanie A. del Rio, Tijana Glavina Tringe, Susannah G. Poulsen, Michael Raffa, Kenneth F. Klepzig, Kier D. Currie, Cameron R. TI Convergent Bacterial Microbiotas in the Fungal Agricultural Systems of Insects SO MBIO LA English DT Article ID LEAF-CUTTER ANTS; GUT MICROBIOTA; PHYLOGENETIC CLASSIFICATION; BARK BEETLES; GROWING ANTS; COMMUNITIES; DIVERSITY; HOST; DATABASE; GENES AB The ability to cultivate food is an innovation that has produced some of the most successful ecological strategies on the planet. Although most well recognized in humans, where agriculture represents a defining feature of civilization, species of ants, beetles, and termites have also independently evolved symbioses with fungi that they cultivate for food. Despite occurring across divergent insect and fungal lineages, the fungivorous niches of these insects are remarkably similar, indicating convergent evolution toward this successful ecological strategy. Here, we characterize the microbiota of ants, beetles, and termites engaged in nutritional symbioses with fungi to define the bacterial groups associated with these prominent herbivores and forest pests. Using culture-independent techniques and the in silico reconstruction of 37 composite genomes of dominant community members, we demonstrate that different insect-fungal symbioses that collectively shape ecosystems worldwide have highly similar bacterial microbiotas comprised primarily of the genera Enterobacter, Rahnella, and Pseudomonas. Although these symbioses span three orders of insects and two phyla of fungi, we show that they are associated with bacteria sharing high whole-genome nucleotide identity. Due to the fine-scale correspondence of the bacterial microbiotas of insects engaged in fungal symbioses, our findings indicate that this represents an example of convergence of entire host-microbe complexes. IMPORTANCE The cultivation of fungi for food is a behavior that has evolved independently in ants, beetles, and termites and has enabled many species of these insects to become ecologically important and widely distributed herbivores and forest pests. Although the primary fungal cultivars of these insects have been studied for decades, comparatively little is known of their bacterial microbiota. In this study, we show that diverse fungus-growing insects are associated with a common bacterial community composed of the same dominant members. Furthermore, by demonstrating that many of these bacteria have high whole-genome similarity across distantly related insect hosts that reside thousands of miles apart, we show that these bacteria are an important and underappreciated feature of diverse fungus-growing insects. Because of the similarities in the agricultural lifestyles of these insects, this is an example of convergence between both the life histories of the host insects and their symbiotic microbiota. C1 [Aylward, Frank O.; Suen, Garret; Scott, Jarrod J.; Currie, Cameron R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Aylward, Frank O.; Scott, Jarrod J.; Currie, Cameron R.] Univ Wisconsin, Dept Energy, Great Lakes Bioenergy Res Ctr, Madison, WI USA. [Biedermann, Peter H. W.] Max Planck Inst Chem Ecol, Insect Symbiosis Res Grp, Jena, Germany. [Adams, Aaron S.; Raffa, Kenneth F.] Univ Wisconsin, Dept Entomol, Madison, WI 53706 USA. [Scott, Jarrod J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Malfatti, Stephanie A.; del Rio, Tijana Glavina; Tringe, Susannah G.] Genome Inst, Dept Energy Joint, Walnut Creek, CA USA. [Poulsen, Michael] Univ Copenhagen, Sect Ecol & Evolut, Dept Biol, Copenhagen, Denmark. [Klepzig, Kier D.] US Forest Serv, USDA, Sourth Res Stn, Asheville, NC USA. RP Aylward, FO (reprint author), Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. EM faylward@hawaii.edu; currie@bact.wisc.edu RI Biedermann, Peter/E-3641-2013; OI Biedermann, Peter/0000-0003-4234-5659; Tringe, Susannah/0000-0001-6479-8427; Suen, Garret/0000-0002-6170-711X; Poulsen, Michael/0000-0002-2839-1715 FU Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; USDA NRI [2008-02438]; National Science Foundation [DEB-0747002, MCB-0702025, MCB-0731822]; DOE Great Lakes Bioenergy Research Center (DOE Office of Science BER) [DE-FC02-07ER64494]; SNSF [PB-BEP3_141472]; STENO grant from The Danish Council for Independent Research-Natural Sciences FX This work was supported by the Office of Science of the U.S. Department of Energy under contract no. DE-AC02-05CH11231, the USDA NRI (2008-02438), National Science Foundation grants DEB-0747002, MCB-0702025, and MCB-0731822 to C.R.C., and the DOE Great Lakes Bioenergy Research Center (DOE Office of Science BER DE-FC02-07ER64494). P.H.W.B. was funded by an SNSF postdoctoral research grant (PB-BEP3_141472), and M.P. was supported by a STENO grant from The Danish Council for Independent Research-Natural Sciences. NR 78 TC 13 Z9 13 U1 5 U2 13 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 2150-7511 J9 MBIO JI mBio PD NOV-DEC PY 2014 VL 5 IS 6 AR e02077-14 DI 10.1128/mBio.02077-14 PG 10 WC Microbiology SC Microbiology GA AX7CE UT WOS:000347073600038 PM 25406380 ER PT J AU Aich, V Zimmermann, A Elsenbeer, H AF Aich, Valentin Zimmermann, Alexander Elsenbeer, Helmut TI Quantification and interpretation of suspended-sediment discharge hysteresis patterns: How much data do we need? SO CATENA LA English DT Article DE Suspended sediment; Hysteresis index; Sediment monitoring; Overland flow; Tropical forest ID OVERLAND-FLOW GENERATION; BARRO COLORADO ISLAND; RAIN-FOREST CATCHMENT; MICRO-TOPOGRAPHY; DRAINAGE-BASIN; DYNAMICS; TRANSPORT; EROSION; RIVER; RUNOFF AB Sediment-discharge hysteresis loops are frequently analyzed to facilitate the understanding of sediment transport processes. Hysteresis patterns, however, are often complex and their interpretation can be complicated. Particularly, quantifying hysteresis patterns remains a problematic issue. Moreover, it is currently unknown how much data is required for analyzing sediment-discharge hysteresis loops in a given area. These open questions and challenges motivated us to develop a new method for quantifying suspended-sediment hysteresis. Subsequently, we applied the new hysteresis index to three suspended-sediment and discharge datasets from a small tropical rainforest catchment. The datasets comprised a different number of events and sampling sites. Our analyses show three main findings: (1) datasets restricted to only few events, which is typical for rapid assessment surveys, were always sufficient to identify the dominating hysteresis pattern in our research area. Furthermore, some of these small datasets contained multiple-peak events that allowed identifying intra-event exhaustion effects and hence, limitations in sediment supply. (2) Datasets comprising complete hydrological years were particularly useful for analyzing seasonal dynamics of hysteresis. These analyses revealed an exhaustion of hysteresis on the inter-event scale which also points to a limited sediment supply. (3) Datasets comprising measurements from two consecutive gauges installed at the catchment outlet and on a slope within that catchment allowed analyzing the change of hysteresis patterns along the flowpath. On the slope, multiple-peak events showed a stronger intra-event exhaustion of hysteresis than at the catchment outlet. Furthermore, exhaustion of hysteresis on the inter-event scale was not evident on the slope but occurred at the catchment outlet. Our results indicate that even small sediment datasets can provide valuable insights into sediment transport processes of small catchments. Furthermore, our results may serve as a first guideline on what to expect from an analysis of hysteresis patterns for datasets of varying quality and quantity. (c) 2014 Elsevier B.V. All rights reserved. C1 [Aich, Valentin; Zimmermann, Alexander; Elsenbeer, Helmut] Univ Potsdam, Inst Earth & Environm Sci, D-14476 Potsdam, Germany. [Elsenbeer, Helmut] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Aich, V (reprint author), Potsdam Inst Climate Impact Res PIK, POB 60 12 03, D-14412 Potsdam, Germany. EM aich@pik-potsdam.de RI Zimmermann, Alexander/B-6831-2011 FU German Research Foundation [El 255/6-1]; STRI FX This research was funded by the German Research Foundation (El 255/6-1). H.E. acknowledges STRI's support during his sabbatical in 2008 on BCI. We wish to thank Oris Acevedo (Smithsonian Tropical Research Institute, STRI) for exceptional logistical support, Sergio dos Santos (STRI) for providing rainfall data, and Simon Horhold and Anna Schurkmann for participating in the field work. Furthermore, we thank three anonymous reviewers for their constructive comments on an earlier version of this manuscript NR 37 TC 9 Z9 9 U1 12 U2 80 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0341-8162 EI 1872-6887 J9 CATENA JI Catena PD NOV PY 2014 VL 122 BP 120 EP 129 DI 10.1016/j.catena.2014.06.020 PG 10 WC Geosciences, Multidisciplinary; Soil Science; Water Resources SC Geology; Agriculture; Water Resources GA AO4ZK UT WOS:000341349700011 ER PT J AU Kobayashi, K Cirtain, J Winebarger, AR Korreck, K Golub, L Walsh, RW De Pontieu, B DeForest, C Title, A Kuzin, S Savage, S Beabout, D Beabout, B Podgorski, W Caldwell, D McCracken, K Ordway, M Bergner, H Gates, R McKillop, S Cheimets, P Platt, S Mitchell, N Windt, D AF Kobayashi, Ken Cirtain, Jonathan Winebarger, Amy R. Korreck, Kelly Golub, Leon Walsh, Robert W. De Pontieu, Bart DeForest, Craig Title, Alan Kuzin, Sergey Savage, Sabrina Beabout, Dyana Beabout, Brent Podgorski, William Caldwell, David McCracken, Kenneth Ordway, Mark Bergner, Henry Gates, Richard McKillop, Sean Cheimets, Peter Platt, Simon Mitchell, Nick Windt, David TI The High-Resolution Coronal Imager (Hi-C) SO SOLAR PHYSICS LA English DT Article DE Solar corona; Solar instrumentation; Solar imaging; Extreme ultraviolet ID SOLAR CORONA; REGION; LOOPS; DYNAMICS; MOSS; RECONNECTION; HINODE; SKYLAB; ENERGY; SCALE AB The High-Resolution Coronal Imager (Hi-C) was flown on a NASA sounding rocket on 11 July 2012. The goal of the Hi-C mission was to obtain high-resolution (a parts per thousand aEuro parts per thousand 0.3 -aEuro parts per thousand 0.4''), high-cadence (a parts per thousand aEuro parts per thousand 5 seconds) images of a solar active region to investigate the dynamics of solar coronal structures at small spatial scales. The instrument consists of a normal-incidence telescope with the optics coated with multilayers to reflect a narrow wavelength range around 19.3 nm (including the Fe xii 19.5-nm spectral line) and a 4096x4096 camera with a plate scale of 0.1''aEuro parts per thousand pixel(-1). The target of the Hi-C rocket flight was Active Region 11520. Hi-C obtained 37 full-frame images and 86 partial-frame images during the rocket flight. Analysis of the Hi-C data indicates the corona is structured on scales smaller than currently resolved by existing satellite missions. C1 [Kobayashi, Ken] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA. [Kobayashi, Ken; Cirtain, Jonathan; Winebarger, Amy R.; Savage, Sabrina; Beabout, Dyana; Beabout, Brent] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Korreck, Kelly; Golub, Leon; Podgorski, William; Caldwell, David; McCracken, Kenneth; Ordway, Mark; Bergner, Henry; Gates, Richard; McKillop, Sean; Cheimets, Peter] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walsh, Robert W.; Platt, Simon; Mitchell, Nick] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England. [De Pontieu, Bart; Title, Alan] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [DeForest, Craig] Southwest Res Inst, Boulder, CO 80302 USA. [Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia. [Windt, David] Reflect Xray Opt LLC, New York, NY 10027 USA. RP Kobayashi, K (reprint author), NASA, George C Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35812 USA. EM ken.kobayashi-1@nasa.gov RI Kuzin, Sergey/M-3435-2015; OI Korreck, Kelly/0000-0001-6095-2490 FU NASA's Low Cost Access to Space program; Presidium of the RAS [22] FX We acknowledge the High-Resolution Coronal Imager instrument grant funded by the NASA's Low Cost Access to Space program. MSFC/NASA led the mission and partners include the Smithsonian Astrophysical Observatory in Cambridge, MA, USA; Lockheed Martin's Solar Astrophysical Laboratory in Palo Alto, CA, USA; the University of Central Lancashire in Lancashire, England; and the Lebedev Physical Institute of the Russian Academy of Sciences in Moscow, Russia. LPI was supported by the Program no. 22 of the Presidium of the RAS. NR 29 TC 19 Z9 19 U1 0 U2 6 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 NOV PY 2014 VL 289 IS 11 BP 4393 EP 4412 DI 10.1007/s11207-014-0544-4 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO6YW UT WOS:000341499800020 ER PT J AU Boyle, MJ Yamaguchi, E Seaver, EC AF Boyle, Michael J. Yamaguchi, Emi Seaver, Elaine C. TI Molecular conservation of metazoan gut formation: evidence from expression of endomesoderm genes in Capitella teleta (Annelida) SO EVODEVO LA English DT Article DE endoderm; digestive system; gut development; kernel; hybridization; spiralian ID INDIRECTLY DEVELOPING POLYCHAETE; MOLLUSK PATELLA-VULGATA; SEA-URCHIN EMBRYO; REGULATORY NETWORK ARCHITECTURE; GATA TRANSCRIPTION FACTORS; NK-2 HOMEOBOX GENE; SP-I; CAENORHABDITIS-ELEGANS; DEVELOPMENTAL EXPRESSION; JUVENILE DEVELOPMENT AB Background: Metazoan digestive systems develop from derivatives of ectoderm, endoderm and mesoderm, and vary in the relative contribution of each germ layer across taxa and between gut regions. In a small number of well-studied model systems, gene regulatory networks specify endoderm and mesoderm of the gut within a bipotential germ layer precursor, the endomesoderm. Few studies have examined expression of endomesoderm genes outside of those models, and thus, it is unknown whether molecular specification of gut formation is broadly conserved. In this study, we utilize a sequenced genome and comprehensive fate map to correlate the expression patterns of six transcription factors with embryonic germ layers and gut subregions during early development in Capitella teleta. Results: The genome of C. teleta contains the five core genes of the sea urchin endomesoderm specification network. Here, we extend a previous study and characterize expression patterns of three network orthologs and three additional genes by in situ hybridization during cleavage and gastrulation stages and during formation of distinct gut subregions. In cleavage stage embryos, Ct-otx, Ct-blimp1, Ct-bra and Ct-nkx2.1a are expressed in all four macromeres, the endoderm precursors. Ct-otx, Ct-blimp1, and Ct-nkx2.1a are also expressed in presumptive endoderm of gastrulae and later during midgut development. Additional gut-specific expression patterns include Ct-otx, Ct-bra, Ct-foxAB and Ct-gsc in oral ectoderm; Ct-otx, Ct-blimp1, Ct-bra and Ct-nkx2.1a in the foregut; and both Ct-bra and Ct-nkx2.1a in the hindgut. Conclusions: Identification of core sea urchin endomesoderm genes in C. teleta indicates they are present in all three bilaterian superclades. Expression of Ct-otx, Ct-blimp1 and Ct-bra, combined with previously published Ct-foxA and Ct-gataB1 patterns, provide the most comprehensive comparison of these five orthologs from a single species within Spiralia. Each ortholog is likely involved in endoderm specification and midgut development, and several may be essential for establishment of the oral ectoderm, foregut and hindgut, including specification of ectodermal and mesodermal contributions. When the five core genes are compared across the Metazoa, their conserved expression patterns suggest that ` gut gene' networks evolved to specify distinct digestive system subregions, regardless of species-specific differences in gut architecture or germ layer contributions within each subregion. C1 [Boyle, Michael J.] Smithsonian Trop Res Inst, Naos Isl Lab, Panama City, Panama. [Yamaguchi, Emi] Univ Hawaii, PBRC, Kewalo Marine Lab, Honolulu, HI 96813 USA. [Seaver, Elaine C.] Univ Florida, Whitney Lab Marine Biosci, Augustine, FL 32080 USA. RP Seaver, EC (reprint author), Univ Florida, Whitney Lab Marine Biosci, 9505 Ocean Shore Blvd St, Augustine, FL 32080 USA. EM seaver@whitney.ufl.edu FU National Science Foundation [NSF EF05-31558, NSF IOB05-44869] FX We thank the following people for cloning and initial expression screening of C. teleta genes: Katrin Thamm (Ct-otx, Ct-nkx2.1a), Kariena Dill (Ct-bra), Olivia Veatch (Ct-nkx2.1a), Andreas Hejnol (Ct-gsc), and Danielle de Jong for Ct-nkx2.1b expression screening. We are grateful to the staff and facilities management of Kewalo Marine Laboratory at the University of Hawaii at Manoa, and the Smithsonian Marine Station at Fort Pierce, Florida. MJB is grateful to Andreas Hejnol for many thoughtful discussions of gut-related gene expression in Metazoa. The National Science Foundation supported this work (ECS as a co-PI for NSF EF05-31558, and as PI for NSF IOB05-44869). This publication is Smithsonian Marine Station contribution no. 964. NR 112 TC 12 Z9 12 U1 1 U2 13 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2041-9139 J9 EVODEVO JI EvoDevo PD OCT 29 PY 2014 VL 5 AR 39 DI 10.1186/2041-9139-5-39 PG 19 WC Evolutionary Biology; Developmental Biology SC Evolutionary Biology; Developmental Biology GA AW5JG UT WOS:000346311100001 PM 25908956 ER PT J AU Alves, OC Srygley, RB Riveros, AJ Barbosa, MA Esquivel, DMS Wajnberg, E AF Alves, Odivaldo C. Srygley, Robert B. Riveros, Andre J. Barbosa, Marcia A. Esquivel, Darci M. S. Wajnberg, Eliane TI Magnetic anisotropy and organization of nanoparticles in heads and antennae of neotropical leaf-cutter ants, Atta colombica SO JOURNAL OF PHYSICS D-APPLIED PHYSICS LA English DT Article DE magnetic characterization; magnetic sensor; spatial orientation; homing ID IRON-OXIDE NANOPARTICLES; APIS-MELLIFERA; FIELD; RESONANCE; MAGNETORECEPTION; ORIENTATION; NAVIGATION; DETECT; SCANS; BIRDS AB Oriented magnetic nanoparticles have been suggested as a good candidate for a magnetic sensor in ants. Behavioural evidence for a magnetic compass in neotropical leaf-cutter ants, Atta colombica (Formicidae: Attini), motivated a study of the arrangement of magnetic particles in the ants' four major body parts by measuring the angular dependence of the ferromagnetic resonance spectra at room temperature. Spectra of the thoraces and those of the abdomens showed no significant angular dependence, while those of the antennae and those of the heads exhibited a periodic dependence relative to the magnetic field. Fitting of the angular dependence of the resonant field resulted in an unexpected magnetic anisotropy with uniaxial symmetry. High values of the first order anisotropy constant were observed for the magnetic material in antennae (-2.9 x 10(5) erg cm(-3)) and heads (-1 x 10(6) erg cm(-3)) as compared to body parts of other social insects. In addition, the magnitude of the anisotropy in the heads was comparable to that observed in magnetite nanoparticles of 4-5 nm diameter. For the antennae, the mean angle of the particles' easy magnetization axis (EA) was estimated to be 41 degrees relative to the straightened antenna's long axis. For the heads, EA was approximately 60 degrees relative to the head's axis running from midway between the spines to the clypeus. These physical characteristics indicate organized magnetic nanoparticles with a potential for directional sensitivity, which is an important feature of magnetic compasses. C1 [Alves, Odivaldo C.] Univ Fed Fluminense, Inst Quim, Dept Fis Quim, BR-24020150 Niteroi, RJ, Brazil. [Barbosa, Marcia A.; Esquivel, Darci M. S.; Wajnberg, Eliane] Ctr Brasileiro Pesquisas Fis, BR-22290180 Rio De Janeiro, RJ, Brazil. [Srygley, Robert B.] USDA ARS, Northern Plains Agr Res Lab, Sidney, MT 59270 USA. [Srygley, Robert B.] Smithsonian Trop Res Inst, Balboa, Panama. [Riveros, Andre J.] Pontificia Univ Javeriana, Fac Med, Dept Ciencias Fisiol, Bogota, Colombia. RP Alves, OC (reprint author), Univ Fed Fluminense, Inst Quim, Dept Fis Quim, Outeiro Sao Joao Batista S-N, BR-24020150 Niteroi, RJ, Brazil. EM elianew@cbpf.br FU Centro Brasileiro de Pesquisas Fisicas (CBPF) of the Ministerio da Ciencia, Tecnologia e Inovacao (MCTI); National Geographic Society Committee for Research and Exploration; US Department of Agriculture; Smithsonian Tropical Research Institute; National Science Foundation FX We thank the Autoridad Nacional del Ambiente (ANAM) of the Republic of Panama for permission to export ants to Brazil for physical analysis. This project was supported in part by Centro Brasileiro de Pesquisas Fisicas (CBPF) of the Ministerio da Ciencia, Tecnologia e Inovacao (MCTI), the National Geographic Society Committee for Research and Exploration, the US Department of Agriculture and the Smithsonian Tropical Research Institute. AJR received support from National Science Foundation. NR 37 TC 0 Z9 0 U1 5 U2 34 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0022-3727 EI 1361-6463 J9 J PHYS D APPL PHYS JI J. Phys. D-Appl. Phys. PD OCT 29 PY 2014 VL 47 IS 43 AR 435401 DI 10.1088/0022-3727/47/43/435401 PG 7 WC Physics, Applied SC Physics GA AQ9EN UT WOS:000343150500021 ER PT J AU Gacesa, M Kharchenko, V AF Gacesa, Marko Kharchenko, Vasili TI Quantum reactive scattering of O(P-3)+H-2 at collision energies up to 4.4 eV SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID LASER-ABSORPTION SPECTROSCOPY; VIBRATIONALLY EXCITED H-2; BORN-OPPENHEIMER APPROXIMATION; ATOMIC OXYGEN; RATE-CONSTANT; REACTION DYNAMICS; RATE COEFFICIENT; HIGH-TEMPERATURE; REDUCED DIMENSIONALITY; REACTION PROBABILITIES AB We report the results of quantum scattering calculations for the O(P-3)+H-2 reaction for a range of collision energies from 0.4 to 4.4 eV, important for astrophysical and atmospheric processes. The total and state-to-state reactive cross sections are calculated using a fully quantum time-independent coupled-channel approach on recent potential energy surfaces of 3A' and 3A" symmetry. A larger basis set than in the previous studies was used to ensure single-surface convergence at higher energies. Our results agree well with the published data at lower energies and indicate the breakdown of reduced dimensionality approach at collision energies higher than 1.5 eV. Differential cross sections and momentum transfer cross sections are also reported. (C) 2014 AIP Publishing LLC. C1 [Gacesa, Marko; Kharchenko, Vasili] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Kharchenko, Vasili] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Gacesa, M (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM gacesa@phys.uconn.edu; kharchenko@phys.uconn.edu RI Gacesa, Marko/F-8027-2011 OI Gacesa, Marko/0000-0001-5145-051X FU NASA [NNX10AB88G] FX We are grateful to the authors of the respective studies for providing the Fortran subroutines for calculating the potential energy surfaces. This work was supported by NASA Grant No. NNX10AB88G. NR 85 TC 2 Z9 2 U1 2 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 OCT 28 PY 2014 VL 141 IS 16 AR 164324 DI 10.1063/1.4899179 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AS9WQ UT WOS:000344589700053 PM 25362316 ER PT J AU Martinez-Garcia, R Calabrese, JM Hernandez-Garcia, E Lopez, C AF Martinez-Garcia, Ricardo Calabrese, Justin M. Hernandez-Garcia, Emilio Lopez, Cristobal TI Minimal mechanisms for vegetation patterns in semiarid regions SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY A-MATHEMATICAL PHYSICAL AND ENGINEERING SCIENCES LA English DT Article DE vegetation patterns; non-local interactions; competitive interactions ID TIGER BUSH; FACILITATION; COMPETITION; EQUATION; ORIGIN; MODEL AB The minimal ecological requirements for the formation of regular vegetation patterns in semiarid systems have been recently questioned. Against the general belief that a combination of facilitative and competitive interactions is necessary, recent theoretical studies suggest that, under broad conditions, non-local competition among plants alone may induce patterns. In this paper, we review results along this line, presenting a series of models that yield spatial patterns when finite-range competition is the only driving force. A preliminary derivation of this type of model from a more detailed one that considers water-biomass dynamics is also presented. C1 [Martinez-Garcia, Ricardo; Hernandez-Garcia, Emilio; Lopez, Cristobal] IFISC CSIC UIB, Inst Fis Interdisciplinar & Sistemas Complejos, Palma De Mallorca 07122, Spain. [Calabrese, Justin M.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. RP Lopez, C (reprint author), IFISC CSIC UIB, Inst Fis Interdisciplinar & Sistemas Complejos, Campus Univ Illes Balears, Palma De Mallorca 07122, Spain. EM clopez@ifisc.uib-csic.es RI Hernandez-Garcia, Emilio/B-1271-2008; Calabrese, Justin/B-9131-2012; OI Hernandez-Garcia, Emilio/0000-0002-9568-8287; Lopez, Cristobal/0000-0002-3445-4284; Martinez-Garcia, Ricardo/0000-0003-2765-8147 FU FEDER; MINECO (Spain) [FIS2012-30634 INTENSE@COSYP, CTM2012-39025-C02-01 ESCOLA]; CSIC FX R.M.-G., C. L. and E. H.-G. acknowledge support from FEDER and MINECO (Spain) through grant nos. FIS2012-30634 INTENSE@COSYP and CTM2012-39025-C02-01 ESCOLA. R. M.-G. is supported by the JAEPredoc program of CSIC. NR 25 TC 5 Z9 5 U1 0 U2 13 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1364-503X EI 1471-2962 J9 PHILOS T R SOC A JI Philos. Trans. R. Soc. A-Math. Phys. Eng. Sci. PD OCT 28 PY 2014 VL 372 IS 2027 SI SI AR 20140068 DI 10.1098/rsta.2014.0068 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ4EH UT WOS:000342745400017 ER PT J AU Knap, M Sau, JD Halperin, BI Demler, E AF Knap, Michael Sau, Jay D. Halperin, Bertrand I. Demler, Eugene TI Transport in Two-Dimensional Disordered Semimetals SO PHYSICAL REVIEW LETTERS LA English DT Article ID METAL-INSULATOR-TRANSITION; HGTE QUANTUM-WELLS; 2 DIMENSIONS; PERCOLATION; CONDUCTIVITY; B=0 AB We theoretically study transport in two-dimensional semimetals. Typically, electron and hole puddles emerge in the transport layer of these systems due to smooth fluctuations in the potential. We calculate the electric response of the electron-hole liquid subject to zero and finite perpendicular magnetic fields using an effective medium approximation and a complementary mapping on resistor networks. In the presence of smooth disorder and in the limit of a weak electron-hole recombination rate, we find for small but finite overlap of the electron and hole bands an abrupt upturn in resistivity when lowering the temperature but no divergence at zero temperature. We discuss how this behavior is relevant for several experimental realizations and introduce a simple physical explanation for this effect. C1 [Knap, Michael; Sau, Jay D.; Halperin, Bertrand I.; Demler, Eugene] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Sau, Jay D.] Univ Maryland, Condensed Matter Theory Ctr, Dept Phys, College Pk, MD 20742 USA. [Sau, Jay D.] Univ Maryland, Joint Quantum Inst, College Pk, MD 20742 USA. RP Knap, M (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM knap@physics.harvard.edu RI Knap, Michael/H-3344-2011 OI Knap, Michael/0000-0002-7093-9502 FU Harvard-MIT CUA; ARO-MURI Quism program; ARO-MURI on Atomtronics; STC Center for Integrated Quantum Materials; NSF [DMR-1231319]; Austrian Science Fund (FWF) Project [J 3361-N20] FX We thank D. Kvon for introducing us to this problem and for sharing experimental results prior to publication. The authors acknowledge support from Harvard-MIT CUA, ARO-MURI Quism program, ARO-MURI on Atomtronics, STC Center for Integrated Quantum Materials, NSF Grant No. DMR-1231319, as well as the Austrian Science Fund (FWF) Project No. J 3361-N20. NR 28 TC 6 Z9 6 U1 4 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 27 PY 2014 VL 113 IS 18 AR 186801 DI 10.1103/PhysRevLett.113.186801 PG 5 WC Physics, Multidisciplinary SC Physics GA CA2HC UT WOS:000348728400003 PM 25396385 ER PT J AU Pimiento, C Clements, CF AF Pimiento, Catalina Clements, Christopher F. TI When Did Carcharocles megalodon Become Extinct? A New Analysis of the Fossil Record SO PLOS ONE LA English DT Article ID CONFIDENCE-INTERVALS; SIGHTING RECORD; SHARKS; MYSTICETI; ACCURACY; CETACEA; RANGES; WHALE; RAYS AB Carcharocles megalodon ("Megalodon") is the largest shark that ever lived. Based on its distribution, dental morphology, and associated fauna, it has been suggested that this species was a cosmopolitan apex predator that fed on marine mammals from the middle Miocene to the Pliocene (15.9-2.6 Ma). Prevailing theory suggests that the extinction of apex predators affects ecosystem dynamics. Accordingly, knowing the time of extinction of C. megalodon is a fundamental step towards understanding the effects of such an event in ancient communities. However, the time of extinction of this important species has never been quantitatively assessed. Here, we synthesize the most recent records of C. megalodon from the literature and scientific collections and infer the date of its extinction by making a novel use of the Optimal Linear Estimation (OLE) model. Our results suggest that C. megalodon went extinct around 2.6 Ma. Furthermore, when contrasting our results with known ecological and macroevolutionary trends in marine mammals, it became evident that the modern composition and function of modern gigantic filter-feeding whales was established after the extinction of C. megalodon. Consequently, the study of the time of extinction of C. megalodon provides the basis to improve our understanding of the responses of marine species to the removal of apex predators, presenting a deep-time perspective for the conservation of modern ecosystems. C1 [Pimiento, Catalina] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Pimiento, Catalina] Univ Florida, Dept Biol, Gainesville, FL USA. [Pimiento, Catalina] Smithsonian Trop Res Inst, Balboa, Panama. [Clements, Christopher F.] Univ Zurich, Inst Evolutionary Biol & Environm Studies, Zurich, Switzerland. RP Pimiento, C (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM pimientoc@ufl.edu FU National Science Foundation NSF [EAR 0418042, PIRE 0966884] FX This project was funded by the National Science Foundation NSF EAR 0418042, PIRE 0966884 (http://www.nsf.gov/funding). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 32 TC 12 Z9 12 U1 9 U2 51 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 22 PY 2014 VL 9 IS 10 AR e111086 DI 10.1371/journal.pone.0111086 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AR6DY UT WOS:000343674800104 PM 25338197 ER PT J AU Mitchell, RM Bakker, JD AF Mitchell, Rachel M. Bakker, Jonathan D. TI Intraspecific Trait Variation Driven by Plasticity and Ontogeny in Hypochaeris radicata SO PLOS ONE LA English DT Article ID PLANT FUNCTIONAL TRAITS; LIFE-HISTORY TRAITS; PHENOTYPIC PLASTICITY; LEAF TRAITS; TRANSGENERATIONAL PLASTICITY; LOCAL ADAPTATION; BETA-DIVERSITY; VARIABILITY; ASTERACEAE; WORLDWIDE AB The importance of intraspecific variation in plant functional traits for structuring communities and driving ecosystem processes is increasingly recognized, but mechanisms governing this variation are less studied. Variation could be due to adaptation to local conditions, plasticity in observed traits, or ontogeny. We investigated 1) whether abiotic stress caused individuals, maternal lines, and populations to exhibit trait convergence, 2) whether trait variation was primarily due to ecotypic differences or trait plasticity, and 3) whether traits varied with ontogeny. We sampled three populations of Hypochaeris radicata that differed significantly in rosette diameter and specific leaf area (SLA). We grew nine maternal lines from each population (27 lines total) under three greenhouse conditions: ambient conditions (control), 50% drought, or 80% shade. Plant diameter and relative chlorophyll content were measured throughout the experiment, and leaf shape, root: shoot ratio, and SLA were measured after five weeks. We used hierarchical mixed-models and variance component analysis to quantify differences in treatment effects and the contributions of population of origin and maternal line to observed variation. Observed variation in plant traits was driven primarily by plasticity. Shade significantly influenced all measured traits. Plant diameter was the only trait that had a sizable proportion of trait variation (30%) explained by population of origin. There were significant ontogenetic differences for both plant diameter and relative chlorophyll content. When subjected to abiotic stress in the form of light or water limitation, Hypochaeris radicata exhibited significant trait variability. This variation was due primarily to trait plasticity, rather than to adaptation to local conditions, and also differed with ontogeny. C1 [Mitchell, Rachel M.; Bakker, Jonathan D.] Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. [Bakker, Jonathan D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Mitchell, RM (reprint author), Univ Washington, Sch Environm & Forest Sci, Seattle, WA 98195 USA. EM rmm57@duke.edu NR 68 TC 3 Z9 3 U1 6 U2 43 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 21 PY 2014 VL 9 IS 10 AR e109870 DI 10.1371/journal.pone.0109870 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AR7AB UT WOS:000343731200020 PM 25333738 ER PT J AU Vogelsberger, M Genel, S Springel, V Torrey, P Sijacki, D Xu, DD Snyder, G Nelson, D Hernquist, L AF Vogelsberger, Mark Genel, Shy Springel, Volker Torrey, Paul Sijacki, Debora Xu, Dandan Snyder, Greg Nelson, Dylan Hernquist, Lars TI Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; cosmology: theory ID MOVING-MESH COSMOLOGY; HALO MASS FUNCTION; ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; EXTRAGALACTIC LEGACY SURVEY; SUPERMASSIVE BLACK-HOLES; GALAXY FORMATION PHYSICS; TULLY-FISHER RELATION; STAR-FORMATION; SCALING RELATIONS AB We introduce the Illustris Project, a series of large-scale hydrodynamical simulations of galaxy formation. The highest resolution simulation, Illustris-1, covers a volume of (106.5 Mpc)(3), has a dark mass resolution of 6.26 x 10(6) M-circle dot, and an initial baryonic matter mass resolution of 1.26 x 10(6) M-circle dot. At z = 0 gravitational forces are softened on scales of 710 pc, and the smallest hydrodynamical gas cells have an extent of 48 pc. We follow the dynamical evolution of 2 x 1820(3) resolution elements and in addition passively evolve 1820(3) Monte Carlo tracer particles reaching a total particle count of more than 18 billion. The galaxy formation model includes: primordial and metal-line cooling with self-shielding corrections, stellar evolution, stellar feedback, gas recycling, chemical enrichment, supermassive black hole growth, and feedback from active galactic nuclei. Here we describe the simulation suite, and contrast basic predictions of our model for the present-day galaxy population with observations of the local universe. At z = 0 our simulation volume contains about 40 000 well-resolved galaxies covering a diverse range of morphologies and colours including early-type, late-type and irregular galaxies. The simulation reproduces reasonably well the cosmic star formation rate density, the galaxy luminosity function, and baryon conversion efficiency at z = 0. It also qualitatively captures the impact of galaxy environment on the red fractions of galaxies. The internal velocity structure of selected well-resolved disc galaxies obeys the stellar and baryonic Tully-Fisher relation together with flat circular velocity curves. In the well-resolved regime, the simulation reproduces the observed mix of early-type and late-type galaxies. Our model predicts a halo mass dependent impact of baryonic effects on the halo mass function and the masses of haloes caused by feedback from supernova and active galactic nuclei. C1 [Vogelsberger, Mark] MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Genel, Shy; Torrey, Paul; Nelson, Dylan; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, Volker; Xu, Dandan] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, D-69120 Heidelberg, Germany. [Sijacki, Debora] Kavli Inst Cosmol, Cambridge, England. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Snyder, Greg] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Vogelsberger, M (reprint author), MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. EM mvogelsb@mit.edu OI Torrey, Paul/0000-0002-5653-0786 FU DFG Research Centre [SFB-881]; European Research Council [ERC-StG EXAGAL-308037]; HST grants programme [HST-AR-12856.01-A]; NASA through Space Telescope Science Institute [12856]; NASA [NAS 5-26555, NNX12AC67G]; NSF [AST-1312095]; Alexander von Humboldt Foundation; PRACE project [RA0844]; [pr85je] FX MV thanks Qi Guo and Federico Marinacci for providing data. VS acknowledges support by the DFG Research Centre SFB-881 'The Milky Way System' through project A1, and by the European Research Council under ERC-StG EXAGAL-308037. GS acknowledges support from the HST grants programme number HST-AR-12856.01-A. Support for programme #12856 (PI: Lotz) 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. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. DX acknowledges support from the Alexander von Humboldt Foundation. Simulations were run on the Harvard Odyssey and CfA/ITC clusters, the Ranger and Stampede supercomputers at the Texas Advanced Computing Center as part of XSEDE, the Kraken supercomputer at Oak Ridge National Laboratory as part of XSEDE, the CURIE supercomputer at CEA/France as part of PRACE project RA0844, and the Super-MUC computer at the Leibniz Computing Centre, Germany, as part of project pr85je. NR 137 TC 273 Z9 274 U1 3 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 OCT 21 PY 2014 VL 444 IS 2 BP 1518 EP 1547 DI 10.1093/mnras/stu1536 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6MF UT WOS:000342926300038 ER PT J AU Greif, TH AF Greif, Thomas H. TI Multifrequency radiation hydrodynamics simulations of H-2 line emission in primordial, star-forming clouds SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; radiative transfer; stars: Population III; galaxies: high-redshift; cosmology: theory; early Universe ID MOLECULAR-HYDROGEN; MOVING-MESH; 1ST STARS; SOBOLEV APPROXIMATION; EARLY UNIVERSE; GAS; FRAGMENTATION; PROTOSTARS; PHOTODISSOCIATION; INSTABILITY AB We investigate the collapse of primordial gas in a minihalo with three-dimensional radiation hydrodynamics simulations that accurately model the transfer of H-2 line emission. For this purpose, we have implemented a multiline, multifrequency ray-tracing scheme in the moving-mesh code AREPO that is capable of adaptively refining rays based on the HEALPIX algorithm, as well as a hybrid equilibrium/ non-equilibrium primordial chemistry solver. We find that a multifrequency treatment of the individual H-2 lines is essential, since for high optical depths the smaller cross-section in the wings of the lines greatly increases the amount of energy that can escape. The influence of Doppler shifts due to bulk velocities is comparatively small, since systematic velocity differences in the cloud are typically smaller than the sound speed. During the initial collapse phase, the radially averaged escape fraction agrees relatively well with the fit of Ripamonti & Abel. However, in general it is not advisable to use a simple density-dependent fitting function, since the escape fraction depends on many factors and does not capture the suppression of density perturbations due to the diffusion of radiation. The Sobolev method overestimates the escape fraction by more than an order of magnitude, since the properties of the gas change on scales smaller than the Sobolev length. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Greif, TH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM tgreif@cfa.harvard.edu NR 56 TC 10 Z9 10 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 21 PY 2014 VL 444 IS 2 BP 1566 EP 1583 DI 10.1093/mnras/stu1532 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6MF UT WOS:000342926300041 ER PT J AU Johnson, CB Hynes, RI Maccarone, T Britt, CT Davis, H Jonker, PG Torres, MAP Steeghs, D Greiss, S Nelemans, G AF Johnson, Christopher B. Hynes, R. I. Maccarone, T. Britt, C. T. Davis, H., III Jonker, P. G. Torres, M. A. P. Steeghs, D. Greiss, S. Nelemans, G. TI HD 314884: a slowly pulsating B star in a close binary SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: pulsations; X-rays: binaries ID NEUTRON-STAR; MASS-DISTRIBUTION; BLACK-HOLE; RAY; ASTEROSEISMOLOGY; IDENTIFICATION; PARAMETERS; CATALOG AB We present the results of a spectroscopic and photometric analysis of HD 314884, a slowly pulsating B star (SPB) in a binary system with detected soft-X-ray emission. We spectrally classify the B star as a B5V-B6V star with T-eff = 15 490 +/- 310 K, log g = 3.75 +/- 0.25 dex, and a photometric period of P-0 = 0.889 521(12) d. A spectroscopic period search reveals an orbital period for the system of P-orb = 1.3654(11) d. The discrepancy in the two periods and the identification of a second and third distinct frequency in the photometric Fourier transform at P-1 = 3.1347(56) and P-2 = 1.517(28) d provides evidence that HD 314884 is an SPB with at least three oscillation frequencies. These frequencies appear to originate from higher order, non-linear tidal pulsations. Using the dynamical parameters obtained from the radial-velocity curve, we find the most probable companion mass to be M-1 = similar to 0.8 M-circle dot assuming a typical mass for the B star and most probable inclination. We conclude that the X-ray source companion to HD 314884 is most likely a coronally active G-type star or a white dwarf, with no apparent emission lines in the optical spectrum. The mass probability distribution of the companion star mass spans 0.6-2.3 M-circle dot at 99 per cent confidence which allows the possibility of a neutron star companion. The X-ray source is unlikely to be a black hole unless it is of a very low mass or low binary inclination. C1 [Johnson, Christopher B.; Hynes, R. I.; Davis, H., III] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Maccarone, T.; Britt, C. T.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Maccarone, T.] Univ Southampton, Southampton SO17 1BJ, Hants, England. [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.; Nelemans, G.] Radbound Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Steeghs, D.; Greiss, S.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Johnson, CB (reprint author), Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. EM cjoh285@lsu.edu RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 FU National Science Foundation [AST-0908789]; Graduate Student Research Award (GSRA) FX This work was supported by the National Science Foundation under grant no. AST-0908789. CBJ acknowledges support from a Graduate Student Research Award (GSRA) administered by the Louisiana Space Grant Consortium (LaSPACE). This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France, and NASA's Astrophysics Data System. Finally, we are very grateful to Dr Eric Mamajek for making available his compilation of stellar colours and temperatures for dwarf stars. The Proposal ID # for the 2.0 m Liverpool Telescope observing run is JL12B01 with P.I. Thomas J. Maccarone. NR 29 TC 1 Z9 1 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 OCT 21 PY 2014 VL 444 IS 2 BP 1584 EP 1590 DI 10.1093/mnras/stu1539 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6MF UT WOS:000342926300042 ER PT J AU Oppenheimer, S Bradley, B Stanford, D AF Oppenheimer, Stephen Bradley, Bruce Stanford, Dennis TI Solutrean hypothesis: genetics, the mammoth in the room SO WORLD ARCHAEOLOGY LA English DT Article DE mtDNA; Solutrean hypothesis; migrations; aDNA; Palaeo-Americans; Archaeogenetics ID MITOCHONDRIAL-DNA; NORTH-AMERICA; HAPLOGROUP-X; POPULATION HISTORY; NATIVE-AMERICANS; MTDNA ANALYSIS; Y-CHROMOSOMES; ANCIENT DNA; NEW-WORLD; CLOVIS AB The Solutrean hypothesis for the origin of the Clovis archaeological culture contends that people came from south-western Europe to North America during the Last Glacial Maximum. This hypothesis has received numerous critiques, but little objective testing, either of cultural or genetic evidence. We contest the assertion that there is NO genetic evidence to support this hypothesis, and detail the published evidence, consistent with a pre-Columbian western Eurasian origin for some founding genetic markers, specifically mtDNA X2a, and some autosomal influence, found in ancient and modern Native American populations. The possibility that the inferred pre-Columbian western autosomal influence came more directly than through Siberia is not even considered in such studies. The mtDNA X2a evidence is more consistent with the Atlantic route and dates suggested by the Solutrean hypothesis and is more parsimonious than the assumption of a single Beringian entry, that assumes retrograde extinction of X in East Eurasia. C1 [Oppenheimer, Stephen] Univ Oxford, Inst Social & Cultural Anthropol, Sch Anthropol, Oxford OX1 2JD, England. [Bradley, Bruce] Univ Exeter, Dept Archaeol, Exeter EX4 4QJ, Devon, England. [Stanford, Dennis] Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. RP Oppenheimer, S (reprint author), Univ Oxford, Inst Social & Cultural Anthropol, Sch Anthropol, Oxford OX1 2JD, England. EM stephen.oppenheimer@ntlworld.com NR 67 TC 2 Z9 2 U1 4 U2 36 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0043-8243 EI 1470-1375 J9 WORLD ARCHAEOL JI World Archaeol. PD OCT 20 PY 2014 VL 46 IS 5 SI SI BP 752 EP 774 DI 10.1080/00438243.2014.966273 PG 23 WC Archaeology SC Archaeology GA AR9OT UT WOS:000343905100006 ER PT J AU Rowley-Conwy, P Zeder, M AF Rowley-Conwy, Peter Zeder, Melinda TI Mesolithic domestic pigs at Rosenhof - or wild boar? A critical re-appraisal of ancient DNA and geometric morphometrics SO WORLD ARCHAEOLOGY LA English DT Article DE geometric morphometrics; ancient DNA; domestic pig; Wild boar; Mesolithic; Rosenhof ID CATTLE AB We challenge the claim by Krause-Kyora et al. (2013) that there were domestic pigs at Mesolithic sites in northern Germany. A small number of animals from Rosenhof and Poel have ancient DNA and geometric morphometric signatures elsewhere associated with domestic animals. At this time Neolithic farming settlements were present 150km to the south, but the Mesolithic specimens are, however, metrically wild boar, much larger than domestic pigs, and cannot be domestic individuals acquired from the farmers. A more likely explanation for these 'domestic' traits is that animals that escaped from farmers' pig herds interbred with local wild boar. Their descendants were morphologically and behaviourally wild, and were shot by Mesolithic foragers in the course of normal hunts. Their presence at Mesolithic sites is not a precursor to agriculture. C1 [Rowley-Conwy, Peter] Univ Durham, Durham DH1 3HP, England. [Zeder, Melinda] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Washington, DC 20560 USA. RP Rowley-Conwy, P (reprint author), Univ Durham, Durham DH1 3HP, England. EM P.A.Rowley-Conwy@durham.ac.uk NR 37 TC 6 Z9 6 U1 0 U2 6 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0043-8243 EI 1470-1375 J9 WORLD ARCHAEOL JI World Archaeol. PD OCT 20 PY 2014 VL 46 IS 5 SI SI BP 813 EP 824 DI 10.1080/00438243.2014.953704 PG 12 WC Archaeology SC Archaeology GA AR9OT UT WOS:000343905100009 ER PT J AU Rowley-Conwy, P Zeder, M AF Rowley-Conwy, Peter Zeder, Melinda TI Wild Boar or Domestic Pigs? Response to Evin et al. SO WORLD ARCHAEOLOGY LA English DT Article DE Mesolithic; domestic pig; ancient DNA; Rosenhof; geometric morphometrics; Wild boar AB We continue to contest the claim by Evin et al. (2014) that Rosenhof E24 and other Mesolithic pigs were domestic. E24's mixture of 'wild' and 'domestic' traits is best explained as indicating a behaviourally wild boar with some domestic ancestry. The fascinating complexities of this situation should not be downplayed in favour of a simplified, more newsworthy (but probably incorrect) conclusion. C1 [Rowley-Conwy, Peter] Univ Durham, Durham DH1 3HP, England. [Zeder, Melinda] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Rowley-Conwy, P (reprint author), Univ Durham, Durham DH1 3HP, England. EM p.a.rowley-conwy@durham.ac.uk; zederm@si.edu NR 10 TC 3 Z9 3 U1 0 U2 4 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0043-8243 EI 1470-1375 J9 WORLD ARCHAEOL JI World Archaeol. PD OCT 20 PY 2014 VL 46 IS 5 SI SI BP 835 EP 840 DI 10.1080/00438243.2014.953712 PG 6 WC Archaeology SC Archaeology GA AR9OT UT WOS:000343905100011 ER PT J AU Balokovic, M Comastri, A Harrison, FA Alexander, DM Ballantyne, DR Bauer, FE Boggs, SE Brandt, WN Brightman, M Christensen, FE Craig, WW Del Moro, A Gandhi, P Hailey, CJ Koss, M Lansbury, GB Luo, B Madejski, GM Marinucci, A Matt, G Markwardt, CB Puccetti, S Reynolds, CS Risaliti, G Rivers, E Stern, D Walton, DJ Zhang, WW AF Balokovic, M. Comastri, A. Harrison, F. A. Alexander, D. M. Ballantyne, D. R. Bauer, F. E. Boggs, S. E. Brandt, W. N. Brightman, M. Christensen, F. E. Craig, W. W. Del Moro, A. Gandhi, P. Hailey, C. J. Koss, M. Lansbury, G. B. . Luo, B. Madejski, G. M. Marinucci, A. Matt, G. Markwardt, C. B. Puccetti, S. Reynolds, C. S. Risaliti, G. Rivers, E. Stern, D. Walton, D. J. Zhang, W. W. TI THE NuSTAR VIEW OF NEARBY COMPTON-THICK ACTIVE GALACTIC NUCLEI: THE CASES OF NGC 424, NGC 1320, AND IC 2560 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 424, NGC 1320, IC 2560); galaxies: nuclei; galaxies: Seyfert; techniques: spectroscopic; X-rays: galaxies ID SEYFERT 2 GALAXIES; RAY LUMINOSITY FUNCTION; XMM-NEWTON OBSERVATIONS; APPROXIMATE-TO 2; STAR-FORMATION; LINE REGION; SWIFT-BAT; MIDINFRARED SPECTROSCOPY; EDDINGTON RATIOS; TOLOLO 0109-383 AB We present X-ray spectral analyses for three Seyfert 2 active galactic nuclei (AGNs), NGC 424, NGC 1320, and IC 2560, observed by NuSTAR in the 3-79 keV band. The high quality hard X-ray spectra allow detailed modeling of the Compton reflection component for the first time in these sources. Using quasi-simultaneous NuSTAR and Swift/XRT data, as well as archival XMM-Newton data, we find that all three nuclei are obscured by Compton-thick material with column densities in excess of similar to 5 x 10(24) cm(-2), and that their X-ray spectra above 3 keV are dominated by reflection of the intrinsic continuum on Compton-thick material. Due to the very high obscuration, absorbed intrinsic continuum components are not formally required by the data in any of the sources. We constrain the intrinsic photon indices and the column density of the reflecting medium through the shape of the reflection spectra. Using archival multi-wavelength data we recover the intrinsic X-ray luminosities consistent with the broadband spectral energy distributions. Our results are consistent with the reflecting medium being an edge-on clumpy torus with a relatively large global covering factor and overall reflection efficiency of the order of 1%. Given the unambiguous confirmation of the Compton-thick nature of the sources, we investigate whether similar sources are likely to be missed by commonly used selection criteria for Compton-thick AGNs, and explore the possibility of finding their high-redshift counterparts. C1 [Balokovic, M.; Harrison, F. A.; Rivers, E.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Alexander, D. M.; Del Moro, A.; Gandhi, P.; Lansbury, G. B. .] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F. E.] Pontificia Univ Catolica Chile 306, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Christensen, F. E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [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.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Koss, M.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Madejski, G. M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Marinucci, A.; Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Markwardt, C. B.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, C. S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Risaliti, G.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Balokovic, M (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X; Puccetti, Simonetta/0000-0002-2734-7835 FU International Fulbright Science and Technology Award; ASI-INAF [I/037/012/0-011/13]; Swiss National Science Foundation [PP00P2_138979/1]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX The authors thank the anonymous referee for useful comments which have improved the manuscript. M.B. acknowledges support from the International Fulbright Science and Technology Award. A.C. acknowledges support from ASI-INAF grant I/037/012/0-011/13. M.K. gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. 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). This research made use of the XRT Data Analysis Software (XRTDAS), archival data, software and on-line services provided by the ASDC. This research has made use of NASA's Astrophysics Data System. NR 102 TC 34 Z9 34 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 OCT 20 PY 2014 VL 794 IS 2 AR 111 DI 10.1088/0004-637X/794/2/111 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800015 ER PT J AU Chen, B Bastian, TS Gary, DE AF Chen, Bin Bastian, T. S. Gary, D. E. TI DIRECT EVIDENCE OF AN ERUPTIVE, FILAMENT-HOSTING MAGNETIC FLUX ROPE LEADING TO A FAST SOLAR CORONAL MASS EJECTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: coronal mass ejections (CMEs); Sun: filaments, prominences; Sun: flares; Sun: magnetic fields ID PROMINENCE CAVITIES; ENERGY-RELEASE; FLARES; ACCELERATION; RECONNECTION; EVOLUTION; MODEL; DYNAMICS; TEMPERATURES; TELESCOPE AB Magnetic flux ropes (MFRs) are believed to be at the heart of solar coronal mass ejections (CMEs). A well-known example is the prominence cavity in the low corona that sometimes makes up a three-part white-light (WL) CME upon its eruption. Such a system, which is usually observed in quiet-Sun regions, has long been suggested to be the manifestation of an MFR with relatively cool filament material collecting near its bottom. However, observational evidence of eruptive, filament-hosting MFR systems has been elusive for those originating in active regions. By utilizing multi-passband extreme-ultraviolet (EUV) observations from Solar Dynamics Observatory/Atmospheric Imaging Assembly, we present direct evidence of an eruptive MFR in the low corona that exhibits a hot envelope and a cooler core; the latter is likely the upper part of a filament that undergoes a partial eruption, which is later observed in the upper corona as the coiled kernel of a fast, WL CME. This MFR-like structure exists more than 1 hr prior to its eruption, and displays successive stages of dynamical evolution, in which both ideal and non-ideal physical processes may be involved. The timing of the MFR kinematics is found to be well correlated with the energy release of the associated long-duration C1.9 flare. We suggest that the long-duration flare is the result of prolonged energy release associated with the vertical current sheet induced by the erupting MFR. C1 [Chen, Bin; Gary, D. E.] New Jersey Inst Technol, Ctr Solar Terr Res, Newark, NJ 07102 USA. [Bastian, T. S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Chen, B (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM bin.chen@cfa.harvard.edu FU NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; NSF [AST-1312802] FX We thank Chang Liu for help on the data analysis, lain Hannah for the DEM inversion code, Gregory Fleishman for insightful discussions, and Wei Liu for providing the first AIA movies. The authors are grateful to the teams of SDO, STEREO, and RHESSI for making the data available. This research was supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administrated by the University Corporation for Atmospheric Research. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. D.G. acknowledges support from NSF grant AST-1312802 to NJIT. NR 68 TC 11 Z9 11 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2014 VL 794 IS 2 AR 149 DI 10.1088/0004-637X/794/2/149 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800053 ER PT J AU Gandhi, P Lansbury, GB Alexander, DM Stern, D Arevalo, P Ballantyne, DR Balokovic, M Bauer, FE Boggs, SE Brandt, WN Brightman, M Christensen, FE Comastri, A Craig, WW Del Moro, A Elvis, M Fabian, AC Hailey, CJ Harrison, FA Hickox, RC Koss, M LaMassa, SM Luo, B Madejski, GM Ptak, AF Puccetti, S Teng, SH Urry, CM Walton, DJ Zhang, WW AF Gandhi, P. Lansbury, G. B. Alexander, D. M. Stern, D. Arevalo, P. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Boggs, S. E. Brandt, W. N. Brightman, M. Christensen, F. E. Comastri, A. Craig, W. W. Del Moro, A. Elvis, M. Fabian, A. C. Hailey, C. J. Harrison, F. A. Hickox, R. C. Koss, M. LaMassa, S. M. Luo, B. Madejski, G. M. Ptak, A. F. Puccetti, S. Teng, S. H. Urry, C. M. Walton, D. J. Zhang, W. W. TI NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34 (vol 792, pg 117, 2014) SO ASTROPHYSICAL JOURNAL LA English DT Correction ID GALAXY; SUZAKU C1 [Gandhi, P.; Lansbury, G. B.; Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arevalo, P.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Luo, B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] 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. [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Comastri, A.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Koss, M.] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. [LaMassa, S. M.; Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Madejski, G. M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Ptak, A. F.; Zhang, W. W.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Gandhi, P (reprint author), Univ Durham, Dept Phys, S Rd, Durham DH1 3LE, England. EM poshak.gandhi@durham.ac.uk RI Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015 OI Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453 NR 12 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 OCT 20 PY 2014 VL 794 IS 2 AR 176 DI 10.1088/0004-637X/794/2/176 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800080 ER PT J AU Greve, TR Leonidaki, I Xilouris, EM Weiss, A Zhang, ZY van der Werf, P Aalto, S Armus, L Diaz-Santos, T Evans, AS Fischer, J Gao, Y Gonzalez-Alfonso, E Harris, A Henkel, C Meijerink, R Naylor, DA Smith, HA Spaans, M Stacey, GJ Veilleux, S Walter, F AF Greve, T. R. Leonidaki, I. Xilouris, E. M. Weiss, A. Zhang, Z. -Y. van der Werf, P. Aalto, S. Armus, L. Diaz-Santos, T. Evans, A. S. Fischer, J. Gao, Y. Gonzalez-Alfonso, E. Harris, A. Henkel, C. Meijerink, R. Naylor, D. A. Smith, H. A. Spaans, M. Stacey, G. J. Veilleux, S. Walter, F. TI STAR FORMATION RELATIONS AND CO SPECTRAL LINE ENERGY DISTRIBUTIONS ACROSS THE J-LADDER AND REDSHIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: ISM; galaxies: starburst; ISM: molecules ID ULTRALUMINOUS INFRARED GALAXIES; DENSE MOLECULAR GAS; LENSED SUBMILLIMETER GALAXIES; HERSCHEL-SPIRE SPECTROSCOPY; FREE-FREE EMISSION; FORMING GALAXIES; INTERSTELLAR-MEDIUM; NEARBY GALAXIES; STARBURST GALAXY; FORMATION LAW AB We present FIR [50-300 mu m]-CO luminosity relations (i.e., log L-FIR = alpha log L'(CO) + beta) for the full CO rotational ladder from J = 1-0 up to J = 13-12 for a sample of 62 local (z <= 0.1) (Ultra) Luminous InfraredGalaxies (LIRGs; LIR[8-1000 mu m] > 10(11) L-circle dot) using data from Herschel SPIRE-FTS and ground-based telescopes. We extend our sample to high redshifts (z > 1) by including 35 submillimeter selected dusty star forming galaxies from the literature with robust CO observations, and sufficiently well-sampled FIR/submillimeter spectral energy distributions (SEDs), so that accurate FIR luminosities can be determined. The addition of luminous starbursts at high redshifts enlarge the range of the FIR-CO luminosity relations toward the high-IR-luminosity end, while also significantly increasing the small amount of mid-J/high-J CO line data (J = 5-4 and higher) that was available prior to Herschel. This new data set (both in terms of IR luminosity and J-ladder) reveals linear FIR-CO luminosity relations (i.e., a similar or equal to 1) for J = 1-0 up to J = 5-4, with a nearly constant normalization (beta similar to 2). In the simplest physical scenario, this is expected from the (also) linear FIR-(molecular line) relations recently found for the dense gas tracer lines (HCN and CS), as long as the dense gas mass fraction does not vary strongly within our (merger/starburst)-dominated sample. However, from J = 6-5 and up to the J = 13-12 transition, we find an increasingly sublinear slope and higher normalization constant with increasing J. We argue that these are caused by a warm (similar to 100 K) and dense (>10(4) cm(-3)) gas component whose thermal state is unlikely to be maintained by star-formation-powered far-UV radiation fields (and thus is no longer directly tied to the star formation rate). We suggest that mechanical heating (e.g., supernova-driven turbulence and shocks), and not cosmic rays, is the more likely source of energy for this component. The global CO spectral line energy distributions, which remain highly excited from J = 6-5 up to J = 13-12, are found to be a generic feature of the (U)LIRGs in our sample, and further support the presence of this gas component. C1 [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Leonidaki, I.; Xilouris, E. M.] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, GR-15236 Penteli, Greece. [Weiss, A.; Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zhang, Z. -Y.] Royal Observ, UK Astron Technol Ctr, Sci & Technol Facil Council, Edinburgh EH9 3HJ, Midlothian, Scotland. [Zhang, Z. -Y.] European So Observ, D-85748 Garching, Germany. [van der Werf, P.; Meijerink, R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Aalto, S.] Chalmers, Dept Earth & Space Sci, Onsala Observ, S-43994 Onsala, Sweden. [Armus, L.; Diaz-Santos, T.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Evans, A. S.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Evans, A. S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Fischer, J.] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Gao, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Gonzalez-Alfonso, E.] Univ Alcala de Henares, Dept Fs, E-28871 Alcala De Henares, Spain. [Harris, A.; Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Henkel, C.] King Abdulaziz Univ, Dept Astron, Jeddah 21589, Saudi Arabia. [Naylor, D. A.] Univ Lethbridge, Inst Space Imaging Sci, Dept Phys & Astron, Lethbridge, AB T1K 3M4, Canada. [Smith, H. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spaans, M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Stacey, G. J.] Cornell Univ, Dept Astron, Ithaca, NY 1485 USA. [Walter, F.] Max Planck Inst Astron, D-691117 Heidelberg, Germany. RP Greve, TR (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM t.greve@ucl.ac.uk RI Xilouris, Emmanuel/K-9459-2013; LEONIDAKI, IOANNA/K-4351-2013; OI Zhang, Zhiyu/0000-0002-7299-2876 FU "DeMoGas" project; European Social Fund (ESF); STEC Advanced Fellowship; Chinese Academy of Sciences Fellowship for Young International Scientists [2012y1ja0006]; European Research Council (ERC); Office of Naval Research; NHSC/JPL FX The authors gratefully acknowledge financial support under the "DeMoGas" project. The project DeMoGas is implemented under the "ARISTELV Action of the "Operational Programme Education and Lifelong Learning." The project is co-funded by the European Social Fund (ESF) and National Resources. T.R.G. acknowledges support from an STEC Advanced Fellowship. T.R.G. was also supported by Chinese Academy of Sciences Fellowship for Young International Scientists (grant no. 2012y1ja0006). Z.Y.Z. acknowledges support from the European Research Council (ERC) in the form of Advanced Grant,COSMICISM. We are indebted to P. P. Papadopoulos for extensive discussions and comments on the paper (He ho'okele wa'a no ka la 'ino). Basic research in infrared astronomy at the Naval Research Laboratory is funded by the Office of Naval Research. J.F. also acknowledges support from the NHSC/JPL. The research presented here 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. Finally, we would like to thank the anonymous referee for a useful and constructive referee report that helped improve the paper. NR 133 TC 26 Z9 26 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2014 VL 794 IS 2 AR 142 DI 10.1088/0004-637X/794/2/142 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800046 ER PT J AU Guo, XY Sironi, L Narayan, R AF Guo, Xinyi Sironi, Lorenzo Narayan, Ramesh TI NON-THERMAL ELECTRON ACCELERATION IN LOW MACH NUMBER COLLISIONLESS SHOCKS. I. PARTICLE ENERGY SPECTRA AND ACCELERATION MECHANISM SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; galaxies: clusters: general; radiation mechanisms: non-thermal; shock waves ID PERPENDICULAR BOW SHOCK; MERGING GALAXY CLUSTER; IN-CELL SIMULATIONS; DRIFT ACCELERATION; ASTROPHYSICAL SHOCKS; ION-ACCELERATION; RADIO RELICS; SOLAR-FLARES; FAST FERMI; INJECTION AB Electron acceleration to non-thermal energies in low Mach number (M-s less than or similar to 5) shocks is revealed by radio and X-ray observations of galaxy clusters and solar flares, but the electron acceleration mechanism remains poorly understood. Diffusive shock acceleration, also known as first-order Fermi acceleration, cannot be directly invoked to explain the acceleration of electrons. Rather, an additional mechanism is required to pre-accelerate the electrons from thermal to supra-thermal energies, so they can then participate in the Fermi process. In this work, we use two-and three-dimensional particle-in-cell plasma simulations to study electron acceleration in low Mach number shocks. We focus on the particle energy spectra and the acceleration mechanism in a reference run with M-s = 3 and a quasi-perpendicular pre-shock magnetic field. We find that about 15% of the electrons can be efficiently accelerated, forming a non-thermal power-law tail in the energy spectrum with a slope of p similar or equal to 2.4. Initially, thermal electrons are energized at the shock front via shock drift acceleration (SDA). The accelerated electrons are then reflected back upstream where their interaction with the incoming flow generates magnetic waves. In turn, the waves scatter the electrons propagating upstream back toward the shock for further energization via SDA. In summary, the self-generated waves allow for repeated cycles of SDA, similarly to a sustained Fermi-like process. This mechanism offers a natural solution to the conflict between the bright radio synchrotron emission observed from the outskirts of galaxy clusters and the low electron acceleration efficiency usually expected in low Mach number shocks. C1 [Guo, Xinyi; Sironi, Lorenzo; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Guo, XY (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX14AB47G]; NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF1-120090, NAS8-03060] FX X.G. and R.N. are supported in part by NASA grant NNX14AB47G. X.G. thanks Philip Mocz for helpful comments on the manuscript and Pierre Christian for useful discussions. We thank R. van Weeren, A. Spitkovsky, and J. Park for helpful comments. L.S. 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. The computations in this paper were run on the Odyssey cluster supported by the FAS Division of Science, Research Computing Group at Harvard University. NR 56 TC 29 Z9 29 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 OCT 20 PY 2014 VL 794 IS 2 AR 153 DI 10.1088/0004-637X/794/2/153 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800057 ER PT J AU Johnson, MD Fish, VL Doeleman, SS Broderick, AE Wardle, JFC Marrone, DP AF Johnson, Michael D. Fish, Vincent L. Doeleman, Sheperd S. Broderick, Avery E. Wardle, John F. C. Marrone, Daniel P. TI RELATIVE ASTROMETRY OF COMPACT FLARING STRUCTURES IN Sgr A* WITH POLARIMETRIC VERY LONG BASELINE INTERFEROMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; Galaxy: center; submillimeter: general; techniques: high angular resolution; techniques: interferometric; techniques: polarimetric ID SUPERMASSIVE BLACK-HOLE; NEAR-INFRARED FLARES; SAGITTARIUS-A; GALACTIC-CENTER; X-RAY; CIRCULAR-POLARIZATION; ACCRETION FLOW; RADIO-SOURCES; HORIZON; EMISSION AB We demonstrate that polarimetric interferometry can be used to extract precise spatial information about compact polarized flares of Sgr A*. We show that, for a faint dynamical component, a single interferometric baseline suffices to determine both its polarization and projected displacement from the quiescent intensity centroid. A second baseline enables two-dimensional reconstruction of the displacement, and additional baselines can self-calibrate using the flare, enhancing synthesis imaging of the quiescent emission. We apply this technique to simulated 1.3 mm wavelength observations of a "hot spot" embedded in a radiatively inefficient accretion disk around Sgr A*. Our results indicate that, even with current sensitivities, polarimetric interferometry with the Event Horizon Telescope can achieve similar to 5 mu as relative astrometry of compact flaring structures near Sgr A* on timescales of minutes. C1 [Johnson, Michael D.; Doeleman, Sheperd S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fish, Vincent L.; Doeleman, Sheperd S.] MIT, Haystack Observ, Westford, MA 01886 USA. [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. [Wardle, John F. C.] Brandeis Univ, Dept Phys MS 057, Waltham, MA 02454 USA. [Marrone, Daniel P.] Univ Arizona, Arizona Radio Observ, Steward Observ, Tucson, AZ 85721 USA. RP Johnson, MD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mjohnson@cfa.harvard.edu OI Marrone, Daniel/0000-0002-2367-1080 FU National Science Foundation [AST-1207752, AST-1310896, AST-1211539]; Gordon and Betty Moore Foundation [GBMF-3561]; Perimeter Institute for Theoretical Physics; Natural Sciences and Engineering Research Council of Canada through a Discovery Grant; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX We thank the National Science Foundation (AST-1207752, AST-1310896, and AST-1211539 and the Gordon and Betty Moore Foundation (GBMF-3561) for financial support of this work. 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. 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. NR 37 TC 12 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 OCT 20 PY 2014 VL 794 IS 2 AR 150 DI 10.1088/0004-637X/794/2/150 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800054 ER PT J AU Li, GJ Naoz, S Valsecchi, F Johnson, JA Rasio, FA AF Li, Gongjie Naoz, Smadar Valsecchi, Francesca Johnson, John Asher Rasio, Frederic A. TI THE DYNAMICS OF THE MULTI-PLANET SYSTEM ORBITING KEPLER-56 SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics ID HIERARCHICAL 3-BODY SYSTEMS; STELLAR ASTROPHYSICS MESA; INTERNAL GRAVITY-WAVES; HOT JUPITERS; EXTRASOLAR PLANETS; EXOPLANETARY SYSTEMS; MULTIPLANET SYSTEMS; KOZAI MECHANISM; BINARY-SYSTEMS; TIDAL FRICTION AB Kepler-56 is a multi-planet system containing two coplanar inner planets that are in orbits misaligned with respect to the spin axis of the host star, and an outer planet. Various mechanisms have been proposed to explain the broad distribution of spin-orbit angles among exoplanets, and these theories fall under two broad categories. The first is based on dynamical interactions in a multi-body system, while the other assumes that disk migration is the driving mechanism in planetary configuration and that the star (or disk) is titled with respect to the planetary plane. Here we show that the large observed obliquity of Kepler 56 system is consistent with a dynamical origin. In addition, we use observations by Huber et al. to derive the obliquity's probability distribution function, thus improving the constrained lower limit. The outer planet may be the cause of the inner planets' large obliquities, and we give the probability distribution function of its inclination, which depends on the initial orbital configuration of the planetary system. We show that even in the presence of precise measurement of the true obliquity, one cannot distinguish the initial configurations. Finally we consider the fate of the system as the star continues to evolve beyond the main sequence, and we find that the obliquity of the system will not undergo major variations as the star climbs the red giant branch. We follow the evolution of the system and find that the innermost planet will be engulfed in similar to 129 Myr. Furthermore we put an upper limit of similar to 155 Myr for the engulfment of the second planet. This corresponds to similar to 3% of the current age of the star. C1 [Li, Gongjie; Naoz, Smadar; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Valsecchi, Francesca; Rasio, Frederic A.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Valsecchi, Francesca; Rasio, Frederic A.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 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; snaoz@cfa.harvard.edu OI Naoz, Smadar/0000-0002-9802-9279 FU NASA through an Einstein Post-doctoral Fellowship; Chandra X-Ray Center; NASA [PF2-130096, NNX12AI86G]; Alfred P. Sloan Packard foundation; David & Lucile Packard foundation FX S.N. is supported by NASA through an Einstein Post-doctoral Fellowship awarded by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract PF2-130096. This work was also supported by NASA grant NNX12AI86G at Northwestern University. J.A.J. gratefully acknowledges funding from the Alfred P. Sloan and David & Lucile Packard foundations. NR 68 TC 8 Z9 8 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2014 VL 794 IS 2 AR 131 DI 10.1088/0004-637X/794/2/131 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800035 ER PT J AU Orosz, JA Steiner, JF McClintock, JE Buxton, MM Bailyn, CD Steeghs, D Guberman, A Torres, MAP AF Orosz, Jerome A. Steiner, James F. McClintock, Jeffrey E. Buxton, Michelle M. Bailyn, Charles D. Steeghs, Danny Guberman, Alec Torres, Manuel A. P. TI THE MASS OF THE BLACK HOLE IN LMC X-3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: black holes; stars: variables: general; X-rays: binaries; X-rays: individual (LMC X-3) ID RADIAL-VELOCITY CURVE; X-RAY BINARIES; LIGHT-CURVE; MODEL ATMOSPHERES; STANDARD STARS; DISCOVERY; LMC-X-3; GALAXY; SPIN AB We analyze a large set of new and archival photometric and spectroscopic observations of LMC X-3 to arrive at a self-consistent dynamical model for the system. Using echelle spectra obtained with the Magellan Inamori Kyocera Echelle instrument on the 6.5 m Magellan Clay telescope and the UVES instrument on the second 8.2 m Very Large Telescope, we find a velocity semiamplitude for the secondary star of K-2 = 241.1 +/- 6.2 kms(-1), where the uncertainty includes an estimate of the systematic error caused by X-ray heating. Using the spectra, we also find a projected rotational velocity of V-rot sin i = 118.5 +/- 6.6 kms(-1). From an analysis of archival B and V light curves as well as new B and V light curves from the SMARTS 1.3 m telescope, we find an inclination of i = 69 degrees.84 +/- 0 degrees.37 for models that do not include X-ray heating and an inclination of i = 69 degrees.24 +/- 0 degrees.72 for models that incorporate X-ray heating. Adopting the latter inclination measurement, we find masses of 3.63 +/- 0.57 M-circle dot and 6.98 +/- 0.56 M-circle dot for the companion star and the black hole, respectively. We briefly compare our results with earlier work and discuss some of their implications. C1 [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Steiner, James F.; McClintock, Jeffrey E.; Torres, Manuel A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buxton, Michelle M.; Bailyn, Charles D.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Steeghs, Danny] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Guberman, Alec] Byram Hills High Sch, Armonk, NY 10504 USA. [Guberman, Alec] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Torres, Manuel A. P.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. RP Orosz, JA (reprint author), San Diego State Univ, Dept Astron, 5500 Campanile Dr, San Diego, CA 92182 USA. EM jorosz@mail.sdsu.edu; jsteiner@cfa.harvard.edu; jem@cfa.harvard.edu; michelle.buxton@yale.edu; charles.bailyn@yale.edu; T.H.Steeghs@warwick.ac.uk; alec.guberman@stonybrook.edu; M.Torres@sron.nl FU NASA [HST-HF-51315.01, NNX11AD08G]; NASA Guest Observer Program; National Science Foundation [AST 0407063, AST 070707] FX JFS was supported by NASA Hubble Fellowship grant HST-HF-51315.01. The work of JEM was supported in part by NASA grant NNX11AD08G. D.S. acknowledges an STFC Advanced Fellowship as well as support through the NASA Guest Observer Program. M.M.B. and C.D.B. acknowledge support from the National Science Foundation via the grants AST 0407063 and AST 070707. NR 53 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 OCT 20 PY 2014 VL 794 IS 2 AR 154 DI 10.1088/0004-637X/794/2/154 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800058 ER PT J AU Rapson, VA Pipher, JL Gutermuth, RA Megeath, ST Allen, TS Myers, PC Allen, LE AF Rapson, V. A. Pipher, J. L. Gutermuth, R. A. Megeath, S. T. Allen, T. S. Myers, P. C. Allen, L. E. TI A SPITZER VIEW OF THE GIANT MOLECULAR CLOUD MON OB1 EAST/NGC 2264 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; ISM: clouds; stars: formation ID YOUNG STELLAR OBJECTS; INFRARED ARRAY CAMERA; INITIAL MASS FUNCTION; BROWN DWARF CANDIDATES; CLUSTER NGC 2264; STAR-FORMATION; SPACE-TELESCOPE; X-RAY; NGC-2264; NEARBY AB We present Spitzer 3.6, 4.5, 5.8, 8.0, and 24 mu m images of the Mon OB1 East giant molecular cloud, which contains the young star forming region NGC 2264, as well as more extended star formation. With Spitzer data and Two Micron All Sky Survey photometry, we identify and classify young stellar objects (YSOs) with dusty circumstellar disks and/or envelopes in Mon OB1 East by their infrared-excess emission and study their distribution with respect to cloud material. We find a correlation between the local surface density of YSOs and column density of molecular gas as traced by dust extinction that is roughly described as a power law in these quantities. NGC 2264 follows a power-law index of similar to 2.7, exhibiting a large YSO surface density for a given gas column density. Outside of NGC 2264 where the surface density of YSOs is lower, the power law is shallower and the region exhibits a larger gas column density for a YSO surface density, suggesting the star formation is more recent. In order to measure the fraction of cloud members with circumstellar disks/envelopes, we estimate the number of diskless pre-main-sequence stars by statistical removal of background star detections. We find that the disk fraction of the NGC 2264 region is 45%, while the surrounding, more distributed regions show a disk fraction of 19%. This may be explained by the presence of an older, more dispersed population of stars. In total, the Spitzer observations provide evidence for heterogenous, non-coeval star formation throughout the Mon OB1 cloud. C1 [Rapson, V. A.] Univ Rochester, Sch Phys & Astron, Rochester Inst Technol, Rochester, NY 14627 USA. [Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Gutermuth, R. A.] Smith Coll, Dept Astron, Coll 5, Northampton, MA 01063 USA. [Megeath, S. T.; Allen, T. S.] Lowell Observ, Flagstaff, AZ 86001 USA. [Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Rapson, VA (reprint author), Univ Rochester, Sch Phys & Astron, Rochester Inst Technol, Rochester, NY 14627 USA. EM var5998@rit.edu FU NASA ADAP [NNX11AD14G, NNX13AF08G]; Caltech/JPL awards [1373081, 1424329, 1440160]; NASA [960541, 960785] FX We gratefully acknowledge funding support from NASA ADAP grants NNX11AD14G and NNX13AF08G and Caltech/JPL awards 1373081, 1424329, and 1440160 in support of Spitzer Space Telescope observing programs. This work received support through that provided to the IRAC and MIPS instruments by NASA through contracts 960541 and 960785, respectively, issued by JPL. Support for this work was also provided by NASA through awards to S.T.M. and J.L.P. issued by JPL/Caltech. NR 57 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 OCT 20 PY 2014 VL 794 IS 2 AR 124 DI 10.1088/0004-637X/794/2/124 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800028 ER PT J AU Rubin, KHR Prochaska, JX Koo, DC Phillips, AC Martin, CL Winstrom, LO AF Rubin, Kate H. R. Prochaska, J. Xavier Koo, David C. Phillips, Andrew C. Martin, Crystal L. Winstrom, Lucas O. TI EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z similar to 0.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: halos; galaxies: ISM; ultraviolet: ISM ID GALAXY REDSHIFT SURVEY; DEEP FIELD-SOUTH; EXTENDED GROTH STRIP; DIGITAL SKY SURVEY; INFRARED-LUMINOUS STARBURSTS; ABSORPTION-LINE PROBES; HUBBLE-SPACE-TELESCOPE; TULLY-FISHER RELATION; GOODS-NORTH FIELD; MG II ABSORPTION AB We analyze Mg II lambda lambda 2796, 2803 and Fe II lambda lambda 72586, 2600 absorption profiles in individual spectra of 105 galaxies at 0.3 < z < 1.4. The galaxies, drawn from redshift surveys of the GOODS fields and the Extended Groth Strip, sample the range in star formation rates (SFRs) occupied by the star-forming sequence with stellar masses log M*/M-circle dot greater than or similar to 9.6 down to SFR greater than or similar to 2 M-circle dot yr(-1) at 0.3 < z < 0.7. Using the Doppler shifts of MgII and Fell absorption as tracers of cool gas kinematics, we detect large-scale winds in 66 +/- 5% of the galaxies. Hubble Space Telescope Advanced Camera for Surveys imaging and our spectral analysis indicate that the outflow detection rate depends primarily on galaxy orientation: winds are detected in similar to 89% of galaxies having inclinations (i) < 30 degrees (face-on), while the wind detection rate is similar to 45% in objects having i > 50 (edge-on). Combined with the comparatively weak dependence of wind detection rate on intrinsic galaxy properties, this implies that biconical outflows are ubiquitous in normal, star-forming galaxies at z similar to 0.5. We find that wind velocity is correlated with galaxy M-* at 3.4 sigma significance, while outflow equivalent width is correlated with SFR at 3.5 sigma significance, suggesting hosts with higher SFR launch more material and/or generate a larger velocity spread for the absorbing clouds. Assuming the gas is driven into halos with isothermal density profiles, the wind velocities (similar to 200-400 km s(-1)) permit escape from the halo potentials only for the lowest-M-* systems in the sample. However, the gas carries sufficient energy to reach distances greater than or similar to 50 kpc, and may therefore be a viable source of material for the massive, cool circumgalactic medium around bright galaxies at z similar to 0. C1 [Rubin, Kate H. R.; Prochaska, J. Xavier] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Rubin, Kate H. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Prochaska, J. Xavier; Koo, David C.; Phillips, Andrew C.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Martin, Crystal L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Winstrom, Lucas O.] Cornell Univ, Newman Lab Elementary Particle Phys, Ithaca, NY 14853 USA. RP Rubin, KHR (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM krubin@cfa.harvard.edu FU NSF [AST-0808133, AST-0507483, AST-0548180, AST-1109288]; Alexander von Humboldt foundation; German Federal Ministry for Education and Research; W. M. Keck Foundation FX The authors are grateful for support for this project from NSF grants AST-0808133, AST-0507483, AST-0548180, and AST-1109288. K.H.R.R. and J.X.P. acknowledge support from the Alexander von Humboldt foundation in the form of the Humboldt Postdoctoral Fellowship and a visitor fellowship to MPIA, respectively. The Humboldt foundation is funded by the German Federal Ministry for Education and Research.; Much of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. NR 155 TC 52 Z9 52 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 OCT 20 PY 2014 VL 794 IS 2 AR 156 DI 10.1088/0004-637X/794/2/156 PG 49 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800060 ER PT J AU Savcheva, AS West, AA Bochanski, JJ AF Savcheva, Antonia S. West, Andrew A. Bochanski, John J. TI A NEW SAMPLE OF COOL SUBDWARFS FROM SDSS: PROPERTIES AND KINEMATICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: late-type; stars: low-mass; stars: statistics; subdwarfs ID DIGITAL SKY SURVEY; STAR SPECTROSCOPIC SURVEY; LOW-MASS STARS; YR(-1) MOTION SAMPLE; M-DWARFS; SOLAR NEIGHBORHOOD; MAGNETIC ACTIVITY; KAPTEYNS STAR; CATALOG; METALLICITY AB We present a new sample of M subdwarfs compiled from the seventh data release of the Sloan Digital Sky Survey. With 3517 new subdwarfs, this new sample significantly increases the number of spectroscopically confirmed low-mass subdwarfs. This catalog also includes 905 extreme and 534 ultra sudwarfs. We present the entire catalog, including observed and derived quantities, and template spectra created from co-added subdwarf spectra. We show color-color and reduced proper motion diagrams of the three metallicity classes, which are shown to separate from the disk dwarf population. The extreme and ultra subdwarfs are seen at larger values of reduced proper motion, as expected for more dynamically heated populations. We determine 3D kinematics for all of the stars with proper motions. The color-magnitude diagrams show a clear separation of the three metallicity classes with the ultra and extreme subdwarfs being significantly closer to the main sequence than the ordinary subdwarfs. All subdwarfs lie below (fainter) and to the left (bluer) of the main sequence. Based on the average (U, V, W) velocities and their dispersions, the extreme and ultra subdwarfs likely belong to the Galactic halo, while the ordinary subdwarfs are likely part of the old Galactic (or thick) disk. An extensive activity analysis of subdwarfs is performed using Ha emission, and 208 active subdwarfs are found. We show that while the activity fraction of subdwarfs rises with spectral class and levels off at the latest spectral classes, consistent with the behavior of M dwarfs, the extreme and ultra subdwarfs are basically flat. C1 [Savcheva, Antonia S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Savcheva, Antonia S.; West, Andrew A.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Bochanski, John J.] Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA. [Bochanski, John J.] Rider Univ, Lawrenceville, NJ 08648 USA. RP Savcheva, AS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asavcheva@cfa.harvard.edu FU NASA; NSF [AST-1109273, AST-1255568, AST-1151462]; Research Corporation for Science Advancement's Cottrell Scholarship; 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 FX A.S.S. acknowledges the NASA Living with a Star Postdoctoral Fellowship. A.A.W. acknowledges funding from NSF grants AST-1109273 and AST-1255568. A.A.W. also acknowledges the support of the Research Corporation for Science Advancement's Cottrell Scholarship. J.J.B. acknowledges the financial support of NSF grant AST-1151462.; 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 hlip://www.sdss.org/.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 73 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 OCT 20 PY 2014 VL 794 IS 2 AR 145 DI 10.1088/0004-637X/794/2/145 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800049 ER PT J AU Stawarz, L Szostek, A Cheung, CC Siemiginowska, A Koziel-Wierzbowska, D Werner, N Simionescu, A Madejski, G Begelman, MC Harris, DE Ostrowski, M Hagino, K AF Stawarz, L. Szostek, A. Cheung, C. C. Siemiginowska, A. Koziel-Wierzbowska, D. Werner, N. Simionescu, A. Madejski, G. Begelman, M. C. Harris, D. E. Ostrowski, M. Hagino, K. TI ON THE INTERACTION OF THE PKS B1358-113 RADIO GALAXY WITH THE A1836 CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (PKS B1358-114); galaxies: jets; intergalactic medium; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DEEP CHANDRA OBSERVATION; LARGE-SCALE SHOCK; X-RAY-EMISSION; INVERSE-COMPTON EMISSION; SUPERMASSIVE BLACK-HOLES; CENTIMETER VLA SURVEY; DIGITAL SKY SURVEY; LESS-THAN 0.3; XMM-NEWTON AB Here we present the analysis of multifrequency data gathered for the Fanaroff-Riley type-II (FR II) radio galaxy PKS B1358-113, hosted in the brightest cluster galaxy in the center of A1836. The galaxy harbors one of the most massive black holes known to date, and our analysis of the acquired optical data reveals that this black hole is only weakly active, with a mass accretion rate (M) over dot(acc) similar to 2 x 10(-4) (M) over dot(Edd) similar to 0.02 M-circle dot yr(-1). Based on analysis of new Chandra and XMM-Newton X-ray observations and archival radio data, and assuming the well-established model for the evolution of FR II radio galaxies, we derive the preferred range for the jet kinetic luminosity L-j similar to (1-6) x 10(-3) L-Edd similar to (0.5-3) x 10(45) erg s(-1). This is above the values implied by various scaling relations proposed for radio sources in galaxy clusters, being instead very close to the maximum jet power allowed for the given accretion rate. We also constrain the radio source lifetime as tau(j) similar to 40-70 Myr, meaning the total amount of deposited jet energy E-tot similar to (2-8) x 10(60) erg. We argue that approximately half of this energy goes into shock heating of the surrounding thermal gas, and the remaining 50% is deposited into the internal energy of the jet cavity. The detailed analysis of the X-ray data provides indication for the presence of a bow shock driven by the expanding radio lobes into the A1836 cluster environment. We derive the corresponding shock Mach number in the range M-sh similar to 2-4, which is one of the highest claimed for clusters or groups of galaxies. This, together with the recently growing evidence that powerful FR II radio galaxies may not be uncommon in the centers of clusters at higher redshifts, supports the idea that jet-induced shock heating may indeed play an important role in shaping the properties of clusters, galaxy groups, and galaxies in formation. In this context, we speculate on a possible bias against detecting stronger jet-driven shocks in poorer environments, resulting from inefficient electron heating at the shock front, combined with a relatively long electron-ion temperature equilibration timescale. C1 [Stawarz, L.; Simionescu, A.; Hagino, K.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.; Szostek, A.; Koziel-Wierzbowska, D.; Ostrowski, M.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Szostek, A.; Werner, N.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Szostek, A.; Werner, N.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Cheung, C. C.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Siemiginowska, A.; Harris, D. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Madejski, G.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Madejski, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Begelman, M. C.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Begelman, M. C.] NIST, Boulder, CO 80309 USA. RP Stawarz, L (reprint author), JAXA, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan. EM stawarz@astro.isas.jaxa.jp OI , kouichi/0000-0003-4235-5304 FU Polish NSC [DEC-2012/04/A/ST9/00083]; Chandra grant [GO0-11144X]; NASA [DPR S-15633-Y, NAS8-03060] FX L.S. and M.O. were supported by Polish NSC grant DEC-2012/04/A/ST9/00083. A.Sz. and G.M. were supported by Chandra grant GO0-11144X. Work by C.C.C. at NRL is supported in part by NASA DPR S-15633-Y. Support for A.S. was provided by NASA contract NAS8-03060. The authors thank the anonymous referee for critical reading of the submitted manuscript and constructive comments which helped to improve the paper. NR 177 TC 3 Z9 3 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 OCT 20 PY 2014 VL 794 IS 2 AR 164 DI 10.1088/0004-637X/794/2/164 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800068 ER PT J AU Xu, J van Dyk, DA Kashyap, VL Siemiginowska, A Connors, A Drake, J Meng, XL Ratzlaff, P Yu, YM AF Xu, Jin van Dyk, David A. Kashyap, Vinay L. Siemiginowska, Aneta Connors, Alanna Drake, Jeremy Meng, Xiao-Li Ratzlaff, Pete Yu, Yaming TI A FULLY BAYESIAN METHOD FOR JOINTLY FITTING INSTRUMENTAL CALIBRATION AND X-RAY SPECTRAL MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; standards; techniques: miscellaneous; X-rays: general ID XMM-NEWTON OBSERVATIONS; ZETA-ORIONIS; STAR; EMISSION; COUNTS; SHERPA AB Owing to a lack of robust principled methods, systematic instrumental uncertainties have generally been ignored in astrophysical data analysis despite wide recognition of the importance of including them. Ignoring calibration uncertainty can cause bias in the estimation of source model parameters and can lead to underestimation of the variance of these estimates. We previously introduced a pragmatic Bayesian method to address this problem. The method is "pragmatic" in that it introduced an ad hoc technique that simplified computation by neglecting the potential information in the data for narrowing the uncertainty for the calibration product. Following that work, we use a principal component analysis to efficiently represent the uncertainty of the effective area of an X-ray (or gamma-ray) telescope. Here, however, we leverage this representation to enable a principled, fully Bayesian method that coherently accounts for the calibration uncertainty in high-energy spectral analysis. In this setting, the method is compared with standard analysis techniques and the pragmatic Bayesian method. The advantage of the fully Bayesian method is that it allows the data to provide information not only for estimation of the source parameters but also for the calibration product-here the effective area, conditional on the adopted spectral model. In this way, it can yield more accurate and efficient estimates of the source parameters along with valid estimates of their uncertainty. Provided that the source spectrum can be accurately described by a parameterized model, this method allows rigorous inference about the effective area by quantifying which possible curves are most consistent with the data. C1 [Xu, Jin; Yu, Yaming] Univ Calif Irvine, Dept Stat, Irvine, CA 92697 USA. [van Dyk, David A.] Univ London Imperial Coll Sci Technol & Med, Stat Sect, London SW7 2AZ, England. [Kashyap, Vinay L.; Siemiginowska, Aneta; Drake, Jeremy; Ratzlaff, Pete] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Meng, Xiao-Li] Harvard Univ, Dept Stat, Cambridge, MA 02138 USA. [Connors, Alanna] Eureka Sci, Sharjah, U Arab Emirates. RP Xu, J (reprint author), Univ Calif Irvine, Dept Stat, Irvine, CA 92697 USA. EM jinx@uci.edu; dvandyk@imperial.ac.uk; vkashyap@cfa.harvard.edu; asiemiginowska@cfa.harvard.edu; jdrake@cfa.harvard.edu; meng@stat.harvard.edu; pratzlaff@cfa.harvard.edu; yamingy@ics.uci.edu FU NASA [NAS8-03060]; NSF [DMS 09-07522, DMS-09-07185, DMS-12-08791, DMS-12-09232]; British Royal Society Wolfson Research Merit Award; European Commission Marie-Curie Career Integration Grant; STFC (UK) FX This work was supported by NASA contract NAS8-03060 to the Chandra X-ray Center (V.L.K., A.s., J.D., P.R.), NSF grants DMS 09-07522, DMS-09-07185, DMS-12-08791, and DMS-12-09232 (D.v.D., X.L.M., Y.Y., A.C., J.X.). In addition, D.v.D. was supported in part by a British Royal Society Wolfson Research Merit Award, by a European Commission Marie-Curie Career Integration Grant, and by the STFC (UK). NR 28 TC 6 Z9 6 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2014 VL 794 IS 2 AR 97 DI 10.1088/0004-637X/794/2/97 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8OF UT WOS:000343085800001 ER PT J AU De Pontieu, B van der Voort, LR McIntosh, SW Pereira, TMD Carlsson, M Hansteen, V Skogsrud, H Lemen, J Title, A Boerner, P Hurlburt, N Tarbell, TD Wuelser, JP De Luca, EE Golub, L McKillop, S Reeves, K Saar, S Testa, P Tian, H Kankelborg, C Jaeggli, S Kleint, L Martinez-Sykora, J AF De Pontieu, B. van der Voort, L. Rouppe McIntosh, S. W. Pereira, T. M. D. Carlsson, M. Hansteen, V. Skogsrud, H. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T. D. Wuelser, J. P. De Luca, E. E. Golub, L. McKillop, S. Reeves, K. Saar, S. Testa, P. Tian, H. Kankelborg, C. Jaeggli, S. Kleint, L. Martinez-Sykora, J. TI On the prevalence of small-scale twist in the solar chromosphere and transition region SO SCIENCE LA English DT Article ID ALFVENIC WAVES; CORONA; ENERGY; ATMOSPHERE; DRIVEN; POWER; WIND; IRIS AB The solar chromosphere and transition region (TR) form an interface between the Sun's surface and its hot outer atmosphere. There, most of the nonthermal energy that powers the solar atmosphere is transformed into heat, although the detailed mechanism remains elusive. High-resolution (0.33-arc second) observations with NASA's Interface Region Imaging Spectrograph (IRIS) reveal a chromosphere and TR that are replete with twist or torsional motions on sub-arc second scales, occurring in active regions, quiet Sun regions, and coronal holes alike. We coordinated observations with the Swedish 1-meter Solar Telescope (SST) to quantify these twisting motions and their association with rapid heating to at least TR temperatures. This view of the interface region provides insight into what heats the low solar atmosphere. C1 [De Pontieu, B.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.] LMSAL, 3251 Hanover St,Org A021S,Bldg 252, Palo Alto, CA 94304 USA. [De Pontieu, B.; van der Voort, L. Rouppe; Pereira, T. M. D.; Carlsson, M.; Hansteen, V.; Skogsrud, H.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [McIntosh, S. W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [De Luca, E. E.; Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Kleint, L.; Martinez-Sykora, J.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. RP De Pontieu, B (reprint author), LMSAL, 3251 Hanover St,Org A021S,Bldg 252, Palo Alto, CA 94304 USA. EM bdp@lmsal.com RI Reeves, Katharine/P-9163-2014 FU Norwegian Space Center through a European Space Agency PRODEX; NASA [NNG09FA40C]; Lockheed Martin Independent Research Program; European Research Council [291058] FX We thank A. Ortiz, E. Scullion, and A. Sainz-Dalda for assistance with SST observations. IRIS is a NASA Small Explorer 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 through a European Space Agency PRODEX contract. IRIS date can be downloaded from iris.lmsal.com. This work is supported by NASA contract NNG09FA40C (IRIS), the Lockheed Martin Independent Research Program, and European Research Council grant no. 291058. The SST is operated on the island of La Palma by the Institute for Solar Physics of Stockholm. University in the Observatorio del Roque de los Muchachos of the Institute de Astrofisica de Canarias. NR 30 TC 38 Z9 38 U1 1 U2 74 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 17 PY 2014 VL 346 IS 6207 AR 1255732 DI 10.1126/science.1255732 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ7ZY UT WOS:000343041100030 PM 25324398 ER PT J AU Hansteen, V De Pontieu, B Carlsson, M Lemen, J Title, A Boerner, P Hurlburt, N Tarbell, TD Wuelser, JP Pereira, TMD De Luca, EE Golub, L McKillop, S Reeves, K Saar, S Testa, P Tian, H Kankelborg, C Jaeggli, S Kleint, L Martinez-Sykora, J AF Hansteen, V. De Pontieu, B. Carlsson, M. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T. D. Wuelser, J. P. Pereira, T. M. D. De Luca, E. E. Golub, L. McKillop, S. Reeves, K. Saar, S. Testa, P. Tian, H. Kankelborg, C. Jaeggli, S. Kleint, L. Martinez-Sykora, J. TI The unresolved fine structure resolved: IRIS observations of the solar transition region SO SCIENCE LA English DT Article ID TEMPERATURE REGION; UPPER-ATMOSPHERE; LOOPS; CORONA; INTERNETWORK; INTERFACE; DYNAMICS; NETWORK; FLUX AB The heating of the outer solar atmospheric layers, i.e., the transition region and corona, to high temperatures is a long-standing problem in solar (and stellar) physics. Solutions have been hampered by an incomplete understanding of the magnetically controlled structure of these regions. The high spatial and temporal resolution observations with the Interface Region Imaging Spectrograph (IRIS) at the solar limb reveal a plethora of short, low-lying loops or loop segments at transition-region temperatures that vary rapidly, on the time scales of minutes. We argue that the existence of these loops solves a long-standing observational mystery. At the same time, based on comparison with numerical models, this detection sheds light on a critical piece of the coronal heating puzzle. C1 [Hansteen, V.; De Pontieu, B.; Carlsson, M.; Pereira, T. M. D.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [De Pontieu, B.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Kleint, L.; Martinez-Sykora, J.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [De Luca, E. E.; Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Kleint, L.; Martinez-Sykora, J.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. RP Hansteen, V (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. EM viggoh@astro.uio.no RI Reeves, Katharine/P-9163-2014 FU Norwegian Space Center (NSC, Norway) through European Space Agency PRODEX; Research Council of Norway; NASA [NNG09FA40C]; Lockheed Martin Independent Research Program; European Research Council [291058]; LMSAL [8100002705] FX IRIS is a NASA Small Explorer mission developed and operated by the Lockheed Martin Solar and Astrophysics Laboratory (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 a European Space Agency PRODEX contract. This research was supported by the Research Council of Norway through the grant "Solar Atmospheric Modelling" and through grants of computing time from the Programme for Supercomputing. This work is supported by NASA contract NNG09FA40C (IRIS), the Lockheed Martin Independent Research Program, and European Research Council grant agreement no. 291058. Authors from the Smithsonian Astrophysical Observatory are supported by LMSAL contract 8100002705. The data presented in this paper may be found on the Hinode Science Data Centre Europe (www.sdc.uio.no). NR 25 TC 26 Z9 26 U1 1 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 17 PY 2014 VL 346 IS 6207 AR 1255757 DI 10.1126/science.1255757 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ7ZY UT WOS:000343041100034 PM 25324399 ER PT J AU Peter, H Tian, H Curdt, W Schmit, D Innes, D De Pontieu, B Lemen, J Title, A Boerner, P Hurlburt, N Tarbell, TD Wuelser, JP Martinez-Sykora, J Kleint, L Golub, L McKillop, S Reeves, KK Saar, S Testa, P Kankelborg, C Jaeggli, S Carlsson, M Hansteen, V AF Peter, H. Tian, H. Curdt, W. Schmit, D. Innes, D. De Pontieu, B. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T. D. Wuelser, J. P. Martinez-Sykora, Juan Kleint, L. Golub, L. McKillop, S. Reeves, K. K. Saar, S. Testa, P. Kankelborg, C. Jaeggli, S. Carlsson, M. Hansteen, V. TI Hot explosions in the cool atmosphere of the Sun SO SCIENCE LA English DT Article ID ELLERMAN BOMBS; H-ALPHA; SOLAR; FLUX; EMERGENCE; REGION; CHROMOSPHERE; CONVECTION AB The solar atmosphere was traditionally represented with a simple one-dimensional model. Over the past few decades, this paradigm shifted for the chromosphere and corona that constitute the outer atmosphere, which is now considered a dynamic structured envelope. Recent observations by the Interface Region Imaging Spectrograph (IRIS) reveal that it is difficult to determine what is up and down, even in the cool 6000-kelvin photosphere just above the solar surface: This region hosts pockets of hot plasma transiently heated to almost 100,000 kelvin. The energy to heat and accelerate the plasma requires a considerable fraction of the energy from flares, the largest solar disruptions. These IRIS observations not only confirm that the photosphere is more complex than conventionally thought, but also provide insight into the energy conversion in the process of magnetic reconnection. C1 [Peter, H.; Curdt, W.; Schmit, D.; Innes, D.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Tian, H.; Golub, L.; McKillop, S.; Reeves, K. K.; Saar, S.; Testa, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Pontieu, B.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Martinez-Sykora, Juan; Kleint, L.] LMSAL, Palo Alto, CA 94304 USA. [Martinez-Sykora, Juan; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94305 USA. [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [De Pontieu, B.; Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. RP Peter, H (reprint author), Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. EM peter@mps.mpg.de RI Reeves, Katharine/P-9163-2014 FU Norwegian Space Centre through European Space Agency PRODEX; NASA [NNG09FA40C, NNX11AO98G]; Lockheed Martin Independent Research Program; European Research Council [291058] FX H.P. thanks LMSAL for hospitality during his visit. We thank R. Rutten for countless comments and good discussions and two anonymous referees for valuable comments. 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 Centre through a European Space Agency PRODEX contract. This work is supported by NASA contract NNG09FA40C (IRIS), the Lockheed Martin Independent Research Program, European Research Council grant agreement 291058, and NASA grant NNX11AO98G. The Solar Dynamics Observatory (SDO) data that we used are provided courtesy of NASA/SDO and the Atmospheric Imaging Assembly and Helioseismic and Magnetic Imager science teams. All data used in this study are publicly available through the Virtual Solar Observatory (http://sdac.virtualsolar.org). The IRIS data are archived at http://iris.lmsal.com/data.html, where manuals for data reduction are also available. NR 27 TC 47 Z9 48 U1 1 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 17 PY 2014 VL 346 IS 6207 AR 1255726 DI 10.1126/science.1255726 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ7ZY UT WOS:000343041100033 PM 25324397 ER PT J AU Testa, P De Pontieu, B Allred, J Carlsson, M Reale, F Daw, A Hansteen, V Martinez-Sykora, J Liu, W DeLuca, EE Golub, L McKillop, S Reeves, K Saar, S Tian, H Lemen, J Title, A Boerner, P Hurlburt, N Tarbell, TD Wuelser, JP Kleint, L Kankelborg, C Jaeggli, S AF Testa, P. De Pontieu, B. Allred, J. Carlsson, M. Reale, F. Daw, A. Hansteen, V. Martinez-Sykora, J. Liu, W. DeLuca, E. E. Golub, L. McKillop, S. Reeves, K. Saar, S. Tian, H. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T. D. Wuelser, J. P. Kleint, L. Kankelborg, C. Jaeggli, S. TI Evidence of nonthermal particles in coronal loops heated impulsively by nanoflares SO SCIENCE LA English DT Article ID X-RAY OBSERVATIONS; SOLAR-FLARES; FREQUENCY-DISTRIBUTIONS; ELECTRON ACCELERATION; WAVES; CHROMOSPHERE; PROPAGATION; STATISTICS; EMISSION; PLASMA AB The physical processes causing energy exchange between the Sun's hot corona and its cool lower atmosphere remain poorly understood. The chromosphere and transition region (TR) form an interface region between the surface and the corona that is highly sensitive to the coronal heating mechanism. High-resolution observations with the Interface Region Imaging Spectrograph (IRIS) reveal rapid variability (similar to 20 to 60 seconds) of intensity and velocity on small spatial scales (less than or similar to 500 kilometers) at the footpoints of hot and dynamic coronal loops. The observations are consistent with numerical simulations of heating by beams of nonthermal electrons, which are generated in small impulsive (less than or similar to 30 seconds) heating events called "coronal nanoflares." The accelerated electrons deposit a sizable fraction of their energy (less than or similar to 10(25) erg) in the chromosphere and TR. Our analysis provides tight constraints on the properties of such electron beams and new diagnostics for their presence in the nonflaring corona. C1 [Testa, P.; DeLuca, E. E.; Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Pontieu, B.; Liu, W.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Kleint, L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [De Pontieu, B.; Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Allred, J.; Daw, A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reale, F.] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy. [Reale, F.] Ist Nazl Astrofis INAF, Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Liu, W.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Testa, P (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014; OI Reale, Fabio/0000-0002-1820-4824 FU Norwegian Space Center (NSC, Norway) through European Space Agency PRODEX; NASA [NNG09FA40C, NNX13AF79G]; Lockheed Martin Independent Research Program; European Research Council from Lockheed-Martin [291058, 8100002705]; Research Council of Norway FX IRIS is a NASA Small Explorer mission, developed and operated by Lockheed Martin Solar and Astrophysics Laboratory 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 European Space Agency PRODEX contract. The IRIS data can be accessed at http://iris.lmsal.com/search/, and the AIA data at www.lmsal.com/get_aia_data/. This work is supported by NASA under contract NNG09FA40C (IRIS) and the Lockheed Martin Independent Research Program, the European Research Council grant agreement no.291058, and contract 8100002705 from Lockheed-Martin to the Smithsonian Astrophysical Observatory. M.C. acknowledges funding from the Research Council of Norway. W.L. is supported by NASA Living with a Star-Targeted Research and Technology grant NNX13AF79G. NR 30 TC 37 Z9 37 U1 4 U2 17 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 17 PY 2014 VL 346 IS 6207 AR 1255724 DI 10.1126/science.1255724 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ7ZY UT WOS:000343041100032 PM 25324396 ER PT J AU Tian, H DeLuca, EE Cranmer, SR De Pontieu, B Peter, H Martinez-Sykora, J Golub, L McKillop, S Reeves, KK Miralles, MP McCauley, P Saar, S Testa, P Weber, M Murphy, N Lemen, J Title, A Boerner, P Hurlburt, N Tarbell, TD Wuelser, JP Kleint, L Kankelborg, C Jaeggli, S Carlsson, M Hansteen, V McIntosh, SW AF Tian, H. DeLuca, E. E. Cranmer, S. R. De Pontieu, B. Peter, H. Martinez-Sykora, J. Golub, L. McKillop, S. Reeves, K. K. Miralles, M. P. McCauley, P. Saar, S. Testa, P. Weber, M. Murphy, N. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Tarbell, T. D. Wuelser, J. P. Kleint, L. Kankelborg, C. Jaeggli, S. Carlsson, M. Hansteen, V. McIntosh, S. W. TI Prevalence of small-scale jets from the networks of the solar transition region and chromosphere SO SCIENCE LA English DT Article ID ALFVENIC WAVES; II SPICULES; WIND; CORONA; ENERGY; RECONNECTION; ORIGIN; SUMER; POWER AB As the interface between the Sun's photosphere and corona, the chromosphere and transition region play a key role in the formation and acceleration of the solar wind. Observations from the Interface Region Imaging Spectrograph reveal the prevalence of intermittent small-scale jets with speeds of 80 to 250 kilometers per second from the narrow bright network lanes of this interface region. These jets have lifetimes of 20 to 80 seconds and widths of = 300 kilometers. They originate from small-scale bright regions, often preceded by footpoint brightenings and accompanied by transverse waves with amplitudes of similar to 20 kilometers per second. Many jets reach temperatures of at least similar to 10(5) kelvin and constitute an important element of the transition region structures. They are likely an intermittent but persistent source of mass and energy for the solar wind. C1 [Tian, H.; DeLuca, E. E.; Cranmer, S. R.; Golub, L.; McKillop, S.; Reeves, K. K.; Miralles, M. P.; McCauley, P.; Saar, S.; Testa, P.; Weber, M.; Murphy, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Pontieu, B.; Martinez-Sykora, J.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Kleint, L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Peter, H.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Kankelborg, C.; Jaeggli, S.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [McIntosh, S. W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hui.tian@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014; McCauley, Patrick/P-7747-2015; OI McCauley, Patrick/0000-0002-1450-7350; Murphy, Nicholas/0000-0001-6628-8033 FU Norwegian Space Center (Norway) through European Space Agency PRODEX; NASA [NNG09FA40C, NNX11AO98G]; Lockheed Martin Independent Research Program; European Research Council from LMSAL [291058, 8100002705] FX IRIS is a NASA Small Explorer mission developed and operated by the Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), with mission operations executed at the NASA Ames Research Center and major contributions to downlink communications funded by the Norwegian Space Center (Norway) through a European Space Agency PRODEX contract. This work is supported by NASA contract NNG09FA40C (IRIS), the Lockheed Martin Independent Research Program, European Research Council grant agreement no. 291058, contract 8100002705 from LMSAL to the Smithsonian Astrophysical Observatory, and NASA grant NNX11AO98G. The publicly available IRIS data (including the data used in this study) are archived at http://iris.lmsal.com/data.html. NR 31 TC 58 Z9 60 U1 2 U2 11 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD OCT 17 PY 2014 VL 346 IS 6207 AR 1255711 DI 10.1126/science.1255711 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ7ZY UT WOS:000343041100031 PM 25324395 ER PT J AU Evangelista, D Cam, S Huynh, T Kwong, A Mehrabani, H Tse, K Dudley, R AF Evangelista, Dennis Cam, Sharlene Tony Huynh Kwong, Austin Mehrabani, Homayun Tse, Kyle Dudley, Robert TI Shifts in stability and control effectiveness during evolution of Paraves support aerial maneuvering hypotheses for flight origins SO PEERJ LA English DT Article DE Stability; Control effectiveness; Maneuvering; Flight; Evolution; Paraves; Biomechanics; Directed aerial descent ID FEATHERED DINOSAUR MICRORAPTOR; ANIMAL FLIGHT; HEXAPEDAL RUNNERS; PHYSICAL MODELS; CRETACEOUS BIRD; AVIAN EVOLUTION; FLAPPING FLIGHT; YAW STABILITY; LEG FEATHERS; CHINA AB The capacity for aerial maneuvering was likely a major influence on the evolution of flying animals. Here we evaluate consequences of paravian morphology for aerial performance by quantifying static stability and control effectiveness of physical models for numerous taxa sampled from within the lineage leading to birds (Paraves). Results of aerodynamic testing are mapped phylogenetically to examine how maneuvering characteristics correspond to tail shortening, forewing elaboration, and other morphological features. In the evolution of Paraves we observe shifts from static stability to inherently unstable aerial planforms; control effectiveness also migrated from tails to the forewings. These shifts suggest that a some degree of aerodynamic control and capacity for maneuvering preceded the evolution of a strong power stroke. The timing of shifts also suggests features normally considered in light of development of a power stroke may play important roles in control. C1 [Evangelista, Dennis; Cam, Sharlene; Tony Huynh; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Kwong, Austin; Mehrabani, Homayun] Univ Calif Berkeley, Dept Bioengn, Berkeley, CA 94720 USA. [Tse, Kyle] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. Univ N Carolina, Chapel Hill, NC USA. RP Evangelista, D (reprint author), Univ N Carolina, Chapel Hill, NC 27515 USA. EM devangel77b@gmail.com FU NSF; UC Chancellor's Fellowship; NSF Integrative Graduate Education and Research Traineeship (IGERT) [DGE-0903711]; University of California Museum of Palaeontology (UCMP) FX DE was supported by an NSF Minority Graduate Research Fellowship, UC Chancellor's Fellowship, and NSF Integrative Graduate Education and Research Traineeship (IGERT) #DGE-0903711. TH was supported by the University of California Museum of Palaeontology (UCMP). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 85 TC 6 Z9 6 U1 0 U2 20 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD OCT 16 PY 2014 VL 2 AR e632 DI 10.7717/peerj.632 PG 25 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY5PF UT WOS:000347623700005 PM 25337460 ER PT J AU Johnson, JB Lyons, JJ Andrews, BJ Lees, JM AF Johnson, Jeffrey B. Lyons, J. J. Andrews, B. J. Lees, J. M. TI Explosive dome eruptions modulated by periodic gas-driven inflation SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SOUFRIERE HILLS VOLCANO; SANTIAGUITO VOLCANO; LAVA DOME; GUATEMALA; MONTSERRAT; BEHAVIOR; TILT AB Volcan Santiaguito (Guatemala) "breathes" with extraordinary regularity as the edifice's conduit system accumulates free gas, which periodically vents to the atmosphere. Periodic pressurization controls explosion timing, which nearly always occurs at peak inflation, as detected with tiltmeters. Tilt cycles in January 2012 reveal regular 26 +/- 6 min inflation/deflation cycles corresponding to at least similar to 10(1) kg/s of gas fluxing the system. Very long period (VLP) earthquakes presage explosions and occur during cycles when inflation rates are most rapid. VLPs locate similar to 300 m below the vent and indicate mobilization of volatiles, which ascend at similar to 50 m/s. Rapid gas ascent feeds pyroclast-laden eruptions lasting several minutes and rising to similar to 1 km. VLPs are not observed during less rapid inflation episodes; instead, gas vents passively through the conduit producing no infrasound and no explosion. These observations intimate that steady gas exsolution and accumulation in shallow reservoirs may drive inflation cycles at open-vent silicic volcanoes. C1 [Johnson, Jeffrey B.] Boise State Univ, Dept Geosci, Boise, ID 83725 USA. [Lyons, J. J.] USGS, Alaska Volcano Observ, Anchorage, AK USA. [Andrews, B. J.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Lees, J. M.] Univ N Carolina, Dept Geol Sci, Chapel Hill, NC USA. RP Johnson, JB (reprint author), Boise State Univ, Dept Geosci, Boise, ID 83725 USA. EM jeffreybjohnson@boisestate.edu FU INSIVUMEH; Policia Nacional Civil de Guatemala; Instituto Guatemalteco de Turismo; National Science Foundation [EAR 0838562]; Smithsonian Natural History Museum Small Grant FX We thank INSIVUMEH, the Policia Nacional Civil de Guatemala, and the Instituto Guatemalteco de Turismo for support. Fieldwork was carried out with support from Armando Pineda and Jake Anderson. The project was supported by a grant from the National Science Foundation (EAR 0838562) and a Smithsonian Natural History Museum Small Grant. We thank IRIS PASSCAL for hardware support. Santiaguito seismic data are available from the IRIS DMC. NR 26 TC 8 Z9 8 U1 3 U2 11 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 OCT 16 PY 2014 VL 41 IS 19 BP 6689 EP 6697 DI 10.1002/2014GL061310 PG 9 WC Geosciences, Multidisciplinary SC Geology GA AT4MP UT WOS:000344913800020 ER PT J AU Mironov, AN Pawson, DL AF Mironov, Alexandr N. Pawson, David L. TI A new species of Western Atlantic sea lily in the family Bathycrinidae (Echinodermata: Crinoidea), with a discussion of relationships between crinoids with xenomorphic stalks SO ZOOTAXA LA English DT Article DE Discolocrinus iselini n. sp.; Bahamas; deep-sea; taxonomy; Echinodermata; Crinoidea; Bathycrinidae; knobby processes ID MOLECULAR-DATA; MORPHOLOGY; PHYLOGENY; GENUS AB A new species in the family Bathycrinidae is described from abyssal depths from the Bahamas. It is referred to the recently established genus Discolocrinus, which formerly comprised a single species D. thieli Mironov, 2008 from the Eastern Pacific. Discolocrinus iselini n. sp. is characterized by large body size, high tegmen with tube-like upper region, extremely elongated IBr1 and IBr2, large knobby processes on primibrachials, and overgrowth of soft tissue on the pinnules, the tissue containing numerous perforated or imperforate ossicles of varying size and form. Differences between Discolocrinus and other bathycrinids may seem to be of taxonomic importance at the family level, but knowledge of the morphology and variability of both species of Discolocrinus is incomplete and, until a richer material becomes available, the genus should remain in family Bathycrinidae. Representatives of five families with xenomorphic stalks were examined to characterize the genera on the basis of number or form of knobby processes. These processes occur in two families with differing external morphology: ten-armed Bathycrinidae and five-armed Bourgueticrinidae. They also occur in the comatulid family Atelecrinidae. This similarity might seem to indicate a close relationship between the three families. However, morphological analysis supports the separation of the families Caledonicrinidae and Septocrinidae from Bathycrinidae despite the fact that they share a xenomorphic stalk and IBr2ax. These conclusions are in agreement with results of recent molecular studies. C1 [Mironov, Alexandr N.] Russian Acad Sci, PP Shirshov Oceanol Inst, Moscow 117997, Russia. [Pawson, David L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Mironov, AN (reprint author), Russian Acad Sci, PP Shirshov Oceanol Inst, Nakhimovsky Prospekt 36, Moscow 117997, Russia. EM miron@ocean.ru; pawsond@si.edu NR 29 TC 1 Z9 1 U1 0 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 OCT 16 PY 2014 VL 3873 IS 3 BP 259 EP 274 PG 16 WC Zoology SC Zoology GA AR2FF UT WOS:000343398300005 PM 25544221 ER PT J AU Hong, T AF Hong, Terry TI The Seventh Day SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20013 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 2014 VL 139 IS 17 BP 86 EP 86 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA AQ4AC UT WOS:000342733600125 ER PT J AU Kral, K McMahon, SM Janik, D Adam, D Vrska, T AF Kral, Kamil McMahon, Sean M. Janik, David Adam, Dusan Vrska, Tomas TI Patch mosaic of developmental stages in central European natural forests along vegetation gradient SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Developmental stage; Stand mosaic; Patch pattern; Mean patch size; Forest dynamics; Spatial analysis ID STAND DEVELOPMENT STAGES; STRUCTURAL DYNAMICS; SPATIAL-PATTERN; BEECH FORESTS; GAP; REGENERATION; CARPATHIANS; CYCLE; BIODIVERSITY; PERSPECTIVE AB The shifting mosaic of patches in different phases of forest development is a widely used framework for describing stand dynamics, structure and biodiversity in European temperate forests. In spite of the common application of patch mapping of developmental stages/phases, an objective and quantified evaluation of patch mosaics has been missing. This approach identifies patches of forest stand according to a developmental trajectory, from Growth, through an Optimum stage to Breakdown. Here we present the first attempt to compare quantitative and qualitative characteristics of patch mosaics of stand developmental stages using three decades of extensive data in five study sites along a vegetation gradient. We do this using the same, observer independent method based on an artificial neural network classifier. We also used the historical stem position datasets to evaluate the change of mosaic characteristics in time. Resulting patch patterns were analyzed by standard mosaic metrics commonly used in landscape ecology, evaluating area, shape, aggregation and connectivity of patches. The mean patch size of the mosaic of four developmental stages showed a relatively narrow range of 570-800 m(2) in all study sites and censuses. The shape of patches in all sites and years had no significant differences, and the aggregation of patches of the same type was similar in all sites at the mosaic level. Conversely, we did find some stage-specific patterns. For example, the Growth stage was usually the most abundant (covering 25-50% of the stand), and had the highest mean patch size, ranging between 590 and 2800 m(2). The Growth stage patches also had the most complex shapes. On the contrary, the Breakdown stage usually had the opposite values, forming constantly small (250-720 m(2)), simple and scattered patches in the mosaic. These basic traits were found in all study sites and were stable in time. We also found some common trends in the dataset, such as increasing mean patch size of the Breakdown stage along the altitudinal vegetation gradient. The complex Steady State stage was generally more abundant than expected according to results of other studies and thus might indicate processes that have not been well described in previous, subjective, applications of the patch mosaic paradigm. (C) 2014 Elsevier B.V. All rights reserved. C1 [Kral, Kamil; Janik, David; Adam, Dusan; Vrska, Tomas] Silva Tarouca Res Inst Landscape & Ornamental Gar, Dept Forest Ecol, CZ-60200 Brno, Czech Republic. [McMahon, Sean M.] Smithsonian Environm Res Ctr, Forest Global Earth Observ, Smithsonian Inst, Edgewater, MD 21037 USA. RP Kral, K (reprint author), Silva Tarouca Res Inst Landscape & Ornamental Gar, Dept Forest Ecol, Lidicka 25-27, CZ-60200 Brno, Czech Republic. EM kamil.kral@vukoz.cz RI Kral, Kamil/E-4415-2014 FU Czech Ministry of Education, Youth and Sports [LH12038] FX We are grateful to all the people who participated in the natural forest sites censuses. Special thanks to Eduard Prusa for establishing the study sites. This research was funded by the Czech Ministry of Education, Youth and Sports (Project KONTAKT II - AMVIS No. LH12038). NR 78 TC 12 Z9 12 U1 3 U2 40 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 OCT 15 PY 2014 VL 330 BP 17 EP 28 DI 10.1016/j.foreco.2014.06.034 PG 12 WC Forestry SC Forestry GA AP7FZ UT WOS:000342244500003 ER PT J AU Khonmee, J Brown, JL Taya, K Rojanasthien, S Punyapornwithaya, V Thumasanukul, D Kongphoemphun, A Siriaroonrat, B Tipkantha, W Pongpiachan, P Thitaram, C AF Khonmee, Jaruwan Brown, Janine L. Taya, Kazuyoshi Rojanasthien, Suvichai Punyapornwithaya, Veerasak Thumasanukul, Dissakul Kongphoemphun, Adisorn Siriaroonrat, Boripat Tipkantha, Wanlaya Pongpiachan, Petai Thitaram, Chatchote TI Assessment of ovarian activity in captive goral (Naemorhedus griseus) using noninvasive fecal steroid monitoring SO THERIOGENOLOGY LA English DT Article DE Goral; Estrogen metabolites; Progestagen metabolites; Noninvasive hormone monitoring; Reproduction; Ovarian function ID CERVUS-ELDI-THAMIN; SEROW CAPRICORNIS-CRISPUS; WHITE-TAILED DEER; IBERIAN RED DEER; ESTROUS-CYCLE; JAPANESE SEROW; PROGESTERONE METABOLITES; PREGNANCY DETECTION; ENZYME-IMMUNOASSAY; REPRODUCTIVE-CYCLE AB To date, there is no information on gonadal steroidogenic activity of female goral (Naemorhedus griseus), a threatened species of Thailand. Captive goral populations have been established to produce animals for ex situ conservation and reintroduction, but as yet none are self-sustaining. The objectives of the present study were to (1) determine the influence of season on ovarian steriodogenic function; and (2) examine the relationship between gonadal hormone excretion and sexual behaviors throughout the year. Fecal samples were collected 5 to 7 days/wk for 15 months from 8 adult females housed at Omkoi Wildlife Breeding Center in Thailand and analyzed for ovarian steroid metabolites using validated enzyme immunoassays. Observations of sexual behaviors and mating were conducted each morning for 30 min/session. Based on fecal estrogen and progestagen metabolite concentrations, the overall estrous cycle length was about 21 days, with a 2- to 3-day follicular phase and an 18- to 20-day luteal phase. Sexual behaviors, most notably tail-up, increased for 2 to 3 days during the time estrogens were elevated during mating. Fecal progestagens were elevated during luteal phases and increased further during gestation, which lasted approximately 7 months. The lactation period was 5 months, and females were anestrus for 2 to 5 of those months, with the exception of one that cycled continuously throughout. Two females conceived around 2 months postpartum and so were pregnant during lactation. Birth records over the past 21 years indicated young are born throughout the year. This combined with the hormonal data suggests that female gorals are not strongly seasonal, at least in captivity, although there was considerable variation among females in estrogen and progestagen patterns. In conclusion, fecal steroid metabolite monitoring is an effective means of assessing ovarian function in this species and will be a useful tool for breeding management and planned development of assisted reproductive techniques such as artificial insemination and embryo transfer. (C) 2014 Elsevier Inc. All rights reserved. C1 [Khonmee, Jaruwan] Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Chiang Mai 50000, Thailand. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Taya, Kazuyoshi] Tokyo Univ Agr & Technol, Fac Agr, Dept Vet Med, Vet Physiol Lab, Tokyo, Japan. [Rojanasthien, Suvichai; Punyapornwithaya, Veerasak] Chiang Mai Univ, Dept Food Anim Clin, Fac Vet Med, Chiang Mai 50000, Thailand. [Thumasanukul, Dissakul; Kongphoemphun, Adisorn] Omkoi Wildlife Sanctuary, Dept Natl Parks Wildlife & Plant Conservat, Chiang Mai, Thailand. [Siriaroonrat, Boripat; Tipkantha, Wanlaya] Zool Pk Org, Bur Conservat Res & Educ, Dusit, Bankok, Thailand. [Pongpiachan, Petai] Chiang Mai Univ, Dept Anim & Aquat Sci, Fac Agr, Chiang Mai 50000, Thailand. [Thitaram, Chatchote] Chiang Mai Univ, Fac Vet Med, Dept Compan Anim & Wildlife Clin, Chiang Mai 50000, Thailand. RP Khonmee, J (reprint author), Chiang Mai Univ, Fac Vet Med, Dept Vet Biosci & Publ Hlth, Chiang Mai 50000, Thailand. EM jaruwan.khonmee@cmu.ac.th FU National Research Council of Thailand [96867]; Graduate School of Chiang Mai University [27-12-2553] FX This study was supported by National Research Council of Thailand (Grant number 96867) and the Graduate School of Chiang Mai University (Grant number 27-12-2553). The authors extend their gratitude to the staff of the Omkoi Wildlife Sanctuary and Zoological Park Organization of Thailand for their assistance in sample collection. The authors are also grateful to Ms. Nicole Presley at the Smithsonian Conservation Biology Institute and staff of the endocrinology laboratory at the Faculty of Veterinary Medicine, Chiang Mai University (Ms. Manisorn Tuantammarak, Ms. Patharanun Wongchai, and Mr. Pallop Tankaew) for technical support. NR 71 TC 2 Z9 2 U1 4 U2 17 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 OCT 15 PY 2014 VL 82 IS 7 BP 997 EP 1006 DI 10.1016/j.theriogenology.2014.07.012 PG 10 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA AP8KW UT WOS:000342328900009 PM 25132101 ER PT J AU Zaiss, J Ravizza, G Goderis, S Sauvage, J Claeys, P Johnson, K AF Zaiss, Jessica Ravizza, Greg Goderis, Steven Sauvage, Justine Claeys, Philippe Johnson, Kirk TI A complete Os excursion across a terrestrial Cretaceous-Paleogene boundary at the West Bijou Site, Colorado, with evidence for recent open system behavior SO CHEMICAL GEOLOGY LA English DT Article DE Osmium isotopes; K-Pg boundary; Rhenium; Iridium ID PLATINUM-GROUP ELEMENTS; OSMIUM ISOTOPIC COMPOSITION; PARTICULATE ORGANIC CARBON; TERTIARY BOUNDARY; BLACK SHALE; CHONDRITIC IMPACTOR; ICP-MS; RHENIUM; SEDIMENTS; RECORD AB The few previously reported values of Os-187/Os-188 ratios from non-marine K-Pg boundary sections are distinctly higher than the range of Os-187/Os-188 ratios measured in chondrites and the range of ratios predicted by models of physical mixing between chondrites and upper crust. Here, Re-Os data from the West Bijou continental K-Pg boundary site, located within the Denver Basin, are used to better constrain the Os isotopic composition of fallout from the Chicxulub ejecta plume. For the first time, full vertical profiles of Os-187/Os-188 ratios and Re and Os concentrations across a continental K-Pg boundary section are reported. Within this section of lignite, the lowest measured Os-187/Os-188 ratio (0.182) coincides with the K-Pg boundary interval as previously determined by palynology and the distribution of shocked quartz in a nearby outcrop. However, sediments with elevated Os concentrations and measured Os-187/Os-188 below 0.23 extend over a 30 cm interval, from similar to 5 cm above the clay-rich boundary interval (similar to 5 cm thick) to similar to 25 cm below. Maximum Ir and Os concentrations occur 3 cm and 10 cm below the K-Pg boundary, respectively, demonstrating greater diagenetic mobility of Os relative to Ir. Low Os-187/Os-188 above the K-Pg boundary suggests that accumulation of impact derived Os at this site persisted after the impact event, perhaps due to redistribution of impact debris in the surrounding area. Importantly, calculated initial Os-187/Os-188 ratios throughout most of the section are impossibly low and require open system behavior, likely in the form of Re addition within the last 10 million years. Within the boundary interval, Re concentrations are among the lowest measured at Bowring Pit and calculated initial Os-187/Os-188 ratios are very similar to those previously reported from the western interior of the United States K-Pg boundary material (similar to 0.14), suggesting super-chondritic Os-187/Os-188 is characteristic of the Chicxulub ejecta plume. Beyond implications for our understanding of Os as an impact tracer, this study emphasizes the dramatic effect diagenesis can have on the Re-Os system in organic-rich environments, especially through post-depositional addition of Re. (C) 2014 Elsevier B.V. All rights reserved. C1 [Zaiss, Jessica; Ravizza, Greg] Univ Hawaii Manoa, Dept Geol & Geophys, SOEST, Honolulu, HI 96822 USA. [Goderis, Steven; Sauvage, Justine; Claeys, Philippe] Vrije Univ Brussel, Brussels, Belgium. [Johnson, Kirk] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Zaiss, J (reprint author), 1680 East West Rd,POST 842A, Honolulu, HI 96822 USA. EM zaiss@hawaii.edu RI Claeys, Philippe/B-4895-2008; Goderis, Steven/F-9908-2011 OI Claeys, Philippe/0000-0002-4585-7687; Goderis, Steven/0000-0002-6666-7153 FU NSF [EAR0843930]; Research Foundation Flanders (FWO) [G0B8513, G009113] FX We would like to thank Laurie Reisberg, Christian Koeberl, and an anonymous reviewer for very helpful suggestions. We would also like to thank Denys VonderHaar for her help in the lab, and ACS-PRF for support while JZ prepared this manuscript. This work was supported by NSF award EAR0843930 to G. Ravizza and Research Foundation Flanders (FWO grants G0B8513 and G009113) to Ph. Claeys. Steven Goderis is an FWO postdoctoral Fellow. Justine Sauvage and Philippe Claeys collected the samples. Property access was allowed by the Plains Conservation Center. NR 67 TC 2 Z9 2 U1 1 U2 17 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 EI 1878-5999 J9 CHEM GEOL JI Chem. Geol. PD OCT 14 PY 2014 VL 385 BP 7 EP 16 DI 10.1016/j.chemgeo.2014.07.010 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AU2IH UT WOS:000345440900002 ER PT J AU Datovo, A de Pinna, MCC Johnson, GD AF Datovo, Alessio de Pinna, Mario C. C. Johnson, G. David TI The Infrabranchial Musculature and Its Bearing on the Phylogeny of Percomorph Fishes (Osteichthyes: Teleostei) SO PLOS ONE LA English DT Article ID MITOCHONDRIAL-DNA SEQUENCES; PHARYNGEAL JAW APPARATUS; RAY-FINNED FISH; MOLECULAR PHYLOGENY; COMPARATIVE ANATOMY; SCOMBROID FISHES; STRIATED-MUSCLES; LABROID FISHES; HEAD-MUSCLES; GILL ARCHES AB The muscles serving the ventral portion of the gill arches (= infrabranchial musculature) are poorly known in bony fishes. A comparative analysis of the infrabranchial muscles in the major percomorph lineages reveals a large amount of phylogenetically-relevant information. Characters derived from this anatomical system are identified and discussed in light of current hypotheses of phylogenetic relationships among percomorphs. New evidence supports a sister-group relationship between the Batrachoidiformes and Lophiiformes and between the Callionymoidei and Gobiesocoidei. Investigated data also corroborate the existence of two monophyletic groups, one including the Pristolepididae, Badidae, and Nandidae, and a second clade consisting of all non-amarsipid stromateiforms. New synapomorphies are proposed for the Atherinomorphae, Blenniiformes, Lophiiformes, Scombroidei (including Sphyraenidae), and Gobiiformes. Within the latter order, the Rhyacichthyidae and Odontobutidae are supported as the successive sister families of all remaining gobiiforms. The present analysis further confirms the validity of infrabranchial musculature characters previously proposed to support the grouping of the Mugiliformes with the Atherinomorphae and the monophyly of the Labriformes with the possible inclusion of the Pholidichthyiformes. Interestingly, most hypotheses of relationships supported by the infrabranchial musculature have been advanced by preceding anatomists on the basis of distinct data sources, but were never recovered in recent molecular phylogenies. These conflicts clearly indicate the current unsatisfactory resolution of the higher-level phylogeny of percomorphs. C1 [Datovo, Alessio; de Pinna, Mario C. C.] Univ Sao Paulo, Museu Zool, Lab Ictiol, Sao Paulo, Brazil. [Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes,MRC 159, Washington, DC 20560 USA. RP Datovo, A (reprint author), Univ Sao Paulo, Museu Zool, Lab Ictiol, Sao Paulo, Brazil. EM adatovo@usp.br RI Datovo, Alessio/K-7133-2016; Museu de Zoologia da USP, MZ-USP/Q-2192-2016 FU Sao Paulo Research Foundation (FAPESP) [2010/18984-9] FX This study was funded by a Postdoctoral Fellowship from Sao Paulo Research Foundation (FAPESP; grant #2010/18984-9). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 117 TC 5 Z9 5 U1 3 U2 10 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 13 PY 2014 VL 9 IS 10 AR e110129 DI 10.1371/journal.pone.0110129 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ9WZ UT WOS:000343210300092 PM 25310286 ER PT J AU Bonafede, A Intema, HT Bruggen, M Russell, HR Ogrean, G Basu, K Sommer, M van Weeren, RJ Cassano, R Fabian, AC Rottgering, HJA AF Bonafede, A. Intema, H. T. Brueggen, M. Russell, H. R. Ogrean, G. Basu, K. Sommer, M. van Weeren, R. J. Cassano, R. Fabian, A. C. Roettgering, H. J. A. TI A giant radio halo in the cool core cluster CL1821+643 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; radiation mechanism: non-thermal; methods: observational; galaxies: clusters: individual: CL1821+643 PSZ1 G094.00+274; galaxies: clusters: intracluster medium; radio continuum: general ID GALAXY CLUSTERS; NONTHERMAL EMISSION; SCALE; DISCOVERY; MERGERS AB Giant radio haloes are Mpc-size sources found in some merging galaxy clusters. The synchrotron emitting electrons are thought to be (re)accelerated by plasma turbulence induced by the merging of two massive clusters. Cool core galaxy clusters have a low-temperature core, likely an indication that a major merger has not recently occurred. CL1821+643 is one of the strongest cool core clusters known so far. Surprisingly, we detect a giant radio halo with a largest linear size of similar to 1.1 Mpc. We discuss the radio and X-ray properties of the cluster in the framework of the proposed models for giant radio haloes. If a merger is causing the radio emission, despite the presence of a cool core, we suggest that it should be off-axis, or in an early phase, or a minor one. C1 [Bonafede, A.; Brueggen, M.; Ogrean, G.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Intema, H. T.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Russell, H. R.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Basu, K.; Sommer, M.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cassano, R.] Ist Radioastron INAF, I-40129 Bologna, Italy. [Roettgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Bonafede, A (reprint author), Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM annalisa.bonafede@hs.uni-hamburg.de RI Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; Cassano, Rossella/0000-0003-4046-0637; van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft [FOR 1254]; ERC; NASA [PF2-130104]; Chandra X-ray Center, SAO for NASA [NAS8-03060] FX We thank F. de Gasperin and F. Vazza for useful discussions. AB and MB acknowledge support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft. HR acknowledges support from ERC Advanced Grant Feedback. RJW is supported by NASA through Einstein Postdoctoral grant PF2-130104 (Chandra X-ray Center, SAO for NASA, contract NAS8-03060). We also thank the staff of the GMRT. NRAO is a facility of the National Science Foundation operated under Associated Universities Inc. NR 28 TC 12 Z9 12 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2014 VL 444 IS 1 BP L44 EP L48 DI 10.1093/mnrasl/slu110 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3MK UT WOS:000344181600008 ER PT J AU Dauser, T Garcia, J Parker, ML Fabian, AC Wilms, J AF Dauser, T. Garcia, J. Parker, M. L. Fabian, A. C. Wilms, J. TI The role of the reflection fraction in constraining black hole spin SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; line: profiles; galaxies: active; galaxies: nuclei ID ACTIVE GALACTIC NUCLEI; X-RAY REFLECTION; K-ALPHA LINE; ACCRETION DISK; CYGNUS X-1; XMM-NEWTON; IRON K; GX 339-4; SPECTRAL VARIABILITY; EMISSION-LINES AB In many active galaxies, the X-ray reflection features from the innermost regions of the accretion disc are relativistically distorted. This distortion allows us to measure parameters of the black hole such as its spin. The ratio in flux between the direct and the reflected radiation, the so-called reflection fraction, is determined directly from the geometry and location of primary source of radiation. We calculate the reflection fraction in the lamp post geometry in order to determine its maximal possible value for a given value of black hole spin. We show that high reflection fractions in excess of two are only possible for rapidly rotating black holes, suggesting that the high spin sources produce the strongest relativistic reflection features. Using simulations we show that taking this constraint into account does significantly improve the determination of the spin values. We make software routines for the most popular X-ray data analysis packages available that incorporate these additional constraints. C1 [Dauser, T.; Wilms, J.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.; Wilms, J.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parker, M. L.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Dauser, T (reprint author), Dr Karl Remeis Observ, Sternwartstr 7, D-96049 Bamberg, Germany. EM thomas.dauser@sternwarte.uni-erlangen.de RI Wilms, Joern/C-8116-2013 OI Wilms, Joern/0000-0003-2065-5410 FU Elitenetzwerk Bayern; Deutsches Zentrum fur Luft- und Raumfahrt [50 OR 1113]; NASA [NNX11AD08G] FX TD acknowledges support by a fellowship from the Elitenetzwerk Bayern, and by the Deutsches Zentrum fur Luft- und Raumfahrt under contract number 50 OR 1113. JG acknowledges the support of NASA grant NNX11AD08G. We thank John E. Davis for the development of the SLXFIG module used to prepare the figures in this letter. This research has made use of ISIS functions provided by ECAP/Remeis observatory and MIT (http://www.sternwarte.uni-erlangen.de/isis/). NR 56 TC 30 Z9 30 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2014 VL 444 IS 1 BP L100 EP L104 DI 10.1093/mnrasl/slu125 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3MK UT WOS:000344181600020 ER PT J AU Kilic, M Brown, WR Gianninas, A Hermes, JJ Prieto, CA Kenyon, SJ AF Kilic, Mukremin Brown, Warren R. Gianninas, A. Hermes, J. J. Allende Prieto, Carlos Kenyon, S. J. TI A new gravitational wave verification source SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational waves; binaries: close; stars: individual (SDSS J093506.93+441106.9, WD 0931+444); white dwarfs ID SMALL-MAGELLANIC-CLOUD; AFRICAN LARGE TELESCOPE; FOCUS IMAGING SPECTROGRAPH; LONG-PERIOD VARIABLES; EMISSION-LINE STARS; D-TYPE SYSTEMS; SYMBIOTIC STARS; GALACTIC BULGE; STELLAR PARAMETERS; PLANETARY-NEBULAE AB We report the discovery of a detached 20-min orbital period binary white dwarf (WD). WD 0931+444 (SDSS J093506.93+441106.9) was previously classified as a WD + M dwarf system based on its optical spectrum. Our time-resolved optical spectroscopy observations obtained at the 8 m Gemini and 6.5 m MMT reveal peak-to-peak radial velocity variations of a parts per thousand 400 km s(-1) every 20 min for the WD, but no velocity variations for the M dwarf. In addition, high-speed photometry from the McDonald 2.1 m telescope shows no evidence of variability nor evidence of a reflection effect. An M dwarf companion is physically too large to fit into a 20 min orbit. Thus, the orbital motion of the WD is almost certainly due to an invisible WD companion. The M dwarf must be either an unrelated background object or the tertiary component of a hierarchical triple system. WD 0931+444 contains a pair of WDs, a 0.32 M-aS (TM) primary and a a parts per thousand yen0.14 M-aS (TM) secondary, at a separation of a parts per thousand yen0.19 R-aS (TM). After J0651+2844, WD 0931+444 becomes the second shortest period detached binary WD currently known. The two WDs will lose angular momentum through gravitational wave radiation and merge in a parts per thousand currency sign9 Myr. The log h a parts per thousand integral -22 gravitational wave strain from WD 0931+444 is strong enough to make it a verification source for gravitational wave missions in the milli-Hertz frequency range, e.g. the evolved Laser Interferometer Space Antenna (eLISA), bringing the total number of known eLISA verification sources to nine. C1 [Kilic, Mukremin; Gianninas, A.] Univ Oklahoma, Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Allende Prieto, Carlos] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP Kilic, M (reprint author), Univ Oklahoma, Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 USA. EM kilic@ou.edu RI Alexandros, Gianninas/B-8352-2016; OI Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X FU Polish National Science Center [DEC-2011/01/B/ST9/06145]; European Research Council under the European Community's Seventh Framework Programme (FP7) / ERC [246678]; National Aeronautics and Space Administration; National Science Foundation; Polish time allocation committee; South African SALT time allocation committee FX Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT) and we would like to thank the Polish and South African SALT time allocation committees for the award of SALT time. We thank the anonymous referees for constructive reports including suggestions that helped improve this work. JM is supported by the Polish National Science Center grant number DEC-2011/01/B/ST9/06145. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement no. 246678 to AU. This research has made use of the SIMBAD data base and VizieR catalogue access tool, operated at CDS, Strasbourg, France. This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 61 TC 15 Z9 15 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 OCT 11 PY 2014 VL 444 IS 1 BP L1 EP L15 DI 10.1093/mnrasl/slu093 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3MK UT WOS:000344181600001 ER PT J AU Pillepich, A Vogelsberger, M Deason, A Rodriguez-Gomez, V Genel, S Nelson, D Torrey, P Sales, LV Marinacci, F Springel, V Sijacki, D Hernquist, L AF Pillepich, Annalisa Vogelsberger, Mark Deason, Alis Rodriguez-Gomez, Vicente Genel, Shy Nelson, Dylan Torrey, Paul Sales, Laura V. Marinacci, Federico Springel, Volker Sijacki, Debora Hernquist, Lars TI Halo mass and assembly history exposed in the faint outskirts: the stellar and dark matter haloes of Illustris galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; Galaxy: formation; Galaxy: halo; galaxies: formation; galaxies: haloes ID MILKY-WAY HALO; SURFACE BRIGHTNESS PROFILE; DRAGONFLY TELEPHOTO ARRAY; TELESCOPE LEGACY SURVEY; LARGE-SCALE STRUCTURE; COSMOLOGICAL SIMULATIONS; OUTER HALO; ACCRETION HISTORIES; FORMATION PHYSICS; ANDROMEDA GALAXY AB We use the Illustris simulations to gain insight into the build-up of the outer, low-surface brightness regions which surround galaxies. We characterize the stellar haloes by means of the logarithmic slope of the spherically averaged stellar density profiles, alpha(STARS) at z = 0, and we relate these slopes to the properties of the underlying dark matter (DM) haloes, their central galaxies, and their assembly histories. We analyse a sample of similar to 5000 galaxies resolved with more than 5 x 10(4) particles each, and spanning a variety of morphologies and halo masses (3 x 10(11) <= M-vir less than or similar to 10(14) M-circle dot). We find a strong trend between stellar halo slope and total halo mass, where more massive objects have shallower stellar haloes than the less massive ones (-5.5 +/- 0.5 < alpha(STARS) < -3.5 +/- 0.2 in the studied mass range). At fixed halo mass, we show that disc-like, blue, young, and more massive galaxies are surrounded by significantly steeper stellar haloes than elliptical, red, older, and less massive galaxies. Overall, the stellar density profiles fall off much more steeply than the underlying DM, and no clear trend holds between stellar slope and DM halo concentration. However, DM haloes which formed more recently, or which accreted larger fractions of stellar mass from infalling satellites, exhibit shallower stellar haloes than their older analogues with similar masses, by up to Delta alpha(STARS) similar to 0.5-0.7. Our findings, combined with the most recent measurements of the strikingly different stellar power-law indices for M31 and the Milky Way, appear to favour a massive M31, and a Milky Way characterized by a much quieter accretion history over the past 10 Gyr than its companion. C1 [Pillepich, Annalisa; Rodriguez-Gomez, Vicente; Genel, Shy; Nelson, Dylan; Torrey, Paul; Sales, Laura V.; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vogelsberger, Mark] MIT, Kavli Inst Astrophys & Space Res, Dept Phys, Cambridge, MA 02139 USA. [Deason, Alis] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Marinacci, Federico; Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Marinacci, Federico; Springel, Volker] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. [Sijacki, Debora] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sijacki, Debora] Univ Cambridge, Kavli Inst Cosmol, Cambridge CB3 0HA, England. RP Pillepich, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apillepich@cfa.harvard.edu OI Torrey, Paul/0000-0002-5653-0786; /0000-0003-3816-7028; Rodriguez-Gomez, Vicente/0000-0002-9495-0079 FU DFG Research Centre through project A1 [SFB-881]; NSF [1066293, AST-1312095]; European Research Council under ERC-StG grant [EXAGAL-308037]; NASA [NNX12AC67G]; CURIE supercomputer at CEA/France as part of PRACE project [RA0844]; SuperMUC computer at the Leibniz Computing Centre, Germany [pr85je] FX AP thanks Akos Bogdan, Arjun Dey, Tomer Tal, and Vasily Belokurov, for useful discussions. FM acknowledges support by the DFG Research Centre SFB-881 'The Milky Way System' through project A1. AP, AD, LS thank the Aspen Center for Physics and the NSF Grant #1066293 for hospitality during the final editing of this paper. VS acknowledges support by the European Research Council under ERC-StG grant EXAGAL-308037. LH acknowledges support from NASA grant NNX12AC67G and NSF award AST-1312095. Simulations were run on the Harvard Odyssey and CfA/ITC clusters, the Ranger and Stampede supercomputers at the Texas Advanced Computing Center as part of XSEDE, the Kraken supercomputer at Oak Ridge National Laboratory as part of XSEDE, the CURIE supercomputer at CEA/France as part of PRACE project RA0844, and the SuperMUC computer at the Leibniz Computing Centre, Germany, as part of project pr85je. NR 88 TC 26 Z9 26 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2014 VL 444 IS 1 BP 237 EP 249 DI 10.1093/mnras/stu1408 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100019 ER PT J AU Siwak, M Rucinski, SM Matthews, JM Guenther, DB Kuschnig, R Moffat, AFJ Rowe, JF Sasselov, D Weiss, WW AF Siwak, Michal Rucinski, Slavek M. Matthews, Jaymie M. Guenther, David B. Kuschnig, Rainer Moffat, Anthony F. J. Rowe, Jason F. Sasselov, Dimitar Weiss, Werner W. TI A stable quasi-periodic 4.18-d oscillation and mysterious occultations in the 2011 MOST light-curve of TW Hya SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion: accretion discs; stars: individual: TW Hya; stars: variables: T Tauri, Herbig Ae/Be ID MAGNETIC NEUTRON-STARS; MAGNETOSPHERIC ACCRETION MODELS; DISK ACCRETION; TAURI STARS; MAGNETOHYDRODYNAMIC SIMULATIONS; AB-AURIGAE; X-RAY; VARIABILITY; HYDRAE; PHOTOMETRY AB We present an analysis of the 2011 photometric observations of TW Hya by the MOST satellite; this is the fourth continuous series of this type. The large-scale light variations are dominated by a strong, quasi-periodic 4.18-d oscillation with superimposed, apparently chaotic flaring activity. The former is probably produced by stellar rotation with one large hotspot created by a stable accretion funnel, while the latter may be produced by small hotspots, created at moderate latitudes by unstable accretion tongues. A new, previously unnoticed feature is a series of semiperiodic, well-defined brightness dips of unknown nature, of which 19 were observed during 43 d of our nearly continuous observations. Re-analysis of the 2009 MOST light-curve revealed the presence of three similar dips. On the basis of recent theoretical results, we tentatively conclude that the dips may represent occultations of the small hotspots created by unstable accretion tongues by hypothetical optically thick clumps of dust. C1 [Siwak, Michal] Cracov Pedag Univ, Mt Suhora Astron Observ, PL-30084 Cracov, Poland. [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Matthews, Jaymie M.; Kuschnig, Rainer] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Guenther, David B.] St Marys Univ, Inst Computat Astrophys, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Siwak, M (reprint author), Cracov Pedag Univ, Mt Suhora Astron Observ, Ul Podchorazych 2, PL-30084 Cracov, Poland. EM siwak@nac.oa.uj.edu.pl FU Polish National Science Centre [2012/05/E/ST9/03915]; Natural Sciences and Engineering Research Council of Canada; FQRNT (Quebec); Canadian Space Agency; Austrian Science Funds [P22691-N16] FX This study was based on data from the MOST satellite, a Canadian Space Agency mission jointly operated by Dynacon Inc., the University of Toronto Institute of Aerospace Studies, and the University of British Columbia, with the assistance of the University of Vienna. It also made use of NASA's Astrophysics Data System (ADS) Bibliographic Services. MS is grateful to the Polish National Science Centre for grant 2012/05/E/ST9/03915, which fully supported his research. The Natural Sciences and Engineering Research Council of Canada supports the research of DBG, JMM, AFJM and SMR. Additional support for AFJM was provided by FQRNT (Quebec). RK is supported by the Canadian Space Agency, and WWW is supported by the Austrian Science Funds (P22691-N16). Special thanks also go to the anonymous referee for highly useful suggestions and comments on a previous version of this paper. NR 36 TC 2 Z9 2 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2014 VL 444 IS 1 BP 327 EP 335 DI 10.1093/mnras/stu1304 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100025 ER PT J AU Heinke, CO Cohn, HN Lugger, PM Webb, NA Ho, WCG Anderson, J Campana, S Bogdanov, S Haggard, D Cool, AM Grindlay, JE AF Heinke, C. O. Cohn, H. N. Lugger, P. M. Webb, N. A. Ho, W. C. G. Anderson, J. Campana, S. Bogdanov, S. Haggard, D. Cool, A. M. Grindlay, J. E. TI Improved mass and radius constraints for quiescent neutron stars in omega Cen and NGC 6397 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE dense matter; stars: neutron; globular clusters: individual: NGC 6397; globular clusters: individual: NGC 5139; X-rays: binaries ID X-RAY BINARY; EQUATION-OF-STATE; GALACTIC GLOBULAR-CLUSTERS; ABSORPTION CROSS-SECTIONS; SOLAR-SYSTEM ABUNDANCES; PULSAR SAX J1808.4-3658; PHOTON IMAGING CAMERA; XMM-NEWTON; 47 TUCANAE; MILLISECOND PULSAR AB We use Chandra and XMM-Newton observations of the globular clusters. Cen and NGC 6397 to measure the spectrum of their quiescent neutron stars (NSs), and thus to constrain the allowed ranges of mass and radius for each. We also use Hubble Space Telescope photometry of NGC 6397 to identify a potential optical companion to the quiescent NS, and find evidence that the companion lacks hydrogen. We carefully consider a number of systematic problems, and show that the choices of atmospheric composition, interstellar medium abundances, and cluster distances can have important effects on the inferred NS mass and radius. We find that for typical NS masses, the radii of both NSs are consistent with the 10-13 km range favoured by recent nuclear physics experiments. This removes the evidence suggested by Guillot and collaborators for an unusually small NS radius, which relied upon the small inferred radius of the NGC 6397 NS. C1 [Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Cohn, H. N.; Lugger, P. M.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Webb, N. A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Webb, N. A.] CNRS, IRAP, F-31028 Toulouse 4, France. [Ho, W. C. G.] Univ Southampton, Math Sci & STAG Res Ctr, Southampton SO17 1BJ, Hants, England. [Anderson, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Campana, S.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Bogdanov, S.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Haggard, D.] Northwestern Univ, Dept Phys & Astron, CIERA, Evanston, IL 60208 USA. [Cool, A. M.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Grindlay, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heinke, CO (reprint author), Univ Alberta, Dept Phys, CCIS 4-183, Edmonton, AB T6G 2E1, Canada. EM heinke@ualberta.ca OI Campana, Sergio/0000-0001-6278-1576; Heinke, Craig/0000-0003-3944-6109 FU NSERC Discovery Grant; Alberta Ingenuity New Faculty Award; Chandra Award [GO2-13057A, GO2-13057B]; NASA [NAS8-03060, NAS 5-26555]; NASA through Space Telescope Science Institute [GO-10257]; ESA Member States FX We thank G. R. Sivakoff for helpful comments. COH is supported by an NSERC Discovery Grant and an Alberta Ingenuity New Faculty Award. DH and AMC are supported by Chandra Award numbers GO2-13057A and GO2-13057B issued by the CXO, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. This work is based in part on observations 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 proposal GO-10257. Support for programme GO-10257 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. A portion of these results was based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research made use of data obtained through observations made by NASA's Chandra X-ray Observatory, data obtained from the Chandra Data Archive, and data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), provided by NASA's Goddard Space Flight Center. This research has made use of the NASA Astrophysics Data System (ADS), the electronic archive arXiv.org maintained by Cornell University Library, and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. NR 113 TC 41 Z9 41 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 OCT 11 PY 2014 VL 444 IS 1 BP 443 EP 456 DI 10.1093/mnras/stu1449 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100035 ER PT J AU Mikolajewska, J Caldwell, N Shara, MM AF Mikolajewska, Joanna Caldwell, Nelson Shara, Michael M. TI First detection and characterization of symbiotic stars in M31 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; binaries: symbiotic; planetary nebulae: general; galaxies: individual: M31 ID CURRENTLY FORMING STARS; EMISSION-LINE STARS; D-TYPE SYSTEMS; H II REGIONS; LOCAL GROUP; SPECTROSCOPIC OBSERVATIONS; PHYSICAL CONDITIONS; ECLIPSING BINARIES; PLANETARY-NEBULAE; ANDROMEDA GALAXY AB Symbiotic binaries are putative progenitors of Type Ia supernovae. The census of Galactic symbiotic binaries is so incomplete that we cannot reliably estimate the total population of these stars, and use it to check whether that number is consistent with the observed Type Ia supernova rate in spiral galaxies. We have thus begun a survey of the nearest counterpart of our own Galaxy, namely M31, where a relatively complete census of symbiotic stars is achievable. We report the first detections and spectrographic characterizations of 35 symbiotic binaries in M31, and compare these stars with the symbiotic population in the Milky Way. These newly detected M31 symbiotic binaries are remarkably similar to Galactic symbiotics, though we are clearly only sampling (in this feasibility study) the most luminous symbiotics in M31. We have also found, in M31, the symbiotic star (M31SyS J004233.17+412720.7) with the highest ionization level known amongst all symbiotics. An optical outburst of the M31 symbiotic star M31SyS J004322.50+413940.9 was probably a nova-like outburst, the first symbiotic outburst detected outside the Milky Way and Magellanic Clouds. C1 [Mikolajewska, Joanna] N Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shara, Michael M.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. RP Mikolajewska, J (reprint author), N Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. EM mikolaj@camk.edu.pl FU Polish NCN grant [DEC-2013/10/M/ST9/00086]; French Institut National des Sciences de l'Univers; CNRS; French Education Ministry; European Southern Observatory; State of Baden-Wuerttemberg; European Commission; Landessternwarte; Heidelberg; Institut d'Astrophysique de Paris; National Aeronautics and Space Administration; National Science Foundation FX This study has been supported in part by the Polish NCN grant DEC-2013/10/M/ST9/00086. We gratefully acknowledge Nathan Sanders for help with the emission line tables, and the fine support at the MMT Observatory, and The Local Group Galaxies Survey conducted at NOAO by PhilMassey and collaborators. MMS thanks Allen Shafter for helpful details about M31N 1993-05. We also thank the referee, R. Corradi, for useful comments. This research has made use of the VizieR catalogue access tool, operated at CDS, Strasbourg, France. This publication makes use of data products of the DENIS and the 2MASS. DENIS is the result of a joint effort involving human and financial contributions of several Institutes mostly located in Europe. It has been supported financially mainly by the French Institut National des Sciences de l'Univers, CNRS, and French Education Ministry, the European Southern Observatory, the State of Baden-Wuerttemberg, and the European Commission under networks of the SCIENCE and Human Capital and Mobility programs, the Landessternwarte, Heidelberg and Institut d'Astrophysique de Paris. 2MASS 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 74 TC 6 Z9 6 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 OCT 11 PY 2014 VL 444 IS 1 BP 586 EP 599 DI 10.1093/mnras/stu1480 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100045 ER PT J AU Offringa, AR McKinley, B Hurley-Walker, N Briggs, FH Wayth, RB Kaplan, DL Bell, ME Feng, L Neben, AR Hughes, JD Rhee, J Murphy, T Bhat, NDR Bernardi, G Bowman, JD Cappallo, RJ Corey, BE Deshpande, AA Emrich, D Ewall-Wice, A Gaensler, BM Goeke, R Greenhill, LJ Hazelton, BJ Hindson, L Johnston-Hollitt, M Jacobs, DC Kasper, JC Kratzenberg, E Lenc, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Kudryavtseva, N Oberoi, D Ord, SM Pindor, B Procopio, P Prabu, T Riding, J Roshi, DA Shankar, NU Srivani, KS Subrahmanyan, R Tingay, SJ Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL AF Offringa, A. R. McKinley, B. Hurley-Walker, N. Briggs, F. H. Wayth, R. B. Kaplan, D. L. Bell, M. E. Feng, L. Neben, A. R. Hughes, J. D. Rhee, J. Murphy, T. Bhat, N. D. R. Bernardi, G. Bowman, J. D. Cappallo, R. J. Corey, B. E. Deshpande, A. A. Emrich, D. Ewall-Wice, A. Gaensler, B. M. Goeke, R. Greenhill, L. J. Hazelton, B. J. Hindson, L. Johnston-Hollitt, M. Jacobs, D. C. Kasper, J. C. Kratzenberg, E. Lenc, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morales, M. F. Morgan, E. Kudryavtseva, N. Oberoi, D. Ord, S. M. Pindor, B. Procopio, P. Prabu, T. Riding, J. Roshi, D. 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 WSCLEAN: an implementation of a fast, generic wide-field imager for radio astronomy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; methods: observational; techniques: interferometric; radio continuum: general ID MURCHISON WIDEFIELD ARRAY; NONCOPLANAR ARRAYS; POINT SOURCES; ALGORITHM; INTERFEROMETRY; DECONVOLUTION; CALIBRATION; REPRESENTATIONS; SUBTRACTION; PROJECTION AB Astronomical wide-field imaging of interferometric radio data is computationally expensive, especially for the large data volumes created by modern non-coplanar many-element arrays. We present a new wide-field interferometric imager that uses the omega-stacking algorithm and can make use of the omega-snapshot algorithm. The performance dependences of CASA's omega-projection and our new imager are analysed and analytical functions are derived that describe the required computing cost for both imagers. On data from the Murchison Widefield Array, we find our new method to be an order of magnitude faster than omega-projection, as well as being capable of full-sky imaging at full resolution and with correct polarization correction. We predict the computing costs for several other arrays and estimate that our imager is a factor of 2-12 faster, depending on the array configuration. We estimate the computing cost for imaging the lowfrequency Square Kilometre Array observations to be 60 PetaFLOPS with current techniques. We find that combining omega-stacking with the omega-snapshot algorithm does not significantly improve computing requirements over pure omega-stacking. The source code of our new imager is publicly released. C1 [Offringa, A. R.; McKinley, B.; Briggs, F. H.; Hughes, J. D.; Rhee, J.; Waterson, M.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Offringa, A. R.; McKinley, B.; Briggs, F. H.; Wayth, R. B.; Bell, M. E.; Rhee, J.; Murphy, T.; Gaensler, B. M.; Lenc, E.; Mitchell, D. A.; Ord, S. M.; Subrahmanyan, R.; Tingay, S. J.; Webster, R. L.] Australian Natl Univ, ARC Ctr Excellence All Sky Astrophys CAASTRO, Canberra, ACT 2611, Australia. [Hurley-Walker, N.; Wayth, R. B.; Bhat, N. D. R.; Emrich, D.; Lynch, M. J.; Kudryavtseva, N.; Ord, S. M.; Tingay, S. J.; Waterson, M.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Bell, M. E.; Murphy, T.; Gaensler, B. M.; Lenc, E.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Feng, L.; Neben, A. R.; Ewall-Wice, A.; Goeke, R.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bernardi, G.] Square Kilometre Array South Africa SKA SA, ZA-7405 Cape Town, South Africa. [Bowman, J. D.; Jacobs, D. C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Cappallo, R. J.; Corey, B. E.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; 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. [Greenhill, L. J.; Kasper, J. C.] 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. [Kasper, J. C.] Univ Michigan, Ann Arbor, MI 48109 USA. [Mitchell, D. A.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Pindor, B.; Procopio, P.; Riding, J.; Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Roshi, D. A.] Natl Radio Astron Observ, Charlottesville & Greenbank, Charlottesville, VA 22903 USA. RP Offringa, AR (reprint author), Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. EM andre.offringa@anu.edu.au RI Wayth, Randall/B-2444-2013; Kasper, Justin/D-1152-2010; Udayashankar , N/D-4901-2012; Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Hurley-Walker, Natasha/B-9520-2013; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI Gaensler, Bryan/0000-0002-3382-9558; Lenc, Emil/0000-0002-9994-1593; Kudryavtseva, Nadia/0000-0002-1372-0942; Wayth, Randall/0000-0002-6995-4131; /0000-0002-0086-7363; Kasper, Justin/0000-0002-7077-930X; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Hurley-Walker, Natasha/0000-0002-5119-4808; Emrich, David/0000-0002-4058-1837; Murphy, Tara/0000-0002-2686-438X 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 the New Zealand Ministry of Economic Development [MEDE1799]; IBM Shared University Research Grant; Commonwealth Scientific and Industrial Research Organization (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund, and the Australia India Strategic Research Fund; Astronomy Australia Limited; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Joint Venture of Curtin University and The University of Western Australia; Western Australian State government FX ARO would like to thank O. M. Smirnov for testing WSCLEAN on VLA data. 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 MEDE1799 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 Organization (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 38 TC 39 Z9 39 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 OCT 11 PY 2014 VL 444 IS 1 BP 606 EP 619 DI 10.1093/mnras/stu1368 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100047 ER PT J AU Russell, HR Fabian, AC McNamara, BR Edge, AC Sanders, JS Nulsen, PEJ Baum, SA Donahue, M O'Dea, CP AF Russell, H. R. Fabian, A. C. McNamara, B. R. Edge, A. C. Sanders, J. S. Nulsen, P. E. J. Baum, S. A. Donahue, M. O'Dea, C. P. TI The bow shock, cold fronts and disintegrating cool core in the merging galaxy group RX J0751.3+5012 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: groups: individual: RX J0751.3+5012; intergalactic medium; X-rays: galaxies: clusters ID KELVIN-HELMHOLTZ INSTABILITIES; BRIGHTEST CLUSTER GALAXIES; MASS-TEMPERATURE RELATION; DIGITAL SKY SURVEY; X-RAY-CLUSTERS; INTERGALACTIC MEDIUM; CHANDRA OBSERVATION; RING GALAXIES; VIRGO CLUSTER; HOT GAS AB We present a new Chandra X-ray observation of the off-axis galaxy group merger RX J0751.3+5012. The hot atmospheres of the two colliding groups appear highly distorted by the merger. The images reveal arc-like cold fronts around each group core, produced by the motion through the ambient medium, and the first detection of a group merger shock front. We detect a clear density and temperature jump associated with a bow shock of Mach number M = 1.9 +/- 0.4 ahead of the northern group. Using galaxy redshifts and the shock velocity of 1100 +/- 300 km s(-1), we estimate that the merger axis is only similar to 10 degrees from the plane of the sky. From the projected group separation of similar to 90 kpc, this corresponds to a time since closest approach of similar to 0.1Gyr. The northern group hosts a dense, cool core with a ram pressure stripped tail of gas extending similar to 100 kpc. The sheared sides of this tail appear distorted and broadened by Kelvin-Helmholtz instabilities. We use the presence of this substructure to place an upper limit on the magnetic field strength and, for Spitzer-like viscosity, show that the development of these structures is consistent with the critical perturbation length above which instabilities can grow in the intragroup medium. The northern group core also hosts a galaxy pair, UGC 4052, with a surrounding IR and near-UV ring similar to 40 kpc in diameter. The ring may have been produced by tidal stripping of a smaller galaxy by UGC 4052 or it may be a collisional ring generated by a close encounter between the two large galaxies. C1 [Russell, H. R.; McNamara, B. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Russell, H. R.; Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Russell, H. R.; Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanders, J. S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Baum, S. A.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Donahue, M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. RP Russell, HR (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. EM hrr27@ast.cam.ac.uk OI Edge, Alastair/0000-0002-3398-6916; Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU Canadian Space Agency Space Science Enhancement Programme; COFUND Junior Research Fellowship at the Durham University Institute of Advanced Study; ERC Advanced Grant Feedback; NASA [NAS8-03060]; NASA Chandra award [GO1-12155B]; U.S. Government [NAGW-2166]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Japan Participation Group; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Korean Scientist Group; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We thank the reviewer for helpful and constructive comments. HRR and BRM acknowledge generous financial support from the Canadian Space Agency Space Science Enhancement Programme. HRR also acknowledges support from a COFUND Junior Research Fellowship at the Durham University Institute of Advanced Study. HRR and ACF acknowledge support from ERC Advanced Grant Feedback. PEJN was supported by NASA contract NAS8-03060. MD acknowledges partial support from NASA Chandra award GO1-12155B. HRR thanks Trevor Ponman, Graham Smith, Lindsay King and Rebecca Canning for helpful discussions.; The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAGW-2166. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory and the University of Washington. NR 90 TC 7 Z9 7 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 OCT 11 PY 2014 VL 444 IS 1 BP 629 EP 641 DI 10.1093/mnras/stu1469 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100049 ER PT J AU Palau, A Zapata, LA Rodriguez, LF Bouy, H Barrado, D Morales-Calderon, M Myers, PC Chapman, N Juarez, C Li, D AF Palau, Aina Zapata, Luis A. Rodriguez, Luis F. Bouy, Herve Barrado, David Morales-Calderon, Maria Myers, Philip C. Chapman, Nicholas Juarez, Carmen Li, Di TI IC 348-SMM2E: a Class 0 proto-brown dwarf candidate forming as a scaled-down version of low-mass stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE brown dwarfs; stars: formation; ISM: individual objects: IC348-SMM2; ISM: jets and outflows; ISM: lines and bands; submillimetre: ISM ID 1ST HYDROSTATIC CORE; SPITZER C2D SURVEY; YOUNG STELLAR OBJECTS; LOW-LUMINOSITY OBJECT; BIPOLAR MOLECULAR OUTFLOW; SUBMILLIMETER ARRAY; DENSE CORE; PROTOSTELLAR CORES; PRESTELLAR CORES; SPACE-TELESCOPE AB We report on Submillimeter Array observations of the 870 mu m continuum and CO (3-2), (CO)-C-13 (2-1), and (CO)-O-18 (2-1) line emission of a faint object, SMM2E, near the driving source of the HH 797 outflow in the IC 348 cluster. The continuum emission shows an unresolved source for which we estimate a mass of gas and dust of 30M(Jup), and the CO (3-2) line reveals a compact bipolar outflow centred on SMM2E, and barely seen also in (CO)-C-13 (2-1). In addition, (CO)-O-18 (2-1) emission reveals hints of a possible rotating envelope/disc perpendicular to the outflow, for which we infer a dynamical mass of similar to 16M(Jup). In order to further constrain the accreted mass of the object, we gathered data from Spitzer, Herschel, and new and archive submillimetre observations, and built the spectral energy distribution (SED). The SED can be fitted with one single-modified blackbody from 70 mu m down to 2.1 cm, using a dust temperature of similar to 24 K, a dust emissivity index of 0.8, and an envelope mass of similar to 35M(Jup). The bolometric luminosity is 0.10 L-circle dot, and the bolometric temperature is 35 K. Thus, SMM2E is comparable to the known Class 0 objects in the stellar domain. An estimate of the final mass indicates that SMM2E will most likely remain substellar, and the SMM2E outflow force matches the trend with luminosity known for young stellar objects. Thus, SMM2E constitutes an excellent example of a Class 0 proto-brown dwarf candidate which forms as a scaled-down version of low-mass stars. Finally, SMM2E seems to be part of a wide (similar to 2400 au) multiple system of Class 0 sources. C1 [Palau, Aina; Zapata, Luis A.; Rodriguez, Luis F.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Bouy, Herve; Barrado, David; Morales-Calderon, Maria] INTA CSIC, Dept Astrofis, Ctr Astrobiol, E-28691 Madrid, Spain. [Myers, Philip C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chapman, Nicholas] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Chapman, Nicholas] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Juarez, Carmen] Inst Ciencies Espai CSIC IEEC, Fac Ciencias, E-08193 Bellaterra, Catalunya, Spain. [Li, Di] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Li, Di] Space Sci Inst, Boulder, CO 80301 USA. RP Palau, A (reprint author), Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, POB 3-72, Morelia 58090, Michoacan, Mexico. EM a.palau@crya.unam.mx RI Bouy, Herve/H-2913-2012; Barrado Navascues, David/C-1439-2017; Morales-Calderon, Maria/C-8384-2017 OI Bouy, Herve/0000-0002-7084-487X; Barrado Navascues, David/0000-0002-5971-9242; Morales-Calderon, Maria/0000-0001-9526-9499 FU UNAM; CONACyT, Mexico; Spanish Ramon y Cajal fellowship programme [RYC-2009-04497]; National Basic Research Program of China (973 program) [2012CB821800]; NSFC [11373038]; Canadian Space Agency; [AYA2010-21161-C02-02]; [AYA2012-38897-C02-01] FX We are deeply grateful to Helen Kirk, Josh Walawender, and Dough Johnstone for sharing the 450 mu m JCMT data, and to Jackie Davidson and Giles Novak for sharing 350 mu m CSO data to compare to the new data acquired at the CSO. The authors are also grateful to the referee for her/his comments that significantly improved the paper. AP, LAZ, and LFR acknowledge the financial support from UNAM and CONACyT, Mexico. HB is funded by the Spanish Ramon y Cajal fellowship programme number RYC-2009-04497. This research has been funded by Spanish grants AYA2010-21161-C02-02 and AYA2012-38897-C02-01. DL acknowledges the support from National Basic Research Program of China (973 program) no. 2012CB821800 and NSFC no. 11373038. This research used the facilities of the CADC operated by the National Research Council of Canada with the support of the Canadian Space Agency. Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the CFHT which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. Based on observations obtained with WIRCam, a joint project of CFHT, Taiwan, Korea, Canada, and France. NR 115 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 OCT 11 PY 2014 VL 444 IS 1 BP 833 EP 845 DI 10.1093/mnras/stu1461 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100064 ER PT J AU Dunham, MM Vorobyov, EI Arce, HG AF Dunham, Michael M. Vorobyov, Eduard I. Arce, Hector G. TI On the reliability of protostellar disc mass measurements and the existence of fragmenting discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE protoplanetary discs; stars: formation ID AURIGA MOLECULAR CLOUD; STAR-FORMATION; TAURUS-AURIGA; MAGNETIC BRAKING; EPISODIC ACCRETION; EVOLUTIONARY SIGNATURES; PROTOPLANETARY DISKS; ENVELOPE STRUCTURE; ALMA OBSERVATIONS; PROTOSTARS. II. AB We couple non-magnetic, hydrodynamical simulations of collapsing protostellar cores with radiative transfer evolutionary models to generate synthetic observations. We then use these synthetic observations to investigate the extent to which a simple method for measuring protostellar disc masses used in the literature recovers the intrinsic masses of the discs formed in the simulations. We evaluate the effects of contamination from the surrounding core, partially resolving out the disc, optical depth, fixed assumed dust temperatures, inclination, and the dust opacity law. We show that the combination of these effects can lead to disc mass underestimates by up to factors of 2-3 at millimetre wavelengths and up to an order of magnitude or larger at submillimetre wavelengths. The optically thin portions of protostellar discs are generally cooler in the Class I stage than the Class 0 stage since Class I discs are typically larger and more optically thick, and thus more shielded. The observed disc mass distribution closely resembles the intrinsic distribution if this effect is taken into account, especially at millimetrewavelengths where optical depth effects are minimized. Approximately 50-70 per cent of protostellar discs observed to date with this method are consistent with the masses of the gravitationally unstable discs formed in the simulations, suggesting that at least some protostellar discs are likely sufficiently massive to fragment. We emphasize key future work needed to confirm these results, including assembling larger, less biased samples, and using molecular line observations to distinguish between rotationally supported, Keplerian discs and magnetically supported pseudodiscs. C1 [Dunham, Michael M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vorobyov, Eduard I.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Vorobyov, Eduard I.] Southern Fed Univ, Inst Phys Res, Rostov Na Donu 344090, Russia. [Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. RP Dunham, MM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM mdunham@cfa.harvard.edu FU Submillimeter Array; Russian Ministry of Education and Science Grant [3.961.2014/K]; NSF [AST-0845619] FX We thank the anonymous referee for comments and suggestions that have improved the quality of this work. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service and the IDL Astronomy Library hosted by the NASA Goddard Space Flight Center. MMD acknowledges support from the Submillimeter Array through an SMA postdoctoral fellow. The simulations were performed on the Shared Hierarchical Academic Research Computing Network (SHARCNET), on the Atlantic Computational Excellence Network (ACEnet), and on the Vienna Scientific Cluster (VSC-2). This project was partly supported by the Russian Ministry of Education and Science Grant (state assignment) 3.961.2014/K. HGA acknowledges support from the NSF through grant AST-0845619. NR 80 TC 13 Z9 13 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 11 PY 2014 VL 444 IS 1 BP 887 EP 901 DI 10.1093/mnras/stu1511 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6LX UT WOS:000342925100069 ER PT J AU Barnacka, A Loeb, A AF Barnacka, Anna Loeb, Abraham TI A SIZE-DURATION TREND FOR GAMMA-RAY BURST PROGENITORS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: general; methods: data analysis ID HOST GALAXY; LONG; VARIABILITY; AFTERGLOW; SUPERNOVAE; COLLAPSARS; FERMI; GRB AB Gamma-ray bursts (GRBs) show a bimodal distribution of durations, separated at a duration of similar to 2 s. Observations have confirmed the association of long GRBs with the collapse of massive stars. The origin of short GRBs is still being explored. We examine constraints on the size of emission regions in short and long GRBs detected by Fermi/GBM. We find that the transverse extent of emission regions during the prompt phase, R, and the burst duration, T-90, are consistent with the relation R similar to c x T-90, for both long and short GRBs. We find the characteristic transverse extent for the prompt emission region to be similar to 2 x 10(10) cm and similar to 4 x 10(11) cm for short and long GRBs, respectively. C1 [Barnacka, Anna; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barnacka, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-20, Cambridge, MA 02138 USA. EM abarnacka@cfa.harvard.edu; aloeb@cfa.harvard.edu OI Barnacka, Anna/0000-0001-5655-4158 FU Department of Energy Office of Science, NASA; Smithsonian Astrophysical Observatory; NCN [DEC-2011/01/M/ST9/01891]; NSF [AST-1312034] FX We thank the referee for valuable comments on the manuscript. We thank Markus Bottcher, Edo Berger, Josh Grindlay, and Raffaella Margutti for comments on the manuscript and for useful discussions. The work of A.B. is supported by the Department of Energy Office of Science, NASA, and the Smithsonian Astrophysical Observatory, and financial support by the NCN grant DEC-2011/01/M/ST9/01891 is acknowledged. This work was also supported in part by NSF grant AST-1312034. NR 36 TC 4 Z9 4 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 OCT 10 PY 2014 VL 794 IS 1 AR L8 DI 10.1088/2041-8205/794/1/L8 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR0YZ UT WOS:000343304300008 ER PT J AU Gwinn, CR Kovalev, YY Johnson, MD Soglasnov, VA AF Gwinn, C. R. Kovalev, Y. Y. Johnson, M. D. Soglasnov, V. A. TI DISCOVERY OF SUBSTRUCTURE IN THE SCATTER-BROADENED IMAGE OF SGR A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE black hole physics; Galaxy: nucleus; ISM: structure; radio continuum: ISM; scattering techniques: interferometric ID SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; COMPACT RADIO-SOURCE; GALACTIC-CENTER; INTERSTELLAR-MEDIUM; MILKY-WAY; VLBI OBSERVATIONS; SCALE STRUCTURE; INTRINSIC SIZE; MODEL AB We have detected substructure within the smooth scattering disk of the celebrated Galactic center radio source Sagittarius A* (Sgr A*). We observed this structure at 1.3 cm wavelength with the Very Long Baseline Array together with the Green Bank Telescope, on baselines of up to 3000 km, long enough to completely resolve the average scattering disk. Such structure is predicted theoretically as a consequence of refraction by large-scale plasma fluctuations in the interstellar medium. Along with the much-studied theta(d) proportional to lambda(2) scaling of angular broadening theta(d) with observing wavelength., our observations indicate that the spectrum of interstellar turbulence is shallow with an inner scale larger than 300 km. The substructure is consistent with an intrinsic size of about 1 mas at 1.3 cm wavelength, as inferred from deconvolution of the average scattering. Further observations of the substructure can set stronger constraints on the properties of scattering material and on the intrinsic size of Sgr A*. These constraints will guide our understanding of the effects of scatter broadening and the emission physics near the black hole in images with the Event Horizon Telescope at millimeter wavelengths. C1 [Gwinn, C. R.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93117 USA. [Kovalev, Y. Y.; Soglasnov, V. A.] Russian Acad Sci, Ctr Astro Space, Lebedev Phys Inst, Moscow 117997, Russia. [Kovalev, Y. Y.] Max Planck Inst Radio Astron, D-53121 Bonn, Germany. [Johnson, M. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gwinn, CR (reprint author), Univ Calif Santa Barbara, Dept Phys, Broida Hall, Santa Barbara, CA 93117 USA. EM cgwinn@physics.ucsb.edu RI Kovalev, Yuri/J-5671-2013; Soglasnov, Vladimir/O-7615-2015 OI Kovalev, Yuri/0000-0001-9303-3263; FU US National Science Foundation [AST-1008865]; Dynasty Foundation FX We thank Leonid Petrov for assistance with detections and their significance; Mikhail Popov, Nikolai Kardashev, Ken Kellermann, Richard Porcas, and Mark Reid for essential discussions; and the referee for encouraging suggestions. We thank the NRAO staff for supporting our observations in their usual highly professional and friendly manner. The Robert C. Byrd Green Bank Telescope and the Very Long Baseline Array are operated by the National Radio Astronomy Observatory, which is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities Inc. C.R.G. acknowledges support of the US National Science Foundation (AST-1008865). Y.Y.K. was supported in part by the Dynasty Foundation. NR 43 TC 20 Z9 20 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 OCT 10 PY 2014 VL 794 IS 1 AR L14 DI 10.1088/2041-8205/794/1/L14 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR0YZ UT WOS:000343304300014 ER PT J AU Qiu, KP Zhang, QZ Menten, KM Liu, HB Tang, YW Girart, JM AF Qiu, Keping Zhang, Qizhou Menten, Karl M. Liu, Hauyu B. Tang, Ya-Wen Girart, Josep M. TI SUBMILLIMETER ARRAY OBSERVATIONS OF MAGNETIC FIELDS IN G240.31+0.07: AN HOURGLASS IN A MASSIVE CLUSTER-FORMING CORE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: magnetic fields; stars: early-type; stars: formation; techniques: interferometric; techniques: polarimetric ID STAR-FORMATION; MOLECULAR OUTFLOW; REGION G240.31+0.07; EVOLUTION; COLLAPSE; FRAGMENTATION; POLARIZATION; CLOUDS AB We report the first detection of an hourglass magnetic field aligned with a well-defined outflow rotation system in a high-mass, star-forming region. The observations were performed with the Submillimeter Array toward G240.31+0.07, which harbors a massive, flattened, and fragmenting molecular cloud core and a wide-angle bipolar outflow. The polarized dust emission at 0.88 mm reveals a clear hourglass-shaped magnetic field aligned within 20 degrees of the outflow axis. Maps of high-density tracing spectral lines, e.g., (HCO+)-C-13 (4-3), show that the core is rotating about its minor axis, which is also aligned with the magnetic field axis. Therefore, both the magnetic field and kinematic properties observed in this region are surprisingly consistent with the theoretical predictions of the classic paradigm of isolated low-mass star formation. The strength of the magnetic field in the plane of sky is estimated to be similar to 1.1 mG, resulting in a mass-to-magnetic flux ratio of 1.4 times the critical value and a turbulent-to-ordered magnetic energy ratio of 0.4. We also find that the specific angular momentum almost linearly decreases from r similar to 0.6 pc to 0.03 pc scales, which is most likely attributed to magnetic braking. C1 [Qiu, Keping] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Qiu, Keping] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210093, Jiangsu, Peoples R China. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, Karl M.] Max Planck Inst Radioastron, D-52425 Bonn, Germany. [Liu, Hauyu B.; Tang, Ya-Wen] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Girart, Josep M.] Fac Ciencies, CSIC, IEEC, Inst Ciencies Espai, E-08193 Bellaterra, Catalonia, Spain. RP Qiu, KP (reprint author), Nanjing Univ, Sch Astron & Space Sci, 22 Hankou Rd, Nanjing 210093, Jiangsu, Peoples R China. EM kpqiu@nju.edu.cn RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 FU 985 project of Nanjing University; NSFC [11328301]; Spanish MINECO [AYA2011-30228-C03-02]; Catalan AGAUR [2009SGR1172] FX We thank the SMA staff for support that made this study possible. Part of this work was conducted when K.Q. was doing postdoctoral research at the Max-Planck-Institut fur Radioastronomie. K.Q. is partially supported by the 985 project of Nanjing University. Q.Z. is partially supported by the NSFC grant 11328301. J.M.G. is supported by the Spanish MINECO AYA2011-30228-C03-02 and Catalan AGAUR 2009SGR1172 grants. NR 35 TC 9 Z9 9 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 10 PY 2014 VL 794 IS 1 AR L18 DI 10.1088/2041-8205/794/1/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR0YZ UT WOS:000343304300018 ER PT J AU Weisz, DR Johnson, BD Conroy, C AF Weisz, Daniel R. Johnson, Benjamin D. Conroy, Charlie TI THE VERY FAINT END OF THE UV LUMINOSITY FUNCTION OVER COSMIC TIME: CONSTRAINTS FROM THE LOCAL GROUP FOSSIL RECORD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dark ages, reionization, first stars; galaxies: evolution; galaxies: high-redshift; galaxies: luminosity function, mass function; Local Group ID STAR-FORMATION HISTORIES; LYMAN-BREAK GALAXIES; COLOR-MAGNITUDE DIAGRAMS; INITIAL MASS FUNCTION; MILKY-WAY SATELLITES; DEEP FIELD CAMPAIGN; SIMILAR-TO 2; STELLAR POPULATIONS; EVOLUTION MODELS; DWARF GALAXIES AB We present a new technique to estimate the evolution of the very faint end of the UV luminosity function (LF) out to z similar to 5. Measured star formation histories (SFHs) from the fossil record of Local Group (LG) galaxies are used to reconstruct the LF down to M-UV similar to -5 at z similar to 5 and M-UV similar to -1.5 at z < 1. Such faint limits are well beyond the current observational limits and are likely to remain beyond the limits of next-generation facilities. The reconstructed LFs, when combined with direct measurements of the LFs at higher luminosity, are well-fit by a standard Schechter function with no evidence of a break to the faintest limits probed by this technique. The derived faint-end slope, alpha, steepens from approximate to-1.2 at z < 1 to approximate to-1.6 at 4 < z < 5. We test the effects of burstiness in the SFHs and find the recovered LFs to be only modestly affected. Incompleteness corrections for the faintest LG galaxies and the (unlikely) possibility of significant luminosity-dependent destruction of dwarf galaxies between high redshift and the present epoch are important uncertainties. These and other uncertainties can be mitigated with more detailed modeling and future observations. The reconstructed faint end LF from the fossil record can therefore be a powerful and complementary probe of the high-redshift faint galaxies believed to play a key role in the reionization of the universe. C1 [Weisz, Daniel R.; Johnson, Benjamin D.; Conroy, Charlie] Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA. [Weisz, Daniel R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Weisz, DR (reprint author), Univ Calif Santa Cruz, Dept Astron, 1156 High St, Santa Cruz, CA 95064 USA. EM drw@ucsc.edu OI Weisz, Daniel/0000-0002-6442-6030 FU NASA - Space Telescope Science Institute [HST-HF-51331.01]; National Science Foundation [PHYS-1066293]; MPIA; Packard and Sloan Foundation Fellowships FX The authors thank Julianne Dalcanton for an insightful discussion on the interpretation of Phi'. 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. was also partially supported in part by the National Science Foundation under grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics, and by Hans-Walter Rix and the MPIA. C.C. is supported by Packard and Sloan Foundation Fellowships. This research made extensive use of NASA's Astrophysics Data System Bibliographic Services. NR 46 TC 20 Z9 20 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 10 PY 2014 VL 794 IS 1 AR UNSP L3 DI 10.1088/2041-8205/794/1/L3 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR0YZ UT WOS:000343304300003 ER PT J AU Bayliss, MB Ashby, MLN Ruel, J Brodwin, M Aird, KA Bautz, MW Benson, BA Bleem, LE Bocquet, S Carlstrom, JE Chang, CL Cho, HM Clocchiattii, A Crawford, TM Crites, AT Desai, S Dobbs, MA Dudley, JP Foley, RJ Forman, WR George, EM Gettings, D Gladders, MD Gonzalez, AH de Haan, T Halverson, NW High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP Mawatari, K McDonald, M McMahon, JJ Mehl, J Meyer, SS Miller, ED Mocanu, L Mohr, JJ Montroy, TE Murray, SS Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shirokoff, E Song, J Stalder, B Suhada, R Spieler, HG Stanford, SA Staniszewski, Z Stark, AA Story, K Stubbs, CW van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, R Zenteno, A AF Bayliss, M. B. Ashby, M. L. N. Ruel, J. Brodwin, M. Aird, K. A. Bautz, M. W. Benson, B. A. Bleem, L. E. Bocquet, S. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiattii, A. Crawford, T. M. Crites, A. T. Desai, S. Dobbs, M. A. Dudley, J. P. Foley, R. J. Forman, W. R. George, E. M. Gettings, D. Gladders, M. D. Gonzalez, A. H. de Haan, T. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. Mawatari, K. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Miller, E. D. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Padin, S. Plagge, T. 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. Stalder, B. Suhada, R. Spieler, H. G. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, R. Zenteno, A. TI SPT-CL J2040-4451: AN SZ-SELECTED GALAXY CLUSTER AT z=1.478 WITH SIGNIFICANT ONGOING STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (SPT-CL J2040-4451); galaxies: distances and redshifts; galaxies: evolution; large-scale structure of universe ID SOUTH-POLE TELESCOPE; COLOR-MAGNITUDE RELATION; ZELDOVICH EFFECT SURVEY; HIGH-REDSHIFT CLUSTERS; IRAC SHALLOW SURVEY; 720 SQUARE DEGREES; GREATER-THAN 1; RED-SEQUENCE; DISTANT CLUSTERS; PHOTOMETRIC REDSHIFTS AB SPT-CL J2040-4451-spectroscopically confirmed at z = 1.478-is the highest-redshift galaxy cluster yet discovered via the Sunyaev-Zel'dovich effect. SPT-CL J2040-4451 was a candidate galaxy cluster identified in the first 720 deg(2) of the South Pole Telescope Sunyaev-Zel'dovich (SPT-SZ) survey, and has been confirmed in follow-up imaging and spectroscopy. From multi-object spectroscopy with Magellan-I/Baade+ IMACS we measure spectroscopic redshifts for 15 cluster member galaxies, all of which have strong [O Pi]lambda lambda 3727 emission. SPT-CL J2040-4451 has an SZ-measured mass of M-500,(SZ) = 3.2 +/- 0.8 x 10(14)M(circle dot) h(-1) 70, corresponding to M-200,M- (SZ) = 5.8 +/- 1.4 x 10(14)M(circle dot) h(70-)(1.) The velocity dispersion measured entirely from blue star-forming members is sv = 1500 +/- 520 km s(-1). The prevalence of star-forming cluster members (galaxies with > 1.5M(circle dot) yr(-1)) implies that this massive, high-redshift cluster is experiencing a phase of active star formation, and supports recent results showing a marked increase in star formation occurring in galaxy clusters at z greater than or similar to 1.4. We also compute the probability of finding a cluster as rare as this in the SPT-SZ survey to be > 99%, indicating that its discovery is not in tension with the concordance Lambda CDM cosmological model. C1 [Bayliss, M. B.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, M. B.; Ashby, M. L. N.; Foley, R. J.; Jones, C.; Mawatari, K.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Bautz, M. W.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA. [Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Desai, S.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Mocanu, L.; Padin, S.; Plagge, T.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiattii, A.] Pontificia Univ Catolica, Dept Astron & Astrophys, Santiago, Chile. [Dobbs, M. A.; Dudley, J. P.; de Haan, T.; Holder, G. P.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, 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.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gettings, D.; 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. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; 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. [Lueker, M.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 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. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [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, R.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, R.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. RP Bayliss, MB (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM mbayliss@cfa.harvard.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996; Forman, William/0000-0002-9478-1682 FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA [NAS 8-03060]; Excellence Cluster Universe; DFG research program [TR33]; NASA; Clay Fellowship; KICP Fellowship; Pennsylvania State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research Fellowship; Smithsonian Institution; 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 ANT-0638937. 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. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. 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. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. The Munich group acknowledges support from the Excellence Cluster Universe and the DFG research program TR33. This work is based in part on observations obtained with the Spitzer Space Telescope (PID 60099), which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. Additional data were obtained with the 6.5 m Magellan Telescopes located at the Las Campanas Observatory, Chile and the Blanco 4 m Telescope at Cerro Tololo Interamerican Observatories in Chile. R.J.F. is supported by a Clay Fellowship. B.A.B is supported by a KICP Fellowship, M. Bautz acknowledges support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. M.D. acknowledges support from an Alfred P. Sloan Research Fellowship, W.F. and C.J. acknowledge support from the Smithsonian Institution. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under contract No. DE-AC02-05CH11231. The authors also thank the referee, B. Lemaux, for his comments that improved the quality of this paper. NR 85 TC 19 Z9 19 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2014 VL 794 IS 1 AR 12 DI 10.1088/0004-637X/794/1/12 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200012 ER PT J AU Connor, T Donahue, M Sun, M Hoekstra, H Mahdavi, A Conselice, CJ McNamara, B AF Connor, Thomas Donahue, Megan Sun, Ming Hoekstra, Henk Mahdavi, Andisheh Conselice, Christopher J. McNamara, Brian TI SCALING RELATIONS AND X-RAY PROPERTIES OF MODERAIE-LUMINOSITY GALAXY CLUS'IERS FROM 0.3 < z < 0.6 WITH XMM-NEWTON SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; PHOTON IMAGING CAMERA; MASS FUNCTION; COSMOLOGICAL CONSTRAINTS; PARAMETER-ESTIMATION; INTRACLUSTER MEDIUM; RICH CLUSTERS; AGN FEEDBACK; ROSAT SURVEY; EVOLUTION AB We present new X-ray temperatures and improved X-ray luminosity estimates for 15 new and archival XMM-Newton observations of galaxy clusters at intermediate redshift with mass and luminosities near the galaxy group/cluster division (M-2500 < 2.4 x 10(14) h(70)(-1) M-circle dot, L < 2 x 10(44) erg s(-1), 0.3 < z < 0.6). These clusters have weak-lensing mass measurements based on Hubble Space Telescope observations of clusters representative of an X-ray-selected sample (the ROSAT 1605D survey). The angular resolution of XMM-Newton allows us to disentangle the emission of these galaxy clusters from nearby point sources, which significantly contaminated previous X-ray luminosity estimates for 6 of the 15 clusters. We extend cluster scaling relations between X-ray luminosity, temperature, and weak-lensing mass for low-mass, X-ray-selected clusters out to redshift similar to 0.45. These relations are important for cosmology and the astrophysics of feedback in galaxy groups and clusters. Our joint analysis with a sample of 50 clusters in a similar redshift range but with larger masses (M-500 < 21.9 x 10(14) M-circle dot, 0.15 <= z <= 0.55) from the Canadian Cluster Comparison Project finds that within r(2500), M proportional to L-0.44 +/- 0.05, T proportional to L-0.23 +/- 0.02, and M a T'9 02 The estimated intrinsic scatter in the M L relation for the combined sample is reduced to (sigma)log(M/L) = 0.10, from (sigma)log(M/L)= 0.26 with the original ROSAT measurements. We also find an intrinsic scatter for the T L relation, (sigma)log(M/L = 0.07 0.01. C1 [Connor, Thomas; Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48823 USA. [Sun, Ming] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Hoekstra, Henk] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Mahdavi, Andisheh] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94131 USA. [Conselice, Christopher J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [McNamara, Brian] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 5M3, Canada. [McNamara, Brian] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [McNamara, Brian] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Connor, T (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48823 USA. EM connort1@msu.edu OI Hoekstra, Henk/0000-0002-0641-3231; Donahue, Megan/0000-0002-2808-0853 FU NASA ADAP award [NNX11AJ60G]; NASA grant [NNX12AE45G] FX The authors thank Seth Bruch for his work planning this project. M.D. and T.C. acknowledge partial support from a NASA ADAP award NNX11AJ60G. A.M. acknowledges support from NASA grant NNX12AE45G. 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. NR 66 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 OCT 10 PY 2014 VL 794 IS 1 AR 48 DI 10.1088/0004-637X/794/1/48 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200048 ER PT J AU Drout, MR Chornock, R Soderberg, AM Sanders, NE McKinnon, R Rest, A Foley, RJ Milisavljevic, D Margutti, R Berger, E Calkins, M Fong, W Gezari, S Huber, ME Kankare, E Kirshner, RP Leibler, C Lunnan, R Mattila, S Marion, GH Narayan, G Riess, AG Roth, KC Scolnic, D Smartt, SJ Tonry, JL Burgett, WS Chambers, KC Hodapp, KW Jedicke, R Kaiser, N Magnier, EA Metcalfe, N Morgan, JS Price, PA Waters, C AF Drout, M. R. Chornock, R. Soderberg, A. M. Sanders, N. E. McKinnon, R. Rest, A. Foley, R. J. Milisavljevic, D. Margutti, R. Berger, E. Calkins, M. Fong, W. Gezari, S. Huber, M. E. Kankare, E. Kirshner, R. P. Leibler, C. Lunnan, R. Mattila, S. Marion, G. H. Narayan, G. Riess, A. G. Roth, K. C. Scolnic, D. Smartt, S. J. Tonry, J. L. Burgett, W. S. Chambers, K. C. Hodapp, K. W. Jedicke, R. Kaiser, N. Magnier, E. A. Metcalfe, N. Morgan, J. S. Price, P. A. Waters, C. TI RAPIDLY EVOLVING AND LUMINOUS TRANSIENTS FROM PAN-STARRS1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID GAMMA-RAY BURSTS; CORE-COLLAPSE SUPERNOVAE; MASS-METALLICITY RELATION; DIGITAL SKY SURVEY; MULTIBAND LIGHT CURVES; STAR-FORMING GALAXIES; HOST GALAXIES; IA SUPERNOVAE; SHOCK BREAKOUT; IC SUPERNOVA AB In the past decade, several rapidly evolving transients have been discovered whose timescales and luminosities are not easily explained by traditional supernovae (SNe) models. The sample size of these objects has remained small due, at least in part, to the challenges of detecting short timescale transients with traditional survey cadences. Here we present the results from a search within the Pan-STARRS1 Medium Deep Survey (PS1-MDS) for rapidly evolving and luminous transients. We identify 10 new transients with a time above half-maximum (t(1/2)) of less than 12 days and -16.5 > M> -20 mag. This increases the number of known events in this region of SN phase space by roughly a factor of three. The median redshift of the PS1-MDS sample is z = 0.275 and they all exploded in star-forming galaxies. In general, the transients possess faster rise than decline timescale and blue colors at maximum light (g(P1) - r(P1) less than or similar to -0.2). Best-fit blackbodies reveal photospheric temperatures/radii that expand/cool with time and explosion spectra taken near maximum light are dominated by a blue continuum, consistent with a hot, optically thick, ejecta. We find it difficult to reconcile the short timescale, high peak luminosity (L> 10(43) erg s(-1)), and lack of UV line blanketing observed in many of these transients with an explosion powered mainly by the radioactive decay of56Ni. Rather, we find that many are consistent with either (1) cooling envelope emission from the explosion of a star with a low-mass extended envelope that ejected very little (<0.03 M-circle dot) radioactive material, or (2) a shock breakout within a dense, optically thick, wind surrounding the progenitor star. After calculating the detection efficiency for objects with rapid timescales in the PS1-MDS we find a volumetric rate of 4800-8000 events yr(-1) Gpc(-3) (4%-7% of the core-collapse SN rate at z = 0.2). C1 [Drout, M. R.; Chornock, R.; Soderberg, A. M.; Sanders, N. E.; McKinnon, R.; Milisavljevic, D.; Margutti, R.; Berger, E.; Calkins, M.; Fong, W.; Kirshner, R. P.; Lunnan, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McKinnon, R.; Riess, A. G.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Foley, R. J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Gezari, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Huber, M. E.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Magnier, E. A.; Morgan, J. S.; Waters, C.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Kankare, E.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Leibler, C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA. [Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Narayan, G.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Riess, A. G.; Scolnic, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Roth, K. C.] Gemini Observ, Hilo, HI 96720 USA. [Smartt, S. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Metcalfe, N.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Drout, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mdrout@cfa.harvard.edu OI Narayan, Gautham/0000-0001-6022-0484; Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402; Margutti, Raffaella/0000-0003-4768-7586 FU NSF through a Graduate Research Fellowship; David and Lucile Packard Foundation Fellowship for Science and Engineering; Jenny and Antti Wihuri Foundation; European Research Council under the European Union [291222]; National Aeronautics and Space Administration [NNX08AR22G]; Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation [AST-1238877]; University of Maryland; Eotvos Lorand University (ELTE); Gemini Observatory [GN-2011B-Q-3, GS-2012A-Q-31] FX M.R.D. thanks Hagai Perets, Jerod Parrent, and Luke Zoltan Kelley for useful conversations regarding this manuscript. M.R.D. is supported in part by the NSF through a Graduate Research Fellowship. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. E.K. acknowledges financial support from the Jenny and Antti Wihuri Foundation. S.J.S. acknowledges European Research Council funding under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement no [291222]; The Pan-STARRS1 Surveys (PS 1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE); This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. Some observations reported here were obtained at the MMT observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Some observations were obtained under Program IDs GN-2011B-Q-3 (PI: Berger) and GS-2012A-Q-31 (PI: Berger) 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). The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 105 TC 19 Z9 20 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 OCT 10 PY 2014 VL 794 IS 1 AR 23 DI 10.1088/0004637X/794/1/23 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200023 ER PT J AU Engle, SG Guinan, EF Harper, GM Neilson, HR Evans, NR AF Engle, Scott G. Guinan, Edward F. Harper, Graham M. Neilson, Hilding R. Evans, Nancy Remage TI THE SECRET LIVES OF CEPHEIDS: EVOLUTIONARY CHANGES AND PULSATION-INDUCED SHOCK HEATING IN THE PROTOTYPE CLASSICAL CEPHEID delta Cep SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: chromospheres; stars: coronae; stars: variables: Cepheids; ultraviolet: stars; X-rays: stars; stars: individual (delta Cep, beta Dor, Polaris, SU Cas, l Car, HD 213307, xi1 cma) ID HUBBLE-SPACE-TELESCOPE; ENHANCED MASS-LOSS; III LINE RATIOS; EMISSION-LINES; IUE SPECTRA; PERIOD; POLARIS; CHROMOSPHERES; CONSTANT; STARS AB Over the past decade, the Secret Lives of Cepheids (SLiC) program has been carried out at Villanova University to study aspects and behaviors of classical Cepheids that are still not well understood. In this, the first of several planned papers on program Cepheids, we report the current results for d Cep, the Cepheid prototype. Ongoing photometry has been obtained to search for changes in the pulsation period, light-curve morphology, and amplitude. Combining our photometry with the times of maximum light compilation by Berdnikov et al. returns a small period change of dP/dt approximate to -0.1006 +/- 0.0002 s yr(-1). There is also evidence for a gradual light amplitude increase of similar to 0.011 mag (V band) and similar to 0.012 mag (B band) per decade over the last similar to 50 years. In addition, Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS) UV spectrophotometry and XMM-Newton X-ray data were carried out to investigate the high-temperature plasmas present above the Cepheid photospheres. In total, from the five visits (eight exposures) with XMM-Newton, delta Cep is found to be a soft X-ray source (L-X (0.3-2 keV) approximate to 4.5-13 x 10(28) erg s(-1)) with peak flux at kT = 0.6-0.9 keV. The X-ray activity is found to vary, possibly in phase with the stellar pulsations. From 2010-2013, nine observations of d Cep were carried out with HST-COS. The UV emissions are also variable and well phased with the stellar pulsations. Maximum UV line emissions occur near, or slightly before, maximum optical light, varying by as much as 20 times. This variability shows that pulsation-induced shock heating plays a significant role in Cepheid atmospheres, possibly in addition to a quiescent, magnetic heating. The results of this study show Cepheid atmospheres to be rather complex and dynamic. C1 [Engle, Scott G.; Guinan, Edward F.] Villanova Univ, Dept Astrophys & Planetary Sci, Villanova, PA 19085 USA. [Harper, Graham M.] Univ Dublin Trinity Coll, Coll Green, Sch Phys, Dublin 2, Ireland. [Neilson, Hilding R.] E Tennessee State Univ, Dept Phys & Astron, Johnson City, TN 37614 USA. [Evans, Nancy Remage] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Engle, Scott G.] James Cook Univ, Ctr Astron, Townsville, Qld 4811, Australia. RP Engle, SG (reprint author), Villanova Univ, Dept Astrophys & Planetary Sci, Villanova, PA 19085 USA. EM scott.engle@villanova.edu FU NSF grant [AST05-07542]; NASA grants [HST-GO11726, HST-GO12302, HST-GO13019]; XMM-Newton: NASA [NNX14AF12G]; NASA through grants from the Space Telescope Science Institute [11726, 12302, 13019]; NASA [NAS 5-26555] FX The authors also thank the financial support of NSF grant AST05-07542; NASA grants HST-GO11726, HST-GO12302, HST-GO13019; and XMM-Newton: NASA NNX14AF12G.; Support for HST programs 11726, 12302, and 13019 was provided by NASA through grants 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. NR 65 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 OCT 10 PY 2014 VL 794 IS 1 AR 80 DI 10.1088/0004-637X/794/1/80 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200080 ER PT J AU Garcia, JA McClintock, JE Steiner, JF Remillard, RA Grinberg, V AF Garcia, Javier A. McClintock, Jeffrey E. Steiner, James F. Remillard, Ronald A. Grinberg, Victoria TI AN EMPIRICAL METHOD FOR IMPROVING THE QUALITY OF RXTE PCA SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE instrumentation: detectors; space vehicles: instruments; X-rays: individual (Crab, GX 339-4, H1743-322, XTE J1550-64) ID RAY-TIMING-EXPLORER; PROPORTIONAL COUNTER ARRAY; HARD X-RAY; CRAB-NEBULA; PERFORMANCE; CALIBRATION; ABUNDANCES; ABSORPTION AB We fitted all of the several hundred RXTE PCA spectra of the Crab individually to a simple power-law model; the total number of counts in the composite spectrum is >10(9). We then used the spectrum of residuals to derive a calibration tool, called pcacorr, that we apply to large samples of spectra for GX 339-4, H1743-322, and XTE J1550-564. Application of the tool improved the quality of all the fits, and the improvement is dramatic for spectra with >= 10(7) counts. The Crab residual spectrum is somewhat different for each of the five Proportional Counter Array (PCA) detectors, but it was relatively stable over the course of the mission. We recommend that pcacorr be routinely applied to spectra with >= 10(6) counts and that one include a systematic error of 0.1%, rather than the 0.5-1% value that has customarily been used. We expect that application of the tool will result in an increase in sensitivity of the PCA to faint spectral features by up to an order of magnitude. C1 [Garcia, Javier A.; McClintock, Jeffrey E.; Steiner, James F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Remillard, Ronald A.; Grinberg, Victoria] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Garcia, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM javier@head.cfa.harvard.edu; jem@cfa.harvard.edu; jsteiner@head.cfa.harvard.edu; rr@space.mit.edu; grinberg@space.mit.edu OI Remillard, Ronald/0000-0003-4815-0481 FU NASA [NNX11AD08G, HST-HF-51315.01, NAS8-03060]; NASA through the Smithsonian Astrophysical Observatory (SAO) [SV3-73016] FX J.G. and J.E.M. acknowledge the support of NASA grant NNX11AD08G. J.F.S. has been supported by NASA Hubble Fellowship grant HST-HF-51315.01. V.G. acknowledges support provided by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of the Chandra X-Ray Center (CXC) and Science Instruments; CXC is operated by SAO for and on behalf of NASA under contract NAS8-03060. We thank the anonymous referee for a careful reading of our paper, thoughtful criticisms and useful suggestions. We also thank Jorn Wilms, Keith Jahoda, Craig Markwardt, and Nikolai Shaposhnikov for useful suggestions and valuable discussions. NR 28 TC 7 Z9 7 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 OCT 10 PY 2014 VL 794 IS 1 AR 73 DI 10.1088/0004-637X/794/1/73 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200073 ER PT J AU Gianninas, A Dufour, P Kilic, M Brown, WR Bergeron, P Hermes, JJ AF Gianninas, A. Dufour, P. Kilic, Mukremin Brown, Warren R. Bergeron, P. Hermes, J. J. TI PRECISE ATMOSPHERIC PARAMETERS FOR THE SHORTEST-PERIOD BINARY WHITE DWARFS: GRAVITATIONAL WAVES, METALS, AND PULSATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: abundances; stars: fundamental parameters; techniques: spectroscopic; white dwarfs ID EXTREMELY LOW-MASS; 3D MODEL ATMOSPHERES; SURFACE GRAVITY DISTRIBUTION; CETI INSTABILITY STRIP; MILLISECOND PULSAR; ECLIPSING BINARY; SPECTROSCOPIC ANALYSIS; DEBRIS DISKS; RADIATIVE LEVITATION; PLANETARY SYSTEMS AB We present a detailed spectroscopic analysis of 61 low-mass white dwarfs and provide precise atmospheric parameters, masses, and updated binary system parameters based on our new model atmosphere grids and the most recent evolutionary model calculations. For the first time, we measure systematic abundances of He, Ca, and Mg for metal-rich, extremely low mass white dwarfs and examine the distribution of these abundances as a function of effective temperature and mass. Based on our preliminary results, we discuss the possibility that shell flashes may be responsible for the presence of the observed He and metals. We compare stellar radii derived from our spectroscopic analysis to model-independent measurements and find good agreement except for white dwarfs with T-eff less than or similar to 10,000 K. We also calculate the expected gravitational wave strain for each system and discuss their significance to the eLISA space-borne gravitational wave observatory. Finally, we provide an update on the instability strip of extremely low mass white dwarf pulsators. C1 [Gianninas, A.; Kilic, Mukremin] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Dufour, P.; Bergeron, P.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Gianninas, A (reprint author), Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 West Brooks St, Norman, OK 73019 USA. EM alexg@nhn.ou.edu RI Alexandros, Gianninas/B-8352-2016 OI Alexandros, Gianninas/0000-0002-8655-4308 FU NSF [AST-1312678]; NASA [NNX14AF65G]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; Smithsonian Institution; NSERC Canada; Fund FRQ-NT (Quebec) FX We thank both referees for a careful reading of our manuscript and for their numerous suggestions that helped to improve this paper. We gratefully acknowledge the support from the NSF and NASA under grants AST-1312678 and NNX14AF65G, respectively. This research makes use of the SAO/NASA Astrophysics Data System Bibliographic Service. This project makes use of data products from the Sloan Digital Sky Survey, which has been funded by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. This work was supported in part by the Smithsonian Institution. This work is funded in part by the NSERC Canada and by the Fund FRQ-NT (Quebec). NR 107 TC 26 Z9 26 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 OCT 10 PY 2014 VL 794 IS 1 AR 35 DI 10.1088/0004-637X/794/1/35 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200035 ER PT J AU Henderson, CB Park, H Sumi, T Udalski, A Gould, A Tsapras, Y Han, C Gaudi, BS Bozza, V Abe, F Bennett, DP Bond, IA Botzler, CS Freeman, M Fukui, A Fukunaga, D Itow, Y Koshimoto, N Ling, CH Masuda, K Matsubara, Y Muraki, Y Namba, S Ohnishi, K Rattenbury, NJ Saito, T Sullivan, DJ Suzuki, D Sweatman, WL Tristram, PJ Tsurumi, N Wada, K Yamai, N Yock, PCM Yonehara, A Szymanski, MK Kubiak, M Pietrzynski, G Soszynski, I Skowron, J Kozlowski, S Poleski, R Ulaczyk, K Wyrzykowski, L Pietrukowicz, P Almeida, LA Bos, M Choi, JY Christie, GW Depoy, DL Dong, S Friedmann, M Hwang, KH Jablonski, F Jung, YK Kaspi, S Lee, CU Maoz, D McCormick, J Moorhouse, D Natusch, T Ngan, H Pogge, RW Shin, IG Shvartzvald, Y Tan, TG Thornley, G Yee, JC Allan, A Bramich, DM Browne, P Dominik, M Horne, K Hundertmark, M Jaimes, RF Kains, N Snodgrass, C Steele, IA Street, RA AF Henderson, C. B. Park, H. Sumi, T. Udalski, A. Gould, A. Tsapras, Y. Han, C. Gaudi, B. S. Bozza, V. Abe, F. Bennett, D. P. Bond, I. A. Botzler, C. S. Freeman, M. Fukui, A. Fukunaga, D. Itow, Y. Koshimoto, N. Ling, C. H. Masuda, K. Matsubara, Y. Muraki, Y. Namba, S. Ohnishi, K. Rattenbury, N. J. Saito, To Sullivan, D. J. Suzuki, D. Sweatman, W. L. Tristram, P. J. Tsurumi, N. Wada, K. Yamai, N. Yock, P. C. M. Yonehara, A. Szymanski, M. K. Kubiak, M. Pietrzynski, G. Soszynski, I. Skowron, J. Kozlowski, S. Poleski, R. Ulaczyk, K. Wyrzykowski, L. Pietrukowicz, P. Almeida, L. A. Bos, M. Choi, J. -Y. Christie, G. W. Depoy, D. L. Dong, S. Friedmann, M. Hwang, K. -H. Jablonski, F. Jung, Y. K. Kaspi, S. Lee, C. -U. Maoz, D. McCormick, J. Moorhouse, D. Natusch, T. Ngan, H. Pogge, R. W. Shin, I. -G. Shvartzvald, Y. Tan, T. -G. Thornley, G. Yee, J. C. Allan, A. Bramich, D. M. Browne, P. Dominik, M. Horne, K. Hundertmark, M. Jaimes, R. Figuera Kains, N. Snodgrass, C. Steele, I. A. Street, R. A. CA MOA Collaboration OGLE Collaboration FUN Collaboration RoboNet Collaboration TI CANDIDAIE GRAVITATIONAL MICROLENSING EVENTS FOR FUTURE DIRECT LENS IMAGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; gravitational lensing: micro ID GALACTIC BULGE; BINARY-LENS; CHEMICAL EVOLUTION; PLANETARY COMPANION; ORBITAL MOTION; OPTICAL DEPTH; MASS PLANET; BROWN DWARF; OGLE-III; PARALLAX AB The mass of the lenses giving rise to Galactic microlensing events can be constrained by measuring the relative lenssource proper motion and lens flux. The flux of the lens can be separated from that of the source, companions to the source, and unrelated nearby stars with high-resolution images taken when the lens and source are spatially resolved. For typical ground-based adaptive optics (AO) or space-based observations, this requires either inordinately long time baselines or high relative proper motions. We provide a list of microlensing events toward the Galactic bulge with high relative lens-source proper motion that are therefore good candidates for constraining the lens mass with future high-resolution imaging. We investigate all events from 2004 to 2013 that display detectable finite-source effects, a feature that allows us to measure the proper motion. In total, we present 20 events with mu >= 8 mas yr(-1). Of these, 14 were culled from previous analyses while 6 are new, including OGLE-2004-BLG-368, MOA-2005-BLG-36, OGLE-2012-BLG-0211, OGLE-2012-BLG-0456, MOA-2012-BLG-532, and MOA-2013-BLG-029. In <= 12 yr from the time of each event the lens and source of each event will be sufficiently separated for ground-based telescopes with AO systems or space telescopes to resolve each component and further characterize the lens system. Furthermore, for the most recent events, comparison of the lens flux estimates from images taken immediately to those estimated from images taken when the lens and source are resolved can be used to empirically check the robustness of the single-epoch method currently being used to estimate lens masses for many events. C1 [Henderson, C. B.; Gould, A.; Gaudi, B. S.; Poleski, R.; Pogge, R. W.; Yee, J. C.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Park, H.; Han, C.; Choi, J. -Y.; Hwang, K. -H.; Jung, Y. K.; Shin, I. -G.] Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. [Sumi, T.; Koshimoto, N.; Namba, S.; Suzuki, D.; Wada, K.] Osaka Univ, Dept Earth & Space Sci, Osaka 5600043, Japan. [Udalski, A.; Szymanski, M. K.; Kubiak, M.; Pietrzynski, G.; Soszynski, I.; Skowron, J.; Kozlowski, S.; Poleski, R.; Ulaczyk, K.; Wyrzykowski, L.; Pietrukowicz, P.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. [Tsapras, Y.; Street, R. A.] Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Tsapras, Y.] Univ London, Sch Math Sci, London E1 4NS, England. [Bozza, V.] Univ Salerno, Dept Phys, I-84084 Fisciano, SA, Italy. [Bozza, V.] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy. [Abe, F.; Fukunaga, D.; Itow, Y.; Masuda, K.; Matsubara, Y.; Muraki, Y.; Tsurumi, N.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Bennett, D. P.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Bond, I. A.; Ling, C. H.; Sweatman, W. L.] Massey Univ, Inst Informat & Math Sci, North Shore Mail Ctr, Auckland 0745, New Zealand. [Botzler, C. S.; Freeman, M.; Rattenbury, N. J.; Yock, P. C. M.] Univ Auckland, Dept Phys, Auckland 1001, New Zealand. [Fukui, A.] Victoria Univ, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Ohnishi, K.] Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan. [Saito, To] Nagano Natl Coll Technol, Nagano 3818550, Japan. [Sullivan, D. J.] Tokyo Metropolitan Coll Aeronaut, Tokyo 1168523, Japan. [Tristram, P. J.] Mt John Univ Observ, Lake Tekapo 8770, New Zealand. [Yamai, N.; Yonehara, A.] Kyoto Sangyo Univ, Fac Sci, Dept Phys, Kyoto 6038555, Japan. [Pietrzynski, G.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Wyrzykowski, L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Almeida, L. A.] Inst Astron Geofis & Ciecias Atmosfer IAG USP, Sao Paulo, Brazil. [Almeida, L. A.] Inst Nacl Pesquisas Espaciais, Sao Jose Dos Campos, SP, Brazil. [Bos, M.] Molehill Astron Observ, North Shore, New Zealand. [Christie, G. W.; Natusch, T.; Ngan, H.] Auckland Observ, Auckland, New Zealand. [Depoy, D. L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Dong, S.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Friedmann, M.; Kaspi, S.; Maoz, D.; Shvartzvald, Y.] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Jablonski, F.] Obsev Pico dos Dias, Brazopolis, MG, Brazil. [Lee, C. -U.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [McCormick, J.] Farm Cove Observ, Ctr Backyard Astrophys, Auckland, New Zealand. [Moorhouse, D.; Thornley, G.] Kumeu Observ, Kumeu, New Zealand. [Natusch, T.] AUT Univ, Inst Radiophys & Space Res, Auckland, New Zealand. [Tan, T. -G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Yee, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Allan, A.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Bramich, D. M.] Qatar Fdn, Qatar Environm & Energy Res Inst, Doha, Qatar. [Browne, P.; Dominik, M.; Horne, K.; Hundertmark, M.; Jaimes, R. Figuera] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Jaimes, R. Figuera; Kains, N.] European So Observ, D-85748 Garching, Germany. [Snodgrass, C.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Steele, I. A.] Liverpool John Moores Univ, Astrophys Res Inst, Wirral CH41 1LD, Merseyside, England. RP Han, C (reprint author), Chungbuk Natl Univ, Inst Astrophys, Dept Phys, Cheongju 371763, South Korea. RI Almeida, L./G-7188-2012; Skowron, Jan/M-5186-2014; Hundertmark, Markus/C-6190-2015; Kozlowski, Szymon/G-4799-2013; OI Skowron, Jan/0000-0002-2335-1730; Hundertmark, Markus/0000-0003-0961-5231; Kozlowski, Szymon/0000-0003-4084-880X; Tan, Thiam-Guan/0000-0001-5603-6895; Snodgrass, Colin/0000-0001-9328-2905 FU National Science Foundation (NSF) [DGE-0822215]; European Research Council under the European Community [246678]; National Research Foundation of Korea [2009-0081561]; NSF [AST-1103471]; NASA [NNX12AB99G]; Chinese Academy of Sciences [XDB09000000]; Qatar National Research Fund (a member of the Qatar Foundation) [NPRP-09-476-1-78, X-019-1-006]; [JSPS23340044]; [JSPS24253004] FX This material is based upon work supported by the National Science Foundation (NSF) Graduate Research Fellowship Program under grant No. DGE-0822215, awarded to C.B.H., and an international travel allowance through the Graduate Research Opportunities Worldwide, also awarded to C.B.H. and taken to Cheongju, Korea. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the NSF. T.S. is supported by the grant JSPS23340044 and JSPS24253004. The OGLE project has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 246678 to A.U. Work by C.H. was supported by the Creative Research Initiative Program (2009-0081561) of the National Research Foundation of Korea. A.G. and B.S.G. acknowledge support from NSF AST-1103471 and from NASA grant NNX12AB99G. S.D. is supported by "The Strategic Priority Research Program-The Emergence of Cosmological Structures" of the Chinese Academy of Sciences (Grant No. XDB09000000). Work by J.C.Y. was performed in part under contract with the California Institute of Technology (Caltech) funded by NASA through the Sagan Fellowship Program. M.D., K.H., M.H., C.S., R.A.S., and Y.T. acknowledge grant NPRP-09-476-1-78 from the Qatar National Research Fund (a member of the Qatar Foundation). This publication was made possible by NPRP grant #X-019-1-006 from the Qatar National Research Fund (a member of the Qatar Foundation). NR 65 TC 7 Z9 7 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2014 VL 794 IS 1 AR 71 DI 10.1088/0004-637X/794/1/71 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200071 ER PT J AU Johnson, JA Huber, D Boyajian, T Brewer, JM White, TR von Braun, K Maestro, V Stello, D Barclay, T AF Johnson, John Asher Huber, Daniel Boyajian, Tabetha Brewer, John M. White, Timothy R. von Braun, Kaspar Maestro, Vicente Stello, Dennis Barclay, Thomas TI THE PHYSICAL PARAMETERS OF THE RETIRED A STAR HD 185351 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: abundances; stars: individual (HD 185351); stars: interiors; stars: oscillations ID SOLAR-LIKE OSCILLATIONS; STELLAR ASTROPHYSICS MESA; BASE-LINE INTERFEROMETRY; VIRTUAL OBSERVATORY TOOL; GIANT IOTA-DRACONIS; SUN-LIKE STAR; K-TYPE STARS; RED-GIANT; CHARA ARRAY; MAIN-SEQUENCE AB We report here an analysis of the physical stellar parameters of the giant star HD 185351 using Kepler short-cadence photometry, optical and near infrared interferometry from CHARA, and high-resolution spectroscopy. Asteroseismic oscillations detected in the Kepler short-cadence photometry combined with an effective temperature calculated from the interferometric angular diameter and bolometric flux yield a mean density rho(star) = 0.0130 +/- 0.0003 rho(circle dot) and surface gravity log g = 3.280+/-0.011. Combining the gravity and density we find R-star = 5.35 +/- 0.20 R-circle dot and M-star=1.99 +/- 0.23M(circle dot). The trigonometric parallax and CHARA angular diameter give a radius R-star = 4.97+/-0.07 R-circle dot. This smaller radius, when combined with the mean stellar density, corresponds to a stellar mass 1.60 +/- 0.08 M-circle dot, which is smaller than the asteroseismic mass by 1.6 sigma. We find that a larger mass is supported by the observation of mixed modes in our high-precision photometry, the spacing of which is consistent only for M-star greater than or similar to 1.8M(circle dot). Our various and independent mass measurements can be compared to the mass measured from interpolating the spectroscopic parameters onto stellar evolution models, which yields a model-based mass M-star, (model) = 1.87+/-0.07 M-circle dot. This mass agrees well with the asteroseismic value, but is 2.6 sigma higher than the mass from the combination of asteroseismology and interferometry. The discrepancy motivates future studies with a larger sample of giant stars. However, all of our mass measurements are consistent with HD 185351 having a mass in excess of 1.5M(circle dot). C1 [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Huber, Daniel; Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Boyajian, Tabetha; Brewer, John M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [White, Timothy R.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [White, Timothy R.; Maestro, Vicente; Stello, Dennis] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [von Braun, Kaspar] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Stello, Dennis] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. RP Johnson, JA (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. OI Brewer, John/0000-0002-9873-1471; Boyajian, Tabetha/0000-0001-9879-9313 FU NASA Science Mission directorate; NASA [NAS5-26555, NNX14AB92G, ADAP12-0172]; NASA Office of Space Science [NNX09AF08G]; W.M. Keck Foundation; Alfred P. Sloan foundation; David and Lucile Packard foundation; National Science Foundation [AST-0606958, AST-0908253]; Georgia State University through the College of Arts and Sciences; W. M. Keck Foundation; Danish National Research Foundation [DNRF106]; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) - European Research Council [267864] FX 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 Kepler Team for their extensive efforts in producing such high quality data. Some of the data presented in this paper were 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 NNX09AF08G and by other grants and contracts.; 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. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Grant Hill and Scott Dahm for support of HIRES and Greg Wirth for support of remote observing. 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.; J.A.J. is grateful for the generous grant support provided by the Alfred P. Sloan and David and Lucile Packard foundations, and acknowledges enlightening conversations with Dimitar Sasselov, Peter Goldreich, Phil Muirhead, Jason Wright, Debra Fischer, Jeff Valenti, James Lloyd and Victoria "Ashley" Villar.; D.H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center administered by Oak Ridge Associated Universities, and NASA Grant NNX14AB92G issued through the Kepler Participating Scientist Program.; T.S.B acknowledges support provided through NASA grant ADAP12-0172.; The CHARA Array is funded by the National Science Foundation through NSF grants AST-0606958 and AST-0908253 and by Georgia State University through the College of Arts and Sciences, as well as the W. M. Keck Foundation.; Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant agreement No.: DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No.: 267864). NR 133 TC 16 Z9 16 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2014 VL 794 IS 1 AR 15 DI 10.1088/0004-637X/794/1/15 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200015 ER PT J AU McDonald, M Benson, BA Vikhlinin, A Aird, KA Allen, SW Bautz, M Bayliss, M Bleem, LE Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Crawford, TM Crites, AT de Haan, T Dobbs, MA Foley, RJ Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Hlavacek-Larrondo, J Holder, GP Holzapfel, WL Hrubes, JD Jones, C Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McMahon, JJ Meyer, SS Miller, ED Mocanu, L Mohr, JJ Murray, SS Padin, S Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shirokoff, E Spieler, HG Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, KT Stubbs, CW Vanderlinde, K Vieira, JD Williamson, R Zahn, O Zenteno, A AF McDonald, M. Benson, B. A. Vikhlinin, A. Aird, K. A. Allen, S. W. Bautz, M. Bayliss, M. Bleem, L. E. Bocquet, S. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Foley, R. J. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Hlavacek-Larrondo, J. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McMahon, J. J. Meyer, S. S. Miller, E. D. Mocanu, L. Mohr, J. J. 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. Spieler, H. G. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. T. Stubbs, C. W. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. Zenteno, A. TI THE REDSHIFT EVOLUTION OF THE MEAN I EMPERATURE, PRESSURE, AND ENTROPY PROFILES IN 80 SPT-SELECTED GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: intracluster medium; early universe; X-rays: galaxies: clusters ID SOUTH-POLE TELESCOPE; ACTIVE GALACTIC NUCLEI; DARK-MATTER HALOES; 720 SQUARE DEGREES; GAS MASS FRACTION; X-RAY-CLUSTERS; M-T RELATION; SUNYAEV-ZELDOVICH; TEMPERATURE PROFILES; XMM-NEWTON AB Confirming earlier results from this data set, we find an absence of strong cool cores at high z, manifested in this analysis as a significantly lower observed pressure in the central 0.1R(500) of the high-z cool-core subset of clusters compared to the low-z cool-core subset. Overall, our observed pressure profiles agree well with earlier lower-redshift measurements, suggesting minimal redshift evolution in the pressure profile outside of the core. We find no measurable redshift evolution in the entropy profile at r <= 0.7R(500)-this may reflect a long-standing balance between cooling and feedback over long timescales and large physical scales. We observe a slight flattening of the entropy profile at r >= R500 in our high-z subsample. This flattening is consistent with a temperature bias due to the enhanced (similar to 3x) rate at which group-mass (similar to 2 keV) halos, which would go undetected at our survey depth, are accreting onto the cluster at z similar to 1. This work demonstrates a powerful method for inferring spatially resolved cluster properties in the case where individual cluster signal-to-noise is low, but the number of observed clusters is high. C1 [McDonald, M.; Bautz, M.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Benson, B. A.] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Keisler, R.; Leitch, E. M.; Mantz, A.; Meyer, S. S.; Mocanu, L.; Padin, S.; Schaffer, K. K.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Padin, S.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bayliss, M.; Forman, W. R.; Jones, C.; Murray, S. S.; Schaffer, K. K.; Stalder, B.; Stark, A. A.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Allen, S. W.; Hlavacek-Larrondo, J.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Allen, S. W.; Hlavacek-Larrondo, J.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Allen, S. W.; Crites, A. T.; Williamson, R.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Bayliss, M.; Stubbs, C. W.] 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.; Liu, J.; McMahon, J. J.; Saro, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Liu, J.; Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Cho, H. M.] NIST, Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrosif, Santiago, Chile. [Lueker, M.; Padin, S.; Shirokoff, E.; Staniszewski, Z.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, 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.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [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. [Hlavacek-Larrondo, J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [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, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [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.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. [Zenteno, A.] Cerro Tololo Interamer Observ, La Serena, Chile. RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mcdonald@space.mit.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Forman, William/0000-0002-9478-1682; Stark, Antony/0000-0002-2718-9996 FU NASA [HST-HF51308.01, 12800071, 12800088, 13800883]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]; National Science Foundation [ANT-0638937, PLR-1248097]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada, Canada Research Chairs program; Canadian Institute for Advanced Research; U.S. Department of Energy [DE-AC02-06CH11357]; NASA through the Einstein Fellowship Program [PF2-130094] FX We thank M. Voit and N. Battaglia for helpful discussions, along with K. Dolag, for sharing their simulated galaxy cluster pressure profiles. M. M. acknowledges support by NASA through a Hubble Fellowship grant HST-HF51308.01-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. The South Pole Telescope program is supported by the National Science Foundation through grants ANT-0638937 and 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. Support for X-ray analysis was provided by NASA through Chandra Award Numbers 12800071, 12800088, and 13800883 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012 and at SAO in part by NSF grants AST-1009649 and MRI-0723073. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. Argonne National Laboratory's work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. J.H.L. is supported by NASA through the Einstein Fellowship Program, grant number PF2-130094. NR 83 TC 25 Z9 25 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 OCT 10 PY 2014 VL 794 IS 1 AR 67 DI 10.1088/0004-637X/794/1/67 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200067 ER PT J AU Nayyeri, H Mobasher, B Hemmati, S De Barros, S Ferguson, HC Wiklind, T Dahlen, T Dickinson, M Giavalisco, M Fontana, A Ashby, M Barro, G Guo, Y Hathi, NP Kassin, S Koekemoer, A Willner, S Dunlop, JS Paris, D Targett, TA AF Nayyeri, H. Mobasher, B. Hemmati, S. De Barros, S. Ferguson, H. C. Wiklind, T. Dahlen, T. Dickinson, M. Giavalisco, M. Fontana, A. Ashby, M. Barro, G. Guo, Y. Hathi, N. P. Kassin, S. Koekemoer, A. Willner, S. Dunlop, J. S. Paris, D. Targett, T. A. TI A STUDY OF MASSIVE AND EVOLVED GALAXIES AT HIGH REDSHIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; DARK-MATTER HALOES; LY-ALPHA EMISSION; DEEP-FIELD-SOUTH; ULTRAVIOLET LUMINOSITY DENSITY; EXTRAGALACTIC LEGACY SURVEY; REST-FRAME ULTRAVIOLET; EXTREMELY RED H; SIMILAR-TO 4 AB We use data taken as part of Hubble Space Telescope (HS7)/Wide Field Camera 3 (WFC3) observations of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) to identify massive and evolved galaxies at 3 < z < 4.5. This is performed using the strength of the Balmer break feature at rest-frame 3648 angstrom, which is a diagnostic of the age of the stellar population in galaxies. Using the WFC3 H-band-selected catalog for the CANDELS GOODS-S field and deep multi-waveband photometry from optical (HST) to mid-infrared (Spitzer) wavelengths, we identify a population of old and evolved post-starburst galaxies based on the strength of their Balmer breaks (Balmer break galaxies, BBGs). The galaxies are also selected to be bright in rest-frame near-IR wavelengths and hence massive. We identify a total of 16 BBGs. Fitting the spectral energy distribution of the BBGs shows that the candidate galaxies have average estimated ages of similar to 800 Myr and average stellar masses of similar to 5 x 10(10) M-circle dot, consistent with being old and massive systems. Two of our BBG candidates are also identified by the criteria that are sensitive to star-forming galaxies (Lyman break galaxy selection). We find a number density of similar to 3.2 x 10(-5) Mpc(-3) for the BBGs, corresponding to a mass density of similar to 2.0 x 10(6) M-circle dot Mpc(-3) in the redshift range covering the survey. Given the old age and the passive evolution, it is argued that some of these objects formed the bulk of their mass only a few hundred million years after the big bang. C1 [Nayyeri, H.; Mobasher, B.; Hemmati, S.; De Barros, S.] Univ Calif Riverside, Riverside, CA 92512 USA. [Ferguson, H. C.; Wiklind, T.; Dahlen, T.; Kassin, S.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Giavalisco, M.] Univ Massachusetts, Amherst, MA 01003 USA. [Fontana, A.; Paris, D.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Ashby, M.; Willner, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barro, G.; Guo, Y.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Hathi, N. P.] Lab Astrophys Marseille, F-13013 Marseille, France. [Dunlop, J. S.; Targett, T. A.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Targett, T. A.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. RP Nayyeri, H (reprint author), Univ Calif Riverside, Riverside, CA 92512 USA. RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Koekemoer, Anton/0000-0002-6610-2048 FU Jet Propulsion Laboratory, California Institute of Technology; NASA [NAS5-26555]; HST [GO-12060]; Space Telescope Science Institute FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for HST Programs GO-12060 is 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 NAS5-26555. The authors also wish to thank the anonymous referee for thoroughly reading the manuscript and providing very useful comments and suggestions. NR 83 TC 15 Z9 15 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2014 VL 794 IS 1 AR 68 DI 10.1088/0004-637X/794/1/68 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200068 ER PT J AU Nguyen, DD Seth, AC Reines, AE den Brok, M Sand, D McLeod, B AF Nguyen, Dieu D. Seth, Anil C. Reines, Amy E. den Brok, Mark Sand, David McLeod, Brian TI Extended Structure and Fate of the Nucleus in Henize 2-10 SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; surveys; techniques: spectroscopic ID MASSIVE BLACK-HOLES; EARLY-TYPE GALAXIES; DIGITAL SKY SURVEY; SURFACE BRIGHTNESS PROFILES; MULTI-GAUSSIAN EXPANSION; DWARF STARBURST GALAXIES; VIRGO-CLUSTER SURVEY; SUPER-STAR-CLUSTERS; X-RAY SURVEY; GLOBULAR-CLUSTERS AB We investigate the structure and nuclear region of the black hole (BH) hosting galaxy Henize 2-10. Surface brightness profiles are analyzed using Magellan/Megacam g- and r-band images. Excluding the central starburst, we find a best-fit two-component Sersic profile with n(in) similar to 0.6, r(eff,in) similar to 260 pc and n(out) similar to 1.8, r similar to 1 kpc. Integrating out to our outermost data point (100 '' similar to 4.3 kpc), we calculate M-g = 19.2 and M-r = 19.8. The corresponding enclosed stellar mass is M-* similar to (10 +/- 3) x 10(9) M-circle dot, similar to 3x larger than previous estimates. Apart from the central less than or similar to 500 pc, with blue colors and an irregular morphology, the galaxy appears to be an early-type system. The outer color is quite red, (g r)(0) = 0.75, suggesting a dominant old population. We study the nuclear region of the galaxy using archival Gemini/NIFS K-band adaptive optics spectroscopy and Hubble Space Telescope imaging. We place an upper limit on the BH mass of similar to 10(7) M-circle dot from the NIFS data, consistent with that from the M-BH-radio X-ray fundamental plane. No coronal lines are seen, but a Br gamma source is located at the position of the BH with a luminosity consistent with the X-ray emission. The starburst at the center of Henize 2-10 has led to the formation of several super star clusters, which are within 100 pc of the BH. We examine the fate of the nucleus by estimating the dynamical masses and dynamical friction timescales of the clusters. The most massive clusters (-106 Mo) have rdyn less than or similar to 200 Myr, and thus Henize 2-10 may represent a rare snapshot of nuclear star cluster formation around a preexisting massive BH. C1 [Nguyen, Dieu D.; Seth, Anil C.; den Brok, Mark] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Reines, Amy E.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Sand, David] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [McLeod, Brian] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nguyen, DD (reprint author), Univ Utah, Dept Phys & Astron, 115 South 1400 East, Salt Lake City, UT 84112 USA. EM dieu.nguyen@utah.edu; aseth@astro.utah.odu; areines@nrao.cdu; denhrok@physics.utah.odu; david.sand@ttu.cdu; bmcleod@cfa.harvard.edu OI Seth, Anil/0000-0003-0248-5470; McLeod, Brian/0000-0002-2924-2893 FU University of Utah, Physics and Astronomy Department; NASA through the Einstein Fellowship Program [PF1-120086] FX We thank Maureen Conroy at the SAO/TDC for providing us the Magellan/Megacam data of g, i, and r bands; Micheva Genoveva for generously sharing us with her SB profiles in five Bessel-Johnson filters UBVHK; and the University of Utah, Physics and Astronomy Department, for supporting this work. The authors also thank Fabio Antonini for helpful discussions. Support for A.E.R. was provided by NASA through the Einstein Fellowship Program, grant PF1-120086. NR 101 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 OCT 10 PY 2014 VL 794 IS 1 AR 34 DI 10.1088/0004-637X/794/1/34 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200034 ER PT J AU Tremaine, S Shen, Y Liu, X Loeb, A AF Tremaine, Scott Shen, Yue Liu, Xin Loeb, Abraham TI RELATIVISTIC REDSHIFTS IN QUASAR BROAD LINES SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: emission lines; relativistic processes ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; PEAKED EMISSION-LINES; ACCRETION DISK; SCALING RELATIONSHIPS; DATA RELEASE; GALAXIES; REVERBERATION; REGION; SAMPLE AB The broad emission lines commonly seen in quasar spectra have velocity widths of a few percent of the speed of light, so special- and general-relativistic effects have a significant influence on the line profile. We have determined the redshift of the broad H beta line in the quasar rest frame (determined from the core component of the [0 III]line) for over 20,000 quasars from the Sloan Digital Sky Survey Data Release 7 quasar catalog. The mean redshift as a function of line width is approximately consistent with the relativistic redshift that is expected if the line originates in a randomly oriented Keplerian disk that is obscured when the inclination of the disk to the line of sight exceeds 30-45, consistent with simple active galactic nucleus unification schemes. This result also implies that the net line-of-sight inflow/outflow velocities in the broad-line region are much less than the Keplerian velocity when averaged over a large sample of quasars with a given line width. C1 [Tremaine, Scott] Inst Adv Study, Princeton, NJ 08540 USA. [Shen, Yue] Carnegie Observ, Pasadena, CA 91101 USA. [Liu, Xin] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Loeb, Abraham] Harvard Univ, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Tremaine, S (reprint author), Inst Adv Study, Olden Lane, Princeton, NJ 08540 USA. EM tremaine@ias.odu; yshen@obs.carnegiescience.edu; xinliu@astro.ucla.du; aloeb@cfa.harvard.edu RI Tremaine, Scott/M-4281-2015 OI Tremaine, Scott/0000-0002-0278-7180 FU NASA grants [NNX11AF29G, NNX14AM24G]; NASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF-51314.01, HST-HF-51307.01]; NASA [NAS 5-26555]; 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 FX We thank Michael Eracleous, Nadia Zakamska, and the anonymous referee for their insights. This research was supported in part by NASA grants NNX11AF29G and NNX14AM24G. Support for the work of Y.S. and X.L. was provided by NASA through Hubble Fellowship grant Nos. HST-HF-51314.01 and HST-HF-51307.01, 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. 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/. NR 43 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 OCT 10 PY 2014 VL 794 IS 1 AR 49 DI 10.1088/0004-637X/794/1/49 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200049 ER PT J AU Vajgel, B Jones, C Lopes, PAA Forman, WR Murray, SS Goulding, A Andrade-Santos, F AF Vajgel, Bruna Jones, Christine Lopes, Paulo A. A. Forman, William R. Murray, Stephen S. Goulding, Andrew Andrade-Santos, Felipe TI X-RAY-SELECTED GALAXY GROUPS IN BOOTES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: groups: general; surveys X-rays: galaxies: clusters ID ABELL CLUSTER SURVEY; WIDE-FIELD SURVEY; LUMINOSITY FUNCTION; SCALING RELATIONS; TEMPERATURE RELATION; EVOLUTION; SAMPLE; CHANDRA; SDSS; DEEP AB We present the X-ray and optical properties of the galaxy groups selected in the Chandra X-Bootes survey. We used follow-up Chandra observations to better define the group sample and their X-ray properties. Group redshifts were measured from the AGN and Galaxy Evolution Survey spectroscopic data. We used photometric data from the NOAO Deep Wide Field Survey to estimate the group richness (N-gals) and the optical luminosity (L-opt). Our final sample comprises 32 systems at z < 1.75 with 14 below z = 0.35. For these 14 systems, we estimate velocity dispersions (sigma(gr)) and perform a virial analysis to obtain the radii (R-200 and R-500) and total masses (M-200 and M-500) for groups with at least 5 galaxy members. We use the Chandra X-ray observations to derive the X-ray luminosity (L-X). We examine the performance of the group properties sigma(gr), L-opt, and L-X, as proxies for the group mass. Understanding how well these observables measure the total mass is important to estimate how precisely the cluster/group mass function is determined. Exploring the scaling relations built with the X-Bootes sample and comparing these with samples from the literature, we find a break in the L-X-M-500 relation at approximately M-500 = 5 x 10(13) M-circle dot (for M-500 > 5 X 10(13) M-circle dot, M-500 proportional to L-X(0.61 +/- 0.02), a while for M-500 <= 5 x 10(13) M-circle dot, M-500 proportional to L-X(0.44 +/- 0.05)). Thus, mass luminosity relation for galaxy groups cannot be described by the same power law as galaxy clusters. A possible explanation for this break is the dynamical friction, tidal interactions, and projection effects that reduce the velocity dispersion values of the galaxy groups. By extending the cluster luminosity function to the group regime, we predict the number of groups that new X-ray surveys, particularly eROSITA, will detect. Based on our cluster/group luminosity function estimates, eROSITA will identify 1800 groups (L-X = 10(41)-10(43) erg s(-1)) within a distance of 200 Mpc. Since groups lie in large-scale filaments, this group sample will map the large-scale structure of the local universe. C1 [Vajgel, Bruna; Lopes, Paulo A. A.] Univ Fed Rio de Janeiro, Observ Valongo, Rio De Janeiro, RJ, Brazil. [Vajgel, Bruna; Jones, Christine; Forman, William R.; Murray, Stephen S.; Goulding, Andrew; Andrade-Santos, Felipe] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Vajgel, B (reprint author), Univ Fed Rio de Janeiro, Observ Valongo, Rio De Janeiro, RJ, Brazil. RI Lopes, Paulo/B-3055-2013; OI Forman, William/0000-0002-9478-1682 FU Chandra grant; NASA grant; Smithsonian Institute grant; CsF/CNPq grant [237321/2012-2] FX The work was supported in part by Chandra grant, NASA grant, Smithsonian Institute grant, and CsF/CNPq grant 237321/2012-2. NR 75 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 OCT 10 PY 2014 VL 794 IS 1 AR 88 DI 10.1888/0004-637X/794/1/88 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200088 ER PT J AU Zhang, SN Wang, QD Ji, L Smith, RK Foster, AR Zhou, X AF Zhang, Shuinai Wang, Q. Daniel Ji, Li Smith, Randall K. Foster, Adam R. Zhou, Xin TI SPECTRAL MODELING OF THE CHARGE-EXCHANGE X-RAY EMISSION FROM M82 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M82); galaxies: starburst; X-rays: galaxies ID STARBURST GALAXY M82; REFLECTION GRATING SPECTROMETER; H-ALPHA EMISSION; GALACTIC WINDS; INTERSTELLAR-MEDIUM; XMM-NEWTON; CHANDRA OBSERVATIONS; HOT GAS; NGC 253; SUPERWINDS AB It has been proposed that the charge-exchange (CX) process at the interface between hot and cool interstellar gases could contribute significantly to the observed soft X-ray emission in star-forming galaxies. We analyze the XMM-Newton/reflection grating spectrometer (RGS) spectrum of M82 using a newly developed CX model combined with a single-temperature thermal plasma to characterize the volume-filling hot gas. The CX process is largely responsible for not only the strongly enhanced forbidden lines of the Ka triplets of various He-like ions but also good fractions of the Ly alpha transitions of C (similar to 87%), 0 VIII, and N VII (>= 50%) as well. In total about a quarter of the X-ray flux in the RGS 6-30 angstrom band originates in the CX. We infer an ion incident rate of 3 x 10(51) s(-1) undergoing CX at the hot and cool gas interface and an effective area of the interface of 2 x 1045 cm2 that is one order of magnitude larger than the cross section of the global biconic outflow. With the CX contribution accounted for, the best-fit temperature of the hot gas is 0.6 keV, and the metal abundances are approximately solar. We further show that the same CX/thermal plasma model also gives an excellent description of the EPIC-pn spectrum of the outflow Cap, projected at 11.6 kpc away from the galactic disk of M82. This analysis demonstrates that the CX is potentially an important contributor to the X-ray emission from starburst galaxies and also an invaluable tool to probe the interface astrophysics. C1 [Zhang, Shuinai; Ji, Li; Zhou, Xin] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Zhang, Shuinai; Ji, Li] Chinese Acad Sci, Key Lab Dark Matter & Space Astron, Nanjing 210008, Jiangsu, Peoples R China. [Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Smith, Randall K.; Foster, Adam R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhou, Xin] Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Jiangsu, Peoples R China. RP Zhang, SN (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. EM snzhang@pmo.ac.cn FU National Natural Science Foundation of China [11203080]; Smithsonian Institution's Competitive Grants; 100 Talents program of the Chinese Academy of Sciences FX We gratefully acknowledge the anonymous referee for the comments that improved this paper. We thank John Houck for help on solving all ISIS software problems, and thank Keith Arnaud for help on the installation of the RGSXSRC script that is removed from the 12.7 version of Xspec. The work is partly supported by the National Natural Science Foundation of China under the grant 11203080 and by the Smithsonian Institution's Competitive Grants for Science. L.J. is also supported by the 100 Talents program of the Chinese Academy of Sciences. NR 54 TC 5 Z9 5 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 OCT 10 PY 2014 VL 794 IS 1 AR 61 DI 10.1088/0004-637X/794/1/61 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ1YO UT WOS:000342581200061 ER PT J AU Ale-Rocha, R Freitas, G Mathis, WN AF Ale-Rocha, Rosaly Freitas, Geovania Mathis, Wayne N. TI Revision of the Neotropical genus Marbenia Malloch (Diptera: Periscelididae) SO ZOOTAXA LA English DT Article DE Periscelidinae; systematics; Neotropical Region; Amazonian Region AB The Neotropical genus Marbenia Malloch is revised and now includes 3 species: Marbenia cinerea, sp. nov., Marbenia pallida, sp. nov. and Marbenia peculiaris Malloch, 1931. The genus is herein recorded from the amazonian region of South America (Bolivia, Brazil and Ecuador), and characters of male and female terminalia are illustrated for the first time. C1 [Ale-Rocha, Rosaly; Freitas, Geovania] Inst Nacl de Pesquisas da Amazonia, BR-69067375 Manaus, Amazonas, Brazil. [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Ale-Rocha, R (reprint author), Inst Nacl de Pesquisas da Amazonia, Av Andr Araujo 2936, BR-69067375 Manaus, Amazonas, Brazil. EM alerocha@inpa.gov.br; geovaniafreitas@bol.com.br; mathisw@si.edu FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Fundacao de Amparo Pesquisa do Estado do Amazonas (FAPEAM); Incremento do conhecimento da diversidade, formacao e fixacao de especialistas em Sistematica de Diptera (Insecta) na Amazonia; Sistematica morfologica de Hybotidae (Diptera, Empidoidea) com enfase nas especies neotropicais de Ocydromiinae e Hybotinae, Edital Universal [471616/2011-7] FX We thank Dr. Orlando Tobias Silveira (MPEG) who kindly loaned some of the specimens used in this study; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) for the support to the first two authors through the fellowship and grant provided to the project Sistematica morfologica de Hybotidae (Diptera, Empidoidea) com enfase nas especies neotropicais de Ocydromiinae e Hybotinae, Edital Universal n. 471616/2011-7, as well to Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) and Fundacao de Amparo Pesquisa do Estado do Amazonas (FAPEAM) by the grant provided to the project Incremento do conhecimento da diversidade, formacao e fixacao de especialistas em Sistematica de Diptera (Insecta) na Amazonia. We are also grateful to two anonymous reviwers who made useful suggestions on the manuscript. NR 10 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 OCT 10 PY 2014 VL 3872 IS 4 BP 365 EP 375 PG 11 WC Zoology SC Zoology GA AQ6BW UT WOS:000342893600003 PM 25544089 ER PT J AU Boys, BL Martin, RV van Donkelaar, A MacDonell, RJ Hsu, NC Cooper, MJ Yantosca, RM Lu, Z Streets, DG Zhang, Q Wang, SW AF Boys, B. L. Martin, R. V. van Donkelaar, A. MacDonell, R. J. Hsu, N. C. Cooper, M. J. Yantosca, R. M. Lu, Z. Streets, D. G. Zhang, Q. Wang, S. W. TI Fifteen-Year Global Time Series of Satellite-Derived Fine Particulate Matter SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID LONG-TERM TREND; AEROSOL OPTICAL-THICKNESS; AIR-POLLUTION; RIVER DELTA; CHINA; CALIBRATION; VISIBILITY; PM2.5; MISR; PERSPECTIVE AB Ambient fine particulate matter (PM2.5) is a leading environmental risk factor for premature mortality. We use aerosol optical depth (AOD) retrieved from two satellite instruments, MISR and SeaWiFS, to produce a unified 15-year global time series (1998-2012) of ground-level PM2.5 concentration at a resolution of 1 degrees x 1 degrees. The GEOS-Chem chemical transport model (CTM) is used to relate each individual AOD retrieval to ground-level PM2.5. Four broad areas showing significant, spatially coherent, annual trends are examined in detail: the Eastern U.S. (-0.39 +/- 0.10 mu g m(-3) yr(-1)), the Arabian Peninsula (0.81 +/- 0.21 mu g m(-3) yr(-1)), South Asia (0.93 +/- 0.22 mu g m(-3) yr(-1)) and East Asia (0.79 +/- 0.27 mu g m(-3) yr(-1)). Over the period of dense in situ observation (1999-2012), the linear tendency for the Eastern U.S. (-0.37 +/- 0.13 mu g m(-3) yr(-1)) agrees well with that from in situ measurements (-0.38 +/- 0.06 mu g m(-3) yr(-1)). A GEOS-Chem simulation reveals that secondary inorganic aerosols largely explain the observed PM2.5 trend over the Eastern U.S., South Asia, and East Asia, while mineral dust largely explains the observed trend over the Arabian Peninsula. C1 [Boys, B. L.; Martin, R. V.; van Donkelaar, A.; MacDonell, R. J.; Cooper, M. J.] Dalhousie Univ, Halifax, NS, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hsu, N. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Yantosca, R. M.] Harvard Univ, Cambridge, MA 02138 USA. [Lu, Z.; Streets, D. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Zhang, Q.; Wang, S. W.] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China. RP Boys, BL (reprint author), Dalhousie Univ, Halifax, NS, Canada. EM briboys@gmail.com RI Chem, GEOS/C-5595-2014; Zhang, Qiang/D-9034-2012; Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 FU NSERC Canada; Izaak Walton Killiam Memorial Scholarship FX Funding for this work was provided by NSERC Canada and by an Izaak Walton Killiam Memorial Scholarship for B. L. Boys. Computational facilities are partially provided by ACEnet, the regional high performance computing consortium for universities in Atlantic Canada. We thank the AERONET, MISR, SeaWiFS, CALIPSO, IMPROVE, and AQS science teams for making their data publicly available. NR 65 TC 36 Z9 36 U1 9 U2 68 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD OCT 7 PY 2014 VL 48 IS 19 BP 11109 EP 11118 DI 10.1021/es502113p PG 10 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA AQ7RJ UT WOS:000343016600014 PM 25184953 ER PT J AU Safavi-Naini, A Capogrosso-Sansone, B Kuklov, A AF Safavi-Naini, A. Capogrosso-Sansone, B. Kuklov, A. TI Quantum phases of hard-core dipolar bosons in coupled one-dimensional optical lattices SO PHYSICAL REVIEW A LA English DT Article ID POLAR-MOLECULES; SYSTEMS; GASES AB Hard-core dipolar bosons trapped in a parallel stack of N >= 2 one-dimensional optical lattices (tubes) can develop several phases made of composites of particles from different tubes: superfluids, supercounterfluids, and insulators as well as mixtures of those. Bosonization analysis shows that these phases are thresholdless with respect to the dipolar interaction, with the key "control knob" being filling factors in each tube, provided the intertube tunneling is suppressed. The effective ab initio quantum Monte Carlo algorithm capturing these phases is introduced and some results are presented. C1 [Safavi-Naini, A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Safavi-Naini, A.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Capogrosso-Sansone, B.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Kuklov, A.] CUNY, CSI, Dept Engn & Phys, Staten Isl, NY 10314 USA. RP Safavi-Naini, A (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. FU NSF [PHY1314469]; CUNY HPCC under NSF [CNS-0855217, CNS-0958379, ACI-1126113]; National Science Foundation [ACI-1053575]; OU Supercomputing Center for Education & Research (OSCER) at the University of Oklahoma (OU) FX This work was supported by the NSF through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, Grant No. PHY1314469, and by a grant from CUNY HPCC under NSF Grants No. CNS-0855217, No. CNS-0958379, and No. ACI-1126113. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation Grant No. ACI-1053575 and the OU Supercomputing Center for Education & Research (OSCER) at the University of Oklahoma (OU). NR 41 TC 4 Z9 4 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD OCT 6 PY 2014 VL 90 IS 4 AR 043604 DI 10.1103/PhysRevA.90.043604 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AS0AR UT WOS:000343941500007 ER PT J AU Hild, S Fukuhara, T Schauss, P Zeiher, J Knap, M Demler, E Bloch, I Gross, C AF Hild, Sebastian Fukuhara, Takeshi Schauss, Peter Zeiher, Johannes Knap, Michael Demler, Eugene Bloch, Immanuel Gross, Christian TI Far-from-Equilibrium Spin Transport in Heisenberg Quantum Magnets SO PHYSICAL REVIEW LETTERS LA English DT Article ID INFINITE-TEMPERATURE; FERMI GAS; DYNAMICS; DIFFUSION; MODEL; INSULATOR; LATTICE; SYSTEM; STATES; TMMC AB We study experimentally the far-from-equilibrium dynamics in ferromagnetic Heisenberg quantum magnets realized with ultracold atoms in an optical lattice. After controlled imprinting of a spin spiral pattern with an adjustable wave vector, we measure the decay of the initial spin correlations through single-site resolved detection. On the experimentally accessible time scale of several exchange times, we find a profound dependence of the decay rate on the wave vector. In one-dimensional systems, we observe diffusionlike spin transport with a dimensionless diffusion coefficient of 0.22(1). We show how this behavior emerges from the microscopic properties of the closed quantum system. In contrast to the one-dimensional case, our transport measurements for two-dimensional Heisenberg systems indicate anomalous superdiffusion. C1 [Hild, Sebastian; Fukuhara, Takeshi; Schauss, Peter; Zeiher, Johannes; Bloch, Immanuel; Gross, Christian] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Knap, Michael; Demler, Eugene] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Bloch, Immanuel] Univ Munich, Fak Phys, D-80799 Munich, Germany. RP Hild, S (reprint author), Max Planck Inst Quantum Opt, D-85748 Garching, Germany. EM shild@mpq.mpg.de RI Gross, Christian/P-5475-2014; Fukuhara, Takeshi/A-6254-2014; Bloch, Immanuel/G-3174-2010; Knap, Michael/H-3344-2011; OI Gross, Christian/0000-0003-2292-5234; Fukuhara, Takeshi/0000-0002-6702-9882; Bloch, Immanuel/0000-0002-0679-4759; Knap, Michael/0000-0002-7093-9502; Schauss, Peter/0000-0002-8505-5195 FU MPG; EU (UQUAM); Harvard-MITCUA; ARO-MURI Quism program; RO-MURI on Atomtronics; Austrian Science Fund (FWF) [J 3361-N20] FX We thank I. Affleck, M. Cheneau, T. Giamarchi, F. Heidrich-Meissner, A. Lauchli, M. Lukin, and J. Thywissen for valuable discussions. The authors acknowledge support from MPG, EU (UQUAM), Harvard-MITCUA, ARO-MURI Quism program, and ARO-MURI on Atomtronics, as well as the Austrian Science Fund (FWF) Project No. J 3361-N20. NR 54 TC 45 Z9 45 U1 2 U2 14 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 3 PY 2014 VL 113 IS 14 AR 147205 DI 10.1103/PhysRevLett.113.147205 PG 5 WC Physics, Multidisciplinary SC Physics GA AS1HI UT WOS:000344031200010 PM 25325657 ER PT J AU Serbyn, M Knap, M Gopalakrishnan, S Papic, Z Yao, NY Laumann, CR Abanin, DA Lukin, MD Demler, EA AF Serbyn, M. Knap, M. Gopalakrishnan, S. Papic, Z. Yao, N. Y. Laumann, C. R. Abanin, D. A. Lukin, M. D. Demler, E. A. TI Interferometric Probes of Many-Body Localization SO PHYSICAL REVIEW LETTERS LA English DT Article ID POLAR-MOLECULES; SPIN-ECHO; RESONANCE; INSULATOR; LATTICE AB We propose a method for detecting many-body localization (MBL) in disordered spin systems. The method involves pulsed coherent spin manipulations that probe the dephasing of a given spin due to its entanglement with a set of distant spins. It allows one to distinguish the MBL phase from a noninteracting localized phase and a delocalized phase. In particular, we show that for a properly chosen pulse sequence the MBL phase exhibits a characteristic power-lawdecay reflecting its slow growth of entanglement. We find that this power-lawdecay is robust with respect to thermal and disorder averaging, provide numerical simulations supporting our results, and discuss possible experimental realizations in solid-state and cold-atom systems. C1 [Serbyn, M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Knap, M.; Gopalakrishnan, S.; Yao, N. Y.; Laumann, C. R.; Lukin, M. D.; Demler, E. A.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Papic, Z.; Laumann, C. R.; Abanin, D. A.] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Papic, Z.; Abanin, D. A.] Inst Quantum Comp, Waterloo, ON N2L 3G1, Canada. [Laumann, C. R.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. RP Serbyn, M (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. RI Knap, Michael/H-3344-2011; Papic, Zlatko/K-6714-2013 OI Knap, Michael/0000-0002-7093-9502; FU Austrian Science Fund (FWF) [J 3361-N20]; NSERC grant; Sloan Research Fellowship; High Performance Computing Center (PICSciE) at Princeton University; Government of Canada; Province of Ontario; Harvard Quantum Optics Center; Harvard-MIT CUA; DARPA OLE program; AFOSR Quantum Simulation MURI; ARO-MURI on Atomtronics; ARO-MURI Quism program FX We thank E. Altman, Y. Bahri, I. Bloch, T. Giamarchi, D. Huse, V. Oganesyan, A. Pal, D. Pekker, and G. Refael for insightful discussions. The authors acknowledge support from the Harvard Quantum Optics Center, Harvard-MIT CUA, the DARPA OLE program, AFOSR Quantum Simulation MURI, ARO-MURI on Atomtronics, the ARO-MURI Quism program, the Austrian Science Fund (FWF) Project No. J 3361-N20, NSERC grant, and Sloan Research Fellowship. Simulations presented in this article were performed on computational resources supported by the High Performance Computing Center (PICSciE) at Princeton University and the Research Computing Center at Harvard University. Research at Perimeter Institute was supported by the Government of Canada and by the Province of Ontario. NR 42 TC 58 Z9 58 U1 3 U2 19 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD OCT 3 PY 2014 VL 113 IS 14 AR 147204 DI 10.1103/PhysRevLett.113.147204 PG 5 WC Physics, Multidisciplinary SC Physics GA AS1HI UT WOS:000344031200009 PM 25325656 ER PT J AU Collins, M AF Collins, Martin TI Untitled SO HISTORY AND TECHNOLOGY LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Collins, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM CollinsM@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0734-1512 EI 1477-2620 J9 HIST TECHNOL JI Hist. Technol. PD OCT 2 PY 2014 VL 30 IS 4 BP 281 EP 282 DI 10.1080/07341512.2015.1011300 PG 2 WC History SC History GA CE3QJ UT WOS:000351742900001 ER PT J AU Todaro, MA Leasi, F Hochberg, R AF Todaro, M. Antonio Leasi, Francesca Hochberg, Rick TI A new species, genus and family of marine Gastrotricha from Jamaica, with a phylogenetic analysis of Macrodasyida based on molecular data SO SYSTEMATICS AND BIODIVERSITY LA English DT Article DE biodiversity; benthos; Caribbean Sea; meiofauna; phylogeny; taxonomy ID RIBOSOMAL-RNA GENES; THAUMASTODERMATIDAE GASTROTRICHA; PAUCITUBULATINA GASTROTRICHA; REPRODUCTIVE-SYSTEM; MEDITERRANEAN SEA; SOUTH-AFRICA; CHAETONOTIDA; MORPHOLOGY; FRESH; INTERRELATIONSHIPS AB Gastrotricha is a phylum of aquatic microinvertebrates counting about 850 species divided into the two orders Chaetonotida and Macrodasyida. Currently, Chaetonotida includes 8 families and 31 genera while Macrodasyida includes 9 families and 32 genera; however, systematics is in a state of flux due to phylogenetic incongruences of the classical systematization. The process of re-systematization will benefit from additional surveys of insufficiently known taxa and especially from the discovery of new species bearing novel characteristics that could help to recognize plesiomorphy in these morphologically diverse animals. Herein, a new and interesting macrodasyidan species from the northwestern shore of Jamaica is described. Specimens up to 1170m in length have: a vermiform body with numerous epidermal glands; naked cuticle; head weakly demarked; posterior end in the form of two caudal pedicles; TbA, arranged in two diagonal rows, inserting directly on the cuticle; TbL/TbVL scarce; TbD and TbV absent; TbP at the tip of each caudal pedicle and along its inner margins; mid-sized terminal mouth; pharynx with pores at the base; PhIJ at U20; intestine rectilinear, anus ventral; hermaphroditic sexual apparatus; gonads paired: female anterior, male posterior; gametes maturing in a caudo-cephalic direction; spermatozoa relatively short, with spiralled head and spiralled tail; sperm ducts directed posteriorly, converging ventrally on the midline and joining the sac-like caudal organ; and frontal organ, dorsal to the intestine, not obviously muscularized. External morphology and layout of the reproductive system appear so unique among Gastrotricha to grant the establishment of a new taxon, for which the name Hummondasys jamaicensis gen. et sp. nov. is proposed. Furthermore, to allocate the new genus, the creation of the new family Hummondasyidae is proposed based both on the morphological peculiarities and results of phylogenetic analyses based on the 18S rRNA gene, which involved all of the relevant macrodasyidan taxa.http://zoobank.org/urn:lsid:zoobank.org:pub:595575EA-5ADF-4D0C-AD8B-8BC87E3D3905 C1 [Todaro, M. Antonio] Univ Modena & Reggio Emilia, Dept Life Sci, Modena, Italy. [Leasi, Francesca] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Hochberg, Rick] Univ Massachusetts, Lowell, MA 01854 USA. RP Todaro, MA (reprint author), Univ Modena & Reggio Emilia, Dept Life Sci, Modena, Italy. EM antonio.todaro@unimore.it RI Todaro, M. Antonio/H-1311-2013; LEASI, FRANCESCA/E-4361-2017 OI Todaro, M. Antonio/0000-0002-6353-7281; FU US-National Science Foundation [DEB 0918499]; UNIMORE (TIOME project) FX This work was mainly supported by a grant from the US-National Science Foundation [n. DEB 0918499] to R. Hochberg; additional funding was provided by UNIMORE (TIOME project) to M. A. Todaro. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 57 TC 7 Z9 8 U1 2 U2 12 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1477-2000 EI 1478-0933 J9 SYST BIODIVERS JI Syst. Biodivers. PD OCT 2 PY 2014 VL 12 IS 4 BP 473 EP 488 DI 10.1080/14772000.2014.942718 PG 16 WC Biodiversity Conservation; Biology SC Biodiversity & Conservation; Life Sciences & Biomedicine - Other Topics GA AR0DC UT WOS:000343235600008 ER PT J AU Kidwell, PA AF Kidwell, Peggy Aldrich TI Mathematics and Logic SO ANNALS OF SCIENCE LA English DT Book Review C1 [Kidwell, Peggy Aldrich] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Kidwell, PA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, 1400 Constitut Ave Northwest, Washington, DC 20560 USA. EM kidwellp@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0003-3790 EI 1464-505X J9 ANN SCI JI Ann. Sci. PD OCT 2 PY 2014 VL 71 IS 4 BP 595 EP 597 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA AQ5BG UT WOS:000342816800015 ER PT J AU Tavares, VD Gardner, AL Ramirez-Chaves, HE Velazco, PM AF Tavares, Valeria Da C. Gardner, Alfred L. Ramirez-Chaves, Hector E. Velazco, Paul M. TI Systematics of Vampyressa melissa Thomas, 1926 (Chiroptera: Phyllostomidae), with descriptions of two new species of Vampyressa SO AMERICAN MUSEUM NOVITATES LA English DT Article ID BATS; STENODERMATINAE AB Vampyressa melissa is a poorly known phyllostomid bat listed as vulnerable by the International Union for Conservation of Nature (IUCN). Since its description in 1926, fewer than 40 V melissa have been reported in the literature, and less than half of these may have been correctly identified. During revisionary studies of Vampyressa, we uncovered two previously unrecognized species related to V melissa, all associated with higher elevation habitats (>1400 m), one from the Andes of Colombia (Vampyressa sinchi, new species) and the other from western Panama (Vampyressa elisabethae, new species) revealing that V melissa, as traditionally defined, is a composite of at least three species. In this paper, we provide a restricted diagnosis for the genus Vampyressa, an emended diagnosis of V melissa, and descriptions of the two new species. The separation of these frugivorous bats, previously identified as V melissa, into three isolated upper-elevation species, each having restricted distributions further highlights their fragile conservation status. C1 [Tavares, Valeria Da C.] INPA, Manaus, Amazonas, Brazil. [Tavares, Valeria Da C.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. [Tavares, Valeria Da C.] CUNY, Grad Ctr, New York, NY USA. [Gardner, Alfred L.] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist MRC 111, Washington, DC 20560 USA. [Ramirez-Chaves, Hector E.] Univ Queensland, Sch Biol Sci, Weisbecker Lab, Brisbane, Qld, Australia. [Velazco, Paul M.] Amer Museum Nat Hist, Dept Vertebrate Paleontol, New York, NY 10024 USA. RP Tavares, VD (reprint author), INPA, Manaus, Amazonas, Brazil. RI Ramirez Chaves, Hector Emilio/B-2909-2016; Velazco, Paul/K-4186-2012 OI Ramirez Chaves, Hector Emilio/0000-0002-2454-9482; Velazco, Paul/0000-0001-7195-7422 FU NASA [NAG5-12333, NAG5-8543]; New York Community Trust; Center for Biodiversity and Conservation at the American Museum of Natural History; CAPES; FAPEAM FX This work was part of V.C.T.'s doctoral studies at City University of New York in a joint program with the American Museum of Natural History; V.C.T. is grateful to the committee members N. Simmons, C. Raxworthy, J. Wahlert, R. Rockwell, and R. Voss; special thanks to N. Simmons for her careful review of an earlier draft of this paper. The following curators and collection staff kindly permitted access to specimens under their care: R. Jenkins and P. Jenkins (BMNH); E.M. Versute (DZSJRP); B.D. Patterson (FMNH); J.E. Castillo (IAvH); H. Lopez Arevalo and Y. Munoz-Saba (ICN); R.M. Timm (KU); M. Rivas Pava (MHNUC); L. Albuja and J. Regalado (MPEN); V. Pacheco (MUSM); J.L. Patton (MVZ); M. de Vivo (MZUSP); L. Gordon (USNM); O.M. Garcia (UV), B. Lim and M. Engstrom (ROM), R.J. Baker (TTU), and P. Myers (UMMZ). We are grateful to Ofelia Mejia-Egas for allowing us to use her photograph of a live individual of Vampyressa sinchi. This material is based upon work supported by the NASA under awards NAG5-12333 and NAG5-8543, the New York Community Trust, S. Donnelley, and the Center for Biodiversity and Conservation at the American Museum of Natural History to V.C.T.; V.C.T. also thanks CAPES and FAPEAM postdoctoral fellowship under the program PRO-DPD/AM-PPGSS. To those people and institutions we express our sincere thanks. We also are grateful to T. Chesser, USGS-PWRC, Biological Survey Unit, National Museum of Natural History; B.D. Patterson, Field Museum of Natural History; one anonymous reviewer; and to R.S. Voss for their comments and recommendation. Any mention of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the United States government. NR 39 TC 2 Z9 2 U1 1 U2 8 PU AMER MUSEUM NATURAL HISTORY PI NEW YORK PA ATTN: LIBRARY-SCIENTIFIC PUBLICATIONS DISTRIBUTION, CENTRAL PK WEST AT 79TH ST, NEW YORK, NY 10024-5192 USA SN 0003-0082 EI 1937-352X J9 AM MUS NOVIT JI Am. Mus. Novit. PD OCT 2 PY 2014 IS 3813 BP 1 EP 27 PG 27 WC Biodiversity Conservation; Zoology SC Biodiversity & Conservation; Zoology GA AQ2KC UT WOS:000342613200001 ER PT J AU Lee, TE Chan, CK AF Lee, Tony E. Chan, Ching-Kit TI Heralded Magnetism in Non-Hermitian Atomic Systems SO PHYSICAL REVIEW X LA English DT Article ID QUANTUM OPTICS; ENTANGLEMENT; MODEL; TRANSITIONS; EXCITATION; MECHANICS; ENSEMBLES; DYNAMICS; DISTANCE AB Quantum phase transitions are usually studied in terms of Hermitian Hamiltonians. However, cold-atom experiments are intrinsically non-Hermitian because of spontaneous decay. Here, we show that non-Hermitian systems exhibit quantum phase transitions that are beyond the paradigm of Hermitian physics. We consider the non-Hermitian XY model, which can be implemented using three-level atoms with spontaneous decay. We exactly solve the model in one dimension and show that there is a quantum phase transition from short-range order to quasi-long-range order despite the absence of a continuous symmetry in the Hamiltonian. The ordered phase has a frustrated spin pattern. The critical exponent nu can be 1 or 1/2. Our results can be seen experimentally with trapped ions, cavity QED, and atoms in optical lattices. C1 [Lee, Tony E.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Lee, TE (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. FU NSF; Croucher Foundation FX We thank S. Sachdev, G. Refael, N. Moiseyev, S. Gopalakrishnan, and M. Foss-Feig for useful discussions. This work was supported by the NSF through a grant to ITAMP. C. K. C. is supported by the Croucher Foundation. NR 63 TC 19 Z9 19 U1 3 U2 17 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2160-3308 J9 PHYS REV X JI Phys. Rev. X PD OCT 2 PY 2014 VL 4 IS 4 AR 041001 DI 10.1103/PhysRevX.4.041001 PG 13 WC Physics, Multidisciplinary SC Physics GA AQ2TE UT WOS:000342641100001 ER PT J AU Vari, RP Calegari, BB AF Vari, Richard P. Calegari, Barbara B. TI New species of the catfish genus Tatia (Siluriformes: Auchenipteridae) from the rio Teles Pires, upper rio Tapajos basin, Brazil SO NEOTROPICAL ICHTHYOLOGY LA English DT Article DE Amazon basin; Centromochlinae; Endemism; Neotropical region; Taxonomy ID OSTARIOPHYSI; STATE AB Analysis of specimens of the auchenipterid catfish genus Tatia collected in the rio Teles Pires, a tributary of the rio Tapajcs, along the border between the states of Para and Mato Grosso, Brazil, revealed it to be an undescribed species. This new species is distinguished from all congeners with the exception of T. carolae and T. musaica by the intense, clearly demarcated, dark coloration on the dorsal and to varying degrees lateral and sometimes ventrolateral portions of the body versus the very lightly colored regions which are translucent in life on the remainder of the body. Various details of head, body and dorsal and caudal-fin pigmentation along with meristic and morphometric features distinguish the new species from T. carolae and T. musaica. The new species provides further evidence that the upper and middle rio Tapajos is a region of ichthyofaunal endemism. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Calegari, Barbara B.] Pontificia Univ Catolica Rio Grande do Sul, Lab Sistemat Vertebrados, BR-90619900 Porto Alegre, RS, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM varir@si.edu; barbara.calegari@gmail.com FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [140439/2011-0]; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) [3918/13-0] FX We are grateful to Fernando Jerep (MZUEL) for suggestions as to the improvement of the paper; Heriberto Gimenes Junior for the photographs of live specimens and information about their habitat; Sandra Raredon (USNM) for the photographs of the holotype and assistance with radiography; Jeffrey Clayton (UNSM) for assistance; and to Scott Schaefer and Barbara Brown (AMNH), Mark Sabaj Perez (ANSP), David Catania (CAS), Lucia R. Py-Daniel (INPA), Christine Thacker and Rick Feeney (LACM), Claudio Oliveira (LBP), Carlos A. S. Lucena (MCP), Paulo Buckup and Marcelo Britto (MNRJ), Osvaldo Oyakawa, Jose Lima de Figueiredo, and Michel Gianeti (MZUSP), Hernan Lopez-Fernandes (ROM), Willian Ohara, Luiz J. de Queiroz and Christian Cramer (UFRO) for the loan of specimens. Support for this project was provided by the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, process # 140439/2011-0), the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, process # 3918/13-0) which funded a visit to the Smithsonian Institution by BBC, and by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution to RPV. NR 11 TC 6 Z9 6 U1 3 U2 12 PU SOC BRASILEIRA ICTIOLOGIA PI SAO PAULO PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO PAULO, SP 05508-900, BRAZIL SN 1679-6225 J9 NEOTROP ICHTHYOL JI Neotrop. Ichthyol. PD OCT-DEC PY 2014 VL 12 IS 4 BP 667 EP 674 DI 10.1590/1982-0224-20130193 PG 8 WC Zoology SC Zoology GA AZ0AU UT WOS:000347909800001 ER PT J AU Calegari, BB Reis, RE Vari, RP AF Calegari, Barbara B. Reis, Roberto E. Vari, Richard P. TI Miniature catfishes of the genus Gelanoglanis (Siluriformes: Auchenipteridae): monophyly and the description of a new species from the upper rio Tapajos basin, Brazil SO NEOTROPICAL ICHTHYOLOGY LA English DT Article DE Amazon; Biodiversity; Endemism; Neotropics; Systematics ID AMAZON BASIN AB Previously proposed synapomorphies for the genus Gelanoglanis of the catfish family Auchenipteridae are evaluated and four additional features involving the relationship between the mesethmoid and premaxilla, the very fleshy anterior portion of the snout, the lack of ossification of the second through fourth infraorbitals, and the incomplete poring of the lateral line are hypothesized as synapomorphic for the members of the genus. A new species of Gelanoglanis is described based on a series of specimens collected in the rio Teles Pires, a tributary of the rio Tapajos in the southern reaches of the Amazon basin. The new species demonstrates a number of features unusual within Gelanoglanis including a fontanel bordered by the frontals, a particularly elongate gonopodium in mature males, reductions in the dentition on the premaxilla, and a shorter posterior extension of the maxilla inside the maxillary barbel. The new species is a miniature as evidenced both by its body size and the reductions of various ossifications of the head, the number of fin rays and of the laterosensory canal system on the head and body. C1 [Calegari, Barbara B.; Reis, Roberto E.] Pontificia Univ Catolica Rio Grande do Sul, Lab Sistemat Vertebrados, BR-90619900 Porto Alegre, RS, Brazil. [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Calegari, BB (reprint author), Pontificia Univ Catolica Rio Grande do Sul, Lab Sistemat Vertebrados, Av Ipiranga 6681, BR-90619900 Porto Alegre, RS, Brazil. EM barbara.calegari@gmail.com; reis@pucrs.br; varir@si.edu RI Reis, Roberto/A-7030-2012 OI Reis, Roberto/0000-0003-3746-6894 FU Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [140439/2011-0, 305180/2010-0, 207038/2013-9]; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) [3918/13-0]; Fundacao de Amparo a Pesquisa do Estado Rio Grande do Sul (FAPERGS) [11/0936-5] FX We are grateful to Fernando Jerep for discussions about characters; Flavio Lima and Paulo Petry for information on various species of Gelanoglanis; Tiago Carvalho and Mariangeles Arce (ANSP) for providing information on species of Gelanoglanis; Zeehan Jaafar to assistance with stereomicroscopic photography to comparative studies; Sandra Raredon (USNM) for the photographs and radiographs of the holotype; G. David Johnson for the photograph of the cleared and stained specimen, Jeffrey Clayton for assistance with loans at USNM; and Mark Sabaj Perez (ANSP), David Catania (CAS), Christine Thacker and Rick Feeney (LACM), Mario de Pinna, Osvaldo Oyakawa, Jose Lima de Figueiredo, and Michel Gianeti (MZUSP), and Larry Page and Rob Robins (UF) for the loan and/or donation of specimens. RER thanks William Crampton for support at the University of Central Florida, where this manuscript was partially completed during a sabbatical semester. Support for this project was provided by the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq, process #140439/2011-0) and Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, process #3918/13-0) to BBC; CNPq (processes #305180/2010-0 and #207038/2013-9) and Fundacao de Amparo a Pesquisa do Estado Rio Grande do Sul (FAPERGS, process #11/0936-5) to RER; and the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution to RPV. NR 15 TC 1 Z9 1 U1 4 U2 5 PU SOC BRASILEIRA ICTIOLOGIA PI SAO PAULO PA UNIV SAO PAULO, DEPT FISIOLOGIA-IB, RUA DO MATAO, TRAVESSA 14 N 321, SAO PAULO, SP 05508-900, BRAZIL SN 1679-6225 J9 NEOTROP ICHTHYOL JI Neotrop. Ichthyol. PD OCT-DEC PY 2014 VL 12 IS 4 BP 699 EP 706 DI 10.1590/1982-0224-20130233 PG 8 WC Zoology SC Zoology GA AZ0AU UT WOS:000347909800004 ER PT J AU West-Eberhard, MJ AF Jane West-Eberhard, Mary TI Darwin's forgotten idea: The social essence of sexual selection SO NEUROSCIENCE AND BIOBEHAVIORAL REVIEWS LA English DT Review DE Social selection; Sexual conflict; Good genes; Sensory bias; Female choice; Evolution of communication; Threat behavior; Sensory systems; Evolution of complexity ID ANTAGONISTIC COEVOLUTION; EVOLUTION; COMPETITION; CONSEQUENCES; CONFLICT; INSECTS; CHOICE; DIVERGENCE; SPECIATION; MAMMALS AB Darwinian sexual selection can now be seen in the broader context of social selection, or social competition for resources (under sexual selection, mates or fertilization success). The social-interaction aspects of sexually selected traits give them special evolutionary properties of interest for neurobiological studies of stimulus-response systems because they can account for highly complex systems with little information content other than stimulatory effectiveness per se. But these special properties have a long history of being forgotten when other factors dominate the analysis of male-female interactions, such as the mistaken belief that differential responsiveness to signals produced by competing rivals ("female choice") requires an esthetic sense; that species recognition explains all species-specific sexual signals; and, more recently, that successful signals must reflect good survival genes; or that male-female conflict involves female resistance rather than stimulus evaluation. A "conflict paradox" results when male-female conflict is seen as driven by natural selection, whose costs should often move the hypothesized "sexually antagonistic co-evolution" of sensory-response systems toward the powerful domain of sexually synergistic co-evolution under sexual selection. Special properties of sexual selection apply to other forms of social competition as well, showing the wisdom of Darwin's setting it apart from natural selection as an explanation of many otherwise puzzling and extreme traits. (C) 2014 Published by Elsevier Ltd. C1 [Jane West-Eberhard, Mary] Louisiana State Univ, Dept Biol Sci, Smithsonian Trop Res Inst, Baton Rouge, LA 70803 USA. [Jane West-Eberhard, Mary] Univ Costa Rica, Escuela Biol, Museum Nat Sci, Facio Brenes, Costa Rica. RP West-Eberhard, MJ (reprint author), Louisiana State Univ, Dept Biol Sci, Smithsonian Trop Res Inst, Baton Rouge, LA 70803 USA. EM mjwe@sent.com NR 67 TC 20 Z9 21 U1 14 U2 82 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0149-7634 EI 1873-7528 J9 NEUROSCI BIOBEHAV R JI Neurosci. Biobehav. Rev. PD OCT PY 2014 VL 46 SI SI BP 501 EP 508 DI 10.1016/j.neubiorev.2014.06.015 PN 4 PG 8 WC Behavioral Sciences; Neurosciences SC Behavioral Sciences; Neurosciences & Neurology GA AZ1QJ UT WOS:000348012800002 PM 25003806 ER PT J AU Boogert, NJ Farine, DR Spencer, KA AF Boogert, Neeltje J. Farine, Damien R. Spencer, Karen A. TI Developmental stress predicts social network position SO BIOLOGY LETTERS LA English DT Article DE corticosterone; development; foraging; social network; stress; zebra finch ID TITS PARUS-MAJOR; CORTICOSTERONE; BEHAVIOR; POPULATION; SONGBIRDS AB The quantity and quality of social relationships, as captured by social network analysis, can have major fitness consequences. Various studies have shown that individual differences in social behaviour can be due to variation in exposure to developmental stress. However, whether these developmental differences translate to consistent differences in social network position is not known. We experimentally increased levels of the avian stress hormone corticosterone (CORT) in nestling zebra finches in a fully balanced design. Upon reaching nutritional independence, we released chicks and their families into two free-flying rooms, where we measured daily social networks over five weeks using passive integrated transponder tags. Developmental stress had a significant effect on social behaviour: despite having similar foraging patterns, CORT chicks had weaker associations to their parents than control chicks. Instead, CORT chicks foraged with a greater number of flock mates and were less choosy with whom they foraged, resulting in more central network positions. These findings highlight the importance of taking developmental history into account to understand the drivers of social organization in gregarious species. C1 [Boogert, Neeltje J.; Spencer, Karen A.] Univ St Andrews, Sch Psychol & Neurosci, St Andrews KY16 9JP, Fife, Scotland. [Farine, Damien R.] Univ Oxford, 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, Ancon, Panama. RP Boogert, NJ (reprint author), Univ St Andrews, Sch Psychol & Neurosci, St Andrews KY16 9JP, Fife, Scotland. EM nb40@st-andrews.ac.uk RI Spencer, Karen/B-3177-2015; OI Spencer, Karen/0000-0002-2851-9379; Farine, Damien/0000-0003-2208-7613 FU Netherlands Organisation for Scientific Research Rubicon; NSF [NSF-IOS1250895]; BBSRC [BB/L006081/1]; BBSRC David Phillips Research Fellowship FX N.J.B. was funded by a Netherlands Organisation for Scientific Research Rubicon grant and D.R.F. was funded by grants from 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. NR 24 TC 20 Z9 20 U1 0 U2 34 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 OCT 1 PY 2014 VL 10 IS 10 AR UNSP 20140561 DI 10.1098/rsbl.2014.0561 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AZ2EB UT WOS:000348046300001 PM 25354917 ER PT J AU Gagne, RJ Graney, L AF Gagne, Raymond J. Graney, Lorraine TI PICEACECIS (DIPTERA: CECIDOMYLIDAE), A NEW GENUS FOR A NON-NATIVE PEST OF NORWAY SPRUCE FROM EUROPE AND ITS NORTH AMERICAN RELATIVE SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Picea; Holarctic; Lasiopteridi; synonymy; new combinations AB Dasineura abietiperda (Henschel), a European pest of Norway spruce, Picea abies (Pinaceae), is reported as new to northeastern North America where the tree is widely planted and valued as an ornamental. Adult gall midges emerge in early spring, mate and deposit eggs on twigs or new shoots. The larvae burrow into tissue causing swellings to form under bud scales and less frequently along shoots or near the terminal bud. Larvae overwinter in the galls. Field symptoms include bent twigs or shoots, swellings in nodes and needle drop. A new genus, Piceacecis Gagne is described to include D. abietiperda and its North American relative, Phytophaga tsugae (Felt), which occurs on native American white spruce, Picea glauca. Both cecidomyiids are redescribed with illustrations. The names of both are new combinations in Piceacecis, and Phytophaga piceae Felt is a new junior synonym of Piceacecis tsugae. In the past these synonyms have been combined also with Mayetiola. C1 [Gagne, Raymond J.] USDA ARS, PSI, Systemat Entomol Lab, Washington, DC 20013 USA. [Graney, Lorraine] Bartlett Tree Res Lab, Charlotte, NC 28278 USA. RP Gagne, RJ (reprint author), USDA ARS, PSI, Systemat Entomol Lab, Smithsonian Inst MRC 168,POB 37012, Washington, DC 20013 USA. EM raymond.gagne@ars.usda.gov; lgraney@bartlett.com NR 30 TC 1 Z9 3 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2014 VL 116 IS 4 BP 378 EP 393 DI 10.4289/0013-8797.116.4.378 PG 16 WC Entomology SC Entomology GA AX4HM UT WOS:000346894100002 ER PT J AU Woodley, NE AF Woodley, Norman E. TI TWO NEW SPECIES OF BRACHYODINA LINDNER FROM THE CARIBBEAN WITH A KEY TO SPECIES OF THE GENUS FROM THE REGION (DIPTERA: STRATIOMYIDAE: PACHYGASTRINAE) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE description; taxonomy; Neotropical Region; West Indies; Hispaniola; Cayman Islands AB Two new species of Brachyodina Lindner from the Caribbean are described, B. janestanleyae Wood ley, new species, from the Dominican Republic and B. caymanensis Wood ley, new species from Grand Cayman Island. A key to the species known from the Caribbean islands is provided. C1 USDA ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, Washington, DC 20013 USA. RP Woodley, NE (reprint author), USDA ARS, Systemat Entomol Lab, Beltsville Agr Res Ctr, Smithsonian Inst,NHB-168,POB 37012, Washington, DC 20013 USA. EM norman.woodley@ars.usda.gov NR 7 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 OCT PY 2014 VL 116 IS 4 BP 429 EP 440 DI 10.4289/0013-8797.116.4.429 PG 12 WC Entomology SC Entomology GA AX4HM UT WOS:000346894100007 ER PT J AU Johnson, JA AF Johnson, John A. TI Energetic flares in the search for habitable exoplanets Replay SO PHYSICS TODAY LA English DT Letter C1 Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Johnson, JA (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM jjohnson@cfa.harvard.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD OCT PY 2014 VL 67 IS 10 BP 11 EP 11 PG 1 WC Physics, Multidisciplinary SC Physics GA AW2MF UT WOS:000346121600010 ER PT J AU Childress, L Walsworth, R Lukin, M AF Childress, Lilian Walsworth, Ronald Lukin, Mikhail TI Atom-like crystal defects: From quantum computers to biological sensors SO PHYSICS TODAY LA English DT Article ID NANOSCALE RESOLUTION; MECHANICAL RESONATOR; MAGNETIC-RESONANCE; DIAMOND; SPIN; MICROSCOPY; CENTERS; QUBITS C1 [Childress, Lilian] McGill Univ, Montreal, PQ H3A 2T5, Canada. [Walsworth, Ronald; Lukin, Mikhail] Harvard Univ, Cambridge, MA 02138 USA. [Walsworth, Ronald] Smithsonian Astrophys Observ, Cambridge, MA USA. RP Childress, L (reprint author), McGill Univ, Montreal, PQ H3A 2T5, Canada. RI Childress, Lilian/H-1359-2012 OI Childress, Lilian/0000-0002-0507-6392 FU NSF; CUA; DARPA; NIST; AFOSR; ARO; CFI; NSERC; FRQNT; Moore Foundation FX We thank NSF, CUA, DARPA, NIST, AFOSR, ARO, CFI, NSERC, FRQNT, and Moore Foundation for supporting this work. NR 21 TC 20 Z9 20 U1 0 U2 34 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 EI 1945-0699 J9 PHYS TODAY JI Phys. Today PD OCT PY 2014 VL 67 IS 10 BP 38 EP 43 PG 6 WC Physics, Multidisciplinary SC Physics GA AW2MF UT WOS:000346121600020 ER PT J AU Phillips, AJ Georgiev, BB Waesehenbach, A Mariaux, J AF Phillips, Anna J. Georgiev, Boyko B. Waesehenbach, Andrea Mariaux, Jean TI Two new and two redescribed species of Anonchotaenia (Cestoda: Paruterinidae) from South American birds SO FOLIA PARASITOLOGICA LA English DT Article DE Anonchotaenia prolixa; Anonchotaenia vaslata; Anonchotaenia brasiliensis; Anonchotaenia macrocephala; new species; new host record; Brazil; Chile; Paraguay; new geographical record ID IVORY-COAST; CYCLOPHYLLIDEA; GENUS; MICROTRICHES; INVALIDATION; SYSTEMATICS; FOREST; BRAZIL AB Morphological examination of novel specimens of paruterinid cestodes from passerine birds from Brazil and Chile and of museum specimens from Paraguay revealed two new species: Anonchotaenia prolixa sp. n. from Elaenia albiceps chilensis Hellmayr from Chile, and Anonchotaenia vaslata sp. n. from Tyrannus melancholicus (Vieillot) (type host) and Myiodynastes maculatus (Statius Muller) from Paraguay. The generic diagnosis of Anonchotaenia Conn, 1900 is amended, prompted by the presence of the armed cirrus and the elongated cirrus sac of A. prolixa. Two species were redescribed: Anonchotaenia brasiliensis Fuhrmann, 1908 from Tachyphonus coronatus (Vieillot) and Thraupis cyanoptera (Vieillot) (new host records) from Brazil, and Thraupis sayaca (Linnaeus) and Volatinia jacarina (Linnaeus) from Paraguay (new host and geographic records); and Anonchotaenia macrocephala Fuhrmann, 1908 from Tachycineta leucorrhoa (Vieillot) (new host record) from Brazil, Tachycineta meyeni (Cabanis) from Chile (new host and geographic record) and Stelgidopteryx ruficollis (Vieillot) from Paraguay (new host and geographic record). Scanning electron microscopy of A. brasiliensis and A. macrocephala revealed less microthrix variation than has been reported for other cyclophyllidean taxa. Sequence data were generated for nuclear ssr- and lsr-DNA and mitochondrial rrnL and cox1 for A. prolixa, A. brasiliensis, and A. macrocephala. Maximum likelihood and Bayesian inference analyses supported each species as distinct, but revealed cryptic diversity among A. brasiliensis specimens from different host families. New host records of A. brasiliensis and A. macrocephala prompted a formal assessment of host specificity. Anonchotaenia prolbca was found to be oioxenous (HSs = 0), A. vaslata and A. macrocephala were found to be metastenoxenous (HSs = 3.000 and 3.302, respectively), whereas A. brasiliensis was found to be euryxenous (HSs = 5.876). Anonchotaenia brasiliensis has been found parasitising several species of different passerine families that participate in mixed-species foraging flocks in the Atlantic Forest. A diversity of species of other families join these flocks and are among the substantial number of South American passerine species yet to be examined for cestodes. C1 [Phillips, Anna J.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT USA. [Georgiev, Boyko B.] Bulgarian Acad Sci, Inst Biodivers & Ecosyst Res, Sofia, Bulgaria. [Waesehenbach, Andrea] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. [Mariaux, Jean] Museum Hist Nat, CH-1211 Geneva, Switzerland. [Mariaux, Jean] Univ Geneva, Dept Genet & Evolut, Geneva, Switzerland. RP Phillips, AJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM phillipsaj@si.edu FU National Science Foundation, PHI [0818696, 0818823] FX We thank Fernando Marques for his help in organising fieldwork and permits for our work in Brazil and Natalia Da Mata Luchetti (both from Laboratorie Helmintologia Evolutiva - Universidad de Sao Paulo) for her effort in organising our fieldwork and for being a valuable member of our team. We are thankful for the ornithological expertise of Luis Fabio Silveira, Luciano Moreira Lima, Deborah Oliveira, Rafael Sobral Marcondes (all MZUSP), Guilherme Renzo Rocha Brito, Marco Aurelio Crozariol and Daniel Honorato Firme (all Museu Nacional, UFRJ). Fieldwork in Chile was possible with the support of the staff of the Huinay Scientific Field Station (HSFS), especially Gunter Fosterra and Vreni Hausserman. We thank the staff of the sequencing facility at the Natural History Museum in London for their sequencing expertise. We are thankful to Janine Caira (University of Connecticut) for her thoughtful comments and insights that greatly improved this manuscript, and to Kent Holsinger (University of Connecticut) for his assistance with the analyses of host specificity. Elizabeth Barbeau (University of Connecticut) and Freya Goetz (Smithsonian's National Museum of Natural History) provided valuable advice and assistance with the figures. This work was funded by the National Science Foundation, PHI grants 0818696 and 0818823. This paper is publication number 87 of the HSFS. NR 49 TC 0 Z9 0 U1 1 U2 5 PU FOLIA PARASITOLOGICA PI CESKE BUDEJOVICE PA BRANISOVSKA 31,, CESKE BUDEJOVICE 370 05, CZECH REPUBLIC SN 0015-5683 EI 1803-6465 J9 FOLIA PARASIT JI Folia Parasitol. PD OCT PY 2014 VL 61 IS 5 BP 441 EP 461 PG 21 WC Parasitology SC Parasitology GA AU6QK UT WOS:000345726900006 PM 25549500 ER PT J AU Altieri, AH Witman, JD AF Altieri, Andrew H. Witman, Jon D. TI Modular mobile foundation species as reservoirs of biodiversity SO ECOSPHERE LA English DT Article DE biodiversity; ecosystems engineer; epifauna; Eucidaris galapagensis; fouling community; foundation species; Galapagos; predation refuge ID GALAPAGOS MARINE RESERVE; COMMUNITY; REEF; ECOSYSTEMS; INVERTEBRATES; CONSEQUENCES; CONSERVATION; FACILITATION; EXTINCTION; DIVERSITY AB The complex structure of biogenic habitats including coral reefs, hemlock forests, and seagrass meadows are widely recognized for the diverse communities they shelter. As human impacts accelerate the loss of such foundation species, we need to identify the general characteristics of previously unrecognized species that can also fulfill the role of habitat provider. We conducted surveys and experiments to test whether the slate-pencil urchin (Eucidaris galapagensis) acts as a foundation species on subtidal walls in the Galapagos archipelago. The spines of slate-pencil urchins are more than 90% encrusted with a diverse epifauna, and a single urchin can host over 20 species (e.g., sponges, ascidians, bryozoans, corals, molluscs, worms, and crustaceans). Like many other foundation species, urchins can provide substrate and a refuge from predators. Urchins are consistently abundant throughout the Galapagos subtidal, and the total surface area of urchin spines can rival that of the primary rock substrate, which is significant since substrate availability can limit small-scale species richness in this system. Our experimental manipulation of spine configuration and exclusion of predators revealed that urchins also enhance epifaunal diversity by providing a predation refuge. Unlike previously recognized foundation species, however, the urchin habitat is modular and mobile, and has the potential to redistribute associated epifauna. Characterizing how previously overlooked foundation species can act as reservoirs of biodiversity in ecosystems, such as the Galapagos where other foundation species such as coral have declined, has important implications for how we identify foundation species, predict ecosystem stability, and prioritize conservation efforts. C1 [Altieri, Andrew H.; Witman, Jon D.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Altieri, Andrew H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Altieri, AH (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. EM AltieriA@si.edu FU Luce Graduate Fellowship from the Watson Institute for International Studies (Brown University); NSF Biological Oceanography [OCE 0222092, 1061475] FX We thank M. Brandt, J. Palardy, and R. Adams for their diving assistance, and S. Banks and the Charles Darwin Foundation for administrative and logistical assistance along with the Galapagos National Park. We offer gratitude to S. Ryan for topside support and field collections and to H. Jager for logistical help. This research was supported by a Luce Graduate Fellowship from the Watson Institute for International Studies (Brown University) to A. H. Altieri and NSF Biological Oceanography grants (OCE 0222092, 1061475) to J. D. Witman. This publication is contribution number 2092 of the Charles Darwin Foundation of the Galapagos Islands. NR 41 TC 1 Z9 1 U1 3 U2 26 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD OCT PY 2014 VL 5 IS 10 AR 124 DI 10.1890/ES14-00018.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AT7DO UT WOS:000345097200002 ER PT J AU Crifo, C Currano, ED Baresch, A Jaramillo, C AF Crifo, Camilla Currano, Ellen D. Baresch, A. Jaramillo, C. TI Variations in angiosperm leaf vein density have implications for interpreting life form in the fossil record SO GEOLOGY LA English DT Article ID RAIN-FOREST TREES; PHOTOSYNTHETIC CAPACITY; EVOLUTION; VENATION; LIGHT; ARCHITECTURE; PLACEMENT; RADIATION; HEIGHT; LITTER AB It is often difficult to interpret plant life form and position within a forest based on fossils of isolated plant organs. Here we propose leaf vein density as a new tool to interpret fossil angiosperm life form, and in particular to trace the emergence of angiosperms as members of the canopy. Angiosperm leaf vein density was analyzed in two tropical forests and one temperate forest. Comparisons of vein density between canopy and understory plants showed that vein density variation mainly reflected the position of the leaf in the canopy, independent of ecological strategy (shade tolerant versus sun demanding), phylogenetic position, and site (tropical versus temperate). Vein density values of a standing forest were reflected in its leaf litter, suggesting that fossil leaf assemblages are representative of past forest ecosystems. Comparison of vein density distributions of Cretaceous-Paleocene paleofloras (132.35-58.0 Ma) to those of a modern tropical leaf litter assemblage suggests that angiosperms emerged in forest canopies by at least 58 Ma. C1 [Crifo, Camilla; Currano, Ellen D.] Miami Univ, Dept Geol & Environm Earth Sci, Oxford, OH 45056 USA. [Crifo, Camilla; Baresch, A.; Jaramillo, C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baresch, A.] Stanford Univ, Dept Geol & Environm Sci, Stanford, CA 94305 USA. RP Crifo, C (reprint author), Univ Washington, Dept Biol, Box 351800, Seattle, WA 98195 USA. EM crifoc@uw.edu OI Crifo, Camilla/0000-0002-2491-5585 FU Smithsonian Tropical Research Institute fellowship; Geological Society of America Research Grant; Kenneth E. & Annie Caster Award of the Paleontological Society; National Science Foundation [EAR-1052478] FX This work was supported by a Smithsonian Tropical Research Institute fellowship, a Geological Society of America Research Grant, and a Kenneth E. & Annie Caster Award of the Paleontological Society to Crifo, and National Science Foundation grant EAR-1052478 to Currano. We thank J. Wright, M. Samaniego, E. Moreno, L. Londono, K. Boyce, G. Parker, J. Parker, S. McMahon, and the Smithsonian Institution Global Earth Observatory (SIGEO) network. The manuscript benefited from comments by T. Feild and three anonymous reviewers. NR 30 TC 0 Z9 0 U1 3 U2 17 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 OCT PY 2014 VL 42 IS 10 BP 919 EP 922 DI 10.1130/G35828.1 PG 4 WC Geology SC Geology GA AU1EL UT WOS:000345363700022 ER PT J AU Tester, PA Kibler, SR Holland, WC Usup, G Vandersea, MW Leaw, CP Teen, LP Larsen, J Mohammad-Noor, N Faust, MA Litaker, RW AF Tester, Patricia A. Kibler, Steven R. Holland, William C. Usup, Gires Vandersea, Mark W. Leaw, Chui Pin Teen, Lim Po Larsen, Jacob Mohammad-Noor, Normawaty Faust, Maria A. Litaker, R. Wayne TI Sampling harmful benthic dinoflagellates: Comparison of artificial and natural substrate methods SO HARMFUL ALGAE LA English DT Article DE Gambierdiscus; Ciguatera fish poisoning; Ostreopsis; Prorocentrum; Cell-based monitoring ID OSTREOPSIS CF. OVATA; PROROCENTRUM-LIMA DINOPHYCEAE; SP-NOV DINOPHYCEAE; TOXIC DINOFLAGELLATE; SPECIES DINOPHYCEAE; MANGROVE ISLAND; ASYMPTOTIC TEST; TWIN-CAYS; CIGUATERA; GAMBIERDISCUS AB This study compared two collection methods for Gambierdiscus and other benthic harmful algal bloom (BHAB) dinoflagellates, an artificial substrate method and the traditional macrophyte substrate method. Specifically, we report the results of a series of field experiments in tropical environments designed to address the correlation of benthic dinoflagellate abundance on artificial substrate and those on adjacent macrophytes. The data indicated abundance of BHAB dinoflagellates associated with new, artificial substrate was directly related to the overall abundance of BHAB cells on macrophytes in the surrounding environment. There was no difference in sample variability among the natural and artificial substrates. BHAB dinoflagellate abundance on artificial substrates reached equilibrium with the surrounding population within 24 h. Calculating cell abundance normalized to surface area of artificial substrate, rather than to the wet weight of macrophytes, eliminates complications related to the mass of different macrophyte species, problems of macrophyte preference by BHAB dinoflagellates and allows data to be compared across studies. The protocols outlined in this study are the first steps to a standardized sampling method for BHAB dinoflagellates that can support a cell-based monitoring program for ciguatera fish poisoning. While this study is primarily concerned with the ciguatera-associated genus Gambierdiscus, we also include data on the abundance of benthic Prorocentrum and Ostreopsis cells. (C) 2014 Elsevier B.V. All rights reserved. C1 [Tester, Patricia A.; Kibler, Steven R.; Holland, William C.; Vandersea, Mark W.; Litaker, R. Wayne] Natl Ocean & Atmospher Adm, Natl Ocean Serv, Natl Ctr Coastal Ocean Sci, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA. [Usup, Gires] Univ Kebangsaan Malaysia, Fak Sains Teknol, Pusat Pengajian Sains Sekitaran Sumber Alam, Program Sains Laut, Bangi 43600, Selangor, Malaysia. [Leaw, Chui Pin] Univ Malyasia Sarawak, Inst Biodivers & Environm Conservat, Kota Samarahan 94300, Sarawak, Malaysia. [Teen, Lim Po] Univ Malaysia Sarawak, Aquat Sci Program, Fac Resource Sci & Technol, Kota Samarahan 94300, Sarawak, Malaysia. [Larsen, Jacob] Dept Phycol & Mycol, IOC Sci & Commun Ctr Harmful Algae, DK-1353 Copenhagen K, Denmark. [Mohammad-Noor, Normawaty] Int Islamic Univ Malaysia, Kulliyyah Sci, Inst Oceanog & Maritime Studies, Kuantan 25200, Pahang, Malaysia. [Faust, Maria A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Tester, PA (reprint author), Natl Ocean & Atmospher Adm, Natl Ocean Serv, Natl Ctr Coastal Ocean Sci, Ctr Coastal Fisheries & Habitat Res, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. EM Patricia.Tester@noaa.gov; Steve.Kibler@noaa.gov; Chris.Holland@noaa.gov; Gires@ukm.my; Mark.W.Vandersea@noaa.gov; Leawcp@ibec.unimas.my; Ptlim@frst.unimas.my; Jacob@bot.ku.dk; Normahwaty@iium.edu.my; FaustM@si.edu; Wayne.Litaker@noaa.gov RI Leaw, Chui Pin/F-5220-2012; Lim, Po Teen/C-9758-2013 OI Leaw, Chui Pin/0000-0003-3336-1438; Lim, Po Teen/0000-0003-2823-0564 FU UNESCO IOC-Yeosu Project of Korea; National Oceanic and Atmospheric Administration's Ecology and Oceanography of Harmful Algal Blooms program [764] FX Funding was provided by the UNESCO IOC-Yeosu Project of Korea. The International Training Workshop on the Ecology and Taxonomy of Benthic Marine Dinoflagellates held 21-31 May 2012 in Pulau Sibu and the Universiti Kebangsaan, Malaysia included a field and laboratory training component and was inspired by the outcome of SCOR and IOC/UNESCO's GEOHAB: HABs in Benthic Systems Open Science Meeting in Honolulu, HI in June 2010. Partial funding was provided as an award from the National Oceanic and Atmospheric Administration's Ecology and Oceanography of Harmful Algal Blooms program (ECOHAB contribution number #764). Dr. M. Toscano, Smithsonian Institution, kindly provided partial support for the February 2012 sampling at Carrie Bow Cay, Belize. We thank the dedicated and hardworking Malaysian workshop participants including (in alphabetical order). Grace Abdala, Kieng Soon Hii, Lu Song Hui, Grace Joy Chin Wei Lie, June Moh, Chi-Thoi Nguyen, Giang Tuong Ngoc Nguyen, Ngoc Lam Nguyen, Arief Rachman, Gan Hui Shan, Mark Skinner, Toh Hii-Tan, Thamrin Thamrin, Ho Van The, Hikmah Thoha, Giang Tuong, Pradem Uttayarnmanee, Noime Walican and Hua Zhang. Also, we had the excellent assistance of Gan Jia Cheng, Gan Hui Shan, Mimi Nora Mansor and Zuhaimi Bin Samat from the Universiti Kebangsaan, Malaysia who facilitated the logistics and field work to make this workshop possible. We gratefully acknowledge the helpful comments from anonymous reviewers that improved to this manuscript. NR 72 TC 9 Z9 9 U1 2 U2 20 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 EI 1878-1470 J9 HARMFUL ALGAE JI Harmful Algae PD OCT PY 2014 VL 39 BP 8 EP 25 DI 10.1016/j.hal.2014.06.009 PG 18 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AU2SZ UT WOS:000345469100002 ER PT J AU Tester, PA Kibler, SR Holland, WC Usup, G Vandersea, MW Leaw, CP Lim, PT Larsen, J Mohammad-Noor, N Faust, MA Litaker, RW AF Tester, Patricia A. Kibler, Steven R. Holland, William C. Usup, Gires Vandersea, Mark W. Leaw, Chui Pin Lim, Po Teen Larsen, Jacob Mohammad-Noor, Normawaty Faust, Maria A. Litaker, R. Wayne TI Sampling harmful benthic dinoflagellates: Comparison of artificial and natural substrate methods (vol 39, pg 8, 2014) SO HARMFUL ALGAE LA English DT Correction C1 [Tester, Patricia A.; Kibler, Steven R.; Holland, William C.; Vandersea, Mark W.; Litaker, R. Wayne] NOAA, Ctr Coastal Fisheries & Habitat Res, Natl Ctr Coastal Ocean Sci, Natl Ocean Serv, Beaufort, NC 28516 USA. [Usup, Gires] Univ Kebangsaan Malaysia, Program Sains Laut, Pusat Pengajian Sains Sekitaran & Sumber Alam, Fak Sains & Teknol, Bangi 43600, Selangor, Malaysia. [Leaw, Chui Pin; Lim, Po Teen] Univ Malaya, Inst Ocean & Earth Sci, Bachok 16310, Kelantan, Malaysia. [Larsen, Jacob] IOC Sci & Commun Ctr Harmful Algae, Dept Phycol & Mycol, DK-1353 Copenhagen K, Denmark. [Mohammad-Noor, Normawaty] Int Islamic Univ Malaysia, Inst Oceanog & Maritime Studies, Kulliyyah Sci, Kuantan 25200, Pahang, Malaysia. [Faust, Maria A.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Tester, PA (reprint author), NOAA, Ctr Coastal Fisheries & Habitat Res, Natl Ctr Coastal Ocean Sci, Natl Ocean Serv, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. EM patricia.tester@noaa.gov RI Lim, Po Teen/C-9758-2013 OI Lim, Po Teen/0000-0003-2823-0564 NR 1 TC 0 Z9 0 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 EI 1878-1470 J9 HARMFUL ALGAE JI Harmful Algae PD OCT PY 2014 VL 39 BP 374 EP 374 DI 10.1016/j.hal.2014.09.004 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AU2SZ UT WOS:000345469100041 ER PT J AU Cooper, NW Sherry, TW Marra, PP AF Cooper, Nathan W. Sherry, Thomas W. Marra, Peter P. TI Modeling three-dimensional space use and overlap in birds SO AUK LA English DT Article DE 3D; American Redstart; home range; joint space use; overlap; territory; volume of intersection index; utilization distribution overlap index ID KERNEL DENSITY-ESTIMATION; HOME-RANGE SIZE; UTILIZATION DISTRIBUTIONS; VERTICAL STRATIFICATION; MIGRATORY PASSERINES; BANDWIDTH MATRICES; AQUATIC ANIMALS; FOREST; ECOLOGY; BEHAVIOR AB How animals use space has fundamental behavioral and ecological implications. Utilization distributions are among the most common methods for quantifying space use and have advanced our knowledge of animal ecology in a variety of ways. However, until recently, they were limited to 2 spatial dimensions (2D), despite the fact that most taxa use their environments in all 3 dimensions (3D). We (1) created 3D utilization distributions via a multivariate kernel density estimator, (2) adapted 2 overlap indices for use with 3D data, (3) estimated the minimum sample sizes required for accurate estimation of territory size, and (4) assessed these methods using data from American Redstarts (Setophaga ruticilla) during their nonbreeding season in Jamaica. We found that, compared to 3D methods, 2D methods overestimated individual (pairwise) spatial overlap by 3% in scrub habitat and 4% in mangrove habitat. Similarly, 2D methods overestimated total (all neighbors combined) spatial overlap by 9% in scrub and 12% in mangrove habitat. This indicates that American Redstarts may partition territorial space in all 3 spatial dimensions. Moreover, using overlap indices, we found that American Redstarts may avoid areas of overlap, possibly to limit agonistic interactions with neighbors. Although 3D methods require larger sample sizes (80-110 locations) than 2D (40-70 locations), we argue that modeling animal space use in 3D is more realistic and will enhance understanding of niche differentiation, interspecific and intraspecific competition, habitat selection and use, and wildlife conservation. C1 [Cooper, Nathan W.; Sherry, Thomas W.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Cooper, Nathan W.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC USA. RP Cooper, NW (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. EM nathanwands@gmail.com FU National Science Foundation [DEB0717243] FX We thank the Petroleum Corporation of Jamaica and the Font Hill staff for access to field sites. We also thank T. Duong for assistance with package "ks," S. D. Hafner for troubleshooting code, and assistants for help with fieldwork. Finally, we thank J. Pointon at OmniSTAR for providing access to subscription satellite service. P.P.M. and T.W.S. supported all research with a grant (DEB0717243) from the National Science Foundation. NR 66 TC 3 Z9 3 U1 7 U2 42 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 EI 1938-4254 J9 AUK JI AUK PD OCT PY 2014 VL 131 IS 4 BP 681 EP 693 DI 10.1642/AUK-14-17.1 PG 13 WC Ornithology SC Zoology GA AT3GF UT WOS:000344823200019 ER PT J AU Nowlan, CR Martin, RV Philip, S Lamsal, LN Krotkov, NA Marais, EA Wang, S Zhang, Q AF Nowlan, C. R. Martin, R. V. Philip, S. Lamsal, L. N. Krotkov, N. A. Marais, E. A. Wang, S. Zhang, Q. TI Global dry deposition of nitrogen dioxide and sulfur dioxide inferred from space-based measurements SO GLOBAL BIOGEOCHEMICAL CYCLES LA English DT Article DE dry deposition; OMI; sulfur dioxide; nitrogen dioxide ID OZONE MONITORING INSTRUMENT; GENERAL-CIRCULATION MODEL; BIOGENIC NOX EMISSIONS; CLEAN-AIR STATUS; UNITED-STATES; REACTIVE NITROGEN; BOUNDARY-LAYER; ATMOSPHERIC DEPOSITION; OXIDIZED NITROGEN; TRENDS NETWORK AB A method is developed to estimate global NO2 and SO2 dry deposition fluxes at high spatial resolution (0.1 degrees x0.1 degrees) using satellite measurements from the Ozone Monitoring Instrument (OMI) on the Aura satellite, in combination with simulations from the Goddard Earth Observing System chemical transport model (GEOS-Chem). These global maps for 2005-2007 provide a data set for use in examining global and regional budgets of deposition. In order to properly assess SO2 on a global scale, a method is developed to account for the geospatial character of background offsets in retrieved satellite columns. Globally, annual dry deposition to land estimated from OMI as NO2 contributes 1.5 0.5Tg of nitrogen and as SO2 contributes 13.7 4.0Tg of sulfur. Differences between OMI-inferred NO2 dry deposition fluxes and those of other models and observations vary from excellent agreement to an order of magnitude difference, with OMI typically on the low end of estimates. SO2 dry deposition fluxes compare well with in situ Clear Air Status and Trends Network-inferred flux over North America (slope=0.98, r=0.71). The most significant NO2 dry deposition flux to land per area occurs in the Pearl River Delta, China, at 13.9 kg N ha(-1) yr(-1), while SO2 dry deposition has a global maximum rate of 72.0 kg S ha(-1) yr(-1) to the east of Jinan in China's Shandong province. Dry deposition fluxes are explored in several urban areas, where NO2 contributes on average 9-36% and as much as 85% of total NOy dry deposition. C1 [Nowlan, C. R.; Martin, R. V.; Philip, S.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Nowlan, C. R.; Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Lamsal, L. N.; Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Marais, E. A.] Harvard Univ, Cambridge, MA 02138 USA. [Wang, S.] Tsinghua Univ, Sch Environm, Beijing 100084, Peoples R China. [Zhang, Q.] Tsinghua Univ, Ctr Earth Syst Sci, Beijing 100084, Peoples R China. RP Nowlan, CR (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM cnowlan@cfa.harvard.edu RI Zhang, Qiang/D-9034-2012; Martin, Randall/C-1205-2014; Krotkov, Nickolay/E-1541-2012; OI Martin, Randall/0000-0003-2632-8402; Krotkov, Nickolay/0000-0001-6170-6750; Nowlan, Caroline/0000-0002-8718-9752; Marais, Eloise/0000-0001-5477-8051 FU Environment Canada; Natural Sciences and Engineering Research Council of Canada (NSERC) FX This work was supported by Environment Canada and the Natural Sciences and Engineering Research Council of Canada (NSERC). We thank Robert Vet for helpful comments during the early stages of this project, Aaron van Donkelaar and Shailesh Kharol for code, Daniel Jacob for comments on urban deposition, and Laurens Ganzeveld for helpful comments on the manuscript. MODIS LAI data were obtained through the NASA Land Processes Distributed Active Archive Center (LP DAAC) USGS/Earth Resources Observation and Science (EROS) Center. Global dry deposition data from this study are available from the authors by request to cnowlan@cfa.harvard.edu. NR 102 TC 8 Z9 8 U1 2 U2 37 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0886-6236 EI 1944-9224 J9 GLOBAL BIOGEOCHEM CY JI Glob. Biogeochem. Cycle PD OCT PY 2014 VL 28 IS 10 BP 1025 EP 1043 DI 10.1002/2014GB004805 PG 19 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA AT2XK UT WOS:000344797500002 ER PT J AU Vanderburg, A Stefani, F Sitzman, A Crawford, M Surls, D Ling, C McDonald, J AF Vanderburg, Andrew Stefani, Francis Sitzman, Alex Crawford, Mark Surls, Dwayne Ling, Chloe McDonald, Jason TI The Electrical Specific Action to Melt of Structural Copper and Aluminum Alloys SO IEEE TRANSACTIONS ON PLASMA SCIENCE LA English DT Article DE Al6061; Al7075; aluminum alloy; C10100; C11000; C18000; C18200; electrical action to melt; exploding wire experiment; specific action to melt AB This paper describes an exploding wire experiment to measure the electrical specific action to melt of structural alloys of copper and aluminum, including C10100, C11000, C18000, C18200, Al6061, and Al7075. These alloys, which are commonly used in railguns and other pulsed power devices, are not produced in fine wire form. Instead of wires, we developed a technique to test macroscopic samples (0.25 mm x 0.5 mm cross section) manufactured with wire electrical discharge machining. This paper includes a description of the design considerations for such macroscopic exploding wire experiments. C1 [Vanderburg, Andrew] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stefani, Francis] Univ Texas Austin, Ctr Aeromech Res, Austin, TX 78712 USA. [Sitzman, Alex] Univ Texas Austin, Dept Elect Engn, Austin, TX 78712 USA. [Crawford, Mark] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Surls, Dwayne] Univ Texas Austin, Ctr Electromech, Austin, TX 78712 USA. [Ling, Chloe] CALTECH, Pasadena, CA 91125 USA. [McDonald, Jason] Bowhead Sci & Technol, Aberdeen, MD 21005 USA. RP Vanderburg, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM andrew.vanderburg@berkeley.edu; stefani@utexas.edu; asitzman@gmail.com; mtc@lanl.gov; d.surls@cem.utexas.edu; cling@caltech.edu; jason.r.mcdonald27.ctr@mail.mil FU U.S. Army Research Laboratory [W911QX-07-D-0002] FX This work was supported by the U.S. Army Research Laboratory under Contract W911QX-07-D-0002. NR 8 TC 3 Z9 3 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0093-3813 EI 1939-9375 J9 IEEE T PLASMA SCI JI IEEE Trans. Plasma Sci. PD OCT PY 2014 VL 42 IS 10 SI SI BP 3167 EP 3172 DI 10.1109/TPS.2014.2313292 PN 2 PG 6 WC Physics, Fluids & Plasmas SC Physics GA AS9EP UT WOS:000344546200041 ER PT J AU Smith, GH Dupree, AK Strader, J AF Smith, Graeme H. Dupree, Andrea K. Strader, Jay TI A Study of the lambda 10830 He I Line Among Red Giants in Messier 13 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GLOBULAR-CLUSTER STARS; NA-O ANTICORRELATION; PROTON CAPTURE CHAINS; COLOR-MAGNITUDE DIAGRAMS; MASS AGB STARS; OMEGA-CENTAURI; ABUNDANCE VARIATIONS; BRIGHT GIANTS; HORIZONTAL-BRANCH; OXYGEN ABUNDANCES AB Two properties of Messier 13 are pertinent to the study of mass loss among metal-poor stars and the chemical evolution of globular clusters: (1) an extended blue horizontal branch, which seems to demand mass loss from red giant progenitor stars and possibly an enhanced helium abundance, and (2) the presence of internal abundance inhomogeneities of elements in the mass range from C to A1. A popular explanation for this second phenomenon is that M13 was self-enriched by intermediate-mass asymptotic giant branch (IM-AGB) stars of a type that may also have been able to instigate helium enrichment. Spectra of the lambda 10830 absorption feature produced by He I have been obtained by using the NIRSPEC spectrometer on the Keck 2 telescope for seven red giants in M13 chosen to have a range in lambda 3883 CN band strengths, oxygen, and sodium abundances. Whereas these spectra do reveal the presence of fast winds among some M13 red giants, they provide little support for helium abundance differences of the type that might have been generated by a burst of IM-AGB star activity within the M13 protocluster. C1 [Smith, Graeme H.] UC Santa Cruz, Dept Astron & Astrophys, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Dupree, Andrea K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Smith, GH (reprint author), UC Santa Cruz, Dept Astron & Astrophys, Lick Observ, Univ Calif Observ, 1156 High St, Santa Cruz, CA 95064 USA. EM graeme@ucolick.org; dupree@cfa.harvard.edu; strader@pa.msu.edu FU NSF [AST-0908757] FX Thanks are extended to Dr. Greg Wirth for serving as the support astronomer on the Keck observing run during which the NIRSPEC observations for this paper were acquired. 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. Thank you to the referee for a useful review of the manuscript. GHS gratefully acknowledges the support of NSF award AST-0908757. NR 81 TC 4 Z9 4 U1 0 U2 0 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 OCT PY 2014 VL 126 IS 944 BP 901 EP 913 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT1WD UT WOS:000344720900002 ER PT J AU Conroy, KE Prsa, A Stassun, KG Bloemen, S Parvizi, M Quarles, B Boyajian, T Barclay, T Shporer, A Latham, DW Abdul-Masih, M AF Conroy, Kyle E. Prsa, Andrej Stassun, Keivan G. Bloemen, Steven Parvizi, Mahmoud Quarles, Billy Boyajian, Tabetha Barclay, Thomas Shporer, Avi Latham, David W. Abdul-Masih, Michael TI Kepler Eclipsing Binary Stars. V. Identification of 31 Candidate Eclipsing Binaries in the K2 Engineering Dataset SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DATA RELEASE; PLANET; I. AB Over 2500 eclipsing binaries were identified and characterized from the ultraprecise photometric data provided by the Kepler space telescope. Kepler is now beginning its second mission, K2, which is proving to again provide ultraprecise photometry for a large sample of eclipsing binary stars. In the 1951 light curves covering 12 days in the K2 engineering dataset, we have identified and determined the ephemerides for 31 candidate eclipsing binaries that demonstrate the capabilities for eclipsing binary science in the upcoming campaigns in K2. Of those, 20 are new discoveries. We describe both manual and automated approaches to harvesting the complete set of eclipsing binaries in the K2 data, provide identifications and details for the full set of candidate eclipsing binaries present in the engineering dataset, and discuss the prospects for application of eclipsing binary searches in the K2 mission. C1 [Conroy, Kyle E.; Stassun, Keivan G.; Parvizi, Mahmoud] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Prsa, Andrej; Abdul-Masih, Michael] Villanova Univ, Dept Astrophys & Planetary Sci, Villanova, PA 19085 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Bloemen, Steven] Radboud Univ Nijmegen, Dept Astrophys, Inst Math Astrophys & Particle Phys, NL-6500 GL Nijmegen, Netherlands. [Bloemen, Steven] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Quarles, Billy; Barclay, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Boyajian, Tabetha] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Barclay, Thomas] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Conroy, KE (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. OI Boyajian, Tabetha/0000-0001-9879-9313 FU NASA Astrophysical Data Analysis Program [NNX12AE22G]; NASA Kepler Participating Scientist Program [NNX12AD20G]; Foundation for Fundamental Research on Matter (FOM), which is part of the Netherlands Organisation for Scientific Research (NWO) FX The authors gratefully acknowledge everybody who has made Kepler, and especially the K2 mission, possible. K. E. C. and K. G. S. gratefully acknowledge support from NASA Astrophysical Data Analysis Program grant NNX12AE22G. A. P. gratefully acknowledges support from the NASA Kepler Participating Scientist Program grant NNX12AD20G. S. B. is supported by the Foundation for Fundamental Research on Matter (FOM), which is part of the Netherlands Organisation for Scientific Research (NWO). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 16 TC 6 Z9 6 U1 0 U2 2 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 OCT PY 2014 VL 126 IS 944 BP 914 EP 922 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT1WD UT WOS:000344720900003 ER PT J AU Vanderburg, A Johnson, JA AF Vanderburg, Andrew Johnson, John Asher TI A Technique for Extracting Highly Precise Photometry for the Two-Wheeled Kepler Mission SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID EARTH-SIZED PLANET; SOLAR-TYPE STARS; BRIGHTNESS VARIATIONS; EXOPLANET; FLICKER; TRANSIT; IDL AB The original Kepler mission achieved high photometric precision thanks to ultrastable pointing enabled by use of four reaction wheels. The loss of two of these reaction wheels reduced the telescope's ability to point precisely for extended periods of time, and as a result, the photometric precision has suffered. We present a technique for generating photometric light curves from pixel-level data obtained with the two-wheeled extended Kepler mission, K2. Our photometric technique accounts for the nonuniform pixel response function of the Kepler detectors by correlating flux measurements with the spacecraft's pointing and removing the dependence. When we apply our technique to the ensemble of stars observed during the Kepler Two-Wheel Concept Engineering Test, we find improvements over raw K2 photometry by factors of 2-5, with noise properties qualitatively similar to Kepler targets at the same magnitudes. We find evidence that the improvement in photometric precision depends on each target's position in the Kepler field of view, with worst precision near the edges of the field. Overall, this technique restores the median-attainable photometric precision within a factor of two of the original Kepler photometric precision for targets ranging from 10th to 15th magnitude in the Kepler bandpass, peaking with a median precision within 35% to that of Kepler for stars between 12th and 13th magnitude in the Kepler bandpass. C1 [Vanderburg, Andrew; Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vanderburg, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM avanderburg@cfa.harvard.edu FU NASA [NAS5-26555]; NASA Office of Space Science [NNX13AC07G]; NASA Science Mission directorate; National Aeronautics and Space Administration under the Exoplanet Exploration Program; NSF Graduate Research Fellowship [DGE 1144152]; David and Lucile Packard Foundation; Alfred P. Sloan Foundation FX We acknowledge the tremendous effort of the K2 team and Ball Aerospace to make the K2 mission a success. We thank the anonymous reviewer for many insightful comments and suggestions. We thank Tom Barclay for helpful conversations and for providing the precise boresight coordinates for the Kepler Two-Wheel Concept Engineering Test. We are grateful to Fabienne Bastien for a useful conversation regarding flicker measurements with K2 data. We thank Eric Agol, Suzanne Aigrain, Juliette Becker, Christian Clanton, Daniel Foreman-Mackey, Heather Knutson, Benjamin Montet, and Jonathan Swift for their helpful comments on the manuscript. Some/all of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant 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 research has made use of NASA's Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. A.V. is supported by the NSF Graduate Research Fellowship, Grant No. DGE 1144152. J.A.J is supported by generous grants from the David and Lucile Packard Foundation and the Alfred P. Sloan Foundation. NR 39 TC 90 Z9 90 U1 0 U2 0 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 OCT PY 2014 VL 126 IS 944 BP 948 EP 958 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AT1WD UT WOS:000344720900006 ER PT J AU Kinney, JR AF Kinney, Jeremy R. TI Blue Sky Metropolis: The Aerospace Century in Southern California SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Kinney, Jeremy R.] Smithsonian Natl Air & Space Museum, Dept Aeronaut, Washington, DC 20560 USA. RP Kinney, JR (reprint author), Smithsonian Natl Air & Space Museum, Dept Aeronaut, Washington, DC 20560 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 OCT PY 2014 VL 55 IS 4 BP 1023 EP 1024 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA AT3KX UT WOS:000344834900030 ER PT J AU Bocchio, M Jones, AP Slavin, JD AF Bocchio, Marco Jones, Anthony P. Slavin, Jonathan D. TI A re-evaluation of dust processing in supernova shock waves SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; dust, extinction; methods: numerical; shock waves ID GRAIN-GRAIN COLLISIONS; INTERSTELLAR-MEDIUM; INFRARED-EMISSION; HOT GAS; INTERMEDIATE-VELOCITY; SIZE DISTRIBUTION; AMORPHOUS-CARBON; ISM DUST; DESTRUCTION; EVOLUTION AB Context. There is a long-standing and large discrepancy between the timescale for dust formation around evolved stars and the rapid dust destruction timescale in interstellar shocks. Aims. We use our latest estimates for dust processing to re-evaluate the dust destruction efficiency in supernova triggered shock waves, estimate the dust lifetime, and calculate the emission and extinction from shocked dust. Methods. We modelled the sputtering and fragmentation of grains in interstellar shocks for shock velocities between 50 kms(-1) and 200 km s(-1). We constrained the dust destruction using our recent dust model. Finally, we coupled our code to the DustEM code in order to estimate the emission and extinction from the dust post-shock. Results. Carbonaceous grains are quickly destroyed, even in a 50 kms(-1) shock, leading to a shorter lifetime than in previous studies. Silicate grains appear to be more resilient, but the new destruction lifetime that we find is similar to previous studies and short compared to the dust injection timescale. Conclusions. The calculated fraction of elements locked in grains is not compatible with the observed values and therefore implies the re-formation of dust in the dense regions of the interstellar medium. Better modelling of the silicate sputtering together with hydrodynamical simulations of interstellar shocks, appears to reduce the silicate destruction and may close the destruction-formation timescale gap. C1 [Bocchio, Marco; Jones, Anthony P.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. [Slavin, Jonathan D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bocchio, M (reprint author), Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR 8617, F-91405 Orsay, France. EM marco.bocchio@ias.u-psud.fr OI Slavin, Jonathan/0000-0002-7597-6935 NR 62 TC 26 Z9 26 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 OCT PY 2014 VL 570 AR A32 DI 10.1051/0004-6361/201424368 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3EE UT WOS:000344158500107 ER PT J AU Coenen, T van Leeuwen, J Hessels, JWT Stappers, BW Kondratiev, VI Alexov, A Breton, RP Bilous, A Cooper, S Falcke, H Fallows, RA Gajjar, V Griessmeier, JM Hassall, TE Karastergiou, A Keane, EF Kramer, M Kuniyoshi, M Noutsos, A Oslowski, S Pilia, M Serylak, M Schrijvers, C Sobey, C ter Veen, S Verbiest, J Weltevrede, P Wijnholds, S Zagkouris, K van Amesfoort, AS Anderson, J Asgekar, A Avruch, IM Bell, ME Bentum, MJ Bernardi, G Best, P Bonafede, A Breitling, F Broderick, J Bruggen, M Butcher, HR Ciardi, B Corstanje, A Deller, A Duscha, S Eisloffel, J Fender, R Ferrari, C Frieswijk, W Garrett, MA de Gasperin, F de Geus, E Gunst, AW Hamaker, JP Heald, G Hoeft, M van der Horst, A Juette, E Kuper, G Law, C Mann, G McFadden, R McKay-Bukowski, D McKean, JP Munk, H Orru, E Paas, H Pandey-Pommier, M Polatidis, AG Reich, W Renting, A Rottgering, H Rowlinson, A Scaife, AMM Schwarz, D Sluman, J Smirnov, O Swinbank, J Tagger, M Tang, Y Tasse, C Thoudam, S Toribio, C Vermeulen, R Vocks, C van Weeren, RJ Wucknitz, O Zarka, P Zensus, A AF Coenen, Thijs van Leeuwen, Joeri Hessels, Jason W. T. Stappers, Ben W. Kondratiev, Vladislav I. Alexov, A. Breton, R. P. Bilous, A. Cooper, S. Falcke, H. Fallows, R. A. Gajjar, V. Griessmeier, J-M. Hassall, T. E. Karastergiou, A. Keane, E. F. Kramer, M. Kuniyoshi, M. Noutsos, A. Oslowski, S. Pilia, M. Serylak, M. Schrijvers, C. Sobey, C. ter Veen, S. Verbiest, J. Weltevrede, P. Wijnholds, S. Zagkouris, K. van Amesfoort, A. S. Anderson, J. Asgekar, A. Avruch, I. M. Bell, M. E. Bentum, M. J. Bernardi, G. Best, P. Bonafede, A. Breitling, F. Broderick, J. Brueggen, M. Butcher, H. R. Ciardi, B. Corstanje, A. Deller, A. Duscha, S. Eisloeffel, J. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. de Gasperin, F. de Geus, E. Gunst, A. W. Hamaker, J. P. Heald, G. Hoeft, M. van der Horst, A. Juette, E. Kuper, G. Law, C. Mann, G. McFadden, R. McKay-Bukowski, D. McKean, J. P. Munk, H. Orru, E. Paas, H. Pandey-Pommier, M. Polatidis, A. G. Reich, W. Renting, A. Rottgering, H. Rowlinson, A. Scaife, A. M. M. Schwarz, D. Sluman, J. Smirnov, O. Swinbank, J. Tagger, M. Tang, Y. Tasse, C. Thoudam, S. Toribio, C. Vermeulen, R. Vocks, C. van Weeren, R. J. Wucknitz, O. Zarka, P. Zensus, A. TI The LOFAR pilot surveys for pulsars and fast radio transients SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE pulsars: general; telescopes; surveys ID ALLEN TELESCOPE ARRAY; SPECTRAL INDEX; STATE CHANGE; EMISSION; MHZ; BURSTS; BINARY; DISCOVERY; POPULATION; ORIGIN AB We have conducted two pilot surveys for radio pulsars and fast transients with the Low-Frequency Array (LOFAR) around 140 MHz and here report on the first low-frequency fast-radio burst limit and the discovery of two new pulsars. The first survey, the LOFAR Pilot Pulsar Survey (LPPS), observed a large fraction of the northern sky, similar to 1.4 x 10(4) deg(2), with 1 h dwell times. Each observation covered similar to 75 deg(2) using 7 independent fields formed by incoherently summing the high-band antenna fields. The second pilot survey, the LOFAR Tied-Array Survey (LOTAS), spanned similar to 600 deg(2), with roughly a 5-fold increase in sensitivity compared with LPPS. Using a coherent sum of the 6 LOFAR "Superterp" stations, we formed 19 tied-array beams, together covering 4 deg(2) per pointing. From LPPS we derive a limit on the occurrence, at 142 MHz, of dispersed radio bursts of <150 day(-1) sky(-1), for bursts brighter than S > 107 Jy for the narrowest searched burst duration of 0.66 ms. In LPPS, we re-detected 65 previously known pulsars. LOTAS discovered two pulsars, the first with LOFAR or any digital aperture array. LOTAS also re-detected 27 previously known pulsars. These pilot studies show that LOFAR can efficiently carry out all-sky surveys for pulsars and fast transients, and they set the stage for further surveying efforts using LOFAR and the planned low-frequency component of the Square Kilometer Array. C1 [Coenen, Thijs; van Leeuwen, Joeri; Hessels, Jason W. T.; Alexov, A.; van der Horst, A.; Law, C.; Rowlinson, A.; Swinbank, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Coenen, Thijs; van Leeuwen, Joeri; Hessels, Jason W. T.; Kondratiev, Vladislav I.; Falcke, H.; Fallows, R. A.; Pilia, M.; Sobey, C.; Wijnholds, S.; van Amesfoort, A. S.; Asgekar, A.; Bentum, M. J.; Deller, A.; Duscha, S.; Frieswijk, W.; Garrett, M. A.; de Geus, E.; Gunst, A. W.; Hamaker, J. P.; Heald, G.; Kuper, G.; McFadden, R.; McKean, J. P.; Munk, H.; Orru, E.; Polatidis, A. G.; Renting, A.; Sluman, J.; Tang, Y.; Toribio, C.; Vermeulen, R.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Stappers, Ben W.; Cooper, S.; Gajjar, V.; Kramer, M.; Weltevrede, P.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Kondratiev, Vladislav I.] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Breton, R. P.; Hassall, T. E.; Broderick, J.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Bilous, A.; Falcke, H.; ter Veen, S.; Corstanje, A.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Gajjar, V.] Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Griessmeier, J-M.; Tagger, M.] LPC2E UMR 7328 CNRS, Lab Phys & Chim Environm Espace, F-45071 Orleans, France. [Griessmeier, J-M.] CNRS INSU, Stn Radioastron Nancay, Observ Paris, F-18330 Nancay, France. [Karastergiou, A.; Serylak, M.; Zagkouris, K.; Fender, R.] Univ Oxford, Oxford OX1 3RH, England. [Keane, E. F.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Keane, E. F.] ARC Ctr Excellence All Sky Astrophys CAASTRO, D-53121 Bonn, Germany. [Kramer, M.; Kuniyoshi, M.; Noutsos, A.; Oslowski, S.; Reich, W.; Wucknitz, O.; Zensus, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Oslowski, S.; Verbiest, J.; Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Schrijvers, C.] SURFsara, NL-1090 GP Amsterdam, Netherlands. [Anderson, J.] Deutsch GeoForschungsZentrum GFZ, Helmholtz Zentrum Potsdam, Dept Geodesy & Remote Sensing 1, D-14473 Potsdam, Germany. [Anderson, J.; Breitling, F.; Mann, G.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Asgekar, A.] Shell Technol Ctr, Bangalore, Karnataka, India. [Avruch, I. M.] SRON Netherlands Insitute Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, I. M.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bell, M. E.] 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, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Eisloeffel, J.; Hoeft, M.] Thuringer Landesternwarte, D-07778 Tautenburg, Germany. [Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR7293, CNRS,Observ Cote dAzur, F-06300 Nice, France. [Garrett, M. A.; Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [de Geus, E.] SmarterVision BV, NL-9401 JX Assen, Netherlands. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Paas, H.] Univ Groningen, CIT, NL-9700 AB Groningen, Netherlands. [Pandey-Pommier, M.] Observ Lyon, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Smirnov, O.] Rhodes Univ, Dept Phys & Elelct, ZA-6140 Grahamstown, South Africa. [Smirnov, O.] SKA South Africa, ZA-7405 Pinelands, South Africa. [Tasse, C.; Zarka, P.] Observ Paris, LESIA, UMR CNRS 8109, F-92195 Meudon, France. RP Coenen, T (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM leeuwen@astron.nl RI Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Kondratiev, Vladislav/N-1105-2015; Breton, Rene/A-5536-2017; OI Tagger, Michel/0000-0003-2962-3220; Bilous, Anna/0000-0002-7177-6987; de Gasperin, Francesco/0000-0003-4439-2627; Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660; Oslowski, Stefan/0000-0003-0289-0732; Kondratiev, Vladislav/0000-0001-8864-7471; Breton, Rene/0000-0001-8522-4983; Swinbank, John/0000-0001-9445-1846 FU Netherlands Research School for Astronomy [NOVA3-NW3-2.3.1]; European Commission [224838]; NWO Veni Fellowship; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX We thank J. Green and P. Abeyratne for help with LPPS processing. This work was supported by grants from the Netherlands Research School for Astronomy (NOVA3-NW3-2.3.1) and by the European Commission (FP7-PEOPLE-2007-4-3-IRG #224838) to JVL; an NWO Veni Fellowship to JWTH; and Agence Nationale de la Recherche grant ANR-09-JCJC-0001-01 to CF. LOFAR is designed and constructed by ASTRON, and is operated by the International LOFAR Telescope (ILT) foundation. LOTAS "bandwidth-on-demand" was provided by SURFnet. LOTAS processing was carried out on the Dutch grid infrastructure supported by the BiGGrid project. NR 59 TC 22 Z9 22 U1 0 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 OCT PY 2014 VL 570 AR A60 DI 10.1051/0004-6361/201424495 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3EE UT WOS:000344158500121 ER PT J AU Fontana, A Dunlop, JS Paris, D Targett, TA Boutsia, K Castellano, M Galametz, A Grazian, A McLure, R Merlin, E Pentericci, L Wuyts, S Almaini, O Caputi, K Chary, RR Cirasuolo, M Conselice, CJ Cooray, A Daddi, E Dickinson, M Faber, SM Fazio, G Ferguson, HC Giallongo, E Giavalisco, M Grogin, NA Hathi, N Koekemoer, AM Koo, DC Lucas, RA Nonino, M Rix, HW Renzini, A Rosario, D Santini, P Scarlata, C Sommariva, V Stark, DP van der Wel, A Vanzella, E Wild, V Yan, H Zibetti, S AF Fontana, A. Dunlop, J. S. Paris, D. Targett, T. A. Boutsia, K. Castellano, M. Galametz, A. Grazian, A. McLure, R. Merlin, E. Pentericci, L. Wuyts, S. Almaini, O. Caputi, K. Chary, R. -R. Cirasuolo, M. Conselice, C. J. Cooray, A. Daddi, E. Dickinson, M. Faber, S. M. Fazio, G. Ferguson, H. C. Giallongo, E. Giavalisco, M. Grogin, N. A. Hathi, N. Koekemoer, A. M. Koo, D. C. Lucas, R. A. Nonino, M. Rix, H. W. Renzini, A. Rosario, D. Santini, P. Scarlata, C. Sommariva, V. Stark, D. P. van der Wel, A. Vanzella, E. Wild, V. Yan, H. Zibetti, S. TI The Hawk-I UDS and GOODS Survey (HUGS): Survey design and deep K-band number counts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE surveys; galaxies: evolution ID EXTRAGALACTIC LEGACY SURVEY; STAR-FORMING GALAXIES; SOUTH FIELD; PHOTOMETRIC REDSHIFTS; LUMINOSITY FUNCTION; MULTICOLOR CATALOG; MUSIC SAMPLE; FAINT; TELESCOPE; CANDELS AB We present the results of a new, ultra-deep, near-infrared imaging survey executed with the Hawk-I imager at the ESO VLT, of which we make all the data (images and catalog) public. This survey, named HUGS (Hawk-I UDS and GOODS Survey), provides deep, high-quality imaging in the K and Y bands over the portions of the UKIDSS UDS and GOODS-South fields covered by the CANDELS HST WFC3/IR survey. In this paper we describe the survey strategy, the observational campaign, the data reduction process, and the data quality. We show that, thanks to exquisite image quality and extremely long exposure times, HUGS delivers the deepest K-band images ever collected over areas of cosmological interest, and in general ideally complements the CANDELS data set in terms of image quality and depth. In the GOODS-S field, the K-band observations cover the whole CANDELS area with a complex geometry made of 6 different, partly overlapping pointings, in order to best match the deep and wide areas of CANDELS imaging. In the deepest region (which includes most of the Hubble Ultra Deep Field) exposure times exceed 80 hours of integration, yielding a 1 - sigma magnitude limit per square arcsec of similar or equal to 28.0 AB mag. The seeing is exceptional and homogeneous across the various pointings, confined to the range 0.38-0.43 arcsec. In the UDS field the survey is about one magnitude shallower (to match the correspondingly shallower depth of the CANDELS images) but includes also Y-band band imaging (which, in the UDS, was not provided by the CANDELS WFC3/IR imaging). In the K-band, with an average exposure time of 13 hours, and seeing in the range 0.37-0.43 arcsec, the 1 - sigma limit per square arcsec in the UDS imaging is similar or equal to 27.3 AB mag. In the Y-band, with an average exposure time similar or equal to 8 h, and seeing in the range 0.45-0.5 arcsec, the imaging yields a 1 - sigma limit per square arcsec of similar or equal to 28.3 AB mag. We show that the HUGS observations are well matched to the depth of the CANDELS WFC3/IR data, since the majority of even the faintest galaxies detected in the CANDELS H-band images are also detected in HUGS. Finally we present the K-band galaxy number counts produced by combining the HUGS data from the two fields. We show that the slope of the number counts depends sensitively on the assumed distribution of galaxy sizes, with potential impact on the estimated extra-galactic background light. C1 [Fontana, A.; Paris, D.; Boutsia, K.; Castellano, M.; Galametz, A.; Grazian, A.; Merlin, E.; Pentericci, L.; Giallongo, E.; Santini, P.; Sommariva, V.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Dunlop, J. S.; Targett, T. A.; McLure, R.; Cirasuolo, M.; Wild, V.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Targett, T. A.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Wuyts, S.; Rosario, D.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. [Almaini, O.; Conselice, C. J.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Caputi, K.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Chary, R. -R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Daddi, E.] CEA Saclay, DSM, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Faber, S. M.; Koo, D. C.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Fazio, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferguson, H. C.; Grogin, N. A.; Koekemoer, A. M.; Lucas, R. A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Giavalisco, M.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Hathi, N.] Aix Marseille Univ, LAM, CNRS, UMR 7326, F-13388 Marseille, France. [Nonino, M.] INAF Osservatorio Astron Trieste, Trieste, Italy. [Rix, H. W.; van der Wel, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Renzini, A.] Osserv Astron Padova, I-35122 Padua, Italy. [Scarlata, C.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN USA. [Scarlata, C.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Stark, D. P.] Univ Arizona, Steward Observ, Dept Astron, Tucson, AZ USA. [Sommariva, V.; Vanzella, E.] INAF Osservatorio Astron Bologna, Bologna, Italy. [Wild, V.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Yan, H.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Zibetti, S.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Fontana, A (reprint author), INAF Osservatorio Astron Roma, Via Frascati 33, I-00040 Rome, Italy. EM adriano.fontana@oa-roma.inaf.it RI Hathi, Nimish/J-7092-2014; Daddi, Emanuele/D-1649-2012; OI Koekemoer, Anton/0000-0002-6610-2048; Hathi, Nimish/0000-0001-6145-5090; Daddi, Emanuele/0000-0002-3331-9590; Castellano, Marco/0000-0001-9875-8263; Nonino, Mario/0000-0001-6342-9662; Santini, Paola/0000-0002-9334-8705; Giallongo, Emanuele/0000-0003-0734-1273; Vanzella, Eros/0000-0002-5057-135X; Almaini, Omar/0000-0001-9328-3991 FU EC FP7 SPACE project ASTRODEEP [312725]; Royal Society via a Wolfson Research Merit Award; ERC through an Advanced Grant; US NSF [AST08-08133]; ERC through the starting grant SEDmorph; ERC via consolidator grant; ESO [60.A-9284, 181.A0717, 186.A-0898] FX This work would not have been possible without the support and dedication of the whole ESO staff. We thank in particular our support astronomer Monika Petr-Gotzens. We are also grateful to the memory of Alan Moorwood, who was fundamental in motivating the development of the Hawk-I instrument, with which our survey has been undertaken. We also thank the referee, V. Manieri, for his accurate report. A. F. and J.S.D. acknowledge the contribution of the EC FP7 SPACE project ASTRODEEP (Ref. No: 312725). J.S.D. also acknowledges the support of the Royal Society via a Wolfson Research Merit Award, and the support of the ERC through an Advanced Grant. D. C. K. and S. M. F. were supported by US NSF grant AST08-08133. V. W. acknowledges support of the ERC through the starting grant SEDmorph. R.J.M. acknowledges ERC funding via the award of a consolidator grant. This work uses data from the following ESO programs: 60.A-9284, 181.A0717, 186.A-0898. NR 41 TC 23 Z9 23 U1 1 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 OCT PY 2014 VL 570 AR A11 DI 10.1051/0004-6361/201423543 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3EE UT WOS:000344158500024 ER PT J AU Louvet, F Motte, F Hennebelle, P Maury, A Bonnell, I Bontemps, S Gusdorf, A Hill, T Gueth, F Peretto, N Duarte-Cabral, A Stephan, G Schilke, P Csengeri, T Luong, QN Lis, DC AF Louvet, F. Motte, F. Hennebelle, P. Maury, A. Bonnell, I. Bontemps, S. Gusdorf, A. Hill, T. Gueth, F. Peretto, N. Duarte-Cabral, A. Stephan, G. Schilke, P. Csengeri, T. Luong, Q. Nguyen Lis, D. C. TI The W43-MM1 mini-starburst ridge, a test for star formation efficiency models SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; stars: protostars; stars: massive; ISM: clouds; submillimeter: ISM; submillimeter: stars ID NEARBY MOLECULAR CLOUDS; YOUNG STELLAR OBJECTS; G30.79 FIR 10; CYGNUS-X; INITIAL HIGHLIGHTS; MASSIVE PROTOSTARS; PRESTELLAR CORES; EARLIEST PHASES; MAGNETIC-FIELDS; FORMING COMPLEX AB Context. Star formation efficiency (SFE) theories are currently based on statistical distributions of turbulent cloud structures and a simple model of star formation from cores. They remain poorly tested, especially at the highest densities. Aims. We investigate the effects of gas density on the SFE through measurements of the core formation efficiency (CFE). With a total mass of similar to 2 x 10(4) M-circle dot, the W43-MM1 ridge is one of the most convincing candidate precursors of Galactic starburst clusters and thus one of the best places to investigate star formation. Methods. We used high-angular resolution maps obtained at 3 mm and 1 mm within the W43-MM1 ridge with the IRAM Plateau de Bure Interferometer to reveal a cluster of 11 massive dense cores, and, one of the most massive protostellar cores known. A Herschel column density image provided the mass distribution of the cloud gas. We then measured the "instantaneous" CFE and estimated the SFE and the star formation rate (SFR) within subregions of the W43-MM1 ridge. Results. The high SFE found in the ridge (similar to 6% enclosed in similar to 8 pc(3)) confirms its ability to form a starburst cluster. There is, however, a clear lack of dense cores in the eastern part of the ridge, which may be currently assembling. The CFE and the SFE are observed to increase with volume gas density, while the SFR per free fall time steeply decreases with the virial parameter, alpha(vir). Statistical models of the SFR may describe the outskirts of the W43-MM1 ridge well, but struggle to reproduce its inner part, which corresponds to measurements at low alpha(vir). It may be that ridges do not follow the log-normal density distribution, Larson relations, and stationary conditions forced in the statistical SFR models. C1 [Louvet, F.; Motte, F.; Hennebelle, P.; Maury, A.] Univ Paris Diderot, CNRS INSU, CEA IRFU, Lab AIM Paris Saclay,CEA Saclay,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Maury, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bonnell, I.] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Bontemps, S.] Univ Bordeaux 1, CNRS INSU, OASU LAB UMR 5804, F-33270 Floirac, France. [Gusdorf, A.] Ecole Normale Super, Observ Paris, CNRS, LERMA,UMR 8112, F-75231 Paris 05, France. [Hill, T.] Joint ALMA Observ, Santiago, Chile. [Gueth, F.] Inst Radioastron Millimetr IRAM, F-38406 St Martin Dheres, France. [Peretto, N.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Duarte-Cabral, A.] Univ Exeter, Sch Phys & Astron, Exeter EX4 4QL, Devon, England. [Schilke, P.] Univ Cologne, Phys Inst, D-50937 Cologne, Germany. [Stephan, G.] Observ Paris, LERMA2, F-75014 Paris, France. [Csengeri, T.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Luong, Q. Nguyen] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Lis, D. C.] CALTECH, Pasadena, CA 91125 USA. [Lis, D. C.] Univ Paris 06, Sorbonne Univ, CNRS, Observ Paris,UMR 811,LERMA, Paris, France. RP Louvet, F (reprint author), Univ Paris Diderot, CNRS INSU, CEA IRFU, Lab AIM Paris Saclay,CEA Saclay,Serv Astrophys, Bat 709, F-91191 Gif Sur Yvette, France. EM fabien.louvet@cea.fr NR 59 TC 19 Z9 19 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 OCT PY 2014 VL 570 AR A15 DI 10.1051/0004-6361/201423603 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3EE UT WOS:000344158500029 ER PT J AU See, V Jardine, M Vidotto, AA Petit, P Marsden, SC Jeffers, SV do Nascimento, JD AF See, V. Jardine, M. Vidotto, A. A. Petit, P. Marsden, S. C. Jeffers, S. V. do Nascimento, J. D., Jr. TI The effects of stellar winds on the magnetospheres and potential habitability of exoplanets SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: magnetic fields; planet-star interactions; stars: low-mass; stars: mass-loss ID MAIN-SEQUENCE STARS; SCALE MAGNETIC TOPOLOGIES; MASS-LOSS RATES; ACTIVITY-ROTATION RELATIONSHIP; EARTH-LIKE EXOPLANETS; EJECTION CME ACTIVITY; BILLION YEARS AGO; SOLAR-LIKE STARS; M DWARFS; TERRESTRIAL EXOPLANETS AB Context. The principle definition of habitability for exoplanets is whether they can sustain liquid water on their surfaces, i.e. that they orbit within the habitable zone. However, the planet's magnetosphere should also be considered, since without it, an exoplanet's atmosphere may be eroded away by stellar winds. Aims. The aim of this paper is to investigate magnetospheric protection of a planet from the effects of stellar winds from solar-mass stars. Methods. We study hypothetical Earth-like exoplanets orbiting in the host star's habitable zone for a sample of 124 solar-mass stars. These are targets that have been observed by the Bcool Collaboration. Using two wind models, we calculate the magnetospheric extent of each exoplanet. These wind models are computationally inexpensive and allow the community to quickly estimate the magnetospheric size of magnetised Earth-analogues orbiting cool stars. Results. Most of the simulated planets in our sample can maintain a magnetosphere of similar to 5 Earth radii or larger. This suggests that magnetised Earth analogues in the habitable zones of solar analogues are able to protect their atmospheres and is in contrast to planets around young active M dwarfs. In general, we find that Earth-analogues around solar-type stars, of age 1.5 Gyr or older, can maintain at least a Paleoarchean Earth sized magnetosphere. Our results indicate that planets around 0.6-0.8 solar-mass stars on the low activity side of the Vaughan-Preston gap are the optimum observing targets for habitable Earth analogues. C1 [See, V.; Jardine, M.; Vidotto, A. A.] Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Vidotto, A. A.] Univ Geneva, Observ Geneve, CH-1290 Sauverny, Switzerland. [Petit, P.] Univ Toulouse, UPS OMP, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Petit, P.] CNRS, Inst Rech Astrophys & Planetol, F-31400 Toulouse, France. [Marsden, S. C.] Univ So Queensland, Computat Engn & Sci Res Ctr, Toowoomba, Qld 4350, Australia. [Jeffers, S. V.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [do Nascimento, J. D., Jr.] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil. [do Nascimento, J. D., Jr.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP See, V (reprint author), Univ St Andrews, SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. EM wcvs@st-andrews.ac.uk OI Petit, Pascal/0000-0001-7624-9222; Vidotto, Aline/0000-0001-5371-2675; Marsden, Stephen/0000-0001-5522-8887 FU STFC studentship; Royal Astronomical Society Fellowship; Ambizione Fellowship from the Swiss National Science Foundation; Deutsche Forschungsgemeinschaft (DFG) [SFB 963/1] FX The authors are thankful for helpful comments from an anonymous referee. V. S. acknowledges the support of an STFC studentship. A.A.V. acknowledges support from a Royal Astronomical Society Fellowship and an Ambizione Fellowship from the Swiss National Science Foundation. S.V.J. acknowledges research funding by the Deutsche Forschungsgemeinschaft (DFG) under grant SFB 963/1, project A16. Partly based on data from the Brazilian CFHT time allocation under the proposals 09.BB03, 11.AB05, PI: J.D. do Nascimento. NR 76 TC 12 Z9 12 U1 0 U2 14 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 OCT PY 2014 VL 570 AR A99 DI 10.1051/0004-6361/201424323 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3EE UT WOS:000344158500102 ER PT J AU Szabo, R Benko, JM Paparo, M Chapellier, E Poretti, E Baglin, A Weiss, WW Kolenberg, K Guggenberger, E Le Borgne, JF AF Szabo, R. Benko, J. M. Paparo, M. Chapellier, E. Poretti, E. Baglin, A. Weiss, W. W. Kolenberg, K. Guggenberger, E. Le Borgne, J. -F. TI Revisiting CoRoT RRLyrae stars: detection of period doubling and temporal variation of additional frequencies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: variables: RR Lyrae; stars: oscillations; stars: interiors; techniques: photometric ID RR-LYRAE STARS; LIGHT CURVES; PHYSICAL PARAMETERS; NONRADIAL MODE; MW LYR; KEPLER; PULSATION; MODULATION; PHOTOMETRY; MISSION AB Context. High-precision, space-based photometric missions like CoRoT and Kepler have revealed new and surprising phenomena in classical variable stars. Such discoveries were the period doubling in RRLyrae stars and the frequent occurrence of additional periodicities some of which can be explained by radial overtone modes, but others are discordant with the radial eigenfrequency spectrum. Aims. We search for signs of period doubling in CoRoT RRLyrae stars. The occurrence of this dynamical effect in modulated RRLyrae stars might help us to gain more information about the mysterious Blazhko effect. The temporal variability of the additional frequencies in representatives of all subtypes of RRLyrae stars is also investigated. Methods. We preprocess CoRoT light curves by applying trend and jump correction and outlier removal. Standard Fourier technique is used to analyze the frequency content of our targets and follow the time-dependent phenomena. Results. The most comprehensive collection of CoRoT RRLyrae stars, including new discoveries is presented and analyzed. We found alternating maxima and in some cases half-integer frequencies in four CoRoT Blazhko RRLyrae stars, as clear signs of the presence of period doubling. This reinforces that period doubling is an important ingredient for understanding the Blazhko effect - a premise we derived previously from the Kepler RRLyrae sample. As expected, period doubling is detectable only for short time intervals in most modulated RRab stars. Our results show that the temporal variability of the additional frequencies in all RRLyrae subtypes is ubiquitous. The ephemeral nature and the highly variable amplitude of these variations suggest a complex underlying dynamics of and an intricate interplay between radial and possibly nonradial modes in RRLyrae stars. The omnipresence of additional modes in all types of RRLyrae - except in non-modulated RRab stars - implies that asteroseismology of these objects should be feasible in the near future. C1 [Szabo, R.; Benko, J. M.; Paparo, M.] Konkoly Observ Budapest, MTA CSFK, H-1121 Budapest, Hungary. [Chapellier, E.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR 7293, Observ Cote Azur, F-06300 Nice, France. [Poretti, E.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Baglin, A.] Univ Paris 07, Univ Paris 06, Observ Paris, LESIA, F-92195 Meudon, France. [Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolenberg, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Guggenberger, E.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. [Guggenberger, E.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Le Borgne, J. -F.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Le Borgne, J. -F.] CNRS, IRAP, F-31400 Toulouse, France. RP Szabo, R (reprint author), Konkoly Observ Budapest, MTA CSFK, Konkoly Thege Miklos Ut 15-14, H-1121 Budapest, Hungary. EM rszabo@konkoly.hu OI Poretti, Ennio/0000-0003-1200-0473; Szabo, Robert/0000-0002-3258-1909 FU ESA PECS [4000103541/11/NL/KML]; Hungarian OTKA [K83790]; European Community [312844, 269194]; ERC [338251]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Austrian Science Fonds [FWF P22691-N16] FX This research made use of the ExoDat database, operated at LAM-OAMP, Marseille, France, on behalf of the CoRoT/Exoplanet program. R.S.z., M. P., and J.M.B. acknowledge the support of the ESA PECS project No. 4000103541/11/NL/KML. This project has been supported by the Hungarian OTKA grant K83790 and the European Community's Seventh Framework Program (FP7/2007-2013) under grant agreements No. 312844 (SPACEINN), No. 269194 (IRSES/ASK) and ERC grant agreement No. 338251 (StellarAges). R.S.z. wishes to acknowledge the support from the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. W. W. was supported by the Austrian Science Fonds (FWF P22691-N16). The authors thank Akos Gyorffy, Peter Papics, and Laszlo Molnar for their help with the ground-based observations. NR 55 TC 17 Z9 17 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 OCT PY 2014 VL 570 AR A100 DI 10.1051/0004-6361/201424522 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3EE UT WOS:000344158500126 ER PT J AU Venuti, L Bouvier, J Flaccomio, E Alencar, SHP Irwin, J Stauffer, JR Cody, AM Teixeira, PS Sousa, AP Micela, G Cuillandre, JC Peres, G AF Venuti, L. Bouvier, J. Flaccomio, E. Alencar, S. H. P. Irwin, J. Stauffer, J. R. Cody, A. M. Teixeira, P. S. Sousa, A. P. Micela, G. Cuillandre, J. -C. Peres, G. TI Mapping accretion and its variability in the young open cluster NGC 2264: a study based on u-band photometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; stars: formation; stars: low-mass; stars: pre-main sequence; ultraviolet: stars; open clusters and associations: individual: NGC 2264 ID T-TAURI STARS; LOW-MASS STARS; DIGITAL SKY SURVEY; MAIN-SEQUENCE STARS; BROWN DWARFS; BOLOMETRIC CORRECTIONS; PROTOPLANETARY DISKS; SPITZER OBSERVATIONS; STELLAR OBJECTS; LIGHT CURVES AB Context. The accretion process has a central role in the formation of stars and planets. Aims. We aim at characterizing the accretion properties of several hundred members of the star-forming cluster NGC 2264 (3 Myr). Methods. We performed a deep ugri mapping as well as a simultaneous u-band+ r-band monitoring of the star-forming region with CFHT/MegaCam in order to directly probe the accretion process onto the star from UV excess measurements. Photometric properties and stellar parameters are determined homogeneously for about 750 monitored young objects, spanning the mass range similar to 0.1-2 M-circle dot. About 40% of the sample are classical (accreting) T Tauri stars, based on various diagnostics (H-alpha, UV and IR excesses). The remaining non-accreting members define the (photospheric + chromospheric) reference UV emission level over which flux excess is detected and measured. Results. We revise the membership status of cluster members based on UV accretion signatures, and report a new population of 50 classical T Tauri star (CTTS) candidates. A large range of UV excess is measured for the CTTS population, varying from a few times 0.1 to similar to 3 mag. We convert these values to accretion luminosities and accretion rates, via a phenomenological description of the accretion shock emission. We thus obtain mass accretion rates ranging from a few 10(-10) to similar to 10(-7) M-circle dot/yr. Taking into account a mass-dependent detection threshold for weakly accreting objects, we find a > 6 sigma correlation between mass accretion rate and stellar mass. A power-law fit, properly accounting for censored data (upper limits), yields. M-acc proportional to M-*(1.4+/-0.3). At any given stellar mass, we find a large spread of accretion rates, extending over about 2 orders of magnitude. The monitoring of the UV excess on a timescale of a couple of weeks indicates that its variability typically amounts to 0.5 dex, i.e., much smaller than the observed spread in accretion rates. We suggest that a non-negligible age spread across the star-forming region may effectively contribute to the observed spread in accretion rates at a given mass. In addition, different accretion mechanisms (like, e. g., short-lived accretion bursts vs. more stable funnel-flow accretion) may be associated to different. M-acc regimes. Conclusions. A huge variety of accretion properties is observed for young stellar objects in the NGC 2264 cluster. While a definite correlation seems to hold between mass accretion rate and stellar mass over the mass range probed here, the origin of the large intrinsic spread observed in mass accretion rates at any given mass remains to be explored. C1 [Venuti, L.; Bouvier, J.] Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. [Venuti, L.; Bouvier, J.] CNRS, IPAG, F-38000 Grenoble, France. [Venuti, L.; Peres, G.] Univ Palermo, Dipartimento Chim & Fis, I-90134 Palermo, Italy. [Flaccomio, E.; Micela, G.] Osservatorio Astron Palermo GS Vaiana, Ist Nazl Astrofis, I-90134 Palermo, Italy. [Alencar, S. H. P.; Sousa, A. P.] Univ Fed Minas Gerais, ICEx, Dept Fis, BR-30270901 Belo Horizonte, MG, Brazil. [Irwin, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stauffer, J. R.; Cody, A. M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Teixeira, P. S.] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Cuillandre, J. -C.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. RP Venuti, L (reprint author), Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France. EM Laura.Venuti@obs.ujf-grenoble.fr RI Alencar, Silvia/C-2803-2013; Teixeira, Paula Stella/O-2289-2013; OI Teixeira, Paula Stella/0000-0002-3665-5784; Micela, Giuseppina/0000-0002-9900-4751; Flaccomio, Ettore/0000-0002-3638-5788; PERES, Giovanni/0000-0002-6033-8180 FU CNPq; CAPES; Fapemig; [ANR 2011 Blanc SIMI5-6 020 01] FX We would like to thank Christian Veillet, former director of CFHT, for granting discretionary time to perform the mapping survey in December 2010, and the Terapix center at Institut d'Astrophysique de Paris, and in particular Yannick Mellier, for the prompt processing of the MegaCam images obtained during this run. We also thank Nadine Manset and Jim Thomas at CFHT for efficient run scheduling and data retrieval procedures. We warmly thank Luisa Rebull for retrieving for us the Lacc values she derived for her 2002 paper on disk-bearing objects in NGC 2264. We thank Kevin Covey for discussions on SDSS dwarf sequences and Lynne Hillenbrand for discussions on bolometric corrections scales; we also acknowledge useful discussion on the. Macc-M* relationship with Beate Stelzer. This publication makes use of data products from the Sloan Digital Sky Survey and the Two Micron All Sky Survey. This project was in part supported by the grant ANR 2011 Blanc SIMI5-6 020 01. S.H.P.A. and A.P.S. acknowledge support from CNPq, CAPES and Fapemig. NR 84 TC 21 Z9 21 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 OCT PY 2014 VL 570 AR A82 DI 10.1051/0004-6361/201423776 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AS3EE UT WOS:000344158500044 ER PT J AU Shik, JZ Schal, C Silverman, J AF Shik, J. Z. Schal, C. Silverman, J. TI Diet specialization in an extreme omnivore: nutritional regulation in glucose-averse German cockroaches SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE Blattella germanica; geometric framework; nutritional ecology ID BLATTELLA-GERMANICA; FOOD SELECTION; RESISTANCE; DICTYOPTERA; ECOLOGY; LOCUSTS; COMPENSATION; CARBOHYDRATE; BLATTODEA; IMBALANCE AB Organisms have diverse adaptations for balancing dietary nutrients, but often face trade-offs between ingesting nutrients and toxins in food. While extremely omnivorous cockroaches would seem excluded from such dietary trade-offs, German cockroaches (Blattella germanica) in multiple populations have rapidly evolved a unique dietary specialization - an aversion to glucose, the phagostimulant in toxic baits used for pest control. We used factorial feeding experiments within the geometric framework to test whether glucose-averse (GA) cockroaches with limited access to this critical metabolic fuel have compensatory behavioural and physiological strategies for meeting nutritional requirements. GA cockroaches had severely constrained intake, fat and N mass, and performance on glucose-based diets relative to wild-type (WT) cockroaches and did not appear to exhibit digestive strategies for retaining undereaten nutrients. However, a GA x WT hybrid' had lower glucose aversion than GA and greater access to macronutrients within glucose-based diets - while still having lower intake and survival than WT. Given these intermediate foraging constraints, hybrids may be a reservoir for this maladaptive trait in the absence of positive selection and may account for the rapid evolution of this trait following bait application. C1 [Shik, J. Z.; Schal, C.; Silverman, J.] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Shik, J. Z.] Smithsonian Trop Res Inst, Washington, Ancon, Panama. [Shik, J. Z.] Univ Copenhagen, Ctr Social Evolut, Dept Biol, DK-2100 Copenhagen, Denmark. RP Shik, JZ (reprint author), Univ Copenhagen, Ctr Social Evolut, Dept Biol, Univ Pk 15, DK-2100 Copenhagen, Denmark. EM jonathan.shik@gmail.com RI Schal, Coby/A-8717-2010 OI Schal, Coby/0000-0001-7195-6358 FU Blanton J. Whitmire endowment at North Carolina State University; U.S. Department of Housing and Urban Development [NCHHU0001-11] FX We thank S. Wood, A. Ko and R. Santangelo for help rearing cockroaches and setting up experiments. D. Raubenheimer provided valuable comments on an earlier draft. L. Lentz of the Soil Science Analytical Services Lab at NCSU performed elemental analyses, B. Willink and D. Nash provided statistical assistance, and D. Bednar provided assistance with fat extractions. This research was funded by the Blanton J. Whitmire endowment at North Carolina State University. CS was supported by a grant from the U.S. Department of Housing and Urban Development (NCHHU0001-11). The authors have no conflict of interest to declare. NR 36 TC 7 Z9 7 U1 1 U2 28 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 OCT PY 2014 VL 27 IS 10 BP 2096 EP 2105 DI 10.1111/jeb.12458 PG 10 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA AR9TT UT WOS:000343920900007 PM 25078384 ER PT J AU Thornberg, HM Culver, SJ Corbett, DR Mallinson, DJ Buzas, MA Shazili, NAM AF Thornberg, Hanna M. Culver, Stephen J. Corbett, D. Reide Mallinson, David J. Buzas, Martin A. Shazili, Noor A. M. TI THE INFLUENCE OF AQUACULTURE ON MODERN FORAMINIFERA AND SEDIMENTS IN THE SETIU ESTUARY AND LAGOON, TERENGGANU, MALAYSIA: A TEMPORAL INVESTIGATION SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID PEARL RIVER ESTUARY; ORGANIC-MATTER; BENTHIC FORAMINIFERA; FISH FARM; PB-210 GEOCHRONOLOGY; ISOTOPE RATIOS; CARBON FLOW; NITROGEN; MARINE; IMPACT AB Foraminiferal assemblages, sediments, and delta C-13, delta N-15, and C:N ratios are used to investigate how aquaculture in the Setiu estuarine-lagoonal system (SEL) in Terengganu, Malaysia has affected environmental quality since the mid-1970s. Three cores were collected beneath floating fish-cage sites, two (S43 and S40) from the lagoon and one (S9A) from the estuary. The delta C-13 and delta N-15 signatures of core sediment indicate terrestrial sources for organic matter, including mangrove vegetation, throughout the cores. Percent carbon, percent nitrogen, and percent mud increase up core throughout S43. In S40, a similar up-core increase reverses, possibly related to the northward migration of an inlet to a more proximal position. In core S9A a similar reversal in these measurements corresponds to recent abandonment of fish cages at this location. Foraminiferal assemblages in cores S43 and S40 are dominated by calcareous taxa, in particular Ammonia aff. A. aoteana and Rosalina globularis. Agglutinated specimens, particularly of Ammobaculites exiguus, increase in abundance near the top of S43 and S40, likely in response to an increase in organic matter. Core S9A contains only agglutinated foraminifera, with Trochammina amnicola, Ammotium directum, Am. exiguus, and Miliammina fusca as the most abundant species. Foraminiferal assemblages do not change at sharp boundaries between sand and mud units in S9A, where T. amnicola dominates assemblages throughout the core except in the uppermost 4 cm. This is likely due to taphonomic loss of the delicate M. fusca down core. The percent of live specimens is relatively low in all three cores. The densities of dead foraminifera at S43 and S40 are extremely high at the base of the cores (i.e., at the onset of aquaculture) and near the surface of S40. These high densities are attributed to a baffling effect created by the fish cages as tidal currents transport sediments northwards in the lagoon. Aquaculture has affected organic-matter content, sediment characteristics, and foraminiferal distributions in the SEL. However, rapid return (probably within one-three years) to pre-aquaculture conditions after the abandonment of S9A and a slower return to pre-aquaculture conditions in S40 suggest that environmental health of the SEL is not overly compromised by the current scale of floating fish-cage aquaculture, particularly where significant tidal flushing occurs. C1 [Thornberg, Hanna M.; Culver, Stephen J.; Corbett, D. Reide; Mallinson, David J.] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. [Corbett, D. Reide] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Shazili, Noor A. M.] Univ Malaysia Terengganu, Inst Oceanog, Kuala Terengganu 21030, Terengganu, Malaysia. RP Culver, SJ (reprint author), E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. EM culvers@ecu.edu FU Universiti Malaysia Terengganu (UMT); East Carolina University; UMT Institute of Oceanography FX We thank Universiti Malaysia Terengganu (UMT) and East Carolina University for funding this research, as well as Dr. Mohd Lokman Husain and the UMT Institute of Oceanography for support in the field. Dr. Peter Parham (UMT) provided input on the timing of inlet closure. Thanks to Alisha Ellis, David Young, Jaimi Flynn, and Megan Javonovich for help in the laboratory and to two anonymous reviewers for their efforts. Clive Jones provided access to the foraminiferal collection at The Natural History Museum, London, and John Whittaker provided valuable taxonomic advice. NR 110 TC 4 Z9 4 U1 2 U2 18 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2014 VL 44 IS 4 BP 365 EP 389 PG 25 WC Paleontology SC Paleontology GA AS7OE UT WOS:000344444300003 ER PT J AU Ellis, AM Culver, SJ Mallinson, DJ Corbett, DR Leorri, E Buzas, MA Shazili, NAM AF Ellis, Alisha M. Culver, Stephen J. Mallinson, David J. Corbett, D. Reide Leorri, Eduardo Buzas, Martin A. Shazili, Noor A. M. TI THE INFLUENCE OF AQUACULTURE ON MODERN FORAMINIFERA AND SEDIMENTS IN THE SETIU ESTUARY AND LAGOON, TERENGGANU, MALAYSIA: A SPATIAL INVESTIGATION SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID SEA-LEVEL RECONSTRUCTIONS; ORGANIC-MATTER; BENTHIC FORAMINIFERA; STABLE-ISOTOPES; BOLINAO AREA; OUTFALL AREA; CARBON FLOW; FISH FARMS; MARINE; IMPACT AB Foraminifera, grain size, and carbon and nitrogen isotope ratios and abundances were analyzed in surface-sediment samples collected from three floating fish-cage complexes to address how aquaculture has influenced the Setiu estuary and lagoon of northeast peninsular Malaysia. Two currently active floating fish-cage complexes, SET11-S43 and SET11-S40, are located in the semi-enclosed Setiu lagoon, within four km of an inlet connecting to the South China Sea. The sampling areas experience salinities in the 20s, and sediments have mixed agglutinated and calcareous foraminiferal [total] assemblages, generally dominated by Ammonia aff. A. aoteana and Ammobaculites exiguus. The majority of live foraminifera at these sites belong to agglutinated species; percent of live specimens is greater around the SET11-S43 fish-cage complex, likely related to the presence of aquaculture-related organic-rich mud. Percent agglutinated specimens in total assemblages (live + dead) decrease towards the inlet as total assemblage density and diversity increase due to increased salinity. At a recently (1-3 years) abandoned fish-cage complex, SET11-S9A, located in a low salinity (<5) estuarine setting, Miliammina fusca and Am. exiguus dominate total assemblages. Surface-sediment grain-size data indicate that fish-cage-related organic-rich mud underlies SET11-S43 and extends tens of meters to the north with a surrounding sandier substrate, typical of most of the Setiu estuary and lagoon system. SET11-S40 is underlain by generally sandy sediment; organic-rich mud characterizes the lagoon immediately to the north of this fish-cage complex. Percent carbon and nitrogen in sediment exhibit distributional patterns that strongly correlate with the distribution of fish-cage mud. Greater amounts of mud, carbon, and nitrogen in sediment are found to the north of the active lagoonal fish-cage complexes. The delta C-13 and delta N-15 signatures of the organic matter in this area are attributed to input from the surrounding mangrove forest, whereas their distribution is a result of the interaction of tidal currents with the physical presence of fish-farm complexes. The environmental influence of the active fish cages at lagoonal site SET11-S40 is minimal as a result of the flushing effects of tidal currents from a nearby inlet. Further north at the SET11-S43 lagoonal fish-cage complex, which receives less marine influence (lower salinity and reduced tidal currents), organic-rich mud has accumulated beneath and to the north of the complex. Foraminiferal and sedimentological data from abandoned estuarine fish-farm complex SET11-S9A are indistinguishable from those of adjacent estuarine sites indicating a rapid return to pre-fish-farm conditions following abandonment. C1 [Ellis, Alisha M.; Culver, Stephen J.; Mallinson, David J.; Corbett, D. Reide; Leorri, Eduardo] E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. [Corbett, D. Reide] E Carolina Univ, Inst Coastal Sci & Policy, Greenville, NC 27858 USA. [Corbett, D. Reide] Univ N Carolina, Inst Coastal Studies, Manteo, NC 27954 USA. [Buzas, Martin A.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Shazili, Noor A. M.] Univ Malaysia Terengganu, Inst Oceanog, Kuala Terengganu 21030, Terengganu, Malaysia. RP Culver, SJ (reprint author), E Carolina Univ, Dept Geol Sci, Greenville, NC 27858 USA. EM culvers@ecu.edu RI Leorri, Eduardo/B-4805-2010 OI Leorri, Eduardo/0000-0002-7475-6279 FU Universiti Malaysia Terengganu (UMT); East Carolina University FX We thank Universiti Malaysia Terengganu (UMT) and East Carolina University for funding this research and Dr. Mohd Lokman Husain and the UMT Institute of Oceanography (INOS) staff, Hanna Thornberg, Jaimi Flynn, and Megan Javonovich, for support in the field and laboratory. Clive Jones provided access to the foraminiferal collection at The Natural History Museum, London, and John Whittaker provided valuable taxonomic advice. NR 98 TC 4 Z9 4 U1 2 U2 10 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2014 VL 44 IS 4 BP 390 EP 415 PG 26 WC Paleontology SC Paleontology GA AS7OE UT WOS:000344444300004 ER PT J AU McCoy, T AF McCoy, Tim TI 2014 Service Award for Roy. S. Clarke Award SO METEORITICS & PLANETARY SCIENCE LA English DT Biographical-Item C1 Smithsonian Inst, Washington, DC 20560 USA. RP McCoy, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 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 OCT PY 2014 VL 49 IS 10 BP 1984 EP 1985 DI 10.1111/maps.12378 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AS0MT UT WOS:000343972000017 ER PT J AU Avalos-Tellez, R Ramirez-Pfeiffer, C Hernandez-Castro, R Diaz-Aparicio, E Sanchez-Dominguez, C Zavala-Norzagaray, A Arellano-Reynoso, B Suarez-Guemes, F Aguirre, AA Aurioles-Gamboa, D AF Avalos-Tellez, Rosalia Ramirez-Pfeiffer, Carlos Hernandez-Castro, Rigoberto Diaz-Aparicio, Efren Sanchez-Dominguez, Carlos Zavala-Norzagaray, Alan Arellano-Reynoso, Beatriz Suarez-Gueemes, Francisco Aguirre, A. Alonso Aurioles-Gamboa, David TI Infection of California sea lions (Zalophus californianus) with terrestrial Brucella spp. SO VETERINARY JOURNAL LA English DT Article DE California sea lion; Brucella spp.; Agar gel immunodiffusion; Fluorescence polarization; PCR; Rose Bengal test ID MARINE MAMMALS; EXPOSURE AB Infections with Brucella ceti and pinnipedialis are prevalent in marine mammals worldwide. A total of 22 California sea lions (Zalophus californianus) were examined to determine their exposure to Brucella spp. at San Esteban Island in the Gulf of California, Mexico, in June and July 2011. Although samples of blood, vaginal mucus and milk cultured negative for these bacteria, the application of rose Bengal, agar gel immunodiffusion, PCR and modified fluorescence polarization assays found that five animals (22.7%) had evidence of exposure to Brucella strains. The data also suggested that in two of these five sea lions the strains involved were of terrestrial origin, a novel finding in marine mammals. Further work will be required to validate and determine the epidemiological significance of this finding. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Avalos-Tellez, Rosalia; Arellano-Reynoso, Beatriz; Suarez-Gueemes, Francisco] Univ Nacl Autonoma Mexico, Fac Med Vet & Zootecnia, Dept Microbiol & Immunol, Coyoacan 04510, Mexico. [Ramirez-Pfeiffer, Carlos] Inst Nacl Invest Forestales & Agr Rio Bravo, Campo Expt Rio Bravo, Tam 88900, Mexico. [Hernandez-Castro, Rigoberto] Hosp Gen Dr Manuel Gea Gonzalez, Direcc Invest, Tlalpan 14080, Mexico. [Diaz-Aparicio, Efren] Inst Nacl Invest Forestales & Agr, Ctr Nacl Invest Disciplinarias Microbiol Anim, Cuajimalpa 05110, Mexico. [Sanchez-Dominguez, Carlos] Chicago Zool Soc Brookfield Zoo, Chicago, IL 60513 USA. [Zavala-Norzagaray, Alan] Inst Politecn Nacl, Ctr Interdisciplinario Invest Desarroll Integral, Unidad Guasave, Sin 81101, Mexico. [Aguirre, A. Alonso] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Aguirre, A. Alonso] Smithsonian Mason Sch Conservat, Front Royal, VA 22630 USA. [Aurioles-Gamboa, David] Inst Politecn Nacl, Ctr Interdisciplinario Ciencias Marinas, La Paz 23096, Baja California, Mexico. RP Ramirez-Pfeiffer, C (reprint author), Univ Mexico Amer Norte AC, Reynosa 88630, Tam, Mexico. EM carlosrami@gmail.com FU REDMA-IPN - Estado de Salud, 'Uso Sustentable y Conservacion del Golfo de California'; EcoHealth Alliance; Marisla Foundation; Panaphil Foundation; [SIP-20120061] FX This study was supported by REDMA-IPN - Estado de Salud, 'Uso Sustentable y Conservacion del Golfo de California', and SIP-20120061 granted to D.A.G. We thank the crew of the Francisco de Ulloa Research Vessel for their support, and Dr. Daniel Ortega-Ochoa from Megafarma S.A. de C.V., for kindly supplying the Brucella abortus FPA test kit. In addition, we acknowledge the financial support of EcoHealth Alliance, and both the Marisla and Panaphil Foundations. Furthermore, we are grateful to Dr. Ricardo Gomez-Flores for his help in revising the manuscript. NR 12 TC 0 Z9 0 U1 1 U2 20 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1090-0233 EI 1532-2971 J9 VET J JI Vet. J. PD OCT PY 2014 VL 202 IS 1 BP 198 EP 200 DI 10.1016/j.tvjl.2014.06.021 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA AS3YR UT WOS:000344211500038 PM 25066000 ER PT J AU Sherman-Broyles, S Bombarely, A Powell, AF Doyle, JL Egan, AN Coate, JE Doyle, JJ AF Sherman-Broyles, Sue Bombarely, Aureliano Powell, Adrian F. Doyle, Jane L. Egan, Ashley N. Coate, Jeremy E. Doyle, Jeff J. TI THE WILD SIDE OF A MAJOR CROP: SOYBEAN'S PERENNIAL COUSINS FROM DOWN UNDER SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Fabaceae; genome-wide variation; Glycine; Glycine max; photosynthesis; polyploidy; phylogenetics; nodulation; soybean ID GLYCINE SUBGENUS GLYCINE; MAX L. MERR.; CHLOROPLAST DNA POLYMORPHISM; RUST PHAKOPSORA-PACHYRHIZI; GENUS GLYCINE; GENETIC DIVERSITY; TOMENTELLA LEGUMINOSAE; POPULATION-STRUCTURE; POLYPLOID COMPLEX; DUPLICATED GENES AB The accumulation of over 30 years of basic research on the biology, genetic variation, and evolution of the wild perennial relatives of soybean (Glycine max) provides a foundation to improve cultivated soybean. The cultivated soybean and its wild progenitor, G. soja, have a center of origin in eastern Asia and are the only two species in the annual subgenus Soja. Systematic and evolutionary studies of the ca. 30 perennial species of subgenus Glycine, native to Australia, have benefited from the availability of the G. max genomic sequence. The perennial species harbor many traits of interest to soybean breeders, among them resistance to major soybean pathogens such as cyst nematode and leaf rust. New species in the Australian subgenus continue to be described, due to the collection of new material and to insights gleaned through systematic studies of accessions in germplasm collections. Ongoing studies in perennial species focus on genomic regions that contain genes for key traits relevant to soybean breeding. These comparisons also include the homoeologous regions that are the result of polyploidy in the common ancestor of all Glycine species. Subgenus Glycine includes a complex of recently formed allopolyploids that are the focus of studies aimed at elucidating genomic, transcriptomic, physiological, taxonomic, morphological, developmental, and ecological processes related to polyploid evolution. Here we review what has been learned over the past 30 years and outline ongoing work on photosynthesis, nitrogen fixation, and floral biology, much of it drawing on new technologies and resources. C1 [Sherman-Broyles, Sue; Bombarely, Aureliano; Powell, Adrian F.; Doyle, Jane L.; Doyle, Jeff J.] Cornell Univ, Ithaca, NY 14853 USA. [Egan, Ashley N.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. [Coate, Jeremy E.] Reed Coll, Dept Biol, Portland, OR 97202 USA. RP Sherman-Broyles, S (reprint author), Cornell Univ, 412 Mann Lib Bldg, Ithaca, NY 14853 USA. EM sls98@cornell.edu RI Bombarely, Aureliano/C-6580-2009 OI Bombarely, Aureliano/0000-0001-6257-8914 FU U. S. National Science Foundation [1257522]; SoyMap2 project [0822258] FX The authors thank E. Peregrine at USDA and our long-time collaborator A. H. D. Brown (CSIRO), who has been instrumental in most of our work on Glycine. Several grants from the U. S. National Science Foundation have supported the authors' research on Glycine over many years, currently 1257522 and the SoyMap2 project (0822258), whose PIs (S. Jackson, J. Schmutz, P. Cregan, and R. Shoemaker) we also thank. NR 177 TC 7 Z9 7 U1 3 U2 46 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 EI 1537-2197 J9 AM J BOT JI Am. J. Bot. PD OCT PY 2014 VL 101 IS 10 BP 1651 EP 1665 DI 10.3732/ajb.1400121 PG 15 WC Plant Sciences SC Plant Sciences GA AS1BD UT WOS:000344010400008 PM 25326613 ER PT J AU Moree, WJ McConnell, OJ Nguyen, DD Sanchez, LM Yang, YL Zhao, XL Liu, WT Boudreau, PD Srinivasan, J Atencio, L Ballesteros, J Gavilan, RG Torres-Mendoza, D Guzman, HM Gerwick, WH Gutierrez, M Dorrestein, PC AF Moree, Wilna J. McConnell, Oliver J. Nguyen, Don D. Sanchez, Laura M. Yang, Yu-Liang Zhao, Xiling Liu, Wei-Ting Boudreau, Paul D. Srinivasan, Jayashree Atencio, Librada Ballesteros, Javier Gavilan, Ronnie G. Torres-Mendoza, Daniel Guzman, Hector M. Gerwick, William H. Gutierrez, Marcelino Dorrestein, Pieter C. TI Microbiota of Healthy Corals Are Active against Fungi in a Light-Dependent Manner SO ACS CHEMICAL BIOLOGY LA English DT Article ID IMAGING MASS-SPECTROMETRY; PSEUDOALTEROMONAS; DESTRUCTANS; REVISION; GEOMYCES; PACIFIC; AMERICA AB Coral reefs are intricate ecosystems that harbor diverse organisms, including 25% of all marine fish. Healthy corals exhibit a complex symbiosis between coral polyps, endosymbiotic alga, and an array of microorganisms, called the coral holobiont. Secretion of specialized metabolites by coral microbiota is thought to contribute to the defense of this sessile organism against harmful biotic and abiotic factors. While few causative agents of coral diseases have been unequivocally identified, fungi have been implicated in the massive destruction of some soft corals worldwide. Because corals are nocturnal feeders, they may be more vulnerable to fungal infection at night, and we hypothesized that the coral microbiota would have the capability to enhance their defenses against fungi in the dark. A Pseudoalteromonas sp. isolated from a healthy octocoral displayed light-dependent antifungal properties when grown adjacent to Penicillium citrinum (P. citrinum) isolated from a diseased Gorgonian octocoral. Microbial MALDI-imaging mass spectrometry (IMS) coupled with molecular network analyses revealed that Pseudoalteromonas produced higher levels of antifungal polyketide alteramides in the dark than in the light. The alteramides were inactivated by light through a photoinduced intramolecular cyclization. Further NMR studies led to a revision of the stereochemical structure of the alteramides. Alteramide A exhibited antifungal properties and elicited changes in fungal metabolite distributions of mycotoxin citrinin and citrinadins. These data support the hypothesis that coral microbiota use abiotic factors such as light to regulate the production of metabolites with specialized functions to combat opportunistic pathogens at night. C1 [Moree, Wilna J.; McConnell, Oliver J.; Sanchez, Laura M.; Gerwick, William H.; Dorrestein, Pieter C.] Univ Calif San Diego, Scripps Inst Oceanog, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92903 USA. [Nguyen, Don D.; Zhao, Xiling; Liu, Wei-Ting; Dorrestein, Pieter C.] Univ Calif San Diego, Scripps Inst Oceanog, Dept Chem & Biochem, La Jolla, CA 92903 USA. [McConnell, Oliver J.; Boudreau, Paul D.; Gerwick, William H.; Dorrestein, Pieter C.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92903 USA. [Yang, Yu-Liang] Acad Sinica, Agr Biotechnol Res Ctr, Taipei 115, Taiwan. [Atencio, Librada; Ballesteros, Javier; Gavilan, Ronnie G.; Torres-Mendoza, Daniel; Gutierrez, Marcelino] Inst Invest Cient & Serv Alta Tecnol INDICASAT, Ciudad Del Saber 084301103, Clayton, Panama. [Gavilan, Ronnie G.] Natl Inst Hlth, Natl Ctr Publ Hlth, Lima 11, Peru. [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Gutierrez, M (reprint author), Inst Invest Cient & Serv Alta Tecnol INDICASAT, Ciudad Del Saber 084301103, Clayton, Panama. EM mgutierrez@indicasat.org.pa; pdorrestein@ucsd.edu OI Torres-Mendoza, Daniel/0000-0002-3540-4238; Sanchez, Laura/0000-0001-9223-7977 FU NIH Fogarty International Center International Cooperative Biodiversity Groups program [TW006634]; Government of Panama SENACYT [COL09-047, COL08-061]; National Institutes of Health IRACDA [K12 GM068524]; [NIHAI095125]; [S10RR029121] FX We thank the laboratories of W. Nierman (JCVI) and P. Jensen (UCSD) for donating the fungal strains. We appreciate the assistance of R. Simkovsky and S. Cohen in the S. Golden lab (UCSD) with the light incubators. S. Mascuch kindly provided the MS/MS spectra of the standard desferrichrome. We acknowledge the Government of Panama (ANAM, ARAP) for granting permissions to make the collections of the corals and Carlos Guevara for field assistance. This work was supported by NIHAI095125 and S10RR029121, by the NIH Fogarty International Center International Cooperative Biodiversity Groups program TW006634, by the Government of Panama SENACYT COL09-047 and COL08-061, and by National Institutes of Health IRACDA K12 GM068524 grant award (L.M.S.). NR 41 TC 9 Z9 9 U1 3 U2 24 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1554-8929 EI 1554-8937 J9 ACS CHEM BIOL JI ACS Chem. Biol. PD OCT PY 2014 VL 9 IS 10 BP 2300 EP 2308 DI 10.1021/cb500432j PG 9 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA AR3ZD UT WOS:000343526900018 PM 25058318 ER PT J AU Kaiser, SA Sillett, TS Webster, MS AF Kaiser, Sara A. Sillett, T. Scott Webster, Michael S. TI Phenotypic plasticity in hormonal and behavioural responses to changes in resource conditions in a migratory songbird SO ANIMAL BEHAVIOUR LA English DT Article DE behavioural plasticity; breeding condition; environmental change; food supplementation; glucocorticoid; mating effort; parental effort; reproductive trade-off; resource allocation; testosterone ID THROATED BLUE WARBLERS; STARLINGS STURNUS-VULGARIS; PLASMA TESTOSTERONE LEVELS; BASE-LINE; ENVIRONMENTAL-CHANGE; NATURAL VARIATION; LIFE-HISTORIES; CLIMATE-CHANGE; AVIAN PLASMA; CHALLENGE HYPOTHESIS AB An emerging question in animal behaviour is whether and how behavioural plasticity will enable organisms to adjust to human-induced, rapid environmental changes that affect breeding conditions. Adaptive behavioural plasticity in response to changing resource conditions will depend on the sensitivity of the neuroendocrine system to food stimuli and on constraints in the mechanisms mediating the expression of reproductive behaviours. We tested the hypotheses that food availability mediates plasticity in androgen and corticosterone (CORT) responses, and that circulating concentrations of these hormones in turn mediate investment into competing mating and parental behaviours in a migratory songbird. We provided supplemental food to black-throated blue warblers, Setophaga caerulescens, breeding in habitats with natural low and high food abundance. The effects of supplemental feeding were most pronounced in food-poor habitat. During their social mates' fertile stage, fed males sang less near their nest sites, had lower plasma androgen and CORT levels, and had higher residual mass than control males. Fed males benefited indirectly from their mates' access to supplemental food because fed females provided more parental effort than control females. Fed males did not increase their own parental effort. Our results suggest that fed males increased mate-guarding effort over extrapair mate attraction while their social mates were fertile and invested additional resources into territorial defence or self-maintenance during the parental stage. These findings reveal plastic patterns of covariation among endocrine parameters and mating behaviours, but not parental behaviours, in response to food supplementation. These responses enabled individuals to adjust their reproductive effort rapidly to changes in resource conditions. Our findings suggest that adaptive reproductive investment in response to environmental change is unlikely to be constrained by the hormonal mechanisms underlying the mediation of competing mating and parental behaviours. (C) 2014 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Kaiser, Sara A.; Webster, Michael S.] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. [Kaiser, Sara A.; Webster, Michael S.] Cornell Lab Ornithol, Macaulay Lib, Ithaca, NY 14850 USA. [Sillett, T. Scott] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. RP Kaiser, SA (reprint author), Cornell Lab Ornithol, 159 Sapsucker Woods Rd, Ithaca, NY 14850 USA. EM sak275@cornell.edu FU U.S. National Science Foundation (NSF) [0640732, 1242563]; U.S. Environmental Protection Agency; Smithsonian Institution; Animal Behavior Society; Sigma Xi; American Ornithologists' Union; Wilson Ornithological Society; Cornell Lab of Ornithology; Neurobiology and Behavior Department at Cornell University; Department of Biological Sciences at Washington State University; Achievement Rewards for College Scientists Foundation; U.S. National Science Foundation FX This research was supported by U.S. National Science Foundation grants awarded to Cornell University, the Smithsonian Institution and Wellesley College (NSF grant numbers 0640732 and 1242563), by fellowships and grants awarded to S.A.K. from the U.S. Environmental Protection Agency, the Smithsonian Institution, the Animal Behavior Society, Sigma Xi, the American Ornithologists' Union, Wilson Ornithological Society, the Cornell Lab of Ornithology and its donors, the Neurobiology and Behavior Department at Cornell University, the Department of Biological Sciences at Washington State University and the Achievement Rewards for College Scientists Foundation. We thank B. Hansen for conducting hormone assays at the Cornell Veterinary College, N. Place for technical advice on assays and L. Nietmann for conducting song analyses. We thank E. Adkins-Regan, D. Winkler, M. Vitousek, T. Wright and two anonymous referees for comments that greatly improved this manuscript. We are especially grateful to the undergraduates and field technicians who participated in this study and to our collaborators, R.T. Holmes and N.L. Rodenhouse, for their valuable guidance and support. This manuscript is a contribution of the Hubbard Brook Ecosystem Study. Hubbard Brook is part of the Long-Term Ecological Research (LTER) network, which is supported by the U.S. National Science Foundation. The Hubbard Brook Experimental Forest is operated and maintained by the U.S. Department of Agriculture Forest Service, Northern Research Station, Newtown Square, PA, U.S.A. NR 88 TC 4 Z9 4 U1 6 U2 72 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD OCT PY 2014 VL 96 BP 19 EP 29 DI 10.1016/j.anbehav.2014.07.004 PG 11 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA AR2LC UT WOS:000343416500005 ER PT J AU Suselbeek, L Adamczyk, VMAP Bongers, F Nolet, BA Prins, HHT van Wieren, SE Jansen, PA AF Suselbeek, Lennart Adamczyk, Vena M. A. P. Bongers, Frans Nolet, Bart A. Prins, Herbert H. T. van Wieren, Sipke E. Jansen, Patrick A. TI Scatter hoarding and cache pilferage by superior competitors: an experiment with wild boar, Sus scrofa SO ANIMAL BEHAVIOUR LA English DT Article DE acorns; cache defence; caching; competition; oaks; olfaction; rodents; seed dispersal; seeds; theft ID OPTIMAL-DENSITY MODEL; DIPODOMYS-MERRIAMI; KANGAROO RATS; ENVIRONMENTAL-CONDITIONS; ACORN DISPERSAL; RED SQUIRREL; WOOD MICE; SEED; BEHAVIOR; RODENTS AB Food-hoarding patterns range between larder hoarding (a few large caches) and scatter hoarding (many small caches), and are, in essence, the outcome of a hoard size-number trade-off in pilferage risk. Animals that scatter hoard are believed to do so, despite higher costs, to reduce loss of cached food to competitors against which they cannot defend their food reserves (henceforth: superior competitors). We tested the underlying assumption that the cost of having more caches under scatter hoarding, thus increasing the likelihood of cache encounter by superior competitors, is outweighed by the benefit of having small caches that are less likely to be detected upon encounter by superior competitors. We carried out a controlled experiment in which we distributed a fixed number of acorns over a fixed number of patches within a fixed area, varying cache size and cache depth, thus mimicking alternative hoarding patterns. We then recorded cache pilferage by a fixed number of wild boar, a well-known pilferer of acorn caches. The time wild boar needed to pilfer the first cache was shortest for scatter hoarding, but the time needed to pilfer all caches was slightly longer for scatter hoarding than for larder hoarding. Overall, however, the rate of pilferage did not differ between scatter hoarding and larder hoarding, and was not affected by cache depth. We conclude that the effects of alternative hoarding patterns on reducing cache pilferage by wild boar were smaller than expected, and that superior competitors may thus not be important drivers of scatter hoarding. Instead, other factors, such as conspecific pilferage or the risk of cross-contamination of food items in large caches, which can also cause catastrophic loss of food reserves, may be more important drivers of scatter hoarding. (C) 2014 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Suselbeek, Lennart; Adamczyk, Vena M. A. P.; Bongers, Frans; Prins, Herbert H. T.; van Wieren, Sipke E.; Jansen, Patrick A.] Univ Wageningen & Res Ctr, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Nolet, Bart A.] Netherlands Inst Ecol NIOO KNAW, Dept Anim Ecol, Wageningen, Netherlands. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Suselbeek, L (reprint author), Univ Wageningen & Res Ctr, Dept Environm Sci, POB 47, NL-6700 AA Wageningen, Netherlands. EM lennart.suselbeek@wur.nl RI Library, Library/A-4320-2012; Nolet, Bart/C-1416-2008; Jansen, Patrick/G-2545-2015; OI Library, Library/0000-0002-3835-159X; Nolet, Bart/0000-0002-7437-4879; Jansen, Patrick/0000-0002-4660-0314; Suselbeek, Lennart/0000-0002-1896-855X FU Netherlands Organisation for Scientific Research [NWO-ALW08056] FX We thank Hans Rosenberg, Gerwin de Vries, Rini van der Weele, Soerin Binda, Marcel van Seventer, Marinde Out, Cher Adamczyk, Jasper Klomp and Marijke Runtuwene for assistance; Geert Groot Bruinderink, Jan den Ouden and Frank van Langevelde for comments; the Stichting Flevolandschap for providing the wild boar; the employees of the experimental animal facility 'De Haar' in Wageningen for help with experimental set-up and animal care; Simon Delany for native English editing; two anonymous referees and the editor for useful comments and suggestions for improvement. This study was funded by the Netherlands Organisation for Scientific Research (NWO-ALW08056). This is publication 5635 of the Netherlands Institute of Ecology. All authors conceived and designed the experiments. L.S. and V.M.A.P.A. performed the experiments. L.S., V.M.A.P.A. and P.A.J. analysed the data. L.S., V.M.A.P.A. and P.A.J. wrote the manuscript; other authors provided editorial advice. NR 76 TC 2 Z9 2 U1 9 U2 39 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD OCT PY 2014 VL 96 BP 107 EP 115 DI 10.1016/j.anbehav.2014.08.001 PG 9 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA AR2LC UT WOS:000343416500014 ER PT J AU Knornschild, M AF Knoernschild, Mirjam TI Vocal production learning in bats SO CURRENT OPINION IN NEUROBIOLOGY LA English DT Article ID SPEAR-NOSED BATS; SAC-WINGED BAT; PHYLLOSTOMUS-DISCOLOR; SACCOPTERYX-BILINEATA; PIPISTRELLUS-NATHUSII; ECHOLOCATION CALLS; FEEDBACK-CONTROL; AUDITORY-CORTEX; COMMUNICATION; SPEECH AB Echo locating bats exhibit excellent control over their acoustic signals emitted and skillfully interpret the returning echoes, allowing orientation and foraging in complete darkness. Echolocation may be a preadaptation for sophisticated vocal communication with conspecifics and, ultimately, vocal learning processes. In humans, the importance of auditory input for correct speech acquisition is obvious, whereas vocal production learning is rare and patchily distributed among non-human mammals. Bats comprise one of the few mammalian taxa capable of. vocal production learning, with current behavioral evidence for three species belonging to two families; more evidence will probably forthcoming. The taxon's speciose nature makes bats well suited for phylogenetically controlled, comparative studies on proximate and ultimate mechanisms of mammalian vocal production learning. C1 [Knoernschild, Mirjam] Univ Ulm, Inst Expt Ecol, Fac Nat Sci, D-89069 Ulm, Germany. [Knoernschild, Mirjam] Smithsonian Trop Res Inst, Balboa, Panama. RP Knornschild, M (reprint author), Univ Ulm, Inst Expt Ecol, Fac Nat Sci, D-89069 Ulm, Germany. EM mirjam.knoernschild@uni-ulm.de FU German Baden-Wurttemberg Stiftung, Eliteprogramme for Postdocs FX I am indebted to the German Baden-Wurttemberg Stiftung, Eliteprogramme for Postdocs, for the financial support of my research. In addition, I thank M. Metz, M. Nagy, H.-U. Schnitzler and G. Jones for fruitful discussions, and T. Fitch for critical comments on the manuscript. NR 61 TC 15 Z9 15 U1 9 U2 65 PU CURRENT BIOLOGY LTD PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0959-4388 EI 1873-6882 J9 CURR OPIN NEUROBIOL JI Curr. Opin. Neurobiol. PD OCT PY 2014 VL 28 BP 80 EP 85 DI 10.1016/j.conb.2014.06.014 PG 6 WC Neurosciences SC Neurosciences & Neurology GA AR1RT UT WOS:000343363000015 PM 25050812 ER PT J AU Ihle, KE Baker, NA Amdam, GV AF Ihle, Kate E. Baker, Nicholas A. Amdam, Gro V. TI Insulin-like peptide response to nutritional input in honey bee workers SO JOURNAL OF INSECT PHYSIOLOGY LA English DT Article DE Apis mellifera; Nutritional homeostasis; Insulin/insulin-like signaling ID APIS-MELLIFERA L.; DROSOPHILA-MELANOGASTER; FORAGING BEHAVIOR; PROTEIN-LEVELS; POLLEN; DIET; HYMENOPTERA; COLONIES; EXPRESSION; GENOTYPE AB The rise in metabolic disorders in the past decades has heightened focus on achieving a healthy dietary balance in humans. This is also an increasingly important issue in the management of honey bees (Apis mellifera) where poor nutrition has negative effects on health and productivity in agriculture, and nutrition is suggested as a contributing factor in the recent global declines in honey bee populations. As in other organisms, the insulin/insulin-like signaling (IIS) pathway is likely involved in maintaining nutrient homeostasis in honey bees. Honey bees have two insulin-like peptides (Ilps) with differing spatial expression patterns in the fat body suggesting that AmIlp1 potentially functions in lipid metabolism while AmIlp2 is a more general indicator of nutritional status. We fed caged worker bees artificial diets high in carbohydrates, proteins or lipids and measured expression of AmIlp1, AmIlp2, and the insulin receptor substrate (IRS) to test their responses to dietary macronutrients. We also measured lifespan, worker weight and gustatory sensitivity to sugar as measures of individual physical condition. We found that expression of AmIlp1 was affected by diet composition and was highest on a diet high in protein. Expression of AmIlp2 and AmIRS were not affected by diet. Workers lived longest on a diet high in carbohydrates and low in protein and lipids. However, bees fed this diet weighed less than those that received a diet high in protein and low in carbohydrates and lipids. Bees fed the high carbohydrates diet were also more responsive to sugar, potentially indicating greater levels of hunger. These results support a role for AmIlp1 in nutritional homeostasis and provide new insight into how unbalanced diets impact individual honey bee health. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Ihle, Kate E.; Baker, Nicholas A.; Amdam, Gro V.] Arizona State Univ, Sch Life Sci, Tempe, AZ USA. [Ihle, Kate E.] Smithsonian Trop Res Inst, Panama City, Panama. [Amdam, Gro V.] Norwegian Univ Life Sci, Dept Chem Biotechnol & Food Sci, As, Norway. RP Ihle, KE (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM kateihle@gmail.com FU Arizona State University; Smithsonian Tropical Research Institution; Research Council of Norway [216776/F11, 213976, 191699]; PEW Charitable Trust FX K.E.I. was supported by a postdoctoral fellowship from Arizona State University and the Smithsonian Tropical Research Institution and The Research Council of Norway (216776/F11). G.V.A. was supported by the PEW Charitable Trust and the Research Council of Norway (213976, 191699). NR 56 TC 5 Z9 5 U1 5 U2 24 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-1910 EI 1879-1611 J9 J INSECT PHYSIOL JI J. Insect Physiol. PD OCT PY 2014 VL 69 BP 49 EP 55 DI 10.1016/j.jinsphys.2014.05.026 PG 7 WC Entomology; Physiology; Zoology SC Entomology; Physiology; Zoology GA AR1JJ UT WOS:000343341200008 PM 24952326 ER PT J AU Post, JE Heaney, PJ AF Post, Jeffrey E. Heaney, Peter J. TI Time-resolved synchrotron X-ray diffraction study of the dehydration behavior of chalcophanite SO AMERICAN MINERALOGIST LA English DT Article DE Chalcophanite; hetaerolite; birnessite; Rietveld; synchrotron ID SYNTHETIC NA-BIRNESSITE; RIETVELD REFINEMENT; POWDER DIFFRACTION; CRYSTAL-STRUCTURE; HEXAGONAL-BIRNESSITE; MANGANESE; EXCHANGE; ZNMN3O7.3H2O; PARAMETERS AB Time-resolved synchrotron X-ray powder diffraction data were used to investigate the dehydration behavior of the chalcophanite (ZnMn3O7 center dot 3H(2)O) structure from 300 to 1060 K. Rietveld refinements revealed two obvious phase changes, at similar to 450 and similar to 950 K, corresponding to the dehydration of chalcophanite followed by transformation to a spinel structure (Mn-hetaerolite). Only small changes were observed in the chalcophanite unit cell from RT to similar to 438 K; the volume increased by similar to 0.8%, mostly caused by thermal expansion of similar to 0.5% along c. Above similar to 427 K, the interlayer water molecules were lost, resulting in a collapse of the interlayer spacing from similar to 7 to similar to 4.8 angstrom. The newly formed anhydrous phase (ZnMn3O7) retained chalcophanite's R (3) over bar space group and a dimension, but the c dimension decreased from similar to 21 to 14.3 angstrom, and the Zn coordination changed from octahedral to tetrahedral. Above similar to 775 K the anhydrous chalcophanite began to transform to a spinel structure, corresponding to a Mn-rich hetaerolite [(Zn0.75Mn0.252+)Mn23+O4]. By similar to 973 K the transformation was complete. The diffraction patterns did not show a significant increase in background during the transformation, indicating that the reaction did not involve transient amorphization. The phase change was likely triggered by loss of 1.25 of seven O atoms in the original anhydrous chalcophanite structure with a corresponding reduction of Mn4+ to Mn3+ and Mn2+. C1 [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Post, JE (reprint author), Smithsonian Inst, Dept Mineral Sci, POB 37012, Washington, DC 20013 USA. EM postj@si.edu FU NSF [EAR07-45374, EAR11-47728]; U.S. Department of Energy, Division of Materials Sciences and Division of Chemical Sciences [DE-AC02-98CH10886] FX Funding for this research was provided by NSF grants EAR07-45374 and EAR11-47728. Thanks go to Jonathan Hanson of the Brookhaven National Lab for his assistance with the diffraction experiments at beamline X7B at the NSLS. We are grateful for the very helpful comments from two anonymous reviewers and the assistance of associate editor Aaron Celestian. This research was carried out at the National Synchrotron Light Source, Brookhaven National Laboratory, which is supported by the U.S. Department of Energy, Division of Materials Sciences and Division of Chemical Sciences, under Contract No. DE-AC02-98CH10886. NR 34 TC 2 Z9 2 U1 0 U2 15 PU MINERALOGICAL SOC AMER PI CHANTILLY PA 3635 CONCORDE PKWY STE 500, CHANTILLY, VA 20151-1125 USA SN 0003-004X EI 1945-3027 J9 AM MINERAL JI Am. Miner. PD OCT PY 2014 VL 99 IS 10 BP 1956 EP 1961 DI 10.2138/am-2014-4760 PG 6 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA AQ6XH UT WOS:000342956700013 ER PT J AU Inman-Narahari, F Ostertag, R Asner, GP Cordell, S Hubbell, SP Sack, L AF Inman-Narahari, Faith Ostertag, Rebecca Asner, Gregory P. Cordell, Susan Hubbell, Stephen P. Sack, Lawren TI Trade-offs in seedling growth and survival within and across tropical forest microhabitats SO ECOLOGY AND EVOLUTION LA English DT Article DE Determinants of plant community diversity and structure; light; performance rank changes; plant population and community dynamics; regeneration niche; relative growth rate; substrate; survival; topography; tropical forest diversity ID DIPTEROCARP RAIN-FOREST; TREE SEEDLINGS; WOODY SEEDLINGS; HABITAT SPECIALIZATION; SPECIES COEXISTENCE; REGENERATION NICHE; DENSITY-DEPENDENCE; UNDERSTOREY LIGHT; FUNCTIONAL TRAITS; SPATIAL VARIATION AB For niche differences to maintain coexistence of sympatric species, each species must grow and/or survive better than each of the others in at least one set of conditions (i.e., performance trade-offs). However, the extent of niche differentiation in tropical forests remains highly debated. We present the first test of performance trade-offs for wild seedlings in a tropical forest. We measured seedling relative growth rate (RGR) and survival of four common native woody species across 18 light, substrate, and topography microhabitats over 2.5 years within Hawaiian montane wet forest, an ideal location due to its low species diversity and strong species habitat associations. All six species pairs exhibited significant performance trade-offs across microhabitats and for RGR versus survival within microhabitats. We also found some evidence of performance equivalence, with species pairs having similar performance in 26% of comparisons across microhabitats. Across species, survival under low light was generally positively associated with RGR under high light. When averaged over all species, topography (slope, aspect, and elevation) explained most of the variation in RGR attributable to microhabitat variables (51-53%) followed by substrate type (35-37%) and light (11-12%). However, the relative effects of microhabitat differed among species and RGR metric (i.e., RGR for height, biomass, or leaf area). These findings indicate that performance trade-offs among species during regeneration are common in low-diversity tropical forest, although other mechanisms may better explain the coexistence of species with small performance differences. C1 [Inman-Narahari, Faith; Hubbell, Stephen P.; Sack, Lawren] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Ostertag, Rebecca] Univ Hawaii, Dept Biol, Hilo, HI 96720 USA. [Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Cordell, Susan] US Forest Serv, USDA, Inst Pacific Isl Forestry, Hilo, HI 96720 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa, Panama. RP Inman-Narahari, F (reprint author), Komohana Res & Extens Ctr, 875 Komohana St, Hilo, HI 96720 USA. EM ohia@ucla.edu RI Asner, Gregory/G-9268-2013; Sack, Lawren/A-5492-2008 OI Asner, Gregory/0000-0001-7893-6421; Sack, Lawren/0000-0002-7009-7202 FU National Science Foundation [EPSCoR 0554657, IOS-0546784]; Smithsonian Tropical Research Institute Center for Tropical Forest Science; University of California, Los Angeles; University of Hawaii; USDA Forest Service Pacific Southwest Research Station Institute of Pacific Islands Forestry (USFS-IPIF) FX We are grateful for substantial help from numerous field assistants, including K. Nelson-Kaula, M. Murphy, R. Moseley, K. Wailani-Nihipali, and others with the Hawaii Community College Tropical Forest Ecosystem and Agroforestry Management program and University of Hawaii at Hilo Pacific Internship Programs for Exploring Science programs. B. Hwang, M. Nullet, P. Scowcroft, and J. Schulten provided invaluable logistical assistance. The National Science Foundation (Grants EPSCoR 0554657 and IOS-0546784); the Smithsonian Tropical Research Institute Center for Tropical Forest Science; the University of California, Los Angeles; the University of Hawaii; and the USDA Forest Service Pacific Southwest Research Station Institute of Pacific Islands Forestry (USFS-IPIF) provided financial and other essential support. We thank USFS-IPIF and the Hawaii Division of Forestry and Wildlife/Department of Land and Natural Resources for access to the Hawaii Experimental Tropical Forest. The Carnegie Airborne Observatory is made possible by the Gordon and Betty Moore Foundation, John D. and Catherine T. 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. Finally, we thank C. Giardina, N. Inman-Narahari, T. Paine, W. Carson, D. J. Johnson, and an anonymous reviewer for insightful comments. NR 85 TC 4 Z9 4 U1 7 U2 45 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD OCT PY 2014 VL 4 IS 19 BP 3755 EP 3767 DI 10.1002/ece3.1196 PG 13 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AQ9KM UT WOS:000343171400004 PM 25614790 ER PT J AU Schachat, SR Labandeira, CC Gordon, J Chaney, D Levi, S Halthore, MN Alvarez, J AF Schachat, Sandra R. Labandeira, Conrad C. Gordon, Jessie Chaney, Dan Levi, Stephanie Halthore, Maya N. Alvarez, Jorge TI PLANT-INSECT INTERACTIONS FROM EARLY PERMIAN (KUNGURIAN) COLWELL CREEK POND, NORTH-CENTRAL TEXAS: THE EARLY SPREAD OF HERBIVORY IN RIPARIAN ENVIRONMENTS SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE Adelgidae; component community; conifer; diet; galling; Late Paleozoic; paleoecology; peltasperm; plant-insect interactions; redbeds ID SEED PLANT; ENDOPHYTIC OVIPOSITION; BEETLE COLEOPTERA; EARLY HISTORY; WIND DAMAGE; SP-NOV; ASSOCIATIONS; ARTHROPOD; LEAVES; USA AB Premise of research. Two previous studies examined the extent of insect herbivory in Early Permian habitats of north-central Texas, with varying results indicating minimal to modest levels of interaction diversity. In a comparison to two previous floras, we tested whether herbivory patterns in a third, slightly younger, assemblage, the Colwell Creek Pond (CCP) flora, most closely reflect plant host taxonomic affiliation, plant conspicuousness, habitat, geologic time, or other variable. Methodology. We assessed the diversity and frequency of insect herbivory on 2140 specimens at CCP. We examined the percent of leaf area removed by herbivory as a third, independent, measure of the effect of insect herbivore removal of host plant photosynthetic tissue. Pivotal results. In a moderately diverse flora of 12 taxa, we found evidence for hole feeding, margin feeding, surface feeding, piercing and sucking, oviposition, galling, seed predation, and wood boring. Some damage was fungally modified. Three herbivory measures consistently indicate that the two overwhelmingly herbivorized taxa were Auritifolia waggoneri, a peltasperm, and Taeniopteris spp., a form genus of unknown affinity. An approximate order of magnitude less herbivory was present for Evolsonia texana, a gigantopterid; indeterminate broad-leaved seed plants, possibly including a mixoneuroid odontopteroid and Rhachiphyllum; and Walchia piniformis, a conifer. A notable association occurred between W. piniformis and an aldegid hemipteran scale insect or precursor lineage. The remaining eight taxa displayed little or no herbivory. About 5% of seeds showed evidence for predation. Conclusions. Herbivory dominance on A. waggoneri and Taeniopteris spp. at CCP supports a hypothesis that the early expansion of herbivory in clastic depositional settings tracked broad-leaved seed plants, a pattern likely modified by other factors, such as conspicuousness. Insects targeted particular host plants and were specialists on certain foliar tissue types, such as galling on A. waggoneri and oviposition on Taeniopteris spp. C1 [Schachat, Sandra R.; Labandeira, Conrad C.; Gordon, Jessie; Chaney, Dan; Levi, Stephanie] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Schachat, Sandra R.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Gordon, Jessie; Levi, Stephanie] Univ Maryland, Dept Biol Sci, College Pk, MD 20742 USA. [Halthore, Maya N.] Virginia Polytech Inst & State Univ, Blacksburg, VA 24061 USA. [Alvarez, Jorge] Univ Puerto Rico, Dept Geol, Mayaguez, PR 00681 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM labandec@si.edu RI Schachat, Sandra/M-5399-2014 OI Schachat, Sandra/0000-0003-3237-5619 FU Department of Paleobiology at the National Museum of Natural History FX We thank Finnegan Marsh for producing the figures. Natalia Ainsfield and Hannah Brown assisted in the early stages of this study. Bill DiMichele was instrumental in implementing this project, through field collections, assistance with plant host identifications, and feedback at critical stages of manuscript preparation. S. Schachat was supported by the Benson, Brown, and Walcott Funds of the Department of Paleobiology at the National Museum of Natural History. Special thanks go to Debra McLaughlin of the University of Maryland, University College, for initial coordination in the CCP project. Bill DiMichele, Michael Dunn, and two anonymous reviewers provided important feedback on an earlier draft of the manuscript. We thank A. B. Wharton and G. Willingham of the W. T. Waggoner Estate, Vernon, Texas, for property access. This is contribution 235 of the Evolution of Terrestrial Ecosystems consortium of the National Museum of Natural History, in Washington, DC. NR 150 TC 13 Z9 13 U1 0 U2 15 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 EI 1537-5315 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD OCT PY 2014 VL 175 IS 8 BP 855 EP 890 DI 10.1086/677679 PG 36 WC Plant Sciences SC Plant Sciences GA AR0AY UT WOS:000343226300001 ER PT J AU Selvans, MM AF Selvans, Michelle M. TI PLANETARY SCIENCE Plate tectonics on ice SO NATURE GEOSCIENCE LA English DT News Item ID EUROPA AB Jupiter's icy moon Europa is criss-crossed by extensional features. A tectonic reconstruction suggests that Europa's extension is balanced by subduction - if so, Earth may not be the only planetary body with a plate tectonic system. C1 Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. RP Selvans, MM (reprint author), Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, POB 37012, Washington, DC 20013 USA. EM selvansm@si.edu NR 6 TC 0 Z9 0 U1 0 U2 12 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD OCT PY 2014 VL 7 IS 10 BP 695 EP 696 PG 2 WC Geosciences, Multidisciplinary SC Geology GA AQ8VC UT WOS:000343112600005 ER PT J AU Wing, SL Johnson, KR Peppe, DJ Green, WA Taylor, DW AF Wing, Scott L. Johnson, Kirk R. Peppe, Daniel J. Green, Walton A. Taylor, David Winship TI The Multi-Stranded Career of Leo J. Hickey SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Editorial Material ID LEAF ARCHITECTURE; WASHINGTON-STATE; DEVON-ISLAND; FOSSIL FLORA; ANGIOSPERM; CANADA; LEAVES; PLANT; BIOTA C1 [Wing, Scott L.; Johnson, Kirk R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Peppe, Daniel J.] Baylor Univ, Dept Geol, Waco, TX 76798 USA. [Green, Walton A.] Harvard Univ, Bot Museum, Cambridge, MA 02138 USA. [Taylor, David Winship] Indiana Univ Southeast, Dept Biol, New Albany, IN 47150 USA. RP Taylor, DW (reprint author), Indiana Univ Southeast, Dept Biol, 4201 Grant Line Rd, New Albany, IN 47150 USA. EM dwtaylo2@ius.edu OI Wing, Scott/0000-0002-2954-8905 NR 31 TC 0 Z9 0 U1 1 U2 3 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2014 VL 55 IS 2 BP 69 EP 78 PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ3WX UT WOS:000342725300001 ER PT J AU Little, SA Green, WA Wing, SL Wilf, P AF Little, Stefan A. Green, Walton A. Wing, Scott L. Wilf, Peter TI Reinvestigation of Leaf Rank, an Underappreciated Component of Leo Hickey's Legacy SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Angiosperm evolution; leaf architecture; leaf rank; leaf venation ID FOSSIL EVIDENCE; ANGIOSPERM LEAVES; VENATION PATTERNS; VEIN EVOLUTION; ARCHITECTURE; CHLORANTHACEAE; ECOPHYSIOLOGY; PHYLOGENETICS; DILLENIACEAE; ECOLOGY AB The widespread recognition of the scientific importance of leaf architecture, the description and interpretation of leaf shape and venation, is a cornerstone contribution of Leo Hickey's career. One leaf architectural trait that Hickey developed is leaf rank, which describes the level of organization of leaf venation in a single, discrete, ordinal variable. He used this scoring system to provide a rapid summary of overall venation complexity and organization in modern and fossil leaves. Leaves with the most reduced and disorganized venation are scored as low rank, whereas leaves with complex and well-organized venation are given high values. Leaf rank data facilitated comparisons of early angiosperms in fossil floras and were invoked in hypotheses regarding angiosperm evolution and ecology. This study presents a large data set of leaf ranks that Leo Hickey scored while he was a researcher at the Smithsonian Institution from 1969 to 1982. The data set represents at least 2,435 observations of US National Herbarium specimens. These formative observations of leaf venation have never been published. Here, we examine Hickey's data in light of current angiosperm phylogeny as a way to reinvestigate several of his hypotheses regarding leaf rank and angiosperm evolution: (1) leaf ranks tend to be consistent within a family; (2) leaf rank was low in early angiosperms, and high-rank venation occurred later; and (3) leaf rank is correlated with environmental conditions, often with reduced leaf rank values appearing in xeric taxa compared with close relatives under mesic conditions. These hypotheses have not been tested in the light of DNA-based, angiosperm-wide phylogeny, which was not available at the time when leaf rank was developed. We show that even with a DNA-based phylogeny, family-level comparisons show significant differences in average leaf rank; inferred leaf rank states along the early backbone of the angiosperm phylogeny are low, with high-rank taxa occurring across derived lineages; and there is a definite trend toward reduced leaf rank in xeric taxa, all consistent with Hickey's hypotheses. This taxonomically rich set of observations can serve as a foundation for further investigations of the evolution of leaf vein organization. C1 [Little, Stefan A.] Univ Victoria, Dept Biol, Ctr Forest Biol, Victoria, BC V8W 3N5, Canada. [Green, Walton A.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Wing, Scott L.] Smithsonian Inst, Nat Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Wilf, Peter] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Little, SA (reprint author), Univ Victoria, Dept Biol, Ctr Forest Biol, POB 3020 Stn CSC, Victoria, BC V8W 3N5, Canada. EM stefan.little@gmail.com; wagreen@bricol.net; wings@si.edu; pwilf@psu.edu OI Wing, Scott/0000-0002-2954-8905 FU David and Lucile Packard Foundation; S.A. Little's position at Pennsylvania State University FX We thank the late Leo Hickey for the generous contribution of his hitherto unpublished leaf rank data set and notes. This work was supported, in part, by the David and Lucile Packard Foundation (http://www.packard.org) (P. Wilf), which funded S.A. Little's position at Pennsylvania State University from 2006 to 2009. The funders had no role in study design, data collection and analysis, the decision to publish or preparation of the manuscript. NR 55 TC 2 Z9 2 U1 0 U2 6 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2014 VL 55 IS 2 BP 79 EP 87 PG 9 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ3WX UT WOS:000342725300002 ER PT J AU Jud, NA AF Jud, Nathan A. TI Morphotype Catalog of a Zone I (Aptian-Earliest Albian) Flora from Fairlington, Virginia, USA SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Paleobotany; morphotype; Early Cretaceous; Potomac Group; angiosperm; Virginia ID POTOMAC GROUP; SP NOV.; NORTHERN GONDWANA; LEAF ARCHITECTURE; WASHINGTON-STATE; FOSSIL EVIDENCE; ANGIOSPERM; EUDICOT; GEN.; ECOPHYSIOLOGY AB Plant fossil collections from Lower Cretaceous floodplain deposits sometimes provide snapshots of local communities that included early herbaceous angiosperms. Here I describe the plant megafossils in a collection made from the lower part of the Potomac Group near Fairlington, Virginia, USA. The collection includes 123 identifiable plant fossils on 42 hand specimens, comprising nine plant morphotypes: three ferns, five gymnosperms and one angiosperm. All but one of the described morphotypes also occur in other collections from the lower Potomac Group. There is one moderately abundant angiosperm species in this collection that has been found at other Potomac Group sites but was incorrectly identified as a fern. Well-preserved specimens of this morphotype clearly show axillary branching, complex leaves and glandular teeth at the apices of lobes on the leaves; together, these characteristics suggest it was an herbaceous eudicot angiosperm. The one new morphotype in this collection is an enigmatic plant of intermediate abundance and unknown affinity. On the basis of the simple, pinnate stenophyllous leaves with two vein orders, reticulate secondary veins and the attachment of one leaf to a carbonized axis roughly 1 cm across with long internodes, I hypothesize that it was a shrubby riparian gymnosperm. This work represents the first step toward a complete morphotype catalog for the flora of the lower Potomac Group. C1 [Jud, Nathan A.] Univ Maryland, Dept Biol Sci, College Pk, MD 20742 USA. [Jud, Nathan A.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. RP Jud, NA (reprint author), Univ Maryland, Dept Biol Sci, 4140 Plant Sci Bldg, College Pk, MD 20742 USA. EM njud@umd.edu FU Smithsonian Peter Buck Pre-Doctoral Fellowship; University of Maryland Program in Behavior, Ecology, Evolution and Systematics; Maryland Agricultural Experiment Station; University of Maryland Graduate School FX I thank Scott L. Wing (Smithsonian) for valuable discussions, guidance and comments. This research was conducted with support from a Smithsonian Peter Buck Pre-Doctoral Fellowship, the University of Maryland Program in Behavior, Ecology, Evolution and Systematics, the Maryland Agricultural Experiment Station and the University of Maryland Graduate School. NR 44 TC 2 Z9 2 U1 0 U2 5 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X EI 2162-4135 J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2014 VL 55 IS 2 BP 135 EP 152 PG 18 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ3WX UT WOS:000342725300005 ER PT J AU Cheng, RC Kuntner, M AF Cheng, Ren-Chung Kuntner, Matjaz TI Phylogeny suggests nondirectional and isometric evolution of sexual size dimorphism in argiopine spiders SO EVOLUTION LA English DT Article DE Argiope; Brownian motion; comparative method; phylogenetically independent contrasts; Rensch's rule; size evolution ID PHYLOGENETICALLY INDEPENDENT CONTRASTS; BODY-SIZE; AQUARIUS-REMIGIS; FEMALE GIGANTISM; WATER-STRIDERS; RENSCHS RULE; ARANEAE; NEPHILA; MODEL; CONSEQUENCES AB Sexual dimorphism describes substantial differences between male and female phenotypes. In spiders, sexual dimorphism research almost exclusively focuses on size, and recent studies have recovered steady evolutionary size increases in females, and independent evolutionary size changes in males. Their discordance is due to negative allometric size patterns caused by different selection pressures on male and female sizes (converse Rensch's rule). Here, we investigated macroevolutionary patterns of sexual size dimorphism (SSD) in Argiopinae, a global lineage of orb-weaving spiders with varying degrees of SSD. We devised a Bayesian and maximum-likelihood molecular species-level phylogeny, and then used it to reconstruct sex-specific size evolution, to examine general hypotheses and different models of size evolution, to test for sexual size coevolution, and to examine allometric patterns of SSD. Our results, revealing ancestral moderate sizes and SSD, failed to reject the Brownian motion model, which suggests a nondirectional size evolution. Contrary to predictions, male and female sizes were phylogenetically correlated, and SSD evolution was isometric. We interpret these results to question the classical explanations of female-biased SSD via fecundity, gravity, and differential mortality. In argiopines, SSD evolution may be driven by these or additional selection mechanisms, but perhaps at different phylogenetic scales. C1 [Cheng, Ren-Chung; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Ctr Behav Ecol & Evolut, Wuhan, Hubei, Peoples R China. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Cheng, RC (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. EM bolasargiope@gmail.com; kuntner@gmail.com FU Slovenian Research Agency [P1-10236] FX We thank all colleagues who provided material for size measurement and molecular work, in particular D. Li, J. Schneider, X. Xu, I. Agnarsson, I. M. Tso, P. Jager, W. Chotwong, J. P. Huang, C. P. Lin, Y. C. Su, V. Settepani, S. Huber, E. A. Yagmur, M. A. Herberstein, and J. N. Huang. We also thank M. Gregoric, N. Vidergar, T. Lokovsek, and S. Kralj-Fiser for kind help in the laboratory. This work was supported by the Slovenian Research Agency (P1-10236 to MK and a Young Researcher fellowship to RCC). The authors declare no conflict of interest. NR 79 TC 11 Z9 11 U1 4 U2 42 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 OCT PY 2014 VL 68 IS 10 BP 2861 EP 2872 DI 10.1111/evo.12504 PG 12 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA AQ6FC UT WOS:000342904300009 PM 25130435 ER PT J AU Yamato, M Koopman, H Niemeyer, M Ketten, D AF Yamato, Maya Koopman, Heather Niemeyer, Misty Ketten, Darlene TI Characterization of lipids in adipose depots associated with minke and fin whale ears: Comparison with "acoustic fats" of toothed whales SO MARINE MAMMAL SCIENCE LA English DT Article ID DOLPHIN TURSIOPS-TRUNCATUS; PORPOISE PHOCOENA-PHOCOENA; SOUND-VELOCITY; WAX ESTERS; BALAENOPTERA-PHYSALUS; ACID-COMPOSITION; ISOVALERIC ACID; SPERM-WHALE; GLOBICEPHALA-MELAENA; BALAENA-MYSTICETUS C1 [Yamato, Maya] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Koopman, Heather] Univ N Carolina, Dept Biol & Marine Biol, Wilmington, NC 28403 USA. [Niemeyer, Misty] Int Fund Anim Welf, Marine Mammal Rescue & Res, Yarmouth Port, MA 02675 USA. [Ketten, Darlene] Woods Hole Oceanog Inst, Dept Biol, Woods Hole, MA 02543 USA. RP Yamato, M (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. EM yamatom@si.edu FU National Science Foundation Graduate Research Fellowship; Woods Hole Oceanographic Institution (WHOI) Coastal Ocean Institute Award; WHOI Ocean Life Institute Fellowship; Massachusetts Institute of Technology Student Assistance Fund; Joint Industry Program; Office of Naval Research; WHOI Academic Programs Office FX This study would not have been possible without the International Fund for Animal Welfare's Marine Mammal Rescue and Research group based in Yarmouth Port, Massachusetts, which provided us with the mysticete tissue samples. Dr. Michael Moore, Julie Arruda, Scott Cramer, Dr. Aran Mooney, Dr. Caroline Harper, and Dr. Joy Reidenberg provided valuable assistance during tissue collection and Dr. Andrew Westgate, Hillary Lane, and Caitlin McKinstry kindly provided assistance for lipid analyses. Dr. Kimberly Popendorf and three anonymous reviewers provided helpful critiques of this manuscript. Funding to pursue this work came from the National Science Foundation Graduate Research Fellowship, Woods Hole Oceanographic Institution (WHOI) Coastal Ocean Institute Award, WHOI Ocean Life Institute Fellowship, Massachusetts Institute of Technology Student Assistance Fund, Joint Industry Program, Office of Naval Research, and the WHOI Academic Programs Office. NR 73 TC 1 Z9 1 U1 1 U2 11 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 EI 1748-7692 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD OCT PY 2014 VL 30 IS 4 BP 1549 EP 1563 DI 10.1111/mms.12120 PG 15 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AQ5GR UT WOS:000342835800014 ER PT J AU Appelhans, MS Wen, J Wagner, WL AF Appelhans, Marc S. Wen, Jun Wagner, Warren L. TI A molecular phylogeny of Acronychia, Euodia, Melicope and relatives (Rutaceae) reveals polyphyletic genera and key innovations for species richness SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Acronychia; Euodia; Fruit types; Melicope; Seed coat; Species richness ID CLADISTIC-ANALYSIS; SEQUENCE DATA; RETICULATE EVOLUTION; BURSERA BURSERACEAE; NONCODING REGIONS; CHLOROPLAST DNA; BIOGEOGRAPHY; SUBFAMILIES; DISPERSAL; INFERENCE AB We present the first detailed phylogenetic study of the genus Melicope, the largest genus of the Citrus family (Rutaceae). The phylogenetic analysis sampled about 50% of the 235 accepted species of Melicope as well as representatives of 26 related genera, most notably Acronychia and Euodia. The results based on five plastid and nuclear markers have revealed that Acronychia, Euodia and Melicope are each not monophyletic in their current circumscriptions and that several small genera mainly from Australia and New Caledonia need to be merged with one of the three genera to ensure monophyly at the generic level. The phylogenetic position of the drupaceous Acronychia in relation to Melicope, which has capsular or follicular fruits, remains unclear and Acronychia might be a separate genus or a part of Melicope. The seed coats of Melicope, Acronychia and related genera show adaptations to bird-dispersal, which might be regarded as key innovations for species radiations. Euodia and its relatives, which lack these adaptations, include only about 20 species while the Melicope-Acronychia group consists of about 340 species. The drupaceous genera Comptonella, Dutaillyea, Picrella and Sarcomelicope are nested within Melicope and need to be merged with Melicope. The expanded genus is a prime example of the artificial classification system of Engler, who defined Rutaceous subfamilies mainly based on gynoecial and fruit characters. (C) 2014 Elsevier Inc. All rights reserved. C1 [Appelhans, Marc S.; Wen, Jun; Wagner, Warren L.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [Appelhans, Marc S.] Univ Gottingen, Dept Systemat Bot, Albrecht von Haller Inst Plant Sci, D-37073 Gottingen, Germany. RP Appelhans, MS (reprint author), Univ Gottingen, Dept Systemat Bot, Albrecht von Haller Inst Plant Sci, Untere Karspule 2, D-37073 Gottingen, Germany. EM Marc.Appelhans@biologie.uni-goettingen.de NR 69 TC 10 Z9 10 U1 2 U2 23 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD OCT PY 2014 VL 79 BP 54 EP 68 DI 10.1016/j.ympev.2014.06.014 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AQ5YP UT WOS:000342884800005 PM 24971739 ER PT J AU Agis-Gonzalez, B Miniutti, G Kara, E Fabian, AC Sanfrutos, M Risaliti, G Bianchi, S Strotjohann, NL Saxton, RD Parker, ML AF Agis-Gonzalez, B. Miniutti, G. Kara, E. Fabian, A. C. Sanfrutos, M. Risaliti, G. Bianchi, S. Strotjohann, N. L. Saxton, R. D. Parker, M. L. TI Black hole spin and size of the X-ray-emitting region(s) in the Seyfert 1.5 galaxy ESO 362-G18 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; AGN MONITORING PROJECT; NARROW-LINE REGION; XMM-NEWTON VIEW; CLUMPY-TORUS; IRON K; M-BH-SIGMA(ASTERISK) RELATION; ABSORPTION VARIABILITY; REVERBERATION LAGS; IRAS 13224-3809 AB We report results from multi-epoch X-ray observations of the Seyfert 1.5 galaxy ESO 362-G18 performed between 2005 November and 2010 June. ESO 362-G18 generally exhibits the typical X-ray spectrum of type 1 active galactic nuclei. A disc-reflection component accounts for broad residuals in the iron K band and above 10 keV, as well as for a significant soft excess. From our best-fitting reflection model, we measure a black hole spin a >= 0.92 at the 99.99 per cent confidence level. ESO 362-G18 is also (typically) mildly absorbed by a column of neutral gas. The absorber is variable and one observation, performed similar to 2 months after a typical mildly absorbed one, is heavily absorbed by a cold column density of similar to 3-4 x 10(23) cm(-2), nearly two orders of magnitude higher than that during any other observation. UV variability between the heavily absorbed observation and the others suggests that the absorber can be identified with a dusty, clumpy torus. The absorption variability time-scale enables us to locate the X-ray-emitting region within the innermost similar to 50 gravitational radii. Such result holds not only for the X-ray continuum, but also for the soft excess. C1 [Agis-Gonzalez, B.; Miniutti, G.; Sanfrutos, M.] ESA, Ctr Astrobiol CSIC INTA, Dept Astrofis, E-28691 Madrid, Spain. [Kara, E.; Fabian, A. C.; Parker, M. L.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, G.] INAF Osservatorio Astron Arcetri, I-50125 Florence, Italy. [Bianchi, S.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Strotjohann, N. L.] Univ Bonn, Inst Phys, D-53115 Bonn, Germany. [Saxton, R. D.] ESA, XMM SOC, E-28691 Madrid, Spain. RP Agis-Gonzalez, B (reprint author), ESA, Ctr Astrobiol CSIC INTA, Dept Astrofis, POB 78, E-28691 Madrid, Spain. EM agisgb@cab.inta-csic.es RI Bianchi, Stefano/B-4804-2010; Miniutti, Giovanni/L-2721-2014; OI Bianchi, Stefano/0000-0002-4622-4240; Miniutti, Giovanni/0000-0003-0707-4531; Risaliti, Guido/0000-0002-3556-977X; Strotjohann, Nora Linn/0000-0002-4667-6730 FU ESA member states; NASA; European Union [312789]; Spanish MINECO [AYA2010-21490-C02-02]; CSIC JAE; ESA through the ESAC 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. We made use of data obtained from the Chandra Data Archive, and software provided by the Chandra X-ray Center (CXC). We acknowledge the use of public data from the Swift data archive. This work also made use of data from the Suzaku observatory, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA). This work 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 was funded by the European Union Seventh Framework Programme (FP7/2007-2013) under grant 312789. BAG thanks the Spanish MINECO for support through the FPI programme associated with grant AYA2010-21490-C02-02. MS thanks the CSIC JAE-Predoc programme for support. NLS acknowledges support by ESA through the ESAC trainee programme. NR 57 TC 9 Z9 9 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2014 VL 443 IS 4 BP 2862 EP 2873 DI 10.1093/mnras/stu1358 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6KX UT WOS:000342922100003 ER PT J AU Foley, RJ Fox, OD McCully, C Phillips, MM Sand, DJ Zheng, W Challis, P Filippenko, AV Folatelli, G Hillebrandt, W Hsiao, EY Jha, SW Kirshner, RP Kromer, M Marion, GH Nelson, M Pakmor, R Pignata, G Ropke, FK Seitenzahl, IR Silverman, JM Skrutskie, M Stritzinger, MD AF Foley, Ryan J. Fox, O. D. McCully, C. Phillips, M. M. Sand, D. J. Zheng, W. Challis, P. Filippenko, A. V. Folatelli, G. Hillebrandt, W. Hsiao, E. Y. Jha, S. W. Kirshner, R. P. Kromer, M. Marion, G. H. Nelson, M. Pakmor, R. Pignata, G. Roepke, F. K. Seitenzahl, I. R. Silverman, J. M. Skrutskie, M. Stritzinger, M. D. TI Extensive HST ultraviolet spectra and multiwavelength observations of SN 2014J in M82 indicate reddening and circumstellar scattering by typical dust SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2014J; dust, extinction; galaxies: individual: M82 ID HUBBLE-SPACE-TELESCOPE; IA SUPERNOVA PROGENITORS; LIGHT-CURVE SHAPES; INTERSTELLAR EXTINCTION; IMPROVED DISTANCES; INFRARED-EMISSION; SODIUM-ABSORPTION; EJECTA VELOCITY; MAXIMUM-LIGHT; K-CORRECTIONS AB SN 2014J in M82 is the closest detected Type Ia supernova (SN Ia) in at least 28 yr and perhaps in 410 yr. Despite its small distance of 3.3 Mpc, SN 2014J is surprisingly faint, peaking at V = 10.6 mag, and assuming a typical SN Ia luminosity, we infer an observed visual extinction of A(V) = 2.0 +/- 0.1 mag. But this picture, with R-V = 1.6 +/- 0.2, is too simple to account for all observations. We combine 10 epochs (spanning a month) of HST/Space Telescope Imaging Spectrograph (STIS) ultraviolet through near-infrared spectroscopy with HST/Wide Field Camera 3 (WFC3), Katzman Automatic Imaging Telescope, and FanCam photometry from the optical to the infrared and nine epochs of high-resolution TRES (Tillinghast Reflection Echelle Spectrograph) spectroscopy to investigate the sources of extinction and reddening for SN 2014J. We argue that the wide range of observed properties for SN 2014J is caused by a combination of dust reddening, likely originating in the interstellar medium of M82, and scattering off circumstellar material. For this model, roughly half of the extinction is caused by reddening from typical dust (E(B - V) = 0.45 mag and R-V = 2.6) and roughly half by scattering off Large Magellanic Cloud-like dust in the circumstellar environment of SN 2014J. C1 [Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Fox, O. D.; Zheng, W.; Filippenko, A. V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [McCully, C.; Jha, S. W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Phillips, M. M.; Hsiao, E. Y.] Las Campanas Observ, Carnegie Observ, La Serena, Chile. [Sand, D. J.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Challis, P.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Folatelli, G.] Univ Tokyo, Kavli Inst Phys & Math Universe, Todai Inst Adv Study, WPI, Kashiwa, Chiba 2778583, Japan. [Hillebrandt, W.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Kromer, M.] Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Kromer, M.] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. [Marion, G. H.; Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Nelson, M.; Skrutskie, M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Pakmor, R.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Pignata, G.] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Pignata, G.] Millennium Inst Astrophys, Santiago, Chile. [Roepke, F. K.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Seitenzahl, I. R.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Stritzinger, M. D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Foley, RJ (reprint author), Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA. EM rfoley@illinois.edu OI Ropke, Friedrich/0000-0002-4460-0097; stritzinger, maximilian/0000-0002-5571-1833 FU NASA [NAS 5-26555]; NSF [PHYS-1066293, AST-1211196, AST-1211916]; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC12009]; Emmy Noether Program of the Deutsche Forschungsgemeinschaft [RO 3676/1-1]; ARCHES prize of the German Ministry of Education and Research (BMBF); NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; ARC Laureate Grant [FL0992131]; Danish Agency for Science and Technology and Innovation; TABASGO Foundation; Christopher R. Redlich Fund; [GO-13286]; [DD-13621] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programmes GO-13286 and DD-13621. We thank the Director for observing SN 2014J through programme DD-13621. We especially thank the STScI staff for accommodating our target-of-opportunity programme A Armstrong, R. Bohlin, S. Holland, S. Meyett, and D. Taylor were critical for the execution of this programme.; This manuscript was completed during the 'Fast and Furious: Understanding Exotic Astrophysical Transients' workshop at the Aspen Center for Physics, which is supported in part by the NSF under grant no. PHYS-1066293. RJF, ODF, AVF, RPK, and JMS thank the Aspen Center for Physics for its hospitality during the 'Fast and Furious' workshop in 2014 June.; Supernova research at Harvard is supported in part by NSF grant AST-1211196. GHM and DJS are visiting Astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration. GP acknowledges support by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics, MAS. FKR was supported by the Emmy Noether Program (RO 3676/1-1) of the Deutsche Forschungsgemeinschaft and the ARCHES prize of the German Ministry of Education and Research (BMBF). JMS is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. IRS is supported by the ARC Laureate Grant FL0992131. MDS gratefully acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. AVF's supernova group at UC Berkeley is supported through NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, Auto Scope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. NR 108 TC 57 Z9 58 U1 2 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT 1 PY 2014 VL 443 IS 4 BP 2887 EP 2906 DI 10.1093/mnras/stu1378 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6KX UT WOS:000342922100005 ER PT J AU Sabin, L Parker, QA Corradi, RLM Guzman-Ramirez, L Morris, RAH Zijlstra, AA Bojicic, IS Frew, DJ Guerrero, M Stupar, M Barlow, MJ Mora, FC Drew, JE Greimel, R Groot, P Irwin, JM Irwin, MJ Mampaso, A Miszalski, B Olguin, L Phillipps, S Garcia, MS Viironen, K Wright, NJ AF Sabin, L. Parker, Q. A. Corradi, R. L. M. Guzman-Ramirez, L. Morris, R. A. H. Zijlstra, A. A. Bojicic, I. S. Frew, D. J. Guerrero, M. Stupar, M. Barlow, M. J. Cortes Mora, F. Drew, J. E. Greimel, R. Groot, P. Irwin, J. M. Irwin, M. J. Mampaso, A. Miszalski, B. Olguin, L. Phillipps, S. Santander Garcia, M. Viironen, K. Wright, N. J. TI First release of the IPHAS catalogue of new extended planetary nebulae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; planetary nebulae: general ID H-ALPHA SURVEY; NORTHERN GALACTIC PLANE; IMAGE SUBTRACTION; SYMBIOTIC STARS; ISM INTERACTION; DISCOVERY; DIAGNOSTICS; POPULATION; ANTICENTER; ABUNDANCES AB We present the first results of our search for new, extended planetary nebulae (PNe) based on careful, systematic, visual scrutiny of the imaging data from the Isaac Newton Telescope Photometric Ha Survey of the Northern Galactic plane (IPHAS). The newly uncovered PNe will help to improve the census of this important population of Galactic objects that serve as key windows into the late-stage evolution of low-to intermediate-mass stars. They will also facilitate study of the faint end of the ensemble Galactic PN luminosity function. The sensitivity and coverage of IPHAS allows PNe to be found in regions of greater extinction in the Galactic plane and/or those PNe in a more advanced evolutionary state and at larger distances compared to the general Galactic PN population. Using a set of newly revised optical diagnostic diagrams in combination with access to a powerful, new, multiwavelength imaging data base, we have identified 159 true, likely and possible PNe for this first catalogue release. The ability of IPHAS to unveil PNe at low Galactic latitudes and towards the Galactic Anticentre, compared to previous surveys, makes this survey an ideal tool to contribute to the improvement of our knowledge of the whole Galactic PN population. C1 [Sabin, L.; Cortes Mora, F.] Univ Guadalajara, CUCEI, Dept Fis, Inst Astron & Meteorol, Guadalajara 44130, Jalisco, Mexico. [Parker, Q. A.; Bojicic, I. S.; Frew, D. J.; Stupar, M.] Macquarie Univ, Res Ctr Astron Astrophys & Astrophoton, Sydney, NSW 2109, Australia. [Parker, Q. A.; Bojicic, I. S.; Frew, D. J.; Stupar, M.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Parker, Q. A.; Bojicic, I. S.] Australian Astron Observ, Epping, NSW 1710, Australia. [Corradi, R. L. M.; Mampaso, A.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Corradi, R. L. M.; Mampaso, A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Guzman-Ramirez, L.] European So Observ, Santiago 19001, Chile. [Morris, R. A. H.; Phillipps, S.] Univ Bristol, Sch Phys, Bristol BS8 1TL, Avon, England. [Zijlstra, A. A.] Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Guerrero, M.] CSIC, IAA, E-18008 Granada, Spain. [Barlow, M. J.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Drew, J. E.; Wright, N. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Greimel, R.] Graz Univ, NAWI Graz, Inst Phys, IGAM, A-8010 Graz, Austria. [Groot, P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Irwin, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Irwin, M. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Miszalski, B.] S African Astron Observ, ZA-7935 Observatory, South Africa. [Miszalski, B.] Southern African Large Telescope Fdn, ZA-7935 Observatory, South Africa. [Olguin, L.] Univ Sonora, Dept Invest Fis, Hermosillo 83190, Sonora, Mexico. [Santander Garcia, M.] Observ Astron Nacl, E-28803 Alcala De Henares, Spain. [Santander Garcia, M.] CSIC, INTA, CAB, E-28850 Madrid, Spain. [Viironen, K.] Ctr Estudios Fis Cosmos Aragon, E-44001 Teruel, Spain. RP Sabin, L (reprint author), Univ Guadalajara, CUCEI, Dept Fis, Inst Astron & Meteorol, Av Vallarta 2602, Guadalajara 44130, Jalisco, Mexico. EM laurence.sabin@gmail.com RI Barlow, Michael/A-5638-2009; Groot, Paul/K-4391-2016; OI Barlow, Michael/0000-0002-3875-1171; Groot, Paul/0000-0002-4488-726X; Morris, Rhys/0000-0002-9210-1567; Guerrero, Martin/0000-0002-7759-106X; Frew, David/0000-0002-3108-5284; Drew, Janet/0000-0003-1192-7082 FU CONACYT [CB-2011-01-0168078]; Spanish MICINN within the programme CONSOLIDER INGENIO [CSD2009-00038]; [PROMEP/103.5/12/3590] FX We would like to thank Margaret Meixner for her careful review and highly appreciate the comments which contributed to improving the quality of the publication. LS is supported by the CONACYT grant CB-2011-01-0168078, MS was partially supported by Spanish MICINN within the programme CONSOLIDER INGENIO 2010, under grant 'Molecular Astrophysics: The Herschel and ALMA Era, ASTROMOL' (ref: CSD2009-00038), LO acknowledges support by project PROMEP/103.5/12/3590. We also thank the Bristol University students Greg Mould, William Howie, Luke Davies, Heidi Naumann, Will Summers, Alex Townshend, Paul May, Matina Mitchell, Finn Hoolahan, Tom Burgess, Ashley Akerman, James Jordan, Simon Palmer, Anna Kovacevic, Jai Tailor, Olivia Smedley and Daniel Huggins for their participation in the search in the framework of their undergraduate thesis. NR 65 TC 11 Z9 12 U1 1 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 OCT 1 PY 2014 VL 443 IS 4 BP 3388 EP 3401 DI 10.1093/mnras/stu1404 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6KX UT WOS:000342922100043 ER PT J AU Baeza, JA Bauer, RT Okuno, J Thiel, M AF Antonio Baeza, J. Bauer, Raymond T. Okuno, Junji Thiel, Martin TI Molecular phylogeny of hinge-beak shrimps (Decapoda: Caridea: Rhyrichocinetes and Cinetorhyrichus) and allies: a formal test of familiar and generic monophyly using a multilocus phylogeny SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Bayesian hypothesis testing; Crustacea; SATe-II ID RHYNCHOCINETES-TYPUS DECAPODA; MULTIPLE SEQUENCE ALIGNMENT; MALE ROCK SHRIMP; JOINT BAYESIAN-ESTIMATION; MATING-BEHAVIOR; SEXUAL SYSTEM; SIMULTANEOUS HERMAPHRODITISM; MAXIMUM-LIKELIHOOD; GENUS LYSMATA; CRUSTACEA AB The Rhynchocinetidae (binge-beak' shrimps) is a family of marine caridean decapods with considerable variation in sexual dimorphism, male weaponry, mating tactics, and sexual systems. Thus, this group is an excellent model with which to analyse the evolution of these important characteristics, which are of interest not only in shrimps specifically but also in animal taxa in general. Yet, there exists no phylogenetic hypothesis, either molecular or morphological, for this taxon against which to test either the evolution of behavioural traits within the Rhynchocinetidae or its genealogical relationships with other caridean taxa. In this study, we tested (1) hypotheses on the phylogenetic relationships of rhynchocinetid shrimps, and (2) the efficacy of different (one-, two-, and three-phase) methods to generate a reliable phylogeny. Total genomic DNA was extracted from tissue samples taken from 17 species of Rhynchocinetidae and five other species currently or previously assigned to the same superfamily (Nematocarcinoidea); six species from other superfamilies were used as outgroups. Sequences from two nuclear genes (H3 and Enolase) and one mitocliondrial gene (12S) were used to construct phylogenies. One-phase playlogenetic analyses (SATe-II) and classical two- and three-phase playlogenetic analyses were employed, using both maximum likelihood and Bayesian inference methods. Both a two-gene data set (H3 and Enolase) and a three-gene data set (H3, Enolase, 12S) were utilized to explore the relationships amongst the targeted species. These analyses showed that the superfamily Nematocarcinoidea, as currently accepted, is polyphyletic. Furthermore, the two major clades recognized by the SATe-II analysis are clearly concordant with the genera Rhynchocinetes and Cinetorhynchus, which are currently recognized in the morphological-based classification (implicit phylogeny) as composing the family Rhynchocinetidae. The SATe-II method is considered superior to the other phylogenetic analyses employed, which failed to recognize these two major clades. Studies using more genes and a more complete species data set are needed to test yet unresolved inter- and intrafamilial systematic and evolutionary questions about this remarkable clade of caridean shrimps. C1 [Antonio Baeza, J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.; Thiel, Martin] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. [Bauer, Raymond T.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Okuno, Junji] Nat Hist Museum & Inst, Coastal Branch, Katsuura, Chiba 2995242, Japan. [Thiel, Martin] CEAZA, Coquimbo, Chile. RP Baeza, JA (reprint author), Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA. EM baeza.antonio@gmail.com FU National Geographic research grant FX This study was partially funded by a National Geographic research grant to J. A. B. Some specimens used in this study were provided by the following colleagues: Arthur Anker and Gustav Paulay (FLMNH, USA), Sammy De Grave (OUMNH, UK), Ivan Hinojosa (University of Tasmania, Australia), Yumiko Osawa (Japan), Alvaro Palma (Pontificia Universidad Catolica de Chile, Chile), and Kareen Schnabel (NIWA, New Zealand). Mr Naoki Shirakawa, a skilled diver from Okinawa, Japan, also kindly donated various specimens used in this study. Jeff Hunt and Lee Weigt (Laboratory of Analytical Biology, NMNH, USA) provided logistical support for the molecular analysis. This is Smithsonian Marine Station at Fort Pierce contribution number 958 and Laboratory of Crustacean Biology, University of Lafayette, Louisiana, contribution number 162. NR 89 TC 3 Z9 3 U1 0 U2 15 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 OCT PY 2014 VL 172 IS 2 BP 426 EP 450 DI 10.1111/zoj.12173 PG 25 WC Zoology SC Zoology GA AQ5DU UT WOS:000342827000006 ER PT J AU Overstreet, LK AF Overstreet, Leslie K. TI The birth, death and resurrection of the "geneticologists" SO ARCHIVES OF NATURAL HISTORY LA English DT Article C1 Smithsonian Inst Lib, Washington, DC 20013 USA. RP Overstreet, LK (reprint author), Smithsonian Inst Lib, NHB CE-G15-MRC 154,POB 37012, Washington, DC 20013 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU EDINBURGH UNIV PRESS PI EDINBURGH PA THE TUN-HOLYROOD RD, 12 2F JACKSONS ENTRY, EDINBURGH EH8 8PJ, ENGLAND SN 0260-9541 EI 1755-6260 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD OCT PY 2014 VL 41 IS 2 BP 357 EP 364 DI 10.3366/anh.2014.0256 PG 8 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA AQ1HX UT WOS:000342533600013 ER PT J AU Parsons, ECM Favaro, B Aguirre, AA Bauer, AL Blight, LK Cigliano, JA Coleman, MA Cote, IM Draheim, M Fletcher, S Foley, MM Jefferson, R Jones, MC Kelaher, BP Lundquist, CJ Mccarthy, JB Nelson, A Patterson, K Walsh, L Wright, AJ Sutherland, WJ AF Parsons, E. C. M. Favaro, Brett Aguirre, A. Alonso Bauer, Amy L. Blight, Louise K. Cigliano, John A. Coleman, Melinda A. Cote, Isabelle M. Draheim, Megan Fletcher, Stephen Foley, Melissa M. Jefferson, Rebecca Jones, Miranda C. Kelaher, Brendan P. Lundquist, Carolyn J. Mccarthy, Julie-Beth Nelson, Anne Patterson, Katheryn Walsh, Leslie Wright, Andrew J. Sutherland, William J. TI Seventy-One Important Questions for the Conservation of Marine Biodiversity SO CONSERVATION BIOLOGY LA English DT Article DE horizon scanning; marine biodiversity; policy; priority setting; research agenda; research questions ID FISHERIES MANAGEMENT; ECOLOGICAL QUESTIONS; CLIMATE-CHANGE; COASTAL; ECOSYSTEMS; RESERVES; IMPACTS; POLICY; GLOBALIZATION; CITIZENSHIP AB The ocean provides food, economic activity, and cultural value for a large proportion of humanity. Our knowledge of marine ecosystems lags behind that of terrestrial ecosystems, limiting effective protection of marine resources. We describe the outcome of 2 workshops in 2011 and 2012 to establish a list of important questions, which, if answered, would substantially improve our ability to conserve and manage the world's marine resources. Participants included individuals from academia, government, and nongovernment organizations with broad experience across disciplines, marine ecosystems, and countries that vary in levels of development. Contributors from the fields of science, conservation, industry, and government submitted questions to our workshops, which we distilled into a list of priority research questions. Through this process, we identified 71 key questions. We grouped these into 8 subject categories, each pertaining to a broad component of marine conservation: fisheries, climate change, other anthropogenic threats, ecosystems, marine citizenship, policy, societal and cultural considerations, and scientific enterprise. Our questions address many issues that are specific to marine conservation, and will serve as a road map to funders and researchers to develop programs that can greatly benefit marine conservation. C1 [Parsons, E. C. M.; Aguirre, A. Alonso; Bauer, Amy L.; Patterson, Katheryn; Wright, Andrew J.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Favaro, Brett; Cote, Isabelle M.] Simon Fraser Univ, Dept Biol Sci, Burnaby, BC V5A 1S6, Canada. [Favaro, Brett] Mem Univ Newfoundland, Fisheries & Marine Inst, Ctr Sustainable Aquat Resources, St John, NF A1C 5R3, Canada. [Aguirre, A. Alonso] Smithsonian Mason Sch Conservat, Front Royal, VA 22630 USA. [Blight, Louise K.] Univ British Columbia, Ctr Appl Conservat Res, Vancouver, BC V6T 1Z4, Canada. [Blight, Louise K.] WWF Canada, Vancouver, BC V6C 1T2, Canada. [Cigliano, John A.] Cedar Crest Muhlenberg Coll, Dept Biol Sci, Allentown, PA 18104 USA. [Coleman, Melinda A.] NSW Fisheries, New South Wales Dept Primary Ind, Coffs Harbour, NSW 2450, Australia. [Coleman, Melinda A.; Kelaher, Brendan P.] So Cross Univ, Natl Marine Sci Ctr, Coffs Harbour, NSW 2450, Australia. [Draheim, Megan] Virginia Tech, Ctr Leadership Global Sustainabil, Nat Resource Programs, Arlington, VA 22203 USA. [Fletcher, Stephen; Jefferson, Rebecca] Univ Plymouth, Ctr Marine & Coastal Policy Res, Plymouth PL4 8AA, Devon, England. [Foley, Melissa M.] Stanford Univ, Stanford Woods Inst Environm, Ctr Ocean Solut, Monterey, CA 93940 USA. [Foley, Melissa M.] US Geol Survey, Pacific Coastal & Marine Sci Ctr, Santa Cruz, CA 95060 USA. [Jones, Miranda C.] Univ British Columbia, Fisheries Ctr, Ocean Res Unit, Vancouver, BC V5Z 1M9, Canada. [Lundquist, Carolyn J.] Natl Inst Water & Atmospher Res Ltd, Hamilton, New Zealand. [Lundquist, Carolyn J.] Univ Auckland, Leigh Marine Lab, Inst Marine Sci, Auckland 1, New Zealand. [Nelson, Anne] Collaborat Ocean Planning, Portland, OR 97293 USA. [Walsh, Leslie] Natl Geog Soc, Washington, DC 20036 USA. [Sutherland, William J.] Univ Cambridge, Dept Zool, Conservat Sci Grp, Cambridge CB2 3EJ, England. RP Parsons, ECM (reprint author), George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. EM ecm-parsons@earthlink.net RI Parsons, Edward Christien/C-2409-2011; Coleman, Melinda A/R-5563-2016; OI Parsons, Edward Christien/0000-0002-0464-1046; Coleman, Melinda A/0000-0003-2623-633X; Sutherland, William/0000-0002-6498-0437; Wright, Andrew/0000-0002-8718-8143; Kelaher, Brendan/0000-0002-7505-4412 FU Society for Conservation Biology's (SCB) Marine Section FX We are grateful to the Society for Conservation Biology's (SCB) Marine Section for funding this exercise. We thank all individuals who submitted questions and who participated in the workshops, as well as the anonymous reviewers whose contributions improved this manuscript. The authors of this paper are all members of the SCB Biology Marine Section Board of Directors or Publications Committee. This paper was edited and submitted in accordance with direction from A. Hummer, SCB's Executive Director, R. Primark, and SCB's legal counsel, and we thank them for their advice. NR 60 TC 17 Z9 17 U1 7 U2 71 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 2014 VL 28 IS 5 BP 1206 EP 1214 DI 10.1111/cobi.12303 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ3DH UT WOS:000342668700011 PM 24779474 ER PT J AU Holmes, I Potvin, C AF Holmes, Ignacia Potvin, Catherine TI Avoiding Re-Inventing the Wheel in a People-Centered Approach to REDD SO CONSERVATION BIOLOGY LA English DT Article DE best practices; community-based conservation; conservation; forest carbon; REDD plus implementation; rural development ID CONCEPTUAL-FRAMEWORK; FOREST GOVERNANCE; HUMAN-NEEDS; CONSERVATION; COMMUNITY; DEFORESTATION; PARTICIPATION; BENEFITS; LESSONS; PLUS AB One important debate regarding Reducing Emissions from Deforestation and Forest Degradation (REDD+) in developing countries concerns the manner in which its implementation might affect local and indigenous communities. New ways to implement this mechanism without harming the interests of local communities are emerging. To inform this debate, we conducted a qualitative research synthesis to identify best practices (BPs) from people-centered approaches to conservation and rural development, developed indicators of BPs, and invited development practitioners and researchers in the field to assess how the identified BPs are being adopted by community-level REDD+ projects in Latin America. BPs included: local participation in all phases of the project; project supported by a decentralized forest governance framework; project objectives matching community livelihood priorities; project addressing community development needs and expectations; project enhancing stakeholder collaboration and consensus building; project applying an adaptive management approach; and project developing national and local capacities. Most of the BPs were part of the evaluated projects. However, limitations of some of the projects related to decentralized forest governance, matching project objectives with community livelihood priorities, and addressing community development needs. Adaptive management and free and prior informed consent have been largely overlooked. These limitations could be addressed by integrating conservation outcomes and alternative livelihoods into longer-term community development goals, testing nested forest governance approaches in which national policies support local institutions for forest management, gaining a better understanding of the factors that will make REDD+ more acceptable to local communities, and applying an adaptive management approach that allows for social learning and capacity building of relevant stakeholders. Our study provides a framework of BPs and indicators that could be used by stakeholders to improve REDD+ project design, monitoring, and evaluation, which may help reconcile national initiatives and local interests without reinventing the wheel. C1 [Holmes, Ignacia; Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Holmes, I (reprint author), McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM ignacia.holmes@mail.mcgill.ca FU Comision Nacional de Investigacion Cientifica y Tecnologica, Gobierno de Chile (CONYCIT) FX We thank all those who evaluated the REDD+ projects. We are also grateful for the 2 anonymous reviewers for their comprehensive reading and remarks that greatly improved this manuscript. We also thank O. Coomes, J. Correa, A. Jacob, K. Kirby, J. Mateo-Vega, W. F. J. Parsons, D. Ross, C. Salisbury, D. Sharma, S. Wilson, and S. Wood for their useful comments and review of this document. Thanks to the Comision Nacional de Investigacion Cientifica y Tecnologica, Gobierno de Chile (CONYCIT) for the scholarship provided to L.I. Holmes. NR 51 TC 2 Z9 2 U1 2 U2 53 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 EI 1523-1739 J9 CONSERV BIOL JI Conserv. Biol. PD OCT PY 2014 VL 28 IS 5 BP 1380 EP 1393 DI 10.1111/cobi.12301 PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ3DH UT WOS:000342668700027 PM 24762062 ER PT J AU Slot, M Rey-Sanchez, C Winter, K Kitajima, K AF Slot, Martijn Rey-Sanchez, Camilo Winter, Klaus Kitajima, Kaoru TI Trait-based scaling of temperature-dependent foliar respiration in a species-rich tropical forest canopy SO FUNCTIONAL ECOLOGY LA English DT Article DE carbon flux; climate change; gas exchange; leaf functional traits; NPP; Panama; Q(10); temperature response of respiration ID LEAF-AREA INDEX; GLOBAL VEGETATION MODEL; CARBON USE EFFICIENCY; RAIN-FOREST; DARK RESPIRATION; EDDY COVARIANCE; ECOSYSTEM RESPIRATION; CHAMBER MEASUREMENTS; THERMAL-ACCLIMATION; ECONOMICS SPECTRUM AB 1. The scarcity of empirical data on leaf respiration (R) and its temperature sensitivity (e.g. Q(10), defined as the proportional increase in R per 10 degrees C warming) causes uncertainty in current estimates of net primary productivity of tropical forests. 2. We measured temperature response curves of R on 123 upper-canopy leaves of 28 species of trees and lianas from a tropical forest in Panama and analysed variations in R and Q(10) in relation to other leaf functional traits. 3. Respiration rates per leaf area at 25 degrees C (R-A) varied widely among species and were significantly higher in trees than in lianas. R-A was best predicted by a multiple regression model containing leaf phosphorus concentration, photosynthetic capacity and leaf mass per area (r(2)=064). The mean Q(10) value (24) was significantly higher than the commonly assumed value of 20. Q(10) was best predicted by the combination of leaf carbohydrate concentration and growth form (trees vs lianas) (r(2)=026). 4. The night-time leaf respiratory carbon flux from this tropical forest was calculated from these multiple regression models to be 45MgCha(-1)year(-1), with an estimated additional 29MgCha(-1)year(-1) being released by respiration during the day. 5. Trait-based modelling has potential for estimating R, thus facilitating carbon flux estimation in species-rich tropical forests. However, in contrast to global analyses, leaf phosphorus content was the most important correlate of R and not leaf nitrogen, so calibration of trait models to the tropics will be important. Leaf traits are poor predictors of Q(10) values, and more empirical data on the temperature sensitivity of respiration are critically needed to further improve our ability to scale temperature-dependent respiration in species-rich tropical forests. C1 [Slot, Martijn; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Slot, Martijn; Rey-Sanchez, Camilo; Winter, Klaus; Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa 084303092, Panama. Univ Rosario, Facultad Ciencias Natur Matemat, Cr 24 63C 69, Bogota 111221, DC, Colombia. RP Slot, M (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM martijnslot78@gmail.com FU NSF-IOS [1051789] FX We thank crane operators Edwin Andrade and Julio Piti, and Danielle Palow, Camila Pizano and Grace Crummer for assistance in the laboratory. We are grateful to SJ Wright for sharing unpublished phosphorus data and to Lourens Poorter and two anonymous reviewers for thoughtful comments on an earlier version of this paper. Financial support came from NSF-IOS grant 1051789. NR 56 TC 9 Z9 9 U1 10 U2 42 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD OCT PY 2014 VL 28 IS 5 BP 1074 EP 1086 DI 10.1111/1365-2435.12263 PG 13 WC Ecology SC Environmental Sciences & Ecology GA AQ2KR UT WOS:000342615100003 ER PT J AU Johnson, CI Rich, RM Kobayashi, C Kunder, A Koch, A AF Johnson, Christian I. Rich, R. Michael Kobayashi, Chiaki Kunder, Andrea Koch, Andreas TI LIGHT, ALPHA, AND Fe-PEAK ELEMENT ABUNDANCES IN THE GALACTIC BULGE SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: bulge; stars: abundances; stars: Population II ID MILKY-WAY BULGE; FLAMES-GIRAFFE SPECTRA; RADIAL-VELOCITY ASSAY; METAL-POOR STARS; HIGH-RESOLUTION SPECTRUM; 1ST DETAILED ABUNDANCES; BAADES WINDOW GIANTS; KECK HIRES SPECTRA; LTE LINE FORMATION; CLUSTER NGC 6553 AB We present radial velocities and chemical abundances of O, Na, Mg, Al, Si, Ca, Cr, Fe, Co, Ni, and Cu for a sample of 156 red giant branch stars in two Galactic bulge fields centered near (l, b) = (+5.25, -3.02) and (0, -12). The (+5.25, -3.02) field also includes observations of the bulge globular cluster NGC 6553. The results are based on high-resolution (R similar to 20,000), high signal-to-noise ration (S/N greater than or similar to 70) FLAMES-GIRAFFE spectra obtained through the European Southern Observatory archive. However, we only selected a subset of the original observations that included spectra with both high S/N and that did not show strong TiO absorption bands. This work extends previous analyses of this data set beyond Fe and the alpha-elements Mg, Si, Ca, and Ti. While we find reasonable agreement with past work, the data presented here indicate that the bulge may exhibit a different chemical composition than the local thick disk, especially at [Fe/H] greater than or similar to -0.5. In particular, the bulge [alpha/Fe] ratios may remain enhanced to a slightly higher [Fe/H] than the thick disk, and the Fe-peak elements Co, Ni, and Cu appear enhanced compared to the disk. There is also some evidence that the [Na/Fe] (but not [Al/Fe]) trends between the bulge and local disk may be different at low and high metallicity. We also find that the velocity dispersion decreases as a function of increasing [Fe/H] for both fields, and do not detect any significant cold, high-velocity populations. A comparison with chemical enrichment models indicates that a significant fraction of hypernovae may be required to explain the bulge abundance trends, and that initial mass functions that are steep, top-heavy (and do not include strong outflow), or truncated to avoid including contributions from stars >40 M-circle dot are ruled out, in particular because of disagreement with the Fe-peak abundance data. For most elements, the NGC 6553 stars exhibit abundance trends nearly identical to comparable metallicity bulge field stars. However, the star-to-star scatter and mean [Na/Fe] ratios appear higher in the cluster, perhaps indicating additional self-enrichment. C1 [Johnson, Christian I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rich, R. Michael] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Kobayashi, Chiaki] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Kunder, Andrea] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Koch, Andreas] Heidelberg Univ, Zentrum Astronom, Heidelberg, Germany. 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; c.kobayashi@herts.ac.uk; akunder@aip.de; akoch@lsw.uni-heidelberg.de OI Kunder, Andrea/0000-0002-2808-1370; Koch, Andreas/0000-0002-9859-4956 FU National Aeronautics and Space Administration; National Science Foundation; Clay Fellowship; Deutsche Forschungsgemeinschaft [Ko 4161/1]; [NSF-AST-1212095] FX We thank the anonymous referee for a careful reading of the manuscript and helpful comments that led to improvement of the manuscript. This research has made use of NASA's Astrophysics Data System Bibliographic Services. 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. C.I.J. gratefully acknowledges support from the Clay Fellowship, administered by the Smithsonian Astrophysical Observatory. R.M.R. acknowledges support from NSF-AST-1212095. A.K. acknowledges the Deutsche Forschungsgemeinschaft for funding from Emmy-Noether grant Ko 4161/1. NR 115 TC 33 Z9 33 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD OCT PY 2014 VL 148 IS 4 AR 67 DI 10.1088/0004-6256/148/4/67 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP7BU UT WOS:000342233400009 ER PT J AU Ramos, AG Nunziata, SO Lance, SL Rodriguez, C Faircloth, BC Gowaty, PA Drummond, H AF Ramos, Alejandra G. Nunziata, Schyler O. Lance, Stacey L. Rodriguez, Cristina Faircloth, Brant C. Gowaty, Patricia Adair Drummond, Hugh TI Interactive effects of male and female age on extra-pair paternity in a socially monogamous seabird SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Age; Female choice; Extra-pair paternity; Extra-pair sire; Infertility; Good genes ID BLUE-FOOTED BOOBY; SULA-NEBOUXII; SEXUAL SELECTION; GOOD GENES; EASTERN BLUEBIRDS; SIALIA-SIALIS; OLDER MALES; TRADE-OFFS; SENESCENCE; BIRDS AB Females sometimes obtain older sires for their offspring through extra-pair interactions, but how female age influences paternity is largely unexplored and interactive effects across the age span of both sexes have not been analyzed. To test whether female choice of sire age varies with female age in the blue-footed booby (Sula nebouxii), we examined associations between ages of both partners and the probability of extra-pair paternity (EPP) in 350 broods of parents up to 22 years old in a single breeding season. Extra-pair paternity enables a female to select an alternative sire for her offspring and could function to avoid or achieve particular combinations of parental ages. A male age x female age interaction revealed that in young females (a parts per thousand currency sign4 years), EPP decreased with increasing age of the social partner, whereas in old females (a parts per thousand yen8 years), it increased. Moreover, sires of extra-pair (EP) chicks of young females paired to young males were on average 6.33 years older than the females' social partners. Since female boobies control copulatory access, this pattern could imply that young females choose old sires for their proven genetic quality and that old females avoid very old males because matings with them may risk infertility or genetic defects in offspring. Taking female age into account and observing across the whole age span may be necessary for understanding female age-based mate choice. C1 [Ramos, Alejandra G.; Rodriguez, Cristina; Drummond, Hugh] Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol Evolut, Mexico City 04510, DF, Mexico. [Nunziata, Schyler O.; Lance, Stacey L.] Univ Georgia, Savannah River Ecol Lab, Aiken, SC USA. [Nunziata, Schyler O.] Univ Kentucky, Dept Biol, Lexington, KY USA. [Faircloth, Brant C.; Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. [Gowaty, Patricia Adair] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Washington, DC USA. RP Ramos, AG (reprint author), Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol Evolut, AP 70-275, Mexico City 04510, DF, Mexico. EM ramos.alejndra@gmail.com RI Lance, Stacey/K-9203-2013; OI Lance, Stacey/0000-0003-2686-1733; Faircloth, Brant/0000-0002-1943-0217 FU Universidad Nacional Autonoma de Mexico (PAPIIT) [IN206610]; Consejo Nacional de Ciencia y Tecnologia [104313]; Universidad Nacional Autonoma de Mexico; US Department of Energy [DEF C090 7SR22506] FX Simon C. Griffith, Lynna M. Kiere, Marcela Osorio-Beristain, Diana Perez-Staples, Oscar Sanchez-Macouzet, and two anonymous reviewers provided helpful comments on the manuscript. We thank numerous volunteers and colleagues who helped in the field and lab, especially Santiago Bautista-Lopez, Jonathan P. Drury, Gabriela Lopez-Carapia, and Janeth Rosas-Morales. The Armada de Mexico, local fishermen, and staff of the Parque Nacional Isla Isabel supplied vital and much appreciated logistical support. This study was financed by the Universidad Nacional Autonoma de Mexico (PAPIIT, IN206610) and the Consejo Nacional de Ciencia y Tecnologia (104313). This manuscript constitutes a partial fulfillment of the Graduate Program in Biomedical Sciences of the Universidad Nacional Autonoma de Mexico. AGR wishes to acknowledge the scholarship and financial support provided by the Consejo Nacional de Ciencia y Tecnologia and the Universidad Nacional Autonoma de Mexico. This research was partially supported by US Department of Energy under award number DEF C090 7SR22506 to the University of Georgia Research Foundation. NR 53 TC 4 Z9 4 U1 10 U2 43 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 OCT PY 2014 VL 68 IS 10 BP 1603 EP 1609 DI 10.1007/s00265-014-1769-9 PG 7 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA AP6ZC UT WOS:000342226200006 ER PT J AU Byers, BA Ash, SR Chaney, D DeSoto, L AF Byers, Bruce A. Ash, Sidney R. Chaney, Dan DeSoto, Lucia TI First known fire scar on a fossil tree trunk provides evidence of Late Triassic wildfire SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Fire scar; Late Triassic; Wood anatomy; Paleoecology; Chinle Formation ID FOREST NATIONAL-PARK; TRAUMATIC RESIN DUCTS; DEBRIS-FLOW ACTIVITY; LARIX-DECIDUA; CHINLE FORMATION; TANGENTIAL ROWS; WOOD ANATOMY; ARIZONA; GROWTH; HISTORY AB Fire scars are well known to fire ecologists and dendrochronologists worldwide, and are used in dating fires and reconstructing the fire histories of modern forests. Evidence of fires in ancient forests, such as fossil charcoal (fusain), is well known to paleontologists and has been reported in geologic formations dating back to the Late Devonian. We describe what we conclude is a fire scar on a fossil tree trunk from the Late Triassic Chinle Formation of southeastern Utah (similar to 200-225 Ma). The external features of the prehistoric scar match those of modern fire scars better than those of scars created by other kinds of wounding events. The fossil specimen also exhibits a number of changes in wood anatomy similar to those reported in modern fire-scarred trees, including a band of very small tracheids that indicate growth suppression immediately associated with the scarring event; an area with a tangential row of probable traumatic resin ducts; and a significant increase in tracheid size following the scarring event that indicates a growth release. No fire scar resembling those in modern trees has previously been described in petrified wood as far as we can determine. The presence of a fire scar not only provides further evidence of ancient fires, but also shows that at least some individual trees survived them, indicating that fire could have been an ecological and evolutionary force in forests at least as early as the late Triassic. (c) 2014 Elsevier B.V. All rights reserved. C1 [Byers, Bruce A.] Bruce Byers Consulting, Falls Church, VA 22046 USA. [Ash, Sidney R.] Univ New Mexico, Dept Earth & Planetary Sci, Albuquerque, NM 87131 USA. [Chaney, Dan] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [DeSoto, Lucia] Univ Coimbra, Dept Life Sci, Ctr Funct Ecol, P-3001401 Coimbra, Portugal. RP Byers, BA (reprint author), Bruce Byers Consulting, 405 Timber Lane, Falls Church, VA 22046 USA. EM bruce.byers@verizon.net RI DeSoto, Lucia/B-6196-2009 OI DeSoto, Lucia/0000-0002-5814-5865 FU Portuguese Fundacao para a Ciencia e a Tecnologia [SFRH/BPD/70632/2010] FX The lead author would like to thank his late father, Cleo Byers, for safeguarding the specimen from the time it was found in the 1980s until his work with fire ecologists allowed him to recognize the characteristics of fire scars. The authors wish to thank pyrodendrochronologists Erica Bigio, Peter Brown, Henri Grissino-Mayer, Mauro Gonzalez, Laurie Huckaby, Rosemary Sherriff, Thomas Swetnam, and Thomas Veblen for independent assessments of the characteristics of the scar on this specimen; Anne-Laure Decombeix, Marc Philippe, and Rodney Savidge for discussions of fossil wood anatomy and identification; Anya and Jonathan Byers for assistance with image preparation; and William Parker for initial contacts to paleobotanists. We would also like to thank Markus Stoffel for constructive comments on an earlier version of the manuscript. Lucia DeSoto was supported by a postdoctoral fellowship from the Portuguese Fundacao para a Ciencia e a Tecnologia (SFRH/BPD/70632/2010). NR 65 TC 3 Z9 3 U1 2 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 EI 1872-616X J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD OCT 1 PY 2014 VL 411 BP 180 EP 187 DI 10.1016/j.palaeo.2014.06.009 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AP7PM UT WOS:000342269200016 ER PT J AU Ielpi, A Gibling, MR Bashforth, AR Lally, C Rygel, MC Al-Silwadi, S AF Ielpi, Alessandro Gibling, Martin R. Bashforth, Arden R. Lally, Corinne Rygel, Michael C. Al-Silwadi, Saif TI Role of vegetation in shaping Early Pennsylvanian braided rivers: Architecture of the Boss Point Formation, Atlantic Canada SO SEDIMENTOLOGY LA English DT Article DE Architecture; Carboniferous; fluvial; log jam; palaeobotany; vegetation ID LARGE WOODY DEBRIS; SOUTH SASKATCHEWAN RIVER; LOWER PLATTE RIVER; NOVA-SCOTIA; JOGGINS FORMATION; CUMBERLAND BASIN; SEDIMENTARY STRUCTURES; CORDAITALEAN TREES; MARITIME CANADA; ALLUVIAL ARCHITECTURE AB Vegetation is a major driver of fluvial dynamics in modern rivers, but few facies models incorporate its influence. This article partially fills that gap by documenting the stratigraphy, architecture and palaeobotany of the Lower Pennsylvanian Boss Point Formation of Atlantic Canada, which contains some of the Earth's earliest accumulations of large woody debris. Braided-fluvial systems occupied channel belts of varied scale within valleys several tens of metres deep and more than 12km wide, and their deposits predominantly consist of sandy and gravelly bedforms with subordinate accretionary macroforms, high flow-strength sand sheets and rippled abandonment facies. Discrete accumulations of clastic detritus and woody debris are up to 6m thick and constitute at least 18% of the in-channel deposits; they represent lags at the base of large and small channels, fills of minor channels and sandy macroforms that developed in central positions in the upper parts of channel fills. Sandstones with roots and other remnants of in situ vegetation demonstrate that vegetated islands were present, and the abundance of discrete channel fills suggests that the formation represents an anabranching, island-braided sandbed river, the earliest example documented to date. Although some sphenopsid and lycopsid remains are present, most woody fragments are derived from cordaitalean trees, and the evolution of this group late in the Mississippian is inferred to have exerted a significant influence on fluvial morphodynamic patterns. The formation records a landscape in which active channel belts alternated with well-drained floodplains colonized by dense, mature forests and local patches of pioneering, disturbance-tolerant vegetation. Lakes and poorly drained floodplains dominated by carbonate and organic deposition, respectively, were also present. A large supply of woody debris triggered channel blockage and avulsion, and active channel margins and islands within the channel belts were initially colonized by pioneer vegetation and subsequently stabilized by large trees. A similar alternation of stable and unstable conditions is observed in modern braided rivers actively influenced by vegetation. C1 [Ielpi, Alessandro] Univ Siena, Dept Earth Sci, I-53100 Siena, Italy. [Gibling, Martin R.; Al-Silwadi, Saif] Dalhousie Univ, Dept Earth Sci, Halifax, NS B3H 4R2, Canada. [Bashforth, Arden R.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Lally, Corinne; Rygel, Michael C.] SUNY Coll Potsdam, Dept Geol, Potsdam, NY 13676 USA. RP Ielpi, A (reprint author), Univ Siena, Dept Earth Sci, Via Laterina 8, I-53100 Siena, Italy. EM ielpi@unisi.it FU International Association of Sedimentologists; Natural Sciences and Engineering Research Council of Canada (NSERC); NSERC; American Chemical Society Petroleum Research Fund Grant [47967-GB8] FX Rhea Hurnik and Brian Hebert offered crucial field support to this study. The Joggins Fossil Centre and particularly Jenna Boon are also acknowledged for helpful cooperation. The authors are greatly indebted to reviewers John Holbrook and Guy Plint for constructive comments that significantly improved the manuscript. Likewise, Associate Editor Nigel Mountney and Editor Stephen Rice are warmly thanked for their assistance. The study was supported by an International Association of Sedimentologists Post-Graduate grant to Alessandro Ielpi, a Discovery Grant from the Natural Sciences and Engineering Research Council of Canada (NSERC) to Martin R. Gibling, a Postdoctoral Fellowship from NSERC to Arden R. Bashforth, and an American Chemical Society Petroleum Research Fund Grant (#47967-GB8) to Michael C. Rygel. NR 180 TC 19 Z9 19 U1 0 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0037-0746 EI 1365-3091 J9 SEDIMENTOLOGY JI Sedimentology PD OCT PY 2014 VL 61 IS 6 BP 1659 EP 1700 DI 10.1111/sed.12109 PG 42 WC Geology SC Geology GA AP8SL UT WOS:000342349100007 ER PT J AU Brown, JK AF Brown, Julie K. TI Connecting Health and Natural History A Failed Initiative at the American Museum of Natural History, 1909-1922 SO AMERICAN JOURNAL OF PUBLIC HEALTH LA English DT Editorial Material AB In 1909, curator Charles-Edward Winslow established a department of public health in New York City's American Museum of Natural History (AMNH). Winslow introduced public health as a biological science that connected human health-the modern sciences of physiology, hygiene, and urban sanitation-to the natural history of plants and animals. This was the only time an American museum created a curatorial department devoted to public health. The AMNH's Department of Public Health comprised a unique collection of live bacterial cultures-a "Living Museum"-and an innovative plan for 15 exhibits on various aspects of health. I show how Winslow, facing opposition from AMNH colleagues, gathered scientific experts and financial support, and explain the factors that made these developments seem desirable and possible. I finish with a discussion of how the Department of Public Health met an abrupt and "inglorious end" in 1922 despite the success of its collections and exhibitions. C1 [Brown, Julie K.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. [Brown, Julie K.] Univ Texas Hlth Sci Ctr San Antonio, Ctr Med Humanities & Eth, San Antonio, TX 78229 USA. RP Brown, JK (reprint author), 4021 Tealwood Dr, Austin, TX 78731 USA. EM mail@juliekbrown.com NR 0 TC 0 Z9 0 U1 1 U2 4 PU AMER PUBLIC HEALTH ASSOC INC PI WASHINGTON PA 800 I STREET, NW, WASHINGTON, DC 20001-3710 USA SN 0090-0036 EI 1541-0048 J9 AM J PUBLIC HEALTH JI Am. J. Public Health PD OCT PY 2014 VL 104 IS 10 BP 1877 EP 1888 DI 10.2105/AJPH.2013.301384 PG 12 WC Public, Environmental & Occupational Health SC Public, Environmental & Occupational Health GA AP1XG UT WOS:000341865000031 PM 24205997 ER PT J AU Chen, JH Goldsmith, PF Viti, S Snell, R Lis, DC Benz, A Bergin, E Black, J Caselli, P Encrenaz, P Falgarone, E Goicoechea, JR Hjalmarson, A Hollenbach, D Kaufman, M Melnick, G Neufeld, D Pagani, L van der Tak, F van Dishoeck, E Yildiz, UA AF Chen, Jo-Hsin Goldsmith, Paul F. Viti, Serena Snell, Ronald Lis, Dariusz C. Benz, Arnold Bergin, Edwin Black, John Caselli, Paola Encrenaz, Pierre Falgarone, Edith Goicoechea, Javier R. Hjalmarson, Ake Hollenbach, David Kaufman, Michael Melnick, Gary Neufeld, David Pagani, Laurent van der Tak, Floris van Dishoeck, Ewine Yildiz, Umut A. TI HERSCHEL HIFI OBSERVATIONS OF O-2 TOWARD ORION: SPECIAL CONDITIONS FOR SHOCK ENHANCED EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: molecules; shock waves ID INTERSTELLAR MOLECULAR CLOUDS; WAVE-ASTRONOMY-SATELLITE; TEMPORAL EVOLUTION; HOT CORE; APERTURE SYNTHESIS; COLOGNE DATABASE; STAR-FORMATION; MASSIVE STARS; RHO-OPHIUCHI; LINE SURVEY AB We report observations of molecular oxygen (O-2) rotational transitions at 487 GHz, 774 GHz, and 1121 GHz toward Orion Peak A. The O-2 lines at 487 GHz and 774 GHz are detected at velocities of 10-12 km s(-1) with line widths similar to 3 km s(-1); however, the transition at 1121 GHz is not detected. The observed line characteristics, combined with the results of earlier observations, suggest that the region responsible for the O-2 emission is similar or equal to 9" (6 x 10(16) cm) in size, and is located close to the H-2 Peak 1 position (where vibrationally excited H-2 emission peaks), and not at Peak A, 23" away. The peak O-2 column density is similar to 1.1 x 10(18) cm(-2). The line velocity is close to that of the 621 GHz water maser emission found in this portion of the Orion Molecular Cloud, and having a shock with velocity vector lying nearly in the plane of the sky is consistent with producing maximum maser gain along the line of sight. The enhanced O-2 abundance compared to that generally found in dense interstellar clouds can be explained by passage of a low-velocity C shock through a clump with preshock density 2 x 10(4) cm(-3), if a reasonable flux of UV radiation is present. The postshock O-2 can explain the emission from the source if its line-of-sight dimension is similar or equal to 10 times larger than its size on the plane of the sky. The special geometry and conditions required may explain why O-2 emission has not been detected in the cores of other massive star-forming molecular clouds. C1 [Chen, Jo-Hsin; Goldsmith, Paul F.; Yildiz, Umut A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Viti, Serena] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Snell, Ronald] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Lis, Dariusz C.] CALTECH, Pasadena, CA 91125 USA. [Lis, Dariusz C.] Sorbonne Univ, Univ Paris 06, CNRS, Observ Paris,UMR 8112,LERMA, Paris, France. [Benz, Arnold] ETH, Inst Astron, CH-8092 Zurich, Switzerland. [Bergin, Edwin] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Black, John; Hjalmarson, Ake] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, SE-43992 Onsala, Sweden. [Caselli, Paola; van Dishoeck, Ewine] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Encrenaz, Pierre; Falgarone, Edith] Observ Paris, UMR8112, CNRS, LRA LERMA, F-75231 Paris 05, France. [Encrenaz, Pierre; Falgarone, Edith] Ecole Normale Super, F-75231 Paris 05, France. [Goicoechea, Javier R.] Inst Ciencia Mat Madrid ICMM CSIC, E-28049 Madrid, Spain. [Hollenbach, David] SETI Inst, Mountain View, CA 94043 USA. [Kaufman, Michael] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Melnick, Gary] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neufeld, David] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Pagani, Laurent] Observ Paris, CNRS, LERMA, F-75014 Paris, France. [Pagani, Laurent] Observ Paris, CNRS, UMR8112, F-75014 Paris, France. [van der Tak, Floris] SRON, Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, Groningen, Netherlands. [van Dishoeck, Ewine] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Chen, JH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Yildiz, Umut/C-5257-2011; Goldsmith, Paul/H-3159-2016; OI Yildiz, Umut/0000-0001-6197-2864; Black, John/0000-0001-7221-7207 FU Spanish MINECO [CSD2009-00038, AYA2009-07304, AYA2012-32032] FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States ( NASA) under the leadership of SRON, Netherlands Institute for Space Research, Groningen, TheNetherlands, and with major contributions from Germany, France, and the US. This work was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology. J.R.G. thanks the Spanish MINECO for funding support under grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. We thank Shiya Wang, Nathan Crockett, and the NASA Herschel Science Center Helpdesk for the help with the data reduction. We appreciate the help from Justin Neill with installing and using XCLASS. We thank Tzu-Cheng Peng for providing the CO map used in Figure 1. We thank the anonymous reviewer for a number of suggestions that improved the clarity of the paper. NR 63 TC 9 Z9 9 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 OCT 1 PY 2014 VL 793 IS 2 AR 111 DI 10.1088/0004-637X/793/2/111 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300042 ER PT J AU Chitta, LP Kariyappa, R van Ballegooijen, AA DeLuca, EE Solanki, SK AF Chitta, L. P. Kariyappa, R. van Ballegooijen, A. A. DeLuca, E. E. Solanki, S. K. TI NONLINEAR FORCE-FREE FIELD MODELING OF THE SOLAR MAGNETIC CARPET AND COMPARISON WITH SDO/HMI AND SUNRISE/IMAX OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: corona; Sun: magnetic fields; Sun: photosphere ID CORONAL BRIGHT POINTS; QUIET-SUN CORONA; EXTREME-ULTRAVIOLET; ENERGY-FLOW; DYNAMICS; CANCELLATION; LOOPS; CHROMOSPHERE; RECONNECTION; INTERNETWORK AB In the quiet solar photosphere, the mixed polarity fields form a magnetic carpet that continuously evolves due to dynamical interaction between the convective motions and magnetic field. This interplay is a viable source to heat the solar atmosphere. In this work, we used the line-of-sight (LOS) magnetograms obtained from the Helioseismic and Magnetic Imager on the Solar Dynamics Observatory, and the Imaging Magnetograph eXperiment instrument on the Sunrise balloon-borne observatory, as time-dependent lower boundary conditions, to study the evolution of the coronal magnetic field. We use a magneto-frictional relaxation method, including hyperdiffusion, to produce a time series of three-dimensional nonlinear force-free fields from a sequence of photospheric LOS magnetograms. Vertical flows are added up to a height of 0.7 Mm in the modeling to simulate the non-force-freeness at the photosphere-chromosphere layers. Among the derived quantities, we study the spatial and temporal variations of the energy dissipation rate and energy flux. Our results show that the energy deposited in the solar atmosphere is concentrated within 2 Mm of the photosphere and there is not sufficient energy flux at the base of the corona to cover radiative and conductive losses. Possible reasons and implications are discussed. Better observational constraints of the magnetic field in the chromosphere are crucial to understand the role of the magnetic carpet in coronal heating. C1 [Chitta, L. P.; Kariyappa, R.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Chitta, L. P.; van Ballegooijen, A. A.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Solanki, S. K.] Max Planck Inst Sonnensyst Forsch, D-37077 Gottingen, Germany. [Solanki, S. K.] Kyung Hee Univ, Sch Space Res, Yongin 446701, Gyeonggi Do, South Korea. RP Chitta, LP (reprint author), Indian Inst Astrophys, Bangalore 560034, Karnataka, India. RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Chitta, Lakshmi Pradeep/0000-0002-9270-6785 FU NASA [NNM07AB07C] FX The authors thank the referee for many comments and suggestions that helped in improving the presentation of the work. L.P.C. was a 2011-2013 SAO Pre-Doctoral Fellow at the Harvard-Smithsonian Center for Astrophysics. Funding for L.P.C. and E.E.D. is provided by NASA contract NNM07AB07C. Courtesy of NASA/SDO and the AIA and HMI science teams. This research has made use of NASA's Astrophysics Data System. NR 50 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 OCT 1 PY 2014 VL 793 IS 2 AR 112 DI 10.1088/0004-637X/793/2/112 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300043 ER PT J AU Hora, JL Witzel, G Ashby, MLN Becklin, EE Carey, S Fazio, GG Ghez, A Ingalls, J Meyer, L Morris, MR Smith, HA Willner, SP AF Hora, J. L. Witzel, G. Ashby, M. L. N. Becklin, E. E. Carey, S. Fazio, G. G. Ghez, A. Ingalls, J. Meyer, L. Morris, M. R. Smith, H. A. Willner, S. P. TI SPITZER/IRAC OBSERVATIONS OF THE VARIABILITY OF Sgr A* AND THE OBJECT G2 AT 4.5 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: center; techniques: photometric ID CENTER CLOUD G2; SUPERMASSIVE BLACK-HOLE; INFRARED ARRAY CAMERA; X-RAY FLARES; GALACTIC-CENTER; SAGITTARIUS-A; SPACE-TELESCOPE; GAS CLOUD; MILKY-WAY; SIMULATIONS AB We present the first detection from the Spitzer Space Telescope of 4.5 mu m variability from Sgr A*, the emitting source associated with the Milky Way's central black hole. The >23 hr continuous light curve was obtained with the Infrared Array Camera (IRAC) instrument in 2013 December. The result characterizes the variability of Sgr A* prior to the closest approach of the tidally deformed G2 object, a putative infalling gas cloud that orbits close to Sgr A*. The high stellar density at the location of Sgr A* produces a background of similar to 250 mJy at 4.5 mu m in each pixel with a large pixel-to-pixel gradient, but the light curve for the highly variable Sgr A* source was successfully measured by modeling and removing the variations due to pointing wobble. The observed flux densities range from the noise level of similar to 0.7 mJy rms in a 6.4 s measurement to greater than or similar to 10 mJy. Emission was seen above the noise level similar to 34% of the time. The light-curve characteristics, including the flux density distribution and structure function, are consistent with those previously derived at shorter infrared wavelengths. We see no evidence in the light curve for activity attributable to the G2 interaction at the observing epoch, similar to 100 days before the expected G2 periapsis passage. The IRAC light curve is more than a factor of two longer than any previous infrared observation, improving constraints on the timescale of the break in the power spectral distribution of Sgr A* flux densities. The data favor the longer of the two previously published values for the timescale. C1 [Hora, J. L.; Ashby, M. L. N.; Fazio, G. G.; Smith, H. A.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Witzel, G.; Becklin, E. E.; Ghez, A.; Meyer, L.; Morris, M. R.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Becklin, E. E.] SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Carey, S.; Ingalls, J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Hora, JL (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA through JPL/Caltech; NSF [AST 09-09218]; European Union [MP0905, 98040] 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 a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. A.G. acknowledges support from NSF grant AST 09-09218. G.W. acknowledges the European Union funded COST Action MP0905: Black Holes in a violent Universe and PECS project No. 98040. We thank the staff of the Spitzer Science Center for their help in planning and executing these demanding observations. We thank Keith Matthews and Arno Witzel for fruitful discussions. NR 56 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 OCT 1 PY 2014 VL 793 IS 2 AR 120 DI 10.1088/0004-637X/793/2/120 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300051 ER PT J AU Kenyon, SJ Bromley, BC Brown, WR Geller, MJ AF Kenyon, Scott J. Bromley, Benjamin C. Brown, Warren R. Geller, Margaret J. TI PREDICTED SPACE MOTIONS FOR HYPERVELOCITY AND RUNAWAY STARS: PROPER MOTIONS AND RADIAL VELOCITIES FOR THE GAIA Era SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: stellar content; Galaxy: structure; stars: early-type ID DYNAMICALLY EJECTED RUNAWAY; HORIZONTAL-BRANCH STARS; SAGITTARIUS-A-ASTERISK; LARGE-MAGELLANIC-CLOUD; MASSIVE BLACK-HOLE; MILKY-WAY HALO; GALACTIC-CENTER; B-STARS; SOLAR NEIGHBORHOOD; DENSITY PROFILE AB We predict the distinctive three-dimensional space motions of hypervelocity stars (HVSs) and runaway stars moving in a realistic Galactic potential. For nearby stars with distances less than 10 kpc, unbound stars are rare; proper motions alone rarely isolate bound HVSs and runaways from indigenous halo stars. At large distances of 20-100 kpc, unbound HVSs are much more common than runaways; radial velocities easily distinguish both from indigenous halo stars. Comparisons of the predictions with existing observations are encouraging. Although the models fail to match observations of solar-type HVS candidates from SEGUE, they agree well with data for B-type HVS and runaways from other surveys. Complete samples of g less than or similar to 20 stars with Gaia should provide clear tests of formation models for HVSs and runaways and will enable accurate probes of the shape of the Galactic potential. C1 [Kenyon, Scott J.; Brown, Warren R.; Geller, Margaret 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; wbrown@cfa.harvard.edu; mgeller@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X; Geller, Margaret/0000-0002-9146-4876 NR 88 TC 7 Z9 7 U1 0 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 OCT 1 PY 2014 VL 793 IS 2 AR 122 DI 10.1088/0004-637X/793/2/122 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300053 ER PT J AU Naoz, S Fabrycky, DC AF Naoz, Smadar Fabrycky, Daniel C. TI MERGERS AND OBLIQUITIES IN STELLAR TRIPLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: general; blue stragglers; stars: general; stars: kinematics and dynamics ID HIERARCHICAL 3-BODY SYSTEMS; ECCENTRIC KOZAI MECHANISM; MULTIPLE-STAR SYSTEMS; SPIN-ORBIT ALIGNMENT; BLACK-HOLE BINARIES; SOLAR-TYPE STARS; CLUSTER NGC 188; BLUE STRAGGLERS; HOT JUPITERS; GLOBULAR-CLUSTERS AB Many close stellar binaries are accompanied by a faraway star. The "eccentric Kozai-Lidov" (EKL) mechanism can cause dramatic inclination and eccentricity fluctuations, resulting in tidal tightening of inner binaries of triple stars. We run a large set of Monte Carlo simulations, including the secular evolution of the orbits, general relativistic precession, and tides, and we determine the semimajor axis, eccentricity, inclination, and spin-orbit angle distributions of the final configurations. We find that the efficiency of forming tight binaries (less than or similar to 16 days) when taking the EKL mechanism into account is similar to 21%, and about 4% of all simulated systems ended up in a merger event. These merger events can lead to the formation of blue stragglers. Furthermore, we find that the spin-orbit angle distribution of the inner binaries carries a signature of the initial setup of the system; thus, observations can be used to disentangle close binaries' birth configuration. The resulting inner and outer final orbits' period distributions and their estimated fraction suggest that secular dynamics may be a significant channel for the formation of close binaries in triples and even blue stragglers. C1 [Naoz, Smadar] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Naoz, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM snaoz@cfa.harvard.edu OI Naoz, Smadar/0000-0002-9802-9279; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF2-130096] FX We thank Aaron Geller for useful discussions, suggestions, and answering many questions. We also thank Tassos Fragos, Ramesh Narayan, Amaury Triaud, Todd Thompson, and Simon Albrecht for useful discussions. We also thank Andrei Tokovinin for discussing our arguments about the comparison between theory and observations. In addition, we thank our anonymous referee for a thorough reading of the paper and providing many useful comments and suggestions. S.N. is supported by NASA through an Einstein Postdoctoral Fellowship awarded by the Chandra X-ray Center, which is operated by the Smith-sonian Astrophysical Observatory for NASA under contract PF2-130096. NR 85 TC 40 Z9 40 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 OCT 1 PY 2014 VL 793 IS 2 AR 137 DI 10.1088/0004-637X/793/2/137 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300068 ER PT J AU O'Sullivan, E Vrtilek, JM David, LP Giacintucci, S Zezas, A Ponman, TJ Mamon, GA Nulsen, P Raychaudhury, S AF O'Sullivan, E. Vrtilek, J. M. David, L. P. Giacintucci, S. Zezas, A. Ponman, T. J. Mamon, G. A. Nulsen, P. Raychaudhury, S. TI DEEP CHANDRA OBSERVATIONS OF HCG 16. II. THE DEVELOPMENT OF THE INTRA-GROUP MEDIUM IN A SPIRAL-RICH GROUP SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: intracluster medium; galaxies: groups: individual (HCG 16); galaxies: individual (NGC 838, NGC 839); galaxies: starburst; X-rays: galaxies ID HICKSON COMPACT-GROUPS; GALAXY GROUPS; STAR-FORMATION; STEPHANS QUINTET; GALACTIC WINDS; XMM-NEWTON; INTERGALACTIC MEDIUM; EMISSION; GAS; MULTIWAVELENGTH AB We use a combination of deep Chandra X-ray observations and radio continuum imaging to investigate the origin and current state of the intra-group medium (IGM) in the spiral-rich compact group HCG 16. We confirm the presence of a faint (L-X,L-bolo = 1.87(-0.66)(+1.03) x 10(41) erg s(-1)), low-temperature (0.30(-0.05)(+0.07) keV) IGM extending throughout the ACIS-S3 field of view, with a ridge linking the four original group members and extending to the southeast, as suggested by previous ROSAT and XMM-Newton observations. This ridge contains 6.6(-3.3)(+3.9) x 10(9) M-circle dot of hot gas and is at least partly coincident with a large-scale H I tidal filament, indicating that the IGM in the inner part of the group is highly multi-phase. We present evidence that the group is not yet virialized, and show that gas has probably been transported from the starburst winds of NGC 838 and NGC 839 into the surrounding IGM. Considering the possible origin of the IGM, we argue that material ejected by galactic winds may have played a significant role, contributing 20%-40% of the observed hot gas in the system. C1 [O'Sullivan, E.; Vrtilek, J. M.; David, L. P.; Zezas, A.; Nulsen, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Zezas, A.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Crete, Greece. [Ponman, T. J.; Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Mamon, G. A.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Mamon, G. A.] UMPC, F-75014 Paris, France. [Raychaudhury, S.] Presidency Univ, Dept Phys, Kolkata 700073, India. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; O'Sullivan, Ewan/0000-0002-5671-6900; Nulsen, Paul/0000-0003-0297-4493; Giacintucci, Simona/0000-0002-1634-9886; Mamon, Gary/0000-0001-8956-5953 FU National Aeronautics and Space Administration (NASA) [G03-14143X, NAS8-03060]; NASA through Einstein Postdoctoral Fellowship, CXC [PF0-110071] FX The authors thank L. Verdes-Montenegro for providing her VLA Hi map of the group, and the anonymous referee for helpful comments on the paper. Support for this work was provided by the National Aeronautics and Space Administration (NASA) through Chandra Award Number G03-14143X issued by the Chandra X-ray Observatory Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060. S.G. acknowledges the support of NASA through the Einstein Postdoctoral Fellowship PF0-110071 awarded by the CXC, and this research has made use of data obtained from the Chandra Data Archive and software provided by the CXC in the application packages CIAO, ChIPS, and Sherpa, as well as SAOImage DS9, developed by SAO. We thank the staff of the GMRT for their help during observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute for Fundamental Research. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). NR 47 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 OCT 1 PY 2014 VL 793 IS 2 AR 74 DI 10.1088/0004-637X/793/2/74 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300005 ER PT J AU O'Sullivan, E Zezas, A Vrtilek, JM Giacintucci, S Trevisan, M David, LP Ponman, TJ Mamon, GA Raychaudhury, S AF O'Sullivan, E. Zezas, A. Vrtilek, J. M. Giacintucci, S. Trevisan, M. David, L. P. Ponman, T. J. Mamon, G. A. Raychaudhury, S. TI DEEP CHANDRA OBSERVATIONS OF HCG 16. I. ACTIVE NUCLEI, STAR FORMATION, AND GALACTIC WINDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: groups: individual (HCG 16); galaxies: individual (NGC 833, NGC 835, NGC 838, NGC 839, NGC 848); galaxies: starburst; X-rays: galaxies ID HICKSON COMPACT-GROUPS; X-RAY-EMISSION; STELLAR POPULATION SYNTHESIS; GALAXY GROUPS; GROUPS. I.; HOT GAS; INTRAGROUP MEDIUM; FORMING GALAXIES; FORMATION RATES; MASS FUNCTION AB We present new, deep Chandra X-ray and Giant Metrewave Radio Telescope 610 MHz observations of the spiral-galaxy-rich compact group HCG 16, which we use to examine nuclear activity, star formation, and high-luminosity X-ray binary populations in the major galaxies. We confirm the presence of obscured active nuclei in NGC 833 and NGC 835, and identify a previously unrecognized nuclear source in NGC 838. All three nuclei are variable on timescales of months to years, and for NGC 833 and NGC 835 this is most likely caused by changes in accretion rate. The deep Chandra observations allow us to detect for the first time an Fe K alpha emission line in the spectrum of the Seyfert 2 nucleus of NGC 835. We find that NGC 838 and NGC 839 are both starburst-dominated systems, with only weak nuclear activity, in agreement with previous optical studies. We estimate the star formation rates in the two galaxies from their X-ray and radio emission, and compare these results with estimates from the infrared and ultraviolet bands to confirm that star formation in both galaxies is probably declining after galaxy-wide starbursts were triggered similar to 400-500 Myr ago. We examine the physical properties of their galactic superwinds, and find that both have temperatures of similar to 0.8 keV. We also examine the X-ray and radio properties of NGC 848, the fifth largest galaxy in the group, and show that it is dominated by emission from its starburst. C1 [O'Sullivan, E.; Zezas, A.; Vrtilek, J. M.; David, L. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Zezas, A.] Univ Crete, Inst Theoret & Computat Phys, GR-71003 Iraklion, Crete, Greece. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Trevisan, M.] Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil. [Ponman, T. J.; Raychaudhury, S.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Mamon, G. A.] CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France. [Mamon, G. A.] UMPC, F-75014 Paris, France. [Raychaudhury, S.] Presidency Univ, Dept Phys, Kolkata 700073, India. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM eosullivan@cfa.harvard.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; O'Sullivan, Ewan/0000-0002-5671-6900; Giacintucci, Simona/0000-0002-1634-9886; Mamon, Gary/0000-0001-8956-5953 FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2012/05142-5]; National Aeronautics and Space Administration (NASA) [G03-14143X, NAS8-03060]; NASA through Einstein Postdoctoral Fellowship, CXC [PF0-110071]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX The authors thank L. Verdes-Montenegro for providing her VLA Hi map of the group, as well as C. Jones and the anonymous referee for their helpful comments on the manuscript. E.O'S. thanks R. Barnard for useful discussions on data analysis. M.T. acknowledges the support of the Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), process no. 2012/05142-5. Support for this work was provided by the National Aeronautics and Space Administration (NASA) through Chandra Award Number G03-14143X issued by the Chandra X-ray Observatory Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060. S.G. acknowledges the support of NASA through the Einstein Postdoctoral Fellowship PF0-110071 awarded by the CXC, and this research has made use of data obtained from the Chandra Data Archive and software provided by the CXC in the application packages CIAO, ChIPS, and Sherpa, as well as SAOImage DS9, developed by SAO. We thank the staff of the GMRT for their help during observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute for Fundamental Research. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). 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/. NR 72 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 OCT 1 PY 2014 VL 793 IS 2 AR 73 DI 10.1088/0004-637X/793/2/73 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300004 ER PT J AU Sato, M Wu, YW Immer, K Zhang, B Sanna, A Reid, MJ Dame, TM Brunthaler, A Menten, KM AF Sato, M. Wu, Y. W. Immer, K. Zhang, B. Sanna, A. Reid, M. J. Dame, T. M. Brunthaler, A. Menten, K. M. TI TRIGONOMETRIC PARALLAXES OF STAR FORMING REGIONS IN THE SCUTUM SPIRAL ARM SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: kinematics and dynamics; Galaxy: structure; masers; parallaxes; stars: formation ID ULTRACOMPACT HII-REGIONS; EXTENDED GREEN OBJECTS; 1ST GALACTIC QUADRANT; GHZ METHANOL MASERS; MILKY-WAY GALAXY; H-II REGIONS; MOLECULAR CLOUDS; FUNDAMENTAL PARAMETERS; NEUTRAL HYDROGEN; VLBI ASTROMETRY AB We report measurements of trigonometric parallaxes for six high-mass star-forming regions in the Scutum spiral arm of the Milky Way as part of the BeSSeL Survey. Combining our measurements with 10 previous measurements from the BeSSeL Survey yields a total sample of 16 sources in the Scutum arm with trigonometric parallaxes in the Galactic longitude range from 5 degrees to 32 degrees. Assuming a logarithmic spiral model, we estimate a pitch angle of 19 degrees.8 +/- 3 degrees.1 for the Scutum arm, which is larger than pitch angles reported for other spiral arms. The high pitch angle of the arm may be due to the arm's proximity to the Galactic bar. The Scutum arm sources show an average peculiar motion of 4 km s(-1) slower than the Galactic rotation and 8 km s(-1) toward the Galactic center. While the direction of this non-circular motion has the same sign as determined for sources in other spiral arms, the motion toward the Galactic center is greater for the Scutum arm sources. C1 [Sato, M.; Wu, Y. W.; Immer, K.; Zhang, B.; Sanna, A.; Brunthaler, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Wu, Y. W.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. [Wu, Y. W.] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sato, M (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM msato@mpifr-bonn.mpg.de FU JSPS; ERC Advanced Investigator Grant GLOSTAR [247078] FX M.S. acknowledges financial support from a JSPS Postdoctoral Fellowship for Research Abroad. This work was partially funded by the ERC Advanced Investigator Grant GLOSTAR (247078). We thank the anonymous referee for insightful comments. NR 73 TC 25 Z9 25 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 OCT 1 PY 2014 VL 793 IS 2 AR 72 DI 10.1088/0004-637X/793/2/72 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300003 ER PT J AU Schroeder, J Halpern, J AF Schroeder, Joshua Halpern, Jules TI OBSERVATIONS AND MODELING OF THE COMPANIONS OF SHORT PERIOD BINARY MILLISECOND PULSARS: EVIDENCE FOR HIGH-MASS NEUTRON STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; gamma rays: stars; pulsars: general ID X-RAY BINARIES; ECLIPSING BINARY; RADIO PULSARS; BLACK WIDOWS; MAXIMUM MASS; LIGHT-CURVE; ATMOSPHERES; EVOLUTION; DISCOVERY; WIND AB We present observations of fields containing eight recently discovered binary millisecond pulsars using the telescopes at MDM Observatory. Optical counterparts to four of these systems are detected, one of which, PSR J2214+3000, is a novel detection. Additionally, we present the fully phase-resolved B, V, and R light curves of the optical counterparts to two objects, PSR J1810+1744 and PSR J2215+5135 for which we employ model fitting using the eclipsing light curve (ELC) model of Orosz & Hauschildt to measure the unknown system parameters. For PSR J1810+1744, we find that the system parameters cannot be fit even assuming that 100% of the spin-down luminosity of the pulsar is irradiating the secondary, and so radial velocity measurements of this object will be required for the complete solution. However, PSR J2215+5135 exhibits light curves that are extremely well constrained using the ELC model and we find that the mass of the neutron star is constrained by these and the radio observations to be M-NS > 1.75 M-circle dot at the 3 sigma level. We also find a discrepancy between the model temperature and the measured colors of this object, which we interpret as possible evidence for an additional high-temperature source such as a quiescent disk. Given this and the fact that PSR J2215+5135 contains a relatively high mass companion (M-c > 0.1 M-circle dot), we propose that similar to the binary pulsar systems PSR J1023+0038 and IGR J18245-2452, the pulsar may transition between accretion- and rotation-powered modes. C1 [Schroeder, Joshua; Halpern, Jules] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Schroeder, Joshua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schroeder, J (reprint author), Columbia Univ, Dept Astron, Mail Code 5246,550 West 120th St, New York, NY 10027 USA. OI Tan, Joshua/0000-0003-3835-8115 NR 49 TC 11 Z9 11 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 OCT 1 PY 2014 VL 793 IS 2 AR 78 DI 10.1088/0004-637X/793/2/78 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300009 ER PT J AU van den Berg, M Homan, J Fridriksson, JK Linares, M AF van den Berg, Maureen Homan, Jeroen Fridriksson, Joel K. Linares, Manuel TI DISCOVERY OF THE NEAR-INFRARED COUNTERPART TO THE LUMINOUS NEUTRON-STAR LOW-MASS X-RAY BINARY GX 3+1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; stars: individual (GX 3+1); X-rays: binaries ID GALACTIC-CENTER; MAGELLAN TELESCOPES; EXTINCTION; BULGE; BURST; IDENTIFICATION; SPECTROSCOPY; CANDIDATES; EVOLUTION; BRIGHT AB Using the High Resolution Camera on board the Chandra X-ray Observatory, we have measured an accurate position for the bright persistent neutron star X-ray binary and atoll source GX 3+1. At a location that is consistent with this new position, we have discovered the near-infrared (NIR) counterpart to GX 3+1 in images taken with the PANIC and FourStar cameras on the Magellan Baade Telescope. The identification of this K-s = 15.8 +/- 0.1 mag star as the counterpart is based on the presence of a Br gamma emission line in an NIR spectrum taken with the Folded-port InfraRed Echelette spectrograph on the Baade Telescope. The absolute magnitude derived from the best available distance estimate to GX 3+1 indicates that the mass donor in the system is not a late-type giant. We find that the NIR light in GX 3+1 is likely dominated by the contribution from a heated outer accretion disk. This is similar to what has been found for the NIR flux from the brighter class of Z sources, but unlike the behavior of atolls fainter (L-X approximate to 10(36)-10(37) erg s(-1)) than GX 3+1, where optically thin synchrotron emission from a jet probably dominates the NIR flux. C1 [van den Berg, Maureen; Fridriksson, Joel K.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [van den Berg, Maureen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Homan, Jeroen] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Linares, Manuel] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, S C De Tenerife, Spain. [Linares, Manuel] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. RP van den Berg, M (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM M.C.vandenBerg@uva.nl FU Chandra [GO2-13048X] FX The authors thank A. Monson for help with the FourStar data reduction and R. Remillard, P. Sullivan, and M. Matejek for obtaining part of the observations. This work is supported by Chandra grant GO2-13048X. NR 45 TC 1 Z9 1 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 OCT 1 PY 2014 VL 793 IS 2 AR 128 DI 10.1088/0004-637X/793/2/128 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300059 ER PT J AU van Weeren, RJ Williams, WL Tasse, C Rottgering, HJA Rafferty, DA van der Tol, S Heald, G White, GJ Shulevski, A Best, P Intema, HT Bhatnagar, S Reich, W Steinmetz, M van Velzen, S Ensslin, TA Prandoni, I de Gasperin, F Jamrozy, M Brunetti, G Jarvis, MJ McKean, JP Wise, MW Ferrari, C Harwood, J Oonk, JBR Hoeft, M Kunert-Bajraszewska, M Horellou, C Wucknitz, O Bonafede, A Mohan, NR Scaife, AMM Klockner, HR van Bemmel, IM Merloni, A Chyzy, KT Engels, D Falcke, H Pandey-Pommier, M Alexov, A Anderson, J Avruch, IM Beck, R Bell, ME Bentum, MJ Bernardi, G Breitling, F Broderick, J Brouw, WN Bruggen, M Butcher, HR Ciardi, B de Geus, E de Vos, M Deller, A Duscha, S Eisloffel, J Fallows, RA Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hamaker, JP Hassall, TE Horandel, J van der Horst, A Iacobelli, M Jackson, NJ Juette, E Kondratiev, VI Kuniyoshi, M Maat, P Mann, G McKay-Bukowski, D Mevius, M Morganti, R Munk, H Offringa, AR Orru, E Paas, H Pandey, VN Pietka, G Pizzo, R Polatidis, AG Renting, A Rowlinson, A Schwarz, D Serylak, M Sluman, J Smirnov, O Stappers, BW Stewart, A Swinbank, J Tagger, M Tang, Y Thoudam, S Toribio, C Vermeulen, R Vocks, C Zarka, P AF van Weeren, R. J. Williams, W. L. Tasse, C. Rottgering, H. J. A. Rafferty, D. A. van der Tol, S. Heald, G. White, G. J. Shulevski, A. Best, P. Intema, H. T. Bhatnagar, S. Reich, W. Steinmetz, M. van Velzen, S. Ensslin, T. A. Prandoni, I. de Gasperin, F. Jamrozy, M. Brunetti, G. Jarvis, M. J. McKean, J. P. Wise, M. W. Ferrari, C. Harwood, J. Oonk, J. B. R. Hoeft, M. Kunert-Bajraszewska, M. Horellou, C. Wucknitz, O. Bonafede, A. Mohan, N. R. Scaife, A. M. M. Kloeckner, H. -R. van Bemmel, I. M. Merloni, A. Chyzy, K. T. Engels, D. Falcke, H. Pandey-Pommier, M. Alexov, A. Anderson, J. Avruch, I. M. Beck, R. Bell, M. E. Bentum, M. J. Bernardi, G. Breitling, F. Broderick, J. Brouw, W. N. Brueggen, M. Butcher, H. R. Ciardi, B. de Geus, E. de Vos, M. Deller, A. Duscha, S. Eisloeffel, J. Fallows, R. A. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hamaker, J. P. Hassall, T. E. Horandel, J. van der Horst, A. Iacobelli, M. Jackson, N. J. Juette, E. Kondratiev, V. I. Kuniyoshi, M. Maat, P. Mann, G. McKay-Bukowski, D. Mevius, M. Morganti, R. Munk, H. Offringa, A. R. Orru, E. Paas, H. Pandey, V. N. Pietka, G. Pizzo, R. Polatidis, A. G. Renting, A. Rowlinson, A. Schwarz, D. Serylak, M. Sluman, J. Smirnov, O. Stappers, B. W. Stewart, A. Swinbank, J. Tagger, M. Tang, Y. Thoudam, S. Toribio, C. Vermeulen, R. Vocks, C. Zarka, P. TI LOFAR LOW-BAND ANTENNA OBSERVATIONS OF THE 3C 295 AND BOOTES FIELDS: SOURCE COUNTS AND ULTRA-STEEP SPECTRUM SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; radio continuum: general; surveys; techniques: interferometric ID REDSHIFT RADIO GALAXIES; ACTIVE GALACTIC NUCLEI; SCALE STRUCTURE SURVEY; FREQUENCY SKY SURVEY; WIDE-FIELD; EXTRAGALACTIC SURVEY; MINI-SURVEY; LARGE ARRAY; 74 MHZ; DEEP AB We present Low Frequency Array (LOFAR) Low Band observations of the Bootes and 3C 295 fields. Our images made at 34, 46, and 62 MHz reach noise levels of 12, 8, and 5 mJy beam(-1), making them the deepest images ever obtained in this frequency range. In total, we detect between 300 and 400 sources in each of these images, covering an area of 17-52 deg(2). From the observations, we derive Euclidean-normalized differential source counts. The 62 MHz source counts agree with previous GMRT 153 MHz and Very Large Array 74 MHz differential source counts, scaling with a spectral index of -0.7. We find that a spectral index scaling of -0.5 is required to match up the LOFAR 34 MHz source counts. This result is also in agreement with source counts from the 38 MHz 8C survey, indicating that the average spectral index of radio sources flattens toward lower frequencies. We also find evidence for spectral flattening using the individual flux measurements of sources between 34 and 1400 MHz and by calculating the spectral index averaged over the source population. To select ultra-steep spectrum (alpha < -1.1) radio sources that could be associated with massive high-redshift radio galaxies, we compute spectral indices between 62 MHz, 153 MHz, and 1.4 GHz for sources in the Bootes field. We cross-correlate these radio sources with optical and infrared catalogs and fit the spectral energy distribution to obtain photometric redshifts. We find that most of these ultra-steep spectrum sources are located in the 0.7 less than or similar to z less than or similar to 2.5 range. C1 [van Weeren, R. J.; Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Williams, W. L.; Rottgering, H. J. A.; Rafferty, D. A.; van der Tol, S.; Garrett, M. A.; Iacobelli, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Williams, W. L.; van der Tol, S.; Heald, G.; McKean, J. P.; Wise, M. W.; Oonk, J. B. R.; van Bemmel, I. M.; Falcke, H.; Avruch, I. M.; Bentum, M. J.; Brouw, W. N.; de Geus, E.; de Vos, M.; Deller, A.; Duscha, S.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Kondratiev, V. I.; Maat, P.; Mevius, M.; Morganti, R.; Munk, H.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Renting, A.; Sluman, J.; Tang, Y.; Toribio, C.; Vermeulen, R.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Tasse, C.; Smirnov, O.] Rhodes Univ, Dept Phys & Elect, ZA-6140 Grahamstown, South Africa. [Tasse, C.; Smirnov, O.] SKA South Afr, ZA-7405 Pinelands, South Africa. [Tasse, C.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92190 Meudon, France. [White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [White, G. J.] Rutherford Appleton Lab, Dept Space Sci, Didcot OX11 0QX, Oxon, England. [Shulevski, A.; McKean, J. P.; Mevius, M.; Morganti, R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Intema, H. T.; Bhatnagar, S.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Reich, W.; Wucknitz, O.; Kloeckner, H. -R.; Falcke, H.; Beck, R.; Kuniyoshi, M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Steinmetz, M.; Anderson, J.; Breitling, F.; Mann, G.; Vocks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [van Velzen, S.; Falcke, H.; Horandel, J.; Thoudam, S.] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Ensslin, T. A.; Ciardi, B.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Prandoni, I.; Brunetti, G.] INAF, Ist Radioastron, I-40129 Bologna, Italy. [de Gasperin, F.; Bonafede, A.; Engels, D.; Brueggen, M.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. [Jamrozy, M.; Chyzy, K. T.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Jarvis, M. J.; Pietka, G.; Serylak, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M. J.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Wise, M. W.; van der Horst, A.; Rowlinson, A.; Swinbank, J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Ferrari, C.] Univ Nice Sophia Antipolis, Observ Cote Azur, CNRS, Lab Lagrange,UMR7293, F-06300 Nice, France. [Harwood, J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Hoeft, M.; Eisloeffel, J.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Kunert-Bajraszewska, M.] Nicholas Copernicus Univ, Fac Phys Astron & Informat, Torun Ctr Astron, PL-87100 Torun, Poland. [Horellou, C.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden. [Mohan, N. R.; Stewart, A.] Natl Ctr Radio Astrophys, TIFR, Pune 411007, Maharashtra, India. [Scaife, A. M. M.; Broderick, J.; Hassall, T. E.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Merloni, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Pandey-Pommier, M.] Univ Lyon, F-69003 Lyon, France. [Pandey-Pommier, M.] Ctr Rech Astrophys Lyon, Observ Lyon, F-69561 St Genis Laval, France. [Pandey-Pommier, M.] Ecole Normale Super Lyon, F-69007 Lyon, France. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AB Groningen, Netherlands. [Bell, M. E.] Univ Sydney, Sydney Inst Astron, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Bentum, M. J.] Univ Twente, NL-7500 AE Enschede, Netherlands. [Butcher, H. R.; Offringa, A. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Mt Stromlo Obs, Weston, ACT 2611, Australia. [de Geus, E.] SmarterVis BV, NL-9401 JX Assen, Netherlands. [Griessmeier, J.; Tagger, M.] Univ Orleans, CNRS, LPC2E, F-45067 Orleans 2, France. [Griessmeier, J.] Univ Orleans, Observ Paris, Stn Radioastron Nancay, CNRS INSU,USR 704 OSUC, F-18330 Nancay, France. [Hassall, T. E.; Jackson, N. J.; Stappers, B. W.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Juette, E.] Ruhr Univ Bochum, Inst Astron, D-44780 Bochum, Germany. [Kondratiev, V. I.] Ctr Astro Space, Lebedev Phys Inst, Moscow 117997, Russia. [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-9712 CP Groningen, Netherlands. [Schwarz, D.] Univ Bielefeld, Fak Phys, D-33501 Bielefeld, Germany. [Zarka, P.] Observ Paris, LESIA, UMR CNRS 8109, F-92195 Meudon, France. RP van Weeren, RJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rvanweeren@cfa.harvard.edu RI Kondratiev, Vladislav/N-1105-2015; Tagger, Michel/O-6615-2014; Kunert-Bajraszewska, Magdalena/F-9060-2014; Shulevski, Aleksandar/E-5591-2015; Jamrozy, Marek/F-4507-2015; Ciardi, Benedetta/N-7625-2015; Harwood, Jeremy/D-9032-2016; Intema, Huib/D-1438-2012 OI de Gasperin, Francesco/0000-0003-4439-2627; Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660; Kondratiev, Vladislav/0000-0001-8864-7471; Prandoni, Isabella/0000-0001-9680-7092; Tagger, Michel/0000-0003-2962-3220; Swinbank, John/0000-0001-9445-1846; Shulevski, Aleksandar/0000-0002-1827-0469; Brunetti, Gianfranco/0000-0003-4195-8613; Harwood, Jeremy/0000-0003-0251-6126; Intema, Huib/0000-0002-5880-2730 FU NASA [PF2-130104]; Chandra X-ray Center; Smithsonian Astrophysical Observatory for NASA [NAS8-03060]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX Support for this work was provided by NASA through 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. Chiara Ferrari acknowledges financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. NR 70 TC 11 Z9 11 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2014 VL 793 IS 2 AR 82 DI 10.1088/0004-637X/793/2/82 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP3HD UT WOS:000341965300013 ER PT J AU Chave, J Rejou-Mechain, M Burquez, A Chidumayo, E Colgan, MS Delitti, WB Duque, A Eid, T Fearnside, PM Goodman, RC Henry, M Martinez-Yrizar, A Mugasha, WA Muller-Landau, HC Mencuccini, M Nelson, BW Ngomanda, A Nogueira, EM Ortiz-Malavassi, E Pelissier, R Ploton, P Ryan, CM Saldarriaga, JG Vieilledent, G AF Chave, Jerome Rejou-Mechain, Maxime Burquez, Alberto Chidumayo, Emmanuel Colgan, Matthew S. Delitti, Welington B. C. Duque, Alvaro Eid, Tron Fearnside, Philip M. Goodman, Rosa C. Henry, Matieu Martinez-Yrizar, Angelina Mugasha, Wilson A. Muller-Landau, Helene C. Mencuccini, Maurizio Nelson, Bruce W. Ngomanda, Alfred Nogueira, Euler M. Ortiz-Malavassi, Edgar Pelissier, Raphael Ploton, Pierre Ryan, Casey M. Saldarriaga, Juan G. Vieilledent, Ghislain TI Improved allometric models to estimate the aboveground biomass of tropical trees SO GLOBAL CHANGE BIOLOGY LA English DT Article DE carbon; forest inventory; global carbon cycling; plant allometry; tree height; tropics ID NET PRIMARY PRODUCTION; FOREST CARBON STOCKS; BELOW-GROUND BIOMASS; GLOBAL LAND AREAS; HEIGHT ALLOMETRY; AMAZON FOREST; RAIN-FOREST; DEFORESTATION; EQUATIONS; EMISSIONS AB Terrestrial carbon stock mapping is important for the successful implementation of climate change mitigation policies. Its accuracy depends on the availability of reliable allometric models to infer oven-dry aboveground biomass of trees from census data. The degree of uncertainty associated with previously published pantropical aboveground biomass allometries is large. We analyzed a global database of directly harvested trees at 58 sites, spanning a wide range of climatic conditions and vegetation types (4004 trees5cm trunk diameter). When trunk diameter, total tree height, and wood specific gravity were included in the aboveground biomass model as covariates, a single model was found to hold across tropical vegetation types, with no detectable effect of region or environmental factors. The mean percent bias and variance of this model was only slightly higher than that of locally fitted models. Wood specific gravity was an important predictor of aboveground biomass, especially when including a much broader range of vegetation types than previous studies. The generic tree diameter-height relationship depended linearly on a bioclimatic stress variable E, which compounds indices of temperature variability, precipitation variability, and drought intensity. For cases in which total tree height is unavailable for aboveground biomass estimation, a pantropical model incorporating wood density, trunk diameter, and the variable E outperformed previously published models without height. However, to minimize bias, the development of locally derived diameter-height relationships is advised whenever possible. Both new allometric models should contribute to improve the accuracy of biomass assessment protocols in tropical vegetation types, and to advancing our understanding of architectural and evolutionary constraints on woody plant development. C1 [Chave, Jerome; Rejou-Mechain, Maxime] CNRS, Lab Evolut & Diversite Biol, UMR 5174, F-31062 Toulouse, France. [Chave, Jerome; Rejou-Mechain, Maxime] Univ Toulouse 3, F-31062 Toulouse, France. [Burquez, Alberto; Martinez-Yrizar, Angelina] Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol Biodiversidad, Hermosillo 83000, Sonora, Mexico. [Chidumayo, Emmanuel] Makeni Savanna Res Project, Lusaka, Zambia. [Colgan, Matthew S.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Delitti, Welington B. C.] Univ Sao Paulo, BR-05508090 Sao Paulo, Brazil. [Duque, Alvaro] Univ Nacl Colombia, Dept Ciencias Forestales, Medellin, Colombia. [Eid, Tron; Mugasha, Wilson A.] Norwegian Univ Life Sci, Dept Ecol & Nat Resource Management, N-1432 As, Norway. [Fearnside, Philip M.; Nelson, Bruce W.; Nogueira, Euler M.] Natl Inst Res Amazon INPA, Dept Environm Dynam, BR-69060000 Manaus, Amazonas, Brazil. [Goodman, Rosa C.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Henry, Matieu] Food & Agr Org United Nations, Forest Dept, I-00153 Rome, Italy. [Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Panama City, Panama. [Mencuccini, Maurizio; Ryan, Casey M.] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3JN, Midlothian, Scotland. [Ngomanda, Alfred] IRET, Libreville, Gabon. [Ortiz-Malavassi, Edgar] Inst Tecnol Costa Rica, Cartago 1597050, Costa Rica. [Pelissier, Raphael; Ploton, Pierre] IRD, AMAP, UMR, F-34000 Montpellier, France. [Vieilledent, Ghislain] BSEF, UPR, CIRAD, F-34398 Montpellier, France. RP Chave, J (reprint author), CNRS, Lab Evolut & Diversite Biol, UMR 5174, F-31062 Toulouse, France. EM jerome.chave@univ-tlse3.fr RI Mencuccini, Maurizio/B-9052-2011; Krammel, Vera/N-4826-2014; Vieilledent, Ghislain/D-8323-2011; Pelissier, Raphael/C-1224-2008; OI Mencuccini, Maurizio/0000-0003-0840-1477; Krammel, Vera/0000-0002-8273-8396; Vieilledent, Ghislain/0000-0002-1685-4997; Pelissier, Raphael/0000-0003-4845-5090; Fearnside, Philip/0000-0003-3672-9082; Ryan, Casey/0000-0002-1802-0128 FU Fondation pour la Recherche sur la Biodiversite; CNES (TOSCA program); Agence Nationale pour la Recherche (ANR; BRIDGE project); ANR [CEBA: ANR-10-LABX-25-01, TULIP: ANR-10-LABX-0041] FX We thank the numerous field workers who contributed the direct tree harvest datasets used in this study, as well as the institutions and funding agencies involved in these projects. We also thank Greg Asner and an anonymous referee for insightful comments on a previous version of the manuscript. It is a pleasure to acknowledge financial support from Fondation pour la Recherche sur la Biodiversite, CNES (TOSCA program), Agence Nationale pour la Recherche (ANR; BRIDGE project), and from Investissement d'Avenir grants of the ANR (CEBA: ANR-10-LABX-25-01; TULIP: ANR-10-LABX-0041). Unpublished data from Cameroon3 were collected in collaboration with Alpicam company within the IRD project PPR FTH-AC 'Changement globaux, biodiversite et sante en zone forestiere d'Afrique Centrale'. NR 89 TC 157 Z9 160 U1 48 U2 192 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 OCT PY 2014 VL 20 IS 10 BP 3177 EP 3190 DI 10.1111/gcb.12629 PG 14 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AP6DU UT WOS:000342168500015 PM 24817483 ER PT J AU Nearns, EH Tavakilian, GL AF Nearns, Eugenio H. Tavakilian, Gerard L. TI Australian Longhorn Beetles (Coleoptera: Cerambycidae), vol 1, Introduction and Subfamily Lamiinae SO SYSTEMATIC ENTOMOLOGY LA English DT Book Review C1 [Nearns, Eugenio H.] Smithsonian Inst, Natl Museum Amer Hist, Dept Entomol, Washington, DC 20560 USA. [Tavakilian, Gerard L.] Museum Natl Hist Nat, Dept Systemat & Evolut, Antenne IRD, F-75231 Paris, France. RP Nearns, EH (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Dept Entomol, Washington, DC 20560 USA. NR 3 TC 0 Z9 0 U1 0 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD OCT PY 2014 VL 39 IS 4 BP 863 EP 863 DI 10.1111/syen.12087 PG 1 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA AP5YE UT WOS:000342153800012 ER PT J AU Steiner, JF McClintock, JE Orosz, JA Remillard, RA Bailyn, CD Kolehmainen, M Straub, O AF Steiner, James F. McClintock, Jeffrey E. Orosz, Jerome A. Remillard, Ronald A. Bailyn, Charles D. Kolehmainen, Mari Straub, Odele TI THE LOW-SPIN BLACK HOLE IN LMC X-3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; stars: individual (LMC X-3); X-rays: binaries ID X-RAY BINARIES; ACCRETION DISK; INNER-DISK; JET POWER; GALAXY; MODEL; GRS-1915+105; ENERGY AB Building upon a new dynamical model for the X-ray binary LMC X-3, we measure the spin of its black hole (BH) primary via the continuum-fitting method. We consider over one thousand thermal-state Rossi X-ray Timing Explorer X-ray spectra of LMC X-3. Using a large subset of these spectra, we constrain the spin parameter of the BH to be a(*) = 0.25(-0.29)(+0.20) (90% confidence). Our estimate of the uncertainty in a(*) takes into account a wide range of systematic errors. We discuss evidence for a correlation between a BH's spin and the complexity of its X-ray spectrum. C1 [Steiner, James F.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Orosz, Jerome A.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Remillard, Ronald A.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bailyn, Charles D.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Kolehmainen, Mari] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Straub, Odele] Univ Paris Diderot, CNRS, LUTH, Observ Paris, F-92190 Meudon, France. RP Steiner, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jsteiner@cfa.harvard.edu OI Remillard, Ronald/0000-0003-4815-0481 FU NASA grant [NNX11AD08G]; NASA Hubble Fellowship grant [HST-HF-51315.01] FX We thank Chris Done and Lijun Gou for enlivening discussions, the anonymous referee, and Colleen Hodge-Wilson for providing data on the Crab's variability. Support for J.E.M. has been provided by NASA grant NNX11AD08G and support for J.F.S. by NASA Hubble Fellowship grant HST-HF-51315.01. NR 44 TC 14 Z9 14 U1 0 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 OCT 1 PY 2014 VL 793 IS 2 AR L29 DI 10.1088/2041-8205/793/2/L29 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP2ES UT WOS:000341885900008 ER PT J AU Kurin, R AF Kurin, Richard TI The Smithsonian Folklife Festival in Museological Perspective SO CURATOR-THE MUSEUM JOURNAL LA English DT Editorial Material AB The Smithsonian Folklife Festival began as a four-day event held over the Fourth of July holiday in 1967, outdoors on the Mall. The impulse for it came from Smithsonian Secretary S. Dillon Ripley. The form of it came from Ralph Rinzler, field research director for the Newport Folk Festival and a documentarian who sought out authentic, grassroots American musicians. The Festival was conceived as giving voice to the less known and under-represented, a philosophy that quickly expanded to encompass the world of what is now called intangible cultural heritage. The Festival's museology has as its core the foregrounding of the cultural exemplars and the primacy of their voices in the presentations. It has energized new possibilities for what can be done in the Smithsonian and on the National Mall, and in the lives of people, communities, and institutions well beyond. C1 Smithsonian Inst, Hist Art & Culture, Washington, DC 20560 USA. RP Kurin, R (reprint author), Smithsonian Inst, Hist Art & Culture, Washington, DC 20560 USA. EM Kurin@si.edu NR 4 TC 0 Z9 0 U1 0 U2 2 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 OCT PY 2014 VL 57 IS 4 BP 405 EP 414 DI 10.1111/cura.12081 PG 10 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6NS UT WOS:000363649700002 ER PT J AU Sheehy, D AF Sheehy, Daniel TI Smithsonian Folkways Recordings: The Role of Music in Breaching the Barriers of the Box SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB Smithsonian Folkways Recordings is the nonprofit record label of the Smithsonian Institution, the United States national museum. Folkways pairs with the Smithsonian's annual Folklife Festival in honoring and bringing to public attention the keepers of intangible cultural heritage traditions from many parts of the world. At the Folklife Festival, which takes place on the National Mall in Washington, D. C. each summer, the culture bearers speak for themselves in a presentational environment designed to promote interaction among the participants and audience members. In 2011, Folkways recordings of regional music from Colombia sparked an entire Folklife Festival program. C1 Smithsonian Ctr Folklife & Cultural Heritage, Smithsonian Folkways Recordings, Washington, DC 20013 USA. RP Sheehy, D (reprint author), Smithsonian Ctr Folklife & Cultural Heritage, Smithsonian Folkways Recordings, Washington, DC 20013 USA. EM sheehyd@si.edu NR 1 TC 1 Z9 1 U1 0 U2 0 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 OCT PY 2014 VL 57 IS 4 BP 415 EP 421 DI 10.1111/cura.12082 PG 7 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CU6NS UT WOS:000363649700003 ER PT J AU Brahney, J Ballantyne, AP Turner, BL Spaulding, SA Otu, M Neff, JC AF Brahney, J. Ballantyne, A. P. Turner, B. L. Spaulding, S. A. Otu, M. Neff, J. C. TI Separating the influences of diagenesis, productivity and anthropogenic nitrogen deposition on sedimentary delta N-15 variations SO ORGANIC GEOCHEMISTRY LA English DT Article DE Nitrogen isotopes; Lake sediments; Diagenesis; Atmospheric nitrogen deposition; C/N ratio; Diatoms ID PEPTIDE-BOND HYDROLYSIS; VARVED LAKE SEDIMENT; ORGANIC-MATTER; ISOTOPE BIOGEOCHEMISTRY; SINKING PARTICLES; STABLE CARBON; FRACTIONATION; PARTICULATE; PACIFIC; USA AB The stable isotopic composition of nitrogen (delta N-15) in organic lake sediments is frequently used to infer changes in the source or cycling of N prior to sedimentation. However, diagenetic processes that occur after sedimentation can systematically alter the primary isotopic signal recorded in sedimentary organic matter and must be accounted for in order to detect changes in the delta N-15 of nitrogen inputs to the sediment surface. Here we present a null model that estimates the diagenetic effect on sedimentary lake delta N-15 records. The model was tested using lake sediment cores from relatively pristine alpine lakes in the Wind River and Teton Ranges of Wyoming, USA. Model-inferred increases in productivity were tested against independent productivity proxies (diatom accumulation rates and the planktonic to benthic ratio), and inferred changes in anthropogenic nitrogen contribution were validated with records of atmospheric nitrogen deposition from the nearby Fremont Glacier, Wyoming. Diagenetic overprinting significantly altered sediment delta N-15 profiles, and the degree of alteration was not constant through time. Of the cores analyzed, similar to 30-70% of the variability can be explained by diagenesis alone, with the remainder explained by either a change in productivity or a change in the isotopic composition of the source material. Our null model of isotopic fractionation proved to be successful at separating the diagenetic overprinting from other causes of isotopic shifts, thereby providing environmental scientists with an analytical tool to partition the effects of diagenesis and environmental change on sedimentary delta N-15 values. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Brahney, J.; Neff, J. C.] Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. [Ballantyne, A. P.] Univ Montana, Dept Ecosyst & Conservat Sci, Missoula, MT 59812 USA. [Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Spaulding, S. A.; Otu, M.] Univ Colorado, Inst Arctic & Alpine Res, Boulder, CO 80309 USA. RP Brahney, J (reprint author), Univ British Columbia, Dept Earth & Environm Sci, 3333 Univ Way, Kelowna, BC V1V 1V7, Canada. EM Janice.Brahney@ubc.ca RI Turner, Benjamin/E-5940-2011; OI Turner, Benjamin/0000-0002-6585-0722; Brahney, Janice/0000-0001-7614-2855 FU NSF DEB [0948823]; NPS [119720]; NSERC PGS-D; Niwot Ridge NSF LTER Award FX Support was provided by NSF DEB Award # 0948823, NPS award #119720, an NSERC PGS-D, and from the Niwot Ridge NSF LTER Award. Thanks to Ted Porwall from the Bridger-Teton Forest Service, Sue O'Ney from Grand Teton National Park, and Ellen Porter, Tamara Blett and Terry Svalberd from the National Park Services Air Resources Division and to all members of the field crews that supported this research. We thank A. Wolfe and the anonymous reviewers for valuable commentary on the manuscript. NR 46 TC 5 Z9 5 U1 4 U2 38 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0146-6380 J9 ORG GEOCHEM JI Org. Geochem. PD OCT PY 2014 VL 75 BP 140 EP 150 DI 10.1016/j.orggeochem.2014.07.003 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AO4QM UT WOS:000341325800014 ER PT J AU Wilson, B Coimbra, JC Hayek, LAC AF Wilson, Brent Coimbra, Joao C. Hayek, Lee-Ann C. TI Ostracoda (Arthropoda, Crustacea) in a Miocene oxygen minimum zone, Trinidad, West Indies: A test of the Platycopid Signal Hypothesis SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Brasso Formation; Assemblage Turnover Index; Bradleya; Munseyella; Argilloecia; Platycopid Signal Hypothesis ID BENTHONIC FORAMINIFERAL PALEOECOLOGY; BRAZILIAN CONTINENTAL-SHELF; BRASSO FORMATION; MIDDLE MIOCENE; EQUATORIAL SHELF; QUARRY AB Studies of Recent ostracodes around the area of South America shed little light on the paleoenvironmental interpretation of Miocene assemblages. Consequently, interpretations of the Miocene ostracode assemblages must be supplemented using evidence from better documented taxa. Benthic foraminifera in samples from the Lower to Middle Miocene Brasso Formation at Brasso Village, Trinidad, have previously been used to distinguish three sample groupings (Beneath, Within and Above) around an oxygen minimum zone (OMZ), this being a layer of water within which dissolved oxygen concentrations can be as low as 0.1-1.0 mL/L. Using these same samples and the foraminiferal assemblage demarcations relative to the OMZ, this paper examines the associated and rich ostracode fauna of the Brasso Formation. The mean recovery of ostracode valves per sample was approximately three times greater in the Within OMZ sample group than in either of the Beneath OMZ or Above OMZ groups, perhaps reflecting the exclusion of macro-predators from within the OMZ. Individual rarefaction of species richness S to N = 300 valves was conducted for each sample group. This showed that S did not differ between the sample groups, ranging from 22.4 to 24.8. We used all ostracode species to model group separation. Based upon the Mahalanobis' criterion, we obtained significant group separation using a model with four taxa: Munseyella ex gr. minuta, Argilloecia posterotruncata, Munseyella sp. and Xestoleberis sp., while a fifth, Argilloecia spp., provided a significant but minor increase in separation probabilities over all groups. The two most abundant species (Bradleya sp., Gangamocytheridea reticulata) were thus not the best species for detecting the OMZ. Platycopid ostracodes of the genus Cytherella were found throughout the section, rather than concentrated within the OMZ, which contradicts the Platycopid Signal Hypothesis that OMZs are characterized by platycopid dominance. The total distribution and turnover of both ostracodal and foraminiferal assemblages were compared and contrasted quantitatively using a total assemblage turnover index (ATI) and the paleoenvironmental importance evaluated. The correlated between-sample ATI is for both groups lowest within the OMZ. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Wilson, Brent] Univ W Indies, Dept Chem Engn, Petr Geosci Programme, St Augustine, Trinid & Tobago. [Coimbra, Joao C.] UFRGS IGEO DPE, BR-91501970 Porto Alegre, RS, Brazil. [Hayek, Lee-Ann C.] Smithsonian Inst Math & Stat NMNH MRC 121, Washington, DC USA. RP Wilson, B (reprint author), Univ W Indies, Dept Chem Engn, Petr Geosci Programme, St Augustine, Trinid & Tobago. EM brent.wilson@sta.uwi.edu NR 54 TC 2 Z9 2 U1 0 U2 6 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 OCT PY 2014 VL 54 BP 210 EP 216 DI 10.1016/j.jsames.2014.06.003 PG 7 WC Geosciences, Multidisciplinary SC Geology GA AN8OQ UT WOS:000340863900014 ER PT J AU Triplett, JK Clark, LG Fisher, AE Wen, J AF Triplett, Jimmy K. Clark, Lynn G. Fisher, Amanda E. Wen, Jun TI Independent allopolyploidization events preceded speciation in the temperate and tropical woody bamboos SO NEW PHYTOLOGIST LA English DT Article DE allopolyploidy; bamboo; genome evolution; grasses; hybridization; phylogeny; polyploid speciation ID PHYLOGENETIC-RELATIONSHIPS; HYBRID SPECIATION; NATURAL HYBRIDIZATION; POLYPLOID SPECIATION; MAXIMUM-LIKELIHOOD; PLANT SPECIATION; SEQUENCE DATA; POACEAE; BAMBUSOIDEAE; EVOLUTION AB The objectives of the current study were to investigate the origin of polyploidy in the woody bamboos and examine putative hybrid relationships in one major lineage (the temperate woody bamboos, tribe Arundinarieae). Phylogenetic analyses were based on sequence data from three nuclear loci and 38 species in 27 genera. We identify six ancestral genome donors for contemporary bamboo lineages: temperate woody bamboos (tribe Arundinarieae) contain genomes A and B, tropical woody bamboos (tribe Bambuseae) contain genomes C and D, and herbaceous bamboos (tribe Olyreae) contain genome H; some hexaploid paleotropical bamboos contain genome E in addition to C and D. Molecular data indicate that allopolyploidy arose independently in temperate (AABB) and tropical woody lineages (CCDD and CCDDEE), and speciation occurred subsequent to polyploidization. Moreover, hybridization has played a surprising and recurrent role in bamboo evolution, generating allohexaploid species in the paleotropical clade and intergeneric hybrids among the allotetraploid temperate bamboos. We suggest this complex history of reticulate evolution is at least partially responsible for the taxonomic difficulty associated with the woody bamboos. This newly-resolved phylogenetic framework reflects a major step forward in our understanding of bamboo biodiversity and has important implications for the interpretation of bamboo phylogenomics. C1 [Triplett, Jimmy K.] Jacksonville State Univ, Dept Biol, Jacksonville, AL 36265 USA. [Clark, Lynn G.] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50011 USA. [Fisher, Amanda E.] Rancho Santa Ana Bot Garden, Claremont, CA 91711 USA. [Fisher, Amanda E.] Claremont Grad Univ, Claremont, CA 91711 USA. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Triplett, JK (reprint author), Jacksonville State Univ, Dept Biol, 700 Pelham Rd N, Jacksonville, AL 36265 USA. EM jtriplett@jsu.edu FU Smithsonian Institution; John D. and Catherine T. MacArthur Foundation; Endowment Grant Program of the Smithsonian Institution; Laboratories of Analytical Biology at the Smithsonian Institution FX The authors thank J. Case, M. Trifas, J. Atchley, H. Scott, L. Nanson, and two anonymous reviewers for assistance during the preparation of this manuscript and H. Chokthaweepanich, G. Johnson, B. Ingram, J. Jamison and J. Lampley for assistance in the laboratory. This research was supported by a Smithsonian Institution Postdoctoral Fellowship to J.K.T., grants from the John D. and Catherine T. MacArthur Foundation, and the Endowment Grant Program of the Smithsonian Institution to J.W., and the Laboratories of Analytical Biology at the Smithsonian Institution. All sequences have been deposited in GenBank (accession nos. KM208956-KM209195). NR 56 TC 21 Z9 21 U1 0 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X EI 1469-8137 J9 NEW PHYTOL JI New Phytol. PD OCT PY 2014 VL 204 IS 1 BP 66 EP 73 DI 10.1111/nph.12988 PG 8 WC Plant Sciences SC Plant Sciences GA AO2YG UT WOS:000341193500009 PM 25103958 ER PT J AU Rodriguez-Reyes, O Falcon-Lang, H Gasson, P Collinson, M Jaramillo, C AF Rodriguez-Reyes, Oris Falcon-Lang, Howard Gasson, Peter Collinson, Margaret Jaramillo, Carlos TI Fossil woods (Malvaceae) from the lower Miocene (early to mid-Burdigalian) part of the Cucaracha Formation of Panama (Central America) and their biogeographic implications SO REVIEW OF PALAEOBOTANY AND PALYNOLOGY LA English DT Article DE South America; Panama Isthmus; Great American Biotic Interchange; Tile cell; Insidewood ID BEND NATIONAL-PARK; OLMOS FORMATION; NORTH-AMERICA; DNA-SEQUENCES; ANATOMY; EVOLUTION; HISTORY; MAMMALS; GENUS; STERCULIACEAE AB Nine fossil wood specimens are described from the Miocene (early to mid-Burdigalian) part of the Cucaracha Formation of Panama, Central America. The calcareous permineralised fossils, which contain Teredolites borings, occur in erosive-based pebbly conglomerate lenses, interpreted as tidally influenced fluvial channels. All specimens show tile cells characteristic of many clades of the diverse and widespread family Malvaceae sensu APG III. Fossils were identified, more precisely, through searches of the Insidewood Database, and detailed study of comparative extant material. Two novel types of fossil wood occur: (1) Guazumaoxylon miocenica gen. et sp. nov shows paratracheal axial parenchyma with a broad-sheath to winged-aliform distribution combined with intermediate-type tile cells, similar to tropical South American species of Guazuma (subfamily Byttnerioideae) and (2) Periplanetoxylon panamense gen. et sp. nov shows apotracheal axial parenchyma in irregular to regular bands > 3 cells wide combined with Pterospermum-type tile cells, similar to tropical South American species of Pentaplaris (subfamily Malvoideae). The occurrence of fossils showing similarities to extant South American taxa in the Miocene of Panama is of palaeogeographic significance, suggesting intercontinental exchange of tree species at least ten million years before the traditional date for the final closure of the Panama Isthmus. (C) 2014 Elsevier B.V. All rights reserved. C1 [Falcon-Lang, Howard; Collinson, Margaret] Royal Holloway Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. [Gasson, Peter] Royal Bot Gardens, Jodrell Lab, Richmond TW9 3DS, Surrey, England. Smithsonian Trop Res Inst, Balboa, Panama. RP Rodriguez-Reyes, O (reprint author), Royal Holloway Univ London, Dept Earth Sci, Egham TW20 0EX, Surrey, England. EM o.rodriguez@es.rhul.ac.uk FU Secretaria Nacional de Ciencia y Tecnologia (SENACyT); Panama Canal Authority [SAA-199520-KRP]; U.S. National Science Foundation (NSF) [0966884, 0824299] FX ORR acknowledges funding from the Secretaria Nacional de Ciencia y Tecnologia (SENACyT), Panama Canal Authority contract SAA-199520-KRP, U.S. National Science Foundation (NSF) Grants 0966884 (OISE, EAR, DRL) and 0824299 (EAR), National Geographic, Smithsonian Tropical Research Institution, Ricardo Perez S.A., and a Crossland Scholarship held at Royal Holloway, University of London. HFL acknowledges a NERC Advanced Fellowship held at Royal Holloway, University of London. We thank Prof. Pieter Baas and Dr. Elisabeth Wheeler for invaluable advice during an early stage of this work. We also thank A. Rincon, C. Sudrez, J. Moreno, F. Moreno, M. Moya, C. De Gracia, L. Oviedo and M-I Barreto for field assistance and Neil Holloway for making thin sections. Special thanks are also extended to Dr. Camilo Montes who provided information regarding the geological context of the fossils, and to Dr. Sila Pla Pueyo and Sebastian Zimmermann for comments on figure design. Emiliano Peralta-Medina is also thanked for advice on an earlier draft of this manuscript. ORR wishes to thank L. Reyes for her great support. Finally, we extend our thanks to the editor, and two anonymous reviewers, whose comments greatly improved this manuscript. NR 102 TC 5 Z9 5 U1 0 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0034-6667 EI 1879-0615 J9 REV PALAEOBOT PALYNO JI Rev. Palaeobot. Palynology PD OCT PY 2014 VL 209 BP 11 EP 34 DI 10.1016/j.revpalbo.2014.05.006 PG 24 WC Plant Sciences; Paleontology SC Plant Sciences; Paleontology GA AN6HM UT WOS:000340695600002 ER PT J AU Wang, J Xu, XG Ding, SG Zeng, J Spurr, R Liu, X Chance, K Mishchenko, M AF Wang, Jun Xu, Xiaoguang Ding, Shouguo Zeng, Jing Spurr, Robert Liu, Xiong Chance, Kelly Mishchenko, Michael TI A numerical testbed for remote sensing of aerosols, and its demonstration for evaluating retrieval synergy from a geostationary satellite constellation of GEO-CAPE and GOES-R SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Testbed of remote sensing of aerosols; GEO-CAPE; TEMPO; GOES-R; Optimization; Linearized codes for radiative transfer and scattering ID ABSORPTION CROSS-SECTIONS; OZONE UV SPECTROSCOPY; RADIATIVE-TRANSFER; NEXT-GENERATION; MISSION; ALGORITHM; CAPABILITIES; TEMPERATURE; SENSITIVITY; MODELS AB We present a numerical testbed for remote sensing of aerosols, together with a demonstration for evaluating retrieval synergy from a geostationary satellite constellation. The testbed combines inverse (optimal-estimation) software with a forward model containing linearized code for computing particle scattering (for both spherical and non-spherical particles), a kernel-based (land and ocean) surface bi-directional reflectance facility, and a linearized radiative transfer model for polarized radiance. Calculation of gas absorption spectra uses the HITRAN (High-resolution TRANsmission molecular absorption) database of spectroscopic line parameters and other trace species cross-sections. The outputs of the testbed include not only the Stokes 4-vector elements and their sensitivities (Jacobians) with respect to the aerosol single scattering and physical parameters (such as size and shape parameters, refractive index, and plume height), but also DFS (Degree of Freedom for Signal) values for retrieval of these parameters. This testbed can be used as a tool to provide an objective assessment of aerosol information content that can be retrieved for any constellation of (planned or real) satellite sensors and for any combination of algorithm design factors (in terms of wavelengths, viewing angles, radiance and/or polarization to be measured or used). We summarize the components of the testbed, including the derivation and validation of analytical formulae for Jacobian calculations. Benchmark calculations from the forward model are documented. In the context of NASA's Decadal Survey Mission GEO-CAPE (GEOstationary Coastal and Air Pollution Events), we demonstrate the use of the testbed to conduct a feasibility study of using polarization measurements in and around the O-2 A band for the retrieval of aerosol height information from space, as well as an to assess potential improvement in the retrieval of aerosol fine and coarse mode aerosol optical depth (AOD) through the synergic use of two future geostationary satellites, GOES-R (Geostationary Operational Environmental Satellite R-series) and TEMPO (Tropospheric Emissions: Monitoring of Pollution). Strong synergy between GEOS-R and TEMPO are found especially in their characterization of surface bi-directional reflectance, and thereby, can potentially improve the AOD retrieval to the accuracy required by GEO-CAPE. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Wang, Jun; Xu, Xiaoguang; Ding, Shouguo; Zeng, Jing] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE 68588 USA. [Spurr, Robert] RT Solut Inc, Cambridge, MA 02138 USA. [Liu, Xiong; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mishchenko, Michael] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP Wang, J (reprint author), Univ Nebraska, Dept Earth & Atmospher Sci, 303 Bessey Hall, Lincoln, NE 68588 USA. EM jwang7@unl.edu RI Mishchenko, Michael/D-4426-2012; 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; Chance, Kelly/0000-0002-7339-7577 FU NASA Earth Science Division, GEO-CAPE mission study and Glory mission science activities FX Funding for this study was provided by the NASA Earth Science Division as part of GEO-CAPE mission study and Glory mission science activities. J. Wang is grateful to Jassim (Jay) A. Al-Saadi and Hal H. Maring for their support, and thanks the GEO-CAPE aerosol working group and science working group for their constructive suggestions and fruitful discussions. The Holland Computing Center of University of Nebraska - Lincoln and NASA High End Computing program are acknowledged for their help in computing. NR 65 TC 12 Z9 13 U1 1 U2 29 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD OCT PY 2014 VL 146 SI SI BP 510 EP 528 DI 10.1016/j.jqsrt.2014.03.020 PG 19 WC Optics; Spectroscopy SC Optics; Spectroscopy GA AM2RA UT WOS:000339697300049 ER PT J AU McKeon, CS Moore, JM AF McKeon, C. Seabird Moore, Jenna M. TI Species and size diversity in protective services offered by coral guard-crabs SO PEERJ LA English DT Article DE Functional diversity; Functional equivalence; Associational refuge; Complementarity; Mutualism; Symbiosis; Trapezia; Partner benefits; Acanthaster; Pocillopora ID OF-THORNS STARFISH; ACANTHASTER-PLANCI; FUNCTIONAL EQUIVALENCE; FEEDING PREFERENCES; COMMUNITY ECOLOGY; EASTERN PACIFIC; MUTUALISM; REEFS; REDUNDANCY; SEAWEED AB Coral guard-crabs in the genus Trapezia are well-documented defenders of their pocilloporid coral hosts against coral predators such as the Crown-of-Thorns seastar (Acanthaster planci complex). The objectives of this study were to examine the protective services of six species of Trapezia against corallivory, and the extent of functional diversity among these Trapezia species. Studies conducted in Mo'orea, French Polynesia showed the Trapezia-coral mutualism protected the host corals from multiple predators through functional diversity in the assemblage of crab symbionts. Species differed in their defensive efficacy, but species within similar size classes shared similar abilities. Smallersize Trapezia species, which were previously thought to be ineffective guards, play important defensive roles against small corallivores. We also measured the benefits of this mutualism to corals in the midst of an Acanthaster outbreak that reduced the live coral cover on the fore reef to less than 4%. The mutualism may positively affect the reef coral demography and potential for recovery during adverse predation events through shelter of multiple species of small corals near the host coral. Our results show that while functional diversity is supported within the genus, some Trapezia species may be functionally equivalent within the same size class, decreasing the threat of gaps in coral protection caused by absence or replacement of any single Trapezia species. C1 [McKeon, C. Seabird; Moore, Jenna M.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [McKeon, C. Seabird] Smithsonian Inst Marine Sci Network, Smithsonian Marine Stn, Ft Pierce, FL USA. RP McKeon, CS (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM mckeons@si.edu FU University of Florida; BIOCODE Mo'orea project FX This project was funded by an Alumni Fellowship from University of Florida to CS McKeon, and the BIOCODE Mo'orea project to G Paulay. Logistical support was provided by the BIOCODE Mo'orea Project. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 50 TC 10 Z9 10 U1 4 U2 24 PU PEERJ INC PI LONDON PA 341-345 OLD ST, THIRD FLR, LONDON, EC1V 9LL, ENGLAND SN 2167-8359 J9 PEERJ JI PeerJ PD SEP 30 PY 2014 VL 2 AR e574 DI 10.7717/peerj.574 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AY5OS UT WOS:000347622400001 PM 25289176 ER PT J AU Cottontail, VM Kalko, EKV Cottontail, I Wellinghausen, N Tschapka, M Perkins, SL Pinto, CM AF Cottontail, Veronika M. Kalko, Elisabeth K. V. Cottontail, Iain Wellinghausen, Nele Tschapka, Marco Perkins, Susan L. Miguel Pinto, C. TI High Local Diversity of Trypanosoma in a Common Bat Species, and Implications for the Biogeography and Taxonomy of the T. cruzi Clade SO PLOS ONE LA English DT Article ID ARTIBEUS-JAMAICENSIS; RIBOSOMAL-RNA; DELIMITATION; GENE; SCHIZOTRYPANUM; IDENTIFICATION; PHYLOGENY; GRADIENTS; RANGELI; MAMMALS AB The Trypanosoma cruzi clade is a group of parasites that comprises T. cruzi sensu lato and its closest relatives. Although several species have been confirmed phylogenetically to belong to this clade, it is uncertain how many more species can be expected to belong into this group. Here, we present the results of a survey of trypanosome parasites of the bat Artibeus jamaicensis from the Panama Canal Zone, an important seed disperser. Using a genealogical species delimitation approach, the Poisson tree processes (PTP), we tentatively identified five species of trypanosomes - all belonging to the T. cruzi clade. A small monophyletic group of three putative Trypanosoma species places at the base of the clade phylogeny, providing evidence for at least five independent colonization events of these parasites into the New World. Artibeus jamaicensis presents a high diversity of these blood parasites and is the vertebrate with the highest number of putative trypanosome species reported from a single locality. Our results emphasize the need for continued efforts to survey mammalian trypanosomes. C1 [Cottontail, Veronika M.; Kalko, Elisabeth K. V.; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Cottontail, Veronika M.; Wellinghausen, Nele] Univ Ulm, Inst Med Microbiol & Hyg, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.; Tschapka, Marco] Smithsonian Trop Res Inst, Balboa, Panama. [Cottontail, Iain] Kbo Isar Amper Klinikum, Taufkirchen, Vils, Germany. [Wellinghausen, Nele] Gaertner & Colleagues Lab, Ravensburg, Germany. [Perkins, Susan L.; Miguel Pinto, C.] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA. [Miguel Pinto, C.] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Miguel Pinto, C.] CUNY, Grad Ctr, New York, NY USA. [Miguel Pinto, C.] Pontificia Univ Catolica Ecuador, Ctr Invest Enfermedades Infecciosas, Quito, Ecuador. RP Pinto, CM (reprint author), Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA. EM mpinto@amnh.org OI Perkins, Susan/0000-0002-5400-5662 FU STRI trust funds; University of Ulm; Annette Kade Fellowship through the American Museum of Natural History; NSF-DDIG [DEB-1311582]; German national Academic Foundation; Cusanuswerk FX Field work was supported by STRI trust funds to EKVK, and field and laboratory work was funded by grants of the Promotionsprogramm in Experimental Medicine of the University of Ulm and the Cusanuswerk to VMC. Data analyses were supported by an Annette Kade Fellowship through the American Museum of Natural History to CMP and NSF-DDIG grant DEB-1311582 to SLP and CMP, and the German national Academic Foundation to VMC. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 44 TC 13 Z9 14 U1 3 U2 19 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 30 PY 2014 VL 9 IS 9 AR e108603 DI 10.1371/journal.pone.0108603 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AR6CW UT WOS:000343671700120 PM 25268381 ER PT J AU Harasewych, MG AF Harasewych, M. G. TI Bartschia (Agassitula) peartae, a new species of colubrariid (Gastropoda: Colubrariidae) from the tropical western Atlantic SO NAUTILUS LA English DT Article DE "Metula" group; protoconch; larval development ID METULA GASTROPODA; BUCCINIDAE; GENUS AB A new western Atlantic species belonging to the "Metula" group is described and assigned to the subgenus Agassitula, which is provisionally included in the genus Bartschia. This new species, Bartschia (Agassitula) peartae, is larger, thinner, more fusiform, and more densely pigmented than other western Atlantic members of the "Metula" group. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA. EM Harasewych@si.edu NR 33 TC 0 Z9 0 U1 0 U2 1 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD SEP 30 PY 2014 VL 128 IS 3 BP 91 EP 96 PG 6 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AQ9PX UT WOS:000343188900002 ER PT J AU Cleeves, LI Bergin, EA Alexander, CMO Du, FJ Graninger, D Oberg, KI Harries, TJ AF Cleeves, L. Ilsedore Bergin, Edwin A. Alexander, Conel M. O'D. Du, Fujun Graninger, Dawn Oeberg, Karin I. Harries, Tim J. TI The ancient heritage of water ice in the solar system SO SCIENCE LA English DT Article ID LOW-MASS PROTOSTARS; PROTOPLANETARY DISKS; DEUTERIUM FRACTIONATION; DEUTERATED WATER; D/H RATIO; NEBULA; ORIGIN; ABUNDANCES; CHEMISTRY; ASTEROIDS AB Identifying the source of Earth's water is central to understanding the origins of life-fostering environments and to assessing the prevalence of such environments in space. Water throughout the solar system exhibits deuterium-to-hydrogen enrichments, a fossil relic of low-temperature, ion-derived chemistry within either (i) the parent molecular cloud or (ii) the solar nebula protoplanetary disk. Using a comprehensive treatment of disk ionization, we find that ion-driven deuterium pathways are inefficient, which curtails the disk's deuterated water formation and its viability as the sole source for the solar system's water. This finding implies that, if the solar system's formation was typical, abundant interstellar ices are available to all nascent planetary systems. C1 [Cleeves, L. Ilsedore; Bergin, Edwin A.; Du, Fujun] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Alexander, Conel M. O'D.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Graninger, Dawn; Oeberg, Karin I.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harries, Tim J.] Univ Exeter, Dept Phys & Astron, Exeter EX4 4QL, Devon, England. RP Cleeves, LI (reprint author), Univ Michigan, Dept Astron, 311 West Hall,1085 South Univ Ave, Ann Arbor, MI 48109 USA. EM cleeves@umich.edu RI Alexander, Conel/N-7533-2013 OI Alexander, Conel/0000-0002-8558-1427 FU NSF [AST-1008800]; NASA [NNA09DA81A, NNX11AG67G, NNX12A193G]; U.K. Science and Technology Facilities Council [ST/J001627/1] FX L.I.C. and E.A.B. acknowledge support by NSF grant AST-1008800. C.M.O'D.A. was partially supported by NASA Astrobiology grant NNA09DA81A and by NASA Cosmochemistry grant NNX11AG67G. F. D. was supported by NASA grant NNX12A193G. T.J.H. was supported by U.K. Science and Technology Facilities Council grant ST/J001627/1. NR 28 TC 47 Z9 47 U1 7 U2 48 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 26 PY 2014 VL 345 IS 6204 BP 1590 EP 1593 DI 10.1126/science.1258066 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AP6CG UT WOS:000342164500039 PM 25258075 ER PT J AU Laliberte, E Zemunik, G Turner, BL AF Laliberte, Etienne Zemunik, Graham Turner, Benjamin L. TI Environmental filtering explains variation in plant diversity along resource gradients SO SCIENCE LA English DT Article ID 2-MILLION-YEAR DUNE CHRONOSEQUENCE; SPECIES RICHNESS; PHOSPHORUS LIMITATION; COMMUNITY; BIODIVERSITY; GRASSLANDS; HYPOTHESIS; STRATEGIES; EVOLUTION; DOMINANCE AB The mechanisms that shape plant diversity along resource gradients remain unresolved because competing theories have been evaluated in isolation. By testing multiple theories simultaneously across a >2-million-year dune chronosequence in an Australian biodiversity hotspot, we show that variation in plant diversity is not explained by local resource heterogeneity, resource partitioning, nutrient stoichiometry, or soil fertility along this strong resource gradient. Rather, our results suggest that diversity is determined by environmental filtering from the regional flora, driven by soil acidification during long-term pedogenesis. This finding challenges the prevailing view that resource competition controls local plant diversity along resource gradients, and instead reflects processes shaping species pools over evolutionary time scales. C1 [Laliberte, Etienne; Zemunik, Graham] Univ Western Australia, Sch Plant Biol, Crawley, WA 6009, Australia. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Laliberte, E (reprint author), Univ Western Australia, Sch Plant Biol, Crawley, WA 6009, Australia. EM etienne.laliberte@uwa.edu.au RI Laliberte, Etienne/B-6855-2008; Turner, Benjamin/E-5940-2011 OI Laliberte, Etienne/0000-0002-3167-2622; Turner, Benjamin/0000-0002-6585-0722 FU Australian Research Council [DE120100352]; University of Western Australia; Paul Hasluck Bequest FX We thank the Western Australia Department of Parks and Wildlife for access to field sites and facilities. This research was supported by a Discovery Early Career Research Award (DE120100352) from the Australian Research Council and research grants from the University of Western Australia to E. L. and a Ph.D. scholarship to G.Z. from the Paul Hasluck Bequest, administered by the Kwongan Foundation. We thank P. Hayes for collection of leaf nutrient data and J. Grace and H. Lambers for providing comments on the manuscript. The vegetation and soil data are available on Dryad (www.datadryad.org). NR 31 TC 36 Z9 37 U1 14 U2 151 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 26 PY 2014 VL 345 IS 6204 BP 1602 EP 1605 DI 10.1126/science.1256330 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AP6CG UT WOS:000342164500043 PM 25258078 ER PT J AU Almeida, ACS Souza, FBC Menegola, CMS Sanner, J Vieira, LM AF Almeida, Ana C. S. Souza, Facelucia B. C. Menegola, Carla M. S. Sanner, Joann Vieira, Leandro M. TI Taxonomic review of the family Colatooeciidae Winston, 2005 (Bryozoa, Cheilostomata), with description of seven new species SO ZOOTAXA LA English DT Article DE bryozoans; Colatooecia; Cigclisula; Trematooecia; new species; new combinations; redescription ID MARINE BRYOZOA; CLASSIFICATION; SEA AB Colatooeciidae includes the genera Colatooecia, Cigclisula and Trematooecia. While Colatooecia is considered a well-defined genus, the differences between Cigclisula and Trematooecia are poorly defined. This taxonomic review was undertaken to understand the morphological differences between Cigclisula and Trematooecia. The type species of Cigclisula is redescribed and the type species of Trematooecia is designated and redescribed. Diagnostic characters of both genera are redefined. Six new species of Cigclisula and one of Trematooecia are described: Cigclisula australis n. sp., Cigclisula buski n. sp., Cigclisula fistulosa n. sp., Cigclisula osburni n. sp., Cigclisula perforata n. sp., Cigclisula winstonae n. sp. and Trematooecia rotunda n. sp. Four species previously assigned to Cigclisula are transferred to Trematooecia: Trematooecia arborescens (Canu & Bassler, 1928) n. comb., Trematooecia gemmea (Winston & Woollacott, 2009) n. comb., Trematooecia hexagonalis (Canu & Bassler, 1930), and Trematooecia verticalis (Maplestone, 1910) n. comb. Two species previously assigned to Trematooecia are transferred to Cigclisula: Cigclisula turrita (Smitt, 1873) and Cigclisula psammophila (Winston & Hakansson, 1986) n. comb. C1 [Almeida, Ana C. S.; Souza, Facelucia B. C.; Menegola, Carla M. S.] Univ Fed Bahia, Museu Zool, BR-40170290 Salvador, BA, Brazil. [Menegola, Carla M. S.] Univ Fed Bahia, Inst Biol, Lab Biol Porifera & Fauna Assoc, BR-40170290 Salvador, BA, Brazil. [Sanner, Joann] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Vieira, Leandro M.] Univ Sao Paulo, Ctr Biol Marinha, BR-11600000 Sao Sebastiao, SP, Brazil. [Vieira, Leandro M.] Univ Fed Pernambuco, Ctr Ciencias Biol, Dept Zool, BR-50670810 Recife, PE, Brazil. RP Almeida, ACS (reprint author), Univ Fed Bahia, Museu Zool, BR-40170290 Salvador, BA, Brazil. EM carol.salmeida@gmail.com RI Vieira, Leandro/B-7712-2011; Museu de Zoologia da USP, MZ-USP/Q-2192-2016; OI Manzoni Vieira, Leandro/0000-0001-8661-8861; Almeida, Ana Carolina/0000-0003-4899-1483 FU FAPESB [4076/2012]; FAPESP [2012/24285-1] FX We are grateful to the Programa de Pos-Graduacao em Diversidade Animal of Universidade Federal da Bahia, the Smithsonian's National Museum of Natural History (USA), Departament of Life Sciences, Natural History Museum of London (NHMUK), Marlene Peso-Aguiar (Laboratorio de Malacologia e Ecologia de Bentos, UFBA) and Orane Alves (Laboratorio de Geoecologia de Sedimentos Marinhos, UFBA) for logistical support. Thanks also to Paul Taylor (NHMUK), Mary Spencer Jones (NHMUK), Masato Hirose (University of Tokyo), Phil Bock (Museum Victoria) and Judith E. Winston (VMNH), who sent comparative images and data of type specimens included in the present study. Funding was provided by FAPESB (Proc. 4076/2012) to A.C.S. Almeida, and FAPESP (Proc. 2012/24285-1) to L.M. Vieira. We also thank Centro de Pesquisa Goncalo Moniz (FIOCRUZ/ BA) for SEMs images. All SEMs images of specimens deposited at the NHMUK (Figs 3, 4, 6, 7, 13, 30 and 32) was used by permission of The Trustees of the Natural History Museum, London. NR 74 TC 1 Z9 1 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 26 PY 2014 VL 3868 IS 1 BP 1 EP 61 PG 61 WC Zoology SC Zoology GA AP5PB UT WOS:000342130000001 PM 25283785 ER PT J AU Witczak-Krempa, W Knap, M Abanin, D AF Witczak-Krempa, William Knap, Michael Abanin, Dmitry TI Interacting Weyl Semimetals: Characterization via the Topological Hamiltonian and its Breakdown SO PHYSICAL REVIEW LETTERS LA English DT Article ID INSULATORS; FERMIONS; GRAPHENE AB Weyl semimetals (WSMs) constitute a 3D phase with linearly dispersing Weyl excitations at low energy, which lead to unusual electrodynamic responses and open Fermi arcs on boundaries. We derive a simple criterion to identify and characterize WSMs in an interacting setting using the exact electronic Green's function at zero frequency, which defines a topological Bloch Hamiltonian. We apply this criterion by numerically analyzing, via cluster and other methods, interacting lattice models with and without time-reversal symmetry. We identify various mechanisms for how interactions move and renormalize Weyl fermions. Our methods remain valid in the presence of long-ranged Coulomb repulsion. Finally, we introduce a WSM-like phase for which our criterion breaks down due to fractionalization: the charge-carrying Weyl quasiparticles are orthogonal to the electron. C1 [Witczak-Krempa, William; Abanin, Dmitry] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Knap, Michael] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Knap, Michael] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Witczak-Krempa, W (reprint author), Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. RI Knap, Michael/H-3344-2011 OI Knap, Michael/0000-0002-7093-9502 FU Austrian Science Fund (FWF) [J 3361-N20]; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX W. W. K. is particularly indebted to D. M. Haldane, Y. B. Kim, S. S. Lee, and T. Senthil for discussions. We acknowledge stimulating exchanges with A. Go, B. I. Halperin, J. Maciejko, E. G. Moon, R. Nandkishore, and A. Vishwanath. W. W. K. is grateful for the hospitality of Harvard and the Princeton Center for Theoretical Physics, where some of the work was completed. M. K. was supported by the Austrian Science Fund (FWF) Project No. J 3361-N20. 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. NR 43 TC 21 Z9 21 U1 3 U2 15 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD SEP 25 PY 2014 VL 113 IS 13 AR 136402 DI 10.1103/PhysRevLett.113.136402 PG 5 WC Physics, Multidisciplinary SC Physics GA CG9RU UT WOS:000353657400007 PM 25302910 ER PT J AU Batista, A Jaramillo, CA Ponce, M Crawford, AJ AF Batista, Abel Jaramillo A., Cesar A. Ponce, Marcos Crawford, Andrew J. TI A new species of Andinobates (Amphibia: Anura: Dendrobatidae) from west central Panama SO ZOOTAXA LA English DT Article DE Andinobates geminisae sp nov.; conservation; DNA barcoding; geographic distribution; molecular phylogenetics; Panama; poison dart frogs ID POISON FROGS; DNA-SEQUENCES; MITOCHONDRIAL-DNA; CLASSIFICATION; APOSEMATISM; SYSTEMATICS; DIVERSITY; RICHNESS; MULTIPLE; REVISION AB Dendrobatid frogs are among the best known anurans in the world, mainly due to their toxicity and associated bright colors. A recently described dendrobatid genus, Andinobates, comprises frogs distributed among the Colombian Andes and Panama. During field work in the Distrito de Donoso, Colon province, Panama, we found a poison frog that we here describe as a new species. The new species belongs to the A. minutus species group and is described herein as Andinobates geminisae sp. nov. This new species differs from all other members of the group by having uniformly orange smooth skin over the entire body and a distinctive male advertisement call. The new species is smaller than other colorful dendrobatids present in the area, such as Oophaga pumilio and O. vicentei. We also provide molecular phylogenetic analyses of mitochondrial DNA sequences of dendrobatids and summarize genetic distances among Andinobates species. Andinobates geminisae occurs in Caribbean versant rainforest on the westernmost edge of the known distribution of A. minutus, and represents the fourth species within this genus in Panama. This is vulnerable to habitat loss and excessive harvesting and requires immediate conservation plans to preserve this species with a restricted geographic range. C1 [Batista, Abel; Ponce, Marcos] Univ Autonoma Chiriqui, David, Panama. [Batista, Abel] Senckenberg Forschungsinst & Nat Museum Frankfurt, D-60325 Frankfurt, Germany. [Jaramillo A., Cesar A.; Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Jaramillo A., Cesar A.; Crawford, Andrew J.] Circulo Herpetol Panama, Panama City, Panama. [Crawford, Andrew J.] Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. [Jaramillo A., Cesar A.] Univ Panama, Fac Med, Dept Histol & Neuroanat Humana, Panama City, Panama. RP Batista, A (reprint author), Univ Autonoma Chiriqui, David, Panama. EM abelbatista@hotmail.com FU MWH-Panama; Minera Panama S.A; CBOL grant FX Collecting permits SC/A-8-09 and SC/A-21-10, as well as the corresponding exportation permits were issued by the Direccion de Areas Protegidas y Vida Silvestre of the Autoridad Nacional del Ambiente (ANAM), Panama City, Panama. This work was supported financially MWH-Panama and Minera Panama S.A. DNA sequences was supported by a CBOL grant in support of DNA barcoding of the vertebrates of Panama. NR 74 TC 1 Z9 1 U1 3 U2 21 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 24 PY 2014 VL 3866 IS 3 BP 333 EP 352 PG 20 WC Zoology SC Zoology GA AP5OI UT WOS:000342128100002 PM 25283663 ER PT J AU Whittaker, RJ Rigal, F Borges, PAV Cardoso, P Terzopoulou, S Casanoves, F Pla, L Guilhaumon, F Ladle, RJ Triantis, KA AF Whittaker, Robert J. Rigal, Francois Borges, Paulo A. V. Cardoso, Pedro Terzopoulou, Sofia Casanoves, Fernando Pla, Laura Guilhaumon, Francois Ladle, Richard J. Triantis, Kostas A. TI Functional biogeography of oceanic islands and the scaling of functional diversity in the Azores SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE island biogeography; saturation; arthropods; assembly rules; habitat destruction ID SPECIES-AREA RELATIONSHIP; LAND-USE CHANGE; ARTHROPODS; RICHNESS; ARCHIPELAGO; EXTINCTIONS; FORESTS; INDEXES; FLORAS; BIRDS AB Analyses of species-diversity patterns of remote islands have been crucial to the development of biogeographic theory, yet little is known about corresponding patterns in functional traits on islands and how, for example, they may be affected by the introduction of exotic species. We collated trait data for spiders and beetles and used a functional diversity index (FRic) to test for nonrandomness in the contribution of endemic, other native (also combined as indigenous), and exotic species to functional-trait space across the nine islands of the Azores. In general, for both taxa and for each distributional category, functional diversity increases with species richness, which, in turn scales with island area. Null simulations support the hypothesis that each distributional group contributes to functional diversity in proportion to their species richness. Exotic spiders have added novel trait space to a greater degree than have exotic beetles, likely indicating greater impact of the reduction of immigration filters and/or differential historical losses of indigenous species. Analyses of species occurring in native-forest remnants provide limited indications of the operation of habitat filtering of exotics for three islands, but only for beetles. Although the general linear (not saturating) pattern of trait-space increase with richness of exotics suggests an ongoing process of functional enrichment and accommodation, further work is urgently needed to determine how estimates of extinction debt of indigenous species should be adjusted in the light of these findings. C1 [Whittaker, Robert J.; Ladle, Richard J.; Triantis, Kostas A.] Univ Oxford, Sch Geog & Environm, Oxford OX1 3QY, England. [Whittaker, Robert J.] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, Copenhagen, Denmark. [Rigal, Francois; Borges, Paulo A. V.; Cardoso, Pedro; Terzopoulou, Sofia; Guilhaumon, Francois; Triantis, Kostas A.] Univ Acores, Azorean Biodivers Grp, CITA A, P-9700042 Terceira, Azores, Portugal. [Rigal, Francois; Borges, Paulo A. V.; Cardoso, Pedro; Terzopoulou, Sofia; Guilhaumon, Francois; Triantis, Kostas A.] Univ Acores, PEERS, Dept Ciencias Agr, P-9700042 Terceira, Azores, Portugal. [Cardoso, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Cardoso, Pedro] Univ Helsinki, Finnish Museum Nat Hist, FIN-00014 Helsinki, Finland. [Terzopoulou, Sofia; Triantis, Kostas A.] Univ Athens, Fac Biol, Dept Ecol & Taxon, GR-15784 Athens, Greece. [Casanoves, Fernando] Ctr Agron Trop Invest Ensenanza, Cartago 30501, Turrialba, Costa Rica. [Pla, Laura] Univ Nacl Expt Francisco Miranda, Complejo Docente El Hatillo, Coro 4101, Venezuela. [Guilhaumon, Francois] Univ Evora, Rui Nabeiro Biodivers Chair, Ctr Invest Biodiversidade & Recursos Genet, P-7000890 Evora, Portugal. [Ladle, Richard J.] Univ Fed Alagoas, Inst Biol Sci & Hlth, Maceio, Alagoas, Brazil. RP Whittaker, RJ (reprint author), Univ Oxford, Sch Geog & Environm, S Parks Rd, Oxford OX1 3QY, England. EM robert.whittaker@ouce.ox.ac.uk RI publicationpage, cmec/B-4405-2017; Borges, Paulo/B-2780-2008; Whittaker, Robert/H-1548-2015; Cardoso, Pedro/A-8820-2008; Ladle, Richard/E-4228-2014; Casanoves, Fernando/I-3588-2016; publist, CMEC/C-3010-2012 OI Guilhaumon, Francois/0000-0003-4707-8932; Borges, Paulo/0000-0002-8448-7623; Whittaker, Robert/0000-0001-7775-3383; Cardoso, Pedro/0000-0001-8119-9960; Ladle, Richard/0000-0003-3200-3946; Casanoves, Fernando/0000-0001-8765-9382; FU Fundacao para a Ciencia e a Tecnologia (FCT) [FCT-PTDC/BIA-BEC/100182/2008]; FCT [SFRH/BPD/44306/2008, FCT-PTDC/BIA-BIC/119255/2010, SFRH/BPD/40688/2007]; "Range Shift" Project [FCT-PTDC/AAC-AMB/098163/2008]; European Social Fund; Azorean Biodiversity Group grant FX For contributing beetle-trait data and measurements, we thank Volker Assing, Andres Baselga, Marina Blas, Simone Fattorini, Rafael Garcia, Maria Kamilari, Elena Gotsi, Jorge Lobo, Pedro Oromi, Wolfgang Rucker, Jose Serrano, Antonio O. Soares, Peter Sprick, Zdenek Svec, and Dmitry Ternov. We thank the journal reviewers and editor for comments. This study was partly financed by Fundacao para a Ciencia e a Tecnologia (FCT) Project FCT-PTDC/BIA-BEC/100182/2008. K. A. T., F. R., and P. C. were supported by FCT Fellowships SFRH/BPD/44306/2008, FCT-PTDC/BIA-BIC/119255/2010, and SFRH/BPD/40688/2007, respectively; F. G. by "Range Shift" Project FCT-PTDC/AAC-AMB/098163/2008, cofinanced by the European Social Fund; and S. T. by an Azorean Biodiversity Group grant. NR 36 TC 23 Z9 23 U1 4 U2 55 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 SEP 23 PY 2014 VL 111 IS 38 BP 13709 EP 13714 DI 10.1073/pnas.1218036111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AP3PC UT WOS:000341988200024 PM 25225395 ER PT J AU Kembel, SW O'Connor, TK Arnold, HK Hubbell, SP Wright, SJ Green, JL AF Kembel, Steven W. O'Connor, Timothy K. Arnold, Holly K. Hubbell, Stephen P. Wright, S. Joseph Green, Jessica L. TI Relationships between phyllosphere bacterial communities and plant functional traits in a neotropical forest SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE tropical forests; host-microbe associations; plant microbiome; microbial ecology ID LEAF ECONOMICS SPECTRUM; HUMAN MICROBIOME; GUT MICROBIOME; RHIZOSPHERE MICROBIOME; ARABIDOPSIS-THALIANA; DIVERSITY PATTERNS; NITROGEN-FIXATION; TROPICAL TREES; ECOLOGY; MICROORGANISMS AB The phyllosphere-the aerial surfaces of plants, including leaves-is a ubiquitous global habitat that harbors diverse bacterial communities. Phyllosphere bacterial communities have the potential to influence plant biogeography and ecosystem function through their influence on the fitness and function of their hosts, but the host attributes that drive community assembly in the phyllosphere are poorly understood. In this study we used high-throughput sequencing to quantify bacterial community structure on the leaves of 57 tree species in a neotropical forest in Panama. We tested for relationships between bacterial communities on tree leaves and the functional traits, taxonomy, and phylogeny of their plant hosts. Bacterial communities on tropical tree leaves were diverse; leaves from individual trees were host to more than 400 bacterial taxa. Bacterial communities in the phyllosphere were dominated by a core microbiome of taxa including Actinobacteria, Alpha-, Beta-, and Gammaproteobacteria, and Sphingobacteria. Host attributes including plant taxonomic identity, phylogeny, growth and mortality rates, wood density, leaf mass per area, and leaf nitrogen and phosphorous concentrations were correlated with bacterial community structure on leaves. The relative abundances of several bacterial taxa were correlated with suites of host plant traits related to major axes of plant trait variation, including the leaf economics spectrum and the wood density-growth/mortality tradeoff. These correlations between phyllosphere bacterial diversity and host growth, mortality, and function suggest that incorporating information on plant-microbe associations will improve our ability to understand plant functional biogeography and the drivers of variation in plant and ecosystem function. C1 [Kembel, Steven W.] Univ Quebec, Dept Sci Biol, Montreal, PQ H3C 3P8, Canada. [Kembel, Steven W.; O'Connor, Timothy K.; Arnold, Holly K.; Green, Jessica L.] Univ Oregon, Inst Ecol & Evolut, Eugene, OR 97403 USA. [O'Connor, Timothy K.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Hubbell, Stephen P.; Wright, S. Joseph] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Green, Jessica L.] Santa Fe Inst, Santa Fe, NM 87501 USA. RP Kembel, SW (reprint author), Univ Quebec, Dept Sci Biol, CP 8888, Montreal, PQ H3C 3P8, Canada. EM kembel.steven_w@uqam.ca RI Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Kembel, Steven/0000-0001-5224-0952 FU Center for Tropical Forest Science Research Grant; Smithsonian Tropical Research Institute; University of Oregon; Canada Research Chairs program; Natural Sciences and Engineering Research Council of Canada; Center for Tropical Forest Science; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund FX We thank Rufino Gonzalez and Omar Hernandez for their assistance in the field. This study was supported by a Center for Tropical Forest Science Research Grant, the Smithsonian Tropical Research Institute, and the University of Oregon. S. W. K. was supported by the Canada Research Chairs program and the Natural Sciences and Engineering Research Council of Canada. The Barro Colorado Island forest dynamics research project was made possible by the National Science Foundation, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Small World Institute Fund, and numerous private individuals, and through the hard work of more than 100 people from 10 countries over the past two decades. NR 75 TC 45 Z9 45 U1 17 U2 154 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 SEP 23 PY 2014 VL 111 IS 38 BP 13715 EP 13720 DI 10.1073/pnas.1216057111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AP3PC UT WOS:000341988200025 PM 25225376 ER PT J AU Bariani, F Singh, S Buchmann, LF Vengalattore, M Meystre, P AF Bariani, F. Singh, S. Buchmann, L. F. Vengalattore, M. Meystre, P. TI Hybrid optomechanical cooling by atomic Lambda systems SO PHYSICAL REVIEW A LA English DT Article ID QUANTUM GROUND-STATE; RECOIL-INDUCED RESONANCES; LASER AB We investigate a hybrid quantum system consisting of a cavity optomechanical device optically coupled to an ultracold quantum gas. We show that the dispersive properties of the ultracold gas can be used to dramatically modify the optomechanical response of the mechanical resonator. We examine hybrid schemes wherein the mechanical resonator is coupled either to the motional or the spin degrees of freedom of the ultracold gas. In either case, we find an enhancement of more than two orders of magnitude in optomechanical cooling due to this hybrid interaction. Significantly, based on demonstrated parameters for the cavity optomechanical device, we identify regimes that enable the ground-state cooling of the resonator from room temperature. In addition, the hybrid system considered here represents a powerful interface for the use of an ultracold quantum gas for state preparation, sensing, and quantum manipulation of a mesoscopic mechanical resonator. C1 [Bariani, F.; Buchmann, L. F.; Meystre, P.] Univ Arizona, Dept Phys, Coll Opt Sci, Tucson, AZ 85721 USA. [Singh, S.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Buchmann, L. F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Vengalattore, M.] Cornell Univ, Atom & Solid State Phys Lab, Ithaca, NY 14853 USA. RP Bariani, F (reprint author), Univ Arizona, Dept Phys, Coll Opt Sci, Tucson, AZ 85721 USA. RI Bariani, Francesco/F-6908-2011; Vengalattore, Mukund/B-2781-2015 OI Bariani, Francesco/0000-0002-8632-6794; FU U.S. Army Research Office; US NSF; Cornell Center for Materials Research; NSF MRSEC program [DMR-1120296]; NSF INSPIRE program; Alfred P. Sloan Foundation; SNSF; DARPA QuASAR program through grant from AFOSR; DARPA ORCHID program through grant from ARO; DARPA QuASAR program through grant from ARO; DARPA ORCHID program through grant from AFOSR FX We thank S. Steinke, Y. S. Patil, S. Chakram, and S. Yelin for useful discussions. This work was supported by the DARPA QuASAR and ORCHID programs through grants from AFOSR and ARO, the U.S. Army Research Office, the US NSF, the Cornell Center for Materials Research with funding from the NSF MRSEC program (DMR-1120296) and the NSF INSPIRE program. M. V. acknowledges support from the Alfred P. Sloan Foundation. L. F. B. acknowledges support from the SNSF. NR 31 TC 16 Z9 17 U1 0 U2 13 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD SEP 22 PY 2014 VL 90 IS 3 AR 033838 DI 10.1103/PhysRevA.90.033838 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AR7AU UT WOS:000343733200020 ER PT J AU Ubler, H Naab, T Oser, L Aumer, M Sales, LV White, SDM AF Uebler, Hannah Naab, Thorsten Oser, Ludwig Aumer, Michael Sales, Laura V. White, Simon D. M. TI Why stellar feedback promotes disc formation in simulated galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: evolution; galaxies: formation; galaxies: spiral ID SMOOTHED PARTICLE HYDRODYNAMICS; COLD DARK-MATTER; ANGULAR-MOMENTUM PROBLEM; LAMBDA-CDM UNIVERSE; STAR-FORMATION; COSMOLOGICAL SIMULATIONS; SUPERNOVA FEEDBACK; METAL ENRICHMENT; INTERSTELLAR-MEDIUM; MOLECULAR-HYDROGEN AB We study how feedback influences baryon infall on to galaxies using cosmological, zoom-in simulations of haloes with present mass M-vir = 6.9 x 10(11) to 1.7 x 10(12)M(circle dot). Starting at z = 4 from identical initial conditions, implementations of weak and strong stellar feedback produce bulge- and disc-dominated galaxies, respectively. Strong feedback favours disc formation: (1) because conversion of gas into stars is suppressed at early times, as required by abundance matching arguments, resulting in flat star formation histories and higher gas fractions; (2) because 50 per cent of the stars form in situ from recycled disc gas with angular momentum only weakly related to that of the z = 0 dark halo; (3) because late-time gas accretion is typically an order of magnitude stronger and has higher specific angular momentum, with recycled gas dominating over primordial infall; (4) because 25-30 per cent of the total accreted gas is ejected entirely before z similar to 1, removing primarily low angular momentum material which enriches the nearby intergalactic medium. Most recycled gas roughly conserves its angular momentum, but material ejected for long times and to large radii can gain significant angular momentum before re-accretion. These processes lower galaxy formation efficiency in addition to promoting disc formation. C1 [Uebler, Hannah; Naab, Thorsten; Aumer, Michael; White, Simon D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Oser, Ludwig] Columbia Univ, Dept Astron & Astrophys, New York, NY 10027 USA. [Sales, Laura V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ubler, H (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany. EM hannah@mpa-garching.mpg.de OI Aumer, Michael/0000-0003-4046-6502 FU DFG excellence cluster 'Origin and Structure of the Universe'; DFG [SPP1573] FX We thank the anonymous referee for valuable comments on the draft. TN and MA acknowledge support from the DFG excellence cluster 'Origin and Structure of the Universe'. TN acknowledges support from the DFG priority program SPP1573. NR 91 TC 28 Z9 28 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 21 PY 2014 VL 443 IS 3 BP 2092 EP 2111 DI 10.1093/mnras/stu1275 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6KL UT WOS:000342920400018 ER PT J AU Ogrean, GA Bruggen, M van Weeren, RJ Burgmeier, A Simionescu, A AF Ogrean, G. A. Brueggen, M. van Weeren, R. J. Burgmeier, A. Simionescu, A. TI No shock across part of a radio relic in the merging galaxy cluster ZwCl 2341.1+0000? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; galaxies: clusters: individual: ZwCl 2341.1+0000; X-rays: galaxies: clusters ID LARGE-SCALE STRUCTURE; X-RAY OBSERVATIONS; CIZA J2242.8+5301; COMA CLUSTER; EMISSION; ACCELERATION; MERGER; FILAMENT; FRONT; WAVES AB The galaxy cluster ZwCl 2341.1+0000 is a merging system at z = 0.27, which hosts two radio relics and a central, faint, filamentary radio structure. The two radio relics have unusually flat integrated spectral indices of -0.49 +/- 0.18 and -0.76 +/- 0.17, values that cannot be easily reconciled with the theory of standard diffusive shock acceleration of thermal particles at weak merger shocks. We present imaging results from XMM-Newton and Chandra observations of the cluster, aimed to detect and characterize density discontinuities in the intracluster medium. As expected, we detect a density discontinuity near each of the radio relics. However, if these discontinuities are the shock fronts that fuelled the radio emission, then their Mach numbers are surprisingly low, both <= 2. We studied the aperture of the density discontinuities, and found that while the NW discontinuity spans the whole length of the NW radio relic, the arc spanned by the SE discontinuity is shorter than the arc spanned by the SE relic. This startling result is in apparent contradiction with our current understanding of the origin of radio relics. Deeper X-ray data are required to confirm our results and to determine the nature of the density discontinuities. C1 [Ogrean, G. A.; Brueggen, M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burgmeier, A.] Deutsch Elektronen Synchrotron DESY, D-22607 Hamburg, Germany. [Simionescu, A.] Japan Aerosp Explorat Agcy, Chofu, Tokyo 1828522, Japan. RP Ogrean, GA (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM gogrean@hs.uni-hamburg.de OI van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft (DFG) [SFB 676]; DFG [FOR 1254]; NASA through Einstein Postdoctoral Fellowship by Chandra X-ray Center [PF2-130104]; NASA [NAS8-03060]; ESA Member States; USA (NASA) FX We thank the referee for helpful comments. GAO is supported by the research group SFB 676, funded by the Deutsche Forschungsgemeinschaft (DFG). MB acknowledges support by the research group FOR 1254, funded by the DFG. RJvW acknowledges support provided by NASA through Einstein Postdoctoral Fellowship 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. This research is based on data from observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research has also made use of data obtained from the Chandra Data Archive, and of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO, CHIPS, and SHERPA. NR 34 TC 7 Z9 7 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 SEP 21 PY 2014 VL 443 IS 3 BP 2463 EP 2474 DI 10.1093/mnras/stu1299 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ6KL UT WOS:000342920400043 ER PT J AU Boroson, B Vrtilek, SD Raymond, J AF Boroson, Bram Vrtilek, Saeqa Dil Raymond, John TI FUSE OBSERVATIONS OF A FULL ORBIT OF SCORPIUS X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: neutron; ultraviolet: stars; X-rays: binaries ID ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; MOLECULAR-HYDROGEN; SCO X-1; DOPPLER TOMOGRAPHY; ACCRETION DISKS; EMISSION-LINES; BAND SYSTEM; HERCULES-X-1; STAR; IUE AB We obtained UV spectra of X-ray binary Scorpius X-1 in the 900-1200 angstrom range with the Far Ultraviolet Spectroscopic Explorer over the full 0.79 day binary orbit. The strongest emission lines are the doublet of OVI at 1032,1038 angstrom and the C III complex at 1175 angstrom. The spectrum is affected by a multitude of narrow interstellar absorption lines, both atomic and molecular. Examination of line variability and Doppler tomograms suggests emission from both the neighborhood of the donor star and the accretion disk. Models of turbulence and Doppler broadened Keplerian disk lines Doppler shifted with the orbit of the neutron star added to narrow Gaussian emission lines with undetermined Doppler shift fit the data with consistent values of disk radius, inclination, and radial line brightness profile. The Doppler shift of the narrow component with the orbit suggests an association with the donor star. We test our line models with previously analyzed near UV spectra obtained with the Hubble Space Telescope (HST) Goddard High Resolution Spectrograph and archival spectra obtained with the HST Cosmic Origins Spectrograph. C1 [Boroson, Bram] Clarion Univ Pennsylvania, Morrow, GA 30260 USA. [Vrtilek, Saeqa Dil; Raymond, John] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Boroson, B (reprint author), Clarion Univ Pennsylvania, 2000 Clayton State Blvd, Morrow, GA 30260 USA. EM bramboroson@clayton.edu; svrtilek@cfa.harvard.edu; jraymond@cfa.harvard.edu FU Johns Hopkins University under NASA [NAS5-32985]; Association of Universities for Research in Astronomy, Inc., under NASA [GO-05874.01-94A] FX Based on observations made with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer (FUSE). FUSE is operated for NASA by the Johns Hopkins University under NASA contract NAS5-32985. Based on observations 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 GO-05874.01-94A. We thank D. Steeghs for providing optical spectra of Sco X-1 NR 40 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 SEP 20 PY 2014 VL 793 IS 1 AR 59 DI 10.1088/0004-637X/793/1/59 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700059 ER PT J AU Bush, SJ Kennicutt, RC Ashby, MLN Johnson, BD Bresolin, F Fazio, G AF Bush, Stephanie J. Kennicutt, Robert C. Ashby, M. L. N. Johnson, Benjamin D. Bresolin, Fabio Fazio, Giovanni TI A PILOT STUDY USING DEEP INFRARED IMAGING TO CONSTRAIN THE STAR FORMATION HISTORY OF THE XUV STELLAR POPULATIONS IN NGC 4625 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: spiral; galaxies: structure; infrared: galaxies ID EXTENDED ULTRAVIOLET DISKS; SPITZER-SPACE-TELESCOPE; EXTREME OUTER DISK; H II REGIONS; NEARBY GALAXIES; COSMOLOGICAL SIMULATIONS; SURFACE PHOTOMETRY; SPIRAL GALAXIES; LOCAL UNIVERSE; GALACTIC DISKS AB In a Lambda CDM universe, disk galaxies' outer regions are the last to form. Characterizing their contents is critical for understanding the ongoing process of disk formation, but observing outer disk stellar populations is challenging due to their low surface brightness. We present extremely deep 3.6 mu m observations (Spitzer/Infrared Array Camera) of NGC 4625, a galaxy known for its radially extended ultraviolet-emitting stellar population. We combine the new imaging with archival UV imaging from the GALEX mission to derive multi-wavelength radial profiles for NGC 4625 and compare them to stellar populations models. The colors can be explained by the young stellar population that is responsible for the UV emission and indicate that the current star formation rates in the outermost disk are recent. Extended star formation in NGC 4625 may have been initiated by an interaction with neighboring galaxies NGC 4618 and NGC 4625a, supporting speculation that minor interactions are a common trigger for outer disk star formation and late stage disk growth. C1 [Bush, Stephanie J.; Ashby, M. L. N.; Fazio, Giovanni] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02143 USA. [Kennicutt, Robert C.; Johnson, Benjamin D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Bresolin, Fabio] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Bush, SJ (reprint author), Univ Reading, Dept Meteorol, Earley Gate, Reading RG6 6BB, Berks, England. EM sbush@cfa.harvard.edu NR 64 TC 2 Z9 2 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 SEP 20 PY 2014 VL 793 IS 1 AR 65 DI 10.1088/0004-637X/793/1/65 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700065 ER PT J AU Damjanov, I Hwang, HS Geller, MJ Chilingarian, I AF Damjanov, Ivana Hwang, Ho Seong Geller, Margaret J. Chilingarian, Igor TI THE NUMBER DENSITY OF QUIESCENT COMPACT GALAXIES AT INTERMEDIATE REDSHIFT SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: stellar content; galaxies: structure ID SIMILAR-TO 2; DIGITAL SKY SURVEY; PASSIVELY EVOLVING GALAXIES; ULTRA-DEEP-FIELD; SUPERDENSE MASSIVE GALAXIES; HUBBLE-SPACE-TELESCOPE; INSIDE-OUT GROWTH; SIZE EVOLUTION; ELLIPTIC GALAXIES; STELLAR POPULATIONS AB Massive compact systems at 0.2 < z < 0.6 are the missing link between the predominantly compact population of massive quiescent galaxies at high redshift and their analogs and relics in the local volume. The evolution in number density of these extreme objects over cosmic time is the crucial constraining factor for the models of massive galaxy assembly. We select a large sample of similar to 200 intermediate-redshift massive compacts from the Baryon Oscillation Spectroscopic Survey (BOSS) spectroscopy by identifying point-like Sloan Digital Sky Survey photometric sources with spectroscopic signatures of evolved redshifted galaxies. A subset of our targets have publicly available high-resolution ground-based images that we use to augment the dynamical and stellar population properties of these systems by their structural parameters. We confirm that all BOSS compact candidates are as compact as their high-redshift massive counterparts and less than half the size of similarly massive systems at z similar to 0. We use the completeness-corrected numbers of BOSS compacts to compute lower limits on their number densities in narrow redshift bins spanning the range of our sample. The abundance of extremely dense quiescent galaxies at 0.2 < z < 0.6 is in excellent agreement with the number densities of these systems at high redshift. Our lower limits support the models of massive galaxy assembly through a series of minor mergers over the redshift range 0 < z < 2. C1 [Damjanov, Ivana] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hwang, Ho Seong; Geller, Margaret J.; Chilingarian, Igor] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chilingarian, Igor] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. RP Damjanov, I (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM idamjanov@cfa.harvard.edu RI Chilingarian, Igor/N-5117-2016; OI Chilingarian, Igor/0000-0002-7924-3253; 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]; Russian Science Foundation [14-22-00041]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX We thank the anonymous referee for thoughtful suggestions that improved the clarity of our manuscript. 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 H.S.H., M.J.G., and I.C. I.C. acknowledges support from the Russian Science Foundation project #14-22-00041. We acknowledge the use of the CADC data collections. This work is based on the SDSS-III data set. 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, NewMexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 79 TC 16 Z9 16 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 SEP 20 PY 2014 VL 793 IS 1 AR 39 DI 10.1088/0004-637X/793/1/39 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700039 ER PT J AU Flaherty, KM Muzerolle, J Wolk, SJ Rieke, G Gutermuth, R Balog, Z Herbst, W Megeath, ST Furlan, E AF Flaherty, K. M. Muzerolle, J. Wolk, S. J. Rieke, G. Gutermuth, R. Balog, Z. Herbst, W. Megeath, S. T. Furlan, E. TI CONNECTING X-RAY AND INFRARED VARIABILITY AMONG YOUNG STELLAR OBJECTS: RULING OUT POTENTIAL SOURCES OF DISK FLUCTUATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; stars: pre-main sequence ID ORION NEBULA CLUSTER; T-TAURI STARS; MAGNETIC-FIELDS; MIDINFRARED VARIABILITY; PROTOPLANETARY DISK; PROTOSTELLAR DISKS; MASS ACCRETION; LIGHT CURVES; CSI 2264; IC-348 AB Variability in the infrared emission from disks around pre-main-sequence stars over the course of days to weeks appears to be common, but the physical cause of the changes in disk structure are not constrained. Here we present coordinated monitoring of one young cluster with the Spitzer and Chandra space telescopes aimed at studying the physical source of the variability. In fall 2011 we obtained 10 epochs of Chandra ACIS photometry over a period of 30 days with a roughly 3 day cadence contemporaneous with 20 epochs of Spitzer [3.6], [4.5] photometry over 40 days with a roughly 2 day cadence of the IC 348 cluster. This cadence allows us to search for week-to month-long responses of the infrared emission to changes in the high-energy flux. We find no strong evidence for a direct link between the X-ray and infrared variability on these timescales among 39 cluster members with circumstellar disks. There is no significant correlation between the shape of the infrared and X-ray light curves or between the sizes of the X-ray and infrared variability. Among the stars with an X-ray flare, none showed evidence of a correlated change in the infrared photometry on timescales of days to weeks following the flare. This lack of connection implies that X-ray heating of the planet-forming region of the disk is not significant, although we cannot rule out rapid or instantaneous changes in infrared emission. C1 [Flaherty, K. M.; Rieke, G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Flaherty, K. M.; Herbst, W.] Wesleyan Univ, Dept Astron, Middletown, CT 06459 USA. [Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Balog, Z.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Furlan, E.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Flaherty, KM (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. EM kflaherty@wesleyan.edu OI Furlan, Elise/0000-0001-9800-6248; Balog, Zoltan/0000-0003-1748-2926 FU National Aeronautics and Space Administration through Chandra Award [G02-13028A]; National Aeronautics Space Administration [NAS8-03060]; NASA; NASA ADAP grants [NNX11AD14G, NNX13AF08G]; Caltech/JPL awards [1373081, 142329, 1440160]; Spitzer Space Telescope observing programs FX We thank the anonymous referee for the substantive comments that greatly improved this paper. The scientific results reported in this article are based in part on observations made by the Chandra X-ray Observatory. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G02-13028A 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. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for the work was provided by NASA through an award issued by JPL/Caltech. R.G. gratefully acknowledges funding support from NASA ADAP grants NNX11AD14G and NNX13AF08G and Caltech/JPL awards 1373081, 142329, and 1440160 in support of Spitzer Space Telescope observing programs. NR 64 TC 9 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 SEP 20 PY 2014 VL 793 IS 1 AR 2 DI 10.1088/0004-637X/793/1/2 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700002 ER PT J AU Guarcello, MG Drake, JJ Wright, NJ Garcia-Alvarez, D Kraemer, KE AF Guarcello, M. G. Drake, J. J. Wright, N. J. Garcia-Alvarez, D. Kraemer, K. E. TI ACCRETION AND OUTFLOW IN THE PROPLYD-LIKE OBJECTS NEAR CYGNUS OB2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; stars: mass-loss; stars: pre-main sequence; stars: protostars ID T-TAURI STARS; HUBBLE-SPACE-TELESCOPE; PHOTOEVAPORATING CIRCUMSTELLAR DISKS; FORBIDDEN-LINE EMISSION; YOUNG STELLAR OBJECTS; ORION NEBULA; MASSIVE STARS; MAGNETOSPHERIC ACCRETION; SPECTROSCOPIC EVIDENCE; ULTRAVIOLET-RADIATION AB Cygnus OB2 is the most massive association within 2 kpc from the Sun, hosting hundreds of massive stars, thousands of young low mass members, and some sights of active star formation in the surrounding cloud. Recently, 10 photoevaporating proplyd-like objects with tadpole-shaped morphology were discovered in the outskirts of the OB association, approximately 6-14 pc away from its center. The classification of these objects is ambiguous, being either evaporating residuals of the parental cloud that are hosting a protostar inside or disk-bearing stars with an evaporating disk, such as the evaporating proplyds observed in the Trapezium Cluster in Orion. In this paper, we present a study based on low-resolution optical spectroscopic observations made with the Optical System for Imaging and low Resolution Integrated Spectroscopy, mounted on the 10.4 m Gran Telescopio CANARIAS, of two of these protostars. The spectrum of one of the objects shows evidence of accretion but not of outflows. In the latter object, the spectra show several emission lines indicating the presence of an actively accreting disk with outflow. We present estimates of the mass loss rate and the accretion rate from the disk, showing that the former exceeds the latter as observed in other known objects with evaporating disks. We also show evidence of a strong variability in the integrated flux observed in these objects as well as in the accretion and outflow diagnostics. C1 [Guarcello, M. G.] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy. [Guarcello, M. G.; Drake, J. J.; Wright, N. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Wright, N. J.] Univ Hertfordshire, CAR STRI, Hatfield AL10 9AB, Herts, England. [Garcia-Alvarez, D.] Univ La Laguna, Dept Astrofis, D-38206 San Cristobal la Laguna, Tenerife, Spain. [Garcia-Alvarez, D.] Grantecan CALP, E-38712 Brena Baja, La Palma, Spain. [Garcia-Alvarez, D.] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Kraemer, K. E.] Boston Coll, Inst Sci Res, Newton, MA 02459 USA. RP Guarcello, MG (reprint author), INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy. OI Kraemer, Kathleen/0000-0002-2626-7155 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; Chandra [GO0-11040X]; NASA [NAS8-03060] FX We thank the anonymous referee who helped us to significantly improve the quality of this manuscript. This paper is based on observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma. This paper is also based on data from the IPHAS and SDSS Data Release 9. The IPHAS survey has been carried out at the INT. The INT is 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. 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. M.G.G. was supported by Chandra grant GO0-11040X during the course of this work. J.J.D. was funded by NASA contract NAS8-03060 to the Chandra X-ray Center and thanks the Director, Belinda Wilkes, for continuing support. M.G.G. also acknowledges grant PRIN-INAF 2012 (PI: E. Flaccomio). NR 99 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 SEP 20 PY 2014 VL 793 IS 1 AR 56 DI 10.1088/0004-637X/793/1/56 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700056 ER PT J AU Nun, I Pichara, K Protopapas, P Kim, DW AF Nun, Isadora Pichara, Karim Protopapas, Pavlos Kim, Dae-Won TI SUPERVISED DETECTION OF ANOMALOUS LIGHT CURVES IN MASSIVE ASTRONOMICAL CATALOGS SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; methods: data analysis; methods: statistical; stars: statistics; stars: variables: general ID LARGE-MAGELLANIC-CLOUD; VARIABLE-STAR INVENTORY; X-RAY BINARIES; MACHO PROJECT LMC; GRAVITATIONAL LENSING EXPERIMENT; LONG-PERIOD VARIABLES; RR LYRAE STARS; OUTLIER DETECTION; GALACTIC BULGE; MICROLENSING EVENTS AB The development of synoptic sky surveys has led to a massive amount of data for which resources needed for analysis are beyond human capabilities. In order to process this information and to extract all possible knowledge, machine learning techniques become necessary. Here we present a new methodology to automatically discover unknown variable objects in large astronomical catalogs. With the aim of taking full advantage of all information we have about known objects, our method is based on a supervised algorithm. In particular, we train a random forest classifier using known variability classes of objects and obtain votes for each of the objects in the training set. We then model this voting distribution with a Bayesian network and obtain the joint voting distribution among the training objects. Consequently, an unknown object is considered as an outlier insofar it has a low joint probability. By leaving out one of the classes on the training set, we perform a validity test and show that when the random forest classifier attempts to classify unknown light curves (the class left out), it votes with an unusual distribution among the classes. This rare voting is detected by the Bayesian network and expressed as a low joint probability. Our method is suitable for exploring massive data sets given that the training process is performed offline. We tested our algorithm on 20 million light curves from the MACHO catalog and generated a list of anomalous candidates. After analysis, we divided the candidates into two main classes of outliers: artifacts and intrinsic outliers. Artifacts were principally due to air mass variation, seasonal variation, bad calibration, or instrumental errors and were consequently removed from our outlier list and added to the training set. After retraining, we selected about 4000 objects, which we passed to a post-analysis stage by performing a cross-match with all publicly available catalogs. Within these candidates we identified certain known but rare objects such as eclipsing Cepheids, blue variables, cataclysmic variables, and X-ray sources. For some outliers there was no additional information. Among them we identified three unknown variability types and a few individual outliers that will be followed up in order to perform a deeper analysis. C1 [Nun, Isadora; Pichara, Karim] Pontificia Univ Catolica Chile, Dept Comp Sci, Santiago, Chile. [Pichara, Karim] Millennium Inst Astrophys, Santiago, Chile. [Protopapas, Pavlos] Harvard Univ, Inst Appl Computat Sci, Cambridge, MA USA. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kim, Dae-Won] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Nun, I (reprint author), Pontificia Univ Catolica Chile, Dept Comp Sci, Alameda 340, Santiago, Chile. FU Pontificia Universidad Catolica de Chile; Ministry of Economy, Development, and Tourism's Millennium Science Initiative [IC 12009] FX We thank M. Stockle and D. Acuna for helpful comments and advice. The analysis in this paper has been done using the Odyssey cluster offered by the FAS Research Computing Group at Harvard. This work is supported by Vicerrectoria de Investigacion (VRI) from Pontificia Universidad Catolica de Chile and by the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC 12009, awarded to The Millennium Institute of Astrophysics. NR 93 TC 8 Z9 8 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2014 VL 793 IS 1 AR 23 DI 10.1088/0004-637X/793/1/23 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700023 ER PT J AU Paul, S Sethi, SK Subrahmanyan, R Shankar, NU Dwarakanath, KS Deshpande, AA Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Emrich, D Gaensler, BM Goeke, RF Greenhill, LJ Hazelton, BJ Hewitt, JN Johnston-Hollitt, M Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, EH Oberoi, D Ord, SM Prabu, T Rogers, AEE Roshi, AA Srivani, KS Tingay, SJ Wayth, RB Waterson, M Webster, RL Whitney, AR Williams, AJ Williams, CL AF Paul, Sourabh Sethi, Shiv K. Subrahmanyan, Ravi Shankar, N. Udaya Dwarakanath, K. S. Deshpande, Avinash A. Bernardi, Gianni Bowman, Judd D. Briggs, Frank Cappallo, Roger J. Corey, Brian E. Emrich, David Gaensler, Bryan M. Goeke, Robert F. Greenhill, Lincoln J. Hazelton, Bryna J. Hewitt, Jacqueline N. Johnston-Hollitt, Melanie Kaplan, David L. Kasper, Justin C. Kratzenberg, Eric Lonsdale, Colin J. Lynch, Mervyn J. McWhirter, S. Russell Mitchell, Daniel A. Morales, Miguel F. Morgan, Edward H. Oberoi, Divya Ord, Stephen M. Prabu, Thiagaraj Rogers, Alan E. E. Roshi, Anish A. Srivani, K. S. Tingay, Steven J. Wayth, Randall B. Waterson, Mark Webster, Rachel L. Whitney, Alan R. Williams, Andrew J. Williams, Christopher L. TI STUDY OF REDSHIFTED H I FROM THE EPOCH OF REIONIZATION WITH DRIFT SCAN SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; cosmology: theory; dark ages, reionization, first stars; techniques: interferometric ID PROBE WMAP OBSERVATIONS; SENSITIVITY; OBSERVATORIES; FLUCTUATIONS; COSMOLOGY; ARRAY AB Detection of the epoch of reionization (EoR) in the redshifted 21 cm line is a challenging task. Here, we formulate the detection of the EoR signal using the drift scan strategy. This method potentially has better instrumental stability compared to the case where a single patch of sky is tracked. We demonstrate that the correlation time between measured visibilities could extend up to 1-2 hr for an interferometer array such as the Murchison Widefield Array, which has a wide primary beam. We estimate the EoR power based on a cross-correlation of visibilities over time and show that the drift scan strategy is capable of detecting the EoR signal with a signal to noise that is comparable/better compared to the tracking case. We also estimate the visibility correlation for a set of bright point sources and argue that the statistical inhomogeneity of bright point sources might allow their separation from the EoR signal. C1 [Paul, Sourabh; Sethi, Shiv K.; Subrahmanyan, Ravi; Shankar, N. Udaya; Dwarakanath, K. S.; Deshpande, Avinash A.; Prabu, Thiagaraj; Srivani, K. S.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Subrahmanyan, Ravi; Briggs, Frank; Gaensler, Bryan M.; Mitchell, Daniel A.; Ord, Stephen M.; Tingay, Steven J.; Wayth, Randall B.; Webster, Rachel L.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Bernardi, Gianni] Sq Kilometre Array South Africa SKA SA, ZA-7405 Pinelands, South Africa. [Bowman, Judd D.] Arizona State Univ, Tempe, AZ USA. [Briggs, Frank; Waterson, Mark] Australian Natl Univ, Canberra, ACT, Australia. [Cappallo, Roger J.; Corey, Brian E.; Goeke, Robert F.; Kratzenberg, Eric; Lonsdale, Colin J.; McWhirter, S. Russell; Rogers, Alan E. E.; Whitney, Alan R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Emrich, David; Lynch, Mervyn J.; Ord, Stephen M.; Tingay, Steven J.; Wayth, Randall B.; Waterson, Mark; Williams, Andrew J.] Curtin Univ, Perth, WA 6845, Australia. [Gaensler, Bryan M.] Univ Sydney, Sydney, NSW 2006, Australia. [Greenhill, Lincoln J.; Kasper, Justin C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hazelton, Bryna J.; Morales, Miguel F.] Univ Washington, Seattle, WA 98195 USA. [Hewitt, Jacqueline N.; Morgan, Edward H.; Williams, Christopher L.] Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Johnston-Hollitt, Melanie] Victoria Univ Wellington, Wellington 6140, New Zealand. [Kaplan, David L.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Mitchell, Daniel A.] CSIRO Astron & Space Sci, Clayton, Vic 3169, Australia. [Oberoi, Divya] Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Roshi, Anish A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Webster, Rachel L.] Univ Melbourne, Melbourne, Vic, Australia. RP Paul, S (reprint author), Raman Res Inst, Bangalore 560080, Karnataka, India. RI Deshpande, Avinash/D-4868-2012; Sethi, Shiv/D-4893-2012; Dwarakanath, K /D-4876-2012; Wayth, Randall/B-2444-2013; Kasper, Justin/D-1152-2010; Udayashankar , N/D-4901-2012; Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012 OI Gaensler, Bryan/0000-0002-3382-9558; Wayth, Randall/0000-0002-6995-4131; Kasper, Justin/0000-0002-7077-930X; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Emrich, David/0000-0002-4058-1837; 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 New Zealand Ministry of Economic Development [MED-E1799]; NVIDIA at Harvard University; International Centre for Radio Astronomy Research (ICRAR); Western Australian State government; Victoria University of Wellington via IBM Shared University Research Grant [MED-E1799]; Commonwealth Scientific and Industrial Research Organisation (CSIRO); National Collaborative Research Infrastructure Strategy, Education Investment Fund; Australia India Strategic Research Fund; Astronomy Australia Limited 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 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. NR 20 TC 3 Z9 3 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2014 VL 793 IS 1 AR 28 DI 10.1088/0004-637X/793/1/28 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700028 ER PT J AU Puccetti, S Comastri, A Fiore, F Arevalo, P Risaliti, G Bauer, FE Brandt, WN Stern, D Harrison, FA Alexander, DM Boggs, SE Christensen, FE Craig, WW Gandhi, P Hailey, CJ Koss, MJ Lansbury, GB Luo, B Madejski, GM Matt, G Walton, DJ Zhang, W AF Puccetti, Simonetta Comastri, Andrea Fiore, Fabrizio Arevalo, Patricia Risaliti, Guido Bauer, Franz E. Brandt, William N. Stern, Daniel Harrison, Fiona A. Alexander, David M. Boggs, Steve E. Christensen, Finn E. Craig, William W. Gandhi, Poshak Hailey, Charles J. Koss, Michael J. Lansbury, George B. Luo, Bin Madejski, Greg M. Matt, Giorgio Walton, Dominic J. Zhang, Will TI THE VARIABLE HARD X-RAY EMISSION OF NGC 4945 AS OBSERVED BY NUSTAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 4945); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC DISTANCE DATABASE; XMM-NEWTON; GALAXY NGC-4945; EDDINGTON RATIO; SPECTRUM; CHANDRA; SPECTROSCOPY; LINE; AGN AB We present a broadband (similar to 0.5-79 keV) spectral and temporal analysis of multiple NuSTAR observations combined with archival Suzaku and Chandra data of NGC 4945, the brightest extragalactic source at 100 keV. We observe hard X-ray (>10 keV) flux and spectral variability, with flux variations of a factor of two on timescales of 20 ks. A variable primary continuum dominates the high-energy spectrum (>10 keV) in all states, while the reflected/scattered flux that dominates at E < 10 keV stays approximately constant. From modeling the complex reflection/transmission spectrum, we derive a Compton depth along the line of sight of tau(Thomson) similar to 2.9, and a global covering factor for the circumnuclear gas of similar to 0.15. This agrees with the constraints derived from the high-energy variability, which implies that most of the high-energy flux is transmitted rather than Compton-scattered. This demonstrates the effectiveness of spectral analysis at constraining the geometric properties of the circumnuclear gas, and validates similar methods used for analyzing the spectra of other bright, Compton-thick active galactic nuclei (AGNs). The lower limits on the e-folding energy are between 200 and 300 keV, consistent with previous BeppoSAX, Suzaku, and Swift Burst Alert Telescope observations. The accretion rate, estimated from the X-ray luminosity and assuming a bolometric correction typical of type 2 AGN, is in the range similar to 0.1-0.3 lambda(Edd) depending on the flux state. The substantial observed X-ray luminosity variability of NGC 4945 implies that large errors can arise from using single-epoch X-ray data to derive L/L-Edd values for obscured AGNs. C1 [Puccetti, Simonetta] ASDC ASI, I-00133 Rome, Italy. [Puccetti, Simonetta; Fiore, Fabrizio] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Comastri, Andrea] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Arevalo, Patricia; Bauer, Franz E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Chile. [Risaliti, Guido] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, Guido] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bauer, Franz E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, William N.; Luo, Bin] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, William N.; Luo, Bin] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Harrison, Fiona A.; Walton, Dominic J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Alexander, David M.; Gandhi, Poshak; Lansbury, George B.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Boggs, Steve E.; Craig, William W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark. [Craig, William W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Hailey, Charles J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Koss, Michael J.] ETH, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [Madejski, Greg M.] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Matt, Giorgio] Univ Roma Tre, Dipartimento Matemat Fis, I-00146 Rome, Italy. [Zhang, Will] NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Puccetti, S (reprint author), ASDC ASI, Via Politecnico, I-00133 Rome, Italy. RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt, William/N-2844-2015; XRAY, SUZAKU/A-1808-2009; Comastri, Andrea/O-9543-2015; OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X; Puccetti, Simonetta/0000-0002-2734-7835; Fiore, Fabrizio/0000-0002-4031-4157 FU NASA [NNG08FD60C, GO3-14109X]; National Aeronautics and Space Administration; ASI/INAF [I/037/12/0-011/13]; STFC [ST/J003697/1, ST/K501979/1, ST/I001573/1]; Leverhulme Trust; Fondecyt [11100449]; Anillo [ACT1101]; Swiss National Science Foundation [PP00P2_138979/1]; California Institute of Technology NuSTAR [44A-1092750]; NASA ADP [NNX10AC99G]; Basal-CATA [PFB-06/2007]; CONICYT-Chile [ACT1101, FONDECYT 1101024]; "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009] FX This work was supported under NASA Contract 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). S.P., A.C., F.F., and G.M. acknowledge support from the ASI/INAF grant I/037/12/0-011/13. A.C. acknowledges the Caltech Kingsley visitor program. P.G. acknowledges support from STFC (grant reference ST/J003697/1). G.B.L. acknowledges support from STFC (grant reference ST/K501979/1). D.M.A. acknowledges support from STFC (grant reference ST/I001573/1) and from the Leverhulme Trust. P.A. acknowledges financial support from Fondecyt grant 11100449 and Anillo ACT1101. G.R. acknowledges financial support from grant NASA GO3-14109X. M.K. gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2_138979/1. W.N.B. and B.L. acknowledge support from California Institute of Technology NuSTAR subcontract 44A-1092750 and NASA ADP Grant NNX10AC99G. F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (grants FONDECYT 1101024 and "EMBIGGEN" Anillo ACT1101), and Project IC120009 "Millennium Institute of Astrophysics (MAS)" of Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. S.P. is grateful to Tahir Yaqoob for useful discussions on the MYTORUS model. NR 59 TC 21 Z9 21 U1 1 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 SEP 20 PY 2014 VL 793 IS 1 AR 26 DI 10.1088/0004-637X/793/1/26 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700026 ER PT J AU Sargent, MT Daddi, E Bethermin, M Aussel, H Magdis, G Hwang, HS Juneau, S Elbaz, D da Cunha, E AF Sargent, M. T. Daddi, E. Bethermin, M. Aussel, H. Magdis, G. Hwang, H. S. Juneau, S. Elbaz, D. da Cunha, E. TI REGULARITY UNDERLYING COMPLEXITY: A REDSHIFT-INDEPENDENT DESCRIPTION OF THE CONTINUOUS VARIATION OF GALAXY-SCALE MOLECULAR GAS PROPERTIES IN THE MASS-STAR FORMATION RATE PLANE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: evolution; galaxies: ISM; galaxies: spiral; surveys ID ULTRALUMINOUS INFRARED GALAXIES; LYMAN BREAK GALAXIES; CO-TO-H-2 CONVERSION FACTOR; ACTIVE GALACTIC NUCLEI; SIMILAR-TO 2; SPECTRAL ENERGY-DISTRIBUTIONS; FORMING DISK GALAXIES; M-ASTERISK PLANE; GREATER-THAN 2; STELLAR-MASS AB Star-forming galaxies (SFGs) display a continuous specific star formation rate (sSFR) distribution, which can be approximated by two log-normal functions: one encompassing the galaxy main sequence (MS), and the other a rarer, starbursting population. Starburst (SB) sSFRs can be regarded as the outcome of a physical process (plausibly merging) taking the mathematical form of a log-normal boosting kernel that enhances star formation activity. We explore the utility of splitting the star-forming population into MS and SB galaxies-an approach we term the "2-Star Formation Mode" framework-for understanding their molecular gas properties. Star formation efficiency (SFE) and gas fraction variations among SFGs take a simple redshift-independent form, once these quantities are normalized to the corresponding values for average MS galaxies. SFE enhancements during SB episodes scale supra-linearly with the SFR increase, as expected for mergers. Consequently, galaxies separate more clearly into loci for SBs and normal galaxies in the Schmidt-Kennicutt plane than in (s) SFR versus M-star space. SBs with large deviations (> 10 fold) from the MS, e.g., local ULIRGs, are not average SBs, but are much rarer events whose progenitors had larger gas fractions than typical MS galaxies. Statistically, gas fractions in SBs are reduced two-to threefold compared to their direct MS progenitors, as expected for short-lived SFR boosts where internal gas reservoirs are depleted more quickly than gas is re-accreted from the cosmic web. We predict variations of the conversion factor alpha(CO) in the SFR-M-star plane and we show that the higher sSFR of distant galaxies is directly related to their larger gas fractions. C1 [Sargent, M. T.; Daddi, E.; Bethermin, M.; Aussel, H.; Juneau, S.; Elbaz, D.] CEA Saclay, DSM, Irfu, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Sargent, M. T.] Univ Sussex, Ctr Astron, Dept Phys & Astron, Brighton BN1 9QH, E Sussex, England. [Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [da Cunha, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Sargent, MT (reprint author), CEA Saclay, DSM, Irfu, Serv Astrophys, F-91191 Gif Sur Yvette, France. EM mark.sargent@cea.fr RI Magdis, Georgios/C-7295-2014; Daddi, Emanuele/D-1649-2012; OI Magdis, Georgios/0000-0002-4872-2294; Daddi, Emanuele/0000-0002-3331-9590; Bethermin, Matthieu/0000-0002-3915-2015; da Cunha, Elisabete/0000-0001-9759-4797 FU EC [ERC-StG/UPGAL 240039, ANR-08-JCJC-0008]; ERC-grant [ERC-StG-257720] FX M.T.S., M.B., and E.D. acknowledge financial support from the EC through ERC-StG/UPGAL 240039 and grant ANR-08-JCJC-0008. S.J. was supported by ERC-grant ERC-StG-257720. NR 226 TC 43 Z9 43 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 SEP 20 PY 2014 VL 793 IS 1 AR 19 DI 10.1088/0004-637X/793/1/19 PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700019 ER PT J AU Wu, J Bussmann, RS Tsai, CW Petric, A Blain, A Eisenhardt, PRM Bridge, CR Benford, DJ Stern, D Assef, RJ Gelino, CR Moustakas, L Wright, EL AF Wu, Jingwen Bussmann, R. Shane Tsai, Chao-Wei Petric, Andreea Blain, Andrew Eisenhardt, Peter R. M. Bridge, Carrie R. Benford, Dominic J. Stern, Daniel Assef, Roberto J. Gelino, Christopher R. Moustakas, Leonidas Wright, Edward L. TI INTERFEROMETRIC FOLLOW-UP OF WISE HYPER-LUMINOUS HOT, DUST-OBSCURED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: high-redshift; galaxies: individual (WISE J014946.17+235014.5,WISE J181417.29+341224.9,WISE J223810.20+265319.7); galaxies: ISM; galaxies: starburst; infrared: galaxies ID SIMILAR-TO 2; SPACE-TELESCOPE MORPHOLOGIES; ADAPTIVE OPTICS SYSTEM; HIGH-REDSHIFT GALAXIES; STAR-FORMING GALAXIES; QUASAR HOST GALAXIES; SUBMILLIMETER GALAXIES; MOLECULAR GAS; CO EMISSION; INFRARED LUMINOSITIES AB The Wide-field Infrared Survey Explorer (WISE) has discovered an extraordinary population of hyper-luminous dusty galaxies that are faint in the two bluer passbands (3.4 mu m and 4.6 mu m) but are bright in the two redder passbands of WISE (12 mu m and 22 mu m). We report on initial follow-up observations of three of these hot, dust-obscured galaxies, or Hot DOGs, using the Combined Array for Research in Millimeter-wave Astronomy and the Submillimeter Array interferometer arrays at submillimeter/millimeter wavelengths. We report continuum detections at similar to 1.3 mm of two sources (WISE J014946.17+235014.5 and WISE J223810.20+265319.7, hereafter W0149+2350 and W2238+2653, respectively), and upper limits to CO line emission at 3 mm in the observed frame for two sources (W0149+2350 and WISE J181417.29+341224.8, hereafter W1814+3412). The 1.3 mm continuum images have a resolution of 1 ''-2 '' and are consistent with single point sources. We estimate the masses of cold dust are 2.0 x 10(8) M-circle dot for W0149+2350 and 3.9 x 10(8) M-circle dot for W2238+2653, comparable to cold dust masses of luminous quasars. We obtain 2 sigma upper limits to the molecular gas masses traced by CO, which are 3.3 x 1010 M-circle dot and 2.3 x 10(10) M-circle dot for W0149+2350 and W1814+3412, respectively. We also present high-resolution, near-IR imaging with the WFC3 on the Hubble Space Telescope for W0149+2653 and with NIRC2 on Keck for W2238+2653. The near-IR images show morphological structure dominated by a single, centrally condensed source with effective radius less than 4 kpc. No signs of gravitational lensing are evident. C1 [Wu, Jingwen; Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Bussmann, R. Shane] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bussmann, R. Shane] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Tsai, Chao-Wei; Moustakas, Leonidas] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Petric, Andreea] Astron Inst, Honolulu, HI 96822 USA. [Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bridge, Carrie R.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Benford, Dominic J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Assef, Roberto J.] Univ Diego Portales, Fac Ingn, Santiago, Chile. [Gelino, Christopher R.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. RP Wu, J (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM jingwen@astro.ucla.edu RI Benford, Dominic/D-4760-2012; OI Benford, Dominic/0000-0002-9884-4206; Moustakas, Leonidas/0000-0003-3030-2360 FU National Aeronautics and Space Administration; National Science Foundation; CARMA partner universities; NASA [NAS 5-26555]; W.M. Keck Foundation [AST 90-15755]; Gemini-CONICYT [32120009] FX This publication makes use of data products from the Widef-ield Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work is based on observations made with the Combined Array for Research in Millimeter-wave Astronomy (CARMA). Support for CARMA construction was derived from the states of California, Illinois, 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. This work is also based on observations made with the Submillimeter Array (SMA). 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. Some of the data are 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. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California and NASA. The Keck Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work uses data from Herschel. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work uses data from CSO, which is operated by the California Institute of Technology under funding from the National Science Foundation, contract AST 90-15755. R.J.A. was supported by Gemini-CONICYT grant number 32120009. NR 81 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 SEP 20 PY 2014 VL 793 IS 1 AR 8 DI 10.1088/0004-637X/793/1/8 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4IW UT WOS:000341301700008 ER PT J AU Sand, DJ Crnojevic, D Strader, J Toloba, E Simon, JD Caldwell, N Guhathakurta, P McLeod, B Seth, AC AF Sand, D. J. Crnojevic, D. Strader, J. Toloba, E. Simon, J. D. Caldwell, N. Guhathakurta, P. McLeod, B. Seth, A. C. TI DISCOVERY OF A NEW FAINT DWARF GALAXY ASSOCIATED WITH NGC 253 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dark matter; galaxies: dwarf ID MILKY-WAY SATELLITES; LARGE-SCALE STRUCTURE; RED GIANT BRANCH; LOCAL GROUP; SKY SURVEY; M81 GROUP; UNIVERSE; CALIBRATION; PHOTOMETRY; COSMOLOGY AB We report the discovery of a new faint dwarf galaxy, which we dub Scl-MM-Dw1, at a projected distance of similar to 65 kpc from the spiral galaxy NGC 253. The discovery results from the Panoramic Imaging Survey of Centaurus and Sculptor (PISCeS), a program with the Magellan/Megacam imager to study faint substructure in resolved stellar light around massive galaxies outside of the Local Group. We measure a tip of the red giant branch distance to Scl-MM-Dw1 of D = 3.9 +/- 0.5 Mpc, consistent with that of NGC 253, making their association likely. The new dwarf's stellar population is complex, with an old, metal-poor red giant branch (greater than or similar to 10 Gyr, [Fe/H] similar to -2), and an asymptotic giant branch with an age of similar to 500 Myr. Scl-MM-Dw1 has a half-light radius of r(h) = 340 +/- 50 pc and an absolute magnitude of M-V = -10.3 +/- 0.6 mag, comparable to the Milky Way's satellites at the same luminosity. Once complete, our imaging survey of NGC 253 and other nearby massive galaxies will provide a census of faint substructure in halos beyond the Local Group, both to put our own environment into context and to confront models of hierarchical structure formation. C1 [Sand, D. J.; Crnojevic, D.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Strader, J.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Toloba, E.; Guhathakurta, P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Toloba, E.; Simon, J. D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Caldwell, N.; McLeod, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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 OI Seth, Anil/0000-0003-0248-5470; Guhathakurta, Puragra/0000-0001-8867-4234; McLeod, Brian/0000-0002-2924-2893 FU Aspen Center for Physics (NSF) [1066293]; NSF [AST-1010039]; Fulbright Program; Spanish Ministry of Education FX We thank K. Hamren for observing help and M. Conroy, J. Roll, S. Moran for their tireless efforts. D. J. S. thanks Aspen Center for Physics (NSF Grant #1066293) for their hospitality during paper writing. P. G. acknowledges NSF grant AST-1010039. E. T. is a Fulbright postdoctoral fellow supported by the Fulbright Program and the Spanish Ministry of Education. NR 36 TC 13 Z9 13 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 SEP 20 PY 2014 VL 793 IS 1 AR L7 DI 10.1088/2041-8205/793/1/L7 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4MP UT WOS:000341313700007 ER PT J AU Seth, AC van den Bosch, R Mieske, S Baumgardt, H den Brok, M Strader, J Neumayer, N Chilingarian, I Hilker, M McDermid, R Spitler, L Brodie, J Frank, MJ Walsh, JL AF Seth, Anil C. van den Bosch, Remco Mieske, Steffen Baumgardt, Holger den Brok, Mark Strader, Jay Neumayer, Nadine Chilingarian, Igor Hilker, Michael McDermid, Richard Spitler, Lee Brodie, Jean Frank, Matthias J. Walsh, Jonelle L. TI A supermassive black hole in an ultra-compact dwarf galaxy SO NATURE LA English DT Article ID INITIAL MASS FUNCTION; MULTI-GAUSSIAN EXPANSION; GLOBULAR-CLUSTER G1; ACS FORNAX CLUSTER; STAR-CLUSTERS; STELLAR-SYSTEMS; HOST GALAXIES; ACCRETION; SPECTRA; MODELS AB Ultra-compact dwarf galaxies are among the densest stellar systems in the Universe. These systems have masses of up to 2 x 10(8) solar masses, but half-light radii of just 3-50 parsecs(1). Dynamicalmass estimates show that many such dwarfs are more massive than expected from their luminosity(2). It remains unclear whether these high dynamical mass estimates arise because of the presence of supermassive black holes or result from a non-standard stellar initial mass function that causes the average stellar mass to be higher than expected(3,4). Here we report adaptive optics kinematic data of the ultra-compact dwarf galaxy M60-UCD1 that show a central velocity dispersion peak exceeding 100 kilometres per second and modest rotation. Dynamical modelling of these data reveals the presence of a supermassive black hole with amass of 2.1 x 10(7) solarmasses. This is 15 per cent of the object's total mass. The high black hole mass and mass fraction suggest that M60-UCD1 is the stripped nucleus of a galaxy. Our analysis also shows that M60-UCD1's stellar mass is consistent with its luminosity, implying a large population of previously unrecognized supermassive black holes in other ultra-compact dwarf galaxies(2). C1 [Seth, Anil C.; den Brok, Mark] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [van den Bosch, Remco; Neumayer, Nadine] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Mieske, Steffen] European So Observ, Santiago 7630355, Chile. [Baumgardt, Holger] Univ Queensland, Sch Math & Phys, St Lucia, Qld 4072, Australia. [Strader, Jay] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Neumayer, Nadine; Hilker, Michael] European So Observ, D-85748 Garching, Germany. [Chilingarian, Igor] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chilingarian, Igor] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [McDermid, Richard; Spitler, Lee] Australian Astron Observ, Sydney, NSW 2113, Australia. [McDermid, Richard; Spitler, Lee] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Brodie, Jean] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Brodie, Jean] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Frank, Matthias J.] Heidelberg Univ, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. [Walsh, Jonelle L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Seth, AC (reprint author), Univ Utah, Dept Phys & Astron, 115 South 1400 East, Salt Lake City, UT 84112 USA. EM aseth@astro.utah.edu RI Chilingarian, Igor/N-5117-2016; Baumgardt, Holger/A-5444-2012; OI Chilingarian, Igor/0000-0002-7924-3253; Neumayer, Nadine/0000-0002-6922-2598; van den Bosch, Remco/0000-0002-0420-6159 FU NSF [AST-1350389, 1102845, AST-1109878]; German Research Foundation [Ko4161/1]; Russian Science Foundation [14-22-00041] FX This work was based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy 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). Work on this paper by A.C.S. was supported by NSF CAREER grant AST-1350389. J.L.W. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award number 1102845. J.B. is supported by NSF grant AST-1109878. M.J.F. is supported by German Research Foundation grant Ko4161/1. I.C. acknowledges support from the Russian Science Foundation grant 14-22-00041. NR 50 TC 69 Z9 69 U1 0 U2 10 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 SEP 18 PY 2014 VL 513 IS 7518 BP 398 EP + DI 10.1038/nature13762 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AP1GD UT WOS:000341814900055 PM 25230660 ER PT J AU Hong, T AF Hong, Terry TI A Map of Betrayal SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20560 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 15 PY 2014 VL 139 IS 15 BP 66 EP 67 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA AO4ZT UT WOS:000341350600106 ER PT J AU McClelland, HLO Taylor, PD O'Dea, A Okamura, B AF McClelland, H. L. O. Taylor, P. D. O'Dea, A. Okamura, B. TI Revising and refining the bryozoan zs-MART seasonality proxy SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Mean annual range of temperature (MART); Palaeoseasonality; Temperature size rule; Zooid variability; Acanthodesia ID TEMPERATURE-SIZE RULE; ZOOID SIZE; CUPULADRIA-EXFRAGMINIS; CHEILOSTOME BRYOZOANS; EOCENE SEASONALITY; ECTOTHERMS; GROWTH; ISOTOPES; COLONIES; ATLANTIC AB The zs-MART (zooid-size derived mean annual range of temperature) seasonality proxy is based on temperature-related variation in the sizes of zooids found in colonies of cheilostome bryozoans. It has been used in a number of studies for inferring palaeoseasonality. Here we present a revised version of the equation for the zs-MART proxy based on an appropriate regression analysis and an estimate of the error associated with predicted values. We use this improved version to recalculate data used in studies that have employed the zs-MART proxy and evaluate their conclusions in light of the revised estimates for seasonal regimes. In order to investigate trans-colony zooid-size profiles in zooid size, length and width, 1195 zooids from 40 transects through 19 fossil and Recent specimens of the malacostegine cheilostome bryozoan Acanthodesia were measured using a stereomicroscope with eyepiece graticule. The position of zooids within bifurcating rows of Acanthodesia colonies is found to influence zooid size, and this exemplifies potential problems for studies based on zooid-size transects and random sampling of zooids. Our demonstration that oscillatory signals in zooid size, possibly attributable to seasonal temperature regimes, can be detected whilst accounting for other sources of variation confirms that a more sophisticated zs-MART proxy may prove useful for constraining parameters in ocean models addressing questions about past climate. However, such a proxy will require more parameters than originally described along with larger raw datasets. Crown Copyright (C) 2014 Published by Elsevier B.V. All rights reserved. C1 [McClelland, H. L. O.; Okamura, B.] Nat Hist Museum, Dept Life Sci, London SW7 5BD, England. [McClelland, H. L. O.; Taylor, P. D.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [O'Dea, A.] Smithsonian Trop Res Inst, Balboa, Panama. [McClelland, H. L. O.] Univ Oxford, Dept Earth Sci, Oxford OX1 3AN, England. RP McClelland, HLO (reprint author), Univ Oxford, Dept Earth Sci, S Parks Rd, Oxford OX1 3AN, England. EM hanym@earth.ox.ac.uk FU NERC; Natural History Museum, London; Imperial College, London; National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation (SENACYT) of Panama FX The work here was conducted as an MSc project supervised by BO and PDT. We thank the NERC, the Natural History Museum, London and Imperial College, London for funding. AO was supported by the National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation (SENACYT) of Panama. We thank Roger Benson, Laura Soul and Steve Hageman for their comments that have improved our manuscript. NR 45 TC 1 Z9 1 U1 0 U2 6 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 15 PY 2014 VL 410 BP 412 EP 420 DI 10.1016/j.palaeo.2014.06.011 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA AN6EM UT WOS:000340687700032 ER PT J AU Mejia, LC Herre, EA Sparks, JP Winter, K Garcia, MN Van Bael, SA Stitt, J Zhang, Y Zhang, YF Guiltinan, MJ Maximova, SN AF Mejia, Luis C. Herre, Edward A. Sparks, Jed P. Winter, Klaus Garcia, Milton N. Van Bael, Sunshine A. Stitt, Joseph Shi, Zi Zhang, Yufan Guiltinan, Mark J. Maximova, Siela N. TI Pervasive effects of a dominant foliar endophytic fungus on host genetic and phenotypic expression in a tropical tree SO FRONTIERS IN MICROBIOLOGY LA English DT Article DE symbiosis; fungal endophytes; Theobroma; Colletotrichum; gene expression; plant defense; Arabidopsis; Populus ID THEOBROMA-CACAO L.; LEAF-CUTTING ANTS; DEFENSE RESPONSE; COLLETOTRICHUM-GLOEOSPORIOIDES; FUNCTIONAL ANNOTATION; PATHOGEN INTERACTIONS; PLANT-PATHOGEN; DIVERSITY; ARABIDOPSIS; RESISTANCE AB It is increasingly recognized that macro-organisms (corals, insects, plants, vertebrates) consist of both host tissues and multiple microbial symbionts that play essential roles in their host's ecological and evolutionary success. Consequently, identifying benefits and costs of symbioses, as well as mechanisms underlying them are research priorities. All plants surveyed under natural conditions harbor foliar endophytic fungi (FEE) in their leaf tissues, often at high densities. Despite producing no visible effects on their hosts, experiments have nonetheless shown that FEE reduce pathogen and herbivore damage. Here, combining results from three genomic, and two physiological experiments, we demonstrate pervasive genetic and phenotypic effects of the apparently asymptomatic endophytes on their hosts. Specifically, inoculation of endophyte-free (E) Theobroma cacao leaves with Colletotrichum tropicale (E+), the dominant FEE species in healthy T cacao, induces consistent changes in the expression of hundreds of host genes, including many with known defensive functions. Further, E+ plants exhibited increased lignin and cellulose content, reduced maximum rates of photosynthesis (A(max)), and enrichment of nitrogen-15 and carbon-13 isotopes. These phenotypic changes observed in E+ plants correspond to changes in expression of specific functional genes in related pathways. Moreover, a cacao gene (Tc00g04254) highly up-regulated by C. tropicale also confers resistance to pathogen damage in the absence of endophytes or their products in host tissues. Thus, the benefits of increased pathogen resistance in E+ plants are derived in part from up-regulation of intrinsic host defense responses, and appear to be offset by potential costs including reduced photosynthesis, altered host nitrogen metabolism, and endophyte heterotrophy of host tissues. Similar effects are likely in most plant-endophyte interactions, and should be recognized in the design and interpretation of genetic and phenotypic studies of plants. C1 [Mejia, Luis C.; Herre, Edward A.; Winter, Klaus; Garcia, Milton N.; Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Unit 9100, Miami, FL 34002 USA. [Mejia, Luis C.; Shi, Zi; Zhang, Yufan; Guiltinan, Mark J.; Maximova, Siela N.] Penn State Univ, Dept Plant Sci, University Pk, PA USA. [Mejia, Luis C.; Shi, Zi; Zhang, Yufan; Guiltinan, Mark J.; Maximova, Siela N.] Penn State Univ, Huck Inst Life Sci, University Pk, PA 16802 USA. [Sparks, Jed P.] Cornell Univ, Dept Ecol & Evolut, Ithaca, NY USA. [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Stitt, Joseph] Mat Res Inst, Social Life & Engn Sci Imaging Ctr, University Pk, PA USA. RP Herre, EA (reprint author), Smithsonian Trop Res Inst, Unit 9100, Box 0948,DPO AA, Miami, FL 34002 USA. EM herrea@si.edu; snm104@psu.edu FU Smithsonian Tropical Research Institute; STRI Tupper Postdoctoral Fellowship; Mellon Foundation; American Cocoa Research Institute Endowed Program in the Molecular Biology of Cocoa at The Pennsylvania State University; Clapperton Award from Mars, UK; Mars, UK FX This study was supported by the Smithsonian Tropical Research Institute, the STRI Tupper Postdoctoral Fellowship, Kari Wenger, Bill Robertson and the Mellon Foundation, the American Cocoa Research Institute Endowed Program in the Molecular Biology of Cocoa at The Pennsylvania State University, and the Clapperton Award from Mars, UK. We thank Mars, UK for their generous sponsorship of the oligo synthesis for the T cacao 3k microarray. We thank Siti Zulkafli, Sharon Pishak, Ann Young, Craig Praul, Deborah Grove, and the staff at the Genomics Core Facility, PSU. We thank Orlando Lozada for providing seeds, Damond Kyllo, Luis Ramirez, Terri Shirshac, Enith Rojas, and Carlos Aguilar for assistance growing the plants, culturing and inoculating the fungi, and conducting the physiological experiments. Merlin Sheldrake, Ron Herzig, Betsy Arnold, Nancy Knowlton, Daniel Wilson, Emma Sayer, Suzanne Ford, Truman Young, Richard Stone, Jan Sapp, Martin Heil and two anonymous reviewers provided useful discussion and/or comments on the manuscript. NR 69 TC 10 Z9 10 U1 7 U2 63 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1664-302X J9 FRONT MICROBIOL JI Front. Microbiol. PD SEP 12 PY 2014 VL 5 AR 479 DI 10.3389/fmicb.2014.00479 PG 16 WC Microbiology SC Microbiology GA AP2RX UT WOS:000341923200001 PM 25309519 ER PT J AU Gama, WA Laughinghouse, HD Anna, CL AF Gama, Watson Arantes, Jr. Laughinghouse, Haywood Dail St Anna, Celia Leite TI How diverse are coccoid cyanobacteria? A case study of terrestrial habitats from the Atlantic Rainforest (Sao Paulo, Brazil) SO PHYTOTAXA LA English DT Article DE Brazilian forest; Chroococcales; cyanobacterial biodiversity; combinatio nova; status novus ID MATA ATLANTICA; STATE; CYANOPROKARYOTES; CHROOCOCCALES; ENTOPHYSALIDACEAE; SCYTONEMATACEAE; CYANOPHYCEAE; BRASILONEMA; BIOFILMS AB The present study analyzed 267 samples of terrestrial habitats from different fragmented areas of the Atlantic Rainforest located in Sao Paulo State (southeastern Brazil), finding 61 taxa of coccoid cyanobacteria, 21 of which we were only capable of identifying at the generic level. The samples were examined using light microscopy and populations were morphometrically separated and taxonomically identified. Among the identified taxa, we propose the elevation of Chroococcus turgidus var. subviolaceus to Chroococcus subviolaceus comb. et stat. nov. Due to the high species richness found, we assume that the Atlantic Rainforest is a 'hotspot' of coccoid cyanobacterial diversity and should be better studied, in addition to other tropical ecosystems and terrestrial habitats, which have been shown to be suitable places for cyanobacterial diversity establishment. C1 [Gama, Watson Arantes, Jr.; St Anna, Celia Leite] Nucleo Pesquisa Ficol, Inst Bot, BR-1031970 Sao Paulo, Brazil. [Laughinghouse, Haywood Dail] Smith Coll, Dept Biol Sci, Northampton, MA 01063 USA. [Laughinghouse, Haywood Dail] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Gama, WA (reprint author), Nucleo Pesquisa Ficol, Inst Bot, CP 3005, BR-1031970 Sao Paulo, Brazil. EM watsonarantes@gmail.com RI Laughinghouse, Haywood/M-5836-2016 OI Laughinghouse, Haywood/0000-0003-1018-6948 FU CNPq [562213/2010-4]; FAPESP fellowship [2012/16430-1] FX Research support was provided by CNPq (process number 562213/2010-4) and WAG Jr had a FAPESP fellowship (process number 2012/16430-1). We are grateful to RM Fischer for revising the English text, to Phytotaxa Editor, Dr. Saul Blanco Lanza, and to anonymous reviewers for the valuable contributions to this manuscript. NR 102 TC 4 Z9 5 U1 1 U2 11 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 EI 1179-3163 J9 PHYTOTAXA JI Phytotaxa PD SEP 12 PY 2014 VL 178 IS 2 BP 61 EP 97 PG 37 WC Plant Sciences SC Plant Sciences GA AP0LC UT WOS:000341751900001 ER PT J AU Glowska, E Schmidt, BK AF Glowska, Eliza Schmidt, Brian K. TI New taxa of the subfamily Picobiinae (Cheyletoidea: Syringophilidae) parasitizing antbirds and gnateaters (Passeriformes: Thamnophilidae, Conopophagidae) in Guyana SO ZOOTAXA LA English DT Article DE Quill mites; Syringophilidae; Phipicobia; Rafapicobia; antbirds; gnateaters; systematics ID MITES; BIRDS AB A new genus and three new species of the picobiin quill mites (Cheyletoidea: Syringophilidae) are described from passeriform birds in Guyana, Phipicobia pygiptilae gen. nov. and sp. nov. parasitizing Pygiptila stellaris (Spix) (Thamnophilidae), Rafapicobia thamnophili sp. nov. from Thamnophilus insignis Salvin et Godman (type host), Myrmoborus leucophrys (Tschudi), Myrmeciza ferruginea (St. Muller), Myrmotherula longipennis Pelzeln, and Hypocnemis cantator (Boddaert) (Thamnophilidae), and Rafapicobia milenskyi sp. nov. from Conopophaga aurita (Gmelin) (Conopophagidae). C1 [Glowska, Eliza] Adam Mickiewicz Univ, Dept Anim Morphol, Fac Biol, PL-61614 Poznan, Poland. [Schmidt, Brian K.] 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 11 TC 4 Z9 4 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 SEP 12 PY 2014 VL 3861 IS 2 BP 193 EP 200 PG 8 WC Zoology SC Zoology GA AO8SL UT WOS:000341624400007 PM 25283403 ER PT J AU Suarez, W Olson, SL AF Suarez, William Olson, Storrs L. TI A new fossil species of small crested caracara (Aves: Falconidae: Caracara) from the Pacific lowlands of western South America SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Caracara seymouri; Ecuador; extinction; fossil birds; La Carolina; Peru; Pleistocene; Talara Tar Seeps ID CUBA AVES; QUATERNARY; DEPOSITS AB A new species of small crested caracara, Caracara seymouri, from Quaternary asphalt deposits of the Talara Tar Seeps, northwestern Peru, is described from most major elements of the skeleton. specimen reported in the literature from late Pleistocene deposits at La Carolina, Ecuador, are referred to the same species. These fossils had previously been identified as Polyborus (now Caracara) plancus, but they possess a combination of characters not present in the living species of caracaras, C. plancus or C. cheriway and are from a much smaller and more gracile bird. Caracara seymouri is similar in size to the extinct species C. creightoni from the Bahamas and Cuba but differs in having the skeletal elements less robust, especially the premaxilla. This is the second paleospecies described for the genus Caracara in the Quaternary of South America. C1 [Olson, Storrs L.] Natl Museum Nat Hist, Smithsonian Inst, Div Birds, Washington, DC 20013 USA. RP Suarez, W (reprint author), POB 16477, W Palm Beach, FL 33165 USA. EM wsbirding@birdlover.com NR 26 TC 2 Z9 2 U1 0 U2 2 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 SEP 11 PY 2014 VL 127 IS 2 BP 299 EP 310 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AQ5UY UT WOS:000342875300001 ER PT J AU Tyler, JC Johnson, GD Jawad, L Brothers, EB AF Tyler, James C. Johnson, G. David Jawad, Laith Brothers, Edward B. TI A developmentally "tail-less" adult cowfish, Lactoria cornuta, from Oman (Ostraciidae, Tetraodontiformes) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE abnormality; caudal fin; caudal peduncle; cowfish; development; Lactoria ID FISHES ACANTHOMORPHA; OCEAN SUNFISHES; PHYLOGENY; TELEOSTEI; MOLIDAE; FINS AB A 145 mm SL specimen of the ostraciid Longhorn Cowfish, Lactoria cornuta (Linnaeus, 1758), collected along the coast of Oman, has only small rudiments of the caudal fin and a much shortened caudal peduncle in which the posteriormost vertebrae are either abnormally developed or fused. The otoliths are too deteriorated to allow aging, but the gonads are mature, and we presume that an adult specimen of this size is several years old. Remarkably, this "tail-less" specimen survived without a functional caudal peduncle and caudal fin, even though the long caudal fin in ostraciid fishes is the main source of the rapid propulsion required for predator avoidance. The anatomical peculiarities of the rudimentary termination of the vertebral column and caudal fin are described and illustrated. We also comment on the potential evolutionary implications of such abnormalities. C1 [Tyler, James C.; Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 159, Washington, DC 20013 USA. [Jawad, Laith] Manukau, Auckland, New Zealand. [Brothers, Edward B.] EFS Consultants, Ithaca, NY 14850 USA. RP Tyler, JC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, MRC 159, POB 37012, Washington, DC 20013 USA. EM tylerj@si.edu; johnsond@si.edu; laith_jawad@hotmail.com; ghotti@gmail.com NR 19 TC 1 Z9 1 U1 1 U2 2 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 SEP 11 PY 2014 VL 127 IS 2 BP 311 EP 322 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AQ5UY UT WOS:000342875300002 ER PT J AU Harasewych, MG Petitt, RE AF Harasewych, M. G. Petitt, Richard E. TI Cancellaria (Cancellaria) coltrorum, a new species of Cancellariidae (Gastropoda: Neogastropoda) from Brazil SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Brazilian Province; Cancellaria petuchi; Cancellaria reticulata; Cancellaria urceolata; biogeography AB Cancellaria (Cancellaria) coltrorum, new species, is described from shallow waters of the southern Brazilian Province, ranging from the Abrolhos Archipelago to Vitoria. This new species co-occurs with C. petuchi Harasewych, Petit & Verhecken, 1992 but may be distinguished from it by having a broader shell with a shorter, wider spire; a proportionally larger aperture that is widest along its adapical half and has fewer, weaker lirae on the outer lip; and, most conspicuously, by having reticulate sculpture that becomes more irregular and dominated by axial ribs in latter whorls, and by being white or faintly mottled in very light tan rather than having dark brown spiral bands. The broad-ranging Cancellaria reticulata (Linnaeus, 1767) differs from both C. petuchi and C. coltrorum in having a shell with finer and more regular spiral and axial sculpture that is equal in prominence and produces a regular, reticulated pattern, as well as in having a thick, bifid posteriormost columellar fold and in lacking a thick callus that obscures the sculpture along the parietal region. Similarities in shell morphology suggest that C. mixta Landau, Petit & Silva, 2012, from the late Miocene of Panama, was a progenitor of C. coltrorum and C. petuchi, as well as the Panamic C. urceolata Hinds, 1843. C1 [Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 7012, Washington, DC 20013 USA. EM harasewych@si.edu NR 17 TC 0 Z9 0 U1 1 U2 1 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 SEP 11 PY 2014 VL 127 IS 2 BP 400 EP 405 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AQ5UY UT WOS:000342875300010 ER PT J AU Glynn, PW Bayer, FM Renegar, DA AF Glynn, Peter W. Bayer, Frederick M. Renegar, D. Abigail TI Coeloplana waltoni, a new species of minute benthic ctenophore (Ctenophora: Platyctenida) from south Florida SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE ectosymbiont; Florida; platyctenid ctenophore; subtropical western Atlantic ID TENTACULATA PLATYCTENIDA; KOREA AB A minute and abundant species of benthic ctenophore is described, resurrected from an unpublished manuscript of Frederick M. Bayer (deceased). It is an ectosymbiont of octocorals in south Florida. Members of the ctenophoran order Platyctenida were unknown from American waters until 1945, when specimens from Miami, Florida were reported by F. G. Walton Smith and referred to the genus Coeloplana. That species subsequently was found in Jamaica, and Rankin (1956) described it under the new generic name Vallicula. A second species of creeping ctenophore was found in the 1960s and rediscovered in 2011, living as an ectosymbiont on octocorals in the coastal waters near Miami. This species belongs to the original genus Coeloplana and is here described as Coeloplana waltoni, new species. This description is based on specimens examined by F. M. Bayer in the 1960s and additional material from collections obtained in 2012-2013. Critical differences between C. waltoni and Vallicula multiformis are noted, based on recently collected specimens of the latter in Biscayne Bay, Miami, Florida. C1 [Glynn, Peter W.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, Miami, FL 33149 USA. [Bayer, Frederick M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Renegar, D. Abigail] Nova Southeastern Univ Oceanog Ctr, Natl Coral Reef Inst, Dania, FL 33004 USA. RP Glynn, PW (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Dept Marine Biol & Ecol, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM pglynn@rsmas.miami.edu; drenegar@nova.edu NR 29 TC 1 Z9 1 U1 2 U2 10 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 SEP 11 PY 2014 VL 127 IS 2 BP 423 EP 436 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AQ5UY UT WOS:000342875300012 ER PT J AU Beutler, F Saito, S Seo, HJ Brinkmann, J Dawson, KS Eisenstein, DJ Font-Ribera, A Ho, S McBride, CK Montesano, F Percival, WJ Ross, AJ Ross, NP Samushia, L Schlegel, DJ Sanchez, AG Tinker, JL Weaver, BA AF Beutler, Florian Saito, Shun Seo, Hee-Jong Brinkmann, Jon Dawson, Kyle S. Eisenstein, Daniel J. Font-Ribera, Andreu Ho, Shirley McBride, Cameron K. Montesano, Francesco Percival, Will J. Ross, Ashley J. Ross, Nicholas P. Samushia, Lado Schlegel, David J. Sanchez, Ariel G. Tinker, Jeremy L. Weaver, Benjamin A. TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: testing gravity with redshift space distortions using the power spectrum multipoles SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitation; surveys; cosmological parameters; cosmology: observations; dark energy; large-scale structure of Universe ID DIGITAL SKY SURVEY; DARK ENERGY SURVEY; LUMINOUS RED GALAXIES; ACOUSTIC-OSCILLATIONS; COSMOLOGICAL CONSTANT; GROWTH-RATE; GENERAL-RELATIVITY; PARAMETER; UNIVERSE; MODEL AB We analyse the anisotropic clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS Data Release 11 (DR11) sample, which consists of 690 827 galaxies in the redshift range 0.43 < z < 0.7 and has a sky coverage of 8498 deg(2). We perform our analysis in Fourier space using a power spectrum estimator suggested by Yamamoto et al. We measure the multipole power spectra in a self-consistent manner for the first time in the sense that we provide a proper way to treat the survey window function and the integral constraint, without the commonly used assumption of an isotropic power spectrum and without the need to split the survey into subregions. The main cosmological signals exploited in our analysis are the baryon acoustic oscillations and the signal of redshift space distortions, both of which are distorted by the Alcock-Paczynski effect. Together, these signals allow us to constrain the distance ratio D-V(z(eff))/r(s)(z(d)) = 13.89 +/- 0.18, the Alcock-Paczynski parameter F-AP(z(eff)) = 0.679 +/- 0.031 and the growth rate of structure f (z(eff))sigma(8)(z(eff)) = 0.419 +/- 0.044 at the effective redshift z(eff) = 0.57. We emphasize that our constraints are robust against possible systematic uncertainties. In order to ensure this, we perform a detailed systematics study against CMASS mock galaxy catalogues and N-body simulations. We find that such systematics will lead to 3.1 per cent uncertainty for f sigma(8) if we limit our fitting range to k = 0.01-0.20 h Mpc(-1), where the statistical uncertainty is expected to be three times larger. We did not find significant systematic uncertainties for D-V/r(s) or FAP. Combining our data set with Planck to test General Relativity (GR) through the simple gamma-parametrization, where the growth rate is given by f (z) = Omega(gamma)(m)(z), reveals a similar to 2 sigma tension between the data and the prediction by GR. The tension between our result and GR can be traced back to a tension in the clustering amplitude sigma(8) between CMASS and Planck. C1 [Beutler, Florian; Saito, Shun; Font-Ribera, Andreu; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Saito, Shun] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Chiba 2778582, Japan. [Saito, Shun] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Saito, Shun] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Seo, Hee-Jong] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, LBL, Berkeley, CA 94720 USA. [Seo, Hee-Jong] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Seo, Hee-Jong] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Brinkmann, Jon] Apache Point Observ, Sunspot, NM 88349 USA. [Dawson, Kyle S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Eisenstein, Daniel J.; McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, Shirley] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Ho, Shirley] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Montesano, Francesco; Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Percival, Will J.; Ross, Ashley J.; Samushia, Lado] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Ross, Nicholas P.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Beutler, F (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. EM fbeutler@lbl.gov RI Ho, Shirley/P-3682-2014; OI Ho, Shirley/0000-0002-1068-160X; Beutler, Florian/0000-0003-0467-5438 FU Japan Society for the Promotion of Science (JSPS) [25887012]; Alfred P. Sloan Foundation; 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; National Science Foundation; U.S. Department of Energy Office of Science; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX FB would like to thank Chris Blake, Uros Seljak, Eric Linder, Beth Reid, Martin White, Morag Scrimgeour and Julien Guy for helpful discussion. SS is supported by a Grant-in-Aid for Young Scientists (Start-up) from the Japan Society for the Promotion of Science (JSPS) (no. 25887012).; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract no. DE-AC02-05CH11231. NR 134 TC 101 Z9 101 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 11 PY 2014 VL 443 IS 2 BP 1065 EP 1089 DI 10.1093/mnras/stu1051 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN2SY UT WOS:000340436800010 ER PT J AU Mao, QQ Berlind, AA McBride, CK Scherrer, RJ Scoccimarro, R Manera, M AF Mao, Qingqing Berlind, Andreas A. McBride, Cameron K. Scherrer, Robert J. Scoccimarro, Roman Manera, Marc TI Constraining primordial non-Gaussianity with moments of the large-scale density field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; inflation; large-scale structure of Universe ID DIGITAL SKY SURVEY; OSCILLATION SPECTROSCOPIC SURVEY; COSMOLOGICAL PERTURBATION-THEORY; 3-POINT CORRELATION-FUNCTION; LUMINOUS RED GALAXIES; POINT CORRELATION-FUNCTIONS; HIGHER-ORDER MOMENTS; SDSS-III; INITIAL CONDITIONS; REDSHIFT SURVEY AB We use cosmological N-body simulations to investigate whether measurements of the moments of large-scale structure can yield constraints on primordial non-Gaussianity. We measure the variance, skewness, and kurtosis of the evolved density field from simulations with Gaussian and three different non-Gaussian initial conditions: a local model with f(NL) = 100, an equilateral model with f(NL) = -400, and an orthogonal model with f(NL) = -400. We show that the moments of the dark matter density field differ significantly between Gaussian and non-Gaussian models. We also make the measurements on mock galaxy catalogues that contain galaxies with clustering properties similar to those of luminous red galaxies. We find that, in the case of skewness and kurtosis, galaxy bias reduces the detectability of non-Gaussianity. However, in the case of the variance, galaxy bias greatly amplifies the detectability of non-Gaussianity. In all cases, we find that redshift distortions do not significantly affect the detectability. When we restrict our measurements to volumes equivalent to the Sloan Digital Sky Survey II or Baryon Oscillation Spectroscopic Survey samples, the probability of detecting a departure from the Gaussian model is high by using measurements of the variance, but very low by using only skewness and kurtosis. We estimate that in order to detect an amount of non-Gaussianity that is consistent with recent cosmic microwave background constraints using skewness or kurtosis, we would need a galaxy survey that is much larger than any planned future survey. However, future surveys should be large enough to place meaningful constraints using galaxy variance measurements. C1 [Mao, Qingqing; Berlind, Andreas A.; Scherrer, Robert J.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Scoccimarro, Roman] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Scoccimarro, Roman] NYU, Dept Phys, New York, NY 10003 USA. [Manera, Marc] UCL, London WC1E 6BT, England. RP Mao, QQ (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. EM qingqing.mao@vanderbilt.edu RI Mao, Qingqing/E-2043-2016 OI Mao, Qingqing/0000-0001-6001-6723 FU National Science Foundation (NSF) through NSF CAREER [AST-1151650]; Department of Energy [DE-FG05-85ER40226]; Vanderbilt University; NSF [AST-1109432]; NASA [NNA10A171G] FX QM and AAB were supported by the National Science Foundation (NSF) through NSF CAREER grant AST-1151650. RJS was supported in part by the Department of Energy (DE-FG05-85ER40226). QM, AAB and RJS were also supported by a Discovery grant from Vanderbilt University. RS is supported in part by grants NSF AST-1109432 and NASA NNA10A171G. The simulations used in this paper were produced by the LasDamas project (http://lss.phy.vanderbilt.edu/lasdamas/); we thank NSF XSEDE for providing the computational resources for LasDamas. NR 83 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 SEP 11 PY 2014 VL 443 IS 2 BP 1402 EP 1415 DI 10.1093/mnras/stu1255 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN2SY UT WOS:000340436800037 ER PT J AU Parker, ML Wilkins, DR Fabian, AC Grupe, D Dauser, T Matt, G Harrison, FA Brenneman, L Boggs, SE Christensen, FE Craig, WW Gallo, LC Hailey, CJ Kara, E Komossa, S Marinucci, A Miller, JM Risaliti, G Stern, D Walton, DJ Zhang, WW AF Parker, M. L. Wilkins, D. R. Fabian, A. C. Grupe, D. Dauser, T. Matt, G. Harrison, F. A. Brenneman, L. Boggs, S. E. Christensen, F. E. Craig, W. W. Gallo, L. C. Hailey, C. J. Kara, E. Komossa, S. Marinucci, A. Miller, J. M. Risaliti, G. Stern, D. Walton, D. J. Zhang, W. W. TI The NuSTAR spectrum of Mrk 335: extreme relativistic effects within two gravitational radii of the event horizon? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: individual: Mrk 335; galaxies: Seyfert ID ACTIVE GALACTIC NUCLEI; X-RAY REFLECTION; ACCRETING BLACK-HOLES; XMM-NEWTON; FLUX STATE; LONG HARD; NGC 4051; IRAS 13224-3809; EMISSION-LINES; 1H 0707-495 AB We present 3-50 keV NuSTAR observations of the active galactic nuclei Mrk 335 in a very low flux state. The spectrum is dominated by very strong features at the energies of the iron line at 5-7 keV and Compton hump from 10-30 keV. The source is variable during the observation, with the variability concentrated at low energies, which suggesting either a relativistic reflection or a variable absorption scenario. In this work, we focus on the reflection interpretation, making use of new relativistic reflection models that self consistently calculate the reflection fraction, relativistic blurring and angle-dependent reflection spectrum for different coronal heights to model the spectra. We find that the spectra can be well fitted with relativistic reflection, and that the lowest flux state spectrum is described by reflection alone, suggesting the effects of extreme light-bending occurring within similar to 2 gravitational radii (R-G) of the event horizon. The reflection fraction decreases sharply with increasing flux, consistent with a point source moving up to above 10 R-G as the source brightens. We constrain the spin parameter to greater than 0.9 at the 3 sigma confidence level. By adding a spin-dependent upper limit on the reflection fraction to our models, we demonstrate that this can be a powerful way of constraining the spin parameter, particularly in reflection dominated states. We also calculate a detailed emissivity profile for the iron line, and find that it closely matches theoretical predictions for a compact source within a few R-G of the black hole. C1 [Parker, M. L.; Wilkins, D. R.; Fabian, A. C.; Kara, E.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Wilkins, D. R.; Gallo, L. C.] St Marys Univ, Halifax, NS B3H 3C3, Canada. [Grupe, D.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Dauser, T.] Dr Karl Remeis Observ, D-96049 Bamberg, Germany. [Dauser, T.] Erlangen Ctr Astroparticle Phys, D-96049 Bamberg, Germany. [Matt, G.; Marinucci, A.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Harrison, F. A.; Walton, D. J.] CALTECH, Pasadena, CA 91125 USA. [Brenneman, L.; Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boggs, S. E.] 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. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Craig, W. W.; Hailey, C. J.] Columbia Univ, New York, NY 10027 USA. [Komossa, S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Parker, ML (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mlparker@ast.cam.ac.uk RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Risaliti, Guido/0000-0002-3556-977X FU NASA [NAS5-00136]; Science and Technology Facilities Council (STFC); Royal Society; Italian Space Agency [ASI/INAFI/037/12/0 - 011/13]; CITA National Fellowship; European Union [312789] FX This work is based on observations made by the NuSTAR mission, a project led by the California Institute of Astronomy, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NUSTARDAS, jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). At Penn State Swift is supported by NASA contract NAS5-00136. MLP acknowledges financial support from the Science and Technology Facilities Council (STFC). ACF thanks the Royal Society for support. AM and GM acknowledge financial support from Italian Space Agency under grant ASI/INAFI/037/12/0 - 011/13. DRW is supported by a CITA National Fellowship. The research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement no. 312789. NR 57 TC 37 Z9 37 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 SEP 11 PY 2014 VL 443 IS 2 BP 1723 EP 1732 DI 10.1093/mnras/stu1246 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN2SY UT WOS:000340436800062 ER PT J AU Sternberg, A Gal-Yam, A Simon, JD Patat, F Hillebrandt, W Phillips, MM Foley, RJ Thompson, I Morrell, N Chomiuk, L Soderberg, AM Yong, D Kraus, AL Herczeg, GJ Hsiao, EY Raskutti, S Cohen, JG Mazzali, PA Nomoto, K AF Sternberg, A. Gal-Yam, A. Simon, J. D. Patat, F. Hillebrandt, W. Phillips, M. M. Foley, R. J. Thompson, I. Morrell, N. Chomiuk, L. Soderberg, A. M. Yong, D. Kraus, A. L. Herczeg, G. J. Hsiao, E. Y. Raskutti, S. Cohen, J. G. Mazzali, P. A. Nomoto, K. TI Multi-epoch high-spectral-resolution observations of neutral sodium in 14 Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; supernovae: general; ISM: general ID WHITE-DWARFS; CIRCUMSTELLAR MATERIAL; ECHELLE SPECTROGRAPH; VIOLENT MERGERS; TRIPLE-SYSTEMS; COLLISIONS; SIMULATIONS; PROGENITORS; ABSORPTION; TELESCOPE AB One of the main questions concerning Type Ia supernovae is the nature of the binary companion of the exploding white dwarf. A major discriminant between different suggested models is the presence and physical properties of circumstellar material at the time of explosion. If present, this material will be ionized by the ultraviolet radiation of the explosion and later recombine. This ionization-recombination should manifest itself as time-variable absorption features that can be detected via multi-epoch high-spectral-resolution observations. Previous studies have shown that the strongest effect is seen in the neutral sodium D lines. We report on observations of neutral sodium absorption features observed in multi-epoch high-resolution spectra of 14 Type Ia supernova events. This is the first multi-epoch high-resolution study to include multiple SNe. No variability in line strength that can be associated with circumstellar material is detected in the events presented in this paper. If we include previously published events, we find that similar to 18 per cent of the events in the extended sample exhibit time-variable sodium features associated with circumstellar material. We explore the implication of this study on our understanding of the progenitor systems of Type Ia supernovae via the current Type Ia supernova multi-epoch high-spectral-resolution sample. C1 [Sternberg, A.; Hillebrandt, W.; Mazzali, P. A.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gal-Yam, A.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Simon, J. D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Patat, F.] European So Observ, D-85748 Garching, Germany. [Phillips, M. M.; Thompson, I.; Morrell, N.; Hsiao, E. Y.] Las Campanas Observ, Carnegie Observ, La Serena, Chile. [Foley, R. J.] Univ Illinois Champagne Urbana, Dept Astron, Urbana, IL 61801 USA. [Chomiuk, L.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yong, D.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Kraus, A. L.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Herczeg, G. J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Raskutti, S.] Princeton Univ, Dept Astrophys, Princeton, NJ 08540 USA. [Cohen, J. G.] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA. [Mazzali, P. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England. [Nomoto, K.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. RP Sternberg, A (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild St 1, D-85741 Garching, Germany. EM asternberg@mpa-garching.mpg.de OI Patat, Ferdinando/0000-0002-0537-3573 FU Minerva Fellowship; EU/FP7 via an ERC grant [307260]; Kimmel award; Minerva ARCHES prize; ESO Telescopes at the La Silla Paranal Observatory, Chile [289.D-5023, 290.D-5010, 290.D-5023, 091.D-0780]; W.M. Keck Foundation FX AS is supported by a Minerva Fellowship. The research of AG is supported by the EU/FP7 via an ERC grant no. 307260, the Minerva ARCHES prize and the Kimmel award.; Partially based on observations made with ESO Telescopes at the La Silla Paranal Observatory, Chile, under programme ID 289.D-5023, 290.D-5010, 290.D-5023, 091.D-0780.; 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 76 TC 21 Z9 21 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 SEP 11 PY 2014 VL 443 IS 2 BP 1849 EP 1860 DI 10.1093/mnras/stu1202 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AN2SY UT WOS:000340436800072 ER PT J AU Khan, I Maldonado, E Vasconcelos, V O'Brien, SJ Johnson, WE Antunes, A AF Khan, Imran Maldonado, Emanuel Vasconcelos, Vitor O'Brien, Stephen J. Johnson, Warren E. Antunes, Agostinho TI Mammalian keratin associated proteins (KRTAPs) subgenomes: disentangling hair diversity and adaptation to terrestrial and aquatic environments SO BMC GENOMICS LA English DT Article DE Concerted evolution; Gene family; Keratin Associated Proteins; Keratin; Hair; Gene conversion; Recombination; Positive selection ID BIASED GENE CONVERSION; DETECTING POSITIVE SELECTION; HIGH-GLYCINE-TYROSINE; AMINO-ACID SITES; FOLLICLE DIFFERENTIATION; PUNCTUATED EQUILIBRIUM; MAXIMUM-LIKELIHOOD; SIZE POLYMORPHISMS; KAP GENES; EVOLUTION AB Background: Adaptation of mammals to terrestrial life was facilitated by the unique vertebrate trait of body hair, which occurs in a range of morphological patterns. Keratin associated proteins (KRTAPs), the major structural hair shaft proteins, are largely responsible for hair variation. Results: We exhaustively characterized the KRTAP gene family in 22 mammalian genomes, confirming the existence of 30 KRTAP subfamilies evolving at different rates with varying degrees of diversification and homogenization. Within the two major classes of KRTAPs, the high cysteine (HS) subfamily experienced strong concerted evolution, high rates of gene conversion/recombination and high GC content. In contrast, high glycine-tyrosine (HGT) KRTAPs showed evidence of positive selection and low rates of gene conversion/recombination. Species with more hair and of higher complexity tended to have more KRATP genes (gene expansion). The sloth, with long and coarse hair, had the most KRTAP genes (175 with 141 being intact). By contrast, the "hairless" dolphin had 35 KRTAPs and the highest pseudogenization rate (74% relative to the 19% mammalian average). Unique hair-related phenotypes, such as scales (armadillo) and spines (hedgehog), were correlated with changes in KRTAPs. Gene expression variation probably also influences hair diversification patterns, for example human have an identical KRTAP repertoire as apes, but much less hair. Conclusions: We hypothesize that differences in KRTAP gene repertoire and gene expression, together with distinct rates of gene conversion/recombination, pseudogenization and positive selection, are likely responsible for micro and macro-phenotypic hair diversification among mammals in response to adaptations to ecological pressures. C1 [Khan, Imran; Maldonado, Emanuel; Vasconcelos, Vitor; Antunes, Agostinho] Univ Porto, Ctr Interdisciplinar Invest Marinha & Ambiental, CIMAR CIIMAR, P-4050123 Oporto, Portugal. [Khan, Imran; Vasconcelos, Vitor; Antunes, Agostinho] Univ Porto, Fac Ciencias, Dept Biol, P-4169007 Oporto, Portugal. [O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199004, Russia. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Ft Lauderdale, FL 33004 USA. [Johnson, Warren E.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Antunes, A (reprint author), Univ Porto, Ctr Interdisciplinar Invest Marinha & Ambiental, CIMAR CIIMAR, Rua Bragas 177, P-4050123 Oporto, Portugal. EM aantunes@ciimar.up.pt RI Vasconcelos, Vitor/A-8933-2008; Johnson, Warren/D-4149-2016; OI Vasconcelos, Vitor/0000-0003-3585-2417; Johnson, Warren/0000-0002-5954-186X; O'Brien, Stephen J./0000-0001-7353-8301; khan, imran/0000-0002-9892-7271; Maldonado, Emanuel/0000-0002-0084-6116 FU Portuguese Fundacao para a Ciencia e a Tecnologia (FCT) [SFRH/BD/48518/2008]; Russian Ministry of Science Mega-grant [11.G34.31.0068]; [PTDC/AAC- AMB/104983/2008 (FCOMP-01-0124-FEDER-008610)]; [PTDC/AAC-AMB/121301/2010 (FCOMP-01-0124-FEDER-019490)]; [PesT-C/MAR/LA0015/2011] FX The authors acknowledge the Portuguese Fundacao para a Ciencia e a Tecnologia (FCT) for financial support to IK (SFRH/BD/48518/2008) and the projects PTDC/AAC- AMB/104983/2008 (FCOMP-01-0124-FEDER-008610), PTDC/AAC-AMB/121301/2010 (FCOMP-01-0124-FEDER-019490) and PesT-C/MAR/LA0015/2011 to AA. SJO was supported as PI by Russian Ministry of Science Mega-grant no. 11.G34.31.0068. We would also like to thank Siby Philip and Joao Paulo Machado for useful discussions during this work. The authors thank the anonymous reviewers for constructive comments on an earlier version of this manuscript. NR 104 TC 7 Z9 7 U1 5 U2 28 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2164 J9 BMC GENOMICS JI BMC Genomics PD SEP 10 PY 2014 VL 15 AR UNSP 779 DI 10.1186/1471-2164-15-779 PG 18 WC Biotechnology & Applied Microbiology; Genetics & Heredity SC Biotechnology & Applied Microbiology; Genetics & Heredity GA AQ0GY UT WOS:000342462400001 PM 25208914 ER PT J AU Gehara, M Crawford, AJ Orrico, VGD Rodriguez, A Lotters, S Fouquet, A Barrientos, LS Brusquetti, F De la Riva, I Ernst, R Urrutia, GG Glaw, F Guayasamin, JM Holting, M Jansen, M Kok, PJR Kwet, A Lingnau, R Lyra, M Moravec, J Pombal, JP Rojas-Runjaic, FJM Schulze, A Senaris, JC Sole, M Rodrigues, MT Twomey, E Haddad, CFB Vences, M Kohler, J AF Gehara, Marcelo Crawford, Andrew J. Orrico, Victor G. D. Rodriguez, Ariel Loetters, Stefan Fouquet, Antoine Barrientos, Lucas S. Brusquetti, Francisco De la Riva, Ignacio Ernst, Raffael Gagliardi Urrutia, Giuseppe Glaw, Frank Guayasamin, Juan M. Hoelting, Monique Jansen, Martin Kok, Philippe J. R. Kwet, Axel Lingnau, Rodrigo Lyra, Mariana Moravec, Jiri Pombal, Jose P., Jr. Rojas-Runjaic, Fernando J. M. Schulze, Arne Senaris, J. Celsa Sole, Mirco Rodrigues, Miguel Trefaut Twomey, Evan Haddad, Celio F. B. Vences, Miguel Koehler, Joern TI High Levels of Diversity Uncovered in a Widespread Nominal Taxon: Continental Phylogeography of the Neotropical Tree Frog Dendropsophus minutus SO PLOS ONE LA English DT Article ID BRAZILIAN ATLANTIC FOREST; LEPTODACTYLUS-FUSCUS SCHNEIDER; MOLECULAR PHYLOGENY; RAIN-FOREST; SPECIES RICHNESS; ANURA-LEPTODACTYLIDAE; TROPICAL AMPHIBIANS; CRYPTIC DIVERSITY; MITOCHONDRIAL-DNA; CROTALUS-DURISSUS AB Species distributed across vast continental areas and across major biomes provide unique model systems for studies of biotic diversification, yet also constitute daunting financial, logistic and political challenges for data collection across such regions. The tree frog Dendropsophus minutus (Anura: Hylidae) is a nominal species, continentally distributed in South America, that may represent a complex of multiple species, each with a more limited distribution. To understand the spatial pattern of molecular diversity throughout the range of this species complex, we obtained DNA sequence data from two mitochondrial genes, cytochrome oxidase I (COI) and the 16S rhibosomal gene (16S) for 407 samples of D. minutus and closely related species distributed across eleven countries, effectively comprising the entire range of the group. We performed phylogenetic and spatially explicit phylogeographic analyses to assess the genetic structure of lineages and infer ancestral areas. We found 43 statistically supported, deep mitochondrial lineages, several of which may represent currently unrecognized distinct species. One major clade, containing 25 divergent lineages, includes samples from the type locality of D. minutus. We defined that clade as the D. minutus complex. The remaining lineages together with the D. minutus complex constitute the D. minutus species group. Historical analyses support an Amazonian origin for the D. minutus species group with a subsequent dispersal to eastern Brazil where the D. minutus complex originated. According to our dataset, a total of eight mtDNA lineages have ranges > 100,000 km(2). One of them occupies an area of almost one million km(2) encompassing multiple biomes. Our results, at a spatial scale and resolution unprecedented for a Neotropical vertebrate, confirm that widespread amphibian species occur in lowland South America, yet at the same time a large proportion of cryptic diversity still remains to be discovered. C1 [Gehara, Marcelo; Rodriguez, Ariel; Vences, Miguel] Tech Univ Carolo Wilhelmina Braunschweig, Inst Zool, Div Evolutionary Biol, Braunschweig, Germany. [Gehara, Marcelo] Univ Fed Rio Grande do Norte, Ctr Biociencias, Posgrad Sistemat & Evolucao, BR-59072970 Natal, RN, Brazil. [Crawford, Andrew J.; Barrientos, Lucas S.] Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia. [Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Orrico, Victor G. D.; Rodrigues, Miguel Trefaut] Univ Sao Paulo, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. [Loetters, Stefan] Univ Trier, Biogeog Dept, Trier, Germany. [Fouquet, Antoine] CNRS Guyane USR3456, Cayenne, French Guiana. [Brusquetti, Francisco] Univ Estadual Paulista, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. [Brusquetti, Francisco] Inst Invest Biol Paraguay, Asuncion, Paraguay. [De la Riva, Ignacio] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. [Ernst, Raffael; Hoelting, Monique] Senckenberg Nat Hist Collect Dresden, Museum Zool, Dresden, Germany. [Gagliardi Urrutia, Giuseppe] Peruvian Ctr Biodivers & Conservat, Nanay, Iquitos, Peru. [Glaw, Frank] Zool Staatssammlung Munchen, Munich, Germany. Univ Tecnol Indoamer, Ctr Invest Biodiversidad & Cambio Climat BioCamp, Cotocollao, Quito, Ecuador. [Jansen, Martin] Senckenberg Gesell Nat Forsch, Frankfurt, Germany. [Kok, Philippe J. R.] Vrije Univ Brussel, Dept Biol, Amphibian Evolut Lab, Brussels, Belgium. [Kwet, Axel] German Herpetol Soc DGHT, Mannheim, Germany. [Lingnau, Rodrigo] Univ Tecnol Fed Parana, Francisco Beltrao, PR, Brazil. [Lyra, Mariana; Haddad, Celio F. B.] Univ Estadual Paulista, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. [Moravec, Jiri] Natl Museum, Dept Zool, Prague, Czech Republic. [Pombal, Jose P., Jr.] Univ Fed Rio de Janeiro, Museu Nacl, Dept Vertebrados, Rio De Janeiro, Brazil. [Rojas-Runjaic, Fernando J. M.] Museo Hist Nat La Salle, Fdn La Salle Ciencias Nat, Caracas, Venezuela. [Schulze, Arne; Koehler, Joern] Hess Landesmuseum Darmstadt, Darmstadt, Germany. [Senaris, J. Celsa] Inst Venezolano Invest Cient, Ctr Ecol, Lab Ecol & Genet Poblac, Caracas, Venezuela. [Sole, Mirco] Univ Estadual Santa Cruz, Dept Ciencias Biol, Ilheus, BA, Brazil. [Twomey, Evan] E Carolina Univ, Dept Biol, Greenville, NC USA. RP Gehara, M (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Zool, Div Evolutionary Biol, Pockelsstr 10A, Braunschweig, Germany. EM marcelo.gehara@gmail.com RI Fachbereich14, Dekanat/C-8553-2015; Rodrigues, Miguel/F-8174-2012; Lingnau, Rodrigo/F-9035-2010; Lyra, Mariana/O-6405-2014; Haddad, Celio/C-4267-2012; Pombal, Jose/C-6365-2015; Rojas-Runjaic, Fernando J. M./K-2555-2014; Orrico, Victor/G-9796-2012; Sole, Mirco/A-9722-2008; OI Crawford, Andrew J./0000-0003-3153-6898; Brusquetti, Francisco/0000-0001-7242-1208; Lingnau, Rodrigo/0000-0001-8406-4439; Lyra, Mariana/0000-0002-7863-4965; Rojas-Runjaic, Fernando J. M./0000-0001-5409-4231; Orrico, Victor/0000-0002-4560-4006; Sole, Mirco/0000-0001-7881-6227; Vences, Miguel/0000-0003-0747-0817; Rodriguez, Ariel/0000-0003-1936-793X FU Alexander von Humboldt foundation; FAPESP [2008/50928-1, s 03/10335-8, 10/51071-7, 11/50146-6]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico - CNPq; Nacional de Incentivo a Investigadores (PRONII, Paraguay); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, Brazil); Ministry of Culture of the Czech Republic [DKRVO 2013/14, DKRVO 2012, 00023272]; KAAD; NSF [DEB 1035184, 1120487]; Deutsche Forschungsgemeinschaft [VE247/7-1]; Belgian Directorate-General of Development Cooperation; King Leopold III Fund for Nature Exploration and Conservation; Percy Sladen Memorial Fund; non-profit organization "les Amis de l'Institut Royal des Sciences Naturelles"; German Research Foundation [DFG ER 589/2*1]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo - FAPESP [2012/12500-5]; Ecopetrol [156-09]; Universidad Tecnologica Indoamerica; FAPERJ FX AR was supported by a Post-Doctoral fellowship of the Alexander von Humboldt foundation. CFBH acknowledges support by FAPESP (proc. 2008/50928-1) and Conselho Nacional de Desenvolvimento Cientifico e Tecnologico - CNPq. FB thanks Programa Nacional de Incentivo a Investigadores (PRONII, Paraguay) and Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES, Brazil) for financial support. JM was financially supported by the Ministry of Culture of the Czech Republic (DKRVO 2012 and DKRVO 2013/14; 00023272). MG was supported by a PhD fellowship of the KAAD. MTR acknowledges support by FAPESP (# s 03/10335-8, 10/51071-7, and 11/50146-6), CNPq, and NSF (DEB 1035184 and 1120487). MV acknowledges support by the Deutsche Forschungsgemeinschaft (grant VE247/7-1). PJRK was mainly supported by the Belgian Directorate-General of Development Cooperation, the King Leopold III Fund for Nature Exploration and Conservation, and the Percy Sladen Memorial Fund, with additional support by the non-profit organization "les Amis de l'Institut Royal des Sciences Naturelles''. RE and MH were supported by a research grant from the German Research Foundation (DFG ER 589/2*1). VGDO acknowledges support by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo - FAPESP (# 2012/12500-5). Laboratory work in Colombia was financed by grant # 156-09 from Ecopetrol. Funding was provided by the Universidad Tecnologica Indoamerica through the project "Patrones de diversidad de los anfibios andinos del Ecuador''. JPP is grateful to CNPq and FAPERJ for financial support. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 124 TC 23 Z9 23 U1 6 U2 52 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 10 PY 2014 VL 9 IS 9 AR e103958 DI 10.1371/journal.pone.0103958 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AP4EP UT WOS:000342030300005 PM 25208078 ER PT J AU Lopez-Morales, M Triaud, AHMJ Rodler, F Dumusque, X Buchhave, LA Harutyunyan, A Hoyer, S Alonso, R Gillon, M Kaib, NA Latham, DW Lovis, C Pepe, F Queloz, D Raymond, SN Segransan, D Waldmann, IP Udry, S AF Lopez-Morales, Mercedes Triaud, Amaury H. M. J. Rodler, Florian Dumusque, Xavier Buchhave, Lars A. Harutyunyan, Avet Hoyer, Sergio Alonso, Roi Gillon, Michael Kaib, Nathan A. Latham, David. W. Lovis, Christophe Pepe, Francesco Queloz, Didier Raymond, Sean N. Segransan, Damien Waldmann, Ingo P. Udry, Stephane TI ROSSITER-MCLAUGHLIN OBSERVATIONS OF 55 Cnc e SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: formation; planets and satellites: individual (55 Cancri e); stars: individual (55 Cancri); techniques: radial velocities; techniques: spectroscopic ID SUPER-NEPTUNE HAT-P-11B; PLANETARY SYSTEM; MASS PLANET; HOT JUPITER; HOST STARS; K-DWARF; EARTH; CANCRI; ROTATION; VELOCITY AB We present Rossiter-McLaughlin observations of the transiting super-Earth 55 Cnc e collected during six transit events between 2012 January and 2013 November with HARPS and HARPS-N. We detect no radial velocity signal above 35 cm s(-1) (3 sigma) and confine the stellar v sin i(*) to 0.2 +/- 0.5 km s(-1). The star appears to be a very slow rotator, producing a very low amplitude Rossiter-McLaughlin effect. Given such a low amplitude, the Rossiter-McLaughlin effect of 55 Cnc e is undetected in our data, and any spin-orbit angle of the system remains possible. We also performed Doppler tomography and reach a similar conclusion. Our results offer a glimpse of the capacity of future instrumentation to study low amplitude Rossiter-McLaughlin effects produced by super-Earths. C1 [Lopez-Morales, Mercedes; Rodler, Florian; Dumusque, Xavier; Buchhave, Lars A.; Latham, David. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Triaud, Amaury H. M. J.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Triaud, Amaury H. M. J.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rodler, Florian] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Harutyunyan, Avet] INAF, Fdn Galileo Galilei, E-738712 Tenerife, Spain. [Hoyer, Sergio; Alonso, Roi] Inst Astrofis Canarias, E-38205 San Cristobal la Laguna, Spain. [Hoyer, Sergio; Alonso, Roi] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Gillon, Michael] Univ Liege, Inst Astrophys Geophys, B-4000 Cointe Ougree, Belgium. [Kaib, Nathan A.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Kaib, Nathan A.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Kaib, Nathan A.; Lovis, Christophe; Pepe, Francesco; Queloz, Didier; Segransan, Damien; Udry, Stephane] Univ Geneva, Astron Observ, CH-1290 Sauverny, Switzerland. [Queloz, Didier] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Raymond, Sean N.] Univ Bordeaux, LAB, UMR 5804, F-33270 Floirac, France. [Raymond, Sean N.] CNRS, LAB, UMR 5804, F-33270 Floirac, France. [Waldmann, Ingo P.] UCL, Dept Phys & Astron, London WC1E 6BT, England. RP Lopez-Morales, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mlopez-morales@cfa.harvard.edu RI Alonso, Roi/D-8799-2014; OI Alonso, Roi/0000-0001-8462-8126; Buchhave, Lars A./0000-0003-1605-5666 FU John Templeton Foundation; European Union Seventh Framework Programme (FP7) [313014]; Swiss National Science Foundation [P300P2-147773]; Alexander-von-Humboldt postdoctoral fellowship program; Swiss National Science Foundation (SNSF); Spanish Ministry of Economy and Competitiveness [SEV-20110187] FX This publication was made possible through the support of a grant from the John Templeton Foundation. The opinions expressed are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. The research leading to these results received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement 313014 (ETAEARTH). This work used the VALD database, operated at Uppsala University, the Institute of Astronomy RAS in Moscow, and the University of Vienna. We thank the anonymous referee for a very constructive review and J. Winn for useful comments. A. H.M.J.T. is a Swiss National Science Foundation fellow under grant number P300P2-147773. F.R. acknowledges funding from the Alexander-von-Humboldt postdoctoral fellowship program. X.D. thanks the Swiss National Science Foundation (SNSF) for its support through an Early Postdoc Mobility fellowship. S.H. acknowledges support from the Spanish Ministry of Economy and Competitiveness under the 2011 Severo Ochoa Program MINECO SEV-20110187. HARPS-N is a collaboration between the Astronomical Observatory of the Geneva University, the CfA in Cambridge, the University of St. Andrews, the Queens University of Belfast, and the TNG-INAF Observatory. We thank all the researchers whose observing programs on HARPS were disrupted by our DDT program and who kindly observed for us. Finally, we thank ESO's director general, Tim de Zeeuw, who granted our HARPS observing time. NR 48 TC 11 Z9 11 U1 0 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 SEP 10 PY 2014 VL 792 IS 2 AR L31 DI 10.1088/2041-8205/792/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KT UT WOS:000341307500007 ER PT J AU Barnard, R Steiner, JF Prestwich, AF Stevens, IR Clark, JS Kolb, UC AF Barnard, R. Steiner, J. F. Prestwich, A. F. Stevens, I. R. Clark, J. S. Kolb, U. C. TI ENERGY-DEPENDENT EVOLUTION IN IC10 X-1: HARD EVIDENCE FOR AN EXTENDED CORONA AND IMPLICATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: black holes; stars: Wolf-Rayet; X-rays: binaries; X-rays: general ID X-RAY BINARY; MASS BLACK-HOLE; ACCRETION DISK CORONA; NGC 5408 X-1; WOLF-RAYET; XMM-NEWTON; ORBITAL PERIOD; IC-10 X-1; NEUTRON-STAR; VELA X-1 AB We have analyzed a similar to 130 ks XMM-Newton observation of the dynamically confirmed black hole + Wolf-Rayet (BH+WR) X-ray binary (XB) IC10 X-1, covering similar to 1 orbital cycle. This system experiences periodic intensity dips every similar to 35 hr. We find that energy-independent evolution is rejected at a >5 sigma level. The spectral and timing evolution of IC10 X-1 are best explained by a compact disk blackbody and an extended Comptonized component, where the thermal component is completely absorbed and the Comptonized component is partially covered during the dip. We consider three possibilities for the absorber: cold material in the outer accretion disk, as is well documented for Galactic neutron star (NS) XBs at high inclination; a stream of stellar wind that is enhanced by traveling through the L1 point; and a spherical wind. We estimated the corona radius (r(ADC)) for IC10 X-1 from the dip ingress to be similar to 10(6) km, assuming absorption from the outer disk, and found it to be consistent with the relation between r(ADC) and 1-30 keV luminosity observed in Galactic NS XBs that spans two orders of magnitude. For the other two scenarios, the corona would be larger. Prior BH mass (M-BH) estimates range over 23-38 M-circle dot, depending on the inclination and WR mass. For disk absorption, the inclination, i, is likely to be similar to 60-80 degrees, with M-BH similar to 24-41 M-circle dot. Alternatively, the L1-enhanced wind requires i similar to 80 degrees, suggesting similar to 24-33 M-circle dot. For a spherical absorber, i similar to 40 degrees, and M-BH similar to 50-65M(circle dot). C1 [Barnard, R.; Steiner, J. F.; Prestwich, A. F.] Harvard Smithsonian Ctr Astrophys CFA, Cambridge, MA 02138 USA. [Stevens, I. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Clark, J. S.; Kolb, U. C.] Open Univ, Milton Keynes MK7 6AA, Bucks, England. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys CFA, Cambridge, MA 02138 USA. FU ESA member states; U.S. (NASA); NASA [GO3-14095X]; NASA Hubble Fellowship [HST-HF-51315.01] FX We thank the referee for insights on how to improve the paper. We thank Paul Crowther for useful discussions about the properties of the wind. This research has made use of data from XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the U.S. (NASA). R.B. was supported by NASA grant GO3-14095X. J.F.S. was supported by NASA Hubble Fellowship grant HST-HF-51315.01. NR 66 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 SEP 10 PY 2014 VL 792 IS 2 AR 131 DI 10.1088/0004-637X/792/2/131 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200049 ER PT J AU David, LP Lim, J Forman, W Vrtilek, J Combes, F Salome, P Edge, A Hamer, S Jones, C Sun, M O'Sullivan, E Gastaldello, F Bardelli, S Temi, P Schmitt, H Ohyama, Y Mathews, W Brighenti, F Giacintucci, S Trung, DV AF David, Laurence P. Lim, Jeremy Forman, William Vrtilek, Jan Combes, Francoise Salome, Philippe Edge, Alastair Hamer, Stephen Jones, Christine Sun, Ming O'Sullivan, Ewan Gastaldello, Fabio Bardelli, Sandro Temi, Pasquale Schmitt, Henrique Ohyama, Youichi Mathews, William Brighenti, Fabrizio Giacintucci, Simona Trung, Dinh-V TI MOLECULAR GAS IN THE X-RAY BRIGHT GROUP NGC 5044 AS REVEALED BY ALMA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: groups: individual (NGC 5044); galaxies: ISM ID EARLY-TYPE GALAXIES; GALACTIC NUCLEUS FEEDBACK; CENTRAL CLUSTER GALAXIES; COOLING FLOW CLUSTERS; STAR-FORMATION; ELLIPTIC GALAXIES; TELESCOPE OBSERVATIONS; SPITZER OBSERVATIONS; LUMINOUS CLUSTERS; HIGH-RESOLUTION AB An ALMA observation of the early-type galaxy NGC 5044, which resides at the center of an X-ray bright group with a moderate cooling flow, detected 24 molecular structures within the central 2.5 kpc. The masses of the molecular structures vary from 3 x 10(5) M-circle dot to 10(7) M-circle dot and the CO(2-1) linewidths vary from 15 to 65 km s(-1). Given the large CO(2-1) linewidths, the observed structures are likely giant molecular associations (GMAs) and not individual giant molecular clouds (GMCs). Only a few of the GMAs are spatially resolved and the average density of these GMAs yields a GMC volume filling factor of about 15%. The masses of the resolved GMAs are insufficient for them to be gravitationally bound, however, the most massive GMA does contain a less massive component with a linewidth of 5.5 km s(-1) (typical of an individual virialized GMC). We also show that the GMAs cannot be pressure confined by the hot gas. Given the CO(2-1) linewidths of the GMAs (i.e., the velocity dispersion of the embedded GMCs) they should disperse on a timescale of about 12 Myr. No disk-like molecular structures are detected and all indications suggest that the molecular gas follows ballistic trajectories after condensing out of the thermally unstable hot gas. The 230 GHz luminosity of the central continuum source is 500 times greater than its low frequency radio luminosity and probably reflects a recent accretion event. The spectrum of the central continuum source also exhibits an absorption feature with a linewidth typical of an individual GMC and an infalling velocity of 250 km s(-1). C1 [David, Laurence P.; Forman, William; Vrtilek, Jan; Jones, Christine; O'Sullivan, Ewan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lim, Jeremy] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Combes, Francoise; Salome, Philippe] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Edge, Alastair; Hamer, Stephen] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Sun, Ming] Univ Alabama, Dept Phys, Huntsville, AL 35899 USA. [Gastaldello, Fabio; Bardelli, Sandro] IASF Milano, INAF, I-20133 Milan, Italy. [Temi, Pasquale] NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. [Schmitt, Henrique] Naval Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Ohyama, Youichi] Acad Sinica, Inst Astron & Astrophys, Taipei, Taiwan. [Mathews, William] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brighenti, Fabrizio] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Trung, Dinh-V] Vietnamese Acad Sci & Technol, Inst Phys, Hanoi, Vietnam. RP David, LP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ldavid@head.cfa.harvard.edu RI Gastaldello, Fabio/N-4226-2015; Bardelli, Sandro/O-9369-2015; OI Gastaldello, Fabio/0000-0002-9112-0184; Bardelli, Sandro/0000-0002-8900-0298; O'Sullivan, Ewan/0000-0002-5671-6900; Edge, Alastair/0000-0002-3398-6916; Forman, William/0000-0002-9478-1682; Combes, Francoise/0000-0003-2658-7893 FU NASA [GO2-13146X]; STFC [ST/I001573/1] FX This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00735. 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. This work was supported in part by NASA grant GO2-13146X. A.C.E. acknowledges support from STFC grant ST/I001573/1. We thank M. Birkinshaw for assistance in learning CASA and analyzing the ALMA data and B. McNamara and P. Nulsen for discussions about their cycle 0 ALMA observations of clusters of galaxies. NR 64 TC 13 Z9 13 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 SEP 10 PY 2014 VL 792 IS 2 AR 94 DI 10.1088/0004-637X/792/2/94 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200012 ER PT J AU Deacon, NR Liu, MC Magnier, EA Aller, KM Best, WMJ Dupuy, T Bowler, BP Mann, AW Redstone, JA Burgett, WS Chambers, KC Draper, PW Flewelling, H Hodapp, KW Kaiser, N Kudritzki, RP Morgan, JS Metcalfe, N Price, PA Tonry, JL Wainscoat, RJ AF Deacon, Niall R. Liu, Michael C. Magnier, Eugene A. Aller, Kimberly M. Best, William M. J. Dupuy, Trent Bowler, Brendan P. Mann, Andrew W. Redstone, Joshua A. Burgett, William S. Chambers, Kenneth C. Draper, Peter W. Flewelling, H. Hodapp, Klaus W. Kaiser, Nick Kudritzki, Rolf-Peter Morgan, Jeff S. Metcalfe, Nigel Price, Paul A. Tonry, John L. Wainscoat, Richard J. TI WIDE COOL AND ULTRACOOL COMPANIONS TO NEARBY STARS FROM Pan-STARRS 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; stars: low-mass; surveys ID BROWN DWARF COMPANION; COMMON PROPER-MOTION; ALL-SKY SURVEY; LOW-MASS STARS; INFRARED-SURVEY-EXPLORER; CANDIDATE SUBSTELLAR COMPANION; INTEGRAL-FIELD SPECTROGRAPH; STELLAR KINEMATIC GROUPS; GENEVA-COPENHAGEN SURVEY; ADAPTIVE OPTICS SYSTEM AB We present the discovery of 57 wide (>5 '') separation, low-mass (stellar and substellar) companions to stars in the solar neighborhood identified from Pan-STARRS 1 (PS1) data and the spectral classification of 31 previously known companions. Our companions represent a selective subsample of promising candidates and span a range in spectral type of K7-L9 with the addition of one DA white dwarf. These were identified primarily from a dedicated common proper motion search around nearby stars, along with a few as serendipitous discoveries from our Pan-STARRS 1 brown dwarf search. Our discoveries include 23 new L dwarf companions and one known L dwarf not previously identified as a companion. The primary stars around which we searched for companions come from a list of bright stars with well-measured parallaxes and large proper motions from the Hipparcos catalog (8583 stars, mostly A-K dwarfs) and fainter stars from other proper motion catalogs (79170 stars, mostly M dwarfs). We examine the likelihood that our companions are chance alignments between unrelated stars and conclude that this is unlikely for the majority of the objects that we have followed-up spectroscopically. We also examine the entire population of ultracool (>M7) dwarf companions and conclude that while some are loosely bound, most are unlikely to be disrupted over the course of similar to 10 Gyr. Our search increases the number of ultracool M dwarf companions wider than 300AU by 88% and increases the number of L dwarf companions in the same separation range by 82%. Finally, we resolve our new L dwarf companion to HIP 6407 into a tight (0 ''.13, 7.4AU) L1+T3 binary, making the system a hierarchical triple. Our search for these key benchmarks against which brown dwarf and exoplanet atmosphere models are tested has yielded the largest number of discoveries to date. C1 [Deacon, Niall R.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Deacon, Niall R.; Liu, Michael C.; Magnier, Eugene A.; Aller, Kimberly M.; Best, William M. J.; Bowler, Brendan P.; Burgett, William S.; Chambers, Kenneth C.; Flewelling, H.; Kaiser, Nick; Kudritzki, Rolf-Peter; Morgan, Jeff S.; Tonry, John L.; Wainscoat, Richard J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dupuy, Trent] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowler, Brendan P.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Mann, Andrew W.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Redstone, Joshua A.] Equatine Labs, Cambridge, MA 02139 USA. [Draper, Peter W.; Metcalfe, Nigel] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Hodapp, Klaus W.] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. [Price, Paul A.] Princeton Univ Observ, Princeton, NJ 08544 USA. RP Deacon, NR (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM deacon@mpia.de OI Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402; Flewelling, Heather/0000-0002-1050-4056 FU National Aeronautics and Space Administration [NNX08AR22G]; National Science Foundation [AST-1238877]; NSF [AST09-09222, AST-0709460]; AFRL [FA9451-06-2-0338] FX The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE). The authors thank Bill Golisch, Dave Griep, and Eric Volqardsen for assisting with the IRTF observations. This research has benefited from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser, at http://www.browndwarfs.org/spexprism. 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. This research has benefited from the M, L, and T dwarf compendium housed at DwarfArchives.org and maintained by Chris Gelino, Davy Kirkpatrick, and Adam Burgasser. M.C.L. and E.A.M. were supported by NSF grants AST09-09222 (awarded to M.C.L.) and AST-0709460 (awarded to E.A.M.). E.A.M. was also supported by AFRL Cooperative Agreement FA9451-06-2-0338. 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. 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 paper makes use of observations processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge. The authors thank Mike Irwin and the team at CASU for making the reduced WFCAM data available promptly and Tim Carroll, Thor Wold, Jack Ehle and Watson Varricatt for assisting with UKIRT observations. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. The VISTA Data Flow System pipeline processing and science archive are described in Irwin et al. (2004) and Hambly et al. (2008). We have used data from the first data release. This paper makes use of the Topcat software package (Taylor 2005). This research has made use of the Washington Double Star Catalog maintained at the U.S. Naval Observatory. We thank Luca Casagrande, Jackie Faherty, Adam Kraus, Eddie Schlafly, and Josh Schlieder for helpful discussions and our referee Sebastien Lepine for many helpful comments which improved the manuscript. Finally, 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 207 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 SEP 10 PY 2014 VL 792 IS 2 AR 119 DI 10.1088/0004-637X/792/2/119 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200037 ER PT J AU Friesen, B Baron, E Wisniewski, JP Parrent, JT Thomas, RC Miller, TR Marion, GH AF Friesen, Brian Baron, E. Wisniewski, John P. Parrent, Jerod T. Thomas, R. C. Miller, Timothy R. Marion, G. H. TI NEAR-INFRARED LINE IDENTIFICATION IN TYPE Ia SUPERNOVAE DURING THE TRANSITIONAL PHASE SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; radiative transfer; supernovae: general; supernovae: individual (SN 2001fe, SN2002bo, SN 2003du, SN 2014J) ID LTE MODEL ATMOSPHERES; MAXIMUM LIGHT; SPECTRA; SPECTROSCOPY; TIME; NUCLEOSYNTHESIS; CONSTRAINTS; EXPLOSION; 2014J; M82 AB We present near-infrared synthetic spectra of a delayed-detonation hydrodynamical model and compare them to observed spectra of four normal Type Ia supernovae ranging from day +56.5 to day +85. This is the epoch during which supernovae are believed to be undergoing the transition from the photospheric phase, where spectra are characterized by line scattering above an optically thick photosphere, to the nebular phase, where spectra consist of optically thin emission from forbidden lines. We find that most spectral features in the near-infrared can be accounted for by permitted lines of Fe II and Co II. In addition, we find that [Ni II] fits the emission feature near 1.98 mu m, suggesting that a substantial mass of Ni-58 exists near the center of the ejecta in these objects, arising from nuclear burning at high density. C1 [Friesen, Brian; Baron, E.; Wisniewski, John P.; Miller, Timothy R.] Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Baron, E.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Parrent, Jerod T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Thomas, R. C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Computat Res Div, Berkeley, CA 94720 USA. [Marion, G. H.] Univ Texas Austin, Austin, TX 78712 USA. RP Friesen, B (reprint author), Homer L Dodge Dept Phys & Astron, 440 West Brooks St,Room 100, Norman, OK 73019 USA. OI Baron, Edward/0000-0001-5393-1608 FU NSF [AST-0707704]; NASA through a grant from the Space Telescope Science Institute [HST-GO-12298.05-A, HST-GO-122948.04-A]; NASA [NAS5-26555]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Hochstleistungs Rechenzentrum Nord (HLRN) FX We are grateful to the referee for a thoughtful review that significantly improved the quality of this work. We also thank Ivo Seitenzahl for pointing out an error in our model's nucleosynthesis properties. This research has made use of NASA's Astrophysics Data System and the Weizmann Interactive Supernova Data Repository (WISeREP), and is based on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. This work has been supported in part by support from NSF grant AST-0707704 and by support for programs HST-GO-12298.05-A, and HST-GO-122948.04-A 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. 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 and the Hochstleistungs Rechenzentrum Nord (HLRN). We thank both these institutions for a generous allocation of computer time. NR 52 TC 14 Z9 14 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 SEP 10 PY 2014 VL 792 IS 2 AR 120 DI 10.1088/0004-637X/792/2/120 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200038 ER PT J AU Gandhi, P Lansbury, GB Alexander, DM Stern, D Arevalo, P Ballantyne, DR Balokovic, M Bauer, FE Boggs, SE Brandt, WN Brightman, M Christensen, FE Comastri, A Craig, WW Del Moro, A Elvis, M Fabian, AC Hailey, CJ Harrison, FA Hickox, RC Koss, M LaMassa, SM Luo, B Madejski, GM Ptak, AF Puccetti, S Teng, SH Urry, CM Walton, DJ Zhang, WW AF Gandhi, P. Lansbury, G. B. Alexander, D. M. Stern, D. Arevalo, P. Ballantyne, D. R. Balokovic, M. Bauer, F. E. Boggs, S. E. Brandt, W. N. Brightman, M. Christensen, F. E. Comastri, A. Craig, W. W. Del Moro, A. Elvis, M. Fabian, A. C. Hailey, C. J. Harrison, F. A. Hickox, R. C. Koss, M. LaMassa, S. M. Luo, B. Madejski, G. M. Ptak, A. F. Puccetti, S. Teng, S. H. Urry, C. M. Walton, D. J. Zhang, W. W. TI NuSTAR UNVEILS A COMPTON-THICK TYPE 2 QUASAR IN MrK 34 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; X-rays: galaxies; X-rays: individual (Mrk 34) ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; SEYFERT 2 GALAXIES; X-RAY-EMISSION; STAR-FORMING GALAXIES; NARROW-LINE REGION; XMM-NEWTON SURVEY; BLACK-HOLE MASS; SWIFT-BAT SURVEY; MIDINFRARED SELECTION AB We present Nuclear Spectroscopic Telescope Array (NuSTAR) 3-40 keV observations of the optically selected Type 2 quasar (QSO2) SDSS J1034+6001 or Mrk 34. The high-quality hard X-ray spectrum and archival XMM-Newton data can be fitted self-consistently with a reflection-dominated continuum and a strong Fe K alpha fluorescence line with equivalent width > 1 keV. Prior X-ray spectral fitting below 10 keV showed the source to be consistent with being obscured by Compton-thin column densities of gas along the line of sight, despite evidence for much higher columns from multiwavelength data. NuSTAR now enables a direct measurement of this column and shows that N-H lies in the Compton-thick (CT) regime. The new data also show a high intrinsic 2-10 keV luminosity of L2-10 similar to 10(44) erg s (1), in contrast to previous low-energy X-ray measurements where L2-10 less than or similar to 10(43) erg s (1) (i.e., X-ray selection below 10 keV does not pick up this source as an intrinsically luminous obscured quasar). Both the obscuring column and the intrinsic power are about an order of magnitude (or more) larger than inferred from pre-NuSTAR X-ray spectral fitting. Mrk 34 is thus a "gold standard" CT QSO2 and is the nearest non-merging system in this class, in contrast to the other local CT quasar NGC 6240, which is currently undergoing a major merger coupled with strong star formation. For typical X-ray bolometric correction factors, the accretion luminosity of Mrk 34 is high enough to potentially power the total infrared luminosity. X-ray spectral fitting also shows that thermal emission related to star formation is unlikely to drive the observed bright soft component below similar to 3 keV, favoring photoionization instead. C1 [Gandhi, P.; Lansbury, G. B.; Alexander, D. M.; Del Moro, A.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Arevalo, P.; Bauer, F. E.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 22, Spain. [Arevalo, P.] Univ Valparaiso, Fac Ciencias, Inst Fis & Astron, Valparaiso, Chile. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Balokovic, M.; Harrison, F. A.; Walton, D. J.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Bauer, F. E.] Millennium Inst Astrophys, Santiago, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Luo, B.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Brandt, W. N.; Luo, B.] 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. [Brightman, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF Osserv Astron Bologna, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R. C.] Dartmouth Coll, Wilder Lab 6127, Dept Phys & Astron, Hanover, NH 03755 USA. [Koss, M.] Swiss Fed Inst Technol, Inst Astron, Dept Phys, CH-8093 Zurich, Switzerland. [LaMassa, S. M.; Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Madejski, G. M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Ptak, A. F.; Zhang, W. W.] NASA Goddard Space Flight Ctr, XRay Astrophys Lab, Greenbelt, MD 20771 USA. [Puccetti, S.] ASDC ASI, I-00133 Rome, Italy. [Puccetti, S.] INAF Osserv Astron Roma, I-00040 Monte Porzio Catone, RM, Italy. [Teng, S. H.] NASA Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP Gandhi, P (reprint author), Univ Durham, Dept Phys, Durham DH1 3LE, England. RI Boggs, Steven/E-4170-2015; Koss, Michael/B-1585-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Boggs, Steven/0000-0001-9567-4224; Koss, Michael/0000-0002-7998-9581; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Puccetti, Simonetta/0000-0002-2734-7835; Urry, Meg/0000-0002-0745-9792 FU STFC [ST/J003697/1, ST/K501979/1, ST/I001573/1]; Leverhulme Trust; NASA Postdoctoral Program; ASI-INAF grant; Anillo [ACT1101]; FONDECYT [1140304]; International Fulbright Science and Technology Award; Swiss National Science Foundation (NSF) [PP00P2 138979/1]; Durham University COFUND fellowship; Basal-CATA [PFB-06/2007]; CONICYT-Chile (FONDECYT [1141218]; "EMBIGGEN" Anillo [ACT1101]; Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo [IC120009]; National Aeronautics and Space Administration (NASA); NuSTAR Operations, Software, and Calibration teams FX Grant and fellowship acknowledgments: STFC ST/J003697/1 (P.G.), ST/K501979/1 (G.B.L.), ST/I001573/1 (D.M.A. and A.D.M.), Leverhulme Trust (D.M.A.), NASA Postdoctoral Program (S.H.T), ASI-INAF grant (A.C.), Anillo ACT1101 and FONDECYT 1140304 (P.A.), International Fulbright Science and Technology Award (M. B.), and Swiss National Science Foundation (NSF) grant PP00P2 138979/1 (M.K.). In addition, F.A.H. acknowledges support from a Durham University COFUND fellowship, and F.E.B. acknowledges support from Basal-CATA PFB-06/2007, CONICYT-Chile (FONDECYT 1141218 and "EMBIGGEN" Anillo ACT1101) Project IC120009 "Millennium Institute of Astrophysics (MAS)" funded by the Iniciativa Cientifica Milenio del Ministerio de Economia, Fomento y Turismo. The authors thank Fred K.Y. Lo for megamaser discussions, and the referee for the report. P.G. thanks James R. Mullaney and Chris M. Harrison for discussions. P.G. is also grateful to Matteo Guainazzi for his comments and insights on the origin of the soft X-ray spectrum.; NuSTAR is a project led by the California Institute of Technology (Caltech), managed by the Jet Propulsion Laboratory (JPL), and funded by the National Aeronautics and Space Administration (NASA). The NuSTAR Operations, Software, and Calibration teams are acknowledged for support with 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 work has made use of data from XMM-Newton and the Sloan Digital Sky Survey. Figure 5 is based upon data from with the NASA/ESA Hubble Space Telescope and obtained from the Hubble Legacy Archive. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by JPL, Caltech, under contract with NASA. NR 137 TC 32 Z9 32 U1 0 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 SEP 10 PY 2014 VL 792 IS 2 AR 117 DI 10.1088/0004-637X/792/2/117 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200035 ER PT J AU Levi, A Sasselov, D Podolak, M AF Levi, A. Sasselov, D. Podolak, M. TI STRUCTURE AND DYNAMICS OF COLD WATER SUPER-EARTHS: THE CASE OF OCCLUDED CH4 AND ITS OUTGASSING SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: interiors; planets and satellites: oceans; planets and satellites: surfaces; planets and satellites: tectonics ID METHANE CLATHRATE HYDRATE; EQUATION-OF-STATE; THERMAL-CONDUCTIVITY; HIGH-PRESSURE; PLANETARY CONDITIONS; TERRESTRIAL PLANETS; AQUEOUS SOLUBILITY; PHASE-TRANSITIONS; MANTLE CONVECTION; PLATE-TECTONICS AB In this work, we study the transport of methane in the external water envelopes surrounding water-rich super-Earths. We investigate the influence of methane on the thermodynamics and mechanics of the water mantle. We find that including methane in the water matrix introduces a new phase (filled ice), resulting in hotter planetary interiors. This effect renders the super-ionic and reticulating phases accessible to the lower ice mantle of relatively low-mass planets (similar to 5 M-E) lacking a H/He atmosphere. We model the thermal and structural profile of the planetary crust and discuss five possible crustal regimes which depend on the surface temperature and heat flux. We demonstrate that the planetary crust can be conductive throughout or partly confined to the dissociation curve of methane clathrate hydrate. The formation of methane clathrate in the subsurface is shown to inhibit the formation of a subterranean ocean. This effect results in increased stresses on the lithosphere, making modes of ice plate tectonics possible. The dynamic character of the tectonic plates is analyzed and the ability of this tectonic mode to cool the planet is estimated. The icy tectonic plates are found to be faster than those on a silicate super-Earth. A mid-layer of low viscosity is found to exist between the lithosphere and the lower mantle. Its existence results in a large difference between ice mantle overturn timescales and resurfacing timescales. Resurfacing timescales are found to be 1 Ma for fast plates and 100 Ma for sluggish plates, depending on the viscosity profile and ice mass fraction. Melting beneath spreading centers is required in order to account for the planetary radiogenic heating. The melt fraction is quantified for the various tectonic solutions explored, ranging from a few percent for the fast and thin plates to total melting of the upwelled material for the thick and sluggish plates. Ice mantle dynamics is found to be important for assessing the composition of the atmosphere. We propose a mechanism for methane release into the atmosphere, where freshly exposed reservoirs of methane clathrate hydrate at the ridge dissociate under surface conditions. We formulate the relation between the outgassing flux and the tectonic mode dynamical characteristics. We give numerical estimates for the global outgassing rate of methane into the atmosphere. We find, for example, that for a 2 M-E planet outgassing can release 10(27)-10(29) molecules s(-1) of methane to the atmosphere. We suggest a qualitative explanation for how the same outgassing mechanism may result in either a stable or a runaway volatile release, depending on the specifics of a given planet. Finally, we integrate the global outgassing rate for a few cases and quantify how the surface atmospheric pressure of methane evolves over time. We find that methane is likely an important constituent of water planets' atmospheres. C1 [Levi, A.; Podolak, M.] Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. [Levi, A.; Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Levi, A (reprint author), Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. EM amitlevi.planetphys@gmail.com OI LEVI, AMIT/0000-0003-1080-1007 FU Origins of Life Initiative at Harvard University FX We convey our thanks to Prof. Richard J. O'Connell for helpful conversations. We also thank the anonymous referee for constructive suggestions. This work was supported by the Origins of Life Initiative at Harvard University. NR 113 TC 3 Z9 3 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2014 VL 792 IS 2 AR 125 DI 10.1088/0004-637X/792/2/125 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200043 ER PT J AU Psaltis, D Ozel, F AF Psaltis, Dimitrios Oezel, Feryal TI PULSE PROFILES FROM SPINNING NEUTRON STARS IN THE HARTLE-THORNE APPROXIMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE gravitation; stars: neutron ID X-RAY PULSARS; ROTATING RELATIVISTIC STARS; LIGHT CURVES; MILLISECOND OSCILLATIONS; EMISSION MODELS; HOT-SPOTS; CONSTRAINTS; MASS; BURSTS; RADIUS AB We present a new numerical algorithm for the calculation of pulse profiles from spinning neutron stars in the Hartle-Thorne approximation. Our approach allows us to formally take into account the effects of Doppler shifts and aberration, of frame dragging, as well as of the oblateness of the stellar surface and of its quadrupole moment. We confirm an earlier result that neglecting the oblateness of the neutron-star surface leads to similar or equal to 5%-30% errors in the calculated profiles and further show that neglecting the quadrupole moment of its spacetime leads to similar or equal to 1%-5% errors at a spin frequency of similar or equal to 600 Hz. We discuss the implications of our results for the measurements of neutron-star masses and radii with upcoming X-ray missions, such as NASA's NICER and ESA's LOFT. C1 [Psaltis, Dimitrios; Oezel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Psaltis, Dimitrios; Oezel, Feryal] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Oezel, Feryal] Harvard Univ, Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. RP Psaltis, D (reprint author), Univ Arizona, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA. EM dpsaltis@email.arizone.edu; fozel@email.arizone.edu FU NSF [AST-1108753]; NSF CAREER award [AST-0746549]; Chandra Theory grant [TM2-13002X]; Radcliffe Institute for Advanced Study at Harvard University FX We thank Michi Baubock for many useful discussions on ray tracing in neutron-star spacetimes and the referee Sharon Morsink for enlightening discussions and comments. This work was supported in part by NSF grant AST-1108753, NSF CAREER award AST-0746549, and Chandra Theory grant TM2-13002X. F.O. gratefully acknowledges support from the Radcliffe Institute for Advanced Study at Harvard University. NR 37 TC 13 Z9 13 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 SEP 10 PY 2014 VL 792 IS 2 AR 87 DI 10.1088/0004-637X/792/2/87 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200005 ER PT J AU Veyette, MJ Williams, BF Dalcanton, JJ Balick, B Caldwell, N Fouesneau, M Girardi, L Gordon, KD Kalirai, J Rosenfield, P Seth, AC AF Veyette, Mark J. Williams, Benjamin F. Dalcanton, Julianne J. Balick, Bruce Caldwell, Nelson Fouesneau, Morgan Girardi, Leo Gordon, Karl D. Kalirai, Jason Rosenfield, Philip Seth, Anil C. TI PANCHROMATIC HUBBLE ANDROMEDA TREASURY. IX. A PHOTOMETRIC SURVEY OF PLANETARY NEBULAE IN M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M31); planetary nebulae: general ID LARGE-MAGELLANIC-CLOUD; LOCAL GROUP GALAXIES; DIGITAL SKY SURVEY; EXCITATION-CLASS; EVOLUTION; STARS; SPECTROGRAPH; KINEMATICS; PARAMETER; REGIONS AB We search the Hubble Space Telescope (HST) Advanced Camera for Surveys and Wide Field Camera 3 broadband imaging data from the Panchromatic Hubble Andromeda Treasury (PHAT) survey to identify detections of cataloged planetary nebulae (PNs). Of the 711 PNs currently in the literature within the PHAT footprint, we find 467 detected in the broadband. For these 467, we are able to refine their astrometric accuracy from similar to 0.'' 3 to 0.'' 05. Using the resolution of the HST, we are able to show that 152 objects currently in the catalogs are definitively not PNs, and we show that 32 objects thought to be extended in ground-based images are actually point-like and therefore good PN candidates. We also find one PN candidate that is marginally resolved. If this is a PN, it is up to 0.7 pc in diameter. With our new photometric data, we develop a method of measuring the level of excitation in individual PNs by comparing broadband and narrowband imaging and describe the effects of excitation on a PN's photometric signature. Using the photometric properties of the known PNs in the PHAT catalogs, we search for more PNs, but do not find any new candidates, suggesting that ground-based emission-line surveys are complete in the PHAT footprint to F475W similar or equal to 24. C1 [Veyette, Mark J.; Williams, Benjamin F.; Dalcanton, Julianne J.; Balick, Bruce; Fouesneau, Morgan] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Veyette, Mark J.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fouesneau, Morgan] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Girardi, Leo] Osserv Astron Padova INAF, I-35122 Padua, Italy. [Gordon, Karl D.; Kalirai, Jason] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gordon, Karl D.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium. [Kalirai, Jason] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Rosenfield, Philip] Univ Padua, Dept Phys & Astron G Galilei, I-35122 Padua, Italy. [Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Veyette, MJ (reprint author), Univ Washington, Dept Astron, POB 351580, Seattle, WA 98195 USA. EM mveyette@uw.edu OI Seth, Anil/0000-0003-0248-5470; Rosenfield, Philip/0000-0001-9306-6049 FU NASA from the Space Telescope Science Institute [GO-12055]; NASA [NAS5-26555] FX Support for this work was provided by NASA through grant GO-12055 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 35 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 SEP 10 PY 2014 VL 792 IS 2 AR 121 DI 10.1088/0004-637X/792/2/121 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200039 ER PT J AU Zhang, QZ Qiu, KP Girart, JM Liu, HY Tang, YW Koch, PM Li, ZY Keto, E Ho, PTP Rao, R Lai, SP Ching, TC Frau, P Chen, HH Li, HB Padovani, M Bontemps, S Csengeri, T Juarez, C AF Zhang, Qizhou Qiu, Keping Girart, Josep M. Liu, Hauyu (Baobab) Tang, Ya-Wen Koch, Patrick M. Li, Zhi-Yun Keto, Eric Ho, Paul T. P. Rao, Ramprasad Lai, Shih-Ping Ching, Tao-Chung Frau, Pau Chen, How-Huan Li, Hua-Bai Padovani, Marco Bontemps, Sylvain Csengeri, Timea Juarez, Carmen TI MAGNETIC FIELDS AND MASSIVE STAR FORMATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (G192, G240, NGC 2264, NGC 6334, G34.41, G35.2N, IRAS18360, W51, DR21 (OH)); ISM: magnetic fields; polarization; stars: formation; submillimeter: ISM; techniques: polarimetric ID HIGH-ANGULAR RESOLUTION; TAURUS MOLECULAR CLOUD; INFRARED DARK CLOUDS; 1333 IRAS 4A; FORMING REGION; DENSE CORES; PROTOSTELLAR CANDIDATES; SUBMILLIMETER ARRAY; CO OUTFLOWS; HIERARCHICAL FRAGMENTATION AB Massive stars ( M > 8 M-circle dot) typically form in parsec-scale molecular clumps that collapse and fragment, leading to the birth of a cluster of stellar objects. We investigate the role of magnetic fields in this process through dust polarization at 870 mu m obtained with the Submillimeter Array (SMA). The SMA observations reveal polarization at scales of less than or similar to 0.1 pc. The polarization pattern in these objects ranges from ordered hour-glass configurations to more chaotic distributions. By comparing the SMA data with the single dish data at parsec scales, we found that magnetic fields at dense core scales are either aligned within 40 degrees of or perpendicular to the parsec-scale magnetic fields. This finding indicates that magnetic fields play an important role during the collapse and fragmentation of massive molecular clumps and the formation of dense cores. We further compare magnetic fields in dense cores with the major axis of molecular outflows. Despite a limited number of outflows, we found that the outflow axis appears to be randomly oriented with respect to the magnetic field in the core. This result suggests that at the scale of accretion disks (less than or similar to 10(3) AU), angular momentum and dynamic interactions possibly due to close binary or multiple systems dominate over magnetic fields. With this unprecedentedly large sample of massive clumps, we argue on a statistical basis that magnetic fields play an important role during the formation of dense cores at spatial scales of 0.01-0.1 pc in the context of massive star and cluster star formation. C1 [Zhang, Qizhou; Keto, Eric; Ho, Paul T. P.; Ching, Tao-Chung; Chen, How-Huan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Qiu, Keping] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Girart, Josep M.; Juarez, Carmen] CSIC IEEC, Fac Ciencies, Inst Ciencies Espai, E-08193 Bellaterra, Catalonia, Spain. [Liu, Hauyu (Baobab); Tang, Ya-Wen; Koch, Patrick M.; Ho, Paul T. P.; Rao, Ramprasad; Lai, Shih-Ping] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Li, Zhi-Yun] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Lai, Shih-Ping; Ching, Tao-Chung] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Lai, Shih-Ping; Ching, Tao-Chung] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. [Frau, Pau] Observ Astron Nacl, E-28014 Madrid, Spain. [Li, Hua-Bai] Chinese Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Padovani, Marco] Ecole Normale Super, CNRS, Lab Radioastron Millimetr, UMR 8112, F-75231 Paris 05, France. [Padovani, Marco] Observ Paris, F-75231 Paris 05, France. [Bontemps, Sylvain] Univ Bordeaux 1, CNRS, OASU LAB UMR5804, F-33270 Floirac, France. [Csengeri, Timea] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Zhang, QZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM qzhang@cfa.harvard.edu RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 FU Spanish MINECO [AYA2011-30228-C03]; Catalan AGAUR [2009SGR1172]; Ministry of Science and Technology Taiwan [NSC 101-2119-M-007-004]; MOST [102-2119-M-007-004-MY3]; Nanjing University [985] FX We are indebted to the SMA staff for their effort in instrument development and observing support. Without their dedication, this large polarization study would not have been possible. Q.Z. is grateful to F.H. Shu for his encouragement, and to R.L. Plambeck and C.L.H. Hull for enlightening discussions. J.M.G. and C.J. are supported by the Spanish MINECO AYA2011-30228-C03 and Catalan AGAUR 2009SGR1172 grants. S.P.L. and T.C.C. are supported by the Ministry of Science and Technology Taiwan with grants NSC 101-2119-M-007-004 and MOST 102-2119-M-007-004-MY3. K.Q. is partially supported by the 985 project of Nanjing University. NR 90 TC 30 Z9 30 U1 0 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 SEP 10 PY 2014 VL 792 IS 2 AR 116 DI 10.1088/0004-637X/792/2/116 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RF UT WOS:000341172200034 ER PT J AU Rabeling, C Schultz, TR Pierce, NE Bacci, M AF Rabeling, Christian Schultz, Ted R. Pierce, Naomi E. Bacci, Mauricio, Jr. TI A Social Parasite Evolved Reproductive Isolation from Its Fungus-Growing Ant Host in Sympatry SO CURRENT BIOLOGY LA English DT Article ID X-LINKED GENES; HYMENOPTERA-FORMICIDAE; ALTERNATIVE ADAPTATIONS; PHYLOGENETIC ANALYSIS; MYCOCEPURUS-SMITHII; SPECIES TREES; SPECIATION; EVOLUTION; SEQUENCES; INQUILINE AB Inquiline social parasitic ant species exploit colonies of other ant species mainly by producing sexual offspring that are raised by the host. Ant social parasites and their hosts are often close relatives (Emery's rule), and two main hypotheses compete to explain the parasites' evolutionary origins: (1) the interspecific hypothesis proposes an allopatric speciation scenario for the parasite, whereas (2) the intraspecific hypothesis postulates that the parasite evolves directly from its host in sympatry [1-10]. Evidence in support of the intraspecific hypothesis has been accumulating for ants [3, 5, 7, 9-12], but sympatric speciation remains controversial as a general speciation mechanism for inquiline parasites. Here we use molecular phylogenetics to assess whether the socially parasitic fungus-growing ant Mycocepurus castrator speciated from its host Mycocepurus goeldii in sympatry. Based on differing patterns of relationship in mitochondrial and individual nuclear genes, we conclude that host and parasite occupy a temporal window in which lineage sorting has taken place in the mitochondrial genes but not yet in the nuclear alleles. We infer that the host originated first and that the parasite originated subsequently from a subset of the host species' populations, providing empirical support for the hypothesis that inquiline parasites can evolve reproductive isolation while living sympatrically with their hosts. C1 [Rabeling, Christian; Pierce, Naomi E.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Rabeling, Christian; Pierce, Naomi E.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Schultz, Ted R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Bacci, Mauricio, Jr.] Sao Paulo State Univ, Ctr Study Social Insects, BR-13506900 Rio Claro, SP, Brazil. RP Rabeling, C (reprint author), Univ Rochester, Dept Biol, Rochester, NY 14627 USA. EM crabeling@gmail.com FU Harvard Society; Green and William F. Milton Funds (Harvard); NSF [DEB-0949689, DEB-0431330, IOS-1257543]; Smithsonian Scholarly Studies Program; Smithsonian Restricted Endowments Fund; FAPSP [2011/50226-0]; CNPq [311562/2012-4, 487639/2012-0] FX We thank CNPq, ICMBio, and IBAMA for permission to conduct fieldwork in Brazil. Paul Armstrong and Eugenia Okonski assisted in the laboratory, and Renate Hellmiss improved the figures. Scott Edwards and James Mallet provided stimulating discussions. Three anonymous reviewers and the editor, Florian Maderspacher, significantly improved this manuscript with constructive comments. C.R.'s research was supported by a Junior Fellowship from the Harvard Society of Fellows and the Green and William F. Milton Funds (Harvard). T.R.S. was supported by NSF grants DEB-0949689 and DEB-0431330, the Smithsonian Scholarly Studies Program, and the Smithsonian Restricted Endowments Fund. N.E.P. acknowledges NSF grant IOS-1257543. M.B. received support from FAPSP (2011/50226-0) and CNPq (311562/2012-4 and 487639/2012-0). NR 49 TC 12 Z9 13 U1 1 U2 57 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 SEP 8 PY 2014 VL 24 IS 17 BP 2047 EP 2052 DI 10.1016/j.cub.2014.07.048 PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA AO7OA UT WOS:000341541300031 PM 25155509 ER PT J AU Ijjas, A Steinhardt, PJ Loeb, A AF Ijjas, Anna Steinhardt, Paul J. Loeb, Abraham TI Inflationary schism SO PHYSICS LETTERS B LA English DT Article ID PARADIGM AB Classic inflation, the theory described in textbooks, is based on the idea that, beginning from typical initial conditions and assuming a simple inflaton potential with a minimum of fine-tuning, inflation can create exponentially large volumes of space that are generically homogeneous, isotropic and flat, with nearly scale-invariant spectra of density and gravitational wave fluctuations that are adiabatic, Gaussian and have generic predictable properties. In a recent paper, we showed that, in addition to having certain conceptual problems known for decades, classic inflation is for the first time also disfavored by data, specifically the most recent data from WMAP, ACT and Planck2013. Guth, Kaiser and Nomura and Linde have each recently published critiques of our paper, but, as made clear here, we all agree about one thing: the problematic state of classic inflation. Instead, they describe an alternative inflationary paradigm that revises the assumptions and goals of inflation, and perhaps of science generally. (C) 2014 The Authors. Published by Elsevier B.V. C1 [Ijjas, Anna] Albert Einstein Inst, AMax Planck Inst Gravitat Phys, D-14476 Golm, Germany. [Steinhardt, Paul J.] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. [Steinhardt, Paul J.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Steinhardt, PJ (reprint author), Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. EM steinh@princeton.edu FU U.S. Department of Energy [DE-FG02-91ER40671]; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DBB30A]; John Templeton Foundation FX We thank T. Baker, J.-L. Lehners, J. Pollack, D. Spergel, and C. Steinhardt for comments on the manuscript. This research was partially supported by the U.S. Department of Energy under grant number DE-FG02-91ER40671 (PJS), by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DBB30A (AL). The work of AI is supported in part by a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation (Grant 37433). AI thanks the Physics Department of Princeton University for hospitality while this research was completed. NR 15 TC 20 Z9 20 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 EI 1873-2445 J9 PHYS LETT B JI Phys. Lett. B PD SEP 7 PY 2014 VL 736 BP 142 EP 146 DI 10.1016/j.physletb.2014.07.012 PG 5 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AO6UR UT WOS:000341487800018 ER PT J AU Reasenberg, RD AF Reasenberg, Robert D. TI A new class of equivalence principle test masses, with application to SR-POEM SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article DE weak equivalence principle; sounding rocket; test mass AB We describe a new class of test masses (TMs) for use in a Galilean test of the equivalence principle, principally in space. These TMs have n >= 2 vertical bars that are joined by an off-center connector. A pair of TMs will be positioned to have interleaved bars. For n >= 3, the principal moments of inertia of a TM can be made equal. With their centers of mass aligned, a TM pair shows decreasing susceptibility to differential acceleration from local mass as n increases. For the Sounding Rocket based Principle Of Equivalence Measurement (SR-POEM), the mission requirements are well met with n = 3, but not met with n = 2. For a 1 kg SR-POEM TM, vibration frequencies can be made to be above 1 kHz and thus not interfere with the operation of the TM suspension system. The SR-POEM housing supports electrodes for a set of capacitance gauges that observes all six kinematic degrees of freedom of each TM. C1 Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Reasenberg, RD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM physics@reasenberg.org NR 10 TC 4 Z9 4 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 EI 1361-6382 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD SEP 7 PY 2014 VL 31 IS 17 AR 175013 DI 10.1088/0264-9381/31/17/175013 PG 13 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA AO6TE UT WOS:000341483600013 ER PT J AU Getzin, S Wiegand, T Hubbell, SP AF Getzin, Stephan Wiegand, Thorsten Hubbell, Stephen P. TI Stochastically driven adult - recruit associations of tree species on Barro Colorado Island SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE Berman test; habitat association; life trait; pattern reconstruction; point pattern analysis; segregation ID HABITAT ASSOCIATIONS; SPATIAL-PATTERNS; NEOTROPICAL FOREST; TROPICAL FOREST; POINT PATTERNS; DEPENDENT RECRUITMENT; SEED DISPERSAL; DIVERSITY; DISTRIBUTIONS; MAINTENANCE AB The spatial placement of recruits around adult conspecifics represents the accumulated outcome of several pattern-forming processes and mechanisms such as primary and secondary seed dispersal, habitat associations or Janzen-Connell effects. Studying the adult-recruit relationship should therefore allow the derivation of specific hypotheses on the processes shaping population and community dynamics. We analysed adult-recruit associations for 65 tree species taken from six censuses of the 50 ha neotropical forest plot on Barro Colorado Island (BCI), Panama. We used point pattern analysis to test, at a range of neighbourhood scales, for spatial independence between recruits and adults, to assess the strength and type of departure from independence, and its relationship with species properties. Positive associations expected to prevail due to dispersal limitation occurred only in 16% of all cases; instead a majority of species showed spatial independence (approximate to 73%). Independence described the placement of recruits around conspecific adults in good approximation, although we found weak and noisy signals of species properties related to seed dispersal. We hypothesize that spatial mechanisms with strong stochastic components such as animal seed dispersal overpower the pattern-forming effects of dispersal limitation, density dependence and habitat association, or that some of the pattern-forming processes cancel out each other. C1 [Getzin, Stephan; Wiegand, Thorsten] UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, D-04318 Leipzig, Germany. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Getzin, S (reprint author), UFZ Helmholtz Ctr Environm Res, Dept Ecol Modelling, Permoserstr 15, D-04318 Leipzig, Germany. EM stephan.getzin@ufz.de RI Wiegand, Thorsten/H-5877-2016 OI Wiegand, Thorsten/0000-0002-3721-2248 FU National Science Foundation; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Celera Foundation; ERC [233066] FX The BCI forest dynamics research project was made possible by National Science Foundation grants to S. P. H., support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Celera Foundation and numerous private individuals, and through the hard work of over 100 people from 10 countries over the past decades. The plot project is part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. S.G. and T.W. were supported by ERC advanced grant no. 233066 to T.W. NR 53 TC 10 Z9 10 U1 5 U2 43 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8452 EI 1471-2954 J9 P ROY SOC B-BIOL SCI JI Proc. R. Soc. B-Biol. Sci. PD SEP 7 PY 2014 VL 281 IS 1790 AR 20140922 DI 10.1098/rspb.2014.0922 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AO1RY UT WOS:000341092700012 ER PT J AU Kim, EJ Wolf, M Ortega-Jimenez, VM Cheng, SH Dudley, R AF Kim, Erica J. Wolf, Marta Ortega-Jimenez, Victor Manuel Cheng, Stanley H. Dudley, Robert TI Hovering performance of Anna's hummingbirds (Calypte anna) in ground effect SO JOURNAL OF THE ROYAL SOCIETY INTERFACE LA English DT Article DE ground effect; hovering; induced velocity; metabolic power; vortex wake ID FLIGHT; ENERGETICS; AERODYNAMICS; KINEMATICS; ENERGY; LIMITS; WINGS; ROTOR; BIRDS; TAIL AB Aerodynamic performance and energetic savings for flight in ground effect are theoretically maximized during hovering, but have never been directly measured for flying animals. We evaluated flight kinematics, metabolic rates and induced flow velocities for Anna's hummingbirds hovering at heights (relative to wing length R 5.5 cm) of 0.7R, 0.9R, 1.1R, 1.7R, 2.2R and 8R above a solid surface. Flight at heights less than or equal to 1.1R resulted in significant reductions in the body angle, tail angle, anatomical stroke plane angle, wake-induced velocity, and mechanical and metabolic power expenditures when compared with flight at the control height of 8R. By contrast, stroke plane angle relative to horizontal, wingbeat amplitude and wingbeat frequency were unexpectedly independent of height from ground. Qualitative smoke visualizations suggest that each wing generates a vortex ring during both down-and upstroke. These rings expand upon reaching the ground and present a complex turbulent interaction below the bird's body. Nonetheless, hovering near surfaces results in substantial energetic benefits for hummingbirds, and by inference for all volant taxa that either feed at flowers or otherwise fly close to plant or other surfaces. C1 [Kim, Erica J.] Univ Calif Berkeley, Biophys Grad Program, Berkeley, CA 94720 USA. [Ortega-Jimenez, Victor Manuel; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Cheng, Stanley H.] Univ Calif Berkeley, Dept Mol Cell Biol, Berkeley, CA 94720 USA. [Wolf, Marta] Lund Univ, Dept Biol, Lund, Sweden. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Ortega-Jimenez, VM (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM vortega@berkeley.edu OI Ortega-Jimenez, Victor Manuel/0000-0003-0024-5086 FU NSF Integrative Graduate Education and Research Traineeship (IGERT) from UC Berkeley's Center for Interdisciplinary Biological Inspiration in Education and Research (CiBER); UC University of California MEXUS-CONACYT fellowship; Swedish Research Council FX E.J.K. was supported by an NSF Integrative Graduate Education and Research Traineeship (IGERT) from UC Berkeley's Center for Interdisciplinary Biological Inspiration in Education and Research (CiBER), V.M.O.-J. was supported by a UC University of California MEXUS-CONACYT fellowship, and M. W. was supported by the Swedish Research Council. Animal care and experimental protocols were approved by the UC Berkeley Institutional Animal Care and Use Committee (IACUC). NR 43 TC 5 Z9 5 U1 2 U2 17 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1742-5689 EI 1742-5662 J9 J R SOC INTERFACE JI J. R. Soc. Interface PD SEP 6 PY 2014 VL 11 IS 98 AR 20140505 DI 10.1098/rsif.2014.0505 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AK6DW UT WOS:000338519300014 PM 24990291 ER PT J AU Xie, HY Cunningham, SA Yeates, DK Thompson, FC AF Xie, Hongyan Cunningham, Saul A. Yeates, David K. Thompson, F. Christian TI A new sericomyiine flower fly from China (Diptera: Syrphidae) SO ZOOTAXA LA English DT Article DE Taxonomy; Sericomyiina; new species; identification key AB A new species of flower flies is described from China (Sichuan & Yunnan: Hengduan Mountains), Sericomyia khamensis Thompson & Xie). A key is provided to the species of the subtribe Sericomyiina found in China along with nomenclatural and taxonomical notes on them. C1 [Xie, Hongyan] Australian Natl Univ, Sch Bot & Zool, Canberra, ACT 0200, Australia. [Cunningham, Saul A.; Yeates, David K.] CSIRO, Black Mt Labs, Ecosyst Sci, Canberra, ACT 2601, Australia. [Thompson, F. Christian] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Thompson, FC (reprint author), Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20560 USA. EM thompsonf@si.edu RI Cunningham, Saul/B-9947-2009; Yeates, David/A-9917-2008 OI Cunningham, Saul/0000-0003-0703-6893; Yeates, David/0000-0001-7729-6143 NR 27 TC 0 Z9 0 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD SEP 3 PY 2014 VL 3860 IS 1 BP 81 EP 86 PG 6 WC Zoology SC Zoology GA AO2RV UT WOS:000341174000004 PM 25283191 ER PT J AU Jew, NP Rick, TC AF Jew, Nicholas P. Rick, Torben C. TI Understanding the Occupation of Small Continental Islands: Seasonality and delta O-18 Evidence From Anacapa Island, California SO JOURNAL OF ISLAND & COASTAL ARCHAEOLOGY LA English DT Article DE stable isotopes; hunter-gatherer settlement; sea surface temperature; Channel Islands ID MIDDEN; SHELLS C1 [Jew, Nicholas P.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. RP Jew, NP (reprint author), Univ Oregon, Dept Anthropol, 308 Condon Hall 1218, Eugene, OR 97403 USA. EM njew@uoregon.edu NR 19 TC 4 Z9 4 U1 0 U2 1 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 1556-4894 EI 1556-1828 J9 J ISL COAST ARCHAEOL JI J. Isl. Coast. Archaeol. PD SEP 2 PY 2014 VL 9 IS 3 BP 430 EP 435 DI 10.1080/15564894.2013.861547 PG 6 WC Archaeology SC Archaeology GA AT0UY UT WOS:000344651400008 ER PT J AU Caldas, A AF Caldas, Astrid TI SPECIES TRAITS OF RELEVANCE FOR CLIMATE VULNERABILITY AND THE PREDICTION OF PHENOLOGICAL RESPONSES TO CLIMATE CHANGE SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE climate change; conservation planning; Lepidoptera; flight phenology; ecological traits ID BUTTERFLIES; EXTINCTIONS; INSECTS; SHIFTS; CO2 AB In many ways, known and unknown, climate change will affect species' distributions, life cycles, phenologies, and ultimately survival. Lepidoptera are among the organisms that have been shown to be strongly impacted by climate change, and their conservation presents challenges that are both unique and unprecedented. Various studies have sought to determine what ecological and life traits of Lepidoptera influence species' responses to climate change, and here I review the few studies that evaluate such responses over a long period of time for a large number of species for common associations. Species with wider geographic distribution and less habitat specificity are generally considered less vulnerable to climate change, while those with opposite traits are deemed more vulnerable. The latter are more likely to change their phenology in response to climate change. Larval diet breadth and composition, overwintering stage, and adult activity period appear to be consistent predictors of changes in flight phenology. The knowledge of these traits for species of concern allows us to assess the implications of the possible phenological changes, and decide what can be done about those changes. Determining how phenological changes may affect current management or conservation practices and defining actions and priorities can be crucial for the success of a conservation plan. C1 [Caldas, Astrid] Defenders Wildlife, Washington, DC 20036 USA. [Caldas, Astrid] Smithsonian Inst, Washington, DC 20013 USA. RP Caldas, A (reprint author), Defenders Wildlife, 1130 17th St NW, Washington, DC 20036 USA. EM astridcaldas@yahoo.com NR 32 TC 1 Z9 1 U1 6 U2 36 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 SEP 2 PY 2014 VL 68 IS 3 BP 197 EP 202 PG 6 WC Entomology SC Entomology GA AO9KM UT WOS:000341674600007 ER PT J AU Marcy, GW Weiss, LM Petigura, EA Isaacson, H Howard, AW Buchhave, LA AF Marcy, Geoffrey W. Weiss, Lauren M. Petigura, Erik A. Isaacson, Howard Howard, Andrew W. Buchhave, Lars A. TI Occurrence and core-envelope structure of 1-4x Earth-size planets around Sun-like stars SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE extrasolar planets; astrobiology; SETI ID MASS-RADIUS RELATIONSHIPS; SOLAR-TYPE STARS; IN SUPER-EARTHS; M-DWARF; TRANSITING PLANETS; SOLID EXOPLANETS; BULK COMPOSITION; HOT NEPTUNE; GJ 436; DENSITY AB Small planets, 1-4x the size of Earth, are extremely common around Sun-like stars, and surprisingly so, as they are missing in our solar system. Recent detections have yielded enough information about this class of exoplanets to begin characterizing their occurrence rates, orbits, masses, densities, and internal structures. The Kepler mission finds the smallest planets to be most common, as 26% of Sun-like stars have small, 1-2 R-circle plus planets with orbital periods under 100 d, and 11% have 1-2 R-circle plus planets that receive 1-4x the incident stellar flux that warms our Earth. These Earth-size planets are sprinkled uniformly with orbital distance (logarithmically) out to 0.4 the Earth-Sun distance, and probably beyond. Mass measurements for 33 transiting planets of 1-4 R-circle plus show that the smallest of them, R < 1.5 R., have the density expected for rocky planets. Their densities increase with increasing radius, likely caused by gravitational compression. Including solar system planets yields a relation: rho = 2.32 + 3.19R/R-circle plus [g cm(-3)]. Larger planets, in the radius range 1.5-4.0 R-circle plus, have densities that decline with increasing radius, revealing increasing amounts of low-density material (H and He or ices) in an envelope surrounding a rocky core, befitting the appellation "mini-Neptunes.'' The gas giant planets occur preferentially around stars that are rich in heavy elements, while rocky planets occur around stars having a range of heavy element abundances. Defining habitable zones remains difficult, without benefit of either detections of life elsewhere or an understanding of life's biochemical origins. C1 [Marcy, Geoffrey W.; Weiss, Lauren M.; Petigura, Erik A.; Isaacson, Howard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Howard, Andrew W.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Buchhave, Lars A.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marcy, GW (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM gmarcy@berkeley.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Weiss, Lauren/0000-0002-3725-3058 FU NASA Science Mission Directorate; W. M. Keck Foundation; NSF [DGE 1106400] FX We thank Leslie Rogers, Eric Lopez, Jonathan Fortney, Dimitar Sasselov, Jack Lissauer, Eugene Chiang, Greg Laughlin, and Sara Seager for valuable conversations. We thank the many observers who contributed to the measurements reported here. The authors wish to extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. We thank the extraordinary group of engineers and scientists who worked tirelessly to produce the Kepler mission. Kepler was competitively selected as the tenth NASA Discovery mission. Funding for this mission is provided by the NASA Science Mission Directorate. 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 Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We thank the NSF Graduate Research Fellowship, Grant DGE 1106400. 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 69 TC 29 Z9 29 U1 1 U2 18 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 SEP 2 PY 2014 VL 111 IS 35 BP 12655 EP 12660 DI 10.1073/pnas.1304197111 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO3LN UT WOS:000341230800040 PM 24912169 ER PT J AU Treanor, V AF Treanor, Virginia TI "Une abondance extra ordinaire": The Porcelain Collection of Amalia van Solms SO EARLY MODERN WOMEN-AN INTERDISCIPLINARY JOURNAL LA English DT Article C1 [Treanor, Virginia] Natl Museum Women Arts, Washington, DC 20005 USA. [Treanor, Virginia] Smithsonian Amer Art Museum, Washington, DC USA. [Treanor, Virginia] Natl Gallery Art, Washington, DC 20565 USA. RP Treanor, V (reprint author), Natl Museum Women Arts, Washington, DC 20005 USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU UNIV MARYLAND-CTR RENAISSANCE & BAROQUE STUD PI COLLEGE PARK PA UNIV MARYLAND, 0139 TALIAFERRO HALL, COLLEGE PARK, MD 20742 USA SN 1933-0065 J9 EARLY MOD WOMEN JI Early Mod. Women PD FAL PY 2014 VL 9 IS 1 BP 141 EP 154 PG 14 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA CB3FL UT WOS:000349513500010 ER PT J AU Wong, RKW Baines, P Aue, A Lee, TCM Kashyap, VL AF Wong, Raymond K. W. Baines, Paul Aue, Alexander Lee, Thomas C. M. Kashyap, Vinay L. TI AUTOMATIC ESTIMATION OF FLUX DISTRIBUTIONS OF ASTROPHYSICAL SOURCE POPULATIONS SO ANNALS OF APPLIED STATISTICS LA English DT Article DE Broken power law; CDFN X-ray survey; interwoven EM algorithm; likelihood computations; logN-log S; Pareto distribution ID N-LOG S; X-RAY; MAXIMUM-LIKELIHOOD; NUMBER; CLUSTERS; CHANDRA AB In astrophysics a common goal is to infer the flux distribution of populations of scientifically interesting objects such as pulsars or supernovae. In practice, inference for the flux distribution is often conducted using the cumulative distribution of the number of sources detected at a given sensitivity. The resulting "log(N > S)-log(S)" relationship can be used to compare and evaluate theoretical models for source populations and their evolution. Under restrictive assumptions the relationship should be linear. In practice, however, when simple theoretical models fail, it is common for astrophysicists to use prespecified piecewise linear models. This paper proposes a methodology for estimating both the number and locations of "breakpoints" in astrophysical source populations that extends beyond existing work in this field. An important component of the proposed methodology is a new interwoven EMalgorithm that computes parameter estimates. It is shown that in simple settings such estimates are asymptotically consistent despite the complex nature of the parameter space. Through simulation studies it is demonstrated that the proposed methodology is capable of accurately detecting structural breaks in a variety of parameter configurations. This paper concludes with an application of our methodology to the Chandra Deep Field North (CDFN) data set. C1 [Wong, Raymond K. W.; Baines, Paul; Aue, Alexander; Lee, Thomas C. M.] Univ Calif Davis, Dept Stat, Davis, CA 95616 USA. [Kashyap, Vinay L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wong, RKW (reprint author), Univ Calif Davis, Dept Stat, 4118 Math Sci Bldg,One Shields Ave, Davis, CA 95616 USA. EM rkwwong@ucdavis.edu; pdbaines@ucdavis.edu; aaue@ucdavis.edu; tcmlee@ucdavis.edu; kashyap@head.cfa.harvard.edu FU NSF [1209226, 1305858, 1007520, 1209232]; NASA [NAS8-03060] FX Supported in part by NSF Grants 1209226 and 1305858.; Supported in part by NSF Grants 1007520, 1209226 and 1209232.; Supported in part by NASA Contract NAS8-03060 to the Chandra X-Ray Center. NR 26 TC 0 Z9 0 U1 0 U2 0 PU INST MATHEMATICAL STATISTICS PI CLEVELAND PA 3163 SOMERSET DR, CLEVELAND, OH 44122 USA SN 1932-6157 J9 ANN APPL STAT JI Ann. Appl. Stat. PD SEP PY 2014 VL 8 IS 3 BP 1690 EP 1712 DI 10.1214/14-AOAS750 PG 23 WC Statistics & Probability SC Mathematics GA AY4DW UT WOS:000347529300017 ER PT J AU Strahan, D Tsukada, M AF Strahan, Donna Tsukada, Masahiko TI Measuring mercury emissions from cinnabar lacquer objects SO STUDIES IN CONSERVATION LA English DT Article; Proceedings Paper CT 25th Biennial IIC International Congress on An Unbroken History - Conserving East Asian Works of Art and Heritage CY 2014 CL Hong Kong, PEOPLES R CHINA SP IIC DE Mercury; Cinnabar; Lacquer; Handling; Health and safety ID HERBARIUM C1 [Strahan, Donna] Smithsonian Inst, Freer Gallery Art, Washington, DC 20560 USA. [Strahan, Donna] Smithsonian Inst, Arthur M Sackler Gallery, Washington, DC 20560 USA. [Tsukada, Masahiko] Metropolitan Museum Art, New York, NY 10028 USA. RP Strahan, D (reprint author), Freer Gallery Art, Dept Conservat & Sci Res, POB 37012,MRC 707, Washington, DC 20013 USA. EM StrahanD@si.edu NR 4 TC 1 Z9 1 U1 1 U2 4 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0039-3630 EI 2047-0584 J9 STUD CONSERV JI Stud. Conserv. PD SEP PY 2014 VL 59 SU 1 BP S137 EP S140 DI 10.1179/204705814X13975704318759 PG 4 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA AW3AB UT WOS:000346156600039 ER PT J AU Tsang, J Madruga, I Williams, D Bosworth, J Hogge, D AF Tsang, Jiasun Madruga, Ines Williams, Don Bosworth, Jenifer Hogge, David TI Conservation of an oil portrait of the Empress Dowager Tze Hsi of China SO STUDIES IN CONSERVATION LA English DT Article; Proceedings Paper CT 25th Biennial IIC International Congress on An Unbroken History - Conserving East Asian Works of Art and Heritage CY 2014 CL Hong Kong, PEOPLES R CHINA SP IIC DE Drying cracks; Empress Dowager of China; Infrared reflectography; Large-scale conservation; Pentimenti C1 [Tsang, Jiasun; Madruga, Ines; Williams, Don; Bosworth, Jenifer; Hogge, David] Smithsonian Inst, Washington, DC 20560 USA. RP Tsang, J (reprint author), Museum Conservat Inst, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM Tsangj@si.edu NR 1 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 0039-3630 EI 2047-0584 J9 STUD CONSERV JI Stud. Conserv. PD SEP PY 2014 VL 59 SU 1 BP S157 EP S160 DI 10.1179/204705814X13975704318957 PG 4 WC Archaeology; Art; Chemistry, Applied; Chemistry, Analytical; Spectroscopy SC Archaeology; Art; Chemistry; Spectroscopy GA AW3AB UT WOS:000346156600044 ER PT J AU Aze, T Pearson, PN Dickson, AJ Badger, MPS Bown, PR Pancost, RD Gibbs, SJ Huber, BT Leng, MJ Coe, AL Cohen, AS Foster, GL AF Aze, T. Pearson, P. N. Dickson, A. J. Badger, M. P. S. Bown, P. R. Pancost, R. D. Gibbs, S. J. Huber, B. T. Leng, M. J. Coe, A. L. Cohen, A. S. Foster, G. L. TI Extreme warming of tropical waters during the Paleocene-Eocene Thermal Maximum SO GEOLOGY LA English DT Article ID PLANKTONIC-FORAMINIFERA; TANZANIA; CARBON; PALEOGENE; RECORDS; OCEAN; ACIDIFICATION; EVOLUTION AB The Paleocene-Eocene Thermal Maximum (PETM), ca. 56 Ma, was a major global environmental perturbation attributed to a rapid rise in the concentration of greenhouse gases in the atmosphere. Geochemical records of tropical sea-surface temperatures (SSTs) from the PETM are rare and are typically affected by post-depositional diagenesis. To circumvent this issue, we have analyzed oxygen isotope ratios (delta O-18) of single specimens of exceptionally well-preserved planktonic foraminifera from the PETM in Tanzania (similar to 19 degrees S paleolatitude), which yield extremely low delta O-18, down to <-5%. After accounting for changes in seawater chemistry and pH, we estimate from the foraminifer delta O-18 that tropical SSTs rose by >3 degrees C during the PETM and may have exceeded 40 degrees C. Calcareous plankton are absent from a large part of the Tanzania PETM record; extreme environmental change may have temporarily caused foraminiferal exclusion. C1 [Aze, T.; Pearson, P. N.] Cardiff Univ, Sch Earth & Ocean Sci, Cardiff CF10 3AT, S Glam, Wales. [Aze, T.] Univ Oxford, Museum Nat Hist, Oxford OX1 3PW, England. [Dickson, A. J.; Coe, A. L.; Cohen, A. S.] Open Univ, Dept Environm Earth & Ecosyst, Milton Keynes MK7 6AA, Bucks, England. [Badger, M. P. S.; Pancost, R. D.] Univ Bristol, Sch Chem, Cabot Inst, Organ Geochem Unit, Bristol BS8 1TS, Avon, England. [Bown, P. R.] UCL, Dept Earth Sci, London WC1E 6BT, England. [Gibbs, S. J.; Foster, G. L.] Univ Southampton, Natl Oceanog Ctr, Southampton SO14 3ZH, Hants, England. [Huber, B. T.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Leng, M. J.] Univ Nottingham, Sch Geog, Ctr Environm Geochem, Nottingham NH7 2RD, England. [Leng, M. J.] British Geol Survey, NERC Isotope Geosci Facil, Nottingham NG12 5GG, England. RP Aze, T (reprint author), Cardiff Univ, Sch Earth & Ocean Sci, Cardiff CF10 3AT, S Glam, Wales. EM tracy.aze@oum.ox.ac.uk RI Badger, Marcus/A-3607-2014; Pearson, Paul/B-2276-2009; OI Badger, Marcus/0000-0001-8195-5244; Pearson, Paul/0000-0003-4628-9818; Bown, Paul/0000-0001-6777-4463 FU DEFRA Ocean Acidification Programme; Natural Environment Research Council (NERC) [IP-12751111]; NERC [NE/F021313/1] FX Aze and Pearson were supported by the DEFRA Ocean Acidification Programme and the Natural Environment Research Council (NERC; grant IP-12751111). Dickson, Cohen, and Coe were supported by NERC grant NE/F021313/1. We thank A. Kuhl of the NERC Life Sciences Mass Spectrometry Facility for assistance with delta13Calk. Badger and Pancost were supported by NERC. NR 28 TC 11 Z9 11 U1 8 U2 39 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 SEP PY 2014 VL 42 IS 9 BP 739 EP 742 DI 10.1130/G35637.1 PG 4 WC Geology SC Geology GA AU1DU UT WOS:000345362100001 ER PT J AU Beran, F Geiselhardt, S Vargas, G Windsor, DM AF Beran, Franziska Geiselhardt, Sven Vargas, Gloria Windsor, Donald M. TI Cuticular Extracts from Acromis sparsa (Coleoptera: Cassidinae) Mediate Arrestment Behavior of the Commensal Canestriniid Mite Grandiella rugosita SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Cassidinae; Canestriniidae; Cuticular hydrocarbons; Host recognition ID APIS-MELLIFERA; LEPTINOTARSA-DECEMLINEATA; VARROA-JACOBSONI; TOBACCO HORNWORM; ACARAPIS-WOODI; MASS-SPECTRA; HONEY-BEES; HYDROCARBONS; HOST; BEETLE AB Astigmatid mites in the family Canestriniidae are often closely associated with tortoise leaf beetles (Chrysomelidae: Cassidinae). For example, the survival of the commensal canestriniid mite Grandiella rugosita depends on dispersal to the cassidine beetle Acromis sparsa. Here, we tested whether the beetle cuticle provides chemical cues for host recognition for G. rugosita. In two-choice assays with cuticular extracts from A. sparsa and the co-occurring, non-host cassidine Chelymorpha alternans offered simultaneously, mites clearly preferred the area treated with extract from their host. In no-choice assays, G. rugosita spent three times longer and moved three times slower on host cuticular extracts compared to non-host extracts and the solvent control. Analyses of the chemical composition of cuticular extracts from males and females of A. sparsa and C. alternans revealed complex mixtures of mainly methyl branched hydrocarbons, which clearly separated both species in a principal component analysis. We found no qualitative difference between males and females of either species, but in C. alternans quantitative differences between males and females were detected. Our results demonstrate that G. rugosita is able to discriminate between cuticular extracts from its host A. sparsa and the non-host C. alternans. The components eliciting the observed arrestment behavior remain to be determined. C1 [Beran, Franziska] Max Planck Inst Chem Ecol, Dept Entomol, D-07745 Jena, Germany. [Geiselhardt, Sven] Free Univ Berlin, Inst Biol, D-12163 Berlin, Germany. [Vargas, Gloria; Windsor, Donald M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Beran, F (reprint author), Max Planck Inst Chem Ecol, Dept Entomol, Hans Knoell Str 8, D-07745 Jena, Germany. EM fberan@ice.mpg.de RI Beran, Franziska/M-6163-2014; OI Geiselhardt, Sven/0000-0001-9058-8589 FU Smithsonian Tropical Research Institute; Freie Universitat Berlin FX We thank the Smithsonian Tropical Research Institute and Freie Universitat Berlin for financial support of this work. Franziska Beran is grateful for the Short Term Fellowship awarded from the Smithsonian Tropical Research Institute in 2011. NR 29 TC 1 Z9 1 U1 4 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 EI 1573-1561 J9 J CHEM ECOL JI J. Chem. Ecol. PD SEP PY 2014 VL 40 IS 9 BP 996 EP 1002 DI 10.1007/s10886-014-0494-1 PG 7 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA AU1PA UT WOS:000345391400005 PM 25224678 ER PT J AU de Sa, RO Grant, T Camargo, A Heyer, WR Ponssa, ML Stanley, E AF de Sa, Rafael O. Grant, Taran Camargo, Arley Heyer, W. Ronald Ponssa, Maria L. Stanley, Edward TI Systematics of the Neotropical Genus Leptodactylus Fitzinger, 1826 (Anura: Leptodactylidae): Phylogeny, the Relevance of Non-molecular Evidence, and Species Accounts SO SOUTH AMERICAN JOURNAL OF HERPETOLOGY LA English DT Article DE Behavior; Distribution; Life history; Morphology; Taxonomy; Vocalization ID MULTIPLE-SEQUENCE ALIGNMENT; WHITE-LIPPED FROG; FOAM-GENERATING BEHAVIOR; NATURAL-HISTORY NOTES; AMAZON RAIN-FOREST; MALE PARENTAL CARE; ADVERTISEMENT CALLS; ANTIMICROBIAL PEPTIDE; REPRODUCTIVE MODES; FUSCUS TADPOLES AB A phylogeny of the species-rich clade of the Neotropical frog genus Leptodactylus sensu stricto is presented on the basis of a total evidence analysis of molecular (mitochondrial and nuclear markers) and non-molecular (adult and larval morphological and behavioral characters) sampled from > 80% of the 75 currently recognized species. Our results support the monophyly of Leptodactylus sensu stricto, with Hydrolaetare placed as its sister group. The reciprocal monophyly of Hydrolaetare and Leptodactylus sensu stricto does not require that we consider Hydrolaetare as either a subgenus or synonym of Leptodactylus sensu lato. We recognize Leptodactylus sensu stricto, Hydrolaetare, Adenomera, and Lithodytes as valid monophyletic genera. Our results generally support the traditionally recognized Leptodactylus species groups, with exceptions involving only a few species that are easily accommodated without proposing new groups or significantly altering contents. The four groups form a pectinate tree, with the Leptodactylus fuscus group diverging first, followed by the L. pentadactylus group, which is sister to the L. latrans and L. melanonotus groups. To evaluate the impact of non-molecular evidence on our results, we compared our total evidence results with results obtained from analyses using only molecular data. Although non-molecular evidence comprised only 3.5% of the total evidence matrix, it had a strong impact on our total evidence results. Only one species group was monophyletic in the molecular-only analysis, and support differed in 86% of the 54 Leptodactylus clades that are shared by the results of the two analyses. Even though no non-molecular evidence was included for Hydrolaetare, exclusion of that data partition resulted in that genus being nested within Leptodactylus, demonstrating that the inclusion of a small amount of non-molecular evidence for a subset of species can alter not only the placement of those species, but also species that were not scored for those data. The evolution of several natural history and reproductive traits is considered in the light of our phylogenic framework. Invasion of rocky outcrops, larval oophagy, and use of underground reproductive chambers are restricted to species of the Leptodactylus fuscus and L. pentadactylus groups. In contrast, larval schooling, larval attendance, and more complex parental care are restricted to the L. latrans and L. melanonotus groups. Construction of foam nests is plesiomorphic in Leptodactylus but their placement varies extensively (e.g., underground chambers, surface of waterbodies, natural or excavated basins). Information on species synonymy, etymology, adult and larval morphology, advertisement call, and geographic distribution is summarized in species accounts for the 30 species of the Leptodactylus fuscus group, 17 species of the L. pentadactylus group, eight species of the L. latrans group, and 17 species of the L. melanonotus group, as well as the three species that are currently unassigned to any species group. C1 [de Sa, Rafael O.; Camargo, Arley; Stanley, Edward] Univ Richmond, Dept Biol, Richmond, VA 23173 USA. [Grant, Taran] Univ Sao Paulo, Inst Biociencias, Dept Zool, BR-05508090 Sao Paulo, Brazil. [Heyer, W. Ronald] Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. [Ponssa, Maria L.] Fdn Miguel Lillo, San Miguel De Tucuman, Tucuman, Argentina. [Stanley, Edward] Calif Acad Sci, San Francisco, CA 94118 USA. RP de Sa, RO (reprint author), Univ Richmond, Dept Biol, Richmond, VA 23173 USA. EM rdesa@richmond.edu; taran.grant@gmail.com; arley.camargo@gmail.com; heyerr@si.edu; mlponssa@hotmail.com; EStanley@calacademy.org RI Grant, Taran/B-7703-2012; OI Grant, Taran/0000-0003-1726-999X; Stanley, Edward/0000-0001-5257-037X FU Collection Study Grant (AMNH); Ernst Mayr Grant (MCZ); Short-Term Visitor Program (SI) [PICT 2008-578]; NSF-DEB Award [DEB0342918, 1144692]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico [307001/2011-3]; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo [2012/10000-5] FX We thank the following individuals and institutions for the loan of specimens, tissue samples, contribution to field work, and/or providing working space at their collections: Reuber Brandao (UnB, Brazil), Janalee P. Caldwell (OSM, USA), Marta Canepa (FML, Argentina), Ulisses Caramaschi (MNRJ, Brazil), Gustavo Carrizo (MACN, Argentina), Carolina Castro Mello (MZUSP, Brazil), Charles Cole (AMNH, USA), Guarino Colli (UnB, Brazil), Luis Coloma (QCAZ, Ecuador), Celso Morato de Carvalho (INPA, Brazil), Ignacio De la Riva (MNCN, Spain), Marcos Di Bernardo (MCP, Brazil), Maureen Donnelly (FIU, USA), J. Faivovich (MACN, Argentina), C.F.B. Haddad (UNESP, Rio Claro, Brazil), James Hanken (MCZ, USA), David Kizirian (AMNH, USA), Sonia Kretzschmann (FML, Argentina), Esteban Lavilla (FML, Argentina), Jose Langone (MNHH, Uruguay), John D. Lynch (ICN, Colombia), Raul Maneyro (FC, Uruguay), Robert Murphy (ROM, Canada), Jose M. Padial (Carniege Museum, USA), Jose Pombal Jr. (MNRJ, Brazil), Ana Prudente (MPEG, Brazil), Steffen Reichle (Bolivia), Jose Rosado (MCZ, USA), Magno Segalla (Brazil), Miguel Trefaut Rodrigues (USP, Brazil), Linda Trueb (KU, USA), James I. Watling (FIU, USA), Jorge Williams (MLP, Argentina), and Hussam Zaher (MZUSP, Brazil). We also thank the individuals and MZUSP (listed in the plates and back of front cover) who generously provided color photos of species of Leptodactylus. Denis Jacob Machado, Luis Lieu, Hussam Zaher, and the MZUSP Board of Directors were instrumental in installing and running the high-performance computer cluster Ace. Maria L. Ponssa ackowledges support from Collection Study Grant (AMNH), Ernst Mayr Grant (MCZ), and Short-Term Visitor Program (SI), PICT 2008-578. Contributions to this work by Arley Camargo, Maria L. Ponssa, Edward Stanley, and Miriam H. Heyer (who assisted with published data on Leptodactylus) were supported under NSF-DEB Award DEB0342918. Taran Grant was supported by Conselho Nacional de Desenvolvimento Cientifico e Tecnologico Proc. 307001/2011-3 and Fundacao de Amparo a Pesquisa do Estado de Sao Paulo Proc. 2012/10000-5. This manuscript was completed under NSF-DEB award 1144692 to Rafael O. de Sa. NR 500 TC 18 Z9 19 U1 1 U2 8 PU SOC BRASILEIRA HERPETOLOGIA PI SAO PAULO PA C/O HUSSAM ZAHER, RECEIVING EDITOR, MUSEU ZOOLOGIA UNIV SAO PAULO, AVENIDA NAZARE, 481 IPIRANGA, SAO PAULO, SP 04263-000, BRAZIL SN 1808-9798 J9 S AM J HERPETOL JI South Am. J. Herpetol. PD SEP PY 2014 VL 9 SI 1 BP S1 EP S128 DI 10.2994/SAJH-D-13-00022.1 PG 128 WC Zoology SC Zoology GA AT9ZS UT WOS:000345283500001 ER PT J AU Gingerich, O AF Gingerich, Owen TI THE COPERNICUS COMPLEX Our Cosmic Significance in a Universe of Planets and Probabilities SO AMERICAN SCHOLAR LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU PHI BETA KAPPA SOC PI WASHINGTON PA 1785 MASSACHUSETTS AVENUE, N W FOURTH FL,, WASHINGTON, DC 20036 USA SN 0003-0937 EI 2162-2892 J9 AM SCHOLAR JI Am. Sch. PD FAL PY 2014 VL 83 IS 4 BP 108 EP 109 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA AS3ZU UT WOS:000344214300036 ER PT J AU Vergara-Asenjo, G Potvin, C AF Vergara-Asenjo, Gerardo Potvin, Catherine TI Forest protection and tenure status: The key role of indigenous peoples and protected areas in Panama SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS LA English DT Article DE Land tenure; Deforestation; Protected areas; Indigenous peoples; REDD ID TROPICAL DEFORESTATION; REDUCING EMISSIONS; REDD; MULTIVARIATE; LOCATION; IMPACTS; PARKS; BIAS AB Using recent land cover maps, we used matching techniques to analyze forest cover and assess effectiveness in avoiding deforestation in three main land tenure regimes in Panama, namely protected areas, indigenous territories and non-protected areas. We found that the tenure status of protected areas and indigenous territories (including comarcas and claimed lands) explains a higher rate of success in avoided deforestation than other land tenure categories, when controlling for covariate variables such us distance to roads, distance to towns, slope, and elevation. In 2008 protected areas and indigenous territories had the highest percentage of forest cover and together they hosted 77% of Panama's total mature forest area. Our study shows the promises of matching techniques as a potential tool for demonstrating and quantifying conservation efforts. We therefore propose that matching could be integrated to methodological approaches allowing compensating forests' protectors. Because conserving forest carbon stocks in forested areas of developing countries is an essential component of REDD+ and its future success, the discussion of our results is relevant to countries or jurisdictions with high forest cover and low deforestation rates. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Vergara-Asenjo, Gerardo; Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Vergara-Asenjo, Gerardo] Forest Res Inst INFOR, Santiago, Chile. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Panama. RP Vergara-Asenjo, G (reprint author), McGill Univ, Dept Biol, 1205 Doctor Penfield Ave, Montreal, PQ H3A 1B1, Canada. EM gerardo.vergaraasenjo@mail.mcgill.ca FU David and Lucile Packard Foundation (Los Altos, CA, USA); Global Environmental and Climate Change Centre (GEC3, Montreal, QC, Canada); Ford Foundation International Fellowship Program [15082258] FX We appreciate the valuable collaboration of Mr. German Hernandez in collecting information from COONAPIP, together with all of the regional and traditional indigenous authorities in Panama who authorized and participated in this study. We are grateful to Panamanian governmental institutions, such as ANAM and PRONAT, for facilitating access to information and data. This study was supported by the David and Lucile Packard Foundation (Los Altos, CA, USA), and the Global Environmental and Climate Change Centre (GEC3, Montreal, QC, Canada). We also thank the Ford Foundation International Fellowship Program Grant Number 15082258 for funding Gerardo Vergara. We also express our gratitude to three anomimous referees for their valuable reviews and contributions, and to Aerin Jacob (McGill University), Sebastien Jodoin (Yale University) and Dr. William F.J. Parsons (Centre d'etude de la foret) for their useful comments and review of this document. NR 79 TC 8 Z9 8 U1 3 U2 33 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0959-3780 EI 1872-9495 J9 GLOBAL ENVIRON CHANG JI Glob. Environ. Change-Human Policy Dimens. PD SEP PY 2014 VL 28 BP 205 EP 215 DI 10.1016/j.gloenvcha.2014.07.002 PG 11 WC Environmental Sciences; Environmental Studies; Geography SC Environmental Sciences & Ecology; Geography GA AR8QG UT WOS:000343839100018 ER PT J AU Steinberg, M AF Steinberg, Monica TI Incongruent Humor, Labor, and Public Fame in Postwar Los Angeles SO ARCHIVES OF AMERICAN ART JOURNAL LA English DT Article C1 [Steinberg, Monica] CUNY, Grad Ctr, New York, NY 10016 USA. [Steinberg, Monica] Smithsonian Inst, Washington, DC 20560 USA. RP Steinberg, M (reprint author), CUNY, Grad Ctr, New York, NY 10016 USA. NR 34 TC 0 Z9 0 U1 0 U2 1 PU SMITHSONIAN INST, ARCHIVES AMER ART PI NEW YORK PA 1285 AVE OF THE AMERICAS, LOBBY LEVEL, NEW YORK, NY 10019 USA SN 0003-9853 EI 2327-0667 J9 ARCH AM ART J JI Arch. Am. Art J. PD FAL PY 2014 VL 53 IS 1-2 BP 4 EP 29 PG 26 WC Art SC Art GA AR2DF UT WOS:000343393100002 ER PT J AU Aleksic, J Ansoldi, S Antonelli, LA Antoranz, P Babic, A Bangale, P de Almeida, UB Barrio, JA Gonzalez, JB Bednarek, W Bernardini, E Biland, A Blanch, O Bonnefoy, S Bonnoli, G Borracci, F Bratz, T Carmona, E Carosi, A Fidalgo, DC Colin, P Colombo, E Contreras, JL Cortina, I Covino, S Da Vela, P Dazzi, F De Angelis, A De Caneva, G De Lotto, B Mendez, CD Doert, M Dominguez, A Presters, DD Dorner, D Doro, M Einecke, S Eisenacher, D Elsaesser, D Farina, E Ferenc, D Fonseca, MV Font, L Frantzen, K Fruck, C Lopez, RJG Garczarczyk, M Terrats, DG Gaug, M Godinovic, N Munoz, AG Gozzini, SR Hadasch, D Hayashida, M Herrera, J Herrero, A Hildebrand, D Hose, J Hrupec, D Idec, W Kadenius, V Kellermann, H 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 Mallotw, K Maneva, G Mankuzhiyil, N Mannheim, K Maraschi, L Marcote, B Mariotti, M Martinez, M Mazin, D Menzel, U Meucci, M Miranda, JM Mirzoyan, R Moralejo, A Munar-Adrover, P Nakajima, D Niedzwiecki, A Nilsson, K Nishijima, K Noda, K Nowak, N Orito, R Overkemping, A Paiano, S Palatiello, M Paneque, D Paoletti, R Paredes, JM Paredes-Fortuny, X Partini, S Persic, M Prada, F Moroni, PGP Prandini, E Preziuso, S Puljak, I Reinthal, R Rhode, W Ribo, M Rico, J Garcia, JR Rugamer, S Saggion, A Saito, T Saito, K Satalecka, K Scalzotto, V Scapin, V Schultz, C Schweizer, T Shore, SN Sillanpaa, A Sitarek, J Snidaric, I Sobczynska, D Spanier, F Stamatescu, V Stamerra, A Steinbring, T Storz, J Strzys, M Sun, S Suric, T 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 Wagner, RM Zandanel, F Zanin, R Lucarelli, F Pittori, C Vercellone, S Verrecchia, F Buson, S D'Ammando, F Stawarz, L Giroletti, M Orienti, M Mundell, C Steele, I Zarpudin, B Raiteri, CM Villata, M Sandrinelli, A Lahteenmaki, A Tammi, J Tornikoski, M Hovatta, T Readhead, ACS Max-Moerbeck, W Richards, JL Jorstad, S Marscher, A Gurwell, MA Larionov, VM Blinov, DA Konstantinova, TS Kopatskaya, EN Larionova, LV Earionova, EG Morozova, DA Troitky, IS Mokrushina, AA Pavlova, YV Chen, WP Lin, HC Panwar, N Agudo, I Casadio, C Gomez, JL Molina, SN Kurtanidze, OM Nikolashvili, MG Kurtanidze, SO Chigladze, RA Acosta-Pulido, JA Carnerero, MI Manilla-Robles, A Ovcharov, E Bozhilov, V Metodieva, I Aller, MF Aller, HD Fuhrman, L Angelakis, E Nestoras, I Krichbaue, TP Zensue, JA Ungerechts, H Sievers, A AF Aleksic, J. Ansoldi, S. Antonelli, L. A. Antoranz, P. Babic, A. Bangale, P. Barres de Almeida, U. Barrio, J. A. Becerra Gonzalez, J. Bednarek, W. Bernardini, E. Biland, A. Blanch, O. Bonnefoy, S. Bonnoli, G. Borracci, F. Bratz, T. Carmona, E. Carosi, A. Carreto Fidalgo, D. Colin, P. Colombo, E. Contreras, J. L. Cortina, I. Covino, S. Da Vela, P. Dazzi, F. De Angelis, A. De Caneva, G. De Lotto, B. Delgado Mendez, C. Doert, M. Dominguez, A. Dominis Presters, D. Dorner, D. Doro, M. Einecke, S. Eisenacher, D. Elsaesser, D. Farina, E. Ferenc, D. Fonseca, M. V. Font, L. Frantzen, K. Fruck, C. Garcia Lopez, R. J. Garczarczyk, M. Garrido Terrats, D. Gaug, M. Godinovic, N. Gonzalez Munoz, A. Gozzini, S. R. Hadasch, D. Hayashida, M. Herrera, J. Herrero, A. Hildebrand, D. Hose, J. Hrupec, D. Idec, W. Kadenius, V. Kellermann, H. 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. Mallotw, K. Maneva, G. Mankuzhiyil, N. Mannheim, K. Maraschi, L. Marcote, B. Mariotti, M. Martinez, M. Mazin, D. Menzel, U. Meucci, M. Miranda, J. M. Mirzoyan, R. Moralejo, A. Munar-Adrover, P. Nakajima, D. Niedzwiecki, A. Nilsson, K. Nishijima, K. Noda, K. Nowak, N. Orito, R. Overkemping, A. Paiano, S. Palatiello, M. Paneque, D. Paoletti, R. Paredes, J. M. Paredes-Fortuny, X. Partini, S. Persic, M. Prada, F. Prada Moroni, P. G. Prandini, E. Preziuso, S. Puljak, I. Reinthal, R. Rhode, W. Ribo, M. Rico, J. Rodriguez Garcia, J. Ruegamer, S. Saggion, A. Saito, T. Saito, K. Satalecka, K. Scalzotto, V. Scapin, V. Schultz, C. Schweizer, T. Shore, S. N. Sillanpaa, A. Sitarek, J. Snidaric, I. Sobczynska, D. Spanier, F. Stamatescu, V. Stamerra, A. Steinbring, T. Storz, J. Strzys, M. Sun, S. Suric, T. 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. Wagner, R. M. Zandanel, F. Zanin, R. Lucarelli, F. Pittori, C. Vercellone, S. Verrecchia, F. Buson, S. D'Ammando, F. Stawarz, L. Giroletti, M. Orienti, M. Mundell, C. Steele, I. Zarpudin, B. Raiteri, C. M. Villata, M. Sandrinelli, A. Lahteenmaki, A. Tammi, J. Tornikoski, M. Hovatta, T. Readhead, A. C. S. Max-Moerbeck, W. Richards, J. L. Jorstad, S. Marscher, A. Gurwell, M. A. Larionov, V. M. Blinov, D. A. Konstantinova, T. S. Kopatskaya, E. N. Larionova, L. V. Earionova, E. G. Morozova, D. A. Troitky, I. S. Mokrushina, A. A. Pavlova, Yu. V. Chen, W. P. Lin, H. C. Panwar, N. Agudo, I. Casadio, C. Gomez, J. L. Molina, S. N. Kurtanidze, O. M. Nikolashvili, M. G. Kurtanidze, S. O. Chigladze, R. A. Acosta-Pulido, J. A. Carnerero, M. I. Manilla-Robles, A. Ovcharov, E. Bozhilov, V. Metodieva, I. Aller, M. F. Aller, H. D. Fuhrman, L. Angelakis, E. Nestoras, I. Krichbaue, T. P. Zensue, J. A. Ungerechts, H. Sievers, A. CA MAGIC Collaboration AGILE Collaboration Fermi-LAT Collaboration TI MAGIC gamma-ray and multi-frequency observations of flat spectrum radio quasar PKS 1510-089 in early 2012 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual: PKS 1510-089 ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; HIGH-ENERGY EMISSION; BASE-LINE ARRAY; BLAZAR 3C 279; MULTIWAVELENGTH OBSERVATIONS; X-RAY; POLARIMETRIC OBSERVATIONS; BACKGROUND-RADIATION; HIGH-FREQUENCIES AB Aims. Amongst more than fifty blazars detected in very high energy (VHE, E > 100 GeV) gamma rays, only three belong to the subclass of flat spectrum radio quasars (FSRQs). The detection of FSRQs in the VHE range is challenging, mainly because of their soft spectra in the GeV-TeV regime. MAGIC observed PKS 1510-089 (z = 0.36) starting 2012 February 3 until April 3 during a high activity state in the high energy (HE, E > 100 MeV) gamma-ray band observed by AGILE and Fermi. MAGIC observations result in the detection of a source with significance of 6.0 standard deviations (sigma). We study the multi-frequency behaviour of the source at the epoch of MAGIC observation, collecting quasi-simultaneous data at radio and optical (GASP-WEBT and F-Gamma collaborations, REM, Steward, Perkins, Liverpool, OVRO, and VLBA telescopes), X-ray (Swift satellite), and HE gamma-ray frequencies. Methods. We study the VHE gamma-ray emission, together with the multi-frequency light curves, 43 GHz radio maps, and spectral energy distribution (SED) of the source. The quasi-simultaneous multi-frequency SED from the millimetre radio band to VHE gamma rays is modelled with a one-zone inverse Compton model. We study two different origins of the seed photons for the inverse Compton scattering, namely the infrared torus and a slow sheath surrounding the jet around the Very Long Baseline Array (VLBA) core. Results. We find that the VHE gamma-ray emission detected from PKS 1510-089 in 2012 February-April agrees with the previous VHE observations of the source from 2009 March-April. We find no statistically significant variability during the MAGIC observations on daily, weekly, or monthly time scales, while the other two known VHE FSRQs (3C 279 and PKS 1222+216) have shown daily scale to sub-hour variability. The gamma-ray SED combining AGILE, Fermi and MAGIC data joins smoothly and shows no hint of a break. The multi-frequency light curves suggest a common origin for the millimetre radio and HE gamma-ray emission, and the HE gamma-ray flaring starts when the new component is ejected from the 43GHz VLBA core and the studied SED models fit the data well. However, the fast HE gamma-ray variability requires that within the modelled large emitting region, more compact regions must exist. We suggest that these observed signatures would be most naturally explained by a turbulent plasma flowing at a relativistic speed down the jet and crossing a standing conical shock. C1 [Aleksic, J.; Blanch, O.; Cortina, I.; Gonzalez Munoz, A.; Hildebrand, D.; Lopez-Coto, R.; Lopez-Oramas, A.; Martinez, M.; Moralejo, A.; Rico, J.; Sitarek, J.; Stamatescu, V.] IFAE, Bellaterra 08193, Spain. [Ansoldi, S.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] Univ Udine, I-33100 Udine, Italy. [Ansoldi, S.; De Angelis, A.; De Lotto, B.; Mankuzhiyil, N.; Palatiello, M.; Persic, M.] INFN Trieste, 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.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Preziuso, S.] Univ Siena, I-53100 Siena, Italy. [Antoranz, P.; Da Vela, P.; Meucci, M.; Miranda, J. M.; Paoletti, R.; Partini, S.; Preziuso, S.] INFN Pisa, I-53100 Siena, Italy. [Babic, A.; Dominis Presters, D.; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Rijeka, Rudjer Boskov Inst, Croatian MAGIC Consortium, Zagreb 10000, Croatia. [Babic, A.; Dominis Presters, D.; Ferenc, D.; Godinovic, N.; Hrupec, D.; Lelas, D.; Puljak, I.; Snidaric, I.; Suric, T.; Terzic, T.] Univ Split, Zagreb 10000, Croatia. [Bangale, P.; Barres de Almeida, U.; Borracci, F.; Colin, P.; Dazzi, F.; Fruck, C.; Hose, J.; Kellermann, H.; Krause, J.; Lorenz, E.; Mazin, D.; Menzel, U.; Mirzoyan, R.; Noda, K.; Nowak, N.; Paneque, D.; Rodriguez Garcia, J.; Schweizer, T.; Strzys, M.; Sun, S.; Teshima, M.; Toyama, T.; Wagner, R. M.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Becerra Gonzalez, J.; Colombo, E.; Garcia Lopez, R. J.; Herrera, J.; Herrero, A.; Tescaro, D.] Univ Complutense, E-28040 Madrid, Spain. [Becerra Gonzalez, J.; Colombo, E.; Garcia Lopez, R. J.; Herrera, J.; Herrero, A.; 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.; Mallotw, K.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Biland, A.; Prandini, E.; Vogler, P.] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland. [Bratz, T.; Dorner, D.; Eisenacher, D.; Elsaesser, D.; Lewandowska, N.; Mannheim, K.; Ruegamer, S.; Spanier, F.; Steinbring, T.; Storz, J.; Tibolla, O.] Univ Wurzburg, D-97074 Wurzburg, Germany. [Carmona, E.; Delgado Mendez, C.] Ctr Invest Energet Medioambientales & Tecnol, Madrid 28040, Spain. [Doert, M.; Einecke, S.; Frantzen, K.; Overkemping, A.; Rhode, W.; Thaele, J.; Uellenbeck, M.] Tech Univ Dortmund, D-44221 Dortmund, Germany. [Dominguez, A.; Prada, F.; Zandanel, F.] Inst Astrofis Andalucia CSIC, Granada 18080, Spain. [Doro, M.; Mariotti, M.; Paiano, S.; Saggion, A.; Scalzotto, V.; Schultz, C.; Buson, S.; Sandrinelli, A.] Univ Padua, I-35131 Padua, Italy. [Doro, M.; Mariotti, M.; Paiano, S.; Saggion, A.; Scalzotto, V.; Schultz, C.; Buson, S.; Sandrinelli, A.] INFN, I-35131 Padua, Italy. [Farina, E.; Treves, A.] Univ Insubria, I-22100 Como, Italy. [Font, L.; Garrido Terrats, D.; Gaug, M.] Univ Autonoma Barcelona, Unitat Fis Radiac, Dept Fis, Bellaterra 08193, Spain. [Font, L.; Garrido Terrats, D.; Gaug, M.] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain. [Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEC CSIC, Barcelona, Spain. [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 Consortitum, Kyoto 6068901, Japan. [Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Tuorla Observ, Finnish MAGIC Consortium, Oulu 900147, Finland. [Kadenius, V.; Lindfors, E.; Nilsson, K.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Oulu, Dept Phys, Oulu 900147, Finland. [Makariev, M.; Maneva, G.; Temnikov, P.] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria. [Marcote, B.; Munar-Adrover, P.; Paredes, J. M.; Paredes-Fortuny, X.; Ribo, M.; Zanin, R.] Univ Barcelona, ICC, IEEC, E-08028 Barcelona, Spain. [Prada Moroni, P. G.; Shore, S. N.] Univ Pisa, I-56126 Pisa, Italy. [Prada Moroni, P. G.; Shore, S. N.] INFN Pisa, I-56126 Pisa, Italy. [Becerra Gonzalez, J.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Becerra Gonzalez, J.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Persic, M.] INAF Trieste, I-34131 Trieste, Italy. [Prada, F.] UAM CSIC, Inst Fis Teor, Madrid 28049, Spain. [D'Ammando, F.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [D'Ammando, F.] INFN Sez Perugia, I-06123 Perugia, Italy. [Lucarelli, F.; Pittori, C.; Verrecchia, F.] INAF OAR, I-00040 Monte Porzio Catone, RM, Italy. [Lucarelli, F.; Pittori, C.; Verrecchia, F.] ASI Sci Data Ctr ASDC, I-00133 Rome, Italy. [Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy. [Mundell, C.; Steele, I.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Zarpudin, B.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Piikkio 21500, Finland. [Raiteri, C. M.; Villata, M.; Carnerero, M. I.] INAF Osservatorio Astrofis Torino, I-10025 Turin, Italy. [Lahteenmaki, A.; Tammi, J.; Tornikoski, M.] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland. 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C.; Panwar, N.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taiwan. [Agudo, I.; Casadio, C.; Gomez, J. L.; Molina, S. N.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Agudo, I.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Kurtanidze, O. M.; Nikolashvili, M. G.; Kurtanidze, S. O.; Chigladze, R. A.] Abastumani Observ, GE-0301 Mt Kanobili, Abastumani, Rep of Georgia. [Kurtanidze, O. M.] Heidelberg Univ, Zentrum Astron, D-69117 Heidelberg, Germany. [Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan 422526, Russia. [Acosta-Pulido, J. A.; Carnerero, M. I.] IAC, Tenerife 38205, Spain. [Acosta-Pulido, J. A.; Carnerero, M. I.; Manilla-Robles, A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Ovcharov, E.; Bozhilov, V.; Metodieva, I.] Univ Sofia, Sofia 1000, Bulgaria. [Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Fuhrman, L.; Angelakis, E.; Nestoras, I.; Krichbaue, T. P.; Zensue, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Ungerechts, H.; Sievers, A.] Inst Radio Astron Millimetr, Granada 18012, Spain. [Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. RP De Caneva, G (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM gessica.de.caneva@desy.de; elilin@utu.fi; ksaito@icrr.utokyo.ac.jp; jsitarek@ifae.es; fabrizio.tavecchio@brera.inaf.it RI Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Grishina, Tatiana/H-6873-2013; Kopatskaya, Evgenia/H-4720-2013; Blinov, Dmitry/G-9925-2013; Pittori, Carlotta/C-7710-2016; Stamatescu, Victor/C-9945-2016; Font, Lluis/L-4197-2014; Contreras Gonzalez, Jose Luis/K-7255-2014; Lopez Moya, Marcos/L-2304-2014; Temnikov, Petar/L-6999-2016; Maneva, Galina/L-7120-2016; Troitskaya, Yuliya/N-2222-2015; Lahteenmaki, Anne/L-5987-2013; Babic, Ana/B-9599-2014; Ribo, Marc/B-3579-2015; GAug, Markus/L-2340-2014; Molina, Sol Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Antoranz, Pedro/H-5095-2015; Miranda, Jose Miguel/F-2913-2013; Fonseca Gonzalez, Maria Victoria/I-2004-2015; Delgado, Carlos/K-7587-2014; Larionov, Valeri/H-1349-2013; Morozova, Daria/H-1298-2013; Makariev, Martin/M-2122-2016; Torres, Diego/O-9422-2016; Barrio, Juan/L-3227-2014; Cortina, Juan/C-2783-2017; OI Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Grishina, Tatiana/0000-0002-3953-6676; Kopatskaya, Evgenia/0000-0001-9518-337X; Blinov, Dmitry/0000-0003-0611-5784; Pittori, Carlotta/0000-0001-6661-9779; Stamatescu, Victor/0000-0001-9030-7513; Font, Lluis/0000-0003-2109-5961; Contreras Gonzalez, Jose Luis/0000-0001-7282-2394; Lopez Moya, Marcos/0000-0002-8791-7908; Temnikov, Petar/0000-0002-9559-3384; Troitskaya, Yuliya/0000-0002-9907-9876; Babic, Ana/0000-0001-9549-9710; GAug, Markus/0000-0001-8442-7877; Molina, Sol Natalia/0000-0002-4112-2157; Agudo, Ivan/0000-0002-3777-6182; Antoranz, Pedro/0000-0002-3015-3601; Miranda, Jose Miguel/0000-0002-1472-9690; Fonseca Gonzalez, Maria Victoria/0000-0003-2235-0725; Delgado, Carlos/0000-0002-7014-4101; Larionov, Valeri/0000-0002-4640-4356; Morozova, Daria/0000-0002-9407-7804; Doro, Michele/0000-0001-9104-3214; Stamerra, Antonio/0000-0002-9430-5264; Prandini, Elisa/0000-0003-4502-9053; Becerra Gonzalez, Josefa/0000-0002-6729-9022; Covino, Stefano/0000-0001-9078-5507; Paredes, Josep M./0000-0002-1566-9044; Lucarelli, Fabrizio/0000-0002-6311-764X; Tavecchio, Fabrizio/0000-0003-0256-0995; Bonnoli, Giacomo/0000-0003-2464-9077; Antonelli, Lucio Angelo/0000-0002-5037-9034; Dominguez, Alberto/0000-0002-3433-4610; Farina, Emanuele Paolo/0000-0002-6822-2254; Ribo, Marc/0000-0002-9931-4557; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Angelakis, Emmanouil/0000-0001-7327-5441; Jorstad, Svetlana/0000-0001-9522-5453; Prada Moroni, Pier Giorgio/0000-0001-9712-9916; Larionova, Liudmila/0000-0002-0274-1481; LA BARBERA, ANTONINO/0000-0002-5880-8913; De Lotto, Barbara/0000-0003-3624-4480; Persic, Massimo/0000-0003-1853-4900; Vercellone, Stefano/0000-0003-1163-1396; Raiteri, Claudia Maria/0000-0003-1784-2784; Torres, Diego/0000-0002-1522-9065; Barrio, Juan/0000-0002-0965-0259; Cortina, Juan/0000-0003-4576-0452; Verrecchia, Francesco/0000-0003-3455-5082; Villata, Massimo/0000-0003-1743-6946 FU German BMBF; MPG; Italian INFN; Swiss National Fund SNF; Spanish MICINN; Spanish Consolider-Ingenio programme [CPAN CSD2007-00042, MultiDark CSD2009-00064]; Bulgarian NSF [DO02-353]; Academy of Finland [127740, 212656, 210338, 121148]; DFG Cluster of Excellence "Origin and Structure of the Universe"; DFG Collaborative Research Centres [SFB823/C4, SFB876/C3]; Polish MNiSzW grant [745/N-HESS-MAGIC/2010/0]; University of Rijeka Project [13.12.1.3.02]; Croatian Science Foundation [09/176]; JSPS KAKENHI [25800105, 24000004]; ERDF; Spanish MINECO [FPA2012-39502, JCI-2011-10019]; National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; ASI [I/089/06/2, I/042/10/0, I/028/12/0]; Shota Rustaveli National Science Foundation [FR/638/6-320/12, 31/77]; NASA [NNX08AW31G, NNX11A043G]; NSF [AST-0808050, AST-1109911]; NASA Fermi Guest Investigator grants [NNX11AQ03G, NNX11AO37G, NNX12AO90G]; BU; Lowell Observatory; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain); International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Bonn; International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the University of Cologne; [NNX08AW56G]; [NNX09AU10G]; [NNX12AO93G] FX We 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 support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the Spanish MICINN is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant DO02-353 of the Bulgarian NSF, by grant 127740 of the Academy of Finland, by the DFG Cluster of Excellence "Origin and Structure of the Universe", by the DFG Collaborative Research Centres SFB823/C4 and SFB876/C3, by the Polish MNiSzW grant 745/N-HESS-MAGIC/2010/0, the University of Rijeka Project 13.12.1.3.02, the Croatian Science Foundation Project 09/176 and by JSPS KAKENHI Grants numbers 24000004. J. S. is supported by ERDF and the Spanish MINECO through FPA2012-39502 and JCI-2011-10019 grants. K. S. is supported by JSPS KAKENHI grant number 25800105. 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. Astrorivelatore Gamma ad Immagini LEggero (AGILE) is a scientific mission of the Italian Space Agency (ASI) with INFN, INAF and CIFS participation. AGILE research partially supported through the ASI grants I/089/06/2, I/042/10/0 and I/028/12/0. Data from the Steward Observatory spectropolarimetric monitoring project were used. This programme is supported by Fermi Guest Investigator grants NNX08AW56G, NNX09AU10G, and NNX12AO93G. 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 programme. The IAC team acknowledges the support from the group of support astronomers and telescope operators of the Observatorio del Teide. 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. The OVRO 40-m monitoring programme is supported in part by NASA grants NNX08AW31G and NNX11A043G, and NSF grants AST-0808050 and AST-1109911. The VLBA is operated by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grants NNX11AQ03G, NNX11AO37G, and NNX12AO90G.; 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 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 Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). This research is partly based on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg and with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). I. Nestoras is funded by the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. NR 129 TC 15 Z9 15 U1 1 U2 27 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 SEP PY 2014 VL 569 AR UNSP A46 DI 10.1051/0004-6361/201423484 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8PZ UT WOS:000343092100046 ER PT J AU Buson, S Longo, F Larsson, S Cutini, S Finke, J Ciprini, S Ojha, R D'Ammando, F Donato, D Thompson, DJ Desiante, R Bastieri, D Wagner, S Hauser, M Fuhrmann, L Dutka, M Muller, C Kadler, M Angelakis, E Zensus, JA Stevens, J Blanchard, JM Edwards, PG Lovell, JEJ Gurwell, MA Wehrle, AE Zook, A AF Buson, S. Longo, F. Larsson, S. Cutini, S. Finke, J. Ciprini, S. Ojha, R. D'Ammando, F. Donato, D. Thompson, D. J. Desiante, R. Bastieri, D. Wagner, S. Hauser, M. Fuhrmann, L. Dutka, M. Mueller, C. Kadler, M. Angelakis, E. Zensus, J. A. Stevens, J. Blanchard, J. M. Edwards, P. G. Lovell, J. E. J. Gurwell, M. A. Wehrle, A. E. Zook, A. TI Unusual flaring activity in the blazar PKS 1424-418 during 2008-2011 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; radiation mechanisms: non-thermal; quasars: individual: PKS 1424-418; gamma rays: galaxies; galaxies: jets ID LARGE-AREA TELESCOPE; GAMMA-RAY FLARE; GALACTIC NUCLEI; COMPTON ANALYSIS; SOURCE CATALOG; RADIO-SOURCES; 3C 454.3; VARIABILITY; EMISSION; MISSION AB Context. Blazars are a subset of active galactic nuclei (AGN) with jets that are oriented along our line of sight. Variability and spectral energy distribution (SED) studies are crucial tools for understanding the physical processes responsible for observed AGN emission. Aims. We report peculiar behavior in the bright gamma-ray blazar PKS 1424 418 and use its strong variability to reveal information about the particle acceleration and interactions in the jet. Methods. Correlation analysis of the extensive optical coverage by the ATOM telescope and nearly continuous gamma-ray coverage by the Fermi Large Area Telescope is combined with broadband, time-dependent modeling of the SED incorporating supplemental information from radio and X-ray observations of this blazar. Results. We analyse in detail four bright phases at optical-GeV energies. These flares of PKS 1424-418 show high correlation between these energy ranges, with the exception of one large optical flare that coincides with relatively low gamma-ray activity. Although the optical/gamma-ray behavior of PKS 1424-418 shows variety, the multiwavelength modeling indicates that these differences can largely be explained by changes in the flux and energy spectrum of the electrons in the jet that are radiating. We find that for all flares the SED is adequately represented by a leptonic model that includes inverse Compton emission from external radiation fields with similar parameters. Conclusions. Detailed studies of individual blazars like PKS 1424 418 during periods of enhanced activity in different wavebands are helping us identify underlying patterns in the physical parameters in this class of AGN. C1 [Buson, S.; Bastieri, D.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Buson, S.; Bastieri, D.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Longo, F.; Desiante, R.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Larsson, S.] Stockholm Univ, Dept Phys, Alballova, S-10691 Stockholm, Sweden. [Larsson, S.] Alballova, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Cutini, S.; Ciprini, S.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00133 Rome, Italy. [Cutini, S.; Ciprini, S.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Rome, Italy. [Finke, J.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ojha, R.; Donato, D.; Thompson, D. J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [D'Ammando, F.; Kadler, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Donato, D.] Ctr Res & Explorat Space Sci & Technol CRESST, Greenbelt, MD 20771 USA. [Donato, D.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [Donato, D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Wagner, S.; Hauser, M.] Heidelberg Univ, D-69117 Heidelberg, Germany. [Fuhrmann, L.; Angelakis, E.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Dutka, M.] Catholic Univ Amer, Washington, DC 20064 USA. [Mueller, C.; Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Mueller, C.; Kadler, M.] Dr Remeis Sternwarte Bamberg, D-96049 Bamberg, Germany. [Kadler, M.] Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany. [Kadler, M.] Univ Space Res Assoc USRA, Columbia, MD 21044 USA. [Stevens, J.] CSIRO Astron & Space Sci, ATNF, Narrabri, NSW 2390, Australia. [Blanchard, J. M.; Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Edwards, P. G.] CSIRO Astron & Space Sci, ATNF, Epping, NSW 1710, Australia. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wehrle, A. E.] Space Sci Inst, Boulder, CO USA. [Zook, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Buson, S (reprint author), Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. EM sara.buson@pd.infn.it; francesco.longo@trieste.infn.it OI Bastieri, Denis/0000-0002-6954-8862; Angelakis, Emmanouil/0000-0001-7327-5441; Kadler, Matthias/0000-0001-5606-6154 FU National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; K. A. Wallenberg Foundation in Sweden; German Deutsche Forschungsgemeinschaft, DFG [Ts 17/2-1]; Commonwealth of Australia; Smithsonian Institution; Academia Sinica; NASA through Fermi Guest Investigator grants [NNH10ZDA001N, NNH09ZDA001N]; [6090777] FX The Fermi LAT Collaboration acknowledges generous on-going 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 from the following agencies is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy and the K. A. Wallenberg Foundation in Sweden for providing a grant in support of a Royal Swedish Academy of Sciences Research fellowship for J.C. Part of this work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Ts 17/2-1. The Australian Long Baseline Array and the Australia Telescope Compact Array are 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 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 was funded in part by NASA through Fermi Guest Investigator grants NNH09ZDA001N and NNH10ZDA001N. This research was 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. We thank Neil Gehrels and the Swift team for scheduling our Target of Opportunity requests. This research was enabled in part through Swift Guest Investigator grants 6090777. We thank Silvia Raino for useful comments and suggestions. NR 61 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 SEP PY 2014 VL 569 AR A40 DI 10.1051/0004-6361/201423367 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8PZ UT WOS:000343092100038 ER PT J AU Konig, S Aalto, S Lindroos, L Muller, S Gallagher, JS Beswick, RJ Petitpas, G Jutte, E AF Koenig, S. Aalto, S. Lindroos, L. Muller, S. Gallagher, J. S., III Beswick, R. J. Petitpas, G. Juette, E. TI Molecular tendrils feeding star formation in the Eye of the Medusa The Medusa merger in high resolution (CO)-C-12 2-1 maps SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: evolution; galaxies: individual: NGC 4194; galaxies: starburst; galaxies: active; radio lines: ISM; ISM: molecules ID LUMINOUS INFRARED GALAXIES; NEARBY GALAXIES; STARBURST GALAXIES; CONVERSION FACTOR; SPIRAL GALAXIES; RADIO-CONTINUUM; CO OBSERVATIONS; MINOR-MERGER; GAS DISK; NGC 1614 AB Studying molecular gas properties in merging galaxies gives us important clues to the onset and evolution of interaction-triggered starbursts. NGC 4194 (the Medusa merger) is particularly interesting to study, since its FIR-to-CO luminosity ratio rivals that of ultraluminous galaxies (ULIRGs), despite its lower luminosity compared to ULIRGs, which indicates a high star formation efficiency (SFE) that is relative to even most spirals and ULIRGs. We study the molecular medium at an angular resolution of 0.65 '' x 0.52 '' (similar to 120 x 98 pc) through our observations of (CO)-C-12 2-1 emission using the Submillimeter Array (SMA). We compare our (CO)-C-12 2-1 maps with the optical Hubble Space Telescope and high angular resolution radio continuum images to study the relationship between molecular gas and the other components of the starburst region. The molecular gas is tracing the complicated dust lane structure of NGC 4194 with the brightest emission being located in an off-nuclear ring-like structure with similar to 320 pc radius, the Eye of the Medusa. The bulk CO emission of the ring is found south of the kinematical center of NGC 4194. The northern tip of the ring is associated with the galaxy nucleus, where the radio continuum has its peak. Large velocity widths associated with the radio nucleus support the notion of NGC 4194 hosting an active galactic nucleus. A prominent, secondary emission maximum in the radio continuum is located inside the molecular ring. This suggests that the morphology of the ring is partially influenced by massive supernova explosions. From the combined evidence, we propose that the Eye of the Medusa contains a shell of swept up material where we identify a number of giant molecular associations. We propose that the Eye may be the site of an efficient starburst of 5-7 M-circle dot yr(-1), but it would still constitute only a fraction of the 30-50 M-circle dot yr(-1) star formation rate of the Medusa. Furthermore, we find that similar to 50% of the molecular mass of NGC 4194 is found in extended filamentary-like structures tracing the minor and major axis dust lanes. We suggest that molecular gas is transported along these lanes, providing the central starburst region with fuel. Interestingly, a comparison with locations of super star clusters (SSCs) reveal that the molecular gas and the SSCs are not co-spatial. C1 [Koenig, S.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [Aalto, S.; Lindroos, L.; Muller, S.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Gallagher, J. S., III] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Beswick, R. J.] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. RP Konig, S (reprint author), Inst Radioastron Millimetr, 300 Rue Piscine,Domaine Univ, F-38406 St Martin Dheres, France. EM koenig@iram.fr OI Lindroos, Lukas/0000-0003-1208-0362; Konig, Sabine/0000-0001-6174-8467; /0000-0002-9931-1313 FU Swedish Research Council [621-2011-414]; Swedish National Space Board (SNSB) [145/11:1-3]; College of Letters & Science, University of Wisconsin-Madison; Smithsonian Institution; Academia Sinica FX We thank the referee for useful comments. S. A. thanks the Swedish Research Council (grant 621-2011-414) and the Swedish National Space Board (SNSB, grant 145/11:1-3) for support. J.S.G. thanks the College of Letters & Science, University of Wisconsin-Madison for partial support of this work. 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. MERLIN/eMERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of STFC. AIPS is produced and maintained 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 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 57 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2014 VL 569 AR A6 DI 10.1051/0004-6361/201423548 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8PZ UT WOS:000343092100048 ER PT J AU Schmalzl, M Launhardt, R Stutz, AM Linz, H Bourke, TL Beuther, H Henning, T Krause, O Nielbock, M Schmiedeke, A AF Schmalzl, M. Launhardt, R. Stutz, A. M. Linz, H. Bourke, T. L. Beuther, H. Henning, Th. Krause, O. Nielbock, M. Schmiedeke, A. TI The Earliest Phases of Star formation (EPoS) Temperature, density, and kinematic structure of the star-forming core CB 17 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE dust, extinction; ISM: molecules; ISM: kinematics and dynamics; stars: formation; stars: low-mass; ISM: individual objects: CB 17 ID 1ST HYDROSTATIC CORE; MOLECULAR CLOUD CORES; PRE-STELLAR CORES; PROTOSTELLAR CORES; INITIAL CONDITIONS; HIGH-MASS; PRESTELLAR CORES; DUST-TEMPERATURE; BOK GLOBULES; HERSCHEL OBSERVATIONS AB Context. The initial conditions for the gravitational collapse of molecular cloud cores and the subsequent birth of stars are still not well constrained. The characteristic cold temperatures (similar to 10 K) in such regions require observations at sub-millimetre and longer wavelengths. The Herschel Space Observatory and complementary ground-based observations presented in this paper have the unprecedented potential to reveal the structure and kinematics of a prototypical core region at the onset of stellar birth. Aims. This paper aims to determine the density, temperature, and velocity structure of the star-forming Bok globule CB 17. This isolated region is known to host (at least) two sources at different evolutionary stages: a dense core, SMM1, and a Class I protostar, IRS. Methods. We modeled the cold dust emission maps from 100 mu m to 1.2mm with both a modified blackbody technique to determine the optical depth-weighted line-of-sight temperature and column density and a ray-tracing technique to determine the core temperature and volume density structure. Furthermore, we analysed the kinematics of CB17 using the high-density gas tracer N2H+. Results. From the ray-tracing analysis, we find a temperature in the centre of SMM1 of T-0 = 10.6K, a flat density profile with radius 9.5 x 10(3) au, and a central volume density of n(H,0) = 2.3 x 10(5) cm(-3). The velocity structure of the N2H+ observations reveal global rotation with a velocity gradient of 4.3 km s(-1) pc(-1). Superposed on this rotation signature we find a more complex velocity field, which may be indicative of differential motions within the dense core. Conclusions. SMM is a core in an early evolutionary stage at the verge of being bound, but the question of whether it is a starless or a protostellar core remains unanswered. C1 [Schmalzl, M.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Schmalzl, M.; Launhardt, R.; Stutz, A. M.; Linz, H.; Beuther, H.; Henning, Th.; Krause, O.; Nielbock, M.; Schmiedeke, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Schmalzl, M.; Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schmiedeke, A.] Univ Cologne, D-50937 Cologne, Germany. RP Schmalzl, M (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM schmalzl@strw.leidenuniv.nl OI Nielbock, Markus/0000-0002-1271-1825; Stutz, Amelia/0000-0003-2300-8200 FU NOVA, the Netherlands Research School for Astronomy; NSF [0708158, 0953142]; Deutsche Forschungsgemeinschaft [1573]; Deutsches Zentrum fur Luft- und Raumfahrt (DLR); Canadian Space Agency FX M.S. acknowledges support from NOVA, the Netherlands Research School for Astronomy. This work was supported by NSF grants 0708158 and 0953142. The work of A. M. S. was supported by the Deutsche Forschungsgemeinschaft priority programme 1573 ("Physics of the Interstellar Medium"). H. L. was funded by the Deutsches Zentrum fur Luft- und Raumfahrt (DLR). This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. M. S. acknowledges the use of the GILDAS software package (http://www.iram.fr/IRAMFR/GILDAS/). NR 74 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2014 VL 569 AR A7 DI 10.1051/0004-6361/201322176 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8PZ UT WOS:000343092100007 ER PT J AU Schmieder, B Tian, H Kucera, T Ariste, AL Mein, N Mein, P Dalmasse, K Golub, L AF Schmieder, B. Tian, H. Kucera, T. Lopez Ariste, A. Mein, N. Mein, P. Dalmasse, K. Golub, L. TI Open questions on prominences from coordinated observations by IRIS, Hinode, SDO/AIA, THEMIS, and the Meudon/MSDP SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: magnetic fields; Sun: filaments, prominences; Sun: transition region ID SOLAR OPTICAL TELESCOPE; MAGNETIC-FIELD VECTOR; QUIESCENT PROMINENCES; FILAMENT CHANNEL; RADIATIVE-TRANSFER; ACTIVE-REGION; LINES; SOHO/SUMER; POLARIZATION; EMERGENCE AB Context. A large prominence was observed by multiple instruments on the ground and in space during an international campaign on September 24, 2013, for three hours (12: 12 UT -15: 12 UT). Instruments used in the campaign included the newly launched (June 2013) Interface Region Imaging Spectrograph (IRIS), THEMIS (Tenerife), the Hinode Solar Optical Telescope (SOT), the Solar Dynamic Observatory's Atmospheric Imaging Assembly (SDO/AIA), and the Multichannel Subtractive Double Pass spectrograph (MSDP) in the Meudon Solar Tower. The movies obtained in 304 angstrom with the EUV imager SDO/AIA, and in Ca II line by SOT show the dynamic nature of the prominence. Aims. The aim of this work is to study the dynamics of the prominence fine structures in multiple wavelengths to understand their formation. Methods. The spectrographs IRIS and MSDP provided line profiles with a high cadence in Mg II h (2803.5 angstrom) and k (2796.4 angstrom) lines along four slit positions (IRIS), and in Ha in a 2D field of view (MSDP). The spectropolarimetry of THEMIS (Tenerife) allowed us to derive the magnetic field of the prominence using the He D-3 line depolarization (Hanle effect combined with the Zeeman effect). Results. The magnetic field is found to be globally horizontal with a relatively weak field strength (8-15 Gauss). On the other hand, the Ca II movie reveals turbulent-like motion that is not organized in specific parts of the prominence. We tested the addition of a turbulent magnetic component. This model is compatible with the polarimetric observations at those places where the plasma turbulence peaks. On the other hand, the Mg II line profiles show multiple peaks well separated in wavelength. This is interpreted by the existence of small threads along the line of sight with a large dispersion of discrete values of Doppler shifts, from 5 km s(-1) (a quasi-steady component) to 60-80 km s(-1). Each peak corresponds to a Gaussian profile, and not to a reversed profile as was expected by the present non-LTE radiative transfer modeling. This is a very surprising behavior for the Mg II line observed in prominences. Conclusions. Turbulent fields on top of the macroscopic horizontal component of the magnetic field supporting the prominence give rise to the complex dynamics of the plasma. The plasma with the high velocities (70 km s(-1) to 100 km s(-1) if we take into account the transverse velocities) may correspond to condensation of plasma along more or less horizontal threads of the arch-shape structure visible in 304 angstrom. The steady flows (5 km s(-1)) would correspond to a more quiescent plasma (cool and prominence-corona transition region) of the prominence packed into dips in horizontal magnetic field lines. The very weak secondary peaks in the Mg II profiles may reflect the turbulent nature of parts of the prominence. C1 [Schmieder, B.; Mein, N.; Mein, P.; Dalmasse, K.] Observ Paris, LESIA, Sect Meudon, F-75014 Paris, France. [Tian, H.; Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kucera, T.] NASA, Gsfc, MD USA. [Lopez Ariste, A.] CNRS, THEMIS, Tenerife 38200, Spain. RP Schmieder, B (reprint author), Observ Paris, LESIA, Sect Meudon, F-75014 Paris, France. EM brigitte.schmieder@obspm.fr OI Kucera, Therese/0000-0001-9632-447X FU Norwegian Space Center (NSC, Norway) through an ESA PRODEX contract; NASA's LWS program; LMSAL [8100002705] FX 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). SDO data are courtesy of NASA/SDO and the AIA science team. T.K. thanks NASA's LWS program for support. We thank also the team of THEMIS and particularly B. Gelly, the director of THEMIS allowing us to obtain coordinated observations of this prominence. We would like to thank D. Shine for providing the HINODE/SOT data, D.Crussaire, and R. Le Cocguen for the observations in the solar tower in Meudon. We thank deeply Peter Martens and Petr Heinzel for their fruitful comments which help us to improve the manuscript. H.T. is supported by contract 8100002705 from LMSAL to SAO. NR 51 TC 14 Z9 14 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 SEP PY 2014 VL 569 AR A85 DI 10.1051/0004-6361/201423922 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AQ8PZ UT WOS:000343092100075 ER PT J AU Sues, HD Averianov, A AF Sues, Hans-Dieter Averianov, Alexander TI Dromaeosauridae (Dinosauria: Theropoda) from the Bissekty Formation (Upper Cretaceous: Turonian) of Uzbekistan and the phylogenetic position of Itemirus medullaris Kurzanov, 1976 SO CRETACEOUS RESEARCH LA English DT Article DE Dinosauria; Theropoda; Paraves; Dromaeosauridae; Cretaceous; Uzbekistan ID ALBERTA AB Skeletal remains of dromaeosaurid theropods are uncommon in the richly fossiliferous continental strata of the Upper Cretaceous (Turonian) Bissekty Formation of the Kyzylkum Desert in Uzbekistan. The phylogenetic position of the first published specimen, a partial braincase designated as the holotype of Itemirus medullaris Kurzanov, 1976, has long been contentious. Our examination of the specimen supports its attribution to Dromaeosauridae. Additional, mostly well-preserved dromaeosaurid skeletal remains from the Bissekty Formation include cranial bones, teeth, vertebrae, and some podial elements. They are tentatively referred to the same taxon, Itemirus medullaris, and establish the presence of dromaeosaurid paravians in present-day Central Asia during the Turonian. Published by Elsevier Ltd. C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Averianov, Alexander] Russian Acad Sci, Inst Zool, St Petersburg 199034, Russia. [Averianov, Alexander] St Petersburg State Univ, Geol Fac, Dept Sedimentary Geol, St Petersburg 199178, Russia. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu; dzharakuduk@mail.ru RI Averianov, Alexander/M-8490-2013 OI Averianov, Alexander/0000-0001-5948-0799 FU National Science Foundation [EAR-9804771, EAR-0207004]; National Geographic Society [5901-97, 6281-98]; Navoi Mining and Metallurgy Combinat; Civilian Research and Development Foundation [RU-G1-2571-ST-04, RUB1-2860-ST-07]; Russian Fund of Basic Research [07-04-91110-AFGIRa]; Russian Scientific Fund [14-14-00015] FX Fieldwork in Uzbekistan was facilitated by and conducted in cooperation with the Zoological Institute of the National Academy of Sciences of Uzbekistan, particularly D.A. Azimov and Y.A. Chikin. For their efforts in the field, scientific expertise, and camaraderie, we thank A.V. Abramov, J.D. Archibald, G.O. Cherepanov, I.G. Danilov, S. Dominguez, C. King, N. Morris, C.M. Redman, A.S. Resvyi, C. Skrabec, P.P. Skutschas, E.V. Syromyatnikova, and D.J. Ward. We are indebted to V.R. Alifanov (Borissiak Paleontological Institute, Russian Academy of Sciences, Moscow) for granting access to the holotype of Itemirus medullaris. We gratefully acknowledge financial support from the National Science Foundation (EAR-9804771 and EAR-0207004 to J.D. Archibald and H.-D. Sues), the National Geographic Society (#5901-97 and #6281-98 to J.D. Archibald and H.-D. Sues), the Navoi Mining and Metallurgy Combinat, the Civilian Research and Development Foundation (RU-G1-2571-ST-04 and RUB1-2860-ST-07), the Russian Fund of Basic Research (07-04-91110-AFGIRa), and the Russian Scientific Fund (14-14-00015). We thank two anonymous reviewers and Editor-in-Chief E. Koutsoukos for helpful comments on a draft of the manuscript. NR 41 TC 3 Z9 3 U1 1 U2 10 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD SEP PY 2014 VL 51 BP 225 EP 240 DI 10.1016/j.cretres.2014.06.007 PG 16 WC Geology; Paleontology SC Geology; Paleontology GA AR1HR UT WOS:000343336800016 ER PT J AU Kennedy, WJ Gale, AS Huber, BT Petrizzo, MR Bown, P Barchetta, A Jenkyns, HC AF Kennedy, W. J. Gale, A. S. Huber, B. T. Petrizzo, M. R. Bown, P. Barchetta, A. Jenkyns, H. C. TI Integrated stratigraphy across the Aptian/Albian boundary at Col de Pre-Guittard (southeast France): A candidate Global Boundary Stratotype Section SO CRETACEOUS RESEARCH LA English DT Article DE Aptian-Albian; GSSP; SE France ID OCEANIC ANOXIC EVENT; SE FRANCE; CALCAREOUS NANNOFOSSILS; VOCONTIAN BASIN; ALBIAN STAGE; AMMONITES; TURNOVER; POSITION; 1B AB The outcrop of the Marnes Bleues at the Col de Pre-Guittard, 11 km north of the village of Remuzat in the Department of Drome in southeastern France is probably the most intensively studied succession spanning the Aptian/Albian boundary interval. Following the rejection of the proposed GSSP for the base of the Albian Stage (based on the first occurrence of the ammonite Leymeriellla tardefurcata in the section at Le Pillart, Tartonne, Alpes-de-Haute Provence), we re-visit the Pre-Guittard section. A new candidate GSSP defined by the first occurrence of the planktonic foraminifera Microhedbergella renilaevis Huber and Leckie, 2011 is here proposed. This first occurrence is placed in a 100 m section with 28 secondary markers, including calcareous nannofossils, planktonic foraminifera, palynomorphs, an inoceramid bivalve, ammonites, stable carbon isotopes, and local marker beds. The outcrop fulfils most of the physical criteria required of a Global Stratotype Section and Point. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Kennedy, W. J.] Univ Oxford, Museum Nat Hist, Oxford OX1 3PW, England. [Gale, A. S.] Univ Portsmouth, Sch Earth & Environm Sci, Portsmouth PO1 3QL, Hants, England. [Huber, B. T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Petrizzo, M. R.; Barchetta, A.] Univ Milan, Dipartimento Sci Terra Arditio Desio, I-20133 Milan, Italy. [Bown, P.] UCL, Dept Geol Sci, London WC1E 6BT, England. [Jenkyns, H. C.] Univ Oxford, Dept Earth Sci, Oxford OX1 3AN, England. RP Gale, AS (reprint author), Univ Portsmouth, Sch Earth & Environm Sci, Portsmouth PO1 3QL, Hants, England. EM andy.gale@port.ac.uk RI Petrizzo, Maria Rose/M-8672-2013; OI Petrizzo, Maria Rose/0000-0002-9584-8471; Jenkyns, Hugh/0000-0002-2728-0984; Bown, Paul/0000-0001-6777-4463 NR 65 TC 8 Z9 9 U1 1 U2 4 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0195-6671 EI 1095-998X J9 CRETACEOUS RES JI Cretac. Res. PD SEP PY 2014 VL 51 BP 248 EP 259 DI 10.1016/j.cretres.2014.06.005 PG 12 WC Geology; Paleontology SC Geology; Paleontology GA AR1HR UT WOS:000343336800018 ER PT J AU Oftedal, OT Nicol, SC Davies, NW Sekii, N Taufik, E Fukuda, K Saito, T Urashima, T AF Oftedal, Olav T. Nicol, Stewart C. Davies, Noel W. Sekii, Nobuhiro Taufik, Epi Fukuda, Kenji Saito, Tadao Urashima, Tadasu TI Can an ancestral condition for milk oligosaccharides be determined? Evidence from the Tasmanian echidna (Tachyglossus aculeatus setosus) SO GLYCOBIOLOGY LA English DT Article DE evolution; fucosylated oligosaccharides; milk; monotreme; O-acetyl-sialyllactose ID SIALATE-O-ACETYLESTERASES; SHORT-BEAKED ECHIDNA; MAMMARY-GLAND; CHEMICAL-CHARACTERIZATION; LACTOSE SULFATE; SIALIC-ACID; STRUCTURAL-ANALYSIS; MASS-SPECTROMETRY; ANCIENT ORIGIN; POLAR BEAR AB The monotreme pattern of egg-incubation followed by extended lactation represents the ancestral mammalian reproductive condition, suggesting that monotreme milk may include saccharides of an ancestral type. Saccharides were characterized from milk of the Tasmanian echidna Tachyglossus aculeatus setosus. Oligosaccharides in pooled milk from late lactation were purified by gel filtration and high-performance liquid chromatography using a porous graphitized carbon column and characterized by H-1 NMR spectroscopy; oligosaccharides in smaller samples from early and mid-lactation were separated by ultra-performance liquid chromatography and characterized by negative electrospray ionization mass spectrometry (ESI-MS) and tandem collision mass spectroscopy (MS/MS) product ion patterns. Eight saccharides were identified by H-1 NMR: lactose, 2'-fucosyllactose, difucosyllactose (DFL), B-tetrasaccharide, B-pentasaccharide, lacto-N-fucopentaose III (LNFP3), 4-O-acetyl-3'-sialyllactose [Neu4,5Ac(alpha 2-3) Gal (beta 1-4)Glc] and 4-O-acetyl-3'-sialyl-3-fucosyllactose [Neu4, 5Ac(alpha 2-3)Gal(beta 1-4)[Fuc(alpha 1-3)]Glc]. Six of these (all except DFL and LNFP3) were present in early and mid-lactation per ESI-MS, although some at trace levels. Four additional oligosaccharides examined by ESI-MS and MS/MS are proposed to be 3'-sialyllactose [Neu5Ac(alpha 2-3)Gal(beta 1-4) Glc], di-O-acetyl-3'-sialyllactose [Neu4,5,UAc3(alpha 2-3) Gal (beta 1-4) Glc where U = 7, 8 or 9], 4-O-acetyl-3'-sialyllactose sulfate [Neu4,5Ac(alpha 2-3)Gal(beta 1-4)GlcS, where position of the sulfate (S) is unknown] and an unidentified 800 Da oligosaccharide containing a 4-O-acetyl-3'-sialyllactose core. 4-O-acetyl-3'-sialyllactose was the predominant saccharide at all lactation stages. 4-O-Acetylation is known to protect sialyllactose from bacterial sialidases and may be critical to prevent microbial degradation on the mammary areolae and/or in the hatchling digestive tract so that sialyllactose can be available for enterocyte uptake. The ability to defend against microbial invasion was probably of great functional importance in the early evolution of milk saccharides. C1 [Oftedal, Olav T.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Nicol, Stewart C.] Univ Tasmania, Sch Biol Sci, Hobart, Tas 7001, Australia. [Davies, Noel W.] Univ Tasmania, Cent Sci Lab, Hobart, Tas 7001, Australia. [Sekii, Nobuhiro; Taufik, Epi; Fukuda, Kenji; Urashima, Tadasu] 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. RP Oftedal, OT (reprint author), Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM oftedalo@si.edu RI Davies, Noel/J-7714-2014; OI Davies, Noel/0000-0002-9624-0935; Taufik, Epi/0000-0003-4617-9037 FU National Geographic Committee for Research and Exploration [9171-12]; Global COE Program "Frontier Program for Animal Global Health and Hygiene", Ministry of Education, Culture, Sports, Science and Technology, Japan [J02] FX The work was supported by the National Geographic Committee for Research and Exploration (grant number 9171-12) and the Global COE Program "Frontier Program for Animal Global Health and Hygiene" (grant number J02), Ministry of Education, Culture, Sports, Science and Technology, Japan. NR 83 TC 6 Z9 6 U1 3 U2 17 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 SEP PY 2014 VL 24 IS 9 SI SI BP 826 EP 839 DI 10.1093/glycob/cwu041 PG 14 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA AR2KF UT WOS:000343413000008 PM 24811545 ER PT J AU Morfeld, KA Ball, RL Brown, JL AF Morfeld, Kari A. Ball, Ray L. Brown, Janine L. TI RECURRENCE OF HYPERPROLACTINEMIA AND CONTINUATION OF OVARIAN ACYCLICITY IN CAPTIVE AFRICAN ELEPHANTS (LOXODONTA AFRICANA) TREATED WITH CABERGOLINE SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Acyclicity; cabergoline; elephant; hyperprolactinemia; prolactin ID SERUM PROLACTIN; MANAGEMENT; INFERTILITY; DIAGNOSIS; MAXIMUS; POPULATION; AMENORRHEA; WOMEN AB Hyperprolactinemia is associated with reproductive acyclicity in zoo African elephants (Loxodonta africana) and may contribute to the non-self-sustainability of the captive population in North America. It is a common cause of infertility in women and other mammals and can be treated with the dopamine agonist cabergoline. The objectives of this study were to assess prolactin responses to cabergoline treatment in hyperprolactinemic, acyclic African elephants and to determine the subsequent impact on ovarian cyclic activity. Five elephants, diagnosed as hyperprolactinemic (>11 ng/ml prolactin) and acyclic (maintenance of baseline progestagens for at least 1 yr), were treated with 1-2 mg cabergoline orally twice weekly for 16-82 wk. Cabergoline reduced (P < 0.05) serum prolactin concentrations during the treatment period compared to pretreatment levels in four of five elephants (11.5 +/- 3.2 vs. 9.1 +/- 3.4 ng/ml; 20.3 +/- 16.7 vs. 7.9 +/- 9.8 ng/ml; 26.4 +/- 15.0 vs. 6.8 +/- 1.5 ng/ml; 42.2 +/- 22.6 vs. 18.6 +/- 8.9 ng/ml). However, none of the females resumed ovarian cyclicity based on serum progestagen analyses up to 1 yr posttreatment. In addition, within 1 to 6 wk after cessation of oral cabergoline, serum prolactin concentrations returned to concentrations that were as high as or higher than before treatment (P < 0.05). One elephant that exhibited the highest pretreatment prolactin concentration (75.2 +/- 10.5 ng/ml) did not respond to cabergoline and maintained elevated levels throughout the study. Thus, oral cabergoline administration reduced prolactin concentrations in elephants with hyperprolactinemia, but there was no resumption of ovarian cyclicity, and a significant prolactin rebound effect was observed. It is possible that higher doses or longer treatment intervals may be required for cabergoline treatment to result in permanent suppression of prolactin secretion and to mitigate associated ovarian cycle problems. C1 [Morfeld, Kari A.; Brown, Janine L.] Smithsonian Conservat Biol Inst, Smithsonian Inst, Natl Zool Pk, Front Royal, VA 22630 USA. [Ball, Ray L.] Tampas Lowry Pk Zoo, Tampa, FL 33604 USA. RP Brown, JL (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Inst, Natl Zool Pk, Front Royal, VA 22630 USA. EM brownjan@si.edu NR 37 TC 1 Z9 1 U1 3 U2 11 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 SEP PY 2014 VL 45 IS 3 BP 569 EP 576 DI 10.1638/2013-0254R.1 PG 8 WC Veterinary Sciences SC Veterinary Sciences GA AR2GG UT WOS:000343401200013 PM 25314824 ER PT J AU Warren, JD Aitken-Palmer, C Citino, SB AF Warren, Joshua D. Aitken-Palmer, Copper Citino, Scott B. TI CRITICAL CARE FOR A HYPOTHERMIC AND HYPOGLYCEMIC WHITE RHINOCEROS (CERATOTHERIUM SIMUM SIMUM) CALF SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Ceratotherium simum simum; critical care; hypoglycemia; hypothermia; neonate; white rhinoceros ID NEONATAL FOALS; MANAGEMENT AB A 3-day-old, 57.3-kg, male white rhinoceros (Ceratotherium simum simum) neonate presented laterally recumbent with comatose mentation, cold extremities, and severe hypothermia, hypoxemia, and hypoglycemia. Critical care support was initiated with aggressive fluid and warming support as well as dextrose and oxygen supplementation. After initial stabilization, additional complications arose in subsequent weeks including intermittent diarrhea, dry skin with loss of epidermal layers, urticaria on the head, and superficial wounds on the face, ears, feet, and penis. There is a lack of critical care information for rhinoceros calves. However, due to similarities to other Perissodactylids, some general guidelines for critical equid neonatal care were implemented. The calf was hand-raised until weaning and is now a subadult white rhinoceros with no abnormalities. C1 [Warren, Joshua D.; Aitken-Palmer, Copper; Citino, Scott B.] White Oak Conservat Ctr, Yulee, FL 32097 USA. [Aitken-Palmer, Copper] Smithsonian Conservat Biol Inst, Dept Conservat Med, Front Royal, VA 22630 USA. RP Warren, JD (reprint author), Iowa Vet Referral Ctr, 4631 Merle Hay Rd, Des Moines, IA 50322 USA. EM jdwarren@alumni.purdue.edu NR 22 TC 0 Z9 0 U1 0 U2 3 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 SEP PY 2014 VL 45 IS 3 BP 650 EP 653 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA AR2GG UT WOS:000343401200025 PM 25314836 ER PT J AU Prena, J Steiner, WE Grebennikov, VV AF Prena, Jens Steiner, Warren E., Jr. Grebennikov, Vasily V. TI BUCHANANIUS SULCATUS (LECONTE) (COLEOPTERA: CURCULIONIDAE: BARIDINAE) REARED FROM THE FRUITING BODIES OF THE ASCOMYCETE FUNGUS TRICHODERMA PELTATUM (BERK.) SAMUELS, JAKLITSCH, AND VOGLMAYR IN MARYLAND, USA SO COLEOPTERISTS BULLETIN LA English DT Editorial Material C1 [Steiner, Warren E., Jr.] Smithsonian Inst, Natl Museum Nat Hist, MRC 187, Washington, DC 20013 USA. [Grebennikov, Vasily V.] Canadian Food Inspect Agcy, Ottawa, ON K1A 0Y9, Canada. RP Prena, J (reprint author), Mhlendamm 8a, D-18055 Rostock, Germany. EM baridinae@gmx.de; steinerw@si.edu; Vasily.Grebennikov@inspection.gc.ca NR 13 TC 0 Z9 0 U1 1 U2 1 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X EI 1938-4394 J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2014 VL 68 IS 3 BP 399 EP 402 PG 4 WC Entomology SC Entomology GA AQ7YG UT WOS:000343035900010 ER PT J AU Zeng, LP Zhang, Q Sun, RR Kong, HZ Zhang, N Ma, H AF Zeng, Liping Zhang, Qiang Sun, Renran Kong, Hongzhi Zhang, Ning Ma, Hong TI Resolution of deep angiosperm phylogeny using conserved nuclear genes and estimates of early divergence times SO NATURE COMMUNICATIONS LA English DT Article ID LONG-BRANCH ATTRACTION; EARLIEST ANGIOSPERMS; MITOCHONDRIAL GENES; SEQUENCE ALIGNMENT; FLOWERING PLANTS; MIXED MODELS; DIVERSIFICATION; GENOME; TREE; EVOLUTION AB Angiosperms are the most successful plants and support human livelihood and ecosystems. Angiosperm phylogeny is the foundation of studies of gene function and phenotypic evolution, divergence time estimation and biogeography. The relationship of the five divergent groups of the Mesangiospermae (similar to 99.95% of extant angiosperms) remains uncertain, with multiple hypotheses reported in the literature. Here transcriptome data sets are obtained from 26 species lacking sequenced genomes, representing each of the five groups: eudicots, monocots, magnoliids, Chloranthaceae and Ceratophyllaceae. Phylogenetic analyses using 59 carefully selected low-copy nuclear genes resulted in highly supported relationships: sisterhood of eudicots and a clade containing Chloranthaceae and Ceratophyllaceae, with magnoliids being the next sister group, followed by monocots. Our topology allows a re-examination of the evolutionary patterns of 110 morphological characters. The molecular clock estimates of Mesangiospermae diversification during the late to middle Jurassic correspond well to the origins of some insects, which may have been a factor facilitating early angiosperm radiation. C1 [Zeng, Liping; Sun, Renran; Zhang, Ning; Ma, Hong] Fudan Univ, State Key Lab Genet Engn, Ctr Evolutionary Biol, Inst Plant Biol,Inst Biodivers Sci,Sch Life Sci, Shanghai 200433, Peoples R China. [Zeng, Liping; Sun, Renran; Zhang, Ning; Ma, Hong] Fudan Univ, Key Lab Biodivers Sci & Ecol Engn,Minist Educ, Collaborat Innovat Ctr Genet & Dev,Ctr Evolutiona, Inst Plant Biol,Inst Biodivers Sci,Sch Life Sci, Shanghai 200433, Peoples R China. [Zhang, Qiang] Guangxi Inst Bot, Guilin 541006, Guangxi Zhuang, Peoples R China. [Zhang, Qiang] Chinese Acad Sci, Guilin 541006, Peoples R China. [Kong, Hongzhi] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. [Zhang, Ning] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Ma, Hong] Fudan Univ, Inst Biomed Sci, Shanghai 200032, Peoples R China. RP Ma, H (reprint author), Fudan Univ, State Key Lab Genet Engn, Ctr Evolutionary Biol, Inst Plant Biol,Inst Biodivers Sci,Sch Life Sci, 220 Handan Rd, Shanghai 200433, Peoples R China. EM peaceful_ning@hotmail.com; hongma@fudan.edu.cn FU National Science Foundation of China [91131007, 31100156]; Smithsonian Postdoctoral Fellowship FX This work was supported by grants from the National Science Foundation of China (91131007 and 31100156) and a Smithsonian Postdoctoral Fellowship to N.Z. We are grateful to Lianming Gao, Dezhu Li, Qingfeng Wang and Xuejun Ge for their assistance in material collection; Ji Qi for help in transcriptome sequence assembly; Haifeng Wang for assistance in sequence analysis; Liang Zhao, Sangtae Kim and Yi Hu for providing plant photographs; Peter K. Endress, Ji Yang, Blair Hedges and Michael Axtell for valuable comments on the manuscript; and Michael Moore for sharing the alignments of plastid genes with us. NR 70 TC 59 Z9 68 U1 9 U2 100 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 SEP PY 2014 VL 5 AR 4956 DI 10.1038/ncomms5956 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AQ7HZ UT WOS:000342984800012 PM 25249442 ER PT J AU Hardion, L Verlaque, R Saltonstall, K Leriche, A Vila, B AF Hardion, Laurent Verlaque, Regine Saltonstall, Kristin Leriche, Agathe Vila, Bruno TI Origin of the invasive Arundo donax (Poaceae): a trans-Asian expedition in herbaria SO ANNALS OF BOTANY LA English DT Article DE Arundo donax; Poaceae; invasive species; archaeophyte; herbarium specimens; phylogeography; domesticated species; Mediterranean; Asia; morphometry; clonal species; crops; giant reed; giant cane ID GIANT REED; CHLOROPLAST DNA; ALIEN PLANTS; CARPOBROTUS AIZOACEAE; BIOLOGICAL INVASIONS; PHRAGMITES-AUSTRALIS; NONCODING REGIONS; HUBBARD POACEAE; UNITED-STATES; NORTH-AMERICA AB Background and Aims The hypothesis of an ancient introduction, i.e. archaeophyte origin, is one of the most challenging questions in phylogeography. Arundo donax (Poaceae) is currently considered to be one of the worst invasive species globally, but it has also been widely utilzed by man across Eurasia for millennia. Despite a lack of phylogenetic data, recent literature has often speculated on its introduction to the Mediterranean region. Methods This study tests the hypothesis of its ancient introduction from Asia to the Mediterranean by using plastid DNA sequencing and morphometric analysis on 127 herbarium specimens collected across sub-tropical Eurasia. In addition, a bioclimatic species distribution model calibrated on 1221 Mediterranean localities was used to identify similar ecological niches in Asia. Key Results Despite analysis of several plastid DNA hypervariable sites and the identification of 13 haplotypes, A. donax was represented by a single haplotype from the Mediterranean to the Middle East. This haplotype is shared with invasive samples worldwide, and its nearest phylogenetic relatives are located in the Middle East. Morphometric data characterized this invasive clone by a robust morphotype distinguishable from all other Asian samples. The ecological niche modelling designated the southern Caspian Sea, southern Iran and the Indus Valley as the most suitable regions of origin in Asia for the invasive clone of A. donax. Conclusions Using an integrative approach, an ancient dispersion of this robust, polyploid and non-fruiting clone is hypothesized from the Middle East to the west, leading to its invasion throughout the Mediterranean Basin. C1 [Hardion, Laurent; Verlaque, Regine; Leriche, Agathe; Vila, Bruno] Aix Marseille Univ, Inst Mediterraneen Biodivers & Ecol, UMR CNRS IRD, F-13331 Marseille, France. [Saltonstall, Kristin] Smithsonian Trop Res Inst, Panama City, Panama. RP Hardion, L (reprint author), Aix Marseille Univ, Inst Mediterraneen Biodivers & Ecol, UMR CNRS IRD, F-13331 Marseille, France. EM laurent.hardion@imbe.fr RI Leriche, Agathe/C-3151-2008 FU CNRS, the Ministry of Ecology (France); Research Federation ECCOREV; Societe Botanique de France; DREAL PACA FX The authors thank the people and institutions who helped us to obtain specimen loans, plant samples and occurrence data, including F. Fleury (MARS Marseille, France), T. Haevermans (MNHN Paris, France), L. Gautier and N. Fumeaux (CJB Geneva, Switzerland), M. Vorontsova (RBG Kew, UK), S. Cubey and A. Smith (RBG Edinburgh, UK), R. Prakash (NHM London, UK), E. Vitek (NHM Vienna, Austria), U. Starck and R. Vogt (BGBM Berlin, Germany), B. Gambin, F. Abdel-Samad, A. Fridlender and F. Medail (Aix-Marseille University, France), H. Akhani (Tehran University, Iran), H. Engels, B. Zehzad and C. Constantinou, and also A. Danin (Flora of Israel, Israel), L. M. Domingo (Anthos, Spain), T. Nikolic (Flora Croatica, Croatia), V. Noble (Silene, France) and A. Strid (Flora Hellenica, Greece). The authors are also grateful to M. Juin and N. Duong (IMBE) for their help in molecular experiments, and to M. Fay and two anonymous reviewers for their relevant comments. This work is included in an Interdisciplinary Program of Research Urban-Environment (PIRVE) financed by the CNRS, the Ministry of Ecology (France) and the DREAL PACA. The authors are also grateful for other financial support provided by the Research Federation ECCOREV and the Societe Botanique de France. NR 73 TC 12 Z9 12 U1 4 U2 54 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 EI 1095-8290 J9 ANN BOT-LONDON JI Ann. Bot. PD SEP PY 2014 VL 114 IS 3 BP 455 EP 462 DI 10.1093/aob/mcu143 PG 8 WC Plant Sciences SC Plant Sciences GA AQ7ZK UT WOS:000343039400003 PM 25081517 ER PT J AU Philipson, CD Dent, DH O'Brien, MJ Chamagne, J Dzulkifli, D Nilus, R Philips, S Reynolds, G Saner, P Hector, A AF Philipson, Christopher D. Dent, Daisy H. O'Brien, Michael J. Chamagne, Juliette Dzulkifli, Dzaeman Nilus, Reuben Philips, Sam Reynolds, Glen Saner, Philippe Hector, Andy TI A trait-based trade-off between growth and mortality: evidence from 15 tropical tree species using size-specific relative growth rates SO ECOLOGY AND EVOLUTION LA English DT Article DE Dipterocarpaceae; functional traits; light; nonlinear growth; plant development and life-history traits; SGR; survival; tropical lowland forest; wood density ID RAIN-FOREST; FUNCTIONAL TRAITS; SHADE TOLERANCE; SEED SIZE; HIGH IRRADIANCE; GOOD PREDICTORS; WOOD DENSITY; CHANGE RANK; PERFORMANCE; LIGHT AB A life-history trade-off between low mortality in the dark and rapid growth in the light is one of the most widely accepted mechanisms underlying plant ecological strategies in tropical forests. Differences in plant functional traits are thought to underlie these distinct ecological strategies; however, very few studies have shown relationships between functional traits and demographic rates within a functional group. We present 8years of growth and mortality data from saplings of 15 species of Dipterocarpaceae planted into logged-over forest in Malaysian Borneo, and the relationships between these demographic rates and four key functional traits: wood density, specific leaf area (SLA), seed mass, and leaf C:N ratio. Species-specific differences in growth rates were separated from seedling size effects by fitting nonlinear mixed-effects models, to repeated measurements taken on individuals at multiple time points. Mortality data were analyzed using binary logistic regressions in a mixed-effects models framework. Growth increased and mortality decreased with increasing light availability. Species differed in both their growth and mortality rates, yet there was little evidence for a statistical interaction between species and light for either response. There was a positive relationship between growth rate and the predicted probability of mortality regardless of light environment, suggesting that this relationship may be driven by a general trade-off between traits that maximize growth and traits that minimize mortality, rather than through differential species responses to light. Our results indicate that wood density is an important trait that indicates both the ability of species to grow and resistance to mortality, but no other trait was correlated with either growth or mortality. Therefore, the growth mortality trade-off among species of dipterocarp appears to be general in being independent of species crossovers in performance in different light environments. C1 [Philipson, Christopher D.] SLF, WSL Inst Snow & Avalanche Res, CH-7260 Davos, Switzerland. [Philipson, Christopher D.; O'Brien, Michael J.; Chamagne, Juliette; Dzulkifli, Dzaeman; Saner, Philippe] Univ Zurich, Inst Evolutionary Biol & Environm Studies, Zurich, Switzerland. [Dent, Daisy H.] Univ Stirling, Stirling FK9 4LA, Scotland. [Dent, Daisy H.] Smithsonian Trop Res Inst, Balboa, Panama. [Nilus, Reuben] Sepilok, Forest Res Ctr, Sandakan, Sabah, Malaysia. [Philips, Sam] Kasanka Natl Pk, Zambia, Cent Province, Zambia. [Reynolds, Glen] Danum Valley Field Ctr, Royal Soc South East Asian Rainforest Res Program, Sabah, Malaysia. [Hector, Andy] Univ Oxford, Dept Plant Sci, Oxford OX1 3RB, England. RP Philipson, CD (reprint author), SLF, WSL Inst Snow & Avalanche Res, Fluelastr 11, CH-7260 Davos, Switzerland. EM christopher.philipson@usys.ethz.ch RI Hector, Andrew/H-4199-2011; Dent, Daisy/L-3549-2016; OI Hector, Andrew/0000-0002-1309-7716; Dent, Daisy/0000-0002-1219-7344; O'Brien, Michael/0000-0003-0943-8423; Philipson, Christopher/0000-0001-8987-7260 FU Royal Society South East Asia Rainforest Research Programme [RS243] FX We thank our hard working staff at the Sabah Biodiversity Experiment, especially the site manager Philip Ulok, without whom none of this work would be possible. An earlier version of this manuscript has been greatly improved by comments from Kaoru Kitajima and Lourens Poorter. The SBE is part of the Royal Society South East Asia Rainforest Research Programme (Project No. RS243). This research is SBE manuscript number 11. NR 70 TC 10 Z9 10 U1 8 U2 71 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD SEP PY 2014 VL 4 IS 18 BP 3675 EP 3688 DI 10.1002/ece3.1186 PG 14 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AQ5KH UT WOS:000342846600015 PM 25478157 ER PT J AU Stanley, JD Clemente, PL AF Stanley, Jean-Daniel Clemente, Pablo L. TI Mica and Heavy Minerals as Markers to Map Nile Delta Coastline Displacements during the Holocene SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE Climate change; coastal processes; grain density; grain shape; human interference; Nile branches; northern delta; provenance; relative sea level; relict distributaries; salinization; shoreline shifts; sediment replenishment; subsidence ID LATE QUATERNARY EVOLUTION; CONTINENTAL-SHELF SEDIMENTS; MEDITERRANEAN COAST; ROSETTA PROMONTORY; SHORELINE CHANGES; EGYPT; ALEXANDRIA; SUBSIDENCE; PATTERNS; POSITION AB Mica and heavy minerals in sediments of Egypt's Nile Delta are examined to test if measured proportions of these two mineral groups and their distributions can be used to define former coastline positions and their shifts in time and space during the Holocene. The premise of the study is based on the sufficiently different attributes of these two components, especially their shape, density, and size, which could induce their segregation and dissimilar dispersal patterns during sediment transport. To test this hypothesis, mineralogical data from more than 1400 samples from 87 sediment cores recovered across the northern third of the delta margin were analyzed. The marked contrast in both temporal and spatial distributions of high proportions of mica and of heavy minerals indicates distinct separation occurred primarily north of the central delta, in an area from similar to 45 km south of the present shoreline to similar to 10-15 km offshore during the time span considered. Additionally, detailed examination of core sediment types demonstrates a relationship between the proportions of these two mineral groups and proportions of clay, silt, and sand fractions in which they occur near the present coast. Mica is preferentially deposited with silt and clay landward of the modern shore, while heavy mineral concentrations are generally associated with coarser silt and sand near and seaward of the shoreline. Shifts of the Nile Delta margin have been triggered by natural processes leading to insufficient sediment replenishment: relative sea-level rise involving delta plain subsidence and shoreline erosion, and intensified human activity, especially during the past two centuries, such as construction of dams, barrages, and entrapment by the delta's expanded canal system. The approach used here helps define two of the three major earlier Holocene coastal shifts, and it could be used to measure ongoing and future landward shoreline advances onto the delta plain. C1 [Stanley, Jean-Daniel; Clemente, Pablo L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, CUSP, Washington, DC 20013 USA. RP Stanley, JD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, CUSP, Washington, DC 20013 USA. EM stanleyd1@outlook.com FU National Museum of Natural History, Smithsonian Institution FX We thank the National Museum of Natural History, Smithsonian Institution, for support during preparation of this study. We also express appreciation to Drs. C. Grifa and M.R. Senatore and Ms. K.A. Corwin for their thoughtful reviews of an earlier draft of this article. NR 100 TC 1 Z9 1 U1 2 U2 9 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0749-0208 EI 1551-5036 J9 J COASTAL RES JI J. Coast. Res. PD SEP PY 2014 VL 30 IS 5 BP 904 EP 921 DI 10.2112/JCOASTRES-D-14A-00003.1 PG 18 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA AQ7BN UT WOS:000342967700004 ER PT J AU Miller, JH Behrensmeyer, AK Du, A Lyons, SK Patterson, D Toth, A Villasenor, A Kanga, E Reed, D AF Miller, Joshua H. Behrensmeyer, Anna K. Du, Andrew Lyons, S. Kathleen Patterson, David Toth, Aniko Villasenor, Amelia Kanga, Erustus Reed, Denne TI Ecological fidelity of functional traits based on species presence-absence in a modern mammalian bone assemblage (Amboseli, Kenya) SO PALEOBIOLOGY LA English DT Article ID MOLLUSCAN DEATH ASSEMBLAGES; TAPHONOMIC BIAS; MORPHOLOGICAL DIVERSIFICATION; FAUNAL IMPOVERISHMENT; TAXONOMIC DIVERSITY; SKELETAL REMAINS; AFRICAN SAVANNA; MARINE BIOTAS; TIME; ECOSYSTEM AB Comparisons between modern death assemblages and their source communities have demonstrated fidelity to species diversity across a variety of environments and taxonomic groups. However, differential species preservation and collection (including body-size bias) in both modern and fossil death assemblages may still skew the representation of other important ecological characteristics. Here, we move beyond live-dead taxonomic fidelity and focus on the recovery of functional ecology (how species interact with their ecosystem) at the community level for a diverse non-volant mammal community (87 species; Amboseli, Kenya). We use published literature to characterize species, using four functional traits and their associated categorical attributes (i) dietary mode (11 attributes; e.g., browser, grazer), (ii) preferred feeding habitat (16 attributes; e.g., grassland, woodland), (iii) preferred sheltering habitat (17 attributes; e.g., grassland, underground cavity), and (iv) activity time (7 attributes; e.g., diurnal, nocturnal, nocturnally dominated crepuscular). For each functional ecological trait we compare the death assemblage's recovered richness and abundance structure of constituent functional attributes with those of the source community, using Jaccard similarity, Spearman's rho, and the Probability of Interspecific Encounter (evenness). We use Monte Carlo simulations to evaluate whether these empirical comparisons are significantly different from expectations calculated from randomized sampling of species from the source community. Results indicate that although the Amboseli death assemblage is significantly overrepresented by large-bodied species relative to the Amboseli source community, it captures many functional dimensions of the ecosystem within expectations of a randomized collection of species. Additional resampling simulations and logistic regressions further illustrate that the size bias inherent to the Amboseli death assemblage is not a major driver of deviations between the functional ecological properties of the death assemblage and its source community. Finally, the Amboseli death assemblage also enhances our understanding of the mammal community by adding nine species and two functional attributes previously unknown from the ecosystem. C1 [Miller, Joshua H.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Miller, Joshua H.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Miller, Joshua H.] Univ Alaska Museum, Dept Geol & Geophys, Fairbanks, AK 99775 USA. [Behrensmeyer, Anna K.; Du, Andrew; Lyons, S. Kathleen; Patterson, David; Toth, Aniko; Villasenor, Amelia] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Behrensmeyer, Anna K.; Du, Andrew; Lyons, S. Kathleen; Patterson, David; Toth, Aniko; Villasenor, Amelia] Smithsonian Inst, Natl Museum Nat Hist, ETE Program, Washington, DC 20013 USA. [Du, Andrew; Patterson, David; Villasenor, Amelia] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Kanga, Erustus] Kenya Wildlife Serv, Ecosyst Conservat & Management Dept, Nairobi 00100, Kenya. [Reed, Denne] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. RP Miller, JH (reprint author), Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. EM josh.miller@uc.edu FU National Museums of Kenya; National Geographic Society [1508, 4339-90, 7525-03, 8784-10]; Smithsonian Institution; National Museum of Natural History for sustained support of the Evolution of Terrestrial Ecosystems Program FX This is publication number 290 of the Evolution of Terrestrial Ecosystems (EYE) Program at the National Museum of Natural History, Smithsonian Institution. We thank D. Western for his long-term collaboration and contributions to our understanding of Amboseli's ecology; J. Altmann, S. Alberts, and C. Moss for much appreciated collaboration and input regarding the Amboseli living ecosystem; and F. L. Odock and the Kenya Wildlife Service and the National Museums of Kenya for their support of the long-term bone survey project in Amboseli. We also thank the National Geographic Society for generous fieldwork support (Grants 1508, 4339-90, 7525-03, and 8784-10) and the Smithsonian Institution and the National Museum of Natural History for sustained support of the Evolution of Terrestrial Ecosystems Program, now in its 27th year. Discussions and suggestions by P. Novack-Gottshall, A. Tomasovych, and an anonymous reviewer greatly contributed to this study. This research grew out of a series of ETE-sponsored data analysis and simulation workshops organized by Behrensmeyer and led by Miller in 2012-2013. NR 122 TC 11 Z9 11 U1 3 U2 17 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 FAL PY 2014 VL 40 IS 4 BP 560 EP 583 DI 10.1666/13062 PG 24 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA AQ7BI UT WOS:000342967200004 ER PT J AU Blonder, B Royer, DL Johnson, KR Miller, I Enquist, BJ AF Blonder, Benjamin Royer, Dana L. Johnson, Kirk R. Miller, Ian Enquist, Brian J. TI Plant Ecological Strategies Shift Across the Cretaceous-Paleogene Boundary SO PLOS BIOLOGY LA English DT Article ID LEAF ECONOMICS SPECTRUM; TERTIARY BOUNDARY; FUNCTIONAL TRAITS; VENATION NETWORKS; MASS EXTINCTION; ATMOSPHERIC CO2; VEIN EVOLUTION; TERRESTRIAL; IMPACT; RECORD AB The Chicxulub bolide impact caused the end-Cretaceous mass extinction of plants, but the associated selectivity and ecological effects are poorly known. Using a unique set of North Dakota leaf fossil assemblages spanning 2.2 Myr across the event, we show among angiosperms a reduction of ecological strategies and selection for fast-growth strategies consistent with a hypothesized recovery from an impact winter. Leaf mass per area (carbon investment) decreased in both mean and variance, while vein density (carbon assimilation rate) increased in mean, consistent with a shift towards "fast'' growth strategies. Plant extinction from the bolide impact resulted in a shift in functional trait space that likely had broad consequences for ecosystem functioning. C1 [Blonder, Benjamin; Enquist, Brian J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Blonder, Benjamin; Enquist, Brian J.] Rocky Mt Biol Labs, Gothic, CO USA. [Royer, Dana L.] Wesleyan Univ, Dept Earth & Environm Sci, Middletown, CT USA. [Johnson, Kirk R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Miller, Ian] Denver Museum Nat & Sci, Denver, CO USA. [Enquist, Brian J.] Santa Fe Inst, Santa Fe, NM 87501 USA. RP Blonder, B (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. EM bblonder@gmail.com OI Royer, Dana/0000-0003-0976-953X; Enquist, Brian/0000-0002-6124-7096 FU Rocky Mountain Biological Laboratory graduate research fellowship; Geological Society of America student research grant; NSF pre-doctoral fellowship; NSF ATB and Macrosystems award [Macrosystems - NSF DEB 1065861, ATB - NSF EF 0742800] FX BB was supported by a Rocky Mountain Biological Laboratory graduate research fellowship, a Geological Society of America student research grant, and a NSF pre-doctoral fellowship. BE was supported by an NSF ATB and Macrosystems award (Grant numbers: Macrosystems - NSF DEB 1065861; ATB - NSF EF 0742800). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 8 Z9 8 U1 2 U2 31 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 SEP PY 2014 VL 12 IS 9 AR e1001949 DI 10.1371/journal.pbio.1001949 PG 7 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA AQ6FL UT WOS:000342905400011 PM 25225914 ER PT J AU Knowlton, JL Flaspohler, DJ Mcinerney, NCR Fleischer, RC AF Knowlton, Jessie L. Flaspohler, David J. Mcinerney, N. C. Rotzel Fleischer, Robert C. TI First Record of Hybridization in the Hawaiian Honeycreepers: 'I'iwi (Vestiaria coccinea) X 'Apapane (Himatione sanguinea) SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article DE adaptive radiation; Big Island of Hawaii; Drepanididae; intergeneric hybrid; microsatellites; 454 sequencing ID MALARIA PLASMODIUM-RELICTUM; DARWINS FINCHES; MATE CHOICE; BIRDS; SPECIATION; AMPLIFICATION; SELECTION; EVOLUTION; ANIMALS; PRIMERS AB The adaptive radiation of the Hawaiian honeycreepers is the largest ever recorded for birds on an oceanic archipelago. Despite including >50 species in 21 genera, no hybridizations across honey-creeper species have ever been confirmed. Here, we report genetic and morphological analyses that verify the first hybrid between two Hawaiian honeycreeper species: the 'I'iwi (Vestiaria coccinea) and 'Apapane (Himatione sanguinea). This hybridization is notable given that the parental species diverged similar to 1.6 mya and show distinct morphological differences. Further, this discovery is important in light of recent evidence that hybridization plays an important role in speciation and genetic diversity in both plants and animals. C1 [Knowlton, Jessie L.; Flaspohler, David J.] Michigan Technol Univ, Sch Forest Resources & Environm Sci, Houghton, MI 49931 USA. [Knowlton, Jessie L.; Mcinerney, N. C. Rotzel; Fleischer, Robert C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. RP Knowlton, JL (reprint author), Michigan Technol Univ, Sch Forest Resources & Environm Sci, 1400 Townsend Dr, Houghton, MI 49931 USA. EM jlknowlt@mtu.edu FU NSF [DEB-1019928, DEB-0643291]; NIFA McIntire-Stennis; Smithsonian Conservation Biology Institute FX We thank P. LoCicero, N. Lancaster, E. Ames, D. Rankin and O. Lansdorp for assistance in the field and J. Lock, C. Hofman and H. Lerner for information or assistance with data analysis. Funding was provided by NSF grants DEB-1019928 and DEB-0643291, NIFA McIntire-Stennis and the Smithsonian Conservation Biology Institute. NR 30 TC 1 Z9 1 U1 5 U2 26 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 SEP PY 2014 VL 126 IS 3 BP 562 EP 568 PG 7 WC Ornithology SC Zoology GA AQ6ZO UT WOS:000342962600015 ER PT J AU Sigel, EM Windham, MD Pryer, KM AF Sigel, Erin M. Windham, Michael D. Pryer, Kathleen M. TI EVIDENCE FOR RECIPROCAL ORIGINS IN POLYPODIUM HESPERIUM (POLYPODIACEAE): A FERN MODEL SYSTEM FOR INVESTIGATING HOW MULTIPLE ORIGINS SHAPE ALLOPOLYPLOID GENOMES SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE allopolyploidy; biogeography; gapCp; multiple origins; plastid haplotype; Polypodiaceae; Polypodium vulgare complex ID LAST GLACIAL MAXIMUM; CHLOROPLAST DNA; PHYLOGENETIC ANALYSES; POLYPLOID SPECIATION; MATERNAL INHERITANCE; RETICULATE EVOLUTION; COMPLEX PTERIDACEAE; VULGARE COMPLEX; PLANTS; TRAGOPOGON AB Premise of the study: Many polyploid species are composed of distinct lineages originating from multiple, independent polyploidization events. In the case of allopolyploids, reciprocal crosses between the same progenitor species can yield lineages with different uniparentally inherited plastid genomes. While likely common, there are few well-documented examples of such reciprocal origins. Here we examine a case of reciprocal allopolyploid origins in the fern Polypodium hesperium and present it as a natural model system for investigating the evolutionary potential of duplicated genomes. Methods: Using a combination of uniparentally inherited plastid and biparentally inherited nuclear sequence data, we investigated the distributions and relative ages of reciprocally formed lineages in Polypodium hesperium, an allotetraploid fern that is broadly distributed in western North America. Key results: The reciprocally derived plastid haplotypes of Polypodium hesperium are allopatric, with populations north and south of 42 degrees N latitude having different plastid genomes. Incorporating biogeographic information and previously estimated ages for the diversification of its diploid progenitors, we estimate middle to late Pleistocene origins of P. hesperium. Conclusions: Several features of Polypodium hesperium make it a particularly promising system for investigating the evolutionary consequences of allopolyploidy. These include reciprocally derived lineages with disjunct geographic distributions, recent time of origin, and extant diploid progenitors. C1 [Sigel, Erin M.; Windham, Michael D.; Pryer, Kathleen M.] Duke Univ, Dept Biol, Durham, NC 27708 USA. RP Sigel, EM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, POB 37012, Washington, DC 20013 USA. EM SigelEM@si.edu FU NSF [DEB-1110775]; Sigma Xi; American Society of Plant Taxonomists FX We thank A. Grusz, L. Huiet, T.-T. Kao, F.-W. Li, and K. Picard for their comments and edits on earlier versions of this manuscript, as well as the staff of the ALA, DUKE, E, MO, UC, and US herbaria for use of specimens. Our gratitude goes to UCBG and RBGE for allowing access to their live collections, and to A. Ebihara, L. Huiet, C. J. Rothfels, and A. L. Vernon, who collected specimens specifically for this work. This manuscript was significantly improved by the comments of two anonymous reviewers. This research was funded in part by an NSF Doctoral Dissertation Improvement Grant to K. M. P. and E. M. S. (DEB-1110775), a Sigma Xi Grant-in-Aid of Research to E. M. S, and a Graduate Student Research Grant to E. M. S. from The American Society of Plant Taxonomists. This article is part of E.M.S.'s doctoral dissertation in Biology at Duke University. NR 70 TC 7 Z9 8 U1 4 U2 13 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 SEP PY 2014 VL 101 IS 9 BP 1476 EP 1485 DI 10.3732/ajb.1400190 PG 10 WC Plant Sciences SC Plant Sciences GA AQ1IW UT WOS:000342536100009 PM 25253708 ER PT J AU Halfwerk, W Dixon, MM Ottens, KJ Taylor, RC Ryan, MJ Page, RA Jones, PL AF Halfwerk, Wouter Dixon, Marjorie M. Ottens, Kristina J. Taylor, Ryan C. Ryan, Michael J. Page, Rachel A. Jones, Patricia L. TI Risks of multimodal signaling: bat predators attend to dynamic motion in frog sexual displays SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Multimodal communication; Eavesdropping; Signal evolution; Co-option; Motion detection; Trachops cirrhosus ID PREY DETECTION; FORAGING BEHAVIOR; EATING BATS; PHYSALAEMUS-PUSTULOSUS; ECHOLOCATING BATS; TRAWLING BATS; MATE CHOICE; COMMUNICATION; CUES; SENSITIVITY AB Many sexual displays contain multiple components that are received through a variety of sensory modalities. Primary and secondary signal components can interact to induce novel receiver responses and become targets of sexual selection as complex signals. However, predators can also use these complex signals for prey assessment, which may limit the evolution of elaborate sexual signals. We tested whether a multimodal sexual display of the male tungara frog (Physalaemus pustulosus) increases predation risk from the fringe-lipped bat (Trachops cirrhosus) when compared with a unimodal display. We gave bats a choice to attack one of two frog models: a model with a vocal sac moving in synchrony with a mating call (multisensory cue), or a control model with the call but no vocal sac movement (unimodal cue). Bats preferred to attack the model associated with the multimodal display. Furthermore, we determined that bats perceive the vocal sac using echolocation rather than visual cues. Our data illustrate the costs associated with multimodal signaling and that sexual and natural selection pressures on the same trait are not always mediated through the same sensory modalities. These data are important when considering the role of environmental fluctuations on signal evolution as different sensory modalities will be differentially affected. C1 [Halfwerk, Wouter; Dixon, Marjorie M.; Ottens, Kristina J.; Ryan, Michael J.; Page, Rachel A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Taylor, Ryan C.] Salisbury Univ, Dept Biol, Salisbury, MD 21801 USA. [Ryan, Michael J.; Jones, Patricia L.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. RP Halfwerk, W (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM wouter.halfwerk@gmail.com FU Netherlands Organisation for Scientific Research [825.11.026]; National Science Foundation [IBN 0517328] FX The research was funded through an Netherlands Organisation for Scientific Research grant (no. 825.11.026) to W.H. and a National Science Foundation grant (IBN 0517328) to R.C.T., M.J.R. and R.A.P. NR 46 TC 7 Z9 8 U1 7 U2 50 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 SEP PY 2014 VL 217 IS 17 BP 3038 EP 3044 DI 10.1242/jeb.107482 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AQ0XJ UT WOS:000342505700016 PM 25165134 ER PT J AU Campione, NE Evans, DC Brown, CM Carrano, MT AF Campione, Nicolas E. Evans, David C. Brown, Caleb M. Carrano, Matthew T. TI Body mass estimation in non-avian bipeds using a theoretical conversion to quadruped stylopodial proportions SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE body mass estimation; dinosaurian; evolutionary biology; linear models; macroevolution; software; statistics; terrestrial bipeds ID LONG BONES; DINOSAURS; SIZE; EVOLUTION; LIMB; LOCOMOTION; BIRDS; MAMMALS; ORIGIN; MORPHOLOGY AB Body mass is strongly related to both physiological and ecological properties of living organisms. As a result, generating robust, broadly applicable models for estimating body mass in the fossil record provides the opportunity to reconstruct palaeobiology and investigate evolutionary ecology on a large temporal scale. A recent study provided strong evidence that the minimum circumference of stylopodial elements (humerus and femur) is conservatively associated with body mass in living quadrupeds. Unfortunately, this model is not directly applicable to extinct bipeds, such as non-avian dinosaurs. This study presents a new equation that mathematically corrects the quadruped equation for use in bipeds. It is derived from the systemic difference in the circumference-to-area scaling relationship of two circles (hypothetical quadruped) and one circle (hypothetical biped), which represent the cross-section of the main weight-bearing limb bones. When applied to a newly constructed data set of femoral circumferences and body masses in living birds, the new equation reveals errors that are significantly lower than other published equations, but significantly higher than the error inherent in the avian data set. Such errors, however, are expected given the unique overall femoral circumference-body mass scaling relationship found in birds. Body mass estimates for a sample of bipedal dinosaurs using the new model are consistent with recent estimates based on volumetric life reconstructions, but, in contrast, this equation is simpler to use, with the concomitant potential to provide a wider set of body mass estimates for extinct bipeds. Although it is evident that no one estimation model is flawless, the combined use of the corrected quadrupedal equations and the previously published quadrupedal equation offer a consistent approach with which to estimate body masses in both quadrupeds and bipeds. These models have implications for conducting large-scale macroevolutionary analyses of body size throughout the evolutionary history of terrestrial vertebrates, and, in particular, across major changes in body plan, such as the evolution of bipedality in archosaurs and quadrupedality in dinosaurs. C1 [Campione, Nicolas E.; Evans, David C.; Brown, Caleb M.] Univ Toronto, Dept Ecol & Evolutionary Biol, Toronto, ON M5S 3B2, Canada. [Campione, Nicolas E.] Uppsala Univ, Palaeobiol Programme, Dept Earth Sci, SE-75236 Uppsala, Sweden. [Campione, Nicolas E.] Uppsala Univ, Subdept Evolut & Dev, Dept Organismal Biol, SE-75236 Uppsala, Sweden. [Evans, David C.] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. [Brown, Caleb M.] Royal Tyrrell Museum Palaeontol, Drumheller, AB T0J 0Y0, Canada. [Carrano, Matthew T.] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA. RP Campione, NE (reprint author), Univ Toronto, Dept Ecol & Evolutionary Biol, 25 Willcocks St, Toronto, ON M5S 3B2, Canada. EM nicolas.campione@geo.uu.se RI Carrano, Matthew/C-7601-2011 OI Carrano, Matthew/0000-0003-2129-1612 FU NSERC FX We thank M. Peck, O. Haddrath, A. Baker, K. Seymour and B. Iwama for access to ROM collections. Special thanks to R. Kim and G. Oliveira Cunha for the assistance collecting the ROM bird data, M. Ryan (CMNH) for providing femoral measurements from a human sample and J. L. Carballido for providing a circumference measurement for Tyrannotitan. Thanks also to R. Benson, R. Blob, A. Dececchi, J. Hutchinson, H. Larsson, R. Reisz and M. Silcox for discussions related to this project. Thanks also to the members of the Evans and Reisz laboratories for their support and discussions. Finally, we greatly appreciate the comments made by the editors, R. Freckleton and L. Revell, and reviewers, J. Hutchinson and two anonymous, that improved the quality of the manuscript. Funding for this project was provided by an NSERC Postgraduate Scholarship and Queen Elizabeth II Graduate Scholarship in Science and Technology (to NEC), an NSERC Discovery Grant (to NEC) and an NSERC Canadian Graduate Scholarship (to CMB). NR 66 TC 14 Z9 15 U1 2 U2 26 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD SEP PY 2014 VL 5 IS 9 BP 913 EP 923 DI 10.1111/2041-210X.12226 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AQ3VR UT WOS:000342722100008 ER PT J AU Puillandre, N Bouchet, P Duda, TF Kauferstein, S Kohn, AJ Olivera, BM Watkins, M Meyer, C AF Puillandre, N. Bouchet, P. Duda, T. F., Jr. Kauferstein, S. Kohn, A. J. Olivera, B. M. Watkins, M. Meyer, C. TI Molecular phylogeny and evolution of the cone snails (Gastropoda, Conoidea) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ancestral state reconstruction; Conidae; Conus; COI; 16SrRNA; 12SrRNA ID TROPICAL MARINE GASTROPOD; INDO-WEST PACIFIC; CAPE-VERDE CONUS; GENUS CONUS; ADAPTIVE EVOLUTION; VENOM EVOLUTION; EASTER-ISLAND; CLASSIFICATION; DIVERSITY; DNA AB We present a large-scale molecular phylogeny that includes 320 of the 761 recognized valid species of the cone snails (Conus), one of the most diverse groups of marine molluscs, based on three mitochondrial genes (COI, 16S rDNA and 12S rDNA). This is the first phylogeny of the taxon to employ concatenated sequences of several genes, and it includes more than twice as many species as the last published molecular phylogeny of the entire group nearly a decade ago. Most of the numerous molecular phylogenies published during the last 15 years are limited to rather small fractions of its species diversity. Bayesian and maximum likelihood analyses are mostly congruent and confirm the presence of three previously reported highly divergent lineages among cone snails, and one identified here using molecular data. About 85% of the species cluster in the single Large Major Cade; the others are divided between the Small Major Cade (similar to 12%), the Conus califomicus lineage (one species), and a newly defined clade (similar to 3%). We also define several subclades within the Large and Small major clades, but most of their relationships remain poorly supported. To illustrate the usefulness of molecular phylogenies in addressing specific evolutionary questions, we analyse the evolution of the diet, the biogeography and the toxins of cone snails. All cone snails whose feeding biology is known inject venom into large prey animals and swallow them whole. Predation on polychaete worms is inferred as the ancestral state, and diet shifts to molluscs and fishes occurred rarely. The ancestor of cone snails probably originated from the Indo-Pacific; rather few colonisations of other biogeographic provinces have probably occurred. A new classification of the Conidae, based on the molecular phylogeny, is published in an accompanying paper. (C) 2014 Elsevier Inc. All rights reserved. C1 [Puillandre, N.; Bouchet, P.] UPMC MNHN EPHE, ISyEB Inst, Dept Systemat & Evolut, Museum Natl Hist Nat,UMR CNRS 7205, F-75231 Paris, France. [Duda, T. F., Jr.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Duda, T. F., Jr.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Duda, T. F., Jr.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Kauferstein, S.] Goethe Univ Frankfurt, Inst Legal Med, D-60596 Frankfurt, Germany. [Kohn, A. J.] Univ Washington, Dept Biol, Seattle, WA 98195 USA. [Olivera, B. M.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Watkins, M.] Univ Utah, Dept Pathol, Salt Lake City, UT 84112 USA. [Meyer, C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Puillandre, N (reprint author), UPMC MNHN EPHE, ISyEB Inst, Dept Systemat & Evolut, Museum Natl Hist Nat,UMR CNRS 7205, 43 Rue Cuvier, F-75231 Paris, France. EM puillandre@mnhn.fr; pbouchet@mnhn.fr; tfduda@umich.edu; kauferstein@em.uni-frankfurt.de; kohn@uw.edu; olivera@biology.utah.edu; maren.watkins@hsc.utah.edu; MeyerC@si.edu FU Total Foundation; French Ministry of Foreign Affairs; Stavros Niarchos Foundation; Lounsbery Foundation; Prince Albert II of Monaco Foundation; Pro-Natura International (PNI); U.S. National Science Foundation [0316338]; Service de Systematique Moleculaire [UMS 2700 CNRS-MNHN]; network "Bibliotheque du Vivant" - CNRS; Museum National d'Histoire Naturelle; INRA; CEA (Centre National de Sequencage); NIH [GM48677]; Fogarty (NIH) [1U01TWO08163]; CONOTAX - French "Agence Nationale de la Recherche" [ANR-13-JSV7-0013-01] FX The PANGLAO 2004 Marine Biodiversity Project was funded by the Total Foundation and the French Ministry of Foreign Affairs; The PANGLAO 2005 cruise on board M/V DA-BFAR associated the USC, MNHN (co-PI Philippe Bouchet) and the Philippines Bureau of Fisheries and Aquatic Research (BFAR; co-PI Ludivina Labe); the MNHN-IRD-PNI Santo 2006 expedition was made possible by grants, among others, from the Total Foundation and the Stavros Niarchos Foundation; the AURORA 2007 cruise was made possible through a grant from the Lounsbery Foundation; The Miriky and Atimo Vatae expeditions were funded by the Total Foundation, Prince Albert II of Monaco Foundation, and Stavros Niarchos Foundation, and conducted by MNHN and Pro-Natura International (PNI) as part of their "Our Planet Reviewed" programme; the Coral Sea and Solomon Islands cruises took place on board R/V Alis deployed from Noumea by the Institut de Recherche pour le Developpement (IRD), and. Bertrand Richer de Forges and Sarah Samadi were cruise leaders for the Solomons, Coral Sea and Vanuatu expeditions. U.S. National Science Foundation Grant 0316338 supported the contributions of AJK, TFD, and CPM. Ellen Strong, Marie-Catherine Boisselier and Sarah Samadi are thanked for their role in molecular sampling during these expeditions. This work was supported the Service de Systematique Moleculaire (UMS 2700 CNRS-MNHN), the network "Bibliotheque du Vivant" funded by the CNRS, the Museum National d'Histoire Naturelle, the INRA and the CEA (Centre National de Sequencage) and the NIH program project grant (GM48677), as well as partial support from the ICBG grant (1U01TWO08163) from Fogarty (NIH). The phylogenetic analyses were performed on the MNHN cluster (UMS 2700 CNRSMNHN). This work was partly supported by the project CONOTAX, funded by the French "Agence Nationale de la Recherche" (grant number ANR-13-JSV7-0013-01). The authors also thank Barbara Buge, Virginie Heros, and Julien Brisset for curation of the voucher specimens in the MNHN and Eric Monnier, Loic Limpalaer and Manuel Tenorio who helped in identifying the specimens. NR 69 TC 40 Z9 42 U1 12 U2 76 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 2014 VL 78 BP 290 EP 303 DI 10.1016/j.ympev.2014.05.023 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AQ0NQ UT WOS:000342480400026 PM 24878223 ER PT J AU Frye, JA Frye, CT Suman, TW AF Frye, Jennifer A. Frye, Christopher T. Suman, Theodore W. TI The Ant Fauna of Inland Sand Dune Communities in Worcester County, Maryland SO NORTHEASTERN NATURALIST LA English DT Article ID PRENOLEPIS-IMPARIS SAY; HYMENOPTERA-FORMICIDAE; UNITED-STATES; BIODIVERSITY; REVISION; INSECT; GUILD; USA AB Ants inhabiting inland dune and ridge woodlands in Worcester County, MD, were surveyed in 2008 and 2009 using a combination of pitfall traps and litter samples. We employed both methods in 2008 and pitfall traps only in 2009. Thirty dune sites were targeted for survey work. We collected and identified a total of 44,930 ants representing 67 species. Data on annual and seasonal variation in the ant community are reported, as is variation in species composition based on trapping method. Expanding survey efforts to include multiple years, seasons, and trapping methodology served to increase the overall number of species encountered primarily through documenting the presence of rare or infrequent species. We provide a list of ant species collected from inland dune and ridge woodlands and discuss the significance of apparent habitat-restricted species. C1 [Frye, Jennifer A.; Frye, Christopher T.] Wildlife & Heritage Serv, Maryland Dept Nat Resources, Nat Heritage Program, Wye Mills, MD 21601 USA. [Suman, Theodore W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Frye, JA (reprint author), Wildlife & Heritage Serv, Maryland Dept Nat Resources, Nat Heritage Program, 909 Wye Mills Rd, Wye Mills, MD 21601 USA. EM jfrye@dnr.state.md.us FU State Wildlife Grant FX We thank the land managers of Chesapeake Forest, Pocomoke State Forest, Shad Landing State Park, and The Nature Conservancy for allowing us to conduct surveys on those properties; Paula Becker, Dana Limpert, Amanda Accamando, Andy Kough, Sarah Majerowicz, and numerous DNR volunteers for assisting with data collection and specimen processing; John LaPolla and Tim Foard for reviewing an early draft of the manuscript; and Ted Schultz, of the Smithsonian NMNH Ant Lab and an anonymous reviewer for providing comments on the final manuscript. We also thank Ted Schultz for allowing us access to the NMNH ant collection and for adding our specimens to the collection. This project was funded through a State Wildlife Grant administered by the USFWS. NR 77 TC 0 Z9 0 U1 3 U2 7 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 EI 1938-5307 J9 NORTHEAST NAT JI Northeast. Nat PD SEP PY 2014 VL 21 IS 3 BP 446 EP 471 DI 10.1656/045.021.0311 PG 26 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AQ0QS UT WOS:000342488400013 ER PT J AU Olson, SL AF Olson, Storrs L. TI Tracks of a Stilt-like Bird from the Early Eocene Green River Formation of Utah: Possible Earliest Evidence of the Recurvirostridae (Charadriiformes) SO WATERBIRDS LA English DT Article DE Cladorhynchus; Eocene; flamingos; Himantopus; ichnology; Juncitarsus; Phoenicopteridae; Presbyornis; Recurvirostridae AB Three avian footprints from a well-known early Eocene fossil track locality in Utah appear to represent an otherwise unknown stilt-like bird, possibly referable to the Recurvirostridae. The bird that made these tracks had very long legs but relatively short toes and was probably somewhat smaller than modern stilts (Himantopus). There was a vestigial hind toe and the feet were webbed, but the webbing was reduced more than in Recurvirostra or Cladorhynchus, but not nearly as much as in Himantopus. This may constitute the oldest evidence yet found of a recurvirostid-like bird, although the family probably originated even earlier if it gave rise to flamingos (Phoenicopteridae), which were already in existence by the early and middle Eocene. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 17 TC 1 Z9 1 U1 2 U2 4 PU WATERBIRD SOC PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 1524-4695 EI 1938-5390 J9 WATERBIRDS JI Waterbirds PD SEP PY 2014 VL 37 IS 3 BP 340 EP 345 PG 6 WC Ornithology SC Zoology GA AQ0LY UT WOS:000342476000012 ER PT J AU Wei, N Dick, CW AF Wei, Na Dick, Christopher W. TI POLYMORPHIC MICROSATELLITE MARKERS FOR A WIND-DISPERSED TROPICAL TREE SPECIES, TRIPLARIS CUMINGIANA (POLYGONACEAE) SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE gene flow; microsatellite marker; PacBio sequencing platform; single-molecule real-time sequencing; Triplaris cumingiana; wind dispersal ID SOFTWARE AB Premise of the study: Novel microsatellite markers were characterized in the wind-dispersed and dioecious neotropical tree Triplaris cumingiana (Polygonaceae) for use in understanding the ecological processes and genetic impacts of pollen-and seed-mediated gene flow in tropical forests. Methods and Results: Sixty-two microsatellite primer pairs were screened, from which 12 markers showing five or more alleles per locus (range 5-17) were tested on 47 individuals. Observed and expected heterozygosities averaged 0.692 and 0.731, respectively. Polymorphism information content was between 0.417 and 0.874. Linkage disequilibrium was observed in one of the 66 pairwise comparisons between loci. Two loci showed deviation from Hardy-Weinberg equilibrium. An additional 14 markers exhibiting lower polymorphism were characterized on a smaller number of individuals. Conclusions: These microsatellite markers have high levels of polymorphism and reproducibility and will be useful in studying gene flow and population structure in T. cumingiana. C1 [Wei, Na; Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Wei, N (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 830 North Univ Ave, Ann Arbor, MI 48109 USA. EM weina@umich.edu RI Dick, Christopher/A-8744-2008 FU CTFS-ForestGEO grant from the Smithsonian Tropical Research Institute; Center for Tropical Forest Science FX This work was supported by a CTFS-ForestGEO grant from the Smithsonian Tropical Research Institute and the Center for Tropical Forest Science. NR 10 TC 0 Z9 0 U1 0 U2 6 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD SEP PY 2014 VL 2 IS 9 AR 1400051 DI 10.3732/apps.1400051 PG 3 WC Plant Sciences SC Plant Sciences GA AQ1SJ UT WOS:000342561000007 ER PT J AU O'Mara, MT Dechmann, DKN Page, RA AF Teague O'Mara, M. Dechmann, Dina K. N. Page, Rachel A. TI Frugivorous bats evaluate the quality of social information when choosing novel foods SO BEHAVIORAL ECOLOGY LA English DT Article DE information center; public information; roost; social learning ID LEARNING STRATEGIES TOURNAMENT; FRUIT-EATING BATS; CENTER HYPOTHESIS; PUBLIC INFORMATION; PREFERENCES; RATS; TRANSMISSION; EVOLUTION; DYNAMICS; INSIGHTS AB The ability to discriminate information quality from multiple social partners may be essential to animals that use social cues in deciding when, where, and what to eat. This may be particularly important in species that rely on ephemeral and widely dispersed resources. We show that tent-making bats, Uroderma bilobatum, socially acquire preferences for novel foods through interactions with roostmates both in captivity and in natural roosts and that these food cues can influence roostmates' decisions at least for several days. More importantly, these bats can distinguish between the quality and information content of 2 different cues that are brought back to their roost. Inexperienced individuals prefer food that has been consumed by a roostmate to food whose odor is present only on the fur of a roostmate that has eaten sugar water. The ability of bats to discriminate odors on breath and fur may allow them to select the most informative cues about the presence or renewed availability of dispersed resources. This selectivity may help stabilize roosts as information centers for the social acquisition of updated information on unpredictable and widely distributed food items. C1 [Teague O'Mara, M.; Dechmann, Dina K. N.; Page, Rachel A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Teague O'Mara, M.] Univ Konstanz, Zukunftskolleg, D-78464 Constance, Germany. [Teague O'Mara, M.; Dechmann, Dina K. N.] Univ Konstanz, Dept Biol, D-78464 Constance, Germany. [Teague O'Mara, M.; Dechmann, Dina K. N.] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. [Teague O'Mara, M.] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. RP O'Mara, MT (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama. EM tomara@orn.mpg.de FU Smithsonian Tropical Research Institute FX Funding was provided by the Smithsonian Tropical Research Institute. NR 50 TC 7 Z9 7 U1 3 U2 30 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1045-2249 EI 1465-7279 J9 BEHAV ECOL JI Behav. Ecol. PD SEP-OCT PY 2014 VL 25 IS 5 BP 1233 EP 1239 DI 10.1093/beheco/aru120 PG 7 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA AP8WN UT WOS:000342360200031 ER PT J AU Dutra, GM de Santana, CD Vari, RP Wosiacki, WB AF Dutra, Guilherme Moreira de Santana, Carlos David Vari, Richard P. Wosiacki, Wolmar Benjamin TI The South American Electric Glass Knifefish Genus Distocyclus (Gymnotiformes: Sternopygidae): Redefinition and Revision SO COPEIA LA English DT Article ID RHABDOLICHOPS GYMNOTIFORMES; PHYLOGENETIC POSITION; FISH ASSEMBLAGES; TELEOSTEI; BRAZIL AB Electric glass knifefishes of the genus Distocyclus, family Sternopygidae, are reviewed. Features previously utilized to diagnose Distocyclus were found uninformative as to whether the two species originally assigned to the genus are sister taxa. Distocyclus goajira was found to lack the derived features present in the type-species of the genus, D. conirostris and instead shares derived features with Archolaemus, Eigenmannia, and/or lapigny; however, the relationships of Distocyclus goajira among those genera cannot be resolved. In light of this evidence, Distocyclus is restricted to its type species, D. conirostris, which is defined on a series of derived characters, and D. goajira is assigned as incertae sedis in the Eigenmanniinae under a new combination of "Eigenmannia" goajira. Distocyclus conirostris is redescribed on the basis of multiple samples from across the Amazon, Essequibo, and Orinoco river basins. C1 [Dutra, Guilherme Moreira; Wosiacki, Wolmar Benjamin] Museu Paraense Emilio Goeldi, BR-66040170 Belem, PA, Brazil. [de Santana, Carlos David; Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. RP Dutra, GM (reprint author), Museu Paraense Emilio Goeldi, Caixa Postal 399, BR-66040170 Belem, PA, Brazil. EM guilhermedutr@yahoo.com.br; wolmar@museu-goeldi.br RI Wosiacki, Wolmar/I-1724-2012 OI Wosiacki, Wolmar/0000-0002-4013-8501 FU Herbert R. and Evelyn Axelrod Chair Systematic Ichthyology of the National Museum of Natural History; Smithsonian Institution; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [245310/2012-6, 304754/2011-0]; CNPq/Ciencia Sem Fronteiras [245622/2012-8] FX We thank B. Brown (AMNH); J. Maclaine (BMNH); D. Catania (CAS); C. Uribe (IAvH); C. Taylor (INHS); L. Rapp Py-Daniel and R. de Oliveira (INPA); Z. Lucena and C. Lucena (MCP); K. Hartel (MCZ); M. Britto (MNRJ); J. Figueiredo and M. Gianetti (MZUSP); and L. Malabarba (UFRGS) for the loan of specimens and assistance during visits to their institutions. S. Raredon assisted with radiographs and produced Figure 1. Funding for the research was provided to RPV and CDS by the Herbert R. and Evelyn Axelrod Chair Systematic Ichthyology of the National Museum of Natural History, Smithsonian Institution. GMD thanks the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) for support and the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) for funding a visit to the Smithsonian Institution through the Programa Ciencia sem Fronteiras (245310/2012-6). CDS was supported by a Postdoctoral Fellowship from the CNPq/Ciencia Sem Fronteiras (245622/2012-8). WBW thanks the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) for the continuing support (process #304754/2011-0). NR 49 TC 3 Z9 5 U1 1 U2 5 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP PY 2014 IS 2 BP 345 EP 354 DI 10.1643/CI-13-066 PG 10 WC Zoology SC Zoology GA AP8NK UT WOS:000342335500019 ER PT J AU Hilton, EJ Smith, DG AF Hilton, Eric J. Smith, David G. TI The Second 50 Years of the American Society of Ichthyologists and Herpetologists: Personal Reflections on the ASIH from Bruce B. Collette SO COPEIA LA English DT Editorial Material ID GENUS ZENARCHOPTERUS; TELEOSTEI; HALFBEAKS; HEMIRAMPHIDAE; BIOGEOGRAPHY; NEEDLEFISH; GUINEA C1 [Hilton, Eric J.] Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Smith, David G.] Museum Support Ctr, Smithsonian Inst, Suitland, MD 20746 USA. RP Hilton, EJ (reprint author), Coll William & Mary, Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. EM ehilton@vims.edu; smithd@si.edu NR 91 TC 1 Z9 1 U1 0 U2 3 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP PY 2014 IS 2 BP 372 EP 380 DI 10.1643/OT-14-070 PG 9 WC Zoology SC Zoology GA AP8NK UT WOS:000342335500022 ER PT J AU Poore, GCB Ahyong, ST Bracken-Grissom, HD Chan, TY Chu, KH Crandall, KA Dworschak, PC Felder, DL Feldmann, RM Hyzny, M Karasawa, E Lemaitre, R Komai, T Li, XZ Mantelatto, FL Martin, JW Nguyen, NH Robles, R Schweitzer, CE Tamaki, A Tsang, LM Tudge, CC AF Poore, Gary. C. B. Ahyong, Shane T. Bracken-Grissom, Heather D. Chan, Tin-Yam Chu, Ka H. Crandall, Keith A. Dworschak, Peter C. Felder, Darryl L. Feldmann, Rodney M. Hyzny, Matus Karasawa, Eroaki Lemaitre, Rafael Komai, Tomoyuki Li, Xinzheng Mantelatto, Fernando L. Martin, Joel W. Nguyen Ngoc-Ho Robles, Rafael Schweitzer, Carrie E. Tamaki, Akio Tsang, Ling M. Tudge, Christopher C. TI ON STABILISING THE NAMES OF THE INFRAORDERS OF THALASSINIDEAN SHRIMPS, AXIIDEA DE SAINT LAURENT, 1979 AND GEBIIDEA DE SAINT LAURENT, 1979 (DECAPODA) SO CRUSTACEANA LA English DT Article ID MOSCOW UNIVERSITY DECAPODA; CRUSTACEA DECAPODA; GHOST SHRIMP; RED-SEA; MORPHOLOGICAL EVOLUTION; CALLIANASSOIDEA DANA; MOLECULAR PHYLOGENY; ZOOLOGICAL MUSEUM; DIVERGENCE TIME; MIDDLE MIOCENE AB The names Gebiidea and Axiidea, erected by de Saint Laurent (1979), have priority over others for the two infraorders of shrimps previously included in Thalassinidea. Importantly, Thalassinidea are not monophyletic and the name should be replaced. Gebiidea and Axiidea, besides having priority and describing two monophyletic taxa, are now in common use (130 citations) and are more stable than alternative schemes proposed by Sakai (2005 and later). The history of the names of higher taxa applied to these groups is reviewed, and all family-group taxa listed. C1 [Poore, Gary. C. B.] Museum Victoria, Melbourne, Vic 3000, Australia. [Ahyong, Shane T.] Australian Museum, Sydney, NSW 2010, Australia. [Ahyong, Shane T.] Univ New S Wales, Sch Biol Earth & Environm Sci, Kensington, NSW 2052, Australia. [Bracken-Grissom, Heather D.] Florida Int Univ, North Miami, FL 33181 USA. [Chan, Tin-Yam; Tsang, Ling M.] Natl Taiwan Ocean Univ, Inst Marine Biol, Keelung 202, Taiwan. [Chan, Tin-Yam; Tsang, Ling M.] Natl Taiwan Ocean Univ, Ctr Excellence Oceans, Keelung 202, Taiwan. [Chu, Ka H.] Chinese Univ Hong Kong, Sch Life Sci, Simon FS Li Marine Sci Lab, Shatin, Hong Kong, Peoples R China. [Crandall, Keith A.] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Crandall, Keith A.; Lemaitre, Rafael; Tudge, Christopher C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Dworschak, Peter C.] Nat Hist Museum, Dritte Zool Abt, A-1010 Vienna, Austria. [Felder, Darryl L.; Robles, Rafael] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Feldmann, Rodney M.] Kent State Univ, Dept Geol, Kent, OH 44240 USA. [Hyzny, Matus] Nat Hist Museum, Geol Palaontol Abt, A-1010 Vienna, Austria. [Hyzny, Matus] Comenius Univ, Fac Nat Sci, Dept Geol & Paleontol, SK-84215 Bratislava, Slovakia. [Karasawa, Eroaki] Mizunami Fossil Museum, Gifu 5096132, Japan. [Komai, Tomoyuki] Nat Hist Museum & Inst, Chuo Ku, Chiba 2608682, Japan. [Li, Xinzheng] Chinese Acad Sci, Inst Oceanol, Qingdao 266071, Peoples R China. [Mantelatto, Fernando L.; Robles, Rafael] Univ Sao Paulo, Fac Philosophy Sci & Letters Ribeirao Preto FFCLR, Lab Bioecol & Crustacean Systemat LBSC, BR-14040901 Ribeirao Preto, SP, Brazil. [Martin, Joel W.] Nat Hist Museum Los Angeles Cty, Los Angeles, CA 90007 USA. [Nguyen Ngoc-Ho] Museum Natl Hist Nat, F-75231 Paris, France. [Schweitzer, Carrie E.] Kent State Univ Stark, Dept Geol, North Canton, OH 44720 USA. [Tamaki, Akio] Nagasaki Univ, Grad Sch Fisheries Sci & Environm Studies, Nagasaki 8528521, Japan. [Tudge, Christopher C.] Amer Univ, Dept Biol, Washington, DC 20016 USA. RP Poore, GCB (reprint author), Museum Victoria, GPO Box 666, Melbourne, Vic 3000, Australia. EM gpoore@museum.vic.gov.au RI Chu, Ka Hou/B-8010-2011; Mantelatto, Fernando/H-2695-2012; Robles, Rafael/F-1967-2010; OI Chu, Ka Hou/0000-0001-8107-5415; Mantelatto, Fernando/0000-0002-8497-187X; Crandall, Keith/0000-0002-0836-3389 FU U.S. National Science Foundation [DEB-0315995, EF-0531603]; NSF [DEB/AToL 0531670, EAR-1223206]; Slovak Research and Development Agency [APVV-0436-12]; Fernando Mantelatto [2013/05663-8, 2010/50188-8] FX This study was supported under funding from the U.S. National Science Foundation to D. Felder (BS&I grant no. DEB-0315995 and DEB/AToL grant no. EF-0531603). Extensive work on diversity and classification of fossil Axiidea and Gebiidea has been conducted under NSF grants DEB/AToL 0531670 to Feldmann and Schweitzer and EAR-1223206 to Schweitzer and Feldmann. Studies on fossil ghost shrimps of the families Callianassidae and Ctenochelidae were supported by the Slovak Research and Development Agency under the contract no. APVV-0436-12 to M. Hyzny Rafael Robles and Fernando Mantelatto received support (Postdoctoral fellowship 2013/05663-8 and Grant no. 2010/50188-8) from a multidisciplinary research project Tematico BIOTA FAPESP (Fundacao de Amparo a Pesquisa do Estado de Sao Paulo, Brazil), which aims to produce a fine-scale assessment of the marine decapod biodiversity. NR 89 TC 8 Z9 9 U1 2 U2 13 PU BRILL ACADEMIC PUBLISHERS PI LEIDEN PA PLANTIJNSTRAAT 2, P O BOX 9000, 2300 PA LEIDEN, NETHERLANDS SN 0011-216X EI 1568-5403 J9 CRUSTACEANA JI Crustaceana PD SEP PY 2014 VL 87 IS 10 BP 1258 EP 1272 DI 10.1163/15685403-00003354 PG 15 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AP8MD UT WOS:000342332200008 ER PT J AU Sapijanskas, J Paquette, A Potvin, C Kunert, N Loreau, M AF Sapijanskas, Jurgis Paquette, Alain Potvin, Catherine Kunert, Norbert Loreau, Michel TI Tropical tree diversity enhances light capture through crown plasticity and spatial and temporal niche differences SO ECOLOGY LA English DT Article DE biodiversity; crown; ecosystem functioning; intraspecific diversity; light competition; niche differences; overyielding; phenology; phenotypic plasticity; plantation; Sardinilla project, Panama; tree ID SPECIES RICHNESS; ECOSYSTEM FUNCTION; BIODIVERSITY EXPERIMENTS; PHENOTYPIC PLASTICITY; FUNCTIONAL DIVERSITY; LITTER PRODUCTION; BRITISH-COLUMBIA; NORWAY SPRUCE; ROOT BIOMASS; CANOPY GAPS AB Light partitioning is often invoked as a mechanism for positive plant diversity effects on ecosystem functioning. Yet evidence for an improved distribution of foliage in space or time in diverse plant communities remains scarce, and restricted mostly to temperate grasslands. Here we identify the mechanisms through which tree species diversity affects community-level light capture in a biodiversity experiment with tropical trees that displays overyielding, i.e., enhanced biomass production in mixtures. Using a combination of empirical data, mechanistic models, and statistical tools, we develop innovative methods to test for the isolated and combined effects of architectural and temporal niche differences among species as well as plastic changes in crown shape within species. We show that all three mechanisms enhanced light capture in mixtures and that temporal niche differences were the most important driver of this result in our seasonal tropical system. Our study mechanistically demonstrates that niche differences and phenotypic plasticity can generate significant biodiversity effects on ecosystem functioning in tropical forests. C1 [Sapijanskas, Jurgis; Potvin, Catherine; Loreau, Michel] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Sapijanskas, Jurgis] AgroParisTech ENGREF, F-75015 Paris, France. [Paquette, Alain] Univ Quebec, Ctr Forest Res, Montreal, PQ H3C 3P8, Canada. [Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Panama. [Kunert, Norbert] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Loreau, Michel] CNRS, Ctr Biodivers Theory & Modelling, Expt Ecol Stn, F-09200 Moulis, France. RP Sapijanskas, J (reprint author), McGill Univ, Dept Biol, 1205 Ave Docteur Penfield, Montreal, PQ H3A 1B1, Canada. EM jurgis.sapijanskas@polytechnique.org OI Kunert, Norbert/0000-0002-5602-6221 FU French Ministry of Agriculture; TULIP Laboratory of Excellence [ANR-10-LABX-41]; Natural Science and Engineering Research Council of Canada; Smithsonian Tropical Research Institute FX We are grateful to Jose Monteza for invaluable help in maintaining the experimental plantation and data collection, Frederic Boivin and Pierre Racine for their help with the Crown Delineator package, Melanie Desrochers, Lady Mancilla, and Daniel Lesieur for mapping the plantation and incorporating information from the digital elevation model developed by Sebastian Wolf, Vincent Calcagno, Benoit Courbaud, Lorena Gomez-Aparicio, Paul Leadley, and Christian Messier for stimulating discussions, Maricarmen Ruiz-Jaen for sharing leaf data, Meaghan Murphy for help with SORTIE ND's source code. J. Sapijanskas was supported by the French Ministry of Agriculture, M. Loreau by the TULIP Laboratory of Excellence (ANR-10-LABX-41), the Sardinilla experiment by the Natural Science and Engineering Research Council of Canada and the Smithsonian Tropical Research Institute. NR 82 TC 13 Z9 15 U1 8 U2 76 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 SEP PY 2014 VL 95 IS 9 BP 2479 EP 2492 PG 14 WC Ecology SC Environmental Sciences & Ecology GA AP8PF UT WOS:000342340200011 ER PT J AU Johnson, DJ Bourg, NA Howe, R McShea, WJ Wolf, A Clay, K AF Johnson, Daniel J. Bourg, Norman A. Howe, Robert McShea, William J. Wolf, Amy Clay, Keith TI Conspecific negative density-dependent mortality and the structure of temperate forests SO ECOLOGY LA English DT Article DE density dependence; Janzen-Connell hypothesis; pair-correlation function; seedling dynamics; spatial distribution; tree diversity ID PLANT-SOIL FEEDBACKS; TROPICAL FORESTS; SPATIAL-PATTERNS; SEEDLING ESTABLISHMENT; NEIGHBORHOOD ANALYSIS; HABITAT ASSOCIATIONS; NEOTROPICAL FOREST; NORTHEASTERN CHINA; SPECIES-DIVERSITY; PRUNUS-SEROTINA AB Factors that control tree seedling dynamics are critical determinants of forest diversity. We examined the role of density-dependent mortality and abiotic factors in the differential establishment and survival of tree seedlings at three, large, mapped forest plots in Indiana, Virginia, and Wisconsin, USA. We tested whether seedling densities and seedling survival are related to local biotic and abiotic factors with generalized linear mixed models. Spatial point pattern analyses were utilized to determine if the distribution patterns of seedlings and saplings are consistent with a pattern generated by negative density-dependent mortality with respect to conspecific trees. Initial sampled seedling density for nearly a third of species showed a positive correlation with increasing conspecific basal area, indicating dispersal limitation, but few had any association with abiotic variables. By contrast, survival of seedlings over one year significantly declined with increasing conspecific basal area. Point pattern analyses indicated that nearly one-third of tree species had significantly over-dispersed point patterns of conspecific seedlings and saplings relative to adult densities; the majority of other species exhibited random spatial arrangements. Our results demonstrate that negative conspecific density-dependent mortality of seedlings could generate the spatial patterns observed at later life stages. By differentially favoring seedlings of other species, this process may contribute to the maintenance of tree diversity in temperate forests, just as others have demonstrated for tropical forests. C1 [Johnson, Daniel J.; Clay, Keith] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. [Bourg, Norman A.; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Howe, Robert; Wolf, Amy] Univ Wisconsin, Dept Biol & Nat & Appl Sci, Green Bay, WI 54311 USA. RP Johnson, DJ (reprint author), 318 W 12th Ave, Columbus, OH 43210 USA. EM johnson.6164@osu.edu OI Bourg, Norman/0000-0002-7443-1992 FU National Science Foundation Doctoral Dissertation Improvement Award [1110533]; FORESTGEO initiative; Smithsonian Institution-National Zoological Park; HSBC Climate Partnership; The 1923 Fund; Cofrin Center for Biodiversity; Smithsonian Institution's Center for Tropical Forest Science; Indiana Academy of Sciences FX We gratefully acknowledge funding for this project provided by the National Science Foundation Doctoral Dissertation Improvement Award No. 1110533 to K. Clay and D. J. Johnson. Funding for the establishment of the SCBI-FORESTGEO Large Forest Dynamics Plot was provided by the FORESTGEO initiative, the Smithsonian Institution-National Zoological Park, and the HSBC Climate Partnership. Field research at the Wabikon Forest Dynamics Plot was supported by grants from The 1923 Fund, the Cofrin Center for Biodiversity, and the Smithsonian Institution's Center for Tropical Forest Science. Funding for the Lilly Dickey Woods Forest Dynamics Plot was provided by the Indiana Academy of Sciences and the Smithsonian Institution's Center for Tropical Forest Science. Earlier versions of the manuscript benefited from comments by James Bever, Spencer Hall, Burnell Fischer, Heather Reynolds, Yan Zhu, and two anonymous reviewers. Field assistance to D. J. Johnson provided by J. Dyche, B. Fulka, R. Johnson, V. Milici, and B. Rush. Thanks goes to the many people who originally collected the tree census data at the three forests used in this study. Statistical advice was provided by the Indiana University Statistical Consulting Center and Chunfeng Huang. NR 56 TC 12 Z9 12 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 SEP PY 2014 VL 95 IS 9 BP 2493 EP 2503 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AP8PF UT WOS:000342340200012 ER PT J AU Fonseca, G Norenburg, J Di Domenico, M AF Fonseca, Gustavo Norenburg, Jon Di Domenico, Maikon TI Editorial: diversity of marine meiofauna on the coast of Brazil SO MARINE BIODIVERSITY LA English DT Editorial Material DE Brazil; Ecology; Marine; Meiofauna; New species; Taxonomy ID NORTHERN BEACHES; SAO-PAULO; STATE AB After a first bout of primarily taxonomical effort, meiofauna studies in Brazilian waters remained virtually neglected until the 1990s. At the end of the last century, taxonomical and ecological studies on meiofauna taxa were again published regularly, especially for Nematoda and Copepoda. In this issue, 18 new species are described and ten species are redescribed from seven Phyla. The five ecological articles cover the spatial distribution of forams and amoeba in a lagunar system, the meiofauna associated with biogenic structures, the relationship between nematodes and granulometry, and the response of sandy-beach meiofauna to a natural, short-term pulse of diatoms. All these contributions show the potential of the Brazilian coast for revealing new species and testing small to large-scale hypotheses about ecological processes. C1 [Fonseca, Gustavo] Univ Fed Sao Paulo, Dept Ciencias Mar, BR-11030400 Santos, SP, Brazil. [Norenburg, Jon] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Di Domenico, Maikon] Univ Campinas UNICAMP, Inst Biol, Zool Museum Prof Dr Adao Jose Cardoso, BR-13083863 Campinas, SP, Brazil. RP Fonseca, G (reprint author), Univ Fed Sao Paulo, Dept Ciencias Mar, Av Alm Saldanha da Gama 89, BR-11030400 Santos, SP, Brazil. EM gfonseca@unifesp.br; maik2dd@gmail.com RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 72 TC 2 Z9 2 U1 3 U2 7 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1867-1616 EI 1867-1624 J9 MAR BIODIVERS JI Mar. Biodivers. PD SEP PY 2014 VL 44 IS 3 BP 459 EP 462 DI 10.1007/s12526-014-0261-0 PG 4 WC Biodiversity Conservation; Marine & Freshwater Biology SC Biodiversity & Conservation; Marine & Freshwater Biology GA AQ0AO UT WOS:000342443800018 ER PT J AU Beck, AW Lawrence, DJ Peplowski, PN Prettyman, TH McCoy, TJ AF Beck, A. W. Lawrence, D. J. Peplowski, P. N. Prettyman, T. H. McCoy, T. J. TI FAST NEUTRONS IN HEDS: NEW INSIGHTS INTO DAWN DATA AND NEUTRON SPECTROSCOPY SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Beck, A. W.; Lawrence, D. J.; Peplowski, P. N.] Johns Hopkins Univ, Appl Phys Lab, Baltimore, MD 21218 USA. [Prettyman, T. H.] Planetary Sci Inst, Tucson, AZ USA. [McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 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 NR 5 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 SEP PY 2014 VL 49 SU 1 SI SI BP A28 EP A28 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200025 ER PT J AU Ivanova, MA Park, C Lorenz, CA Krot, AN Bullock, ES Nakashima, D Tenner, TJ Kita, NT MacPherson, GJ AF Ivanova, M. A. Park, C. Lorenz, C. A. Krot, A. N. Bullock, E. S. Nakashima, D. Tenner, T. J. Kita, N. T. MacPherson, G. J. TI PLASTICALLY DEFORMED FORSTERITE-BEARING TYPE B CAI FROM NWA 3118 (CV3). SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Ivanova, M. A.; Lorenz, C. A.] Vernadsky Inst, St Petersburg, Russia. [Ivanova, M. A.; Bullock, E. S.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA. [Park, C.; Krot, A. N.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Nakashima, D.; Tenner, T. J.; Kita, N. T.] Univ Wisconsin, Madison, WI 53706 USA. [Nakashima, D.] Toholu Univ, Sendai, Miyagi, Japan. NR 4 TC 0 Z9 0 U1 0 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 SEP PY 2014 VL 49 SU 1 SI SI BP A185 EP A185 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200182 ER PT J AU Jilly, CE Huss, GR Nagashima, K Schrader, DL AF Jilly, C. E. Huss, G. R. Nagashima, K. Schrader, D. L. TI OXYGEN ISOTOPES AND GEOTHERMOMETRY OF SECONDARY MINERALS IN CR CHONDRITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID FRACTIONATION C1 [Jilly, C. E.; Huss, G. R.; Nagashima, K.] Univ Hawaii Manoa, HIGP, Honolulu, HI 96822 USA. [Schrader, D. L.] Smithsonian Inst, Washington, DC 20560 USA. EM cjilly@hawaii.edu RI Schrader, Devin/H-6293-2012 OI Schrader, Devin/0000-0001-5282-232X NR 9 TC 0 Z9 0 U1 0 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 SEP PY 2014 VL 49 SU 1 SI SI BP A188 EP A188 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200185 ER PT J AU Lunning, NG Corrigan, CM McSween, HY Tenner, TJ Kita, N AF Lunning, N. G. Corrigan, C. M. McSween, H. Y., Jr. Tenner, T. J. Kita, N. TI CM CHONDRITE IMPACT MELT CLAST IDENTIFIED IN A REGOLITHIC HOWARDITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Lunning, N. G.; McSween, H. Y., Jr.] Univ Tennessee, Knoxville, TN 37996 USA. [Corrigan, C. M.] NMNH, Smithsonian Inst, Washington, DC USA. [Tenner, T. J.; Kita, N.] Univ Wisconsin, WiscSIMS, Madison, WI 53706 USA. EM nlunning@utk.edu 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 SEP PY 2014 VL 49 SU 1 SI SI BP A245 EP A245 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200242 ER PT J AU Park, C Ivanova, MA Nagashima, K Krot, AN MacPherson, GJ AF Park, C. Ivanova, M. A. Nagashima, K. Krot, A. N. MacPherson, G. J. TI Al-Mg SYSTEMATICS OF ULTRAREFRACTORY CAIs FROM CV3 CHONDRITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc ID DIFFUSION C1 [Park, C.; Nagashima, K.; Krot, A. N.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. [Ivanova, M. A.] Vernadsky Inst, Moscow, Russia. [Ivanova, M. A.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA. EM ckpark@higp.hawaii.edu NR 5 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 SEP PY 2014 VL 49 SU 1 SI SI BP A314 EP A314 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200311 ER PT J AU Steele, A McCubbin, FM Benning, LG Siljestrom, S Cody, GD Goreva, Y Hauri, EH Wang, J Kilcoyne, ALD Grady, M Verchovsky, A Sabbah, H Smith, C Freissinet, C Glavin, DP Burton, AS Fries, MD Blanco, JDR Glamoclija, M Rogers, KL Mikhail, S Zare, RN Wu, Q Ismail, A Dworkin, JP Bhartia, R AF Steele, A. McCubbin, F. M. Benning, L. G. Siljestroem, S. Cody, G. D. Goreva, Y. Hauri, E. H. Wang, J. Kilcoyne, A. L. D. Grady, M. Verchovsky, A. Sabbah, H. Smith, C. Freissinet, C. Glavin, D. P. Burton, A. S. Fries, M. D. Blanco, Rodriguez J. D. Glamoclija, M. Rogers, K. L. Mikhail, S. Zare, R. N. Wu, Q. Ismail, A. Dworkin, J. P. Bhartia, R. TI Hydrothermal Organic Synthesis on Mars: Evidence from the Tissint Meteorite SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Steele, A.; Siljestroem, S.; Cody, G. D.; Glamoclija, M.; Rogers, K. L.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [McCubbin, F. M.] Univ New Mexico, Dept Earth & Planetary Sci, Inst Meteorit, Albuquerque, NM 87131 USA. [Benning, L. G.; Blanco, Rodriguez J. D.] Univ Leeds, Sch Earth & Environm, Leeds LS2 9JT, W Yorkshire, England. [Siljestroem, S.] SP Tech Res Inst Sweden, Dept Chem Mat & Surfaces, Boras, Sweden. [Siljestroem, S.; Goreva, Y.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Hauri, E. H.; Wang, J.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Kilcoyne, A. L. D.] Adv Light Source, Berkeley, CA USA. [Grady, M.; Verchovsky, A.] Stanford Univ, Ctr Earth Planetary Space & Astron Res, Stanford, CA 94305 USA. [Sabbah, H.; Zare, R. N.; Wu, Q.; Ismail, A.] Stanford Univ, Dept Chem, Stanford, CA 94305 USA. [Sabbah, H.] Univ Toulouse, Toulouse, France. [Sabbah, H.] CNRS, Toulouse, France. [Smith, C.] Nat Hist Museum, Dept Mineral, London, England. [Freissinet, C.; Glavin, D. P.; Dworkin, J. P.] NASA, Goddard Space Flight Ctr, Houston, TX USA. [Burton, A. S.; Fries, M. D.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Blanco, Rodriguez J. D.] Univ Copenhagen, Dept Chem, Nanosci Ctr, DK-1168 Copenhagen, Denmark. [Glamoclija, M.] Rutgers State Univ, Dept Earth & Planetary Sci, Piscataway, NJ 08855 USA. [Rogers, K. L.] Rensselaer Polytech Inst, Troy, NY 12181 USA. [Mikhail, S.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9YL, Midlothian, Scotland. [Ismail, A.] King Abdulaziz Univ, Dept Chem, Rabigh, Saudi Arabia. [Bhartia, R.] CALTECH, Jet Prop Lab, Pasadena, CA USA. RI Ismail, Ali/I-7595-2012; Glavin, Daniel/D-6194-2012; Kilcoyne, David/I-1465-2013; Dworkin, Jason/C-9417-2012 OI Ismail, Ali/0000-0001-9556-5140; Glavin, Daniel/0000-0001-7779-7765; Dworkin, Jason/0000-0002-3961-8997 NR 0 TC 1 Z9 1 U1 1 U2 16 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 SEP PY 2014 VL 49 SU 1 SI SI BP A376 EP A376 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200373 ER PT J AU Zanetti, M Wittmann, A Nemchin, A Carpenter, P Vicenzi, EP Jolliff, B AF Zanetti, M. Wittmann, A. Nemchin, A. Carpenter, P. Vicenzi, E. P. Jolliff, B. TI DECOMPOSITION OF ZIRCON IN MISTASTIN LAKE IMPACT MELT GLASS: AN INTEGRATED SIMS, HYPERSPECTRAL-CL, RAMAN AND EPMA STUDY SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 77th Annual Meeting of the Meteoritical-Society CY SEP 08-13, 2014 CL Casablanca, MOROCCO SP Meteorit Soc C1 [Zanetti, M.; Wittmann, A.; Carpenter, P.; Jolliff, B.] Washington Univ, St Louis, MO USA. [Zanetti, M.; Wittmann, A.; Carpenter, P.; Jolliff, B.] McDonnell Ctr Space Sci, St Louis, MO USA. [Nemchin, A.] Curtin Univ, Perth, WA 6845, Australia. [Vicenzi, E. P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. EM Michael.Zanetti@wustl.edu NR 4 TC 1 Z9 1 U1 0 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 SEP PY 2014 VL 49 SU 1 SI SI BP A449 EP A449 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AP2PA UT WOS:000341914200446 ER PT J AU Beaumont, CN Goodman, AA Kendrew, S Williams, JP Simpson, R AF Beaumont, Christopher N. Goodman, Alyssa A. Kendrew, Sarah Williams, Jonathan P. Simpson, Robert TI THE MILKY WAY PROJECT: LEVERAGING CITIZEN SCIENCE AND MACHINE LEARNING TO DETECT INTERSTELLAR BUBBLES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE H II regions; ISM: bubbles; methods: data analysis; stars: formation ID MASSIVE-STAR-FORMATION; H-II REGIONS; FAR-INFRARED LOOPS; GALACTIC PLANE; AUTOMATIC DETECTION; MOLECULAR CLOUDS; SHELLS; GALAXY; EVOLUTION; COLLECT AB We present Brut, an algorithm to identify bubbles in infrared images of the Galactic midplane. Brut is based on the Random Forest algorithm, and uses bubbles identified by >35,000 citizen scientists from the Milky Way Project to discover the identifying characteristics of bubbles in images from the Spitzer Space Telescope. We demonstrate that Brut's ability to identify bubbles is comparable to expert astronomers. We use Brut to re-assess the bubbles in the Milky Way Project catalog, and find that 10%-30% of the objects in this catalog are non-bubble interlopers. Relative to these interlopers, high-reliability bubbles are more confined to the mid-plane, and display a stronger excess of young stellar objects along and within bubble rims. Furthermore, Brut is able to discover bubbles missed by previous searches-particularly bubbles near bright sources which have low contrast relative to their surroundings. Brut demonstrates the synergies that exist between citizen scientists, professional scientists, and machine learning techniques. In cases where "untrained" citizens can identify patterns that machines cannot detect without training, machine learning algorithms like Brut can use the output of citizen science projects as input training sets, offering tremendous opportunities to speed the pace of scientific discovery. A hybrid model of machine learning combined with crowdsourced training data from citizen scientists can not only classify large quantities of data, but also address the weakness of each approach if deployed alone. C1 [Beaumont, Christopher N.; Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Beaumont, Christopher N.; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kendrew, Sarah; Simpson, Robert] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. RP Beaumont, CN (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM beaumont@ifa.hawaii.edu RI Goodman, Alyssa/A-6007-2010; OI Goodman, Alyssa/0000-0003-1312-0477; Williams, Jonathan/0000-0001-5058-695X; Kendrew, Sarah/0000-0002-7612-0469 FU National Science Foundation [0908159]; Microsoft Research; [NSF-AST1108907] FX This research made use of the Scikit-Learn (Pedregosa et al. 2011), Astropy (Astropy Collaboration et al. 2013), and WiseRF software packages. WsieRF is a product of wise.io, Inc., and we thank them for making an academic license freely available. J.P.W. acknowledges support from NSF-AST1108907. This material is based upon work supported by the National Science Foundation under grant No. 0908159. C.B. and A.G. acknowledge Microsoft Research for Funding. NR 59 TC 5 Z9 5 U1 0 U2 13 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 SEP PY 2014 VL 214 IS 1 AR 3 DI 10.1088/0067-0049/214/1/3 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TP UT WOS:000341777800003 ER PT J AU Britt, CT Hynes, RI Johnson, CB Baldwin, A Jonker, PG Nelemans, G Torres, MAP Maccarone, T Steeghs, D Greiss, S Heinke, C Bassa, CG Collazzi, A Villar, A Gabb, M Gossen, L AF Britt, C. T. Hynes, R. I. Johnson, C. B. Baldwin, A. Jonker, P. G. Nelemans, G. Torres, M. A. P. Maccarone, T. Steeghs, D. Greiss, S. Heinke, C. Bassa, C. G. Collazzi, A. Villar, A. Gabb, M. Gossen, L. TI VARIABILITY OF OPTICAL COUNTERPARTS IN THE CHANDRA GALACTIC BULGE SURVEY SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE accretion, accretion disks; Galaxy: bulge; stars: black holes; stars: dwarf novae; stars: flare; stars: neutron; stars: variables: general; surveys; X-rays: binaries ID X-RAY BINARIES; GRAVITATIONAL LENSING EXPERIMENT.; NEAR-INFRARED COUNTERPARTS; HOLE EVENT HORIZONS; SHORTEST ORBITAL PERIOD; OGLE-III CATALOG; LOW-MASS; GLOBULAR-CLUSTERS; CATACLYSMIC VARIABLES; DYNAMICAL FORMATION AB We present optical light curves of variable stars consistent with the positions of X-ray sources identified with the Chandra X-ray Observatory for the Chandra Galactic Bulge Survey (GBS). Using data from the Mosaic-II instrument on the Blanco 4 m Telescope at CTIO, we gathered time-resolved photometric data on timescales from similar to 2 hr to 8 days over the 3/4 of the X-ray survey containing sources from the initial GBS catalog. Among the light curve morphologies we identify are flickering in interacting binaries, eclipsing sources, dwarf nova outbursts, ellipsoidal variations, long period variables, spotted stars, and flare stars. Eighty-seven percent of X-ray sources have at least one potential optical counterpart. Twenty-seven percent of these candidate counterparts are detectably variable; a much greater fraction than expected for randomly selected field stars, which suggests that most of these variables are real counterparts. We discuss individual sources of interest, provide variability information on candidate counterparts, and discuss the characteristics of the variable population. C1 [Britt, C. T.; Hynes, R. I.; Johnson, C. B.; Baldwin, A.; Collazzi, A.; Gossen, L.] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. [Britt, C. T.; Maccarone, T.] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Nelemans, G.; Torres, M. A. P.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Steeghs, D.; Greiss, S.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Heinke, C.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. [Bassa, C. G.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Villar, A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Gabb, M.] Florida Atlantic Univ, Dept Phys, Boca Raton, FL 33431 USA. RP Britt, CT (reprint author), Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA. RI Nelemans, Gijs/D-3177-2012; OI Nelemans, Gijs/0000-0002-0752-2974; Heinke, Craig/0000-0003-3944-6109 FU National Science Foundation [AST-0908789]; Louisiana Board of Regents Fellowship; NAS/Louisiana Board of Regents grant [NNX07AT62A/LEQSF]; Netherlands Organisation for Scientific Research FX This work was supported by the National Science Foundation under grant No. AST-0908789, by the Louisiana Board of Regents Fellowship, by the NAS/Louisiana Board of Regents grant NNX07AT62A/LEQSF(2007-2010) Phase 3-02. P.G.J. and M.A.P.T. acknowledge support from the Netherlands Organisation for Scientific Research. This research has made use of NASA's Astrophysics Data System Bibliographic Services and of SAOImage DS9, developed by Smithsonian Astrophysical Observatory. T.J.M. thanks Reba Bandyopadhyay for useful discussions, especially illustrating the possibility of SyXBs. NR 83 TC 5 Z9 5 U1 0 U2 2 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 SEP PY 2014 VL 214 IS 1 AR 10 DI 10.1088/0067-0049/214/1/10 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TP UT WOS:000341777800010 ER PT J AU Hasoglu, MF Abdel-Naby, SA Gatuzz, E Garcia, J Kallman, TR Mendoza, C Gorczyca, TW AF Hasoglu, M. F. Abdel-Naby, Sh. A. Gatuzz, E. Garcia, J. Kallman, T. R. Mendoza, C. Gorczyca, T. W. TI K-SHELL PHOTOABSORPTION OF MAGNESIUM IONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE atomic data; atomic processes; ISM: abundances; line: formation ID X-RAY SPECTROSCOPY; PHOTOIONIZATION CROSS-SECTIONS; XMM-NEWTON OBSERVATION; INTERSTELLAR-MEDIUM; FLUORESCENCE YIELDS; ATOMIC OXYGEN; ABSORPTION; CHANDRA; AUGER; ABUNDANCES AB X-ray photoabsorption cross sections have been computed for all magnesium ions with three or more electrons using the R-matrix method. A comparison with other available data for Mg II-Mg x shows good qualitative agreement in the resultant resonance shapes. However, for the lower ionization stages, and for singly ionized Mg II in particular, the previous R-matrix results overestimate the K-edge position due to the neglect of important orbital relaxation effects, and a global shift downward in photon energy of those cross sections is therefore warranted. We have found that the cross sections for Mg I and Mg II are further complicated by the M-shell (n = 3) occupancy. As a result, the treatment of spectator Auger decay of 1s -> np resonances using a method based on multichannel quantum defect theory and an optical potential becomes problematic, making it necessary to implement an alternative, approximate treatment of Auger decay for neutral Mg I. The new cross sections are used to fit the Mg K edge in XMM-Newton spectra of the low-mass X-ray binary GS 1826-238, where most of the interstellar Mg is found to be in ionized form. C1 [Hasoglu, M. F.] Hasan Kalyoncu Univ, Dept Comp Engn, TR-27100 Sahinbey, Gaziantep, Turkey. [Abdel-Naby, Sh. A.] Auburn Univ, Dept Phys, Auburn, AL 36849 USA. [Gatuzz, E.; Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020, Venezuela. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mendoza, C.; Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. RP Hasoglu, MF (reprint author), Hasan Kalyoncu Univ, Dept Comp Engn, TR-27100 Sahinbey, Gaziantep, Turkey. OI Mendoza, Claudio/0000-0002-2854-4806 FU NASA APRA grant [NNX11AF32G] FX This work was supported in part by the NASA APRA grant NNX11AF32G. NR 55 TC 3 Z9 3 U1 1 U2 7 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 SEP PY 2014 VL 214 IS 1 AR 8 DI 10.1088/0067-0049/214/1/8 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TP UT WOS:000341777800008 ER PT J AU Ueda, J Iono, D Yun, MS Crocker, AF Narayanan, D Komugi, S Espada, D Hatsukade, B Kaneko, H Matsuda, Y Tamura, Y Wilner, DJ Kawabe, R Pan, HA AF Ueda, Junko Iono, Daisuke Yun, Min S. Crocker, Alison F. Narayanan, Desika Komugi, Shinya Espada, Daniel Hatsukade, Bunyo Kaneko, Hiroyuki Matsuda, Yuichi Tamura, Yoichi Wilner, David J. Kawabe, Ryohei Pan, Hsi-An TI COLD MOLECULAR GAS IN MERGER REMNANTS. I. FORMATION OF MOLECULAR GAS DISKS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: interactions; galaxies: ISM; galaxies: kinematics and dynamics; radio lines: galaxies ID LUMINOUS INFRARED GALAXIES; INTEGRAL FIELD SPECTROSCOPY; ACTIVE GALACTIC NUCLEI; POLAR-RING GALAXIES; MU-M SPECTROSCOPY; SPACE-TELESCOPE OBSERVATIONS; YOUNG GLOBULAR-CLUSTERS; STAR-FORMING KNOTS; H-ALPHA EMISSION; ELLIPTIC GALAXIES AB We present the less than or similar to 1 kpc resolution (CO)-C-12 imaging study of 37 optically selected local merger remnants using new and archival interferometric maps obtained with ALMA, CARMA, the Submillimeter Array, and the Plateau de Bure Interferometer. We supplement a sub-sample with single-dish measurements obtained at the Nobeyama Radio Observatory 45 m telescope for estimating the molecular gas mass (10(7-11) M-circle dot) and evaluating the missing flux of the interferometric measurements. Among the sources with robust CO detections, we find that 80% (24/30) of the sample show kinematical signatures of rotating molecular gas disks (including nuclear rings) in their velocity fields, and the sizes of these disks vary significantly from 1.1 kpc to 9.3 kpc. The size of the molecular gas disks in 54% of the sources is more compact than the K-band effective radius. These small gas disks may have formed from a past gas inflow that was triggered by a dynamical instability during a potential merging event. On the other hand, the rest (46%) of the sources have gas disks that are extended relative to the stellar component, possibly forming a late-type galaxy with a central stellar bulge. Our new compilation of observational data suggests that nuclear and extended molecular gas disks are common in the final stages of mergers. This finding is consistent with recent major-merger simulations of gas-rich progenitor disks. Finally, we suggest that some of the rotation-supported turbulent disks observed at high redshifts may result from galaxies that have experienced a recent major merger. C1 [Ueda, Junko; Iono, Daisuke; Komugi, Shinya; Espada, Daniel; Hatsukade, Bunyo; Matsuda, Yuichi; Kawabe, Ryohei] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Ueda, Junko] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1330033, Japan. [Ueda, Junko; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Iono, Daisuke; Espada, Daniel; Matsuda, Yuichi; Pan, Hsi-An] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. [Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Crocker, Alison F.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. [Narayanan, Desika] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Espada, Daniel] Joint ALMA Observ, Santiago 7630355, Chile. [Kaneko, Hiroyuki] Univ Tsukuba, Grad Sch Pure & Appl Sci, Tsukuba, Ibaraki 3058577, Japan. [Tamura, Yoichi] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Pan, Hsi-An] Natl Astron Observ Japan, Nobeyama Radio Observ, Minamimaki, Nagano 3841305, Japan. [Pan, Hsi-An] Hokkaido Univ, Fac Sci, Dept Phys, Kita Ku, Sapporo, Hokkaido 0600810, Japan. RP Ueda, J (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM junko.ueda@nao.ac.jp OI Kaneko, Hiroyuki/0000-0002-2699-4862 FU Smithsonian Institution; Academia Sinica; National Science Foundation; CARMA partner universities; National Aeronautics and Space Administration; Japan Society for the Promotion of Science for Young Scientists; Sasakawa Scientific Research Grant from The Japan Science Society; JSPS [2580016]; US NSF [AST-144560]; Gordon and Betty Moore Foundation; Kenneth T. and Eileen L. Norris Foundation; Betty Moore Foundation; James S. McDonnell Foundation; Associates of the California Institute of Technology; University of Chicago; states of California, Illinois, and Maryland 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.; 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.; 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.; Finally, J.U. is financially supported by a Research Fellowship from the Japan Society for the Promotion of Science for Young Scientists and the Sasakawa Scientific Research Grant from The Japan Science Society. D.I. is supported by JSPS KAKENHI grant Number 2580016. D.N. acknowledges support from the US NSF via grant AST-144560. NR 209 TC 23 Z9 23 U1 0 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 SEP PY 2014 VL 214 IS 1 AR 1 DI 10.1088/0067-0049/214/1/1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TP UT WOS:000341777800001 ER PT J AU Davis, FW Chornesky, EA AF Davis, Frank W. Chornesky, Elizabeth A. TI Adapting to climate change in California SO BULLETIN OF THE ATOMIC SCIENTISTS LA English DT Article DE climate adaptation; climate change; ecosystem services; endangered species; sea level; water supply ID FUTURE; IMPACT AB Many aspects of the Californian approach to controlling the greenhouse gases that cause climate change now have a sufficient track record to provide potential models or lessons for national and even international action. In comparison, the state's efforts on climate change adaptation, although multifaceted, are less well developed and thus far have focused largely on information sharing, impact assessments, and planning. Still, adaptation could advance more quickly in California than in many other regions, given relatively high public awareness and concern, extensive scientific information, a strong tradition of local and regional planning, and some enabling policies and institutions. Much more political support and sufficient financing will have to be mustered at state and local levels to enable new projects and initiatives to cope with sea level rise, water management, and ecosystem adaptation, not to mention public health and other key areas of concern. Even so, California's initial efforts to adapt to unavoidable changes in climate may offer insights for other governments that will, inevitably, need to fashion their own adaptation strategies. C1 [Davis, Frank W.] Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. [Davis, Frank W.] NCEAS, Santa Barbara, CA USA. [Davis, Frank W.] Amer Assoc Advancement Sci, Washington, DC USA. [Davis, Frank W.] Nat Conservancy Calif, Bakersfield, CA USA. [Chornesky, Elizabeth A.] Smithsonian Inst, Washington, DC 20560 USA. [Chornesky, Elizabeth A.] Lehigh Univ, Bethlehem, PA USA. RP Davis, FW (reprint author), Univ Calif Santa Barbara, Bren Sch Environm Sci & Management, Santa Barbara, CA 93106 USA. RI Davis, Frank/B-7010-2009 OI Davis, Frank/0000-0002-4643-5718 NR 27 TC 0 Z9 0 U1 6 U2 21 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0096-3402 EI 1938-3282 J9 B ATOM SCI JI Bull. Atom. Scient. PD SEP-OCT PY 2014 VL 70 IS 5 BP 62 EP 73 DI 10.1177/0096340214546839 PG 12 WC International Relations; Social Issues SC International Relations; Social Issues GA AP1NQ UT WOS:000341837800011 ER PT J AU Herrera-Cubilla, A Jackson, JBC AF Herrera-Cubilla, Amalia Jackson, Jeremy B. C. TI PHYLOGENY OF GENUS CUPULADRIA (BRYOZOA, CHEILOSTOMATA) IN THE NEOGENE OF TROPICAL AMERICA SO JOURNAL OF PALEONTOLOGY LA English DT Article ID OPPOSITE SIDES; PANAMA; ISTHMUS; TAXONOMY; EVOLUTION; TEMPO AB We used 57 morphometric characters to discriminate 17 extant and fossil Cupuladria species and analyzed their phylogenetic relationships in relation to extant Discoporella species. Data were gathered from 496 extant and fossil Cupuladria specimens ranging in age from early Miocene to Recent and distributed from the Caribbean to tropical eastern Pacific. A first series of discriminant analyses distinguished three morphological groups: Cupuladria with vicarious avicularia, Cupuladria without vicarious avicularia, and Discoporella. Further discriminant analyses identified 17 species of Cupuladria. Cladistic analyses of these three groups yielded four equally parsimonious trees. All of the consensus trees exhibited the same topology, dividing the 25 tropical American cupuladriids into four distinct monophyletic clades, including Discoporella, and are consistent with previous molecular phylogenies except that there are no molecular data for the C-V2 clade. Diversification of species was higher in the C-V1 and C-V2 clades than C-NV clade, and involved mostly Caribbean species. Cupuladria with vicarious clade 1 (C-V1) includes: C. monotrema, C. pacificiensis, C. exfragminis, C. cheethami, C. biporosa, and four new species: C. pervagata, C. floridensis, C. colonensis and C. dominicana. Cupuladria with vicarious clade 2 (C-V2) includes: C. multesima, C. incognita, and three new species C. collyrida, C. veracruxiensis and C. planissima. Cupuladria clade without vicarious (C-NV) includes: C. surinamensis, C. panamensis, and one new species C. gigas. The stratigraphic occurrence of species is consistent with cladogram topology within clades. However hypothesized cladistic relations among clades are the reverse of their stratigraphic occurrence with younger clade C-NV appearing as the hypothetical ancestor of the two older clades C-V1 and C-V2. More extensive collections of early to middle Miocene specimens of Cupuladria and Discoporella will be required to resolve this apparent paradox. C1 [Herrera-Cubilla, Amalia; Jackson, Jeremy B. C.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, Panama City, Panama. [Jackson, Jeremy B. C.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, La Jolla, CA 92093 USA. [Jackson, Jeremy B. C.] Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Herrera-Cubilla, A (reprint author), Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archeol, MRC 0580-01 Box 0843-03092, Panama City, Panama. EM herreraa@si.edu; jeremybcjackson@gmail.com FU STRI SE; SENACYT [78 2010] FX A. Cheetham made helpful comments on the manuscript. Our thanks to colleagues and institutions who provided collection material that have enriched this manuscript: H. Lessios, R. Collin, R. Robertson, A. O'Dea and F. Rodriguez (Smithsonian Tropical Research Institute); J. Sanner (National Museum of Natural History); K. Sindemark (Swedish Museum of Natural History); M. C. Boyett (Harvard University); L. Smith (Louisiana State University); C. W. Poag (Scientist Emeritus U. S. Geological Survey); M. S. Jones, P. Taylor (Natural History Museum); P. G. Weaver (NC Museum of Natural Sciences); P. Florez (Instituto de Investigaciones Marinas y Costeras); R. W. Portell (Florida Museum of Natural History). Also to J. Ceballos and R. Chong for their valuable help with the SEM and the preparation of crispy plates and figures. Financial support has been provided by STRI S&E 2008 Fund to J. B. C. Jackson, STRI S&E 2009 to A. Herrera-Cubilla, and SENACYT Project 78 2010 to A. Herrera-Cubilla. NR 57 TC 1 Z9 1 U1 1 U2 7 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 SEP PY 2014 VL 88 IS 5 BP 851 EP 894 DI 10.1666/13-031 PG 44 WC Paleontology SC Paleontology GA AP2MZ UT WOS:000341907900002 ER PT J AU Heller, R Williams, D Kipping, D Limbach, MA Turner, E Greenberg, R Sasaki, T Bolmont, E Grasset, O Lewis, K Barnes, R Zuluaga, JI AF Heller, Rene Williams, Darren Kipping, David Limbach, Mary Anne Turner, Edwin Greenberg, Richard Sasaki, Takanori Bolmont, Emeline Grasset, Olivier Lewis, Karen Barnes, Rory Zuluaga, Jorge I. TI Formation, Habitability, and Detection of Extrasolar Moons SO ASTROBIOLOGY LA English DT Review DE Astrobiology; Extrasolar planets; Habitability; Planetary science; Tides ID TRANSIT TIMING VARIATIONS; TIME-SERIES PHOTOMETRY; SOLAR-LIKE STARS; GIANT PLANETS; GALILEAN SATELLITES; LIGHT CURVES; SOUTH-POLE; REGULAR SATELLITES; TIDAL DISSIPATION; SUBSURFACE OCEAN AB The diversity and quantity of moons in the Solar System suggest a manifold population of natural satellites exist around extrasolar planets. Of peculiar interest from an astrobiological perspective, the number of sizable moons in the stellar habitable zones may outnumber planets in these circumstellar regions. With technological and theoretical methods now allowing for the detection of sub-Earth-sized extrasolar planets, the first detection of an extrasolar moon appears feasible. In this review, we summarize formation channels of massive exomoons that are potentially detectable with current or near-future instruments. We discuss the orbital effects that govern exomoon evolution, we present a framework to characterize an exomoon's stellar plus planetary illumination as well as its tidal heating, and we address the techniques that have been proposed to search for exomoons. Most notably, we show that natural satellites in the range of 0.1-0.5 Earth mass (i) are potentially habitable, (ii) can form within the circumplanetary debris and gas disk or via capture from a binary, and (iii) are detectable with current technology. C1 [Heller, Rene] McMaster Univ, Dept Phys & Astron, Origins Inst, Hamilton, ON L8S 4M1, Canada. [Williams, Darren] Penn State Erie, Behrend Coll, Sch Sci, Erie, PA USA. [Kipping, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Limbach, Mary Anne; Turner, Edwin] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Limbach, Mary Anne] Princeton Univ, Dept Mech & Aerosp Engn, Princeton, NJ 08544 USA. [Turner, Edwin] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba, Japan. [Greenberg, Richard] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Sasaki, Takanori] Kyoto Univ, Dept Astron, Kyoto, Japan. [Bolmont, Emeline] Univ Bordeaux, LAB, UMR 5804, Floirac, France. [Bolmont, Emeline] CNRS, LAB, UMR 5804, Floirac, France. [Grasset, Olivier] Univ Nantes, CNRS, Nantes, France. [Lewis, Karen] Tokyo Inst Technol, Tokyo 152, Japan. [Barnes, Rory] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barnes, Rory] NASA, Astrobiol Inst, Virtual Planetary Lab, Lead Team, Washington, DC USA. [Zuluaga, Jorge I.] Univ Antioquia, FACom, FCEN, Inst Fis, Medellin, Colombia. RP Heller, R (reprint author), McMaster Univ, Dept Phys & Astron, Origins Inst, Hamilton, ON L8S 4M1, Canada. EM rheller@physics.mcmaster.ca OI Zuluaga, Jorge I./0000-0002-6140-3116 FU Origins Institute at McMaster University; Canadian Astrobiology Training Program, a Collaborative Research and Training Experience Program - Natural Sciences and Engineering Research Council of Canada (NSERC); Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; Global COE Program, "From the Earth to 'Earths,''' MEXT, Japan; JSPS KAKENHI [24740120]; NSF [AST-1108882]; NASA Astrobiology Institute [NNH05ZDA001C]; CODI/UdeA; World Premier International Research Center Initiative, MEXT, Japan FX The helpful comments of two referees are very much appreciated. We thank Alexis Carlotti, Jill Knapp, Matt Mountain, George Rieke, Dave Spiegel, and Scott Tremaine for useful conversations and Ted Stryk for granting permission to use a reprocessed image of Europa. Rene Heller is supported by the Origins Institute at McMaster University and by the Canadian Astrobiology Training Program, a Collaborative Research and Training Experience Program funded by the Natural Sciences and Engineering Research Council of Canada (NSERC). Darren Williams is a member of the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Takanori Sasaki was supported by a grant for the Global COE Program, "From the Earth to 'Earths,''' MEXT, Japan, and Grant-in-Aid for Young Scientists (B), JSPS KAKENHI Grant Number 24740120. Rory Barnes acknowledges support from NSF grant AST-1108882 and the NASA Astrobiology Institute's Virtual Planetary Laboratory lead team under cooperative agreement no. NNH05ZDA001C. Jorge I. Zuluaga is supported by CODI/UdeA. This research has been supported in part by World Premier International Research Center Initiative, MEXT, Japan. This work has made use of NASA's Astrophysics Data System Bibliographic Services. NR 261 TC 20 Z9 20 U1 4 U2 24 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD SEP PY 2014 VL 14 IS 9 BP 798 EP 835 DI 10.1089/ast.2014.1147 PG 38 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA AP1GM UT WOS:000341815900005 PM 25147963 ER PT J AU Longworth, JB Mesquita, RC Bentos, TV Moreira, MP Massoca, PE Williamson, GB AF Longworth, J. Benjamin Mesquita, Rita C. Bentos, Tony V. Moreira, Marcelo P. Massoca, Paulo E. Williamson, G. Bruce TI Shifts in Dominance and Species Assemblages over Two Decades in Alternative Successions in Central Amazonia SO BIOTROPICA LA English DT Article DE basal area; Cecropia; forest regeneration; secondary succession; species density; stem density; Vismia ID SECONDARY SUCCESSION; ABANDONED PASTURES; EASTERN AMAZONIA; USE-HISTORY; OLD-GROWTH; FOREST; SOIL; COMMUNITY; FIRE; RESTORATION AB Following perturbation, different assemblages that originate under the same abiotic conditions initiate successional pathways that may continue to diverge or converge toward an eventual climax. Forest regeneration in the Central Amazon begins with alternative successional pathways associated with prior land use. In a 12-yr study of secondary forests, initially ranging between 2 and 19yrs after abandonment, we compared species compositions through time along two pathways, abandoned clear-cuts dominated by Cecropia and abandoned pastures dominated by Vismia; prior results at these sites have not directly evaluated species composition. At all ages, the Chao-Jaccard similarity index of species composition was highest comparing pasture transects to each other, lowest comparing pastures transects to clear-cut transects, and intermediate comparing clear-cut transects to each other. Through time, clear-cut transects became less similar to each other, as did pasture transects. Changes in similarity reflected declining dominance along both pathways, but Cecropia dominance of clear-cut transects declined more rapidly than Vismia dominance of pasture transects. A rich association of species replaced Cecropia in clear-cut transects, resulting in decreased similarity among them. In pasture transects one genus, Bellucia, replaced the lost Vismia, so similarity of Vismia transects was maintained despite some turnover in dominance. Overall, even with turnover of individuals and decline of the dominant pioneers, the alternative pathways exhibited strikingly different species assemblies after two decades of succession, suggesting that the effect of land use persists well beyond initial floristic composition. C1 [Longworth, J. Benjamin; Williamson, G. Bruce] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Mesquita, Rita C.; Bentos, Tony V.; Massoca, Paulo E.] Inst Nacl de Pesquisas da Amazonia, Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project, BR-69060001 Manaus, AM, Brazil. [Moreira, Marcelo P.] Fundacao Vitoria Amazonica, BR-69060093 Manaus, AM, Brazil. RP Williamson, GB (reprint author), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. EM btwill@lsu.edu RI Massoca, Paulo/A-4325-2015 OI Massoca, Paulo/0000-0001-6396-8244 FU NASA LBA; CNPq; US National Science Foundation [DEB-0639114, DEB-1147434]; Biological Dynamics of Forest Fragments Project (BDFFP); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); BDFFP-INPA-SI [645] FX We thank Joao de Deus Fragata for field assistance and Paulo Apostolo for plant identification. This project was supported by NASA LBA, CNPq, the US National Science Foundation (DEB-0639114 and DEB-1147434) and the Biological Dynamics of Forest Fragments Project (BDFFP). TVB was supported by fellowships from the Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) and the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES). This is publication # 645 in the Technical Series of the Biological Dynamics of Forest Fragments Project BDFFP-INPA-SI. NR 38 TC 8 Z9 8 U1 2 U2 33 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 SEP PY 2014 VL 46 IS 5 BP 529 EP 537 DI 10.1111/btp.12143 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AO8YF UT WOS:000341641100004 ER PT J AU Casares, J Jonker, PG AF Casares, J. Jonker, P. G. TI Mass Measurements of Stellar and Intermediate-Mass Black Holes SO SPACE SCIENCE REVIEWS LA English DT Review DE Black holes; X-ray binaries; Accretion disks ID X-RAY NOVA; TRANSIENT SWIFT J1357.2-0933; DISC INSTABILITY MODEL; BINARY GRO J0422+32; CYGNUS X-1; DYNAMICAL EVIDENCE; XTE J1118+480; GLOBULAR-CLUSTER; COMPACT OBJECT; OPHIUCHI 1977 AB We discuss the method, and potential systematic effects therein, used for measuring the mass of stellar-mass black holes in X-ray binaries. We restrict our discussion to the method that relies on the validity of Kepler's laws; we refer to this method as the dynamical method. We briefly discuss the implications of the mass distribution of stellar-mass black holes and provide an outlook for future measurements. Further, we investigate the evidence for the existence of intermediate-mass black holes i.e. black holes with masses above 100 M-aS (TM), the limit to the black hole mass that can be produced by stellar evolution in the current Universe. C1 [Casares, J.] Inst Astrofis Canarias, San Cristobal la Laguna 38205, Sc De Tenerife, Spain. [Casares, J.] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Sc De Tenerife, Spain. [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. RP Casares, J (reprint author), Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38206, Sc De Tenerife, Spain. EM jorge.casares@iac.es FU Spanish Ministerio de Economia y Competitividad (MINECO) [AYA2010-18080] FX We thanks Cristina Zurita, Andrew Cantrell and Rob Hynes for providing us with Figs. 5, 6 and 11, respectively. J.C. acknowledges support by the Spanish Ministerio de Economia y Competitividad (MINECO) under grant AYA2010-18080. NR 222 TC 37 Z9 37 U1 1 U2 8 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD SEP PY 2014 VL 183 IS 1-4 BP 223 EP 252 DI 10.1007/s11214-013-0030-6 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP1XZ UT WOS:000341866900012 ER PT J AU McClintock, JE Narayan, R Steiner, JF AF McClintock, Jeffrey E. Narayan, Ramesh Steiner, James F. TI Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets SO SPACE SCIENCE REVIEWS LA English DT Review DE Black hole physics; Accretion disks; X-Ray binaries; Stars: winds, outflows ID X-RAY BINARIES; MICROQUASAR XTE J1550-564; THIN ACCRETION DISKS; QUASI-PERIODIC OSCILLATIONS; MAGNETIC-FIELD GEOMETRY; CYGNUS X-1; LMC X-1; RELATIVISTIC JETS; GRO J1655-40; OBSERVATIONAL EVIDENCE AB The spins of ten stellar black holes have been measured using the continuum-fitting method. These black holes are located in two distinct classes of X-ray binary systems, one that is persistently X-ray bright and another that is transient. Both the persistent and transient black holes remain for long periods in a state where their spectra are dominated by a thermal accretion disk component. The spin of a black hole of known mass and distance can be measured by fitting this thermal continuum spectrum to the thin-disk model of Novikov and Thorne; the key fit parameter is the radius of the inner edge of the black hole's accretion disk. Strong observational and theoretical evidence links the inner-disk radius to the radius of the innermost stable circular orbit, which is trivially related to the dimensionless spin parameter a (au) of the black hole (|a (au)|< 1). The ten spins that have so far been measured by this continuum-fitting method range widely from a (au)a parts per thousand 0 to a (au)> 0.95. The robustness of the method is demonstrated by the dozens or hundreds of independent and consistent measurements of spin that have been obtained for several black holes, and through careful consideration of many sources of systematic error. Among the results discussed is a dichotomy between the transient and persistent black holes; the latter have higher spins and larger masses. Also discussed is recently discovered evidence in the transient sources for a correlation between the power of ballistic jets and black hole spin. C1 [McClintock, Jeffrey E.; Narayan, Ramesh; Steiner, James F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McClintock, JE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jem@cfa.harvard.edu; narayan@cfa.harvard.edu; jsteiner@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX11AD08G]; NASA grant [NNX11AE16G]; NASA Hubble Fellowship grant [HST-HF-51315.01] FX The authors thank S. W. Davis for important input on Sect. 5.3. We also thank C. Brocksopp, E. Kuulkers, M. L. McCollough, C. Sanchez-Fernandez and C. Zurita for help in preparing Fig. 2; J. Garcia and T. Fragos for their comments on a version of the manuscript; R. Fender for discussions on MeerKAT; and an anonymous referee for several important criticisms. JEM was supported in part by NASA grant NNX11AD08G and RN by NASA grant NNX11AE16G. JFS was supported by NASA Hubble Fellowship grant HST-HF-51315.01. NR 162 TC 69 Z9 69 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD SEP PY 2014 VL 183 IS 1-4 BP 295 EP 322 DI 10.1007/s11214-013-0003-9 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP1XZ UT WOS:000341866900015 ER PT J AU Shik, JZ Kay, AD Silverman, J AF Shik, Jonathan Z. Kay, Adam D. Silverman, Jules TI Aphid honeydew provides a nutritionally balanced resource for incipient Argentine ant mutualists SO ANIMAL BEHAVIOUR LA English DT Article DE Argentine ant; invasive species; life history; Linepithema humile; mutualism; nutritional ecology ID LINEPITHEMA-HUMILE; HYMENOPTERA-FORMICIDAE; SOLENOPSIS-INVICTA; ECOLOGICAL STOICHIOMETRY; LABORATORY COLONIES; FOOD DISTRIBUTION; STORAGE PROTEINS; TROPHIC ECOLOGY; PROPAGULE SIZE; MANDUCA-SEXTA AB Food-for-protection mutualisms can provide resources that subsidize ecological dominance, although their stability often depends on the nutritional match between the traded food and traits to which it is allocated. A well-studied food-for-protection mutualism is the protection by Argentine ants, Linepithema humile, of hemipteran mutualists in return for honeydew, which is generally assumed to be a nutritionally imbalanced food, high in carbohydrates and low in protein. We tested an alternative hypothesis, that the nutritional value of honeydew depends on the composition of life history traits related to survival (worker maintenance) and colony growth (brood production). Using a factorial design, we manipulated ant colony access to aphids, baseline levels of nutritional deprivation, and, by adding or subtracting queens, the ability to invest in growth. We found that aphid access primarily benefited colonies on high-protein, low-carbohydrate diets, suggesting colony nutritional state influences the value of aphid associations. Unexpectedly, we found that worker survival and brood production were positively correlated across treatments, and both decreased with the ants' percentage of nitrogen mass, a proxy for body protein. Moreover, the workers' percentage of fat mass was generally lower in brood-producing colonies, particularly in high-protein treatments, suggesting strong competition among investments for limited carbohydrates. These results suggest that carbohydrate access generally constrains Argentine ant life history and clarifies the links between the nutritional composition of food rewards and the stability of ecologically important mutualisms. (C) 2014 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. C1 [Shik, Jonathan Z.; Silverman, Jules] N Carolina State Univ, Dept Entomol, Raleigh, NC 27695 USA. [Kay, Adam D.] Smithsonian Trop Res Inst, Ancon, Panama. [Shik, Jonathan Z.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, Copenhagen, Denmark. [Kay, Adam D.] Univ St Thomas, Dept Biol, St Paul, MN USA. RP Shik, JZ (reprint author), Univ Copenhagen, Ctr Social Evolut, Dept Biol, Univ Pk 15, DK-2100 Copenhagen, Denmark. EM jonathan.shik@gmail.com FU North Carolina State University FX We thank David Bednar for help with lipid extractions, Shanna Wood for assistance maintaining experiments and Consuello Arellano for statistical support. This research was funded by the Blanton J. Whitmire endowment at North Carolina State University. NR 51 TC 3 Z9 3 U1 7 U2 52 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD SEP PY 2014 VL 95 BP 33 EP 39 DI 10.1016/j.anbehav.2014.06.008 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA AO5BN UT WOS:000341355900005 ER PT J AU Ramos, AG Nunziata, SO Lance, SL Rodriguez, C Faircloth, BC Gowaty, PA Drummond, H AF Ramos, Alejandra G. Nunziata, Schyler O. Lance, Stacey L. Rodriguez, Cristina Faircloth, Brant C. Gowaty, Patricia Adair Drummond, Hugh TI Habitat structure and colony structure constrain extrapair paternity in a colonial bird SO ANIMAL BEHAVIOUR LA English DT Article DE blue-footed booby; colonial seabird; extrapair paternity; extrapair sire; habitat structure; microsatellite; nest density; spatial location; Sula nebouxii ID BLUE-FOOTED BOOBY; PAIR PATERNITY; ACADIAN FLYCATCHERS; SULA-NEBOUXII; MATE; FEMALE; QUALITY; HETEROZYGOSITY; POPULATIONS; HYPOTHESIS AB Individual variation in sexual fidelity and extrapair paternity (EPP) is widely attributed to environmental heterogeneity, but the only variables known to be influential are food abundance and density of conspecific breeders (potential extrapair partners). Habitat structure is thought to impact EPP but is rarely measured and, when considered, is usually confounded with food abundance and predation pressure. To sidestep these confounds, we tested whether EPP is associated with habitat structure variables and with local conspecific density in a species whose nesting habitat is not used for feeding and lacks predators. In a blue-footed booby, Sula nebouxii, colony, the probability of EPP in a female's nest was highest in parts of the study plot where there were few obstacles to locomotion, and was quadratically related to local density of sexually active males, even though local males did not sire the EP chicks. The probability of a male breeder siring EP (extrapair) chicks elsewhere was quadratically related to local density of sexually active males around his nest. From these patterns we infer that both sexes may foray for EP interactions, that males and females nesting at intermediate density are most likely to be accessed by forayers, and that obstacles in the vicinity of a female's nest constrain access of foraying males. To our knowledge, this is the first demonstration that individual variation in EPP is associated with habitat structure in the absence of confounding variation in food availability, predation pressure or breeder quality, and the first evidence that EPP opportunities of female and male breeders are reduced by high density of conspecific breeders above a particular threshold. (C) 2014 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Ramos, Alejandra G.; Rodriguez, Cristina; Drummond, Hugh] Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol & Evolut, Mexico City 04510, DF, Mexico. [Nunziata, Schyler O.; Lance, Stacey L.] Univ Georgia, Savannah River Ecol Lab, Aiken, SC USA. [Nunziata, Schyler O.] Univ Kentucky, Dept Biol, Lexington, KY USA. [Faircloth, Brant C.; Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. [Gowaty, Patricia Adair] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Washington, DC USA. RP Ramos, AG (reprint author), Univ Nacl Autonoma Mexico, Inst Ecol, Dept Ecol & Evolut, AP 70-275, Mexico City 04510, DF, Mexico. EM ramos.alejndra@gmail.com RI Lance, Stacey/K-9203-2013; OI Lance, Stacey/0000-0003-2686-1733; Faircloth, Brant/0000-0002-1943-0217 FU UNAM (PAPIIT) [IN206610]; CONACyT [104313]; Consejo Nacional de Ciencia y Tecnologia; Universidad Nacional Autonoma de Mexico; U.S. Department of Energy [DE-FC09-07SR22506] FX We are grateful to Simon C. Griffith, Lynna M. Kiere, Marcela Osorio-Beristain, Diana Perez-Staples, Oscar Sanchez-Macouzet and two anonymous referees for helpful comments on the manuscript, and to numerous volunteers and colleagues for help in the field and lab, especially Santiago Bautista-Lopez, Jonathan P. Drury, Gabriela Lopez-Carapia, Janeth Rosas-Morales and David Schneider. We are grateful to Pablo Frank-Bolton, who kindly wrote the script used to estimate neighbourhood nest density. The Armada de Mexico, local fishermen and staff of the Parque Nacional Isla Isabel supplied vital and much appreciated logistical support. This study was financed by UNAM (PAPIIT, IN206610) and CONACyT (104313). This manuscript constitutes a partial fulfilment of the Graduate Program in Biomedical Sciences of the Universidad Nacional Autonoma de Mexico. A.G.R. wishes to thank and acknowledge the scholarship and financial support provided by the Consejo Nacional de Ciencia y Tecnologia and the Universidad Nacional Autonoma de Mexico. This research was partially supported by U.S. Department of Energy under Award Number DE-FC09-07SR22506 to the University of Georgia Research Foundation. NR 51 TC 6 Z9 6 U1 1 U2 31 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD SEP PY 2014 VL 95 BP 121 EP 127 DI 10.1016/j.anbehav.2014.07.003 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA AO5BN UT WOS:000341355900014 ER PT J AU Farine, DR Aplin, LM Garroway, CJ Mann, RP Sheldon, BC AF Farine, Damien R. Aplin, Lucy M. Garroway, Colin J. Mann, Richard P. Sheldon, Ben C. TI Collective decision making and social interaction rules in mixed-species flocks of songbirds SO ANIMAL BEHAVIOUR LA English DT Article DE collective behaviour; Cyanistes caeruleus; decision making; interspecific interaction; mixed-species flocking; Paridae; Parus major; social information use ID FISH SHOALS; NETWORK ANALYSIS; ANIMAL BEHAVIOR; INFORMATION USE; SELFISH HERD; ORGANIZATION; EVOLUTION; ECOLOGY; PREY AB Associations in mixed-species foraging groups are common in animals, yet have rarely been explored in the context of collective behaviour. Despite many investigations into the social and ecological conditions under which individuals should form groups, we still know little about the specific behavioural rules that individuals adopt in these contexts, or whether these can be generalized to heterospecifics. Here, we studied collective behaviour in flocks in a community of five species of woodland passerine birds. We adopted an automated data collection protocol, involving visits by RFID-tagged birds to feeding stations equipped with antennae, over two winters, recording 91576 feeding events by 1904 individuals. We demonstrated highly synchronized feeding behaviour within patches, with birds moving towards areas of the patch with the largest proportion of the flock. Using a model of collective decision making, we then explored the underlying decision rule birds may be using when foraging in mixed-species flocks. The model tested whether birds used a different decision rule for conspecifics and heterospecifics, and whether the rules used by individuals of different species varied. We found that species differed in their response to the distribution of conspecifics and heterospecifics across foraging patches. However, simulating decisions using the different rules, which reproduced our data well, suggested that the outcome of using different decision rules by each species resulted in qualitatively similar overall patterns of movement. It is possible that the decision rules each species uses may be adjusted to variation in mean species abundance in order for individuals to maintain the same overall flock-level response. This is likely to be important for maintaining coordinated behaviour across species, and to result in quick and adaptive flock responses to food resources that are patchily distributed in space and time. (C) 2014 The Authors. Published on behalf of The Association for the Study of Animal Behaviour by Elsevier Ltd. C1 [Farine, Damien R.; Aplin, Lucy M.; Garroway, Colin J.; Sheldon, Ben C.] 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, Ancon, Panama. [Aplin, Lucy M.] Australian Natl Univ, Res Sch Biol, Div Ecol Evolut & Genet, Acton, ACT, Australia. [Mann, Richard P.] Uppsala Univ, Dept Math, Uppsala, Sweden. 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 RI Sheldon, Ben/A-8056-2010; Mann, Richard/N-9779-2014 OI Sheldon, Ben/0000-0002-5240-7828; Mann, Richard/0000-0003-0701-1274 FU ERC [AdG 250164]; BBSRC [BB/L006081/1]; NSF [NSF-IOS 1250895]; Australian Postgraduate Award; ERC starting grant FX We thank Iain Couzin, Gonzalo de Polavieja, Andy King and Noam Miller for extensive discussion on the manuscript, in particular in defining the model and its parameters. We are grateful to the many fieldworkers who helped with individual marking of tits, particularly to the EGI social network group. In particular, we thank Julian Howe for assistance in the field. The work was funded by grants from the ERC (AdG 250164) and BBSRC (BB/L006081/1) to B.C.S., D.R.F. was cofunded by an NSF grant (NSF-IOS 1250895) awarded to Margaret C. Crofoot, L.M.A. was funded by an Australian Postgraduate Award, and R.P.M. was funded by an ERC starting grant (IDCAB) to David J.T. Sumpter. NR 53 TC 14 Z9 15 U1 6 U2 95 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD SEP PY 2014 VL 95 BP 173 EP 182 DI 10.1016/j.anbehav.2014.07.008 PG 10 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA AO5BN UT WOS:000341355900020 PM 25214653 ER PT J AU Hales, AS De Gregorio-Monsalvo, I Montesinos, B Casassus, S Dent, WFR Dougados, C Eiroa, C Hughes, AM Garay, G Mardones, D Menard, F Palau, A Perez, S Phillips, N Torrelles, JM Wilner, D AF Hales, A. S. De Gregorio-Monsalvo, I. Montesinos, B. Casassus, S. Dent, W. F. R. Dougados, C. Eiroa, C. Hughes, A. M. Garay, G. Mardones, D. Menard, F. Palau, Aina Perez, S. Phillips, N. Torrelles, J. M. Wilner, D. TI A CO SURVEY IN PLANET-FORMING DISKS: CHARACTERIZING THE GAS CONTENT IN THE EPOCH OF PLANET FORMATION SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems; protoplanetary disks ID HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; CIRCUMSTELLAR DUST DISKS; MOLECULAR CLOUD COMPLEX; INTERMEDIATE-MASS STARS; VEGA-EXCESS STARS; SUN-LIKE STARS; T-TAURI STARS; MYR OLD STAR; PROTOPLANETARY DISKS AB We carried out a (CO)-C-12(3-2) survey of 52 southern stars with a wide range of IR excesses (L-IR/L-*) using the single-dish telescopes APEX and ASTE. The main aims were (1) to characterize the evolution of molecular gas in circumstellar disks using L-IR/L-* values as a proxy of disk dust evolution, and (2) to identify new gas-rich disk systems suitable for detailed study with ALMA. About 60% of the sample (31 systems) have L-IR/L-* > 0.01, typical of T Tauri or Herbig AeBe stars, and the rest (21 systems) have L-IR/L-* <0.01, typical of debris disks. We detect CO(3-2) emission from 20 systems, and 18 (90%) of these have L-IR/L-* > 0.01. However, the spectra of only four of the newly detected systems appear free of contamination from background or foreground emission from molecular clouds. These include the early-type stars HD 104237 (A4/5V, 116 pc) and HD 98922 (A2 III, 507 pc, as determined in this work), where our observations reveal the presence of CO-rich circumstellar disks for the first time. Of the other detected sources, many could harbor gaseous circumstellar disks, but our data are inconclusive. For these two newly discovered gas-rich disks, we present radiative transfer models that simultaneously reproduce their spectral energy distributions and the (CO)-C-12(3-2) line profiles. For both of these systems, the data are fit well by geometrically fiat disks, placing them in the small class of non-flaring disks with significant molecular gas reservoirs. C1 [Hales, A. S.; De Gregorio-Monsalvo, I.; Dent, W. F. R.; Phillips, N.] Joint ALMA Observ, Santiago 7630355, Chile. [Hales, A. S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [De Gregorio-Monsalvo, I.; Dent, W. F. R.; Phillips, N.] European So Observ, D-85748 Garching, Germany. [Montesinos, B.] CSIC INTA, Ctr Astrobiol CAB, Dept Astrophys, E-28691 Madrid, Spain. [Casassus, S.; Dougados, C.; Garay, G.; Mardones, D.; Menard, F.; Perez, S.] Univ Chile, Dept Astron, Santiago, Chile. [Dougados, C.; Menard, F.] CNRS INSU, France UMI 3386, UMI FCA, Paris, France. [Eiroa, C.] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. [Hughes, A. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Palau, Aina] Inst Ciencies Espai CSIC IEEC, E-08193 Bellaterra, Catalunya, Spain. [Torrelles, J. M.] Inst Ciencies Espai CSIC IEEC, E-08028 Barcelona, Spain. [Torrelles, J. M.] Inst Ciencies Cosmos UB IEEC, E-08028 Barcelona, Spain. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hales, AS (reprint author), Joint ALMA Observ, Alonso de Cordova 3107, Santiago 7630355, Chile. EM ahales@alma.cl RI Mardones, Diego/I-5719-2016; Casassus, Simon/I-8609-2016; Garay, Guido/H-8840-2013; Montesinos, Benjamin/C-3493-2017; OI Garay, Guido/0000-0003-1649-7958; Montesinos, Benjamin/0000-0002-7982-2095; Torrelles, Jose Maria/0000-0002-6896-6085 FU Millennium Science Initiative, Chilean Ministry of Economy [Nucleus P10-022-F]; MICINN (Spain) [AYA2011-30228-C03]; FEDER; AGAUR (Catalonia) [2009SGR1172] FX We are grateful to Mario van den Ancker and Andre Muller for providing the UVES/VLT spectrum of HD 98922 and for fruitful discussions on the determination of the parameters for this star. This work is based on observations carried out with the Atacama Pathfinder Experiment telescope (APEX). APEX is a collaboration between the Max-Planck Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. The ASTE project is driven by the Nobeyama Radio Observatory (NRO), a branch of the National Astronomical Observatory of Japan (NAOJ), in collaboration with the University of Chile, and Japanese institutes including the University of Tokyo, Nagoya University, Osaka Prefecture University, Ibaraki University, and Hokkaido University. A.H., S.C., F.M., S.P., and W.F.R.D. acknowledge support from the Millennium Science Initiative, Chilean Ministry of Economy: Nucleus P10-022-F. A.P. and J.M.T. acknowledge support from MICINN (Spain) AYA2011-30228-C03 grants (co-funded with FEDER funds) and AGAUR (Catalonia) 2009SGR1172 grant. The ICC (UB) is a CSIC-Associated Unit through the ICE (CSIC). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. Finally, we would like to thank our anonymous referee for a very careful and detailed review that we think has very significantly improved our paper. NR 145 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD SEP PY 2014 VL 148 IS 3 AR 47 DI 10.1088/0004-6256/148/3/47 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO3JQ UT WOS:000341225900009 ER PT J AU Lin, HW Abad, GG Loeb, A AF Lin, Henry W. Abad, Gonzalo Gonzalez Loeb, Abraham TI DETECTING INDUSTRIAL POLLUTION IN THE ATMOSPHERES OF EARTH-LIKE EXOPLANETS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrobiology; planets and satellites: atmospheres; white dwarfs ID WHITE-DWARFS; EXTRATERRESTRIAL INTELLIGENCE; BROWN DWARFS; PLANETS; STAR; BIOSIGNATURE; EVOLUTION; SYSTEMS; SEARCH; DISKS AB Detecting biosignatures, such as molecular oxygen in combination with a reducing gas, in the atmospheres of transiting exoplanets has been a major focus in the search for alien life. We point out that in addition to these generic indicators, anthropogenic pollution could be used as a novel biosignature for intelligent life. To this end, we identify pollutants in the Earth's atmosphere that have significant absorption features in the spectral range covered by the James Webb Space Telescope. We focus on tetrafluoromethane (CF4) and trichlorofluoromethane (CCl3F), which are the easiest to detect chlorofluorocarbons (CFCs) produced by anthropogenic activity. We estimate that similar to 1.2 days (similar to 1.7 days) of total integration time will be sufficient to detect or constrain the concentration of CCl3F (CF4) to similar to 10 times the current terrestrial level. C1 [Lin, Henry W.] Harvard Univ, Cambridge, MA 02138 USA. [Abad, Gonzalo Gonzalez; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, HW (reprint author), Harvard Univ, Cambridge, MA 02138 USA. EM henrylin@college.harvard.edu; ggonzalezabad@cfa.harvard.edu; aloeb@cfa.harvard.edu OI Gonzalez Abad, Gonzalo/0000-0002-8090-6480; Lin, Henry/0000-0003-2767-6142 FU NSF [AST-1312034]; Harvard Origins of Life Initiative FX This work was supported in part by NSF grant AST-1312034, and the Harvard Origins of Life Initiative. NR 34 TC 8 Z9 9 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2014 VL 792 IS 1 AR L7 DI 10.1088/2041-8205/792/1/L7 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KO UT WOS:000341306900007 ER PT J AU Pereira, TMD De Pontieu, B Carlsson, M Hansteen, V Tarbell, TD Lemen, J Title, A Boerner, P Hurlburt, N Wulser, JP Martinez-Sykora, J Kleint, L Golub, L McKillop, S Reeves, KK Saar, S Testa, P Tian, H Jaeggli, S Kankelborg, C AF Pereira, T. M. D. De Pontieu, B. Carlsson, M. Hansteen, V. Tarbell, T. D. Lemen, J. Title, A. Boerner, P. Hurlburt, N. Wuelser, J. P. Martinez-Sykora, J. Kleint, L. Golub, L. McKillop, S. Reeves, K. K. Saar, S. Testa, P. Tian, H. Jaeggli, S. Kankelborg, C. TI AN INTERFACE REGION IMAGING SPECTROGRAPH FIRST VIEW ON SOLAR SPICULES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: atmosphere; Sun: chromosphere; Sun: transition region ID OPTICAL TELESCOPE; II SPICULES; K LINES; MG II; IRIS; DYNAMICS; HINODE; CHROMOSPHERE; MISSION; EVENTS AB Solar spicules have eluded modelers and observers for decades. Since the discovery of the more energetic type II, spicules have become a heated topic but their contribution to the energy balance of the low solar atmosphere remains unknown. Here we give a first glimpse of what quiet-Sun spicules look like when observed with NASA's recently launched Interface Region Imaging Spectrograph (IRIS). Using IRIS spectra and filtergrams that sample the chromosphere and transition region, we compare the properties and evolution of spicules as observed in a coordinated campaign with Hinode and the Atmospheric Imaging Assembly. Our IRIS observations allow us to follow the thermal evolution of type II spicules and finally confirm that the fading of Ca II H spicules appears to be caused by rapid heating to higher temperatures. The IRIS spicules do not fade but continue evolving, reaching higher and falling back down after 500-800 s. Ca II H type II spicules are thus the initial stages of violent and hotter events that mostly remain invisible in Ca II H filtergrams. These events have very different properties from type I spicules, which show lower velocities and no fading from chromospheric passbands. The IRIS spectra of spicules show the same signature as their proposed disk counterparts, reinforcing earlier work. Spectroheliograms from spectral rasters also confirm that quiet-Sun spicules originate in bushes from the magnetic network. Our results suggest that type II spicules are indeed the site of vigorous heating (to at least transition region temperatures) along extensive parts of the upward moving spicular plasma. C1 [Pereira, T. M. D.; De Pontieu, B.; Carlsson, M.; Hansteen, V.] Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. [De Pontieu, B.; Tarbell, T. D.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Wuelser, J. P.; Martinez-Sykora, J.; Kleint, L.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, J.; Kleint, L.] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Kleint, L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Golub, L.; McKillop, S.; Reeves, K. K.; Saar, S.; Testa, P.; Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jaeggli, S.; Kankelborg, C.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Pereira, TMD (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. EM tiago.pereira@astro.uio.no RI Reeves, Katharine/P-9163-2014 FU NSC (Norway); European Research Council [291058]; NASA [NNM07AA01C, NNG09FA40C] FX IRIS is a NASA Small Explorer mission developed and operated by LMSAL with mission operations executed at NASA ARC and major contributions to downlink communications funded by the NSC (Norway). Hinode is a Japanese mission developed by ISAS/JAXA, with the NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated in cooperation with ESA and NSC (Norway). This work was supported by the European Research Council grant No. 291058 and by NASA under contracts NNM07AA01C (Hinode), and NNG09FA40C (IRIS). NR 30 TC 27 Z9 27 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 SEP 1 PY 2014 VL 792 IS 1 AR L15 DI 10.1088/2041-8205/792/1/L15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KO UT WOS:000341306900015 ER PT J AU Post, S Park, S Badenes, C Burrows, DN Hughes, JP Lee, JJ Mori, K Slane, PO AF Post, Seth Park, Sangwook Badenes, Carles Burrows, David N. Hughes, John P. Lee, Jae-Joon Mori, Koji Slane, Patrick O. TI ASYMMETRY IN THE OBSERVED METAL-RICH EJECTA OF THE GALACTIC TYPE IA SUPERNOVA REMNANT G299.2-2.9 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (G299.2-2.9 supernova remnant); ISM: supernova remnants; X-rays: ISM ID CHANDRA-X-RAY; CCD IMAGING SPECTROMETER; CIRCUMSTELLAR MATERIAL; PROGENITOR; MODELS; NUCLEOSYNTHESIS; EMISSION; EXPLOSION; EVOLUTION; SYSTEMS AB We have performed a deep Chandra observation of the Galactic Type Ia supernova remnant G299.2-2.9. Here we report the initial results from our imaging and spectral analysis. The observed abundance ratios of the central ejecta are in good agreement with those predicted by delayed-detonation Type Ia supernovae models. We reveal inhomogeneous spatial and spectral structures of metal-rich ejecta in G299.2-2.9. The Fe/Si abundance ratio in the northern part of the central ejecta region is higher than that in the southern part. A significant continuous elongation of ejecta material extends out to the western outermost boundary of the remnant. In this western elongation, both the Si and Fe are enriched with a similar abundance ratio to that in the southern part of the central ejecta region. These structured distributions of metal-rich ejecta material suggest that this Type Ia supernova might have undergone a significantly asymmetric explosion and/or has been expanding into a structured medium. C1 [Post, Seth; Park, Sangwook] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Badenes, Carles] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Badenes, Carles] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. [Burrows, David N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Lee, Jae-Joon] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Mori, Koji] Miyazaki Univ, Dept Appl Phys, Miyazaki 8892192, Japan. [Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Post, S (reprint author), Univ Texas Arlington, Dept Phys, Box 19059, Arlington, TX 76019 USA. EM seth.post@mavs.uta.edu; badenes@pitt.edu; burrows@astro.psu.edu; jph@physics.rutgers.edu; mori@astro.miyazaki-u.ac.jp; slane@cfa.harvard.edu FU NASA under Chandra grant [GO0-11076X]; NASA [NAS8-03060] FX This work has been supported in part by NASA under Chandra grant GO0-11076X and NASA contract NAS8-03060. NR 41 TC 1 Z9 1 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2014 VL 792 IS 1 AR L20 DI 10.1088/2041-8205/792/1/L20 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KO UT WOS:000341306900020 ER PT J AU Saarela, M Bull, RD Peterson, PM Soreng, RJ Paszko, B AF Saarela, M. Bull, R. D. Peterson, P. M. Soreng, R. J. Paszko, B. TI Phylogenetic relationships among the genera and tribes of the "Aveneae-type plastid DNA" grasses (Poaceae: Pooideae: Poeae) SO BOTANY-BOTANIQUE LA English DT Meeting Abstract C1 [Saarela, M.; Bull, R. D.] Canadian Museum Nat, Ottawa, ON K1P 6P4, Canada. [Peterson, P. M.; Soreng, R. J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. [Paszko, B.] Polish Acad Sci, W Szafer Inst Bot, PL-00901 Warsaw, Poland. NR 0 TC 1 Z9 1 U1 1 U2 5 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 1916-2790 EI 1916-2804 J9 BOTANY JI Botany PD SEP PY 2014 VL 92 IS 9 BP 672 EP 672 PG 1 WC Plant Sciences SC Plant Sciences GA AO7FW UT WOS:000341518800104 ER PT J AU Herrera, F Manchester, SR Velez-Juarbe, J Jaramillo, C AF Herrera, Fabiany Manchester, Steven R. Velez-Juarbe, Jorge Jaramillo, Carlos TI PHYTOGEOGRAPHIC HISTORY OF THE HUMIRIACEAE (PART 2) SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE endocarps; fossils; Malpighiales; Neotropics; paleobiogeography; Panama; Peru; Puerto Rico; wood ID PUERTO-RICO; RAIN-FORESTS; PANAMA; PALEOBOTANY; OLIGOCENE; PHYLOGENY; AMERICA; FRUITS AB Premise of research. Humiriaceae occupy predominantly Neotropical lowland rainforests, with only a single Old World species in western Africa. Molecular divergence time estimates suggest that the family might have originated during the middle Cretaceous; however, fossil occurrences are lacking prior to the Paleocene. Here we provide new fossil evidence that expands our understanding of the paleobiogeographic history and evolution of this family. Methodology. Fossil endocarps and wood were compared with extant relatives of the family. Transverse and longitudinal sections of fossil and modern fruits were studied anatomically and morphologically. Pivotal results. Fruits of the new species, Duckesia berryi sp. n., from the Oligocene of Pacific coastal Peru (ca. 30-28.5 Ma), provide the earliest fossil evidence of Duckesia-the genus is now confined to Amazonia. We also document the earliest fossil fruit record for Sacoglottis tertiaria, from the early Oligocene (ca. 33.9-28.4 Ma) of Puerto Rico, and a new occurrence of Vantanea cipaconensis fruits, from the late Miocene of Panama (ca. 9-8.5 Ma). The new fossil wood, Humiriaceoxylon ocuensis gen. et. sp. n., from the late Eocene (ca. 37.2-33.9 Ma) of Ocu, Panama, confirms that this family was represented by large trees anatomically consistent with the extant genera. Conclusions. Humiriaceae originated in the Neotropics, with the oldest-known occurrences being fruits of Lacunofructus cuatrecasana and wood of H. ocuensis from the late Eocene of Panama. The family was generically diverse and widely distributed geographically across northern South America and Central America by the early Miocene. The new fossils also provide further evidence of regional extinctions within the Neotropics; extirpation of particular genera from Central America, the Caribbean, and coastal Peru indicate that Neogene orogenic and climatic events had an important effect on the modern-day distribution of the family. C1 [Herrera, Fabiany; Manchester, Steven R.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Herrera, Fabiany; Manchester, Steven R.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Herrera, Fabiany; Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Anco n, Panama. [Velez-Juarbe, Jorge] Nat Hist Museum Los Angeles Cty, Dept Mammal, Los Angeles, CA 90007 USA. RP Herrera, F (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM fherrera@flmnh.ufl.edu FU NSF [0966884, DEB-0733725, EAR-0957679]; OISE; EAR; DRL; Evolving Earth Foundation; Geological Society of America Foundation; Asociacion Colombiana de Geologos y Geofisicos del Petroleo-ARES; Smithsonian Institution; Gary S. Morgan Student Research Award; Lewis and Clark Foundation-American Philosophical Society; Panama Canal Authority (ACP); M. Tupper, and R. Perez SA; [NSF-DEB-1210404] FX This research was made possible through funding from NSF-DEB-1210404 (Dissertation Research Improvement grant), PCP PIRE (Partnerships for International Research and Education, NSF grant 0966884, OISE, EAR, DRL), the Evolving Earth Foundation, the Geological Society of America Foundation, Asociacion Colombiana de Geologos y Geofisicos del Petroleo-ARES, the Smithsonian Institution, the Gary S. Morgan Student Research Award, and the Lewis and Clark Foundation-American Philosophical Society to F. Herrera. Funding NSF DEB-0733725, EAR-0957679, Panama Canal Authority (ACP), M. Tupper, and R. Perez SA to C. Jaramillo. We thank E. Wheeler and N. Boonchai for their helpful suggestions concerning wood anatomy; S. Wing and J. Wingerath for access to the USNM collection; J.-N. Martinez and F. Navarro for assistance in field reconnaissance and collecting in Peru; and O. Rodriguez, A. Hendy, R. Portell, A. Wood, L. Londono, and M.-I. Barreto for their assistance in the Panama field trips. W. Judd, M. Brenner, J. Bloch, T. Lott, and an anonymous reviewer provided helpful criticisms to the manuscript. Special thanks to C. F. De Gracia for collecting the Gatun fossils. NR 39 TC 1 Z9 2 U1 0 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 EI 1537-5315 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD SEP PY 2014 VL 175 IS 7 BP 828 EP 840 DI 10.1086/676818 PG 13 WC Plant Sciences SC Plant Sciences GA AO7EK UT WOS:000341514700009 ER PT J AU Larabee, FJ Suarez, AV AF Larabee, Fredrick J. Suarez, Andrew V. TI The evolution and functional morphology of trap-jaw ants (Hymenoptera: Formicidae) SO MYRMECOLOGICAL NEWS LA English DT Review DE Review; trap-jaw ants; functional morphology; biomechanics; Odontomachus; Anochetus; Myrmoteras; Dacetini ID GENUS ANOCHETUS HYMENOPTERA; FAST MANDIBLE STRIKE; DACETINE ANTS; KEY INNOVATIONS; PREY CAPTURE; ODONTOMACHUS LATREILLE; JUMPING PERFORMANCE; FROGHOPPER INSECTS; PREDATORY BEHAVIOR; PHILIPPINE ISLANDS AB We review the biology of trap-jaw ants whose highly specialized mandibles generate extreme speeds and forces for predation and defense. Trap-jaw ants are characterized by elongated, power-amplified mandibles and use a combination of latches and springs to generate some of the fastest animal movements ever recorded. Remarkably, trap jaws have evolved at least four times in three subfamilies of ants. In this review, we discuss what is currently known about the evolution, morphology, kinematics, and behavior of trap-jaw ants, with special attention to the similarities and key differences among the independent lineages. We also highlight gaps in our knowledge and provide suggestions for future research on this notable group of ants. C1 [Larabee, Fredrick J.; Suarez, Andrew V.] Univ Illinois, Dept Entomol, Urbana, IL 61801 USA. [Larabee, Fredrick J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Suarez, Andrew V.] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. RP Larabee, FJ (reprint author), Univ Illinois, Dept Entomol, 320 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA. EM larabee@life.illinois.edu; avsuarez@life.illinois.edu FU University of Illinois School of Integrative Biology; Sigma Xi; Peter and Carmen Lucia Buck Foundation; National Science Foundation [DEB 1020979] FX We would like to thank the following people for their help and insight: J. Lattke for bringing Protalaridris armata to our attention as a possible trap-jaw ant; P.S. Ward for discussion on the relationships among the myrmicine genera, especially the Dacetini and for sharing his unpublished tree; M.K. Larabee for helpful comments on this manuscript; two anonymous reviewers for helpful comments; and the Suarez Lab for general support. This work was supported by the University of Illinois School of Integrative Biology (Francis M. and Harlie M. Clark Research Support Grant), Sigma Xi (Grants-in-Aid of Research), and the Peter and Carmen Lucia Buck Foundation (Peter Buck Predoctoral Fellowship) to FIL and by the National Science Foundation Grant (DEB 1020979) to AVS. NR 124 TC 7 Z9 7 U1 6 U2 28 PU OESTERREICHISCHE GESELL ENTOMOFAUNISTIK, C/O NATURHISTOR MUSEUM WIEN PI WIEN PA ZWEITE ZOOLOGISCHE ABTEILUNG (INSEKTEN), BURGRING 7, WIEN, AUSTRIA SN 1994-4136 J9 MYRMECOL NEWS JI Myrmecol. News PD SEP PY 2014 VL 20 BP 25 EP 36 PG 12 WC Entomology SC Entomology GA AO7QG UT WOS:000341547100004 ER PT J AU Quintero, I Gonzalez-Caro, S Zalamea, PC Cadena, CD AF Quintero, Ignacio Gonzalez-Caro, Sebastian Zalamea, Paul-Camilo Daniel Cadena, Carlos TI Asynchrony of Seasons: Genetic Differentiation Associated with Geographic Variation in Climatic Seasonality and Reproductive Phenology SO AMERICAN NATURALIST LA English DT Article DE birds; reproduction; breeding phenology; genetic distance; allochronic speciation; temporal asynchrony ID INCIPIENT ALLOCHRONIC SPECIATION; POPULATION DIVERGENCE; FOOD AVAILABILITY; TROPICAL BIRDS; ANNUAL CYCLES; FOREST BIRD; EVOLUTIONARY; PATTERNS; TIME; PRECIPITATION AB Many organisms exhibit distinct breeding seasons tracking food availability. If conspecific populations inhabit areas that experience different temporal cycles in food availability spurred by variation in precipitation regimes, then they should display asynchronous breeding seasons. Thus, such populations might exhibit a temporal barrier to gene flow, which may potentially promote genetic differentiation. We test a central prediction of this hypothesis, namely, that individuals living in areas with more asynchronous precipitation regimes should be more genetically differentiated than individuals living in areas with more similar precipitation regimes. Using mitochondrial DNA sequences, climatic data, and geographical/ecological distances between individuals of 57 New World bird species mostly from the tropics, we examined the effect of asynchronous precipitation (a proxy for asynchronous resource availability) on genetic differentiation. We found evidence for a positive and significant cross-species effect of precipitation asynchrony on genetic distance after accounting for geographical/ecological distances, suggesting that current climatic conditions may play a role in population differentiation. Spatial asynchrony in climate may thus drive evolutionary divergence in the absence of overt geographic barriers to gene flow; this mechanism contrasts with those invoked by most models of biotic diversification emphasizing physical or ecological changes to the landscape as drivers of divergence. C1 [Quintero, Ignacio; Gonzalez-Caro, Sebastian; Daniel Cadena, Carlos] Univ Los Andes, Dept Ciencias Biol, Lab Biol Evolut Vertebrados, Bogota, Colombia. [Zalamea, Paul-Camilo] Smithsonian Trop Res Inst, Ancon, Panama. RP Quintero, I (reprint author), Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. EM ignacio.quintero@yale.edu NR 90 TC 3 Z9 3 U1 3 U2 31 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD SEP PY 2014 VL 184 IS 3 BP 352 EP 363 DI 10.1086/677261 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AN8HG UT WOS:000340844300009 PM 25141144 ER PT J AU Shik, JZ Santos, JC Seal, JN Kay, A Mueller, UG Kaspari, M AF Shik, Jonathan Z. Santos, Juan C. Seal, Jon N. Kay, Adam Mueller, Ulrich G. Kaspari, Michael TI Metabolism and the Rise of Fungus Cultivation by Ants SO AMERICAN NATURALIST LA English DT Article DE colony size; tribe Attini; hunter-gatherer; metabolic scaling; evolutionary transition ID LEAF-CUTTING ANT; MAJOR EVOLUTIONARY TRANSITIONS; FLORIDA HARVESTER ANT; ATTINE ANT; INDEPENDENT CONTRASTS; LIFE-HISTORY; FORMICIDAE; HYMENOPTERA; GARDENS; WORKERS AB Most ant colonies are comprised of workers that cooperate to harvest resources and feed developing larvae. Around 50 million years ago (MYA), ants of the attine lineage adopted an alternative strategy, harvesting resources used as compost to produce fungal gardens. While fungus cultivation is considered a major breakthrough in ant evolution, the associated ecological consequences remain poorly understood. Here, we compare the energetics of attine colony-farms and ancestral hunter-gatherer colonies using metabolic scaling principles within a phylogenetic context. We find two major energetic transitions. First, the earliest lower-attine farmers transitioned to lower mass-specific metabolic rates while shifting significant fractions of biomass from ant tissue to fungus gardens. Second, a transition 20 MYA to specialized cultivars in the higher-attine clade was associated with increased colony metabolism (without changes in garden fungal content) and with metabolic scaling nearly identical to hypometry observed in hunter-gatherer ants, although only the hunter-gatherer slope was distinguishable from isometry. Based on these evolutionary transitions, we propose that shifting living-tissue storage from ants to fungal mutualists provided energetic storage advantages contributing to attine diversification and outline critical assumptions that, when tested, will help link metabolism, farming efficiency, and colony fitness. C1 [Shik, Jonathan Z.; Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Shik, Jonathan Z.] Univ Copenhagen, Dept Biol, Ctr Social Evolut, DK-2100 Copenhagen, Denmark. [Shik, Jonathan Z.; Kaspari, Michael] Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Santos, Juan C.] Univ British Columbia, Dept Zool, Biodivers Res Ctr, Vancouver, BC V6T 1Z4, Canada. [Santos, Juan C.] Natl Evolutionary Synth Ctr, Durham, NC 27705 USA. [Seal, Jon N.] Univ Texas Tyler, Dept Biol, Tyler, TX 75799 USA. [Kay, Adam] Univ St Thomas, Dept Biol, St Paul, MN 55105 USA. [Mueller, Ulrich G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. RP Shik, JZ (reprint author), Smithsonian Trop Res Inst, Balboa, Ancon, Panama. EM jonathan.shik@gmail.com OI Kaspari, Michael/0000-0002-9717-5768 FU National Science Foundation at the National Evolutionary Synthesis Center [DEB-0842038, DEB-0639879, IOS-0920138, EF-0423641, EF-0905606]; Biodiversity Research Centre's Collaborative Research and Training Experience program at the University of British Columbia FX We thank R. Adams, D. Donoso, and S. Van Bael for help collecting and cultivating attine colonies. D. Donoso also contributed unpublished cytochrome oxidase I sequences used to estimate the chronogram of the ants. This project was funded by the National Science Foundation via grants DEB-0842038 to A.K. and M.K.; DEB-0639879 to U.G.M.; IOS-0920138 to J.N.S. and U.G.M.; and EF-0423641 and EF-0905606 to J.C.S. at the National Evolutionary Synthesis Center. J.C.S. received additional support from the Biodiversity Research Centre's Collaborative Research and Training Experience program at the University of British Columbia. NR 70 TC 5 Z9 5 U1 3 U2 33 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD SEP PY 2014 VL 184 IS 3 BP 364 EP 373 DI 10.1086/677296 PG 10 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA AN8HG UT WOS:000340844300010 PM 25141145 ER PT J AU Jew, NP Erlandson, JM Rick, TC Reeder-Myers, L AF Jew, Nicholas P. Erlandson, Jon M. Rick, Torben C. Reeder-Myers, Leslie TI Oxygen isotope analysis of California mussel shells: seasonality and human sedentism at an 8,200-year-old shell midden on Santa Rosa Island, California SO ARCHAEOLOGICAL AND ANTHROPOLOGICAL SCIENCES LA English DT Article DE Shellfish; Mytilus californianus; Northern Channel Islands; Early Holocene; Human mobility ID CHANNEL-ISLANDS; MYTILUS-EDULIS; PACIFIC COAST; GROWTH; BIOLOGY; AGE; OCCUPATION; RESPONSES; AMERICA; SITES AB To evaluate coastal settlement and land use strategies among maritime hunter-gatherers, we analyzed oxygen isotope (delta O-18) data from 131 marine carbonate samples from 21 California mussel (Mytilus californianus) shells obtained from a large similar to 8,200-year-old shell midden (CA-SRI-666) on California's Santa Rosa Island. Seasonal distributions of the isotopic data were assigned using a paleo-sea surface temperature model created by comparing modern sea surface temperatures (SST) to a fully profiled similar to 8,200-year-old shell. For 20 additional shells, we used two sampling strategies to compare season-of-harvest inferences and explore whether the Early Holocene site occupants were sedentary. Estimated season-of-harvest differed by 35 % between the two sampling methods, corroborating recent isotope analysis of an 8,800-year-old shell midden on San Miguel Island. Shellfish appear to have been collected year-round at CA-SRI-666 from intertidal or subtidal water temperatures similar to modern SST in the vicinity of eastern Santa Rosa Island. The isotope results are consistent with other evidence from CA-SRI-666 that suggest that the site served as a residential base for relatively sedentary maritime people. C1 [Jew, Nicholas P.; Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Jew, Nicholas P.; Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Reeder-Myers, Leslie] So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA. RP Jew, NP (reprint author), Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. EM njew@uoregon.edu; jerland@uoregon.edu; rickt@si.edu; lreeder@smu.edu OI Erlandson, Jon/0000-0002-4705-4319 FU National Science Foundation [0917677, 1212418]; Channel Islands National Park (ARPA Permit) [PWR-1979-09-CA-04] FX The research design for stable isotope analysis was conducted by the senior author, in consultation with Brendan Culleton, Douglas Kennett, and Jack Watts. Our research was supported by the National Science Foundation (#0917677 to Erlandson and Rick and #1212418 to Erlandson and Jew), Channel Islands National Park (ARPA Permit PWR-1979-09-CA-04), and our home institutions. We thank Frances White for help with our statistical analyses and the editor and reviewers of Archaeological and Anthropological Sciences for help with the review, revision, and production of this manuscript. NR 58 TC 7 Z9 7 U1 2 U2 13 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1866-9557 EI 1866-9565 J9 ARCHAEOL ANTHROP SCI JI Archaeol. Anthropol. Sci. PD SEP PY 2014 VL 6 IS 3 BP 293 EP 303 DI 10.1007/s12520-013-0156-1 PG 11 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA AN4XD UT WOS:000340592100007 ER PT J AU Ade, PAR Aikin, RW Amiri, M Barkats, D Benton, SJ Bischoff, CA Bock, JJ Brevik, JA Buder, I Bullock, E Davis, G Day, PK Dowell, CD Duband, L Filippini, JP Fliescher, S Golwala, SR Halpern, M Hasselfield, M Hildebrandt, SR Hilton, GC Irwin, KD Karkare, KS Kaufman, JP Keating, BG Kernasovskiy, SA Kovac, JM Kuo, CL Leitch, EM Llombart, N Lueker, M Netterfield, CB Nguyen, HT O'Brient, R Ogburn, RW Orlando, A Pryke, C Reintsema, CD Richter, S Schwarz, R Sheehy, CD Staniszewski, ZK Story, KT Sudiwala, RV Teply, GP Tolan, JE Turner, AD Vieregg, AG Wilson, P Wong, CL Yoon, KW AF Ade, P. A. R. Aikin, R. W. Amiri, M. Barkats, D. Benton, S. J. Bischoff, C. A. Bock, J. J. Brevik, J. A. Buder, I. Bullock, E. Davis, G. Day, P. K. Dowell, C. D. Duband, L. Filippini, J. P. Fliescher, S. Golwala, S. R. Halpern, M. Hasselfield, M. Hildebrandt, S. R. Hilton, G. C. Irwin, K. D. Karkare, K. S. Kaufman, J. P. Keating, B. G. Kernasovskiy, S. A. Kovac, J. M. Kuo, C. L. Leitch, E. M. Llombart, N. Lueker, M. Netterfield, C. B. Nguyen, H. T. O'Brient, R. Ogburn, R. W. Orlando, A. Pryke, C. Reintsema, C. D. Richter, S. Schwarz, R. Sheehy, C. D. Staniszewski, Z. K. Story, K. T. Sudiwala, R. V. Teply, G. P. Tolan, J. E. Turner, A. D. Vieregg, A. G. Wilson, P. Wong, C. L. Yoon, K. W. CA Bicep2 Collaboration TI BICEP2. II. EXPERIMENT AND THREE-YEAR DATA SET SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; gravitational waves; inflation; instrumentation: polarimeters; telescopes ID TRANSITION-EDGE SENSORS; BACKGROUND POLARIZATION EXPERIMENTS; ANGULAR SCALE POLARIZATION; POWER SPECTRA; GRAVITY-WAVES; SOUTH-POLE; MICROWAVE; ANISOTROPY; RADIATION; PROBE AB We report on the design and performance of the BICEP2 instrument and on its three-year data set. BICEP2 was designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 1 degrees-5 degrees(l = 40-200), near the expected peak of the B-mode polarization signature of primordial gravitational waves from cosmic inflation. Measuring B-modes requires dramatic improvements in sensitivity combined with exquisite control of systematics. The BICEP2 telescope observed from the South Pole with a 26 cm aperture and cold, on-axis, refractive optics. BICEP2 also adopted a new detector design in which beam-defining slot antenna arrays couple to transition-edge sensor (TES) bolometers, all fabricated on a common substrate. The antenna-coupled TES detectors supported scalable fabrication and multiplexed readout that allowed BICEP2 to achieve a high detector count of 500 bolometers at 150 GHz, giving unprecedented sensitivity to B-modes at degree angular scales. After optimization of detector and readout parameters, BICEP2 achieved an instrument noise-equivalent temperature of 15.8 mu K root s. The full data set reached Stokes Q and U map depths of 87.2 nK in square-degree pixels (5'.2 mu K) over an effective area of 384 deg(2) within a 1000 deg(2) field. These are the deepest CMB polarization maps at degree angular scales to date. The power spectrum analysis presented in a companion paper has resulted in a significant detection of B-mode polarization at degree scales. 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.; Lueker, M.; Staniszewski, Z. K.; Teply, G. P.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. [Amiri, M.; Hasselfield, M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada. [Barkats, D.] ESO, Joint ALMA Observ, Santiago, Chile. [Benton, S. J.; Netterfield, C. B.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Bischoff, C. A.; Buder, I.; Karkare, K. S.; Kovac, J. M.; Richter, S.; Vieregg, A. G.; Wong, C. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bock, J. J.; Day, P. K.; Dowell, C. D.; Hildebrandt, S. R.; Llombart, N.; Nguyen, H. T.; O'Brient, R.; Turner, A. D.; Wilson, P.] 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. [Fliescher, S.; Schwarz, R.; Sheehy, C. D.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Hilton, G. C.; Irwin, K. D.; Reintsema, C. D.] NIST, Boulder, CO 80305 USA. [Irwin, K. D.; Kernasovskiy, S. A.; Kuo, C. L.; Ogburn, R. W.; Tolan, J. E.; Yoon, K. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Irwin, K. D.; Ogburn, R. W.; Yoon, K. W.] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [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, Chicago, IL 60637 USA. RP Ade, PAR (reprint author), Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. EM ogburn@stanford.edu OI Orlando, Angiola/0000-0001-8004-5054; Karkare, Kirit/0000-0002-5215-6993; Barkats, Denis/0000-0002-8971-1954; Bischoff, Colin/0000-0001-9185-6514 FU U.S. National Science Foundation [ANT-0742818, ANT-1044978, ANT-0742592, ANT-1110087]; NASA APRA and SAT programs [06-ARPA206-0040, 10-SAT10-0017]; Gordon and Betty Moore Foundation at Caltech; Canada Foundation for Innovation; W.M. Keck Foundation; FAS Science Division Research Computing Group at Harvard University; JPL Research and Technology Development Fund FX BICEP2 was supported by the U.S. National Science Foundation under grants ANT-0742818 and ANT-1044978 (Caltech/Harvard) and ANT-0742592 and ANT-1110087 (Chicago/Minnesota). 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. The receiver development was supported in part by a grant from the W.M. Keck Foundation. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Tireless administrative support was provided by Irene Coyle and Kathy Deniston. NR 71 TC 64 Z9 64 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 SEP 1 PY 2014 VL 792 IS 1 AR 62 DI 10.1088/0004-637X/792/1/62 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100062 ER PT J AU Foley, RJ McCully, C Jha, SW Bildsten, L Fong, WF Narayan, G Rest, A Stritzinger, MD AF Foley, Ryan J. McCully, Curtis Jha, Saurabh W. Bildsten, Lars Fong, Wen-Fai Narayan, Gautham Rest, Armin Stritzinger, Maximilian D. TI POSSIBLE DETECTION OF THE STELLAR DONOR OR REMNANT FOR THE TYPE Iax SUPERNOVA 2008ha SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (UGC 12682); supernovae: general; supernovae: individual (SN 2008ha) ID SINGLE-DEGENERATE SCENARIO; MASSIVE WHITE-DWARF; HELIUM NOVA; SN 2005HK; LOW-LUMINOSITY; V445 PUPPIS; EXPLOSION; MODELS; IMPACT; STAR AB Type Iax supernovae (SNe Iax) are thermonuclear explosions that are related to SNe Ia, but are physically distinct. The most important differences are that SNe Iax have significantly lower luminosity (1%-50% that of typical SNe Ia), lower ejecta mass (similar to 0.1-0.5 M-circle dot), and may leave a bound remnant. The most extreme SN Iax is SN 2008ha, which peaked at M-V = -14.2 mag, about 5 mag below that of typical SNe Ia. Here, we present Hubble Space Telescope (HST) images of UGC 12682, the host galaxy of SN 2008ha, taken 4.1 yr after the peak brightness of SN 2008ha. In these deep, high-resolution images, we detect a source coincident (0.86 HST pixels; 0.'' 043; 1.1 sigma) with the position of SN 2008ha with M-F814W = -5.4 mag. We determine that this source is unlikely to be a chance coincidence, but that scenario cannot be completely ruled out. If this source is directly related to SN 2008ha, it is either the luminous bound remnant of the progenitor white dwarf (WD) or its companion star. The source is consistent with being an evolved >3 M-circle dot initial mass star, and is significantly redder than the SN Iax 2012Z progenitor system, the first detected progenitor system for a thermonuclear SN. If this source is the companion star for SN 2008ha, there is a diversity in SN Iax progenitor systems, perhaps related to the diversity in SN Iax explosions. If the source is the bound remnant of the WD, it must have expanded significantly. Regardless of the nature of this source, we constrain the progenitor system of SN 2008ha to have an age of <80 Myr. C1 [Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [McCully, Curtis; Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Bildsten, Lars] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bildsten, Lars] Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Fong, Wen-Fai] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narayan, Gautham] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Rest, Armin] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Stritzinger, Maximilian D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Foley, RJ (reprint author), Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA. OI Narayan, Gautham/0000-0001-6022-0484; stritzinger, maximilian/0000-0002-5571-1833; McCully, Curtis/0000-0001-5807-7893 FU Association of Universities for Research in Astronomy, Inc., under NASA [NAS 5-26555]; NASA/HST [GO-12913.01]; National Science Foundation (NSF) CAREER award [AST-0847157]; Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant; NSF [PHY 11-25915, AST 11-09174]; [GO-12999] FX 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. These observations are associated with program GO-12999.; This research at Rutgers University was supported through NASA/HST grant GO-12913.01, and National Science Foundation (NSF) CAREER award AST-0847157 to S.W.J. M.D.S. gratefully acknowledges generous support provided by the Danish Agency for Science and Technology and Innovation realized through a Sapere Aude Level 2 grant. This work was supported by the NSF under grants PHY 11-25915 and AST 11-09174. NR 42 TC 24 Z9 24 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2014 VL 792 IS 1 AR 29 DI 10.1088/0004-637X/792/1/29 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100029 ER PT J AU Hermes, JJ Brown, WR Kilic, M Gianninas, A Chote, P Sullivan, DJ Winget, DE Bell, KJ Falcon, RE Winget, KI Mason, PA Harrold, ST Montgomery, MH AF Hermes, J. J. Brown, Warren R. Kilic, Mukremin Gianninas, A. Chote, Paul Sullivan, D. J. Winget, D. E. Bell, Keaton J. Falcon, R. E. Winget, K. I. Mason, Paul A. Harrold, Samuel T. Montgomery, M. H. TI RADIUS CONSTRAINTS FROM HIGH-SPEED PHOTOMETRY OF 20 LOW-MASS WHITE DWARF BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: stellar content; stars: variables: general; white dwarfs ID INITIAL MASS; NLTT 11748; KEPLER OBSERVATIONS; ECLIPSING BINARY; MERGER SYSTEMS; METAL-RICH; HELIUM; EVOLUTION; STARS; COMPANION AB We carry out high-speed photometry on 20 of the shortest-period, detached white dwarf binaries known and discover systems with eclipses, ellipsoidal variations (due to tidal deformations of the visible white dwarf), and Doppler beaming. All of the binaries contain low-mass white dwarfs with orbital periods of less than four hr. Our observations identify the first eight tidally distorted white dwarfs, four of which are reported for the first time here. We use these observations to place empirical constraints on the mass-radius relationship for extremely low-mass (<= 0.30 M-circle dot) white dwarfs. We also detect Doppler beaming in several of these binaries, which confirms their high-amplitude radial-velocity variability. All of these systems are strong sources of gravitational radiation, and long-term monitoring of those that display ellipsoidal variations can be used to detect spin-up of the tidal bulge due to orbital decay. C1 [Hermes, J. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Hermes, J. J.; Winget, D. E.; Bell, Keaton J.; Falcon, R. E.; Winget, K. I.; Harrold, Samuel T.; Montgomery, M. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kilic, Mukremin; Gianninas, A.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Chote, Paul; Sullivan, D. J.] Victoria Univ Wellington, Sch Chem & Phys Sci, Wellington 6140, New Zealand. [Mason, Paul A.] Univ Texas El Paso, Dept Phys, El Paso, TX 79968 USA. RP Hermes, JJ (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM j.j.hermes@warwick.ac.uk RI Alexandros, Gianninas/B-8352-2016 OI Alexandros, Gianninas/0000-0002-8655-4308 FU NSF [AST-0909107, AST-1312678]; Norman Hackerman Advanced Research Program [003658-0252-2009]; European Research Council under the European Union's Seventh Framework Programme/ERC [320964]; NASA [NNX12AC96G] FX We thank the referee M. H. van Kerkwijk for useful comments that greatly improved this manuscript, as well as T. R. Marsh, B. T. Gansicke, and E. L. Robinson for helpful discussions. Some of the McDonald Observatory observations were assisted by G. Miller, K. Luecke, A. Rost, J. Pelletier, S. Wang, G. Earle, M. Moore, A. McCarty, and J. Aguilar, undergraduate students in the University of Texas Freshmen Research Initiative. J. J. H., M. H. M., and D. E. W. gratefully acknowledge the support of the NSF under grants AST-0909107 and AST-1312678, and the Norman Hackerman Advanced Research Program under grant 003658-0252-2009. J. J. H. additionally acknowledges funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC grant agreement No. 320964 (WDTracer). M. K. acknowledges support from the NSF under grant AST-1312678, and thanks Ben Strickland and Steven Ferguson for useful discussions. M. H. M. additionally acknowledges the support of NASA under grant NNX12AC96G. The authors are grateful to the essential assistance of the McDonald Observatory support staff, especially Dave Doss and John Kuehne. Based on observations obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona, as well as 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 70 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 SEP 1 PY 2014 VL 792 IS 1 AR 39 DI 10.1088/0004-637X/792/1/39 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100039 ER PT J AU McIntosh, SW Wang, X Leamon, RJ Davey, AR Howe, R Krista, LD Malanushenko, AV Markel, RS Cirtain, JW Gurman, JB Pesnell, WD Thompson, MJ AF McIntosh, Scott W. Wang, Xin Leamon, Robert J. Davey, Alisdair R. Howe, Rachel Krista, Larisza D. Malanushenko, Anna V. Markel, Robert S. Cirtain, Jonathan W. Gurman, Joseph B. Pesnell, William D. Thompson, Michael J. TI DECIPHERING SOLAR MAGNETIC ACTIVITY. I. ON THE RELATIONSHIP BETWEEN THE SUNSPOT CYCLE AND THE EVOLUTION OF SMALL MAGNETIC FEATURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: atmosphere; Sun: evolution; Sun: general; Sun: interior; Sun: rotation; sunspots ID DIFFERENTIAL ROTATION; MERIDIONAL CIRCULATION; DYNAMO SIMULATION; BRIGHT POINTS; CORONAL HOLE; SUN-SPOTS; FIELD; FLUX; FLOW; OSCILLATIONS AB Sunspots are a canonical marker of the Sun's internal magnetic field which flips polarity every similar to 22 yr. The principal variation of sunspots, an similar to 11 yr variation, modulates the amount of the magnetic field that pierces the solar surface and drives significant variations in our star's radiative, particulate, and eruptive output over that period. This paper presents observations from the Solar and Heliospheric Observatory and Solar Dynamics Observatory indicating that the 11 yr sunspot variation is intrinsically tied to the spatio-temporal overlap of the activity bands belonging to the 22 yr magnetic activity cycle. Using a systematic analysis of ubiquitous coronal brightpoints and the magnetic scale on which they appear to form, we show that the landmarks of sunspot cycle 23 can be explained by considering the evolution and interaction of the overlapping activity bands of the longer-scale variability. C1 [McIntosh, Scott W.; Wang, Xin; Markel, Robert S.; Thompson, Michael J.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Wang, Xin] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Leamon, Robert J.; Malanushenko, Anna V.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Davey, Alisdair R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howe, Rachel] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Krista, Larisza D.] Univ Colorado, Cooperat Inst Res Environm Sci, Boulder, CO 80205 USA. [Malanushenko, Anna V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Cirtain, Jonathan W.] Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Gurman, Joseph B.; Pesnell, William D.] NASA, Goddard Space Flight Ctr, Solar Phys Lab, Greenbelt, MD 20771 USA. RP McIntosh, SW (reprint author), Natl Ctr Atmospher Res, High Altitude Observ, POB 3000, Boulder, CO 80307 USA. EM mscott@ucar.edu RI Pesnell, William/D-1062-2012; OI Pesnell, William/0000-0002-8306-2500; McIntosh, Scott/0000-0002-7369-1776 FU NASA [NNX08AU30G, NNX08AL23G, NNM07AA01C-Hinode, NNG09FA40C-IRIS, NNG04EA00C]; National Science Foundation FX The data used in this paper are openly available from the SOHO, SDO, and the Virtual Solar Observatory (VSO; http://virtualsolar.org) data archives. S.W.M., R.J.L., A.R.D., and R.S.M. were partly funded by NASA grants (NNX08AU30G, NNX08AL23G, NNM07AA01C-Hinode, NNG09FA40C-IRIS). A.V.M. is supported by NASA grant NNG04EA00C (SDO/AIA). SOHO is a project of international collaboration between ESA and NASA. Sunspot data are from David Hathaway and the World Data Center SILSO, Royal Observatory of Belgium, Brussels. S.W.M. is grateful to Matthias Rempel, Yuhong Fan, Dick Altrock, SaraMartin, Roger Ulrich, Paul Charbonneau, Mark Miesch, and Eugene Parker for helpful discussions. NCAR is sponsored by the National Science Foundation. NR 53 TC 13 Z9 13 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 SEP 1 PY 2014 VL 792 IS 1 AR 12 DI 10.1088/0004-637X/792/1/12 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100012 ER PT J AU Pan, LB Padoan, P Scalo, J AF Pan, Liubin Padoan, Paolo Scalo, John TI TURBULENCE-INDUCED RELATIVE VELOCITY OF DUST PARTICLES. III. THE PROBABILITY DISTRIBUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; planets and satellites: formation; protoplanetary disks; turbulence ID BIDISPERSE INERTIAL PARTICLES; ISOTROPIC TURBULENCE; PROTOPLANETARY DISKS; GROWTH PEBBLES; PLANETESIMAL FORMATION; BOUNCING BARRIER; COLLISION; STATISTICS; GRAINS; SIMULATIONS AB Motivated by its important role in the collisional growth of dust particles in protoplanetary disks, we investigate the probability distribution function (PDF) of the relative velocity of inertial particles suspended in turbulent flows. Using the simulation from our previous work, we compute the relative velocity PDF as a function of the friction timescales, tau(p1) and tau(p2), of two particles of arbitrary sizes. The friction time of the particles included in the simulation ranges from 0.1 tau(eta) to 54T(L), where tau(eta) and T-L are the Kolmogorov time and the Lagrangian correlation time of the flow, respectively. The relative velocity PDF is generically non-Gaussian, exhibiting fat tails. For a fixed value of tau(p1), the PDF shape is the fattest for equal-size particles (tau(p2) = tau(p1)), and becomes thinner at both tau(p2) < tau(p1) and tau(p2) > tau(p1). Defining f as the friction time ratio of the smaller particle to the larger one, we find that, at a given f in (1/2) less than or similar to f less than or similar to 1, the PDF fatness first increases with the friction time tau(p,h) of the larger particle, peaks at tau(p,h) similar or equal to tau(eta), and then decreases as tp, h increases further. For 0 <= f less than or similar to (1/4), the PDF becomes continuously thinner with increasing tau(p,h). The PDF is nearly Gaussian only if tau(p,h) is sufficiently large (>> T-L). These features are successfully explained by the Pan & Padoan model. Using our simulation data and some simplifying assumptions, we estimated the fractions of collisions resulting in sticking, bouncing, and fragmentation as a function of the dust size in protoplanetary disks, and argued that accounting for non-Gaussianity of the collision velocity may help further alleviate the bouncing barrier problem. C1 [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Padoan, Paolo] Univ Barcelona, ICREA, E-08028 Barcelona, Spain. [Padoan, Paolo] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Scalo, John] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Pan, LB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lpan@cfa.harvard.edu; ppadoan@icc.ub.edu; parrot@astro.as.utexas.edu OI Padoan, Paolo/0000-0002-5055-5800 NR 57 TC 4 Z9 4 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 SEP 1 PY 2014 VL 792 IS 1 AR 69 DI 10.1088/0004-637X/792/1/69 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100069 ER PT J AU Ruel, J Bazin, G Bayliss, M Brodwin, M Foley, RJ Stalder, B Aird, KA Armstrong, R Ashby, MLN Bautz, M Benson, BA Bleem, LE Bocquet, S Carlstrom, JE Chang, CL Chapman, SC Cho, HM Clocchiatti, A Crawford, TM Crites, AT De Haan, T Desai, S Dobbs, MA Dudley, JP Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Harrington, NL High, FW Holder, GP Holzapfel, WL Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Mohr, JJ Montroy, TE Murray, SS Natoli, T Nurgaliev, D Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Song, J Suhada, R Spieler, HG Stanford, SA Staniszewski, Z Starsk, AA Story, K Stubbs, CW Van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF Ruel, J. Bazin, G. Bayliss, M. Brodwin, M. Foley, R. J. Stalder, B. Aird, K. A. Armstrong, R. Ashby, M. L. N. Bautz, M. Benson, B. A. Bleem, L. E. Bocquet, S. Carlstrom, J. E. Chang, C. L. Chapman, S. C. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. De Haan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. L. High, F. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. 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. Mehl, J. Meyer, S. S. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Natoli, T. Nurgaliev, D. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Song, J. Suhada, R. Spieler, H. G. Stanford, S. A. Staniszewski, Z. Starsk, A. A. Story, K. Stubbs, C. W. Van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI OPTICAL SPECTROSCOPY AND VELOCITY DISPERSIONS OF GALAXY CLUSTERS FROM THE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: clusters: general ID SOUTH-POLE TELESCOPE; BLANCO COSMOLOGY SURVEY; ZELDOVICH EFFECT SURVEY; 720 SQUARE DEGREES; GREATER-THAN 1; SAMPLE; MASS; ANISOTROPY; REDSHIFTS; CATALOG AB We present optical spectroscopy of galaxies in clusters detected through the Sunyaev-Zel'dovich (SZ) effect with the South Pole Telescope (SPT). We report our own measurements of 61 spectroscopic cluster redshifts, and 48 velocity dispersions each calculated with more than 15 member galaxies. This catalog also includes 19 dispersions of SPT-observed clusters previously reported in the literature. The majority of the clusters in this paper are SPT-discovered; of these, most have been previously reported in other SPT cluster catalogs, and five are reported here as SPT discoveries for the first time. By performing a resampling analysis of galaxy velocities, we find that unbiased velocity dispersions can be obtained from a relatively small number of member galaxies (less than or similar to 30), but with increased systematic scatter. We use this analysis to determine statistical confidence intervals that include the effect of membership selection. We fit scaling relations between the observed cluster velocity dispersions and mass estimates from SZ and X-ray observables. In both cases, the results are consistent with the scaling relation between velocity dispersion and mass expected from dark-matter simulations. We measure a similar to 30% log-normal scatter in dispersion at fixed mass, and a similar to 10% offset in the normalization of the dispersion-mass relation when compared to the expectation from simulations, which is within the expected level of systematic uncertainty. C1 [Ruel, J.; Bayliss, M.; Nurgaliev, D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bazin, G.; Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bazin, G.; Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Bayliss, M.; Foley, R. J.; Stalder, B.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Murray, S. S.; Starsk, A. A.; Stubbs, C. W.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Foley, R. J.; Vieira, J. D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, R. J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Armstrong, R.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Inst Astrofis, Santiago, Chile. [De Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; Van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [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. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; 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. [Lueker, M.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 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. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [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, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP Ruel, J (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM mbayliss@cfa.harvard.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080; 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 NASA; National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; NASA [12800071, 12800088, 13800883, NAS 8-03060]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Cluster of Excellence "Origin and Structure of the Universe," - Excellence Initiative of the Federal Government of Germany, EXC project [153]; Clay Fellowship; KICP Fellowship; Pennsylvania State University [2834-MIT-SAO-4018]; Alfred P. Sloan Research Fellowship; Smithsonian Institution; Brinson Foundation; PFB-06 CATA, Chile; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; Blanco 4 m at Cerro Tololo Interamerican Observatories [2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598] FX Optical imaging data from the Blanco 4 m at Cerro Tololo Interamerican Observatories (programs 2005B-0043, 2009B-0400, 2010A-0441, 2010B-0598) are included in this work. Additional imaging data were obtained with the 6.5 m Magellan Telescopes and the Swope telescope, which are located at the Las Campanas Observatory in Chile. This work is based in part on observations made with the Spitzer Space Telescope (PIDs 60099, 70053), which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech.; The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. 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. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012. Galaxy cluster research at SAO is supported in part by NSF grants AST-1009649 and MRI-0723073. Support for X-ray analysis was provided by NASA through Chandra Award Nos. 12800071, 12800088, and 13800883 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. 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. X-ray research at the CfA is supported through NASA Contract NAS 8-03060. The Munich group was supported by The Cluster of Excellence "Origin and Structure of the Universe," funded by the Excellence Initiative of the Federal Government of Germany, EXC project number 153. R.J.F. is supported by a Clay Fellowship. B. A. B is supported by a KICP Fellowship, M. B. and M. M. acknowledge support from contract 2834-MIT-SAO-4018 from the Pennsylvania State University to the Massachusetts Institute of Technology. M. D. acknowledges support from an Alfred P. Sloan Research Fellowship, W. F. and C.J. acknowledge support from the Smithsonian Institution. B. S. acknowledges support from the Brinson Foundation. A. C. received support from PFB-06 CATA, Chile. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 58 TC 30 Z9 30 U1 1 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 SEP 1 PY 2014 VL 792 IS 1 AR 45 DI 10.1088/0004-637X/792/1/45 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100045 ER PT J AU Zahid, HJ Kashino, D Silverman, JD Kewley, LJ Daddi, E Renzini, A Rodighiero, G Nagao, T Arimoto, N Sanders, DB Kartaltepe, J Lilly, SJ Maier, C Geller, MJ Capak, P Carollo, CM Chu, J Hasinger, G Ilbert, O Kajisawa, M Koekemoer, AM Kovac, K Le Fevre, O Masters, D McCracken, HJ Onodera, M Scoville, N Strazzullo, V Sugiyama, N Taniguchi, Y AF Zahid, H. J. Kashino, D. Silverman, J. D. Kewley, L. J. Daddi, E. Renzini, A. Rodighiero, G. Nagao, T. Arimoto, N. Sanders, D. B. Kartaltepe, J. Lilly, S. J. Maier, C. Geller, M. J. Capak, P. Carollo, C. M. Chu, J. Hasinger, G. Ilbert, O. Kajisawa, M. Koekemoer, A. M. Kovac, K. Le Fevre, O. Masters, D. McCracken, H. J. Onodera, M. Scoville, N. Strazzullo, V. Sugiyama, N. Taniguchi, Y. CA COSMOS TEAM TI THE FMOS-COSMOS SURVEY OF STAR-FORMING GALAXIES AT z similar to 1.6. II. THE MASS-METALLICITY RELATION AND THE DEPENDENCE ON STAR FORMATION RATE AND DUST EXTINCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: fundamental parameters; galaxies: ISM ID DIGITAL SKY SURVEY; STELLAR POPULATION SYNTHESIS; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT; PHYSICAL-PROPERTIES; OXYGEN ABUNDANCES; SUBARU-TELESCOPE; GAS METALLICITY; LOCAL UNIVERSE; HOST GALAXIES AB We investigate the relationships between stellar mass, gas-phase oxygen abundance (metallicity), star formation rate (SFR), and dust content of star-forming galaxies at z similar to 1.6 using Subaru/FMOS spectroscopy in the COSMOS field. The mass-metallicity (MZ) relation at z similar to 1.6 is steeper than the relation observed in the local universe. The steeper MZ relation at z similar to 1.6 is mainly due to evolution in the stellar mass where the MZ relation begins to turnover and flatten. This turnover mass is 1.2 dex larger at z similar to 1.6. The most massive galaxies at z similar to 1.6 (similar to 10(11) M-circle dot) are enriched to the level observed in massive galaxies in the local universe. The MZ relation we measure at z similar to 1.6 supports the suggestion of an empirical upper metallicity limit that does not significantly evolve with redshift. We find an anti-correlation between metallicity and SFR for galaxies at a fixed stellar mass at z similar to 1.6, which is similar to trends observed in the local universe. We do not find a relation between stellar mass, metallicity, and SFR that is independent of redshift; rather, our data suggest that there is redshift evolution in this relation. We examine the relation between stellar mass, metallicity, and dust extinction, and find that at a fixed stellar mass, dustier galaxies tend to be more metal rich. From examination of the stellar masses, metallicities, SFRs, and dust extinctions, we conclude that stellar mass is most closely related to dust extinction. C1 [Zahid, H. J.; Sanders, D. B.; Chu, J.; Hasinger, G.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Kashino, D.; Sugiyama, N.] Nagoya Univ, Grad Sch Sci, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan. [Silverman, J. D.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Kewley, L. J.; Sugiyama, N.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Daddi, E.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Renzini, A.] INAF Osserv Astron Padova, I-35122 Padua, Italy. [Rodighiero, G.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Nagao, T.; Kovac, K.] Kyoto Univ, Hakubi Ctr Adv Res, Kyoto 6068302, Japan. [Arimoto, N.] Subaru Telescope, Natl Astron Observ Japan, Hilo, HI 96720 USA. [Arimoto, N.; Strazzullo, V.] Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. [Kartaltepe, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Lilly, S. J.; Carollo, C. M.; Onodera, M.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Maier, C.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Geller, M. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Capak, P.] CALTECH, Pasadena, CA 91125 USA. [Capak, P.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Ilbert, O.; Le Fevre, O.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Kajisawa, M.; Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Koekemoer, A. M.] Space Telescope Sci Inst, HST & JWST Instruments, Baltimore, MD 21218 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Div Sci, Baltimore, MD 21218 USA. [Masters, D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [McCracken, H. J.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Scoville, N.] CALTECH, Pasadena, CA 91125 USA. RP Zahid, HJ (reprint author), Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. EM jabran@ifa.hawaii.edu RI Daddi, Emanuele/D-1649-2012; OI Daddi, Emanuele/0000-0002-3331-9590; Maier, Christian/0000-0001-6405-2182; Kashino, Daichi/0000-0001-9044-1747; Chu, Jason/0000-0003-3955-2470; Rodighiero, Giulia/0000-0002-9415-2296; Koekemoer, Anton/0000-0002-6610-2048 FU World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan; Program for Leading Graduate Schools PhD Professional; Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan; [22340056]; [23224005]; [25707010] FX We thank the anonymous referee for a careful reading and for many useful suggestions that greatly improved this paper. This work is possible through the important contribution of Kentaro Aoki and the Subaru Telescope staff who assisted in acquiring much of the data presented in this work. This work was supported by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan. This work has been partially supported by the Grant-in-Aid for the Scientific Research Fund under grant Nos. 22340056: N.S., 23224005: N.A., 25707010 and Program for Leading Graduate Schools PhD Professional: Gateway to Success in Frontier Asia commissioned by the Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan. We are also grateful to INAF for regular support through grant "PRIN-2010." We acknowledge the importance of Mauna Kea within the indigenous Hawaiian community and with all respect say mahalo for the use of this sacred site. NR 106 TC 50 Z9 50 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 SEP 1 PY 2014 VL 792 IS 1 AR 75 DI 10.1088/0004-637X/792/1/75 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100075 ER PT J AU Zhu, L Long, RJ Mao, S Peng, EW Liu, CZ Caldwell, N Li, B Blakeslee, JP Cote, P Cuillandre, JC Durrell, P Emsellem, E Ferrarese, L Gwyn, S Jordan, A Lancon, A Mei, S Munoz, R Puzia, T AF Zhu, Ling Long, R. J. Mao, Shude Peng, Eric W. Liu, Chengze Caldwell, Nelson Li, Biao Blakeslee, John P. Cote, Patrick Cuillandre, Jean-Charles Durrell, Patrick Emsellem, Eric Ferrarese, Laura Gwyn, Stephen Jordan, Andres Lancon, Ariane Mei, Simona Munoz, Roberto Puzia, Thomas TI THE NEXT GENERATION VIRGO CLUSTER SURVEY. V. MODELING THE DYNAMICS OF M87 WITH THE MADE-TO-MEASURE METHOD SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M87); Galaxy: kinematics and dynamics; globular clusters: general; methods: numerical; surveys ID EARLY-TYPE GALAXIES; DARK-MATTER HALO; BLACK-HOLE MASS; X-RAY BRIGHT; GLOBULAR-CLUSTERS; ELLIPTIC GALAXIES; LENTICULAR GALAXIES; SAURON PROJECT; ORBITAL STRUCTURE; PARTICLE MODELS AB We study the dynamics of the giant elliptical galaxy M87 from the central to the outermost regions with the made-to-measure (M2M) method. We use a new catalog of 922 globular cluster line-of-sight velocities extending to a projected radius of 180 kpc (equivalent to 25 M87 effective radii), and SAURON integral field unit data within the central 2.4 kpc. There are 263 globular clusters, mainly located beyond 40 kpc, newly observed by the Next Generation Virgo Survey. For the M2M modeling, the gravitational potential is taken as a combination of a luminous matter potential with a constant stellar mass-to-light ratio and a dark matter potential modeled as a logarithmic potential. Our best-fit dynamical model returns a stellar mass-to-light ratio in the I band of M/L-I = 6.0 +/- 0.3 M circle dot L circle dot-1 with a dark matter potential scale velocity of 591 +/- 50 km s(-1) and scale radius of 42 +/- 10 kpc. We determine the total mass of M87 within 180 kpc to be (1.5 +/- 0.2) x 10(13) M-circle dot. The mass within 40 kpc is smaller than previous estimates determined using globular cluster kinematics that did not extend beyond similar to 45 kpc. With our new globular cluster velocities at much larger radii, we see that globular clusters around 40 kpc show an anomalously large velocity dispersion which affected previous results. The mass we derive is in good agreement with that inferred from ROSAT X-ray observation out to 180 kpc. Within 30 kpc our mass is also consistent with that inferred from Chandra and XMM-Newton X-ray observations, while within 120 kpc it is about 20% smaller. The model velocity dispersion anisotropy beta parameter for the globular clusters in M87 is small, varying from -0.2 at the center to 0.2 at similar to 40 kpc, and gradually decreasing to zero at similar to 120 kpc. C1 [Zhu, Ling; Long, R. J.; Mao, Shude] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Zhu, Ling] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Zhu, Ling] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Zhu, Ling] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. [Long, R. J.; Mao, Shude] Univ Manchester, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Peng, Eric W.; Li, Biao] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Peng, Eric W.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Liu, Chengze] Shanghai Jiao Tong Univ, Dept Phys & Astron, Shanghai 200240, Peoples R China. [Liu, Chengze] Shanghai Jiao Tong Univ, INPAC, Dept Phys, Shanghai 200240, Peoples R China. [Liu, Chengze] Shanghai Jiao Tong Univ, Shanghai Key Lab Particle Phys & Cosmol, Shanghai 200240, Peoples R China. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blakeslee, John P.; Cote, Patrick; Ferrarese, Laura; Gwyn, Stephen] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Cuillandre, Jean-Charles] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Durrell, Patrick] Youngstown State Univ, Dept Phys & Astron, Youngstown, OH 44555 USA. [Emsellem, Eric] Univ Lyon 1, Observ Lyon, CRAL, ENS Lyon,CNRS,UMR 5574, F-69230 St Genis Laval, France. [Emsellem, Eric] European So Observ, D-85748 Garching, Germany. [Jordan, Andres; Munoz, Roberto; Puzia, Thomas] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Lancon, Ariane] Univ Strasbourg, CNRS, Observ astronom Strasbourg, UMR 7550, F-67000 Strasbourg, France. [Mei, Simona] Observ Paris, GEPI, F-67000 Strasbourg, France. [Mei, Simona] Univ Paris Denis Diderot, F-75205 Paris 13, France. RP Zhu, L (reprint author), Chinese Acad Sci, Natl Astron Observ, A20 Datun Rd, Beijing 100012, Peoples R China. EM lzhu@mpia-hd.mpg.de RI Liu, Chengze/O-1034-2015; OI Liu, Chengze/0000-0002-4718-3428; Jordan, Andres/0000-0002-5389-3944; Blakeslee, John/0000-0002-5213-3548 NR 84 TC 18 Z9 18 U1 0 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 SEP 1 PY 2014 VL 792 IS 1 AR 59 DI 10.1088/0004-637X/792/1/59 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2RE UT WOS:000341172100059 ER PT J AU Andrews, BJ AF Andrews, Benjamin J. TI Dispersal and air entrainment in unconfined dilute pyroclastic density currents SO BULLETIN OF VOLCANOLOGY LA English DT Article DE Pyroclastic density currents; Experimental volcanology; Entrainment; Explosive volcanism ID FLOW HAZARD ASSESSMENT; TAUPO IGNIMBRITE; ERUPTION; VOLCANO; DYNAMICS; EMPLACEMENT; VESUVIUS; DEPOSITS; THERMODYNAMICS; SEDIMENTATION AB Unconfined scaled laboratory experiments show that 3D structures control the behavior of dilute pyroclastic density currents (PDCs) during and after liftoff. Experiments comprise heated and ambient temperature 20 mu m talc powder turbulently suspended in air to form density currents within an unobstructed 8.5x6x2.6-m chamber. Comparisons of Richardson, thermal Richardson, Froude, Stokes, and settling numbers and buoyant thermal to kinetic energy densities show good agreement between experimental currents and dilute PDCs. The experimental Reynolds numbers are lower than those of PDCs, but the experiments are fully turbulent; thus, the large-scale dynamics are similar between the two systems. High-frequency, simultaneous observation in three orthogonal planes shows that the currents behave very differently than previous 2D (i.e., confined) currents. Specifically, whereas ambient temperature currents show radial dispersal patterns, buoyancy reversal, and liftoff of heated currents focuses dispersal along narrow axes beneath the rising plumes. The aspect ratios, defined as the current length divided by a characteristic width, are typically 2.5-3.5 in heated currents and 1.5-2.5 in ambient temperature currents, reflecting differences in dispersal between the two types of currents. Mechanisms of air entrainment differ greatly between the two currents: entrainment occurs primarily behind the heads and through the upper margins of ambient temperature currents, but heated currents entrain air through their lateral margins. That lateral entrainment is much more efficient than the vertical entrainment, >0.5 compared to similar to 0.1, where entrainment is defined as the ratio of cross-stream to streamwise velocity. These experiments suggest that generation of coignimbrite plumes should focus PDCs along narrow transport axes, resulting in elongate rather than radial deposits. C1 Smithsonian Inst, Global Volcanism Program, Washington, DC 20560 USA. RP Andrews, BJ (reprint author), Smithsonian Inst, Global Volcanism Program, Washington, DC 20560 USA. EM andrewsb@si.edu FU Smithsonian Institution Grand Challenges program; National Museum of Natural History Small Grants program; SI Competitive Grants Program for Science FX R. Dennen was instrumental in the construction of the experimental facility used in this research. T. Gooding provided technical insights regarding instrumentation of the facility. R. Dennen and G. Ramirez helped run many of the experiments presented in this paper. M. Manga provided helpful feedback on an early draft of this manuscript. Thorough and thoughtful comments by O. Roche and B. Brand improved this paper. This research was supported by funding from the Smithsonian Institution Grand Challenges program, the National Museum of Natural History Small Grants program, and the SI Competitive Grants Program for Science. NR 35 TC 9 Z9 9 U1 2 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0258-8900 EI 1432-0819 J9 B VOLCANOL JI Bull. Volcanol. PD SEP PY 2014 VL 76 IS 9 AR 852 DI 10.1007/s00445-014-0852-4 PG 14 WC Geosciences, Multidisciplinary SC Geology GA AO5EM UT WOS:000341366100003 ER PT J AU Huffer, D Chappell, D AF Huffer, Damien Chappell, Duncan TI The mainly nameless and faceless dead: an exploratory study of the illicit traffic in archaeological and ethnographic human remains SO CRIME LAW AND SOCIAL CHANGE LA English DT Article ID REPATRIATION; TROPHIES; OBJECTS AB This paper represents an exploratory study of what is known about the current global trade in human remains, and in particular, specimens from archaeological or ethnographic contexts, regardless of which source countries they derive from and where they are destined. The paper is in four parts. In Part 1, we explain how the analysis of human remains forms an important component of archaeological research, and why looting activity at burial sites prejudice this research. In Part 2 we review the existing and relevant archaeological, ethnographic and criminological literature on the subject while in Part 3 we describe our own research into the online trade in human remains, both licit and illicit. To assess the current global prevalence and distribution of public and private dealers in human remains, keyword searches on common search engines (Google, Yahoo, Bing), and online sites like eBay and Amazon were conducted. In Part 4 we draw some conclusions about our research and point in particular to various policy and law reform issues which require further consideration and study. C1 [Huffer, Damien] MSC, Smithsonian Museum Conservat Inst, Suitland, MD 20746 USA. [Chappell, Duncan] Univ Sydney, Fac Law, Inst Criminol, Darlinghurst, NSW 2006, Australia. RP Huffer, D (reprint author), MSC, Smithsonian Museum Conservat Inst, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM hufferd@si.edu; Duncan.Chappell@usyd.edu.au NR 83 TC 1 Z9 1 U1 0 U2 6 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0925-4994 EI 1573-0751 J9 CRIME LAW SOCIAL CH JI Crime Law Soc. Change PD SEP PY 2014 VL 62 IS 2 BP 131 EP 153 DI 10.1007/s10611-014-9528-4 PG 23 WC Criminology & Penology; Social Sciences, Interdisciplinary SC Criminology & Penology; Social Sciences - Other Topics GA AN4WE UT WOS:000340588800003 ER PT J AU McDonald, KA Collin, R Lesoway, MP AF McDonald, Kathryn A. Collin, Rachel Lesoway, Maryna P. TI Poecilogony in the caenogastropod Calyptraea lichen (Mollusca: Gastropoda) SO INVERTEBRATE BIOLOGY LA English DT Article DE adelphophagy; Calyptraeidae; polyphenism; mode of development; plasticity ID BOCCARDIA-PROBOSCIDEA POLYCHAETA; MARINE-INVERTEBRATES; LARVAL DEVELOPMENT; PHYLOGENETIC-RELATIONSHIPS; EVOLUTIONARY TRANSITIONS; CREPIDULA GASTROPODA; NORTHERN CHILE; MODE; POPULATION; SPIONIDAE AB In marine invertebrates, polymorphism and polyphenism in mode of development are known as "poecilogony." Understanding the environmental correlates of poecilogony and the developmental mechanisms that produce it could contribute to a better understanding of evolutionary transitions in mode of development. However, poecilogony is rare in marine invertebrates, with only ten recognized, well-documented cases. Five examples occur in sacoglossan gastropods, and five occur in spionid polychaetes. Here, we document the eleventh case, and the first in a caenogastropod mollusc. Females of Calyptraea lichen collected in the field or reared in the laboratory often produce broods of planktotrophic larvae. They can also be collected with mixed broods, in which each capsule contains planktotrophic larvae, nurse embryos, and adelphophagic embryos. Adelphophages eat the nurse embryos and hatch as short-lived lecithotrophic larvae, or even as juveniles. Mitochondrial COI and 16S DNA sequences for females with different types of broods differ by less than 0.5%, supporting conspecific status. Some females collected in the field with mixed broods subsequently produced planktotrophic broods, demonstrating that females can produce two different kinds of broods. Calyptraea lichen is therefore polyphenic in two ways: mode of development can vary among embryos within a capsule, and females can change the types of broods they produce. C1 [McDonald, Kathryn A.; Collin, Rachel; Lesoway, Maryna P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Lesoway, Maryna P.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP McDonald, KA (reprint author), Humboldt State Univ, Dept Biol Sci, Arcata, CA 95521 USA. EM kamcdon@post.harvard.edu OI Collin, Rachel/0000-0001-5103-4460 FU Smithsonian Tropical Research Institute Tupper Postdoctoral fellowship; United States National Science Foundation [IOS-1019727] FX We thank Collin Lab members for help in the lab and field, Axel Calderon for DNA sequencing, and Carolyn Savoldelli for measuring embryos in three broods. Comments from two anonymous reviewers greatly improved this manuscript. This work was supported by a Smithsonian Tropical Research Institute Tupper Postdoctoral fellowship to KM and a United States National Science Foundation grant IOS-1019727 to RC. NR 38 TC 4 Z9 5 U1 2 U2 9 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1077-8306 EI 1744-7410 J9 INVERTEBR BIOL JI Invertebr. Biol. PD SEP PY 2014 VL 133 IS 3 BP 213 EP 220 DI 10.1111/ivb.12057 PG 8 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA AO2TT UT WOS:000341179600002 ER PT J AU Reeder-Myers, LA AF Reeder-Myers, Leslie A. TI Multi-scalar foraging decisions in the Santa Barbara Channel, southern California SO JOURNAL OF ANTHROPOLOGICAL ARCHAEOLOGY LA English DT Article DE Spatial modeling; Central place foraging; Santa Barbara Channel; GIS; Settlement patterns; Multi-criteria decision analysis; Species distribution modeling; Northern Channel Islands ID DAISY CAVE CA-SMI-261; MIGUEL ISLAND; ROSA ISLAND; BEHAVIORAL ECOLOGY; CURRENT SYSTEM; CLIMATE-CHANGE; NORTH-AMERICA; HUMAN IMPACTS; GREAT-BASIN; BODY-SIZE AB Hunter-gatherer decisions about where to live were influenced by many behaviors, some easier to see in the archaeological record (i.e. hunting or trapping vertebrates, gathering shellfish, quarrying and flint knapping) and some more difficult (i.e. gathering and processing plants, environmental variability, spiritual meaning, social relationships). Spatial modeling provides a tool to examine some of those decisions based on how they influenced the location of sites. This study uses the tenets of central place foraging theory to build a multi-scalar settlement model for the Santa Barbara Channel of southern California, where rising sea levels during the Late Pleistocene and Early Holocene erased a large portion of the existing archaeological record and studies of macrobotanical remains are limited. The model is evaluated through comparison with the archaeological record, and reveals a complex set of priorities in decisions about landscape use. People appear to have evaluated different resource categories freshwater, protein, carbohydrates, and lithic raw materials at different spatial scales depending in part on their importance to subsistence but also on the variable productivity and distribution of the resources themselves. Spatial modeling has considerable potential for both analyzing the existing record and generating hypotheses for future research. (C) 2014 Elsevier Inc. All rights reserved. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. RP Reeder-Myers, LA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. EM reeder-myersL@si.edu NR 130 TC 2 Z9 2 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 0278-4165 EI 1090-2686 J9 J ANTHROPOL ARCHAEOL JI J. Anthropol. Archaeol. PD SEP PY 2014 VL 35 BP 202 EP 219 DI 10.1016/j.jaa.2014.06.002 PG 18 WC Anthropology; Archaeology SC Anthropology; Archaeology GA AN7WE UT WOS:000340810900015 ER PT J AU Sohn, JC AF Sohn, Jae-Cheon TI A new genus and species of Urodidae (Lepidoptera: Urodoidea) from Sri Lanka SO JOURNAL OF ASIA-PACIFIC ENTOMOLOGY LA English DT Article DE New genus and species; Oriental Region; Sri Lanka; Taxonomy; Urodidae ID WOCKIA HEINEMANN AB A new genus of Urodidae, Geoesthia gen. nov., is described with the type species, Geoesthia ceylonica sp. nov. from Sri Lanka. This is the second urodid genus from the Oriental Region. The new species is the only urodid recorded from Sri Lanka. The new genus is distinguished from all the known genera within Urodidae by a combination of four characteristics: the lack of scale tufts on the labial palpi; the absence of raised scales of two subbasal spots on the forewings; the presence of M-stem on the hindwings; and the female corpus bursae bearing five signa. Key to the genera and species of Urodidae from the Oriental Region is 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] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Sohn, Jae-Cheon] Natl Museum Nat Hist, Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. RP Sohn, JC (reprint author), Univ Maryland, Dept Entomol, 4112 Plant Sci Bldg, College Pk, MD 20742 USA. EM jsohn@umd.edu FU US National Science Foundation's Assembling the Tree of Life program [0531769] FX I would like to thank Jon (Buck) Lewis (retired, US Department of Agriculture, TN, USA) for reviewing an early stage of the manuscript. I am also grateful to Kevin Tuck (Natural History Museum, London) for allowing me to examine the museum specimens under his care. My visit to the Natural History Museum, London, was partly supported by the US National Science Foundation's Assembling the Tree of Life program, award number 0531769. NR 12 TC 0 Z9 0 U1 1 U2 7 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 SEP PY 2014 VL 17 IS 3 BP 441 EP 443 DI 10.1016/j.aspen.2014.03.008 PG 3 WC Entomology SC Entomology GA AN6VY UT WOS:000340737700036 ER PT J AU Lee, MY Munroe, TA Shao, KT AF Lee, M-Y Munroe, T. A. Shao, K-T TI Description of a new cryptic, shallow-water tonguefish (Pleuronectiformes: Cynoglossidae: Symphurus) from the western North Pacific Ocean SO JOURNAL OF FISH BIOLOGY LA English DT Article DE cryptic species; DNA barcoding; Symphurus leucochilus; Symphurus microrhynchus; Symphurus orientalis ID 16S RIBOSOMAL-RNA; GULF-OF-CALIFORNIA; HYDROTHERMAL VENTS; LARVAL DEVELOPMENT; TAXONOMIC STATUS; ATLANTIC-OCEAN; IDENTIFICATION; PERCIFORMES; DIVERGENCE; AUSTRALIA AB Combined results based on morphological characters and analyses of partial sequences of the 16s rRNA and coI genes confirm the validity of a new, cryptic, symphurine tonguefish from the western North Pacific Ocean. Symphurus leucochilus n. sp., a diminutive species reaching sizes to c. 67 mm standard length, is described from nine specimens that were collected from fish-landing ports and from trawls made at c. 150 m off Taiwan and Japan. Symphurus leucochilus shares many similar features with those of Symphurus microrhynchus and that of several undescribed species that are morphologically similar to S. microrhynchus. Symphurus leucochilus has also been misidentified as Symphurus orientalis in fish collections because of shared similarities in some aspects of their morphology. The new species differs from all congeners by the following combination of meristic, morphological and pigmentation features: a predominant 1-2-2-2-2 pattern of interdigitation of proximal dorsal-fin pterygiophores and neural spines; 12 caudal-fin rays; 89-92 dorsal-fin rays; 76-80 anal-fin rays; 49-51 total vertebrae; four hypurals; 75-83 longitudinal scale rows; 32-35 transverse scales; 15-17 scale rows on the head posterior to the lower orbit; absence of a fleshy ridge on the ocular-side lower jaw and a membranous connection between the anterior nostril and lower part of the eye; a narrow interorbital space and dorsal-fin origin anterior to the vertical through the anterior margin of the upper eye; absence of both dermal spots at bases of anterior dorsal-fin rays and melanophores on the isthmus; uniformly yellow to light-brown ocular-side colouration without bands; dorsal and anal fins with alternating series of dark rectangular blotches and unpigmented areas; a uniform white blind side and a bluish-black peritoneum. Despite overall similarities in morphology between S. leucochilus and S. orientalis, as well as between two of the nominal species morphologically similar to S. microrhynchus, analyses of partial 16s rRNA and coI gene sequences show that S. leucochilus, S. orientalis and the two other nominal species represent three distinct lineages within the genus Symphurus. (C) 2014 The Fisheries Society of the British Isles C1 [Lee, M-Y] Natl Taiwan Ocean Univ, Dept Aquaculture, Keelung 20224, Taiwan. [Munroe, T. A.] NOAA, Natl Marine Fisheries Serv, Natl Systemat Lab, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. [Shao, K-T] Acad Sinica, Lab Fish Ecol & Evolut, Biodivers Res Ctr, Taipei 11529, Taiwan. RP Shao, KT (reprint author), Acad Sinica, Lab Fish Ecol & Evolut, Biodivers Res Ctr, Taipei 11529, Taiwan. EM zoskt@gate.sinica.edu.tw FU National Science Council [NSC 96-2628-B-001-006-MY3, NSC 99-2621-B-001-008-MY3]; Biodiversity Research Center, Academia Sinica FX This work represents a portion of a collecting activities grant investigating the biodiversity and systematics of deep-sea fishes in Taiwanese waters supported by the National Science Council (NSC 96-2628-B-001-006-MY3 and NSC 99-2621-B-001-008-MY3) and awarded to K.-T.S., Biodiversity Research Center, Academia Sinica. The authors thank H.-C. Ho, P. and L.-P. Lin who assisted with collecting specimens, and with loans and shipments of specimens used in this study. They are especially grateful to H.-C. Ho for providing tissue samples of S. cf. microrhynchus from Viet Nam. K.-C. Hsu advised M.-Y.L. regarding molecular aspects of this research study. M. Nizinski provided assistance and support during M.-Y.L.'s visit to the National Museum of Natural History, Smithsonian Institution. H. Endo, N. Nakayama and R. Asaoka provided assistance and support during M.-Y.L.'s visit to the Department of Biology, Faculty of Science, Kochi University. They also provided three important fresh specimens of S. leucochilus from Japanese waters that assisted with the discovery of this sympatric cryptic species. L. Willis, NMFS-NSL, assisted with literature and specimens. J. Clayton and D. Smith, USNM, assisted with accessioning and cataloguing specimens. M.-Y.L. also extends his appreciation to all members of the Laboratory of Fish Ecology and Evolution for their support and assistance, especially to H. Lee who made the distribution map for this study. NR 66 TC 2 Z9 2 U1 1 U2 12 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 SEP PY 2014 VL 85 IS 3 BP 563 EP 585 DI 10.1111/jfb.12440 PG 23 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA AN8HR UT WOS:000340845500001 PM 25040425 ER PT J AU Ocampo, EH Nunez, JD Cledon, M Baeza, JA AF Ocampo, Emiliano H. Nunez, Jesus D. Cledon, Maximiliano Antonio Baeza, J. TI Parasitic castration in slipper limpets infested by the symbiotic crab Calyptraeotheres garthi SO MARINE BIOLOGY LA English DT Article ID PINNOTHERES-OSTREUM-SAY; PEA CRAB; LIFE-HISTORY; CREPIDULA-CACHIMILLA; GASTROPODA; REPRODUCTION; GROWTH; ARGENTINA; BIOLOGY; CALYPTRAEIDAE AB Two ill-explored hypotheses might explain host castration by parasitic pea crabs. The 'energy drain' hypothesis states that castration is caused by host-derived nutrient consumption of parasites that ultimately diminishes host-energy intake. The 'steric interference' hypothesis states that castration occurs when parasites physically inhibit host reproduction. This study evaluated whether Calyptraeotheres garthi, a pea crab from the southwestern Atlantic, is a parasitic castrator and explored whether the two hypotheses above explain castration in the limpet Crepidula cachimilla. None of three studied limpet species brooded embryos during the reproductive season when infested by mature female pea crabs. Also, limpets of C. cachimilla infested by C. garthi did not reproduce during a 90-day experimental period while crab-free limpets did spawn embryos during this period. Limpets resumed reproduction soon after pea crabs were experimentally removed from their brooding chamber. Thus, C. garthi does castrate limpets, and castration is reversible. Pea crabs 'steal' food from limpets, and infested limpets did not modify their feeding behavior to counteract nutrient loss. Thus, infested limpets are expected to ingest less food which provides partial support for the 'energy drain' hypothesis. However, the limpet's body condition increased or was not affected by pea crabs during the breeding season which argues against the same hypothesis. Furthermore, that limpets promptly recovered reproductive activity once pea crabs were experimentally removed, that castration was not induced by the smallest pea crabs in the population (that fill only partially the brooding chamber), and that parasitized limpets did exhibit fully mature ovaries, support the 'steric interference' hypothesis explaining parasitic castration. C1 [Ocampo, Emiliano H.; Nunez, Jesus D.] CONICET UNMDP, Lab Invertebrados, IIMYC Inst Invest Marinas & Costeras, RA-7600 Buenos Aires, DF, Argentina. [Cledon, Maximiliano] CONICET UNMDP, EGEM Lab Ecol & Genet Especies Marinas, IIMYC, RA-7600 Buenos Aires, DF, Argentina. [Antonio Baeza, J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29632 USA. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Coquimbo, Chile. RP Ocampo, EH (reprint author), CONICET UNMDP, Lab Invertebrados, IIMYC Inst Invest Marinas & Costeras, Funes 3350, RA-7600 Buenos Aires, DF, Argentina. EM eocampo@mdp.edu.ar FU CONICET-Consejo Nacional de Investigaciones Cientificas y Tecnicas de Argentina [PIP 2008 112-384 200-801-02190]; UNMdP-Universidad Nacional de Mar del Plata, Argentina [EXA 515/10]; CONICET FX We are grateful to Emiliano Pisani for providing us with phytoplankton, Nicolas Chiaradia for helping us with photographs, and the fishermen Mario (el Ruso) and Gabriel for helping us in collecting limpets at Piedras Coloradas. We also thank Enrique Morsan and colleagues at IBMP (Instituto de Biolog a Marina y Pesquera, Almirante Storni) for their hospitality during sampling at San Matias Gulf. Part of the material used for the present study was collected by E.O. during the campaign Mejillon II-2009, on board the Oceanographic R/V Puerto Deseado. We are grateful to two anonymous reviewers for valuable suggestions on the manuscript. The present work was partially supported by PIP 2008 112-384 200-801-02190 (CONICET-Consejo Nacional de Investigaciones Cientificas y Tecnicas de Argentina) and EXA 515/10 (UNMdP-Universidad Nacional de Mar del Plata, Argentina). E.O. received scholarship support from CONICET. The present results are part of the PhD dissertation of E.O. This is a contribution of the Smithsonian Marine Station at Fort Pierce, Smithsonian Institution. NR 47 TC 3 Z9 3 U1 0 U2 9 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 EI 1432-1793 J9 MAR BIOL JI Mar. Biol. PD SEP PY 2014 VL 161 IS 9 BP 2107 EP 2120 DI 10.1007/s00227-014-2490-y PG 14 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AN8QT UT WOS:000340869600012 ER PT J AU Assefa, Z Pleurdeau, D Duquesnoy, F Hovers, E Pearson, O Asrat, A Lam, YM AF Assefa, Zelalem Pleurdeau, David Duquesnoy, Frederique Hovers, Erella Pearson, Osbjorn Asrat, Asfawossen Lam, Yin Man CA Constantinos T Tsion TI Survey and explorations of caves in southeastern Ethiopia: Middle Stone Age and Later Stone Age archaeology and Holocene rock art SO QUATERNARY INTERNATIONAL LA English DT Article ID PORC-EPIC CAVE; EAST-AFRICA; SPELEOTHEM PALEOCLIMATE; FOOD-PRODUCTION; DIRE-DAWA; SOUTH; STALAGMITE; EVOLUTION; BEHAVIOR; MECHARA AB The horn of Africa provides the setting for the evolution of early modern humans and their dispersal out of Africa as well as for the entry, many thousands of years later, of pastoralists who brought Near Eastern and, later, South Asian livestock into Africa. However, significant gaps remain in our understanding of the late Upper Pleistocene archaeological record of the horn of Africa, mainly due to the paucity of well-stratified sites from the period. The discovery in southeastern Ethiopia of a number of caves with rich Upper Pleistocene and Holocene archaeological deposits, many of which also had rock art depicting domestic animals, offers an unprecedented opportunity for exploring the later prehistory of the region. In 2007, 2008 our survey documented twenty-one cave sites and shelters with evidence of cultural deposits, including Middle Stone Age (MSA) and Later Stone Age (LSA) stone artifacts, faunal remains, and rock art. Active and fossil speleothems, important for paleoclimatic reconstructions and chronology, were found from two other caves in eastern and western Harerghe. Test excavations were conducted at three sites, with abundant archaeological material documented from stratified deposits at two of these sites - Gilbo Tate and Goda Buticha. The latter is a subject of another paper in this volume. Rock art was recorded at eighteen sites, three of which (in western Harerghe) had not previously been documented. At many of the sites, much of the art is faded and in a vulnerable state, and continued efforts to document and conserve this art are urgently needed. (C) 2013 Elsevier Ltd and INQUA. All rights reserved. C1 [Assefa, Zelalem] Natl Museum Nat Hist, Smithsonian Inst, Archaeobiol Program, Dept Anthropol, Washington, DC 20560 USA. [Assefa, Zelalem] Natl Museum Nat Hist, Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. [Pleurdeau, David] CNRS, Museum Natl Hist Naturelle, Dept Prehist UMR 7194, F-75700 Paris, France. [Duquesnoy, Frederique] Univ Aix Marseille 1, F-13331 Marseille 3, France. [Hovers, Erella] Hebrew Univ Jerusalem, Inst Archaeol, Jerusalem, Israel. [Pearson, Osbjorn] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. [Asrat, Asfawossen] Univ Addis Ababa, Dept Earth Sci, Addis Ababa, Ethiopia. [Constantinos T Tsion] Natl Musuem Ethnol, Addis Ababa, Ethiopia. [Lam, Yin Man] Univ Victoria, Dept Anthropol, Victoria, BC V8W 2Y2, Canada. RP Assefa, Z (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Archaeobiol Program, Dept Anthropol, 1000 Constitution Ave, Washington, DC 20560 USA. EM zassefa@gmail.com; dpleurd@mnhn.fr; frederique.duquesnoy@netcourrier.com; hovers@mscc.huji.ac.il; ompear@unm.edu; asrata@geol.aau.edu.et; ymlam@uvic.ca FU National Geographic Society [8110-06, 8510-08] FX We thank the Authority for Research and Conservation of Cultural Heritages (ARCCH) for permission to explore the study area. This research was supported by grants from the National Geographic Society (grants # 8110-06 and #8510-08). Fieldwork on this project was greatly aided by the efforts of Tilahun G/Selassie, Workalemahu Bekele, Hadis, Haptewold H/Michael, and many others. We would like to thank the French Center for Ethiopian Studies for providing technical support for the missions and funding a part of the laboratory work. We thank zonal and local Tourism and Culture Offices of the Eastern Harerghe, Western Harerghe, the Dire Dawa Administration, and Harari National Regional State for fieldwork administrative support and information on many sites. NR 60 TC 5 Z9 5 U1 1 U2 12 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 EI 1873-4553 J9 QUATERN INT JI Quat. Int. PD SEP 1 PY 2014 VL 343 BP 136 EP 147 DI 10.1016/j.quaint.2013.07.132 PG 12 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AN9ET UT WOS:000340909600011 ER PT J AU Jaafar, Z Dexiang, C AF Jaafar, Z. Dexiang, C. TI Goby and shrimp associations: more than meets the eye SO CORAL REEFS LA English DT Editorial Material C1 [Jaafar, Z.] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Dexiang, C.] Natl Pk Board, Singapore 259569, Singapore. RP Jaafar, Z (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20004 USA. EM jaafarz@si.edu NR 3 TC 2 Z9 2 U1 2 U2 8 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 EI 1432-0975 J9 CORAL REEFS JI Coral Reefs PD SEP PY 2014 VL 33 IS 3 BP 863 EP 863 DI 10.1007/s00338-014-1143-4 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA AN2DZ UT WOS:000340395300029 ER PT J AU Pinto-Sanchez, NR Crawford, AJ Wiens, JJ AF Rocio Pinto-Sanchez, Nelsy Crawford, Andrew J. Wiens, John J. TI Using historical biogeography to test for community saturation SO ECOLOGY LETTERS LA English DT Article DE Amphibians; biogeography; community assembly; dispersal; Great American Biotic Interchange; local richness; phylogeny; saturation; Terrarana ID AMERICAN BIOTIC INTERCHANGE; SPECIES RICHNESS; RANGE SHIFTS; DIVERSITY; FROGS; DIVERSIFICATION; EVOLUTION; NICHE; TIME; ELEUTHERODACTYLUS AB Saturation is the idea that a community is effectively filled with species, such that no more can be added without extinctions. This concept has important implications for many areas of ecology, such as species richness, community assembly, invasive species and climate change. Here, we illustrate how biogeography can be used to test for community saturation, when combined with data on local species richness, phylogeny and climate. We focus on a clade of frogs (Terrarana) and the impact of the Great American Biotic Interchange on patterns of local richness in Lower Middle America and adjacent regions. We analyse data on species richness at 83 sites and a time-calibrated phylogeny for 363 species. We find no evidence for saturation, and show instead that biotic interchange dramatically increased local richness in the region. We suggest that historical biogeography offers thousands of similar long-term natural experiments that can be used to test for saturation. C1 [Rocio Pinto-Sanchez, Nelsy; Crawford, Andrew J.] Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia. [Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Crawford, Andrew J.] Circulo Herpetol Panama, Panama City, Panama. [Wiens, John J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. RP Wiens, JJ (reprint author), Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. EM wiensj@email.arizona.edu OI Crawford, Andrew J./0000-0003-3153-6898; Wiens, John/0000-0003-4243-1127; Pinto-Sanchez, Nelsy Rocio/0000-0001-7561-2982 NR 50 TC 12 Z9 12 U1 15 U2 69 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 SEP PY 2014 VL 17 IS 9 BP 1077 EP 1085 DI 10.1111/ele.12310 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AN2HW UT WOS:000340406200003 PM 24920382 ER PT J AU Jansen, PA Visser, MD Wright, SJ Rutten, G Muller-Landau, HC AF Jansen, Patrick A. Visser, Marco D. Wright, S. Joseph Rutten, Gemma Muller-Landau, Helene C. TI Negative density dependence of seed dispersal and seedling recruitment in a Neotropical palm SO ECOLOGY LETTERS LA English DT Article DE Clumping; competition for dispersers; escape; intraspecific competition; Janzen-Connell; population regulation; recruitment limitation; seed limitation; species coexistence; tropical forest ID SCATTER-HOARDING RODENT; TROPICAL TREE; SPATIAL-PATTERNS; PLANT DIVERSITY; FOREST; COMPETITION; REMOVAL; CONSEQUENCES; MECHANISMS; HERBIVORES AB Negative density dependence (NDD) of recruitment is pervasive in tropical tree species. We tested the hypotheses that seed dispersal is NDD, due to intraspecific competition for dispersers, and that this contributes to NDD of recruitment. We compared dispersal in the palm Attalea butyracea across a wide range of population density on Barro Colorado Island in Panama and assessed its consequences for seed distributions. We found that frugivore visitation, seed removal and dispersal distance all declined with population density of A. butyracea, demonstrating NDD of seed dispersal due to competition for dispersers. Furthermore, as population density increased, the distances of seeds from the nearest adult decreased, conspecific seed crowding increased and seedling recruitment success decreased, all patterns expected under poorer dispersal. Unexpectedly, however, our analyses showed that NDD of dispersal did not contribute substantially to these changes in the quality of the seed distribution; patterns with population density were dominated by effects due solely to increasing adult and seed density. C1 [Jansen, Patrick A.; Visser, Marco D.; Wright, S. Joseph; Rutten, Gemma; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Jansen, Patrick A.; Visser, Marco D.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Jansen, Patrick A.; Rutten, Gemma] Univ Groningen, Community & Conservat Ecol Grp, NL-9700 CC Groningen, Netherlands. [Visser, Marco D.] Radboud Univ Nijmegen, Dept Expt Plant Ecol, NL-6500 GL Nijmegen, Netherlands. [Rutten, Gemma] Univ Bern, Inst Plant Sci, CH-3013 Bern, Switzerland. RP Jansen, PA (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Ancon, Panama. EM patrick.jansen@wur.nl RI Wright, Stuart/M-3311-2013; Jansen, Patrick/G-2545-2015 OI Wright, Stuart/0000-0003-4260-5676; Jansen, Patrick/0000-0002-4660-0314 NR 53 TC 18 Z9 21 U1 9 U2 108 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 SEP PY 2014 VL 17 IS 9 BP 1111 EP 1120 DI 10.1111/ele.12317 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AN2HW UT WOS:000340406200007 PM 25039608 ER PT J AU Lasky, JR Uriarte, M Boukili, VK Erickson, DL Kress, WJ Chazdon, RL AF Lasky, Jesse R. Uriarte, Maria Boukili, Vanessa K. Erickson, David L. Kress, W. John Chazdon, Robin L. TI The relationship between tree biodiversity and biomass dynamics changes with tropical forest succession SO ECOLOGY LETTERS LA English DT Article DE Disturbance; functional traits; leaf dry matter content; productivity; specific leaf area; tropical rainforest; wood specific gravity ID NORTHEASTERN COSTA-RICA; SPECIES RICHNESS; FUNCTIONAL DIVERSITY; PHYLOGENETIC DIVERSITY; ECONOMICS SPECTRUM; ECOSYSTEM-FUNCTION; PLANT DIVERSITY; CARBON STOCKS; PRODUCTIVITY; DISTURBANCE AB Theory predicts shifts in the magnitude and direction of biodiversity effects on ecosystem function (BEF) over succession, but this theory remains largely untested. We studied the relationship between aboveground tree biomass dynamics (biomass) and multiple dimensions of biodiversity over 8-16years in eight successional rainforests. We tested whether successional changes in diversity-biomass correlations reflect predictions of niche theories. Diversity-biomass correlations were positive early but weak later in succession, suggesting saturation of niche space with increasing diversity. Early in succession, phylogenetic diversity and functional diversity in two leaf traits exhibited the strongest positive correlations with biomass, indicating complementarity or positive selection effects. In mid-successional stands, high biodiversity was associated with greater mortality-driven biomass loss, i.e. negative selection effects, suggesting successional niche trade-offs and loss of fast-growing pioneer species. Our results demonstrate that BEF relationships are dynamic across succession, thus successional context is essential to understanding BEF in a given system. C1 [Lasky, Jesse R.] Columbia Univ, Earth Inst, New York, NY 10027 USA. [Lasky, Jesse R.; Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY USA. [Boukili, Vanessa K.; Chazdon, Robin L.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT USA. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Lasky, JR (reprint author), Columbia Univ, Earth Inst, New York, NY 10027 USA. EM jl3985@columbia.edu OI Chazdon, Robin/0000-0002-7349-5687 NR 49 TC 37 Z9 37 U1 10 U2 147 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 SEP PY 2014 VL 17 IS 9 BP 1158 EP 1167 DI 10.1111/ele.12322 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AN2HW UT WOS:000340406200012 PM 24986005 ER PT J AU Rick, TC Reeder-Myers, LA Cox, CJ Sperling, ST Jansen, A Hines, AH AF Rick, Torben C. Reeder-Myers, Leslie A. Cox, C. Jane Sperling, Stephanie T. Jansen, Alex Hines, Anson H. TI Shell Middens, Cultural Chronologies, and Coastal Settlement on the Rhode River Sub-Estuary of Chesapeake Bay, Maryland, USA SO GEOARCHAEOLOGY-AN INTERNATIONAL JOURNAL LA English DT Article ID RADIOCARBON AGE CALIBRATION; DELTA-R VALUES; MIDDLE ATLANTIC; SOUTH-AFRICA; RESERVOIR CORRECTIONS; ACCUMULATION RATES; MARINE RESOURCES; ARCHAIC PERIOD; NORTH-AMERICA; BIG SITES AB North America's Atlantic Coast has been a focus of human settlement and subsistence for millennia, but sea-level rise, sedimentation, and other processes pose significant challenges for archaeological research. Radiocarbon dating of 31 shell middens near the Rhode River Estuary, Maryland provides an opportunity to evaluate human land use, settlement, and cultural chronologies on the Chesapeake Bay. Sixty calibrated radiocarbon dates on eastern oyster (Crassostrea virginica) shell and charcoal demonstrate that Native Americans, colonial, and historic peoples harvested oysters and other shellfish from at least 3200 years ago through the 19th century. The number of dated sites increases during the Late Woodland period after about 1000 cal yr B.P., a factor probably related to greater site visibility and preservation, as well as increased human exploitation of the watershed. Accumulation rates for five of the shell middens provide preliminary indications that some of the sites accumulated rapidly suggesting, along with other evidence, that many of the region's shell middens were logistical or perhaps seasonal camps. Our study demonstrates the importance of regional watershed surveys and radiocarbon dating programs to help build and refine cultural chronologies in coastal regions threatened by sea-level rise and other processes. (C) 2014 Wiley Periodicals, Inc. C1 [Rick, Torben C.; Reeder-Myers, Leslie A.; Jansen, Alex] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Cox, C. Jane; Sperling, Stephanie T.] Anne Arundel Cty Off Planning & Zoning, Cultural Resources Div, Annapolis, MD USA. [Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. EM rickt@si.edu FU National Geographic Society Committee for Research and Exploration [8960-11]; National Museum of Natural History, Smithsonian Institution; Maryland Historical Trust FX This research was supported by a grant from the National Geographic Society Committee for Research and Exploration (#8960-11) and a small grant from the National Museum of Natural History, Smithsonian Institution. Previous work at SERC by the Lost Towns Project was supported by the Maryland Historical Trust. We thank Midge Kramer, Rob Aguilar, Matt Ogburn, and other researchers at the SERC Crab Lab for help with accessing sites. Edgar Alarcon, Sarah Dickey, Elaine Hall, Courtney Hofman, Sean McCanty, and Dan Weller helped in the field and lab. We thank two anonymous reviewers, Loren Davis, and Jamie Woodward for comments on an earlier version of this manuscript. NR 76 TC 6 Z9 6 U1 0 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0883-6353 EI 1520-6548 J9 GEOARCHAEOLOGY JI Geoarchaeology PD SEP-OCT PY 2014 VL 29 IS 5 BP 371 EP 388 DI 10.1002/gea.21484 PG 18 WC Archaeology; Geosciences, Multidisciplinary SC Archaeology; Geology GA AN2NN UT WOS:000340422600002 ER PT J AU Yasuhara, M Okahashi, H Cronin, TM Rasmussen, TL Hunt, G AF Yasuhara, Moriaki Okahashi, Hisayo Cronin, Thomas M. Rasmussen, Tine L. Hunt, Gene TI Response of deep-sea biodiversity to abrupt deglacial and Holocene climate changes in the North Atlantic Ocean SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Abrupt climate change; decadal-centennial time-scales; deep sea; deepwater circulation; Foraminifera; macroecology; Ostracoda; palaeoecology; species diversity; temperature ID HIGH-RESOLUTION RECORD; SPECIES-DIVERSITY; BENTHIC FORAMINIFERA; ARCTIC-OCEAN; LAST DEGLACIATION; VARIABILITY; SCALE; PATTERNS; GRADIENT; PLEISTOCENE AB Aim Little is known about how marine biodiversity responds to oceanographic and climatic changes over the decadal to centennial time-scales which are most relevant for predicted climate changes due to greenhouse gas forcing. This paper aims to reveal decadal-centennial scale deep-sea biodiversity dynamics for the last 20,000 years and then explore potential environmental drivers. Location The North Atlantic Ocean. Methods We investigated deep-sea benthic microfossil records to reveal biodiversity dynamics and subsequently applied comprehensive ecological modelling to test possible environmental factors (i.e. surface productivity, seasonality of productivity or deepwater circulation related to bottom-water temperature) that may have influenced deep-sea biodiversity over these time-scales. Results Deep-sea biodiversity changed synchronously with stadial-interstadial climate changes over the last 20,000 years across a large area of the North Atlantic in both ostracod crustaceans and foraminiferan protozoa (in spite of their different dispersal abilities). Species diversity rapidly increased during abrupt stadial events during the last deglacial and the Holocene interglacial periods. These include the well-known Heinrich 1, the Younger Dryas and the 8.2 ka events when the strength of Atlantic Meridional Overturning Circulation (AMOC) decreased. There is also evidence for quasi-cyclic changes in biodiversity at a c. 1500-year periodicity, consistent with the well-known '1500-year climatic cycle'. Statistical analyses revealed that AMOC variability (probably specifically the variability in AMOC-driven bottom-water temperature) is correlated with deep-sea biodiversity. Main conclusions Our finding of a significant AMOC-diversity relationship may indicate pervasive control of the diversity of deep-sea benthic species by rapidly changing climate, specifically bottom-water temperature, over decadal to centennial time-scales. Our results, based on highly resolved fossil records, may portend pervasive, synchronous and sudden ecosystem responses to human-induced changes to climate and ocean circulation in this century. C1 [Yasuhara, Moriaki; Okahashi, Hisayo] Univ Hong Kong, Sch Biol Sci, Swire Inst Marine Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki; Okahashi, Hisayo] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. [Cronin, Thomas M.] US Geol Survey, Reston, VA 20192 USA. [Rasmussen, Tine L.] Univ Tromso, Dept Geol, N-9037 Tromso, Norway. [Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Yasuhara, M (reprint author), Univ Hong Kong, Sch Biol Sci, Kadoorie Biol Sci Bldg,Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. EM moriakiyasuhara@gmail.com RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 FU Smithsonian Postdoctoral Fellowship; Smithsonian Marine Science Network Postdoctoral Fellowship; Japan Society for the Promotion of Science FX We thank D. W. Oppo for providing core samples, radiocarbon dates and isotope data; J. Dyszynski for sample processing; and D. J. Currie, M. Rex and three anonymous referees for helpful comments and constructive criticisms. This work was supported by a Smithsonian Postdoctoral Fellowship, a Smithsonian Marine Science Network Postdoctoral Fellowship and the Japan Society for the Promotion of Science Postdoctoral Fellowships for Research Abroad (to M.Y.). NR 56 TC 7 Z9 8 U1 3 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X EI 1466-8238 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD SEP PY 2014 VL 23 IS 9 BP 957 EP 967 DI 10.1111/geb.12178 PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA AN2OU UT WOS:000340426000001 ER PT J AU Jaafar, Z Loh, TL AF Jaafar, Zeehan Loh, Tse-Lynn TI Linking land, air and sea: potential impacts of biomass burning and the resultant haze on marine ecosystems of Southeast Asia SO GLOBAL CHANGE BIOLOGY LA English DT Article ID OCEAN WATER-QUALITY; PEAT SWAMP FORESTS; MAJOR OIL-SPILL; SLASH-AND-BURN; REEF CORALS; SMOKE-HAZE; STYLOPHORA-PISTILLATA; NUTRIENT ENRICHMENT; FIRES; INDONESIA C1 [Jaafar, Zeehan] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Loh, Tse-Lynn] John G Shedd Aquarium, Daniel P Haerther Ctr Conservat & Res, Chicago, IL 60613 USA. RP Jaafar, Z (reprint author), Smithsonian Inst, Natl Museum Nat Hist, 10th & Constitut Ave NW, Washington, DC 20560 USA. EM jaafarz@si.edu RI Xiongfei, Zhao/G-7690-2015; OI Loh, Tse-Lynn/0000-0003-1360-1991 NR 97 TC 6 Z9 6 U1 4 U2 52 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 SEP PY 2014 VL 20 IS 9 BP 2701 EP 2707 DI 10.1111/gcb.12539 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AN0PU UT WOS:000340287300002 PM 24604729 ER PT J AU Slot, M Rey-Sanchez, C Gerber, S Lichstein, JW Winter, K Kitajima, K AF Slot, Martijn Rey-Sanchez, Camilo Gerber, Stefan Lichstein, Jeremy W. Winter, Klaus Kitajima, Kaoru TI Thermal acclimation of leaf respiration of tropical trees and lianas: response to experimental canopy warming, and consequences for tropical forest carbon balance SO GLOBAL CHANGE BIOLOGY LA English DT Article DE carbon flux; climate change; DGVM; experimental leaf warming; global warming; NPP; Panama; respiration; tropical forest ID PLANT RESPIRATION; CLIMATE-CHANGE; DARK RESPIRATION; TEMPERATURE SENSITIVITY; GROWTH TEMPERATURE; FOLIAR RESPIRATION; POPULUS-DELTOIDES; PINUS-BANKSIANA; PIONEER TREE; PHOTOSYNTHESIS AB Climate warming is expected to increase respiration rates of tropical forest trees and lianas, which may negatively affect the carbon balance of tropical forests. Thermal acclimation could mitigate the expected respiration increase, but the thermal acclimation potential of tropical forests remains largely unknown. In a tropical forest in Panama, we experimentally increased nighttime temperatures of upper canopy leaves of three tree and two liana species by on average 3 degrees C for 1 week, and quantified temperature responses of leaf dark respiration. Respiration at 25 degrees C (R-25) decreased with increasing leaf temperature, but acclimation did not result in perfect homeostasis of respiration across temperatures. In contrast, Q(10) of treatment and control leaves exhibited similarly high values (range 2.5-3.0) without evidence of acclimation. The decrease in R-25 was not caused by respiratory substrate depletion, as warming did not reduce leaf carbohydrate concentration. To evaluate the wider implications of our experimental results, we simulated the carbon cycle of tropical latitudes (24 degrees S-24 degrees N) from 2000 to 2100 using a dynamic global vegetation model (LM3VN) modified to account for acclimation. Acclimation reduced the degree to which respiration increases with climate warming in the model relative to a no-acclimation scenario, leading to 21% greater increase in net primary productivity and 18% greater increase in biomass carbon storage over the 21st century. We conclude that leaf respiration of tropical forest plants can acclimate to nighttime warming, thereby reducing the magnitude of the positive feedback between climate change and the carbon cycle. C1 [Slot, Martijn; Lichstein, Jeremy W.; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Rey-Sanchez, Camilo; Winter, Klaus; Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa 084303092, Panama. [Rey-Sanchez, Camilo] Univ Rosario, Fac Ciencias Nat & Math, Bogota, Colombia. [Gerber, Stefan] Univ Florida, Soil & Water Sci Dept, Gainesville, FL 32611 USA. RP Slot, M (reprint author), Smithsonian Trop Res Inst, Balboa 084303092, Panama. EM martijnslot78@gmail.com FU NSF-IOS [1051789] FX We thank Edwin Andrade and Julio Piti for operating the canopy crane, Phil Nguyen for assistance with data collection, Grace Crummer for assistance with the elemental analyzer, and three anonymous reviewers for thoughtful comments on an earlier version of this paper. Financial support came from NSF-IOS grant 1051789. NR 69 TC 23 Z9 24 U1 16 U2 99 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 SEP PY 2014 VL 20 IS 9 BP 2915 EP 2926 DI 10.1111/gcb.12563 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AN0PU UT WOS:000340287300019 PM 24604769 ER PT J AU Uribe, MC De la Rosa-Cruz, G Grier, HJ AF Carmen Uribe, Mari De la Rosa-Cruz, Gabino Grier, Harry J. TI Proliferation of Oogonia and Folliculogenesis in the Viviparous Teleost Ilyodon whitei (Goodeidae) SO JOURNAL OF MORPHOLOGY LA English DT Article DE oogenesis; viviparity; previtellogenesis; cell nests; germinal epithelium ID SYNBRANCHUS-MARMORATUS BLOCH; OVARIAN GERMINAL EPITHELIUM; REPRODUCTIVE-CYCLE; NEOTOCA BILINEATA; HETERANDRIA FORMOSA; OOCYTE DEVELOPMENT; SWAMP EEL; FISHES; GROWTH; MEMBER AB Oogonial proliferation in fishes is an essential reproductive strategy to generate new ovarian follicles and is the basis for unlimited oogenesis. The reproductive cycle in viviparous teleosts, besides oogenesis, involves development of embryos inside the ovary, that is, intraovarian gestation. Oogonia are located in the germinal epithelium of the ovary. The germinal epithelium is the surface of ovarian lamellae and, therefore, borders the ovarian lumen. However, activity and seasonality of the germinal epithelium have not been described in any viviparous teleost species regarding oogonial proliferation and folliculogenesis. The goal of this study is to identify the histological features of oogonial proliferation and folliculogenesis during the reproductive cycle of the viviparous goodeid Ilyodon whitei. Ovaries during nongestation and early and late gestation were analyzed. Oogonial proliferation and folliculogenesis in I. whitei, where intraovarian gestation follows the maturation and fertilization of oocytes, do not correspond to the late oogenesis, as was observed in oviparous species, but correspond to late gestation. This observation offers an example of ovarian physiology correlated with viviparous reproduction and provides elements for understanding the regulation of the initiation of processes that ultimately result in the origin of the next generation. These processes include oogonia proliferation and development of the next batch of germ cells into the complex process of intraovarian gestation. J. Morphol. 275:1004-1015, 2014. (c) 2014 Wiley Periodicals, Inc. C1 [Carmen Uribe, Mari; De la Rosa-Cruz, Gabino] Univ Nacl Autonoma Mexico, Lab Biol Reprod Anim, Dept Biol Comparada, Fac Ciencias, Mexico City 04510, DF, Mexico. [Grier, Harry J.] Florida Fish & Wildlife Res Inst, St Petersburg, FL 33701 USA. [Grier, Harry J.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Uribe, MC (reprint author), Univ Nacl Autonoma Mexico, Lab Biol Reprod Anim, Dept Biol Comparada, Fac Ciencias, Ciudad Univ, Mexico City 04510, DF, Mexico. EM mari3uribe3@gmail.com NR 37 TC 4 Z9 4 U1 3 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0362-2525 EI 1097-4687 J9 J MORPHOL JI J. Morphol. PD SEP PY 2014 VL 275 IS 9 BP 1004 EP 1015 DI 10.1002/jmor.20277 PG 12 WC Anatomy & Morphology SC Anatomy & Morphology GA AN0SQ UT WOS:000340294700004 PM 24796532 ER PT J AU Pacucci, F Mesinger, A Mineo, S Ferrara, A AF Pacucci, Fabio Mesinger, Andrei Mineo, Stefano Ferrara, Andrea TI The X-ray spectra of the first galaxies: 21 cm signatures SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: high-redshift; cosmology: theory; X-rays: binaries; X-rays: diffuse background; X-rays: galaxies; X-rays: ISM ID STAR-FORMING GALAXIES; FORMATION RATE INDICATOR; EARLY UNIVERSE; INTERSTELLAR-MEDIUM; RADIATIVE-TRANSFER; INFRARED GALAXIES; LYMAN-WERNER; DARK-MATTER; REIONIZATION; EMISSION AB The cosmological 21 cm signal is a physics-rich probe of the early Universe, encoding information about both the ionization and the thermal history of the intergalactic medium (IGM). The latter is likely governed by X-rays from star formation processes inside very high redshift (z a parts per thousand(3) 15) galaxies. Due to the strong dependence of the mean free path on the photon energy, the X-ray spectral energy distribution (SED) can have a significant impact on the interferometric signal from the cosmic dawn. Recent Chandra observations of nearby, star-forming galaxies show that their SEDs are more complicated than is usually assumed in 21 cm studies. In particular, these galaxies have ubiquitous, sub-keV thermal emission from the hot interstellar medium (ISM), which generally dominates the soft X-ray luminosity (with energies a parts per thousand(2)1 keV, sufficiently low to significantly interact with the IGM). Using illustrative soft and hard SEDs, we show that the IGM temperature fluctuations in the early Universe would be substantially increased if the X-ray spectra of the first galaxies were dominated by the hot ISM, compared with X-ray binaries with harder spectra. The associated large-scale power of the 21 cm signal would be higher by a factor of similar to 3. More generally, we show that the peak in the redshift evolution of the large-scale (k similar to 0.2 Mpc(-1)) 21 cm power is a robust probe of the soft-band SED of the first galaxies, and importantly, is not degenerate with their bolometric luminosities. On the other hand, the redshift of the peak constrains the X-ray luminosity and halo masses which host the first galaxies. C1 [Pacucci, Fabio; Mesinger, Andrei; Ferrara, Andrea] Scuola Normale Super Pisa, I-56126 Pisa, Italy. [Mineo, Stefano] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ferrara, Andrea] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. RP Pacucci, F (reprint author), Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy. EM fabio.pacucci@sns.it FU NASA's Astrophysics Data Analysis Program (ADAP) grant [NNH13CH56C] FX We thank Bret Lehmer for stimulating conversations which contributed to motivating this work. SM acknowledges support from the NASA's Astrophysics Data Analysis Program (ADAP) grant NNH13CH56C. NR 72 TC 34 Z9 34 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 SEP 1 PY 2014 VL 443 IS 1 BP 678 EP 686 DI 10.1093/mnras/stu1240 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5UR UT WOS:000339927000053 ER PT J AU Morlok, A Mason, AB Anand, M Lisse, CM Bullock, ES Grady, MM AF Morlok, Andreas Mason, Andrew B. Anand, Mahesh Lisse, Carey M. Bullock, Emma S. Grady, Monica M. TI Dust from collisions: A way to probe the composition of exo-planets? SO ICARUS LA English DT Article DE Debris disks; Extra-solar planets; Infrared observations; Earth; Mars; Planetary Formation ID INFRARED-ABSORPTION-SPECTRA; INTERSTELLAR SILICATE MINERALOGY; MIDINFRARED TRANSMISSION SPECTRA; EXTRASOLAR MINOR PLANET; SUN-LIKE STARS; BETA-PICTORIS; GIANT IMPACT; WHITE-DWARFS; DEBRIS-DISK; CRYSTALLINE SILICATES AB In order to link infrared observations of dust formed during planet formation in debris disks to mid-infrared spectroscopic data of planetary materials from differentiated terrestrial and asteroidal bodies, we obtained absorption spectra of a representative suite of terrestrial crustal and mantle materials, and of typical martian meteorites. A series of debris disk spectra characterized by a strong feature in the 9.0-9.5 mu m range (HD23514, HD15407a, HD172555 and HD165014), is comparable to materials that underwent shock, collision or high temperature events. These are amorphous materials such as tektites, SiO2-glass, obsidian, and highly shocked shergottites as well as inclusions from mesosiderites (group A). A second group (BD+20307, Beta Pictoris, HD145263, ID8, HD113766, HD69830, P1121, and Eta Corvi) have strong pyroxene and olivine bands in the 9-12 mu m range and is very similar to ultramafic rocks (e.g. harzburgite, dunite) (group B). This could indicate the occurrence of differentiated materials similar to those in our Solar System in these other systems. However, mixing of projectile and target material, as well as that of crustal and mantle material has to be taken into account in large scale events like hit-and-run and giant collisions or even large-scale planetary impacts. This could explain the olivine-dominated dust of group B. The crustal-type material of group A would possibly require the stripping of upper layers by grazing-style hit-and run encounters or high energy events like evaporation/condensation in giant collisions. In tidal disruptions or the involvement of predominantly icy/water bodies the resulting mineral dust would originate mainly in one of the involved planetesimals. This could allow attributing the observed composition to a specific body (such as e.g. Eta Corvi). (C) 2014 Elsevier Inc. All rights reserved. C1 [Morlok, Andreas; Anand, Mahesh] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [Morlok, Andreas; Anand, Mahesh] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Mason, Andrew B.] Univ Turku, Tuorla Observ, Finnish Ctr Astron ESO FINCA, FI-21500 Piikkio, Finland. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Bullock, Emma S.; Grady, Monica M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Morlok, A (reprint author), Univ Munster, Inst Planetol, Wilhelm Klemm Str, D-48149 Munster, Germany. EM morlokan@uni-muenster.de; andmas@utu.fi; m.anand@open.ac.uk; carey.lisse@jhuapl.edu; bullocke@si.edu; m.m.grady@open.ac.uk RI Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Grady, Monica/0000-0002-4055-533X FU UK PPARC (STFC); Jet Propulsion Laboratory, California Institute of Technology, under NASA [1407] FX A.M. and MMG were funded for part of the research by the UK PPARC (STFC).; This work is partially 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. NR 108 TC 4 Z9 4 U1 2 U2 11 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 2014 VL 239 BP 1 EP 14 DI 10.1016/j.icarus.2014.05.024 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM3WE UT WOS:000339782700001 ER PT J AU Rosenfeld, CE McCormack, ML Martinez, CE AF Rosenfeld, Carla E. McCormack, M. Luke Martinez, Carmen E. TI A novel approach to study composition of in situ produced root-derived dissolved organic matter SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Rhizosphere; Exudates; Dissolved organic matter; NMR; Stable isotopes; Pulse-chase ID IONIZATION MASS-SPECTROMETRY; LOLIUM-PERENNE; FOREST SOILS; CARBON; RHIZOSPHERE; ACIDS; RHIZODEPOSITION; RESPIRATION; INTERFACE; PLANTS AB Carbon (C) compounds released from plant roots comprise a significant and reactive fraction of belowground C pools. These root-derived compounds modify rhizosphere soil and play a vital role in the mobility of nutrients and contaminants within ecosystems. Due to their low concentration, fast turnover, and limited spatial distribution throughout the soil, root-derived compounds are difficult to study. This study combined a C-13 pulse-chase technique and 1D and 2D nuclear magnetic resonance (NMR) spectroscopy techniques to analyze root-derived compounds produced in real soil. The pulsed samples displayed distinct enrichment in aliphatic and carbohydrate-type compounds indicating that pulse-chase approaches are a viable technique for isolating root-derived from background DOM. However, multiple NMR techniques may be necessary to develop a full profile of root-derived DOM. This is the first use of combined pulse-chase-NMR methodologies to analyze in situ produced root-derived DOM. Such a combination is applicable to various experimental designs and/or environmental scenarios, and can provide valuable information for future rhizosphere science. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Rosenfeld, Carla E.; McCormack, M. Luke; Martinez, Carmen E.] Penn State Univ, Dept Ecosyst Sci & Management, University Pk, PA 16802 USA. RP Rosenfeld, CE (reprint author), Smithsonian Inst, POB 37012,MRC 119, Washington, DC 20013 USA. EM RosenfeldC@si.edu OI McCormack, Michael Luke/0000-0002-8300-5215 FU PSU Department of Crop and Soil Sciences; NSF GK-12 fellowship [0947962]; College of Agricultural Sciences FX Research was supported by PSU Department of Crop and Soil Sciences, College of Agricultural Sciences, and NSF GK-12 fellowship (NSF Award #: 0947962). We thank L. Kochian for seeds, E. Hatzakis for NMR assistance and T. Adams for helpful suggestions. All NMR work was performed at PSU NMR Spectroscopy Facility. NR 22 TC 0 Z9 2 U1 14 U2 109 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD SEP PY 2014 VL 76 BP 1 EP 4 DI 10.1016/j.soilbio.2014.04.026 PG 4 WC Soil Science SC Agriculture GA AM2QM UT WOS:000339695900001 ER PT J AU Savcheva, AS McKillop, SC McCauley, PI Hanson, EM DeLuca, EE AF Savcheva, A. S. McKillop, S. C. McCauley, P. I. Hanson, E. M. DeLuca, E. E. TI A New Sigmoid Catalog from Hinode and the Solar Dynamics Observatory: Statistical Properties and Evolutionary Histories SO SOLAR PHYSICS LA English DT Article DE Flares, dynamics; Magnetic fields, corona ID CORONAL MASS EJECTIONS; FLUX ROPE; ACTIVE-REGION; YOHKOH SXT; CHIRALITY; FILAMENT; HELICITY; ERUPTION; FLARES AB We present a new sigmoid catalog covering the duration of the Hinode mission and the Solar Dynamics Observatory (SDO) until the end of 2012. The catalog consists of 72 mostly long-lasting sigmoids. We collect and make available all X-ray and EUV data from Hinode, SDO, and the Solar TErrestrial RElations Observatory (STEREO), and we determine the sigmoid lifetimes, sizes, and aspect ratios. We also collect the line-of-sight magnetograms from the Helioseismic and Magnetic Imager (HMI) for SDO or the Michelson Doppler Imager (MDI) on the Solar and Heliospheric Observatory (SOHO) to measure flux versus time for the lifetime of each region. We determine that the development of a sigmoidal shape and eruptive activity is more strongly correlated with flux cancelation than with emergence. We find that the eruptive properties of the regions correlate well with the maximum flux, largest change, and net change in flux in the regions. These results have implications for constraining future flux-rope models of ARs and gaining insight into their evolutionary properties. C1 [Savcheva, A. S.; McKillop, S. C.; McCauley, P. I.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hanson, E. M.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Savcheva, AS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asavcheva@cfa.harvard.edu RI McCauley, Patrick/P-7747-2015; DeLuca, Edward/L-7534-2013 OI McCauley, Patrick/0000-0002-1450-7350; DeLuca, Edward/0000-0001-7416-2895 FU Smithsonian Astrophysical Observatory (SAO) - Hinode/XRT [NNM07AB07C]; Smithsonian Astrophysical Observatory (SAO) - SDO/AIA [SP02H1701R]; NASA; NSF [ATM-0851866]; Science & Technology Facility Council; Deutsches Zentrum fur Luftund Raumfahrt e.V. (DLR); Belgian Science Policy Office; Centre National d'Etudes Spatiales (CNES); Centre National de la Recherche Scientifique (CNRS); USAF Space Test Program; Office of Naval Research FX Support for this work was provided by the Smithsonian Astrophysical Observatory (SAO) via funding from Hinode/XRT through grant NNM07AB07C and SDO/AIA through grant SP02H1701R. AS is supported by a NASA Jack Eddy postdoctoral fellowship. EH is supported by the NSF Research Experience for Undergraduates (REU) grant ATM-0851866 to SAO. We thank D. Mackay and K. Meyer for providing us with a magnetogram noise-reduction method.; 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). SDO is a NASA satellite, and the AIA instrument team is led by Lockheed Martin, with SAO as the major subcontractor. The SDO data used here are provided courtesy of NASA/SDO and the AIA and HMI science teams. The STEREO/SECCHI data used here were produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany), Centre Spatiale de Liege (Belgium), Institut d'Optique Theorique et Appliquee (France), and Institut d'Astrophysique Spatiale (France). The USA institutions were funded by NASA, the UK institutions by the Science & Technology Facility Council (which used to be the Particle Physics and Astronomy Research Council, PPARC), the German institutions by Deutsches Zentrum fur Luftund Raumfahrt e.V. (DLR), the Belgian institutions by Belgian Science Policy Office, and the French institutions by Centre National d'Etudes Spatiales (CNES) and the Centre National de la Recherche Scientifique (CNRS). The NRL effort was also supported by the USAF Space Test Program and the Office of Naval Research. This articles uses data from the CACTus CME catalog, generated and maintained by the SIDC at the Royal Observatory of Belgium, and H alpha images from the Kanzelhohe Solar Observatory, operated by the Institute for Geophysics, Astrophysics, and Meteorology (IGAM) of the University of Graz (Austria), and the Global Oscillation Network Group (GONG) program, managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. The data were acquired by instruments operated by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory. NR 33 TC 11 Z9 11 U1 0 U2 1 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 SEP PY 2014 VL 289 IS 9 BP 3297 EP 3311 DI 10.1007/s11207-013-0469-3 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL3AL UT WOS:000338997200004 ER PT J AU Bertini, G Baeza, JA AF Bertini, Giovana Antonio Baeza, J. TI Fecundity and fertility in a freshwater population of the neotropical amphidromous shrimp Macrobrachium acanthurus from the southeastern Atlantic SO INVERTEBRATE REPRODUCTION & DEVELOPMENT LA English DT Article DE freshwater prawn; reproduction; scaling; allometry; exploited species ID REPRODUCTIVE-BIOLOGY; EGG-PRODUCTION; DECAPOD CRUSTACEANS; AMAZONICUM HELLER; CARIDEAN SHRIMPS; CRANGON-CRANGON; LIFE-HISTORY; CARCINUS L.; RIVER PRAWN; BROOD LOSS AB The neotropical amphidromous shrimp Macrobrachium acanthurus is one of various freshwater crustaceans heavily exploited in the southwestern Atlantic. Fecundity (n degrees early embryos female(-1)) was examined during 2007 at four different localities (Iguape, Registro, Sete Barras, and Eldorado) along a stretch of river extending over 85 km (Ribeira de Iguape, Sao Paulo State, Brazil). Also, fertility (n degrees hatched larvae female(-1)) was examined at one locality (Registro) during 2009-2010. Fecundity (mean +/- SD: 5191 +/- 2635; range: 1086-13,014 embryos female(-1)) did not vary throughout the segment of river studied. Fecundity increased with female body size (carapace length, CL). However, fecundity scaled negatively with shrimp body size; females produce disproportionably fewer eggs with a unit increase in CL. The conditions explaining the negative allometric relationship between fecundity and female body size in M. acanthurus remain to be addressed. Nevertheless, natural food constraints limiting the ability of large but not small females to acquire enough resources to produce and fill their gonads with oocytes represents a plausible explanation for the negative scaling of fecundity with body size. Fertility varied between 545 and 12,465 hatched larvae female(-1) with an average (+/- SD) of 3981 (+/- 2693) and increased isometrically with a unit increase in female body size. M. acanthurus has an average fecundity and fertility that represents one of the extremes regarding the trade-off between fecundity/fertility and egg-size reported for caridean shrimps. All of this information needs to be considered in assessing shrimp stocks and establishing a sustainable management plan for this exploited species in the southwestern Atlantic. C1 [Bertini, Giovana] Univ Estadual Paulista, LABCRUST Lab Biol & Cult Crustaceos, UNESP, BR-11900000 Sao Paulo, Brazil. [Bertini, Giovana] NEBECC Crustacean Biol Ecol & Culture Study Grp, Botucatu, SP, Brazil. [Antonio Baeza, J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Univ Catolica Norte, Dept Biol Marina, Fac Ciencias Mar, Larrondo 1281, Coquimbo, Chile. RP Baeza, JA (reprint author), Clemson Univ, Dept Biol Sci, 132 Long Hall, Clemson, SC 29634 USA. EM baeza.antonio@gmail.com RI Bertini, Giovana/O-5323-2015 OI Bertini, Giovana/0000-0003-4489-0351 FU FAPESP (Fundacao de Amparo Pesquisa do Estado de Sao Paulo) [05/56131-0] FX GB thanks the FAPESP (Fundacao de Amparo Pesquisa do Estado de Sao Paulo) for providing financial support (05/56131-0). We also thank students and technicians for their help during field work. Sampling was conducted according to the Sao Paulo state and Brazilian federal laws. J.A.B. is most grateful to Maria Lucia Negreiros-Fransozo, Paula Araujo, Adilson Fransozo, Alexandre Oliveira de Almeida, and the Sociedade Brasileira de Carcinologia that made possible his visit to Brazil during 2010 and this collaboration. We also thank two anonymous reviewers for comments on the manuscript. This is contribution number 946 of the Smithsonian Marine Station at Fort Pierce. NR 92 TC 2 Z9 2 U1 2 U2 28 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0792-4259 EI 2157-0272 J9 INVERTEBR REPROD DEV JI Invertebr. Reprod. Dev. PD SEP PY 2014 VL 58 IS 3 BP 207 EP 217 DI 10.1080/07924259.2014.894948 PG 11 WC Reproductive Biology; Zoology SC Reproductive Biology; Zoology GA AK0LY UT WOS:000338105700007 ER PT J AU Alna'Washi, GA Lu, M Habibi, M Esteves-Macaluso, D Wang, JC Phaneuf, RA Kilcoyne, ALD Cisneros, C McLaughlin, BM AF Alna'Washi, G. A. Lu, M. Habibi, M. Esteves-Macaluso, D. Wang, J. C. Phaneuf, R. A. Kilcoyne, A. L. D. Cisneros, C. McLaughlin, B. M. TI Valence-shell single photoionization of chlorine-like K2+ ions: Experiment and theory SO PHYSICAL REVIEW A LA English DT Article ID ATOMIC CHLORINE; CROSS-SECTIONS; OSCILLATOR-STRENGTHS; RR TELESCOPII; ENERGY-LEVELS; SPECTROSCOPY; SPECTRA; FORBIDDEN; LINES; 3S AB The absolute single-photoionization cross section was measured for Cl-like K2+ over the photon energy range from 44.2 to 69.7 eV at a constant energy resolution of 0.045 eV. The experiments were performed by merging an ion beam with a beam of synchrotron radiation from an undulator. The ground-state ionization threshold was measured at 0.004-eV energy resolution to be 45.717 +/- 0.030 eV. The measurements are rich in resonance structure due to multiple Rydberg series of transitions to autoionizing states. These series are assigned spectroscopically using the quantum defect method, guided by pseudorelativistic Hartree-Fock calculations for the energies and oscillator strengths of transitions to autoionizing states. The experimental results, which include significant contributions from K2+ ions initially in metastable states, are in satisfactory agreement with a linear superposition of semirelativistic R-matrix calculations of photoionization cross sections from these initial states. C1 [Alna'Washi, G. A.; Lu, M.; Habibi, M.; Esteves-Macaluso, D.; Wang, J. C.; Phaneuf, R. A.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. [Kilcoyne, A. L. D.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Cisneros, C.] Univ Nacl Autonoma Mexico, Inst Ciencias Fis, Cuernavaca 62210, Morelos, Mexico. [McLaughlin, B. M.] Inst Theoret Atom & Mol Phys, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Alna'Washi, GA (reprint author), Univ Nevada, Dept Phys, Reno, NV 89557 USA. EM alnawashi@hu.edu.jo RI Kilcoyne, David/I-1465-2013 FU Division of Chemical Sciences, Geosciences, and Biosciences of the US Department of Energy [DE-FG02-03ER15424, DE-AC03-76SF-00098]; PAPIT-UNAM, Mexico [IN107912-IN10261]; US National Science Foundation, under the visitors program; Queen's University Belfast; National Science Foundation [OCI-1053575]; Office of Science, Office of Basic Energy Sciences of the U.S. Department of Energy [DE-AC02-05CH11231] FX The Division of Chemical Sciences, Geosciences, and Biosciences of the US Department of Energy supported this research under Grant No. DE-FG02-03ER15424 and Contract No. DE-AC03-76SF-00098. C.C. acknowledges support from PAPIT-UNAM Grant No. IN107912-IN10261, Mexico. B.M.McL. acknowledges support by the US National Science Foundation, under the visitors program, through a grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics, where this work was completed, and a visiting research fellowship from Queen's University Belfast. The computational work was performed at the National Energy Research Scientific Computing Center in Oakland, California, and on the Kraken XT5 facility at the National Institute for Computational Science (NICS) in Knoxville, Tennessee. The Kraken XT5 facility is a resource of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation Grant No. OCI-1053575. The Advanced Light Source is supported by the Director, Office of Science, Office of Basic Energy Sciences of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 49 TC 0 Z9 1 U1 0 U2 2 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 29 PY 2014 VL 90 IS 2 AR 023417 DI 10.1103/PhysRevA.90.023417 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AO0TV UT WOS:000341026200003 ER PT J AU Raghavan, M DeGiorgio, M Albrechtsen, A Moltke, I Skoglund, P Korneliussen, TS Gronnow, B Appelt, M Gullov, HC Friesen, TM Fitzhugh, W Malmstrom, H Rasmussen, S Olsen, J Melchior, L Fuller, BT Fahrni, SM Stafford, T Grimes, V Renouf, MAP Cybulski, J Lynnerup, N Lahr, MM Britton, K Knecht, R Arneborg, J Metspalu, M Cornejo, OE Malaspinas, AS Wang, Y Rasmussen, M Raghavan, V Hansen, TVO Khusnutdinova, E Pierre, T Dneprovsky, K Andreasen, C Lange, H Hayes, MG Coltrain, J Spitsyn, VA GotherstrOm, A Orlando, L Kivisild, T Villems, R Crawford, MH Nielsen, FC Dissing, J Heinemeier, J Meldgaard, M Bustamante, C O'Rourke, DH Jakobsson, M Gilbert, MTP Nielsen, R Willerslev, E AF Raghavan, Maanasa DeGiorgio, Michael Albrechtsen, Anders Moltke, Ida Skoglund, Pontus Korneliussen, Thorfinn S. Gronnow, Bjarne Appelt, Martin Gullov, Hans Christian Friesen, T. Max Fitzhugh, William Malmstrom, Helena Rasmussen, Simon Olsen, Jesper Melchior, Linea Fuller, Benjamin T. Fahrni, Simon M. Stafford, Thomas, Jr. Grimes, Vaughan Renouf, M. A. Priscilla Cybulski, Jerome Lynnerup, Niels Lahr, Marta Mirazon Britton, Kate Knecht, Rick Arneborg, Jette Metspalu, Mait Cornejo, Omar E. Malaspinas, Anna-Sapfo Wang, Yong Rasmussen, Morten Raghavan, Vibha Hansen, Thomas V. O. Khusnutdinova, Elza Pierre, Tracey Dneprovsky, Kirill Andreasen, Claus Lange, Hans Hayes, M. Geoffrey Coltrain, Joan Spitsyn, Victor A. Gotherstrom, Anders Orlando, Ludovic Kivisild, Toomas Villems, Richard Crawford, Michael H. Nielsen, Finn C. Dissing, Jorgen Heinemeier, Jan Meldgaard, Morten Bustamante, Carlos O'Rourke, Dennis H. Jakobsson, Mattias Gilbert, M. Thomas P. Nielsen, Rasmus Willerslev, Eske TI The genetic prehistory of the New World Arctic SO SCIENCE LA English DT Article ID POPULATION HISTORY; GENOME SEQUENCE; MTDNA VARIATION; GREENLAND; ADMIXTURE; AMERICA; CANADA; ESKIMO; DORSET; DIVERSITY AB The New World Arctic, the last region of the Americas to be populated by humans, has a relatively well-researched archaeology, but an understanding of its genetic history is lacking. We present genome-wide sequence data from ancient and present-day humans from Greenland, Arctic Canada, Alaska, Aleutian Islands, and Siberia. We show that Paleo-Eskimos (similar to 3000 BCE to 1300 CE) represent a migration pulse into the Americas independent of both Native American and Inuit expansions. Furthermore, the genetic continuity characterizing the Paleo-Eskimo period was interrupted by the arrival of a new population, representing the ancestors of present-day Inuit, with evidence of past gene flow between these lineages. Despite periodic abandonment of major Arctic regions, a single Paleo-Eskimo metapopulation likely survived in near-isolation for more than 4000 years, only to vanish around 700 years ago. C1 [Raghavan, Maanasa; Korneliussen, Thorfinn S.; Malmstrom, Helena; Stafford, Thomas, Jr.; Malaspinas, Anna-Sapfo; Rasmussen, Morten; Pierre, Tracey; Orlando, Ludovic; Meldgaard, Morten; Gilbert, M. Thomas P.; Willerslev, Eske] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, DK-1350 Copenhagen, Denmark. [DeGiorgio, Michael] Penn State Univ, Dept Biol, University Pk, PA 16802 USA. [Albrechtsen, Anders; Moltke, Ida] Univ Copenhagen, Dept Biol, Bioinformat Ctr, DK-2200 Copenhagen, Denmark. [Moltke, Ida] Univ Chicago, Dept Human Genet, Chicago, IL 60637 USA. [Skoglund, Pontus; Malmstrom, Helena; Jakobsson, Mattias] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. [Skoglund, Pontus] Harvard Univ, Sch Med, Dept Genet, Boston, MA 02115 USA. [Gronnow, Bjarne; Appelt, Martin; Gullov, Hans Christian] Natl Museum Denmark, Arctic Ctr, Ethnog Collect SILA, DK-1220 Copenhagen, Denmark. [Friesen, T. Max] Univ Toronto, Dept Anthropol, Toronto, ON M5S 2S2, Canada. [Fitzhugh, William] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Arctic Studies Ctr, Washington, DC 20013 USA. [Rasmussen, Simon] Tech Univ Denmark, Dept Syst Biol, Ctr Biol Sequence Anal, DK-2800 Lyngby, Denmark. [Olsen, Jesper; Stafford, Thomas, Jr.; Heinemeier, Jan] Aarhus Univ, Dept Phys & Astron, AMS Dating Ctr 14C, DK-8000 Aarhus C, Denmark. [Melchior, Linea; Lynnerup, Niels; Dissing, Jorgen] Univ Copenhagen, Fac Hlth Sci, Inst Forens Med, Anthropol Lab, DK-2100 Copenhagen, Denmark. [Fuller, Benjamin T.; Fahrni, Simon M.] Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. [Grimes, Vaughan; Renouf, M. A. Priscilla] Mem Univ Newfoundland, Dept Archaeol, Queens Coll, St John, NF A1C 5S7, Canada. [Grimes, Vaughan; Britton, Kate] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. [Cybulski, Jerome] Canadian Museum Hist, Gatineau, PQ K1A 0M8, Canada. [Cybulski, Jerome] Univ Western Ontario, Dept Anthropol, London, ON N6A 5C2, Canada. [Lahr, Marta Mirazon] Univ Cambridge, Dept Archaeol & Anthropol, Leverhulme Ctr Human Evolutionary Studies, Cambridge CB2 1QH, England. [Britton, Kate; Knecht, Rick] Univ Aberdeen, Dept Archaeol, Aberdeen AB24 3UF, Scotland. [Arneborg, Jette] Natl Museum Denmark, DK-1220 Copenhagen, Denmark. [Arneborg, Jette] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland. [Metspalu, Mait; Kivisild, Toomas; Villems, Richard] Estonian Bioctr, Evolutionary Biol Grp, EE-51010 Tartu, Estonia. [Metspalu, Mait; Villems, Richard] Univ Tartu, Dept Evolutionary Biol, EE-51010 Tartu, Estonia. [Cornejo, Omar E.; Bustamante, Carlos] Stanford Univ, Sch Med, Dept Genet, Stanford, CA 94305 USA. [Cornejo, Omar E.] Washington State Univ, Sch Biol Sci, Pullman, WA 99164 USA. [Wang, Yong; Nielsen, Rasmus] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Wang, Yong] Ancestry Com DNA LLC, San Francisco, CA 94107 USA. [Raghavan, Vibha] Ontario Inst Canc Res, Toronto, ON M5G 0A3, Canada. [Hansen, Thomas V. O.; Nielsen, Finn C.] Univ Copenhagen, Rigshosp, Ctr Genom Med, DK-2100 Copenhagen, Denmark. [Khusnutdinova, Elza] Russian Acad Sci, Ufa Sci Ctr, Inst Biochem & Genet, Ufa 450001, Russia. [Khusnutdinova, Elza] Bashkir State Univ, Dept Genet & Fundamental Med, Ufa 450074, Bashkortostan, Russia. [Dneprovsky, Kirill] State Museum Oriental Art, Moscow 119019, Russia. [Andreasen, Claus; Lange, Hans] Greenland Natl Museum & Arch, Nuuk 3900, Greenland. [Hayes, M. Geoffrey] Northwestern Univ, Feinberg Sch Med, Dept Med, Div Endocrinol Metab & Mol Med, Chicago, IL 60611 USA. [Hayes, M. Geoffrey] Northwestern Univ, Weinberg Coll Arts & Sci, Dept Anthropol, Evanston, IL 60208 USA. [Hayes, M. Geoffrey] Northwestern Univ, Feinberg Sch Med, Ctr Genet Med, Chicago, IL 60611 USA. [Coltrain, Joan; O'Rourke, Dennis H.] Univ Utah, Dept Anthropol, Salt Lake City, UT 84112 USA. [Spitsyn, Victor A.] Russian Acad Med Sci, Res Ctr Med Genet, Moscow 115478, Russia. [Gotherstrom, Anders] Stockholm Univ, Dept Archaeol & Class Studies, S-10691 Stockholm, Sweden. [Kivisild, Toomas] Univ Cambridge, Dept Archaeol & Anthropol, Cambridge CB2 1QH, England. [Crawford, Michael H.] Univ Kansas, Lab Biol Anthropol, Lawrence, KS 66045 USA. RP Willerslev, E (reprint author), Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, Oster Voldgade 5-7, DK-1350 Copenhagen, Denmark. EM ewillerslev@snm.ku.dk RI Korneliussen, Thorfinn Sand/F-6421-2014; Gilbert, Marcus/A-8936-2013; Metspalu, Mait/G-8671-2015; Moltke, Ida/C-6158-2011; Rasmussen, Simon/G-6258-2016; Khusnutdinova, Elza/A-4810-2013; Jakobsson, Mattias/A-6116-2011; Albrechtsen, Anders/K-4281-2013; Olsen, Jesper/F-1656-2013; Malmstrom, Helena/C-2476-2017; Spitsyn, Viktor/O-8137-2015; Orlando, Ludovic/A-8932-2013; OI Korneliussen, Thorfinn Sand/0000-0001-7576-5380; Gilbert, Marcus/0000-0002-5805-7195; Metspalu, Mait/0000-0003-3099-9161; Moltke, Ida/0000-0001-7052-8554; Rasmussen, Simon/0000-0001-6323-9041; Jakobsson, Mattias/0000-0001-7840-7853; Albrechtsen, Anders/0000-0001-7306-031X; Olsen, Jesper/0000-0002-4445-5520; Malmstrom, Helena/0000-0002-6456-8055; Spitsyn, Viktor/0000-0002-4354-2905; Skoglund, Pontus/0000-0002-3021-5913; Orlando, Ludovic/0000-0003-3936-1850; Malaspinas, Anna-Sapfo/0000-0003-1001-7511; Raghavan, Maanasa/0000-0003-1997-0739 FU Danish National Research Foundation; Lundbeck Foundation; Villum Foundation; Swiss National Science Foundation [PBSKP3_143259]; The Rock Foundation; Social Sciences and Humanities Research Council of Canada; National Science Foundation Office of Polar Programs [OPP-9974623, OPP-0327641, OPP-9726126, OPP-9977931, OPP-9813044]; Northern Worlds Initiative; Augustinus Foundation; Danish Council for Independent Research; National Science Foundation [0732327, OPP-9905090, OPP-0327676]; Wenner-Gren Foundation for Anthropological Research [6364]; Natural Sciences and Engineering Research Council of Canada; University of Utah; EU Marie Curie FP7 Initial Training Network Grant [FP7-ITN-215362-2]; Arts and Humanities Research Council [AH/K006029/1]; Memorial University Faculty of Arts Research Initiative; Memorial University Office of Research Grant; EU European Regional Development Fund through Centre of Excellence in Genomics to Estonian Biocentre; Estonian Institutional Research [IUT24-1]; Estonian Science Foundation [8973] FX We thank the Danish National Sequencing Centre, T. B. Brand, and P. S. Olsen for technical assistance; anonymous donors for providing DNA samples; A. Helgason and S. Sunna Ebenesersdottir from deCODE for their input on mtDNA phylogenies; A, Di Rienzo for access to genotyping data from Siberian populations; J. R. Southon (B. T. F.), Kitikmeot Heritage Society (T. M. F.), Polar Continental Shelf Project (T. M. F.), Inuit Heritage Trust (D. H. O'R., Je.C., Jo.C., M. G. H.), Kivalliq Inuit Association (D. H. O'R., Jo.C., M. G. H.), communities of Coral Harbor and Chesterfield Inlet (D. H. O'R., Jo.C., M. G. H.), Canadian Museum of History (D. H. O'R., Je. C., Jo.C., M. G. H.), D. Morrison (D. H. O'R., Je. C., Jo.C., M. G. H.), L. Wood (D. H. O'R., Jo.C., M. G. H.), J. Young (D. H. O'R., Je. C., Jo.C., M. G. H.), D. Stenton (D. H. O'R., Je. C., Jo.C., M. G. H.), S. Girling-Christie (Je. C.), Commission for Scientific Research in Greenland (J. A.), Greenland National Museum and Archives (J. A.), Parks Canada (M. A. P. R., V. G.), Memorial University (V. G., M. A. P. R.), Government of Newfoundland and Labrador (V. G.), The Rooms Inc. (V. G.), Innu Nation (V. G.), Nunatsiavut Government (V. G.), Miawpukek First Nation (V. G.), D. Lavers (V. G.), R. Anstey (V. G.), W. Jones and Qanirtuuq Inc., Quinhagak, Alaska (K. B. and R. K.), the residents of Quinhagak, Alaska (K. B. and R. K.), Nunivak Island Mekoryuk Alaska Corporation, Mekoryuk, Alaska (K. B. and R. K.), and the Carnegie Trust for the Universities of Scotland (K. B. and R. K.). Supported by the Danish National Research Foundation (E. W.) Lundbeck Foundation (E. W., N.L.), Villum Foundation (A. A.), Swiss National Science Foundation Fellowship (A.S.-M, PBSKP3_143259), The Rock Foundation (B. G., M. A.), Social Sciences and Humanities Research Council of Canada (T. M. F.), National Science Foundation Office of Polar Programs (D, H, O'R.: OPP-9974623 and OPP-0327641; Jo.C.: OPP-9726126 and OPP-9977931; M. G. H.: OPP-9813044), Northern Worlds Initiative (H. C. G.), Augustinus Foundation (H. C. G.), the Danish Council for Independent Research (I. M.), National Science Foundation (J. A.: International Polar Year grant 0732327; M. H. C., OPP-9905090 and OPP-0327676), Wenner-Gren Foundation for Anthropological Research (M. G. H.: no. 6364), Natural Sciences and Engineering Research Council of Canada Postgraduate Fellowship (M. G. H.), University of Utah Graduate Research Fellowship (M. G. H.), EU Marie Curie FP7 Initial Training Network Grant (Ma.R.: FP7-ITN-215362-2), Arts and Humanities Research Council (K. B. and R. K.: AH/K006029/1), Memorial University Faculty of Arts Research Initiative (V. G.), Memorial University Office of Research Grant (V. G.), Social Sciences and Humanities Research Council of Canada (M. A. P. R.), EU European Regional Development Fund through the Centre of Excellence in Genomics to Estonian Biocentre (M. M. and R. V.), Estonian Institutional Research (M. M. and R. V.: grant IUT24-1), and Estonian Science Foundation (M. M. and R. V.: grant 8973). Informed consent was obtained for the genome sequencing of the modern individuals, with ethical approval from The National Committee on Health Research Ethics, Denmark (H-3-2012-FSP21). Sequence data for the ancient samples are available for download through European Nucleotide Archive (ENA) accession no. PRJEB6516, and for the Illumina genotype data through Gene Expression Omnibus (GEO) series accession no. GSE59546 and at www.ebc.ee/free_data.; Alignment files (BAMs) for the ancient genomes sequenced in this study are available at www.cbs.dtu.dk/suppl/arctic. The data for the modern populations are available for demographic research under data access agreement with E. W. The Thule samples from Silumiut, Kamarvik, and Sadlermiut were made available by D. H. O'R. under agreement with the Canadian Museum of Civilization and local communities who provided research access to the samples. C. B. is on the advisory board of a project at 23andMe and on the scientific advisory boards of Personalis Inc.; InVitae; Etalon Inc.; and Ancestry.com. The authors declare no competing financial interests. NR 84 TC 63 Z9 64 U1 9 U2 85 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 29 PY 2014 VL 345 IS 6200 BP 1020 EP + AR 1255832 DI 10.1126/science.1255832 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AN8RE UT WOS:000340870900030 PM 25170159 ER PT J AU Melis, C Reid, MJ Mioduszewski, AJ Stauffer, JR Bower, GC AF Melis, Carl Reid, Mark J. Mioduszewski, Amy J. Stauffer, John R. Bower, Geoffrey C. TI A VLBI resolution of the Pleiades distance controversy SO SCIENCE LA English DT Article ID ECLIPSING BINARY HD-23642; OPEN CLUSTERS; HIPPARCOS-PARALLAXES; CATALOG; CONSTRAINTS; ASTROMETRY; ACCURACY; ERRORS; STARS AB Because of its proximity and its youth, the Pleiades open cluster of stars has been extensively studied and serves as a cornerstone for our understanding of the physical properties of young stars. This role is called into question by the "Pleiades distance controversy," wherein the cluster distance of 120.2 +/- 1.5 parsecs (pc) as measured by the optical space astrometry mission Hipparcos is significantly different from the distance of 133.5 +/- 1.2 pc derived with other techniques. We present an absolute trigonometric parallax distance measurement to the Pleiades cluster that uses very long baseline radio interferometry (VLBI). This distance of 136.2 +/- 1.2 pc is the most accurate and precise yet presented for the cluster and is incompatible with the Hipparcos distance determination. Our results cement existing astrophysical models for Pleiades-age stars. C1 [Melis, Carl] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mioduszewski, Amy J.] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA. [Stauffer, John R.] CALTECH, SSC, Pasadena, CA 91125 USA. [Bower, Geoffrey C.] ASIAA, Hilo, HI 96720 USA. RP Melis, C (reprint author), Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr, La Jolla, CA 92093 USA. EM cmelis@ucsd.edu FU U.S. National Science Foundation [AST-1313428, AST-1003318]; Lawrence Livermore National Laboratory; Spitzer Science Center Visiting Graduate Student Program; Academica Sinica Institute for Astronomy and Astrophysics FX We thank the National Radio Astronomy Observatory, Green Bank Telescope, Arecibo Observatory, and Effelsberg Telescope staff who coordinated, conducted, and correlated observations for this project. All data presented in this paper are maintained in the National Radio Astronomy Observatory archive. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work made use of the Swinburne University of Technology software correlator, developed as part of the Australian Major National Research Facilities Programme and operated under license. C. M. acknowledges financial support from the U.S. National Science Foundation through awards AST-1313428 and AST-1003318, from a Lawrence Livermore National Laboratory minigrant to the University of California-Los Angeles, and from the Spitzer Science Center Visiting Graduate Student Program. G.C.B. acknowledges support from the Academica Sinica Institute for Astronomy and Astrophysics. NR 27 TC 45 Z9 45 U1 0 U2 5 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD AUG 29 PY 2014 VL 345 IS 6200 BP 1029 EP 1032 DI 10.1126/science.1256101 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AN8RE UT WOS:000340870900033 PM 25170147 ER PT J AU Kirshner, RP AF Kirshner, Robert P. TI ASTROPHYSICS Supernova seen through gamma-ray eyes SO NATURE LA English DT Editorial Material C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kirshner, RP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rkirshner@cfa.harvard.edu NR 7 TC 0 Z9 0 U1 0 U2 1 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 28 PY 2014 VL 512 IS 7515 BP 375 EP 376 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AN8GC UT WOS:000340840600018 PM 25164743 ER PT J AU Janousek, WM Marra, PP Kilpatrick, AM AF Janousek, William M. Marra, Peter P. Kilpatrick, A. Marm TI Avian roosting behavior influences vector-host interactions for West Nile virus hosts SO PARASITES & VECTORS LA English DT Article DE Sociality; Group size; Vector-host contact rates; Vector:host ratio; Model; Flocking; Fitness; Evolution ID CULEX-PIPIENS COMPLEX; DIPTERA-CULICIDAE; INFECTION RATES; BRIDGE VECTOR; SHELBY COUNTY; SELFISH HERD; TRANSMISSION; MOSQUITOS; BIRDS; AMPLIFICATION AB Background: Extensive work has shown that vectors almost never feed at random. Often, a subset of individual hosts and host species are fed on much more frequently than expected from their abundance and this can amplify pathogen transmission. However, the drivers of variation in contact patterns between vectors and their hosts are not well understood, even in relatively well-studied systems such as West Nile virus (WNV). Methods: We compared roosting height and roost aggregation size of seven avian host species of WNV with patterns of host-seeking mosquito (Culex pipiens) abundance at communal and non-communal roost sites. Results: First, host-seeking mosquito abundance increased with height and paralleled increased mosquito feeding preferences on species roosting higher in the tree canopy. Second, there were several hundred-fold fewer mosquitoes per bird trapped at American robin (Turdus migratorius) communal roosts compared to non-communal roost sites, which could reduce transmission from and to this key amplifying host species. Third, seasonal changes in communal roost formation may partly explain observed seasonal changes in mosquito feeding patterns, including a decrease in feeding on communal roosting robins. Conclusions: These results illustrate how variation in habitat use by hosts and vectors and social aggregation by hosts influence vector-host interactions and link the behavioral ecology of birds and the transmission of vector-borne diseases to humans. C1 [Janousek, William M.; Kilpatrick, A. Marm] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Janousek, WM (reprint author), Univ Montana, Dept Ecosyst & Conservat Sci, Avian Sci Ctr, Missoula, MT 59802 USA. EM janousek12@gmail.com; akilpatr@ucsc.edu FU NSF [EF-0914866]; NIH [1R01AI090159] FX We would like to thank the residents and Neighborhood Nestwatch participants from Takoma Park, MD and Foggy Bottom, DC for allowing us to conduct research on their property. A special thanks to T. Austin, M. Bouboulis, G. Jones, E. Perryman, E. Piller, L. Reifel for assistance in the field, and R. Reitsma for logistical support. Funding was provided by NSF grant EF-0914866 and NIH grant 1R01AI090159. NR 59 TC 8 Z9 8 U1 5 U2 36 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 28 PY 2014 VL 7 AR 399 DI 10.1186/1756-3305-7-399 PG 11 WC Parasitology SC Parasitology GA AO3BX UT WOS:000341204300001 PM 25167979 ER PT J AU Pepe, A Goodman, A Muench, A Crosas, M Erdmann, C AF Pepe, Alberto Goodman, Alyssa Muench, August Crosas, Merce Erdmann, Christopher TI How Do Astronomers Share Data? Reliability and Persistence of Datasets Linked in AAS Publications and a Qualitative Study of Data Practices among US Astronomers SO PLOS ONE LA English DT Article ID EDUCATION; TELESCOPE AB We analyze data sharing practices of astronomers over the past fifteen years. An analysis of URL links embedded in papers published by the American Astronomical Society reveals that the total number of links included in the literature rose dramatically from 1997 until 2005, when it leveled off at around 1500 per year. The analysis also shows that the availability of linked material decays with time: in 2011, 44% of links published a decade earlier, in 2001, were broken. A rough analysis of link types reveals that links to data hosted on astronomers' personal websites become unreachable much faster than links to datasets on curated institutional sites. To gauge astronomers' current data sharing practices and preferences further, we performed in-depth interviews with 12 scientists and online surveys with 173 scientists, all at a large astrophysical research institute in the United States: the Harvard-Smithsonian Center for Astrophysics, in Cambridge, MA. Both the in-depth interviews and the online survey indicate that, in principle, there is no philosophical objection to data-sharing among astronomers at this institution. Key reasons that more data are not presently shared more efficiently in astronomy include: the difficulty of sharing large data sets; over reliance on non-robust, non-reproducible mechanisms for sharing data (e.g. emailing it); unfamiliarity with options that make data-sharing easier (faster) and/or more robust; and, lastly, a sense that other researchers would not want the data to be shared. We conclude with a short discussion of a new effort to implement an easy-to-use, robust, system for data sharing in astronomy, at theastrodata.org, and we analyze the uptake of that system to-date. C1 [Pepe, Alberto; Goodman, Alyssa; Muench, August; Erdmann, Christopher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pepe, Alberto; Goodman, Alyssa; Crosas, Merce] Harvard Univ, Inst Quantitat Social Sci, Cambridge, MA 02138 USA. RP Pepe, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alberto.pepe@gmail.com RI Goodman, Alyssa/A-6007-2010; OI Goodman, Alyssa/0000-0003-1312-0477; Erdmann, Christopher/0000-0003-2554-180X; Muench, August/0000-0003-0666-6367 FU National Aeronautics and Space Administration through the Astrophysical Data Analysis Program (ADAP) [NNX12AE11G] FX This material is based upon work supported by the National Aeronautics and Space Administration under Grant/Contract/Agreement No. NNX12AE11G issued through the Astrophysical Data Analysis Program (ADAP). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 15 TC 5 Z9 6 U1 0 U2 6 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD AUG 28 PY 2014 VL 9 IS 8 AR e104798 DI 10.1371/journal.pone.0104798 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO4JP UT WOS:000341303700014 PM 25165807 ER PT J AU Cooper, M Martin, RV Wespes, C Coheur, PF Clerbaux, C Murray, LT AF Cooper, Matthew Martin, Randall V. Wespes, Catherine Coheur, Pierre-Francois Clerbaux, Cathy Murray, Lee T. TI Tropospheric nitric acid columns from the IASI satellite instrument interpreted with a chemical transport model: Implications for parameterizations of nitric oxide production by lightning SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PACIFIC EXPLORATORY MISSION; ATMOSPHERIC-CHEMISTRY; OZONE PRODUCTION; NITROGEN-OXIDES; AIRBORNE MEASUREMENTS; TROPICAL PACIFIC; NOX PRODUCTION; GEOS-CHEM; DISTRIBUTIONS; EMISSIONS AB This paper interprets tropical tropospheric nitric acid columns from the Infrared Atmospheric Sounding Interferometer (IASI) satellite instrument with a global chemical transport model (GEOS-Chem). GEOS-Chemand IASI columns generally agree over the tropical ocean to within 10%. However, the GEOS-Chem simulation underestimates IASI nitric acid over Southeast Asia by a factor of 2. The regional nitric acid bias is confirmed by comparing the GEOS-Chem simulation with additional satellite (High Resolution Dynamics Limb Sounder, Atmospheric Chemistry Experiment Fourier Transform Spectrometer) and aircraft (Pacific Exploratory Mission (PEM)-Tropics A and PEM-West B) observations of the middle and upper troposphere. This bias appears to be driven by the lightning NOx parameterization, both in terms of the magnitude of the NOx source and the ozone production efficiency of concentrated lightning NOx plumes. We tested a subgrid lightning plume parameterization and found that an ozone production efficiency of 15 mol/mol in lightning plumes over Southeast Asia in conjunction with an additional 0.5 Tg N would reduce the regional nitric acid bias from 92% to 6% without perturbing the rest of the tropics. Other sensitivity studies such as modified NOx yield per flash, increased altitude of lightning NOx emissions, decreased convective mass flux, or increased scavenging of nitric acid required unrealistic changes to reduce the bias. C1 [Cooper, Matthew; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wespes, Catherine; Coheur, Pierre-Francois; Clerbaux, Cathy] Univ Libre Bruxelles, Brussels, Belgium. [Clerbaux, Cathy] Univ Paris 06, Sorbonne Univ, Paris, France. [Clerbaux, Cathy] Univ Versailles St Quentin, Paris, France. [Clerbaux, Cathy] LATMOS IPSL, CNRS INSU, Paris, France. [Murray, Lee T.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Murray, Lee T.] Columbia Univ, Lamont Doherty Earth Observ, New York, NY USA. RP Cooper, M (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. EM cooperm2@dal.ca RI Chem, GEOS/C-5595-2014; Murray, Lee/F-2296-2014; Martin, Randall/C-1205-2014; clerbaux, cathy/I-5478-2013 OI Murray, Lee/0000-0002-3447-3952; Martin, Randall/0000-0003-2632-8402; FU Natural Sciences and Engineering Research Council of Canada; Belgian State Federal Office for Scientific, Technical and Cultural Affairs; European Space Agency (ESA Prodex IASI.Flow); EUMETSAT (O3MSAF) FX IASI HNO3 data are available on request by contacting P.-F Coheur. IASI CO data were provided by LATMOS/CNRS and ULB and are available online at the Ether database at http://www.pole-ether.fr/. HIRDLS data products are available online at NASA's Goddard Earth Sciences Data and Information Services Center. ACE-FTS data are available on request by contacting the ACE Science Team at info@scisat.ca. Aircraft data from PEM West and PEM-Tropics campaigns are made available online at NASA's Global Tropospheric Experiment webpage at http://www-gte.larc.nasa.gov/gte_fld.htm. SHADOZ ozonesonde measurements are available online at http://croc.gsfc.nasa.gov/shadoz/. Information on accessing GEOS-Chem code can be found online at geos-chem.org. This work was supported by the Natural Sciences and Engineering Research Council of Canada. P.-F. Coheur and C. Wespes are, respectively, Senior Research Associate and Postdoctoral Researcher with F.R.S.-FNRS. The research in Belgium was also funded by the Belgian State Federal Office for Scientific, Technical and Cultural Affairs and the European Space Agency (ESA Prodex IASI.Flow), as well as by EUMETSAT (O3MSAF). NR 62 TC 5 Z9 5 U1 0 U2 27 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 AUG 27 PY 2014 VL 119 IS 16 BP 10068 EP 10079 DI 10.1002/2014JD021907 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA AP3RF UT WOS:000341994000030 ER PT J AU Guevara, L Sanchez-Cordero, V Leon-Paniagua, L Woodman, N AF Guevara, Lazaro Sanchez-Cordero, Victor Leon-Paniagua, Livia Woodman, Neal TI A new species of small-eared shrew (Mammalia, Eulipotyphla, Cryptotis) from the Lacandona rain forest, Mexico SO JOURNAL OF MAMMALOGY LA English DT Article DE Chiapas; Cryptotis nigrescens species group; North America; protected area; Soricidae; tropical forests ID CYTOCHROME-B GENE; MORPHOLOGICAL VARIATION; SORICOMORPHA SORICIDAE; DISTRIBUTIONAL RECORDS; YUCATAN PENINSULA; CHIAPAS; INSECTIVORA; GUATEMALA; HIGHLANDS; HONDURAS AB The diversity and distribution of mammals in the American tropics remain incompletely known. We describe a new species of small-eared shrew (Soricidae, Cryptotis) from the Lacandona rain forest, Chiapas, southern Mexico. The new species is distinguished from other species of Cryptotis on the basis of a unique combination of pelage coloration, size, dental, cranial, postcranial, and external characters, and genetic distances. It appears most closely related to species in the Cryptotis nigrescens species group, which occurs from southern Mexico to montane regions of Colombia. This discovery is particularly remarkable because the new species is from a low-elevation habitat (approximately 90 m), whereas most shrews in the region are restricted to higher elevations, typically > 1,000 m. The only known locality for the new shrew is in one of the last areas in southern Mexico where relatively undisturbed tropical vegetation is still found. The type locality is protected by the Mexican government as part of the Yaxchilan Archaeological Site on the border between Mexico and Guatemala. C1 [Guevara, Lazaro] Univ Nacl Autonoma Mexico, Coyoacan 04360, DF, Mexico. [Guevara, Lazaro; Sanchez-Cordero, Victor] Univ Nacl Autonoma Mexico, Inst Biol, Dept Zool, Mexico City 04510, DF, Mexico. [Leon-Paniagua, Livia] Univ Nacl Autonoma Mexico, Fac Ciencias, Dept Evolut Biol, Museo Zool Alfonso L Herrera, Mexico City 04510, DF, Mexico. [Woodman, Neal] US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Guevara, L (reprint author), Univ Nacl Autonoma Mexico, Av Ciudad Univ 3000, Coyoacan 04360, DF, Mexico. EM llg@st.ib.unam.mx OI Woodman, Neal/0000-0003-2689-7373 FU Posgrado en Ciencias Biologicas (UNAM); Consejo Nacional de Ciencias y Tecnologia (CONACYT); Comision Nacional para el Conocimiento y Uso de la Biodiversidad (CONABIO) [FB1587/JM044/12] FX We thank the following curators and collection managers for the facilities offered to examine specimens in the collections under their care: N. B. Simmons, R. S. Voss, and E. Westwig (AMNH); R. C. Dowler (ASNHC); P. D. Jenkins, R. Portela M., and L. Tomsett (BMNH); L. F. Baptista (CAS); S. McLaren and J. R. Wible (CMNH); Fernando A. Cervantes (CNMA); Consuelo Lorenzo (ECO-SC-M); S. T Alvarez (ENCB), L. R. Heaney, B. D. Patterson, and W. S. Stanley (FMNH); R. M. Timm (KU); J. M. Chupasko (MCZ); S. Jansa (MMNH); G. Pothet, M. Tranier, and C. Denys (MNHN); A. Engilis, Jr. (WFB); F. Spitzenberger (NMW); M. D. Engstrom (ROM); G. Storch (SMF); G. D. Schrimper (SUI); J. Ramirez-Pulido and N. Gonzalez-Ruiz (UAMI); S. Betancourt (UADY); P. Myers (UMMZ); S. G. Perez (USAC); and S. Peurach (USNM). We express our gratitude to M. Garcia-Varela and C. Pinacho for facilitating use of the molecular lab, C. Loyola for her assistance with the production of photographs, and E. Esparza for drawing the upper tooth row. S. Ortega-Garcia provided invaluable support with database of shrews. We thank O. F. Francke for comments on Lacandona's biodiversity. LG is grateful to Posgrado en Ciencias Biologicas (UNAM), and Consejo Nacional de Ciencias y Tecnologia (CONACYT) for grants and fellowships. Funding for the biological data cleaning was provided by Comision Nacional para el Conocimiento y Uso de la Biodiversidad (CONABIO, FB1587/JM044/12). L. Carraway and an anonymous reviewer provided useful feedback on a previous version of our 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 51 TC 0 Z9 1 U1 0 U2 13 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 22 PY 2014 VL 95 IS 4 BP 739 EP 753 DI 10.1644/14-MAMM-A-018 PG 15 WC Zoology SC Zoology GA AO1IG UT WOS:000341065200006 ER PT J AU Voss, RS Helgen, KM Jansa, SA AF Voss, Robert S. Helgen, Kristofer M. Jansa, Sharon A. TI Extraordinary claims require extraordinary evidence: a comment on Cozzuol et al. (2013) SO JOURNAL OF MAMMALOGY LA English DT Article DE mammals; Neotropical; Perissodactyla; Tapiridae; Tapirus kabomani; taxonomy ID TAPIR; PERISSODACTYLA; SYSTEMATICS; MAMMALIA AB The recent description of a new species of Amazonian tapir is inadequately supported by the genetic, morphological, and ethnographic information provided by the authors. C1 [Voss, Robert S.] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Jansa, Sharon A.] Univ Minnesota, Dept Ecol Evolut & Behav, St Paul, MN 55108 USA. [Jansa, Sharon A.] Univ Minnesota, JF Bell Museum Nat Hist, St Paul, MN 55108 USA. RP Voss, RS (reprint author), Amer Museum Nat Hist, Dept Mammal, West 79th St, New York, NY 10024 USA. EM voss@amnh.org NR 24 TC 3 Z9 3 U1 1 U2 17 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 22 PY 2014 VL 95 IS 4 BP 893 EP 898 DI 10.1644/14-MAMM-A-054 PG 6 WC Zoology SC Zoology GA AO1IG UT WOS:000341065200020 ER PT J AU Akre, KL Bernal, X Rand, AS Ryan, MJ AF Akre, Karin L. Bernal, Ximena Stanley Rand, A. Ryan, Michael J. TI Harmonic calls and indifferent females: no preference for human consonance in an anuran SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE animal communication; consonance; music; receiver psychology; signal evolution ID BULLFROG RANA-CATESBEIANA; PHYSALAEMUS-PUSTULOSUS; SEXUAL SELECTION; COMPARATIVE PERSPECTIVE; SENSORY EXPLOITATION; VOCAL PRODUCTION; COMPLEX SOUNDS; TUNGARA FROG; MUSIC; PERCEPTION AB The human music faculty might have evolved from rudimentary components that occur in non-human animals. The evolutionary history of these rudimentary perceptual features is not well understood and rarely extends beyond a consideration of vertebrates that possess a cochlea. One such antecedent is a preferential response to what humans perceive as consonant harmonic sounds, which are common in many animal vocal repertoires. We tested the phonotactic response of female tungara frogs (Physalaemus pustulosus) to variations in the frequency ratios of their harmonically structured mating call to determine whether frequency ratio influences attraction to acoustic stimuli in this vertebrate that lacks a cochlea. We found that the ratio of frequencies present in acoustic stimuli did not influence female response. Instead, the amount of inner ear stimulation predicted female preference behaviour. We conclude that the harmonic relationships that characterize the vocalizations of these frogs did not evolve in response to a preference for frequency intervals with low-integer ratios. Instead, the presence of harmonics in their mating call, and perhaps in the vocalizations of many other animals, is more likely due to the biomechanics of sound production rather than any preference for 'more musical' sounds. C1 [Akre, Karin L.] Duke Univ, Dept Biol, Durham, NC 27708 USA. [Akre, Karin L.] Hunter Coll, Dept Psychol, New York, NY 10065 USA. [Bernal, Ximena] Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. [Bernal, Ximena; Stanley Rand, A.; Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Panama. [Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. RP Akre, KL (reprint author), Duke Univ, Dept Biol, Durham, NC 27708 USA. EM karin.akre@duke.edu; mryan@utexas.edu FU NSF IBN [98-16564] FX The Smithsonian Tropical Research Institute provided excellent support with fieldwork. Funding was provided to M.R. by NSF IBN 98-16564. NR 45 TC 2 Z9 2 U1 1 U2 30 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 22 PY 2014 VL 281 IS 1789 AR 20140986 DI 10.1098/rspb.2014.0986 PG 5 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AL5HM UT WOS:000339164400021 PM 24990679 ER PT J AU Aplin, LM Farine, DR Mann, RP Sheldon, BC AF Aplin, Lucy M. Farine, Damien R. Mann, Richard P. Sheldon, Ben C. TI Individual-level personality influences social foraging and collective behaviour in wild birds SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE collective decision-making; leader-follower; social information; group foraging; behavioural type; Parus major ID TIT PARUS-MAJOR; DECISION-MAKING; GREAT TITS; EXPLORATORY-BEHAVIOR; AVIAN PERSONALITIES; BARNACLE GEESE; ANIMAL GROUPS; RISK-TAKING; LEADERSHIP; EVOLUTION AB There is increasing evidence that animal groups can maintain coordinated behaviour and make collective decisions based on simple interaction rules. Effective collective action may be further facilitated by individual variation within groups, particularly through leader-follower polymorphisms. Recent studies have suggested that individual-level personality traits influence the degree to which individuals use social information, are attracted to conspecifics, or act as leaders/followers. However, evidence is equivocal and largely limited to laboratory studies. We use an automated data-collection system to conduct an experiment testing the relationship between personality and collective decision-making in the wild. First, we report that foraging flocks of great tits (Parus major) show strikingly synchronous behaviour. A predictive model of collective decision-making replicates patterns well, suggesting simple interaction rules are sufficient to explain the observed social behaviour. Second, within groups, individuals with more reactive personalities behave more collectively, moving to within-flock areas of higher density. By contrast, proactive individuals tend to move to and feed at spatial periphery of flocks. Finally, comparing alternative simulations of flocking with empirical data, we demonstrate that variation in personality promotes within-patch movement while maintaining group cohesion. Our results illustrate the importance of incorporating individual variability in models of social behaviour. C1 [Aplin, Lucy M.; Farine, Damien R.; Sheldon, Ben C.] Univ Oxford, Edward Grey Inst Field Ornithol, Oxford OX1 3PS, England. [Aplin, Lucy M.] Australian Natl Univ, Res Sch Biol, Acton, ACT 2600, Australia. [Farine, Damien R.] Univ Calif Davis, Dept Anthropol, Davis, CA 95616 USA. [Farine, Damien R.] Smithsonian Trop Res Inst, Ancon, Panama. [Mann, Richard P.] Uppsala Univ, Dept Math, S-75106 Uppsala, Sweden. RP Farine, DR (reprint author), Univ Oxford, Edward Grey Inst Field Ornithol, Oxford OX1 3PS, England. EM damien.farine@zoo.ox.ac.uk RI Sheldon, Ben/A-8056-2010; Mann, Richard/N-9779-2014 OI Sheldon, Ben/0000-0002-5240-7828; Mann, Richard/0000-0003-0701-1274 FU Australian Postgraduate Award; European Research Council [AdG 250164, IDCAB 220/104702003]; ERC [AdG 250164]; BBSRC [BB/L006081/1] FX The study was supported by an Australian Postgraduate Award to L.M.A., and a European Research Council grant to B.C.S. (AdG 250164). R.P.M. was supported by a European Research Council grant to D. Sumpter (IDCAB 220/104702003). The work was funded by grants from the ERC (AdG 250164) and BBSRC (BB/L006081/1) to B.C.S. NR 63 TC 38 Z9 39 U1 16 U2 160 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 22 PY 2014 VL 281 IS 1789 AR 20141016 DI 10.1098/rspb.2014.1016 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AL5HM UT WOS:000339164400024 PM 24990682 ER PT J AU Vantyghem, AN McNamara, BR Russell, HR Main, RA Nulsen, PEJ Wise, MW Hoekstra, H Gitti, M AF Vantyghem, A. N. McNamara, B. R. Russell, H. R. Main, R. A. Nulsen, P. E. J. Wise, M. W. Hoekstra, H. Gitti, M. TI Cycling of the powerful AGN in MS 0735.6+7421 and the duty cycle of radio AGN in clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: individual: MS 0735.6+7421; galaxies: clusters: intracluster medium; galaxies: jets; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; LARGE-SCALE SHOCK; X-RAY-CLUSTERS; GALAXY CLUSTERS; INTRACLUSTER MEDIUM; HYDRA-A; NEARBY CLUSTERS; PERSEUS CLUSTER; LIMITED SAMPLE AB We present an analysis of deep Chandra X-ray observations of the galaxy cluster MS 0735.6+7421, which hosts the most energetic radio active galactic nucleus (AGN) known. Our analysis has revealed two cavities in its hot atmosphere with diameters of 200-240 kpc. The total cavity enthalpy, mean age, and mean jet power are 9 x 10(61) erg, 1.6 x 10(8) yr, and 1.7 x 10(46) erg s(-1), respectively. The cavities are surrounded by nearly continuous temperature and surface brightness discontinuities associated with an elliptical shock front of Mach number 1.26 (1.17-1.30) and age of 1.1 x 10(8) yr. The shock has injected at least 4 x 10(61) erg into the hot atmosphere at a rate of 1.1 x 10(46) erg s(-1). A second pair of cavities and possibly a second shock front are located along the radio jets, indicating that the AGN power has declined by a factor of 30 over the past 100 Myr. The multiphase atmosphere surrounding the central galaxy is cooling at a rate of 40 M(aS (TM))yr(-1), but does not fuel star formation at an appreciable rate. In addition to heating, entrainment in the radio jet may be depleting the nucleus of fuel and preventing gas from condensing out of the intracluster medium. Finally, we examine the mean time intervals between AGN outbursts in systems with multiple generations of X-ray cavities. We find that, like MS0735, their AGN rejuvenate on a time-scale that is approximately 1/3 of their mean central cooling time-scales, indicating that jet heating is outpacing cooling in these systems. C1 [Vantyghem, A. N.; McNamara, B. R.; Russell, H. R.; Main, R. A.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [McNamara, B. R.] Perimeter Inst Theoret Phys, Waterloo, ON, Canada. [McNamara, B. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wise, M. W.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Hoekstra, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Gitti, M.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Gitti, M.] Ist Radioastron, INAF, I-40129 Bologna, Italy. RP Vantyghem, AN (reprint author), Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. EM a2vantyg@uwaterloo.ca OI Gitti, Myriam/0000-0002-0843-3009; Nulsen, Paul/0000-0003-0297-4493; Hoekstra, Henk/0000-0002-0641-3231 FU Natural Sciences and Engineering Research Council of Canada; Chandra X-ray Observatory Cycle 10 Large Project [MS0735] FX We thank the anonymous referee for helpful comments that improved the paper. ANV thanks Julie Hlavacek-Larrondo for helpful comments. ANV, BRM, HRR, and RAM acknowledge support from the Natural Sciences and Engineering Research Council of Canada. BRM acknowledges funding from the Chandra X-ray Observatory Cycle 10 Large Project proposal for MS0735. The scientific results reported in this article are based on observations made by the Chandra X-ray Observatory. NR 61 TC 9 Z9 9 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 2014 VL 442 IS 4 BP 3192 EP 3205 DI 10.1093/mnras/stu1030 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TZ UT WOS:000339924900031 ER PT J AU Bassett, R Glazebrook, K Fisher, DB Green, AW Wisnioski, E Obreschkow, D Cooper, EM Abraham, RG Damjanov, I McGregor, PJ AF Bassett, Robert Glazebrook, Karl Fisher, David B. Green, Andrew W. Wisnioski, Emily Obreschkow, Danail Cooper, Erin Mentuch Abraham, Roberto G. Damjanov, Ivana McGregor, Peter J. TI DYNAMO - II. Coupled stellar and ionized-gas kinematics in two low-redshift clumpy discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: kinematics and dynamics; galaxies: evolution ID STAR-FORMING GALAXIES; INTEGRAL-FIELD SPECTROSCOPY; INITIAL MASS FUNCTION; ULTRA DEEP FIELD; FORMATION HISTORY; SCALING RELATIONS; VELOCITY DISPERSION; SPIRAL GALAXIES; GALACTIC DISKS; COSMOLOGICAL SIMULATIONS AB We study the spatially resolved stellar kinematics of two star-forming galaxies at z similar to 0.1 from the larger DYnamics of Newly Assembled Massive Objects (DYNAMO) sample. These galaxies, which have been characterized by high levels of star formation and large ionized-gas velocity dispersions, are considered possible analogues to high-redshift clumpy discs. They were observed using the Gemini Multi-Object Spectrograph instrument in integral field spectroscopy (IFS) mode at the Gemini Observatory with high spectral resolution (R similar or equal to 5400, equivalent to sigma similar or equal to 24 km s(-1) at the observed wavelengths) and similar to 6 h exposure times in order to measure the resolved stellar kinematics via absorption lines. We also obtain higher quality emission-line kinematics than previous observations. The spatial resolution (1.2 kpc) is sufficient to show that the ionized gas in these galaxies (as traced by H beta emission) is morphologically irregular, forming multiple giant clumps while stellar continuum light is smooth and well described by an exponential profile. Clumpy gas morphologies observed in IFS data are confirmed by complementary narrow-band H alpha imaging from the Hubble Space Telescope. Morphological differences between the stars and ionized gas are not reflected dynamically as stellar kinematics are found to be closely coupled to the kinematics of the ionized gas: both components are smoothly rotating with large velocity dispersions (similar to 40 km s(-1)) suggesting that the high gas dispersions are not primarily driven by star formation feedback. In addition, the stellar population ages of these galaxies are estimated to be quite young (60-500 Myr). The large velocity dispersions measured for these young stars suggest that we are seeing the formation of thick discs and/or stellar bulges in support of recent models which produce these from clumpy galaxies at high redshift. C1 [Bassett, Robert; Glazebrook, Karl; Fisher, David B.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Glazebrook, Karl; Obreschkow, Danail] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Green, Andrew W.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Wisnioski, Emily] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Obreschkow, Danail] Univ Western Australia, Int Ctr Radio Astron Res ICRAR, Crawley, WA 6009, Australia. [Cooper, Erin Mentuch] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Abraham, Roberto G.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Damjanov, Ivana] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McGregor, Peter J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Bassett, R (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia. EM rbassett.astro@gmail.com RI Glazebrook, Karl/N-3488-2015; OI Glazebrook, Karl/0000-0002-3254-9044; Green, Andrew/0000-0003-3052-0819 FU Victorian Department of State Development, Business and Innovation through the Victorian International Research Scholarship (VIRS); ARC Discovery Project [DP130101460]; Gemini Observatory [GN-2011B-Q-54, GS-2011B-Q-88] FX Support for this project is provided in part by the Victorian Department of State Development, Business and Innovation through the Victorian International Research Scholarship (VIRS). We also acknowledge support from ARC Discovery Project DP130101460. This work is based on observations obtained at the Gemini Observatory (programmes GN-2011B-Q-54 and GS-2011B-Q-88), 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 85 TC 6 Z9 6 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2014 VL 442 IS 4 BP 3206 EP 3221 DI 10.1093/mnras/stu1029 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TZ UT WOS:000339924900032 ER PT J AU Nielsen, MTB Gilfanov, M Bogdan, A Woods, TE Nelemans, G AF Nielsen, M. T. B. Gilfanov, M. Bogdan, A. Woods, T. E. Nelemans, G. TI Upper limits on the luminosity of the progenitor of Type Ia supernova SN 2014J SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; supernovae: general; white dwarfs; X-rays: binaries ID X-RAY SOURCES; WHITE-DWARFS; BOLOMETRIC LUMINOSITIES; SUPERSOFT SOURCES; GALAXY; MASS; BINARIES; MODELS; 2007ON AB We analysed archival data of Chandra pre-explosion observations of the position of SN 2014J in M82. No X-ray source at this position was detected in the data, and we calculated upper limits on the luminosities of the progenitor. These upper limits allow us to firmly rule out an unobscured supersoft X-ray source progenitor with a photospheric radius comparable to the radius of white dwarf near the Chandrasekhar mass (similar to 1.38 M-circle dot) and mass accretion rate in the interval where stable nuclear burning can occur. However, due to a relatively large hydrogen column density implied by optical observations of the supernova, we cannot exclude a supersoft source with lower temperatures, kT less than or similar to 70 eV. We find that the supernova is located in the centre of a large structure of soft diffuse emission, about 200 pc across. The mass, similar to 3 x 10(4) M-circle dot and short cooling time of the gas, tau(cool) similar to 8 Myr, suggest that it is a supernova-inflated superbubble, associated with the region of recent star formation. If SN 2014J is indeed located inside the bubble, it likely belongs to the prompt population of Type Ia supernovae, with a delay time as short as similar to 50 Myr. Finally, we analysed the one existing post-supernova Chandra observation and placed upper limit of similar to(1-2) x 10(37) erg s(-1) on the X-ray luminosity of the supernova itself. C1 [Nielsen, M. T. B.; Gilfanov, M.; Woods, T. E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Bogdan, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Nelemans, G.] Katholieke Univ Leuven, Inst Astron, B-3001 Leuven, Belgium. RP Nielsen, MTB (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1,Postfach 1317, D-85741 Garching, Germany. EM medesen@gmail.com RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 NR 39 TC 15 Z9 15 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 21 PY 2014 VL 442 IS 4 BP 3400 EP 3406 DI 10.1093/mnras/stu913 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TZ UT WOS:000339924900048 ER PT J AU Beky, B Kipping, DM Holman, MJ AF Beky, Bence Kipping, David M. Holman, Matthew J. TI spotrod: a semi-analytic model for transits of spotted stars SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; stars: individual: HAT-P-11; starspots ID PLANETARY TRANSIT; NEPTUNE HAT-P-11B; RADIAL-VELOCITY; SYSTEM; PHOTOMETRY; KEPLER; ORBIT; SOAP; TOOL AB The Hubble Space Telescope and the Kepler space mission observed a large number of planetary transits showing anomalies due to starspot eclipses, with more such observations expected in the near future by the K2 mission and the Transiting Exoplanet Survey Satellite. To facilitate analysis of this phenomenon, we present spotrod, a model for planetary transits of stars with an arbitrary limb darkening law and a number of homogeneous, circular spots on their surface. A free, open source implementation written in c, ready to use in python, is available for download. We analyse Kepler observations of the planetary host star HAT-P-11, and study the size and contrast of more than 200 starspots. We find that the flux ratio of spots ranges at least from 0.6 to 0.9, corresponding to an effective temperature approximately 100-450 K lower than the stellar surface, although it is possible that some spots are darker than 0.5. The largest detected spots have a radius less than approximately 0.2 stellar radii. C1 [Beky, Bence; Kipping, David M.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Beky, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bbeky@cfa.harvard.edu FU NASA from the Kepler Participating Scientist Program [NNX09AB28G]; Origins programme [NNX09AB33G, NNX13A124G]; NASA Carl Sagan Fellowships; NASA Science Mission directorate FX Work by BB and MJH was supported by NASA under grant NNX09AB28G from the Kepler Participating Scientist Program and grants NNX09AB33G and NNX13A124G under the Origins programme. DMK is funded by the NASA Carl Sagan Fellowships. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. The MCMC computations in this paper were run on the Odyssey 2.0 cluster supported by the FAS Science Division Research Computing Group at Harvard University. BB is grateful to Robert Noyes for useful comments on the manuscript, and to John A. Johnson for suggesting the name SPOTROD. NR 27 TC 8 Z9 8 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 21 PY 2014 VL 442 IS 4 BP 3686 EP 3699 DI 10.1093/mnras/stu1061 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TZ UT WOS:000339924900069 ER PT J AU Bhat, NDR Ord, SM Tremblay, SE Tingay, SJ Deshpande, AA van Straten, W Oronsaye, S Bernardi, G Bowman, JD Briggs, F Cappallo, RJ Corey, BE Emrich, D Goeke, R Greenhill, LJ Hazelton, BJ Hewitt, JN Johnston-Hollitt, M Kaplan, DL Kasper, JC Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Mitchell, DA Morales, MF Morgan, E Oberoi, D Prabu, T Rogers, AEE Roshi, DA Shankar, NU Srivani, KS Subrahmanyan, R Waterson, M Wayth, RB Webster, RL Whitney, AR Williams, A Williams, CL AF Bhat, N. D. R. Ord, S. M. Tremblay, S. E. Tingay, S. J. Deshpande, A. A. van Straten, W. Oronsaye, S. Bernardi, G. Bowman, J. D. Briggs, F. Cappallo, R. J. Corey, B. E. Emrich, D. Goeke, R. Greenhill, L. J. Hazelton, B. J. Hewitt, J. N. Johnston-Hollitt, M. 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. Prabu, T. Rogers, A. E. E. Roshi, D. A. Shankar, N. Udaya Srivani, K. S. Subrahmanyan, R. Waterson, M. Wayth, R. B. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. TI THE LOW-FREQUENCY CHARACTERISTICS OF PSR J0437-4715 OBSERVED WITH THE MURCHISON WIDE-FIELD ARRAY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: interferometers; methods: observational; pulsars: general; pulsars: individual (PSR J0437-4715) ID MILLISECOND PULSAR J0437-4715; LONG-TERM SCINTILLATION; INTERSTELLAR SCINTILLATION; DISPERSION MEASURE; LOCAL BUBBLE; VELOCITIES; PSR-J0437-4715; POLARIZATION; EMISSION; MHZ AB We report on the detection of the millisecond pulsar PSR J0437-4715 with the Murchison Wide-field Array (MWA) at a frequency of 192 MHz. Our observations show rapid modulations of pulse intensity in time and frequency that arise from diffractive scintillation effects in the interstellar medium (ISM), as well as prominent drifts of intensity maxima in the time-frequency plane that arise from refractive effects. Our analysis suggests that the scattering screen is located at a distance of similar to 80-120 pc from the Sun, in disagreement with a recent claim that the screen is closer (similar to 10 pc). Comparisons with higher frequency data from Parkes reveal a dramatic evolution of the pulse profile with frequency, with the outer conal emission becoming comparable in strength to that from the core and inner conal regions. As well as demonstrating the high time resolution science capabilities currently possible with the MWA, our observations underscore the potential to conduct low-frequency investigations of timing-array millisecond pulsars, which may lead to increased sensitivity in the detection of nanoHertz gravitational waves via the accurate characterization of ISM effects. C1 [Bhat, N. D. R.; Ord, S. M.; Tremblay, S. E.; Tingay, S. J.; Oronsaye, S.; Emrich, D.; Lynch, M. J.; Waterson, M.; Wayth, R. B.; Williams, A.] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. [Bhat, N. D. R.; Ord, S. M.; Tremblay, S. E.; Tingay, S. J.; van Straten, W.; Oronsaye, S.; Briggs, F.; Mitchell, D. A.; Subrahmanyan, R.; Wayth, R. B.; Webster, R. L.] Curtin Univ, ARC Ctr Excellence All sky Astrophys CAASTRO, Bentley, WA 6102, Australia. [Deshpande, A. A.; Prabu, T.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [van Straten, W.] Swinburne Univ, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bernardi, G.] Sq Kilometre Array South Afr, 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. [Goeke, R.; Hewitt, J. N.; Morgan, E.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [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. [Kasper, J. C.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Mitchell, D. A.] CSIRO Astron & Space Sci, Marsfield, NSW 2122, Australia. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune 411007, Maharashtra, India. [Roshi, D. A.] Natl Radio Astron Observ, Charlottesville, VA USA. [Roshi, D. A.] Natl Radio Astron Observ, Green Bank, WV USA. [Webster, R. L.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. RP Bhat, NDR (reprint author), Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia. RI Wayth, Randall/B-2444-2013; Kasper, Justin/D-1152-2010; Udayashankar , N/D-4901-2012; Williams, Andrew/K-2931-2013; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Emrich, David/B-7002-2013; Subrahmanyan, Ravi/D-4889-2012; OI Wayth, Randall/0000-0002-6995-4131; Kasper, Justin/0000-0002-7077-930X; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Emrich, David/0000-0002-4058-1837; van Straten, Willem/0000-0003-2519-7375 FU Curtin Research Fellowship; 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 ARC Centre of Excellence) [CE110001020]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; Victoria University of Wellington via from the New Zealand Ministry of Economic Development [MED-E1799]; NVIDIA at Harvard University; Western Australian State government; International Centre for Radio Astronomy Research; Curtin University FX We thank the referee for several insightful comments that helped improve the Letter. 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. N.D.R.B. is supported by a Curtin Research Fellowship. We thank Matthew Bailes and Bryan Gaensler for useful comments, and Dick Manchester and Lawrence Toomey for help with access to the 430 MHz archival data. 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 ARC 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, a joint venture of Curtin University and The University of Western Australia, funded by the Western Australian State government. NR 48 TC 6 Z9 6 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 20 PY 2014 VL 791 IS 2 AR L32 DI 10.1088/2041-8205/791/2/L32 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KK UT WOS:000341306200014 ER PT J AU Cranmer, SR AF Cranmer, Steven R. TI SUPRATHERMAL ELECTRONS IN THE SOLAR CORONA: CAN NONLOCAL TRANSPORT EXPLAIN HELIOSPHERIC CHARGE STATES? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE conduction; solar wind; Sun: atmosphere; Sun: corona; Sun: heliosphere ID WIND ION COMPOSITION; VELOCITY DISTRIBUTION-FUNCTIONS; COMPOSITION SPECTROMETER; ATOMIC DATABASE; IN-SITU; TEMPERATURE; IONIZATION; EMISSION; DISTRIBUTIONS; GENERATION AB There have been several ideas proposed to explain how the Sun's corona is heated and how the solar wind is accelerated. Some models assume that open magnetic field lines are heated by Alfven waves driven by photospheric motions and dissipated after undergoing a turbulent cascade. Other models posit that much of the solar wind's mass and energy is injected via magnetic reconnection from closed coronal loops. The latter idea is motivated by observations of reconnecting jets and also by similarities of ion composition between closed loops and the slow wind. Wave/turbulence models have also succeeded in reproducing observed trends in ion composition signatures versus wind speed. However, the absolute values of the charge-state ratios predicted by those models tended to be too low in comparison with observations. This Letter refines these predictions by taking better account of weak Coulomb collisions for coronal electrons, whose thermodynamic properties determine the ion charge states in the low corona. A perturbative description of nonlocal electron transport is applied to an existing set of wave/turbulence models. The resulting electron velocity distributions in the low corona exhibit mild suprathermal tails characterized by "kappa" exponents between 10 and 25. These suprathermal electrons are found to be sufficiently energetic to enhance the charge states of oxygen ions, while maintaining the same relative trend with wind speed that was found when the distribution was assumed to be Maxwellian. The updated wave/turbulence models are in excellent agreement with solar wind ion composition measurements. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu FU NASA [NNX10AC11G, NNX14AG99G]; NSF SHINE program [AGS-1259519] FX The author gratefully acknowledges Jack Scudder, Ruth Esser, and John Raymond for many valuable discussions. This work was supported by NASA grants NNX10AC11G and NNX14AG99G, and NSF SHINE program grant AGS-1259519. NR 41 TC 9 Z9 9 U1 2 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 AUG 20 PY 2014 VL 791 IS 2 AR L31 DI 10.1088/2041-8205/791/2/L31 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4KK UT WOS:000341306200013 ER PT J AU Avestruz, C Lau, ET Nagai, D Vikhlinin, A AF Avestruz, Camille Lau, Erwin T. Nagai, Daisuke Vikhlinin, Alexey TI TESTING X-RAY MEASUREMENTS OF GALAXY CLUSTER OUTSKIRTS WITH COSMOLOGICAL SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: clusters: general; methods: numerical; X-rays: galaxies: clusters ID INTRACLUSTER MEDIUM; VIRIAL RADIUS; BLACK-HOLES; XMM-NEWTON; TEMPERATURE; CHANDRA; GAS; SUZAKU; MASS; SAMPLE AB The study of galaxy cluster outskirts has emerged as one of the new frontiers in extragalactic astrophysics and cosmology with the advent of new observations in X-ray and microwave. However, the thermodynamic properties and chemical enrichment of this diffuse and azimuthally asymmetric component of the intracluster medium (ICM) are still not well understood. This work, for the first time, systematically explores potential observational biases in these regions. To assess X-ray measurements of galaxy cluster properties at large radii (>R-500c), we use mock Chandra analyses of cosmological galaxy cluster simulations. The pipeline is identical to that used for Chandra observations, but the biases discussed in this paper are relevant for all X-ray observations outside of R-500c. We find the following from our analysis: (1) filament regions can contribute as much as 50% at R-200c to the emission measure; (2) X-ray temperatures and metal abundances from model fitted mock X-ray spectra in a multi-temperature ICM respectively vary to the level of 10% and 50%; (3) resulting density profiles vary to within 10% out to R-200c, and gas mass, total mass, and baryon fractions all vary to within a few percent; (4) the bias from a metal abundance extrapolated a factor of five higher than the true metal abundance results in total mass measurements biased high by 20% and total gas measurements biased low by 10%; and (5) differences in projection and dynamical state of a cluster can lead to gas density slope measurements that differ by a factor of 15% and 30%, respectively. The presented results can partially account for some of the recent gas profile measurements in cluster outskirts by, e.g., Suzaku. Our findings are pertinent to future X-ray cosmological constraints from cluster outskirts, which are least affected by non-gravitational gas physics, as well as to measurements probing gas properties in filamentary structures. C1 [Avestruz, Camille; Lau, Erwin T.; Nagai, Daisuke] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Avestruz, Camille; Lau, Erwin T.; Nagai, Daisuke] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Nagai, Daisuke] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Avestruz, C (reprint author), Yale Univ, Dept Phys, New Haven, CT 06520 USA. EM camille.avestruz@yale.edu OI Avestruz, Camille/0000-0001-8868-0810 FU NSF grant [AST-1009811]; NASA ATP grant [NNX11AE07G]; NASA Chandra grants [GO213004B, TM4-15007X]; NSF Graduate Student Research Fellowship; Yale University FX We thank the referee for useful feedback, and Elena Rasia for comments on the manuscript. This work is supported by NSF grant AST-1009811, NASA ATP grant NNX11AE07G, NASA Chandra grants GO213004B and TM4-15007X, and by the facilities and staff of the Yale University Faculty of Arts and Sciences High Performance Computing Center. C.A. acknowledges support from the NSF Graduate Student Research Fellowship and the Alan D. Bromley Fellowship from Yale University. NR 42 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 2014 VL 791 IS 2 AR 117 DI 10.1088/0004-637X/791/2/117 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400044 ER PT J AU Bai, XN AF Bai, Xue-Ning TI HALL-EFFECT-CONTROLLED GAS DYNAMICS IN PROTOPLANETARY DISKS. I. WIND SOLUTIONS AT THE INNER DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; magnetohydrodynamics (MHD); methods: numerical; protoplanetary disks; turbulence ID X-RAY IONIZATION; T-TAURI DISKS; PROTOSTELLAR ACCRETION DISCS; WEAKLY MAGNETIZED DISKS; SURFACE-LAYER ACCRETION; UNSPLIT GODUNOV METHOD; MAGNETOROTATIONAL-INSTABILITY; AMBIPOLAR DIFFUSION; NONLINEAR EVOLUTION; DRIVEN ACCRETION AB The gas dynamics of protoplanetary disks (PPDs) is largely controlled by non-ideal magnetohydrodynamic (MHD) effects including Ohmic resistivity, the Hall effect, and ambipolar diffusion. Among these the role of the Hall effect is the least explored and most poorly understood. In this series, we have included, for the first time, all three non-ideal MHD effects in a self-consistent manner to investigate the role of the Hall effect on PPD gas dynamics using local shearing-box simulations. In this first paper, we focus on the inner region of PPDs, where previous studies (Bai & Stone 2013; Bai 2013) excluding the Hall effect have revealed that the inner disk up to similar to 10AU is largely laminar, with accretion driven by a magnetocentrifugal wind. We confirm this basic picture and show that the Hall effect modifies the wind solutions depending on the polarity of the large-scale poloidal magnetic field B-0 threading the disk. When B-0 . Omega > 0, the horizontal magnetic field is strongly amplified toward the disk interior, leading to a stronger disk wind (by similar to 50% or less in terms of the wind-driven accretion rate). The enhanced horizontal field also leads to much stronger large-scale Maxwell stress (magnetic braking) that contributes to a considerable fraction of the wind-driven accretion rate. When B-0 . Omega > 0, the horizontal magnetic field is reduced, leading to a weaker disk wind (by similar to 20%) and negligible magnetic braking. Under fiducial parameters, we find that when B-0 . Omega > 0, the laminar region extends farther to similar to 10(-15)AU before the magnetorotational instability sets in, while for B-0 . Omega > 0, the laminar region extends only to similar to 3(-)5AU for a typical accretion rate of similar to 10(-8) to 10(-7) M-circle dot yr(-1). Scaling relations for the wind properties, especially the wind-driven accretion rate, are provided for aligned and anti-aligned field geometries. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 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 NR 126 TC 48 Z9 49 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 2014 VL 791 IS 2 AR 137 DI 10.1088/0004-637X/791/2/137 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400064 ER PT J AU Brittain, SD Carr, JS Najita, JR Quanz, SP Meyer, MR AF Brittain, Sean D. Carr, John S. Najita, Joan R. Quanz, Sascha P. Meyer, Michael R. TI NIR SPECTROSCOPY OF THE HAeBe STAR HD 100546. III. FURTHER EVIDENCE OF AN ORBITING COMPANION? SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: formation; stars: individual (HD 100546); techniques: spectroscopic ID HERBIG AE/BE STARS; NEAR-INFRARED SPECTROSCOPY; CO EMISSION-LINES; CIRCUMSTELLAR DISK; GAS ACCRETION; INNER DISKS; HD-100546; PLANET; MASS; SIMULATIONS AB We report high-resolution NIR spectroscopy of CO and OH emission from the Herbig Be star HD 100546. We discuss how our results bear striking resemblance to several theoretically predicted signposts of giant planet formation. The properties of the CO and OH emission lines are consistent with our earlier interpretation that these diagnostics provide indirect evidence for a companion that orbits the star close to the disk wall (at similar to 13AU). The asymmetry of the OH spectral line profiles and their lack of time variability are consistent with emission from gas in an eccentric orbit at the disk wall that is approximately stationary in the inertial frame. The time variable spectroastrometric properties of the CO upsilon = 1-0 emission line point to an orbiting source of CO emission with an emitting area similar to that expected for a circumplanetary disk (similar to 0.1AU(2)) assuming the CO emission is optically thick. We also consider a counterhypothesis to this interpretation, namely that the variable CO emission arises from a bright spot on the disk wall. We conclude with a brief suggestion of further work that can distinguish between these scenarios. C1 [Brittain, Sean D.] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29634 USA. [Carr, John S.] Naval Res Lab, Washington, DC 20375 USA. [Najita, Joan R.] Natl Optic Astron Observ, Tucson, AZ 85719 USA. [Najita, Joan R.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Quanz, Sascha P.; Meyer, Michael R.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. RP Brittain, SD (reprint author), Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29634 USA. EM sbritt@clemson.edu FU European Organization for Astronomical Research in the Southern Hemisphere, Chile [090.C-0571(A)]; National Science Foundation [AST-0954811]; Naval Research Laboratory [6.1]; Institute for Theory; Computation at the Harvard-Smithsonian Center for Astrophysics FX Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere, Chile, under program number 090.C-0571(A). S. D. B. acknowledges support for this work from the National Science Foundation under grant number AST-0954811. Basic research in infrared astronomy at the Naval Research Laboratory is supported by 6.1 base funding. J.N. gratefully acknowledges support from the Institute for Theory and Computation at the Harvard-Smithsonian Center for Astrophysics. NR 41 TC 16 Z9 16 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 2014 VL 791 IS 2 AR 136 DI 10.1088/0004-637X/791/2/136 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400063 ER PT J AU Cowperthwaite, PS Reynolds, CS AF Cowperthwaite, Philip S. Reynolds, Christopher S. TI NONLINEAR DYNAMICS OF ACCRETION DISKS WITH STOCHASTIC VISCOSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; methods: numerical ID X-RAY BINARIES; BLACK-HOLES; ACTIVE GALAXIES; FLUCTUATIONS; VARIABILITY; CYGNUS-X-1; NOISE; MODEL AB We present a nonlinear numerical model for a geometrically thin accretion disk with the addition of stochastic nonlinear fluctuations in the viscous parameter. These numerical realizations attempt to study the stochastic effects on the disk angular momentum transport. We show that this simple model is capable of reproducing several observed phenomenologies of accretion-driven systems. The most notable of these is the observed linear rms-flux relationship in the disk luminosity. This feature is not formally captured by the linearized disk equations used in previous work. A Fourier analysis of the dissipation and mass accretion rates across disk radii show coherence for frequencies below the local viscous frequency. This is consistent with the coherence behavior observed in astrophysical sources such as Cygnus X-1. C1 [Cowperthwaite, Philip S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cowperthwaite, Philip S.; Reynolds, Christopher S.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Reynolds, Christopher S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Cowperthwaite, PS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pcowpert@cfa.harvard.edu OI Cowperthwaite, Philip/0000-0002-2478-6939 FU NSF [DGE1144152]; NASA [NNX10AE41G] FX We thank Phil Uttley for helpful discussion about this work. We also thank our anonymous referee for helpful comments about this work. P.S.C. is grateful for support provided by the NSF through the Graduate Research Fellowship Program, grant DGE1144152. C.S.R. thanks NASA for funding under the Astrophysical Theory Program grant NNX10AE41G. NR 19 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 AUG 20 PY 2014 VL 791 IS 2 AR 126 DI 10.1088/0004-637X/791/2/126 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400053 ER PT J AU Dai, YS Elvis, M Bergeron, J Fazio, GG Huang, JS Wilkes, BJ Willmer, CNA Omont, A Papovich, C AF Dai, Y. Sophia Elvis, Martin Bergeron, Jacqueline Fazio, Giovanni G. Huang, Jia-Sheng Wilkes, Belinda J. Willmer, Christopher N. A. Omont, Alain Papovich, Casey TI MID-INFRARED-SELECTED QUASARS. I. VIRIAL BLACK HOLE MASS AND EDDINGTON RATIOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: active; galaxies: high-redshift; galaxies: Seyfert; infrared: galaxies; quasars: general; quasars: supermassive black holes ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; RADIUS-LUMINOSITY RELATIONSHIP; BROAD-LINE REGION; SPITZER-SPACE-TELESCOPE; FIBER-FED SPECTROGRAPH; GALAXY REDSHIFT SURVEY; QUASI-STELLAR OBJECTS; 7TH DATA RELEASE AB We provide a catalog of 391 mid-infrared-selected (MIR; 24 mu m) broad-emission-line (BEL; type 1) quasars in the 22 deg(2) SWIRE Lockman Hole field. This quasar sample is selected in the MIR from Spitzer MIPS with S-24 > 400 mu Jy, jointly with an optical magnitude limit of r (AB) < 22.5 for broad line identification. The catalog is based on MMT and Sloan Digital Sky Survey (SDSS) spectroscopy to select BEL quasars, extending the SDSS coverage to fainter magnitudes and lower redshifts, and recovers a more complete quasar population. The MIR-selected quasar sample peaks at z similar to 1.4 and recovers a significant and constant (20%) fraction of extended objects with SDSS photometry across magnitudes, which were not included in the SDSS quasar survey dominated by point sources. This sample also recovers a significant population of z < 3 quasars at i > 19.1. We then investigate the continuum luminosity and line profiles of these MIR quasars, and estimate their virial black hole masses and the Eddington ratios. The supermassive black hole mass shows evidence of downsizing, although the Eddington ratios remain constant at 1 < z < 4. Compared to point sources in the same redshift range, extended sources at z < 1 show systematically lower Eddington ratios. The catalog and spectra are publicly available online. C1 [Dai, Y. Sophia; Elvis, Martin; Fazio, Giovanni G.; Huang, Jia-Sheng; Wilkes, Belinda J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dai, Y. Sophia] CALTECH, IPAC, Pasadena, CA 91125 USA. [Bergeron, Jacqueline; Omont, Alain] CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Willmer, Christopher N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Papovich, Casey] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. RP Dai, YS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ydai@caltech.edu OI Papovich, Casey/0000-0001-7503-8482; Wilkes, Belinda/0000-0003-1809-2364 FU Smithsonian Astrophysical Observatory (SAO) through the SAO Predoctoral Fellowship; 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 FX Y.S.D. acknowledges support from the Smithsonian Astrophysical Observatory (SAO) through the SAO Predoctoral Fellowship. We thank the anonymous referee for suggestions that led to the improvement of the manuscript. We thank Yue Shen for sharing the spectral measurement code, and Richard Cool for sharing and supporting of the HSRED reduction code.; Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This work is also based partly on observations made with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. 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/. NR 119 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 2014 VL 791 IS 2 AR 113 DI 10.1088/0004-637X/791/2/113 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400040 ER PT J AU Dawson, RI Johnson, JA Fabrycky, DC Foreman-Mackey, D Murray-Clay, RA Buchhave, LA Cargile, PA Clubb, KI Fulton, BJ Hebb, L Howard, AW Huber, D Shporer, A Valenti, JA AF Dawson, Rebekah I. Johnson, John Asher Fabrycky, Daniel C. Foreman-Mackey, Daniel Murray-Clay, Ruth A. Buchhave, Lars A. Cargile, Phillip A. Clubb, Kelsey I. Fulton, Benjamin J. Hebb, Leslie Howard, Andrew W. Huber, Daniel Shporer, Avi Valenti, Jeff A. TI LARGE ECCENTRICITY, LOW MUTUAL INCLINATION: THE THREE-DIMENSIONAL ARCHITECTURE OF A HIERARCHICAL SYSTEM OF GIANT PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems ID TRANSIT TIMING VARIATIONS; CANDIDATE HOST STARS; CLOSE-IN PLANETS; HOT JUPITERS; LIGHT CURVES; DYNAMICAL INSTABILITIES; ORBITAL EVOLUTION; ERROR-CORRECTION; V-ANDROMEDAE; STELLAR SPIN AB We establish the three-dimensional architecture of the Kepler-419 (previously KOI-1474) system to be eccentric yet with a low mutual inclination. Kepler-419b is a warm Jupiter at semi-major axis a = 0.370(-0.006)(+0.007) AU with a large eccentricity (e = 0.85(-0.07)(+0.08)) measured via the "photoeccentric effect." It exhibits transit timing variations (TTVs) induced by the non-transiting Kepler-419c, which we uniquely constrain to be a moderately eccentric (e = 0.184 +/- 0.002), hierarchically separated (a = 1.68 +/- 0.03 AU) giant planet (7.3 +/- 0.4 M-Jup). We combine 16 quarters of Kepler photometry, radial-velocity (RV) measurements from the HIgh Resolution Echelle Spectrometer on Keck, and improved stellar parameters that we derive from spectroscopy and asteroseismology. From the RVs, we measure the mass of the inner planet to be 2.5 +/- 0.3 M-Jup and confirm its photometrically measured eccentricity, refining the value to e = 0.83 +/- 0.01. The RV acceleration is consistent with the properties of the outer planet derived from TTVs. We find that despite their sizable eccentricities, the planets are coplanar to within 9(-6)(+8) degrees, and therefore the inner planet's large eccentricity and close-in orbit are unlikely to be the result of Kozai migration. Moreover, even over many secular cycles, the inner planet's periapse is most likely never small enough for tidal circularization. Finally, we present and measure a transit time and impact parameter from four simultaneous ground-based light curves from 1 m class telescopes, demonstrating the feasibility of ground-based follow-up of Kepler giant planets exhibiting large TTVs. C1 [Dawson, Rebekah I.; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Johnson, John Asher; Murray-Clay, Ruth A.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60664 USA. [Foreman-Mackey, Daniel] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Cargile, Phillip A.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Fulton, Benjamin J.; Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hebb, Leslie] Hobart & William Smith Coll, Dept Phys, Geneva, NY 14456 USA. [Huber, Daniel] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Huber, Daniel] SETI Inst, Mountain View, CA 94043 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Valenti, Jeff A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Dawson, RI (reprint author), Univ Calif Berkeley, Dept Astron, Hearst Field Annex B-20, Berkeley, CA 94720 USA. EM rdawson@berkeley.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Buchhave, Lars A./0000-0003-1605-5666; Fabrycky, Daniel/0000-0003-3750-0183 FU Alfred P. Sloan and David and Lucile Packard foundations; NASA [NNX12AI50G, NNX14AB92G]; National Science Foundation [IIS-1124794]; NASA Postdoctoral Program at Ames Research Center; NASA Science Mission directorate; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; W. M. Keck Foundation FX We are grateful to the referee for a helpful report. We thank David Hogg, Gongjie Li, Katherine Deck, Joshua Carter, Guillaume Hebrard, Boas Katz, Yoram Lithwick, Smadar Naoz, Eugene Chiang, Scott Tremaine, Ellen Price, Leslie Rogers, Eric Ford, Cristobal Petrovich, and Doug Lin for helpful discussions. R. I. D. gratefully acknowledges the Miller Institute for Basic Research in Science, University of California Berkeley. J. A. J. is grateful for the generous grant support provided by the Alfred P. Sloan and David and Lucile Packard foundations. D. F. M. is supported by NASA under grant NNX12AI50G and the National Science Foundation under grant IIS-1124794. D. H. acknowledges support by an appointment to the NASA Postdoctoral Program at Ames Research Center administered by Oak Ridge Associated Universities, and NASA Grant NNX14AB92G issued through the Kepler Participating Scientist Program. This work benefited from the Summer Program on Modern Statistical and Computational Methods for Analysis of Kepler Data, held at SAMSI, Research Triangle Park, NC in 2013 June.; 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 Kepler Team for their extensive efforts in producing such high-quality data. Some of the data presented in this paper were 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 NNX09AF08G and by other grants and contracts.; We are very grateful to Geoff Marcy and Howard Isaacson for contributing to the radial-velocity observations of Kepler-419. J. A. J. is grateful for Keck/HIRES time allocated through the Caltech Time Allocation Committee for some of the spectra used herein. The spectroscopic and radial-velocity measurements 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 gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Scott Dahm, Greg Doppman, Hien Tran, and Grant Hill for support of HIRES and GregWirth for support of remote observing. We extend special thanks to those of Hawai'ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible. NR 87 TC 21 Z9 21 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 2014 VL 791 IS 2 AR 89 DI 10.1088/0004-637X/791/2/89 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400016 ER PT J AU Foster, JB Arce, HG Kassis, M Sanhueza, P Jackson, JM Finn, SC Offner, S Sakai, T Sakai, N Yamamoto, S Guzman, AE Rathborne, JM AF Foster, Jonathan B. Arce, Hector G. Kassis, Marc Sanhueza, Patricio Jackson, James M. Finn, Susanna C. Offner, Stella Sakai, Takeshi Sakai, Nami Yamamoto, Satoshi Guzman, Andres E. Rathborne, Jill M. TI DISTRIBUTED LOW-MASS STAR FORMATION IN THE IRDC G34.43+00.24 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: jets and outflows; stars: low-mass; stars: massive; stars: pre-main sequence; stars: protostars ID INFRARED DARK CLOUD; YOUNG STELLAR OBJECTS; WIDE-FIELD CAMERA; MOLECULAR OUTFLOWS; MSXDC G034.43+00.24; PHOTOMETRIC SYSTEM; CLUSTER FORMATION; FORMING REGION; GALACTIC PLANE; SIO EMISSION AB We have used deep near-infrared observations with adaptive optics to discover a distributed population of low-mass protostars within the filamentary Infrared Dark Cloud G34.43+00.24. We use maps of dust emission at multiple wavelengths to determine the column density structure of the cloud. In combination with an empirically verified model of the magnitude distribution of background stars, this column density map allows us to reliably determine overdensities of red sources that are due to embedded protostars in the cloud. We also identify protostars through their extended emission in the K band, which comes from excited H-2 in protostellar outflows or reflection nebulosity. We find a population of distributed low-mass protostars, suggesting that low-mass protostars may form earlier than, or contemporaneously with, high-mass protostars in such a filament. The low-mass protostellar population may also produce the narrow line-width SiO emission observed in some clouds without high-mass protostars. Finally, we use a molecular line map of the cloud to determine the virial parameter per unit length along the filament and find that the highest mass protostars form in the most bound portion of the filament, as suggested by theoretical models. C1 [Foster, Jonathan B.] Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Arce, Hector G.; Offner, Stella] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Kassis, Marc] WM Keck Observ, Kamuela, HI 96743 USA. [Sanhueza, Patricio; Jackson, James M.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Finn, Susanna C.] UMASS Lowell, Ctr Atmospher Res, Lowell, MA 01854 USA. [Sakai, Takeshi] Univ Electrocommun, Grad Sch Informat & Engn, Chofu, Tokyo 1828585, Japan. [Sakai, Nami; Yamamoto, Satoshi] Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. [Guzman, Andres E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rathborne, Jill M.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Foster, JB (reprint author), Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. EM jonathan.b.foster@yale.edu RI SAKAI, NAMI/G-4893-2014; Sakai, Nami/N-7438-2015; OI SAKAI, NAMI/0000-0002-3297-4497; Sakai, Nami/0000-0002-3297-4497; Guzman, Andres/0000-0003-0990-8990 FU NASA [NNX12AI55G, NNX10AD68G]; ALMA [2011.0.00656] FX A.E.G. acknowledges support from NASA grants NNX12AI55G and NNX10AD68G. This research made use of Astropy, a community-developed core Python package for astronomy (Astropy Collaboration et al. 2013). This research has made use of NASA's Astrophysics Data System. This research made use of APLpy, an open-source plotting package for Python hosted at http://aplpy.github.com. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The authors thank the staff at the Green Bank Telescope in particular for their assistance during observations with the KFPA. This paper makes use of the following ALMA data: ADS/JAO. ALMA# 2011.0.00656. 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 65 TC 11 Z9 11 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 2014 VL 791 IS 2 AR 108 DI 10.1088/0004-637X/791/2/108 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400035 ER PT J AU Ko, JW Hwang, HS Im, MS Le Borgne, D Lee, JC Elbaz, D AF Ko, Jongwan Hwang, Ho Seong Im, Myungshin Le Borgne, Damien Lee, Jong Chul Elbaz, David TI TRACING RECENT STAR FORMATION OF RED EARLY-TYPE GALAXIES OUT TO z similar to 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: stellar content; infrared: galaxies ID ORIGINS DEEP SURVEY; DIGITAL SKY SURVEY; GOODS-SOUTH FIELD; COLOR-MAGNITUDE RELATION; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; EXTRAGALACTIC LEGACY SURVEY; NEAR-INFRARED SPECTROSCOPY; SUPERMASSIVE BLACK-HOLES; REDSHIFT SURVEY AB We study the mid-infrared (IR) excess emission of early-type galaxies (ETGs) on the red sequence at z < 1 using a spectroscopic sample of galaxies in the fields of Great Observatories Origins Deep Survey (GOODS). In the mass-limited sample of 1025 galaxies with M-star > 10(10.5) M-circle dot and 0.4 < z < 1.05, we identify 696 Spitzer 24 mu m detected (above the 5 sigma) galaxies and find them to have a wide range of NUV-r and r-[12 mu m] colors despite their red optical u-r colors. Even in the sample of very massive ETGs on the red sequence with M-star > 10(11.2) M-circle dot, more than 18% show excess emission over the photospheric emission in the mid-IR. The combination with the results of red ETGs in the local universe suggests that the recent star formation is not rare among quiescent, red ETGs at least out to z similar to 1 if the mid-IR excess emission results from intermediate-age stars or/and from low-level ongoing star formation. Our color-color diagram including near-UV and mid-IR emissions are efficient not only for identifying ETGs with recent star formation, but also for distinguishing quiescent galaxies from dusty star-forming galaxies. C1 [Ko, Jongwan; Lee, Jong Chul] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Im, Myungshin] Seoul Natl Univ, Ctr Explorat Origin Univ Astron Program, Dept Phys & Astron, Seoul, South Korea. [Le Borgne, Damien] Univ Paris 06, Sorbonne Univ, Inst Astrophys Paris, UMR 7095, F-75005 Paris, France. [Le Borgne, Damien] CNRS, Inst Astrophys Paris, UMR 7095, F-75005 Paris, France. [Elbaz, David] Univ Paris Diderot, CNRS, CE Saclay, CEA,DSM,Irfu,Lab AIM Paris Saclay, F-91191 Gif sur Yvette, France. RP Ko, JW (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM jwko@kasi.re.kr OI Im, Myungshin/0000-0002-8537-6714 FU National Research Foundation of Korea (NRF) - Korea government (MSIP) [2008-0060544]; French National Agency for Research (ANR) [ANR-09-BLAN-0224] FX J. K. and J. C. L. are the members of Dedicated Researchers for Extragalactic AstronoMy (DREAM) in Korea Astronomy and Space Science Institute (KASI). H. S. H. acknowledges the Smithsonian Institution for the support of his post-doctoral fellowship. M. I. acknowledges the support from the National Research Foundation of Korea (NRF) grant, No. 2008-0060544, funded by the Korea government (MSIP). D. L. B. acknowledges the French National Agency for Research (ANR) for their support (ANR-09-BLAN-0224). NR 123 TC 4 Z9 4 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 AUG 20 PY 2014 VL 791 IS 2 AR 134 DI 10.1088/0004-637X/791/2/134 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400061 ER PT J AU Lee, SH Patnaude, DJ Ellison, DC Nagataki, S Slane, PO AF Lee, Shiu-Hang Patnaude, Daniel J. Ellison, Donald C. Nagataki, Shigehiro Slane, Patrick O. TI REVERSE AND FORWARD SHOCK X-RAY EMISSION IN AN EVOLUTIONARY MODEL OF SUPERNOVA REMNANTS UNDERGOING EFFICIENT DIFFUSIVE SHOCK ACCELERATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; ISM: supernova remnants; shock waves ID NONLINEAR PARTICLE-ACCELERATION; ION TEMPERATURE EQUILIBRATION; BROAD-BAND EMISSION; EARTHS BOW SHOCK; HYDRO-NEI MODEL; COLLISIONLESS SHOCKS; IA SUPERNOVA; NONEQUILIBRIUM IONIZATION; LINE EMISSION; EJECTA AB We present new models for the forward and reverse shock thermal X-ray emission from core-collapse and Type Ia supernova remnants (SNRs) that include the efficient production of cosmic rays (CR) via nonlinear diffusive shock acceleration (DSA). Our CR-hydro-NEI code takes into account non-equilibrium ionization, hydrodynamic effects of efficient CR production on the SNR evolution, and collisional temperature equilibration among heavy ions and electrons in both the shocked supernova (SN) ejecta and the shocked circumstellar material. While X-ray emission is emphasized here, our code self-consistently determines both thermal and non-thermal broadband emission from radio to TeV energies. We include Doppler broadening of the spectral lines by thermal motions of the ions and by the remnant expansion. We study, in general terms, the roles that the ambient environment, progenitor models, temperature equilibration, and processes related to DSA have on the thermal and non-thermal spectra. The study of X-ray line emission from young SNRs is a powerful tool for determining specific SN elemental contributions and for providing critical information that helps to understand the type and energetics of the explosion, the composition of the ambient medium in which the SN exploded, and the ionization and dynamics of the hot plasma in the shocked SN ejecta and interstellar medium. With the approaching launch of the next-generation X-ray satellite Astro-H, observations of spectral lines with unprecedented high resolution will become a reality. Our self-consistent calculations of the X-ray spectra from various progenitors will help interpret future observations of SNRs. C1 [Lee, Shiu-Hang] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Lee, Shiu-Hang; Nagataki, Shigehiro] RIKEN, Astrophys Big Bang Lab, Wako, Saitama 3510198, Japan. [Patnaude, Daniel J.; Slane, Patrick O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. 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; don_ellison@ncsu.edu; shigehiro.nagataki@riken.jp; slane@cfa.harvard.edu FU NASA [NAS8-03060, NNX11AE03G]; Japan Society for the Promotion of Science [23340069, 24.02022, 25.03786, 25610056]; [2503018] FX We thank C. Badenes, M. Hashimoto, A. Heger, T. Nozawa, M. Ono, and T. Shigeyama for generously providing SN progenitor and nucleosynthesis data for the completion of this work. We also express special thanks to C. Badenes and the anonymous referees for their valuable comments and suggestions for the improvement of the manuscript. S.-H.L. acknowledges support from Grants-in-Aid for Foreign JSPS Fellow (No. 2503018). D.J.P. and P.O.S. acknowledge support from NASA contract NAS8-03060. D. C. E. acknowledges support from NASA grant NNX11AE03G. S.N. acknowledges support from the Japan Society for the Promotion of Science (Nos. 23340069, 24.02022, 25.03786, and 25610056). NR 65 TC 4 Z9 4 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 2014 VL 791 IS 2 AR 97 DI 10.1088/0004-637X/791/2/97 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400024 ER PT J AU Li, GJ Naoz, S Holman, M Loeb, A AF Li, Gongjie Naoz, Smadar Holman, Matt Loeb, Abraham TI CHAOS IN THE TEST PARTICLE ECCENTRIC KOZAI-LIDOV MECHANISM SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; celestial mechanics ID BLACK-HOLE BINARIES; HIERARCHICAL 3-BODY SYSTEMS; TRIPLE STARS; GLOBULAR-CLUSTERS; ORBITAL EVOLUTION; STELLAR BINARIES; TIDAL FRICTION; HOT JUPITERS; DYNAMICS; PERTURBATIONS AB The Kozai-Lidov mechanism can be applied to a vast variety of astrophysical systems involving hierarchical three-body systems. Here, we study the Kozai-Lidov mechanism systematically in the test particle limit at the octupole level of approximation. We investigate the chaotic and quasi-periodic orbital evolution by studying the surfaces of section and the Lyapunov exponents. We find that the resonances introduced by the octupole level of approximation cause orbits to flip from prograde to retrograde and back as well as cause significant eccentricity excitation, and chaotic behavior occurs when the mutual inclination between the inner and the outer binary is high. We characterize the parameter space that allows large amplitude oscillations in eccentricity and inclination. C1 [Li, Gongjie; Naoz, Smadar; Holman, Matt; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 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 OI Naoz, Smadar/0000-0002-9802-9279 FU NSF [AST-1312034] FX We thank Konstantin Batygin for helpful remarks. This work was supported in part by NSF grant AST-1312034 (for A. L.). NR 39 TC 24 Z9 24 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 2014 VL 791 IS 2 AR 86 DI 10.1088/0004-637X/791/2/86 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400013 ER PT J AU Onofrio, R Wegner, GA AF Onofrio, Roberto Wegner, Gary A. TI SEARCH FOR HIGGS SHIFTS IN WHITE DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; gravitation; white dwarfs ID FOCUS IMAGING SPECTROGRAPH; MODEL ATMOSPHERE ANALYSIS; AFRICAN LARGE TELESCOPE; COSMOLOGICAL CONSTANT; SCALAR FIELD; MOLECULAR BANDS; BOSON; MASS; PROCYON; CARBON AB We report on a search for differential shifts between electronic and vibronic transitions in carbon-rich white dwarfs BPM 27606 and Procyon B. The absence of differential shifts within the spectral resolution and taking into account systematic effects such as space motion and pressure shifts allows us to set the first upper bound of astrophysical origin on the coupling between the Higgs field and the Kreschmann curvature invariant. Our analysis provides the basis for a more general methodology to derive bounds to the coupling of long-range scalar fields to curvature invariants in an astrophysical setting complementary to the ones available from high-energy physics or table-top experiments. C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Wegner, Gary A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Via Marzolo 8, I-35131 Padua, Italy. EM onofrior@gmail.com; gary.a.wegner@dartmouth.edu FU National Science Foundation through Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University; Smithsonian Astrophysical Laboratory FX We are grateful to Susanne Yelin for a critical reading of the manuscript. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT) under proposals 2013-1-DC-001 and 2014-1-DC-001. Additional data used observations made with the NASA/ESA Hubble Space Telescope, and were obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). This work was also partially funded by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University, and the Smithsonian Astrophysical Laboratory. NR 75 TC 3 Z9 3 U1 0 U2 9 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 2014 VL 791 IS 2 AR 125 DI 10.1088/0004-637X/791/2/125 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400052 ER PT J AU Paterno-Mahler, R Randall, SW Bulbul, E Andrade-Santos, F Blanton, EL Jones, C Murray, S Johnson, RE AF Paterno-Mahler, R. Randall, S. W. Bulbul, E. Andrade-Santos, F. Blanton, E. L. Jones, C. Murray, S. Johnson, R. E. TI MERGER SIGNATURES IN THE GALAXY CLUSTER A98 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A98); galaxies: interactions; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID X-RAY-ABSORPTION; DEEP CHANDRA OBSERVATION; XMM-NEWTON OBSERVATIONS; ACTIVE GALACTIC NUCLEI; COLD FRONTS; RICH CLUSTERS; SCALING RELATION; NEARBY CLUSTERS; PERSEUS CLUSTER; RADIO GALAXIES AB We present results from Chandra and XMM-Newton observations of Abell 98 (A98), a galaxy cluster with three major components: a relatively bright subcluster to the north (A98N), a disturbed subcluster to the south (A98S), and a fainter subcluster to the far south (A98SS). We find evidence for surface brightness and temperature asymmetries in A98N consistent with a shock-heated region to the south, which could be created by an early stage merger between A98N and A98S. Deeper observations are required to confirm this result. We also find that A98S has an asymmetric core temperature structure, likely due to a separate ongoing merger. Evidence for this is also seen in optical data. A98S hosts a wide-angle tail radio source powered by a central active galactic nucleus (AGN). We find evidence for a cavity in the intracluster medium that has been evacuated by one of the radio lobes, suggesting that AGN feedback is operating in this system. Examples of cavities in non-cool core clusters are relatively rare. The three subclusters lie along a line in projection, suggesting the presence of a large-scale filament. We observe emission along the filament between A98N and A98S, and a surface brightness profile shows emission consistent with the overlap of the subcluster extended gas halos. We find the temperature of this region is consistent with the temperature of the gas at similar radii outside this bridge region. Lastly, we examine the cluster dynamics using optical data. We conclude A98N and A98S are likely bound to one another with a 67% probability, while A98S and A98SS are not bound at a high level of significance. C1 [Paterno-Mahler, R.; Blanton, E. L.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Paterno-Mahler, R.; Blanton, E. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Randall, S. W.; Bulbul, E.; Andrade-Santos, F.; Jones, C.; Murray, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Johnson, R. E.] Gettysburg Coll, Dept Phys, Gettysburg, PA 17325 USA. RP Paterno-Mahler, R (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM rachelpm@bu.edu; rachelpm@bu.edu; ebulbul@head.cfa.harvard.edu; fsantos@cfa.harvard.edu; eblanton@bu.edu; cjones@cfa.harvard.edu; ssm@pha.jhu.edu; rjohnson@gettysburg.edu OI Randall, Scott/0000-0002-3984-4337 FU ADP grant [NNX13AE83G]; National Science Foundation [NSF AST-1313229]; Chandra X-ray Center through NASA [NAS8-03060]; Smithsonian Institution; Chandra X-Ray Observatory grant [GO2-13161X]; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U. S. Department of Energy Office of Science FX RPM was partially supported by ADP grant NNX13AE83G and partially supported by the National Science Foundation through NSF AST-1313229. S.W.R. was supported by the Chandra X-ray Center through NASA contract NAS8-03060, the Smithsonian Institution, and by Chandra X-Ray Observatory grant GO2-13161X.; 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/. NR 62 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 20 PY 2014 VL 791 IS 2 AR 104 DI 10.1088/0004-637X/791/2/104 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400031 ER PT J AU Zahid, HJ Dima, GI Kudritzki, RP Kewley, LJ Geller, MJ Hwang, HS Silverman, JD Kashino, D AF Zahid, H. Jabran Dima, Gabriel I. Kudritzki, Rolf-Peter Kewley, Lisa J. Geller, Margaret J. Hwang, Ho Seong Silverman, John D. Kashino, Daichi TI THE UNIVERSAL RELATION OF GALACTIC CHEMICAL EVOLUTION: THE ORIGIN OF THE MASS-METALLICITY RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift ID STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; H II REGIONS; STELLAR MASS; QUANTITATIVE SPECTROSCOPY; FORMATION RATES; FUNDAMENTAL RELATION; REDSHIFT EVOLUTION; ABUNDANCE RATIOS; COSMIC EVOLUTION AB We examine the mass-metallicity relation for z less than or similar to 1.6. The mass-metallicity relation follows a steep slope with a turnover, or "knee," at stellar masses around 10(10) M-circle dot. At stellar masses higher than the characteristic turnover mass, the mass-metallicity relation flattens as metallicities begin to saturate. We show that the redshift evolution of the mass-metallicity relation depends only on the evolution of the characteristic turnover mass. The relationship between metallicity and the stellar mass normalized to the characteristic turnover mass is independent of redshift. We find that the redshift-independent slope of the mass-metallicity relation is set by the slope of the relationship between gas mass and stellar mass. The turnover in the mass-metallicity relation occurs when the gas-phase oxygen abundance is high enough that the amount of oxygen locked up in low-mass stars is an appreciable fraction of the amount of oxygen produced by massive stars. The characteristic turnover mass is the stellar mass, where the stellar-to-gas mass ratio is unity. Numerical modeling suggests that the relationship between metallicity and the stellar-to-gas mass ratio is a redshift-independent, universal relationship followed by all galaxies as they evolve. The mass-metallicity relation originates from this more fundamental universal relationship between metallicity and the stellar-to-gas mass ratio. We test the validity of this universal metallicity relation in local galaxies where stellar mass, metallicity, and gas mass measurements are available. The data are consistent with a universal metallicity relation. We derive an equation for estimating the hydrogen gas mass from measurements of stellar mass and metallicity valid for z less than or similar to 1.6 and predict the cosmological evolution of galactic gas masses. C1 [Zahid, H. Jabran; Dima, Gabriel I.; Kudritzki, Rolf-Peter] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Zahid, H. Jabran; Geller, Margaret J.; Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kewley, Lisa J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Silverman, John D.] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan. [Kashino, Daichi] Nagoya Univ, Div Particle & Astrophys Sci, Nagoya, Aichi 4648602, Japan. RP Zahid, HJ (reprint author), Univ Hawaii Manoa, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. OI Geller, Margaret/0000-0002-9146-4876; Kashino, Daichi/0000-0001-9044-1747 FU NSF grants [AST-95-09298, AST-0071048, AST-0507428, AST-0507483]; NASA LTSA grant [NNG04GC89G]; National Science Foundation [AST-1008798]; 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; W. M. Keck Foundation; NSF [AST-95-09298, AST-0071048, AST-0507428, AST-0507483]; NASA LTSA [NNG04GC89G] FX We thank Molly Peeples, Paul Torrey, Manolis Papastergis, and Charlie Conroy for useful discussions contributing to this work. This work was supported by the National Science Foundation under grant AST-1008798 to R. P. K. 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. Mahalo.; 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/.; 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 Galaxy Redshift Survey has been provided by NSF grants AST-95-09298, AST-0071048, AST-0507428, and AST-0507483 as well as NASA LTSA grant NNG04GC89G. NR 114 TC 76 Z9 76 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 20 PY 2014 VL 791 IS 2 AR 130 DI 10.1088/0004-637X/791/2/130 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM7EV UT WOS:000340028400057 ER PT J AU Wang, F McShea, WJ Wang, DJ Li, S Zhao, Q Wang, H Lu, Z AF Wang, Fang McShea, William J. Wang, Dajun Li, Sheng Zhao, Qing Wang, Hao Lu, Zhi TI Evaluating Landscape Options for Corridor Restoration between Giant Panda Reserves SO PLOS ONE LA English DT Article ID FOPING-NATURE-RESERVE; WOLONG NATURE-RESERVE; HABITAT SUITABILITY; MINSHAN MOUNTAINS; CHINA; CONSERVATION; SCENARIO; MODELS; REGION; FOREST AB The establishment of corridors can offset the negative effects of habitat fragmentation by connecting isolated habitat patches. However, the practical value of corridor planning is minimal if corridor identification is not based on reliable quantitative information about species-environment relationships. An example of this need for quantitative information is planning for giant panda conservation. Although the species has been the focus of intense conservation efforts for decades, most corridor projects remain hypothetical due to the lack of reliable quantitative researches at an appropriate spatial scale. In this paper, we evaluated a framework for giant panda forest corridor planning. We linked our field survey data with satellite imagery, and conducted species occupancy modelling to examine the habitat use of giant panda within the potential corridor area. We then conducted least-cost and circuit models to identify potential paths of dispersal across the landscape, and compared the predicted cost under current conditions and alternative conservation management options considered during corridor planning. We found that due to giant panda's association with areas of low elevation and flat terrain, human infrastructures in the same area have resulted in corridor fragmentation. We then identified areas with high potential to function as movement corridors, and our analysis of alternative conservation scenarios showed that both forest/bamboo restoration and automobile tunnel construction would significantly improve the effectiveness of corridor, while residence relocation would not significantly improve corridor effectiveness in comparison with the current condition. The framework has general value in any conservation activities that anticipate improving habitat connectivity in human modified landscapes. Specifically, our study suggested that, in this landscape, automobile tunnels are the best means to remove current barriers to giant panda movements caused by anthropogenic interferences. C1 [Wang, Fang; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Wang, Fang; Wang, Dajun; Li, Sheng; Wang, Hao; Lu, Zhi] Peking Univ, Sch Life Sci, Beijing 100871, Peoples R China. [Zhao, Qing] Colorado State Univ, Dept Fish Wildlife & Conservat Biol, Ft Collins, CO USA. RP Wang, F (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM wangf@si.edu RI Zhao, Qing/K-3486-2015 OI Zhao, Qing/0000-0003-2759-1114 FU Ocean Park Conservation Foundation, Hong Kong (OPCFHK); Conservation International (CI) FX This research was funded by Ocean Park Conservation Foundation, Hong Kong (OPCFHK, www.opcf.org.hk) and Conservation International (CI, www.conservation.org). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 3 Z9 4 U1 10 U2 121 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 18 PY 2014 VL 9 IS 8 AR e105086 DI 10.1371/journal.pone.0105086 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO4JF UT WOS:000341302700067 PM 25133757 ER PT J AU Baek, KH Kim, JH Park, RJ Chance, K Kurosu, TP AF Baek, K. H. Kim, Jae H. Park, Rokjin J. Chance, Kelly Kurosu, Thomas P. TI Validation of OMI HCHO data and its analysis over Asia SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE OMI HCHO; EOF; SVD; Megacity pollution; Biomass burning ID ISOPRENE EMISSIONS; SATELLITE-OBSERVATIONS; COLUMN OBSERVATIONS; NORTH-AMERICA; FORMALDEHYDE; VARIABILITY; SPACE; AIR; OZONE; CHEMISTRY AB OMI HCHO is validated over the continental US (CONUS), and used to analyze regional sources in Northeast Asia (NA) and Southeast Asia (SA). OMI HCHO Version 2.0 data show unrealistic trends, which prompted the production of a corrected OMI HCHO data set. EOF and SVD are utilized to compare the spatial and temporal variability between OMI HCHO against GOME and SCIAMACHY, and against GEOS-Chem. CONUS HCHO chemistry is well studied; its concentrations are greatest in the southeastern US with annual cycle maximums corresponding to the summer vegetation. The corrected OMI HCHO agrees with this understanding as well as with the other sensors measurements and has no unrealistic trends. In NA the annual cycle is super-posed by extremely large concentrations in polluted mega-cities. The other sensors generally agree with NA's OMI HCHO regional distribution, but megacity signal is not seen in GEOS-Chem. Our study supports the findings proposed by others that the emission inventory used in GEOS-Chem significantly underestimates anthropogenic influence on HCHO emission over megacities. The persistent mega-city signal is also present in SA. In SA the spatial and temporal patterns of OMI HCHO show a maximum in the dry season. The patterns are in remarkably good agreement with fire counts, which illustrates that the variability of HCHO over SA is strongly influenced by biomass burning. The corrected OMI HCHO data has realistic trends, conforms to well-known sources over CONUS, and has shown a stationary large concentration over polluted Asian mega-cities, and a widespread biomass burning in SA. (C) 2014 Elsevier B.V. All rights reserved. C1 [Baek, K. H.; Kim, Jae H.] Pusan Natl Univ, Dept Atmospher Sci, Pusan, South Korea. [Park, Rokjin J.] Seoul Natl Univ, Sch Earth & Environm Sci, Seoul, South Korea. [Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Kurosu, Thomas P.] CA Inst Technol, Jet Prop Lab, Pasadena, CA USA. RP Kim, JH (reprint author), Pusan Natl Univ, Dept Atoms Sci, Room 525-1, Pusan, South Korea. EM jaekim@pusan.ac.kr RI Chem, GEOS/C-5595-2014; Park, Rokjin/I-5055-2012; OI Park, Rokjin/0000-0001-8922-0234; Chance, Kelly/0000-0002-7339-7577 FU National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology [2012R1A1A2040757] FX This research was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (2012R1A1A2040757). NR 44 TC 0 Z9 0 U1 2 U2 19 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD AUG 15 PY 2014 VL 490 BP 93 EP 105 DI 10.1016/j.scitotenv.2014.04.108 PG 13 WC Environmental Sciences SC Environmental Sciences & Ecology GA AY0NT UT WOS:000347293800011 PM 24840284 ER PT J AU Liu, Q Liu, H Wen, J Peterson, PM AF Liu, Qing Liu, Huan Wen, Jun Peterson, Paul M. TI Infrageneric Phylogeny and Temporal Divergence of Sorghum (Andropogoneae, Poaceae) Based on Low-Copy Nuclear and Plastid Sequences SO PLOS ONE LA English DT Article ID GENUS SORGHUM; PHOSPHOENOLPYRUVATE CARBOXYLASE; ALLOTETRAPLOID ORIGIN; C-4 PHOTOSYNTHESIS; CHLOROPLAST GENOME; CLIMATIC-CHANGE; EVOLUTIONARY; GRASSES; BICOLOR; PLANT AB The infrageneric phylogeny and temporal divergence of Sorghum were explored in the present study. Sequence data of two low-copy nuclear (LCN) genes, phosphoenolpyruvate carboxylase 4 (Pepc4) and granule-bound starch synthase I (GBSSI), from 79 accessions of Sorghum plus Cleistachne sorghoides together with those from outgroups were used for maximum likelihood (ML) and Bayesian inference (BI) analyses. Bayesian dating based on three plastid DNA markers (ndhA intron, rpl32-trnL, and rps16 intron) was used to estimate the ages of major diversification events in Sorghum. The monophyly of Sorghum plus Cleistachne sorghoides (with the latter nested within Sorghum) was strongly supported by the Pepc4 data using BI analysis, and the monophyly of Sorghum was strongly supported by GBSSI data using both ML and BI analyses. Sorghum was divided into three clades in the Pepc4, GBSSI, and plastid phylograms: the subg. Sorghum lineage; the subg. Parasorghum and Stiposorghum lineage; and the subg. Chaetosorghum and Heterosorghum lineage. Two LCN homoeologous loci of Cleistachne sorghoides were first discovered in the same accession. Sorghum arundinaceum, S. bicolor, S. x drummondii, S. propinquum, and S. virgatum were closely related to S. x almum in the Pepc4, GBSSI, and plastid phylograms, suggesting that they may be potential genome donors to S. almum. Multiple LCN and plastid allelic variants have been identified in S. halepense of subg. Sorghum. The crown ages of Sorghum plus Cleistachne sorghoides and subg. Sorghum are estimated to be 12.7 million years ago (Mya) and 8.6 Mya, respectively. Molecular results support the recognition of three distinct subgenera in Sorghum: subg. Chaetosorghum with two sections, each with a single species, subg. Parasorghum with 17 species, and subg. Sorghum with nine species and we also provide a new nomenclatural combination, Sorghum sorghoides. C1 [Liu, Qing; Liu, Huan] Chinese Acad Sci, South China Bot Garden, Key Lab Plant Resources Conservat & Sustainable U, Guangzhou, Guangdong, Peoples R China. [Liu, Huan] Univ Chinese Acad Sci, Beijing, Peoples R China. [Wen, Jun; Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Liu, Q (reprint author), Chinese Acad Sci, South China Bot Garden, Key Lab Plant Resources Conservat & Sustainable U, Guangzhou, Guangdong, Peoples R China. EM liuqing@scib.ac.cn; peterson@si.edu FU National Natural Science Foundation of China [31270275, 31310103023]; Special Basic Research Foundation of Ministry of Science and Technology of the People's Republic of China [2013FY112100]; Key Laboratory of Plant Resources Conservation and Sustainable Utilization, South China Botanical Garden, CAS [201212ZS]; 42nd Scientific Research Foundation for the Returned Overseas Chinese Scholars, State Education Ministry [2011-1139]; Laboratories of Analytical Biology of the National Museum of Natural History, Smithsonian Institution FX This work was supported by the National Natural Science Foundation of China (31270275, 31310103023), the Special Basic Research Foundation of Ministry of Science and Technology of the People's Republic of China (2013FY112100), the Key Project of Key Laboratory of Plant Resources Conservation and Sustainable Utilization, South China Botanical Garden, CAS (201212ZS), the 42nd Scientific Research Foundation for the Returned Overseas Chinese Scholars, State Education Ministry (2011-1139), and the Laboratories of Analytical Biology of the National Museum of Natural History, Smithsonian Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 108 TC 6 Z9 6 U1 3 U2 23 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 14 PY 2014 VL 9 IS 8 AR e104933 DI 10.1371/journal.pone.0104933 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO0QT UT WOS:000341017000077 PM 25122516 ER PT J AU Crowley, BE Wheatley, PV AF Crowley, Brooke E. Wheatley, Patrick V. TI To bleach or not to bleach? Comparing treatment methods for isolating biogenic carbonate SO CHEMICAL GEOLOGY LA English DT Article DE Bioapatite; Bone; Dentine; Enamel; Carbonate; Stable isotopes ID OXYGEN-ISOTOPE VALUES; STABLE CARBON; BIOLOGICAL APATITE; BONE APATITE; RECONSTRUCTION; TOOTH; DIAGENESIS; BIOAPATITE; COLLAGEN; FRACTIONATION AB Stable carbon and oxygen isotope ratios in tooth enamel and bone hydroxyapatite are used to answer a variety of ecological questions. Researchers employ chemical treatments to reduce contaminants that may interfere with the isotope ratios in hydroxyapatite. Chemical treatment should remove exogenous as well as non lattice-bound molecules without affecting the isotopic composition of the biogenic carbonate or introducing secondary carbonate material. However, there is growing concern that some of the most frequently used chemicals may alter biogenic isotope ratios, thus compromising isotope data. Despite a considerable body of literature, there is still no consensus as to which chemical treatment methods are "the best". Here we test the isotopic effects of a suite of chemical experimental treatments on modern and fossil enamel carbonate, including six published protocols. We also test the degree to which carbon and oxygen isotope ratios in bone and dentine are affected by commonly used treatment chemicals. We conclude that treatment with hydrogen peroxide followed by Ca-buffered acetic acid yields the "best" results. This combination results in less extreme carbon, oxygen, and weight percent carbonate values compared to other treatments. Although sequential treatment with sodium hypochlorite (bleach) and Ca-buffered acetic acid produces similar results for enamel, bleach is not recommended for tissues with a higher organic content, such as bone or dentine. (C) 2014 Elsevier B. V. All rights reserved. C1 [Crowley, Brooke E.; Wheatley, Patrick V.] Univ Calif Santa Cruz, Dept Earth & Planetary Sci, Santa Cruz, CA 95064 USA. [Crowley, Brooke E.] Univ Cincinnati, Dept Geol, Cincinnati, OH 45221 USA. [Crowley, Brooke E.] Univ Cincinnati, Dept Anthropol, Cincinnati, OH 45221 USA. [Wheatley, Patrick V.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Crowley, BE (reprint author), Univ Cincinnati, Dept Geol, 2100 West Clifton Ave,Geol & Phys Bldg, Cincinnati, OH 45221 USA. EM brooke.crowley@uc.edu OI Crowley, Brooke/0000-0002-8462-6806 FU NSF [EAR-0819943] FX We thank Dyke Andreasen, Andrew Czaja and David Rogow for their analytical assistance. Steven Bohaty provided much of the initial work for the transducer calibration. We thank Adam Rountrey and Libby Stern for their valuable references, and technical discussion. We also thank Dr. Stern, Dr. Paul Koch, and two anonymous reviewers for providing advice and comments on the initial drafts of this manuscript. This project was funded by NSF Grant EAR-0819943. NR 36 TC 11 Z9 11 U1 2 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 EI 1878-5999 J9 CHEM GEOL JI Chem. Geol. PD AUG 14 PY 2014 VL 381 BP 234 EP 242 DI 10.1016/j.chemgeo.2014.05.006 PG 9 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AM9NO UT WOS:000340208500020 ER PT J AU Otterbach, J Lemeshko, M AF Otterbach, Johannes Lemeshko, Mikhail TI Dissipative Preparation of Spatial Order in Rydberg-Dressed Bose-Einstein Condensates SO PHYSICAL REVIEW LETTERS LA English DT Article ID DIPOLE-DIPOLE INTERACTIONS; QUANTUM SIMULATOR; ATOMS; GAS; OPTICS; SYSTEMS; DRIVEN; STATES; IONS AB We propose a technique for engineering momentum-dependent dissipation in Bose-Einstein condensates with nonlocal interactions. The scheme relies on the use of momentum-dependent dark states in close analogy to velocity-selective coherent population trapping. During the short-time dissipative dynamics, the system is driven into a particular finite-momentum phonon mode, which in real space corresponds to an ordered structure with nonlocal density-density correlations. Dissipation-induced ordering can be observed and studied in present-day experiments using cold atoms with dipole-dipole or off-resonant Rydberg interactions. Because of its dissipative nature, the ordering does not require artificial breaking of translational symmetry by an optical lattice or harmonic trap. This opens up a perspective of direct cooling of quantum gases into strongly interacting phases. C1 [Otterbach, Johannes; Lemeshko, Mikhail] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Lemeshko, Mikhail] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Otterbach, J (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM jotterbach@physics.harvard.edu; mikhail.lemeshko@gmail.com FU NSF through the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University; Smithsonian Astrophysical Observatory; Harvard Quantum Optics Center FX We thank H. Weimer, T. Pohl, J. Bohn, and R. Schmidt for insightful discussions. This work was supported by NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory, as well as the Harvard Quantum Optics Center. NR 62 TC 11 Z9 11 U1 2 U2 24 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD AUG 11 PY 2014 VL 113 IS 7 AR 070401 DI 10.1103/PhysRevLett.113.070401 PG 6 WC Physics, Multidisciplinary SC Physics GA AO1ZL UT WOS:000341114000001 PM 25170691 ER PT J AU Hayward, CC Torrey, P Springel, V Hernquist, L Vogelsberger, M AF Hayward, Christopher C. Torrey, Paul Springel, Volker Hernquist, Lars Vogelsberger, Mark TI Galaxy mergers on a moving mesh: a comparison with smoothed particle hydrodynamics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE hydrodynamics; methods: numerical; galaxies: active; galaxies: formation; galaxies: interactions; galaxies: starburst ID SUPERMASSIVE BLACK-HOLES; LYMAN-ALPHA FOREST; SIMILAR-TO 2; REDSHIFT SUBMILLIMETER GALAXIES; STAR-FORMING GALAXIES; DARK-MATTER MODEL; BH-SIGMA RELATION; GAS-RICH MERGERS; HOT GASEOUS HALO; ELLIPTIC GALAXIES AB Galaxy mergers have been investigated for decades using smoothed particle hydrodynamics (SPH), but recent work highlighting inaccuracies inherent in the traditional SPH technique calls into question the reliability of previous studies. We explore this issue by comparing a suite of gadget-3 SPH simulations of idealized (i.e. non-cosmological) isolated discs and galaxy mergers with otherwise identical calculations performed using the moving-mesh code arepo. When black hole (BH) accretion and active galactic nucleus (AGN) feedback are not included, the star formation histories (SFHs) obtained from the two codes agree well. When BHs are included, the code- and resolution-dependent variations in the SFHs are more significant, but the agreement is still good, and the stellar mass formed over the course of a simulation is robust to variations in the numerical method. During a merger, the gas morphology and phase structure are initially similar prior to the starburst phase. However, once a hot gaseous halo has formed from shock heating and AGN feedback (when included), the agreement is less good. In particular, during the post-starburst phase, the SPH simulations feature more prominent hot gaseous haloes and spurious clumps, whereas with arepo, gas clumps and filaments are less apparent and the hot halo gas can cool more efficiently. We discuss the origin of these differences and explain why the SPH technique yields trustworthy results for some applications (such as the idealized isolated disc and galaxy merger simulations presented here) but not others (e.g. gas flows on to galaxies in cosmological hydrodynamical simulations). C1 [Hayward, Christopher C.; Springel, Volker] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Torrey, Paul; Hernquist, Lars; Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, Volker] Heidelberg Univ, Zentrum Astron, Astron Rechen Inst, D-69120 Heidelberg, Germany. RP Hayward, CC (reprint author), Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. EM christopher.hayward@h-its.org RI Hayward, Christopher/I-4756-2012; OI Hayward, Christopher/0000-0003-4073-3236; Torrey, Paul/0000-0002-5653-0786 FU Klaus Tschira Foundation; National Science Foundation [PHY-1066293]; European Research Council under ERC-StG grant [EXAGAL-308037] FX We thank Shy Genel, Phil Hopkins, Federico Marinacci, Rudiger Pakmor, Ewald Puchwein, and Debora Sijacki for useful discussion; Jorge Moreno and Francois Schweizer for detailed comments on the manuscript; and the anonymous referee for a critical report that helped to improve the paper. CCH is grateful to the Klaus Tschira Foundation for financial support, acknowledges the hospitality of the Aspen Center for Physics, which is supported by the National Science Foundation Grant no. PHY-1066293, and heartily thanks Andreas Bauer for many PYTHON tips, which were very helpful for (almost completely) curing a long-standing IDL dependence. VS acknowledges support from the European Research Council under ERC-StG grant EXAGAL-308037. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 153 TC 40 Z9 40 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 AUG 11 PY 2014 VL 442 IS 3 BP 1992 EP 2016 DI 10.1093/mnras/stu957 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300008 ER PT J AU Dutson, KL Edge, AC Hinton, JA Hogan, MT Gurwell, MA Alston, WN AF Dutson, K. L. Edge, A. C. Hinton, J. A. Hogan, M. T. Gurwell, M. A. Alston, W. N. TI A non-thermal study of the brightest cluster galaxy NGC 1275-the Gamma-Radio connection over four decades SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; galaxies: active; galaxies: clusters: individual: Perseus; galaxies: individual: NGC 1275; gamma rays: galaxies; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; MILLIMETER CONTINUUM MEASUREMENTS; H-ALPHA FILAMENTS; PERSEUS CLUSTER; RAY-EMISSION; SOURCE CATALOG; COOLING FLOWS; FLUX-DENSITY; 3C 84 AB Emission from the active nucleus in the core of the brightest cluster galaxy of the Perseus cluster, NGC 1275, has varied dramatically over the past four decades. Prompted by the Fermi detection of flaring in the gamma-ray band, we present the recent increased activity of this source in the context of its past radio and gamma-ray output. The broad correspondence between the high-frequency radio data and the high-energy (HE) emission is striking. However, on short time-scales this correlation breaks down and the 1.3 mm Submillimeter Array flux is apparently unaffected during Fermi -detected flaring activity. The fact that NGC 1275 is also detected at TeV energies during the periods of HE gamma-ray flaring suggests that the short-time-scale variation might be primarily related to changes in the inverse Compton scattering of photons by the electron population in the jet. The longer-time-scale changes suggest a 30-40 year variation in the fuelling of the black hole that affects the power of the inner jet. NCG 1275 is a laboratory for the class of brightest cluster galaxies, and its variability on these time-scales has implications for our understanding of massive galaxies in cooling-core clusters. The case of NGC 1275 highlights the need for wide coverage across the radio band to correctly account for the contribution to emission from a synchrotron self-absorbed core (for example when considering contamination of Sunyaev-Zel'dovich effect observations), and the danger of variability biases in radio surveys of galaxies. C1 [Dutson, K. L.; Hinton, J. A.; Alston, W. N.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Edge, A. C.; Hogan, M. T.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alston, W. N.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Dutson, KL (reprint author), Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. EM kate.dutson@leicester.ac.uk OI Edge, Alastair/0000-0002-3398-6916 FU Smithsonian Institution; Academia Sinica; NASA; National Science Foundation; University of Michigan; STFC [ST/I505780/1, ST/J501104/1, ST/I505656/1, ST/I001573/1]; EU; STRONGGRAVITY; Leverhulme Trust FX 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. This work has made use of public Fermi data and Science Tools provided by the Fermi Science Support Centre, the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and the SIMBAD and VIZIER data bases, operated at CDS, Strasbourg, France. We thank Margo Aller for permission to use data from the University of Michigan Radio Astronomy Observatory, which was supported by the National Science Foundation and NASA, and by funds from the University of Michigan. We thank also Richard White, whose automated Fermi tool chain improved the time-efficiency of much of the analysis carried out. KLD acknowledges support from the STFC studentship ST/I505780/1 and the STFC Doctrinal Training Grant ST/J501104/1, MTH from the STFC studentship ST/I505656/1, WNA from the EU FP7-SPACE research project, STRONGGRAVITY., JAH from the Leverhulme Trust, and ACE from STFC grant ST/I001573/1. NR 68 TC 9 Z9 9 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 11 PY 2014 VL 442 IS 3 BP 2048 EP 2057 DI 10.1093/mnras/stu975 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300011 ER PT J AU Kovacs, G Hartman, JD Bakos, GA Quinn, SN Penev, K Latham, DW Bhatti, W Csubry, Z de Val-Borro, M AF Kovacs, Geza Hartman, Joel D. Bakos, Gaspar A. Quinn, Samuel N. Penev, Kaloyan Latham, David W. Bhatti, Waqas Csubry, Zoltan de Val-Borro, Miguel TI Stellar rotational periods in the planet hosting open cluster Praesepe SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planetary systems; stars: rotation; starspots; stars: variables: delta Scuti; open clusters and associations: individual: Praesepe ID TREND FILTERING ALGORITHM; CLOSE-IN PLANETS; LOW-MASS STARS; MAGNETIC ACTIVITY; PROPER MOTIONS; COMA BERENICES; SOLAR-TYPE; KEPLER; FIELD; PHOTOMETRY AB By using the dense coverage of the extrasolar planet survey project HATNet (Hungarian-made Automated Telescope Network), we Fourier analyse 381 high-probability members of the nearby open cluster Praesepe (Beehive/M44/NGC 2632). In addition to the detection of 10 variables (of delta Scuti and other types), we identify 180 rotational variables (including the two known planet hosts). This sample increases the number of known rotational variables in this cluster for spectral classes earlier than M by more than a factor of 3. These stars closely follow a colour/magnitude-period relation from early F to late K stars. We approximate this relation by polynomials for an easier reference to the rotational characteristics in different colours. The total (peak-to-peak) amplitudes of the large majority (94 per cent) of these variables span the range of 0.005-0.04 mag. The periods cover a range from 2.5 to 15 d. These data strongly confirm that Praesepe and the Hyades have the same gyrochronological ages. Regarding the two planet hosts, Pr0211 (the one with the shorter orbital period) has a rotational period that is similar to 2 d shorter than the one expected from the main rotational pattern in this cluster. This, together with other examples discussed in the paper, may hint that star-planet interaction via tidal dissipation can be significant in some cases in the rotational evolution of stars hosting hot Jupiters. C1 [Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary. [Kovacs, Geza] Univ N Dakota, Dept Phys & Astrophys, Grand Forks, ND 58202 USA. [Hartman, Joel D.; Bakos, Gaspar A.; Penev, Kaloyan; Bhatti, Waqas; Csubry, Zoltan; de Val-Borro, Miguel] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Quinn, Samuel N.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kovacs, G (reprint author), Konkoly Observ Budapest, Konkoly Thege MU 15-17, Budapest, Hungary. EM kovacs@konkoly.hu OI Penev, Kaloyan/0000-0003-4464-1371; Hartman, Joel/0000-0001-8732-6166 FU National Aeronautics and Space Administration; National Science Foundation; Robert Martin Ayers Sciences Fund; Hungarian Scientific Research Foundation (OTKA) [K-81373]; NASA [NNG04GN74G, NNX13AJ15G, NNX09AB29G, NNX14AF87G, NNX13AQ62G]; NSF [AST-1108686, DGE-1051030] FX We thank the referee Aleks Scholz for the valuable comments that helped to improve the paper. 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. This research was made possible through the use of the AAVSO Photometric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund, the SIMBAD data base and the VizieR catalogue access tool, operated at CDS, Strasbourg, France. GK thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. HATNet observations have been funded by NASA grants NNG04GN74G and NNX13AJ15G. GAB, ZC and KP acknowledge partial support from NASA grant NNX09AB29G. JH acknowledges partial support from NSF grant AST-1108686 and NASA grant NNX14AF87G. KP acknowledges support from NASA grant NNX13AQ62G. SQ acknowledges support from NSF grant DGE-1051030. NR 57 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 AUG 11 PY 2014 VL 442 IS 3 BP 2081 EP 2093 DI 10.1093/mnras/stu946 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300014 ER PT J AU Torricelli-Ciamponi, G Pietrini, P Risaliti, G Salvati, M AF Torricelli-Ciamponi, G. Pietrini, P. Risaliti, G. Salvati, M. TI Search for X-ray occultations in active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: Seyfert; X-rays: galaxies ID BLACK-HOLE MASS; XMM-NEWTON; SWIFT J2127.4+5654; EMITTING REGION; BEPPOSAX VIEW; LINE; GALAXIES; NGC-4151; AGN; ABSORPTION AB Recent time-resolved spectral studies of a few active galactic nuclei (AGNs) in hard X-rays revealed occultations of the X-ray primary source probably by broad-line region (BLR) clouds. An important open question on the structure of the circumnuclear medium of AGN is whether this phenomenon is common, i.e. whether a significant fraction of the X-ray absorption in AGN is due to BLR clouds. Here, we present the first attempt to perform this kind of analysis in a homogeneous way, on a statistically representative sample of AGN, consisting of the similar to 40 brightest sources with long XMM-Newton and/or Suzaku observations. We describe our method, based on a simple analysis of hardness-ratio light curves, and its validation through a complete spectroscopic analysis of a few cases. We find that X-ray eclipses, most probably due to clouds at the distance of the BLR, are common in sources where the expected occultation time is compatible with the observation time, while they are not found in sources with longer estimated occultation times. Overall, our results show that occultations by BLR clouds may be responsible for most of the observed X-ray spectral variability at energies higher than 2 keV, on time-scales longer than a few ks. C1 [Torricelli-Ciamponi, G.; Risaliti, G.; Salvati, M.] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Pietrini, P.] Univ Florence, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Torricelli-Ciamponi, G (reprint author), INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy. EM torricel@arcetri.astro.it RI XRAY, SUZAKU/A-1808-2009; OI Risaliti, Guido/0000-0002-3556-977X FU NASA [NNX08AN48G]; PRIN-MIUR; PRIN-INAF FX This work has been partly supported by grants NASA NNX08AN48G, PRIN-MIUR 2010-2011 'The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid' and PRIN-INAF 2011 'Black hole growth and AGN feedback through the cosmic time'. NR 47 TC 10 Z9 10 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 AUG 11 PY 2014 VL 442 IS 3 BP 2116 EP 2130 DI 10.1093/mnras/stu969 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300016 ER PT J AU Nascimbeni, V Bedin, LR Heggie, DC van den Berg, M Giersz, M Piotto, G Brogaard, K Bellini, A Milone, AP Rich, RM Pooley, D Anderson, J Ubeda, L Ortolani, S Malavolta, L Cunial, A Pietrinferni, A AF Nascimbeni, V. Bedin, L. R. Heggie, D. C. van den Berg, M. Giersz, M. Piotto, G. Brogaard, K. Bellini, A. Milone, A. P. Rich, R. M. Pooley, D. Anderson, J. Ubeda, L. Ortolani, S. Malavolta, L. Cunial, A. Pietrinferni, A. TI The M 4 Core Project with HST - III. Search for variable stars in the primary field SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; binaries: general; stars: variables: general; globular clusters: individual: NGC 6121 ID GLOBULAR-CLUSTER M4; TRANSIT SURVEY; MAIN-SEQUENCE; SPACED DATA; ACS SURVEY; CATALOG; PHOTOMETRY; BINARIES AB We present the results of a photometric search for variable stars in the core of the Galactic globular cluster Messier 4 (M 4). The input data are a large and unprecedented set of deep Hubble Space Telescope WFC3 images (large programme GO-12911; 120 orbits allocated), primarily aimed at probing binaries with massive companions by detecting their astrometric wobbles. Though these data were not optimized to carry out a time-resolved photometric survey, their exquisite precision, spatial resolution and dynamic range enabled us to firmly detect 38 variable stars, of which 20 were previously unpublished. They include 19 cluster-member eclipsing binaries (confirming the large binary fraction of M 4), RR Lyrae and objects with known X-ray counterparts. We improved and revised the parameters of some among published variables. C1 [Nascimbeni, V.; Bedin, L. R.; Piotto, G.; Ortolani, S.; Malavolta, L.; Cunial, A.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Heggie, D. C.] Univ Edinburgh, Sch Math, Edinburgh EH9 3JZ, Midlothian, Scotland. [Heggie, D. C.] Univ Edinburgh, Maxwell Inst Math Sci, Edinburgh EH9 3JZ, Midlothian, Scotland. [van den Berg, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [van den Berg, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giersz, M.] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Piotto, G.; Ortolani, S.; Malavolta, L.; Cunial, A.] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35122 Padua, Italy. [Brogaard, K.] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark. [Brogaard, K.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Bellini, A.; Anderson, J.; Ubeda, L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Milone, A. P.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Rich, R. M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Pooley, D.] Sam Houston State Univ, Dept Phys, Huntsville, TX 77341 USA. [Pooley, D.] Eureka Sci Inc, Oakland, CA 94602 USA. [Pietrinferni, A.] Osservatorio Astron Teramo, INAF, I-64100 Teramo, Italy. RP Nascimbeni, V (reprint author), Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy. EM valerio.nascimbeni@unipd.it OI ORTOLANI, SERGIO/0000-0001-7939-5348; Pietrinferni, Adriano/0000-0003-3795-9031; bedin, luigi/0000-0003-4080-6466; Brogaard, Karsten/0000-0003-2001-0276; Piotto, Giampaolo/0000-0002-9937-6387 FU PRIN-INAF; STScI [GO-12911]; Villum Foundation; Australian Research Council [DP120100475]; National Science Centre [DEC-2012/07/B/ST9/04412]; INAF-OAPd [19/2013, 42/2013]; European Union [313014]; CARIPARO foundation FX LRB, GP, VN, SO, AP and LM acknowledge PRIN-INAF 2012 funding under the project entitled: 'TheM4 Core Project with Hubble Space Telescope'. JA, AB, LU and RMR acknowledge support from STScI grants GO-12911. KB acknowledges support from the Villum Foundation. APM acknowledges the financial support from the Australian Research Council through Discovery Project grant DP120100475. MG acknowledges partial support by the National Science Centre through the grant DEC-2012/07/B/ST9/04412. VN acknowledges partial support from INAF-OAPd through the grant 'Analysis of HARPS-N data in the framework of GAPS project' (# 19/2013) and 'Studio preparatorio per le osservazioni della missione ESA/CHEOPS' (#42/2013). LM acknowledges support from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement #313014 (ETAEARTH). AC acknowledges support by the CARIPARO foundation through the grant 'Ricerca di pianeti extra-solari: nuove tecniche per trovare pianeti simili alla Terra'. Some tasks of our data analysis have been carried out with the VARTOOLS (Hartman et al. 2008) and NR 42 TC 7 Z9 7 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 AUG 11 PY 2014 VL 442 IS 3 BP 2381 EP 2391 DI 10.1093/mnras/stu930 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300037 ER PT J AU Gonzalez-Nuevo, J Lapi, A Negrello, M Danese, L De Zotti, G Amber, S Baes, M Bland-Hawthorn, J Bourne, N Brough, S Bussmann, RS Cai, ZY Cooray, A Driver, SP Dunne, L Dye, S Eales, S Ibar, E Ivison, R Liske, J Loveday, J Maddox, S Michalowski, MJ Robotham, ASG Scott, D Smith, MWL Valiante, E Xia, JQ AF Gonzalez-Nuevo, J. Lapi, A. Negrello, M. Danese, L. De Zotti, G. Amber, S. Baes, M. Bland-Hawthorn, J. Bourne, N. Brough, S. Bussmann, R. S. Cai, Z. -Y. Cooray, A. Driver, S. P. Dunne, L. Dye, S. Eales, S. Ibar, E. Ivison, R. Liske, J. Loveday, J. Maddox, S. Michalowski, M. J. Robotham, A. S. G. Scott, D. Smith, M. W. L. Valiante, E. Xia, J. -Q. TI Herschel(a similar to...)-ATLAS/GAMA: SDSS cross-correlation induced by weak lensing SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; cosmology: observations; large-scale structure of Universe; infrared: galaxies ID LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; SCIENCE DEMONSTRATION PHASE; ANGULAR-CORRELATION FUNCTION; LENSED SUBMILLIMETER GALAXY; AZTEC MILLIMETER SURVEY; STELLAR MASS FUNCTIONS; HERSCHEL-ATLAS; HIGH-REDSHIFT; COSMIC MAGNIFICATION AB We report a highly significant (> 10 sigma) spatial correlation between galaxies with S-350 mu m a parts per thousand yen 30 mJy detected in the equatorial fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) with estimated redshifts a parts per thousand(3) 1.5, and Sloan Digital Sky Survey (SDSS) or Galaxy And Mass Assembly (GAMA) galaxies at 0.2 a parts per thousand currency sign z a parts per thousand currency sign 0.6. The significance of the cross-correlation is much higher than those reported so far for samples with non-overlapping redshift distributions selected in other wavebands. Extensive, realistic simulations of clustered sub-mm galaxies amplified by foreground structures confirm that the cross-correlation can be explained by weak gravitational lensing (mu < 2). The simulations also show that the measured amplitude and range of angular scales of the signal are larger than can be accounted for by galaxy-galaxy weak lensing. However, for scales a parts per thousand(2) 2 arcmin, the signal can be reproduced if SDSS/GAMA galaxies act as signposts of galaxy groups/clusters with halo masses in the range 10(13.2)-10(14.5) M-aS (TM). The signal detected on larger scales appears to reflect the clustering of such haloes. C1 [Gonzalez-Nuevo, J.] CSIC UC, Inst Fis Cantabria, E-39005 Santander, Spain. [Gonzalez-Nuevo, J.; Lapi, A.; Danese, L.; De Zotti, G.; Cai, Z. -Y.] SISSA, I-34136 Trieste, Italy. [Lapi, A.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Negrello, M.; De Zotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Amber, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Baes, M.] Univ Ghent, Sterrenkundig Observatorium, B-9000 Ghent, Belgium. [Bland-Hawthorn, J.] Univ Sydney, Sydney Inst Astron, Sch Phys, Sydney, NSW 2006, Australia. [Bourne, N.; Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bourne, N.; Ivison, R.; Michalowski, M. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Brough, S.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cooray, A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Driver, S. P.; Robotham, A. S. G.] Univ Western Australia, ICRAR, Crawley, WA 6009, Australia. [Driver, S. P.] Univ St Andrews, Scottish Univ Phys Alliance SUPA, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Eales, S.; Smith, M. W. L.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Ibar, E.] Univ Valparaiso, Inst Fis & Astron, Valparaiso 2360102, Chile. [Liske, J.] European Southern Observ, D-85748 Garching, Germany. [Loveday, J.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Xia, J. -Q.] Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China. RP Gonzalez-Nuevo, J (reprint author), CSIC UC, Inst Fis Cantabria, E-39005 Santander, Spain. EM gnuevo@ifca.unican.es RI Driver, Simon/H-9115-2014; Gonzalez-Nuevo, Joaquin/I-3562-2014; Ivison, R./G-4450-2011 OI Driver, Simon/0000-0001-9491-7327; Gonzalez-Nuevo, Joaquin/0000-0003-1354-6822; Ivison, R./0000-0001-5118-1313 FU Spanish Ministerio de Ciencia e Innovacion [AYA2012-39475-C02-01]; Consolider-Ingenio [CSD2010-00064]; ASI/INAF [I/072/09/0]; Spanish CSIC; European Social Fund; PRIN INAF; STFC (UK); ARC (Australia); AAO; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy Office of Science FX I thank Michael D. Schneider for useful suggestions and comments on the manuscript. The work has been supported in part by the Spanish Ministerio de Ciencia e Innovacion, AYA2012-39475-C02-01, and Consolider-Ingenio 2010, CSD2010-00064, projects and by ASI/INAF Agreement I/072/09/0 for the Planck LFI activity of Phase E2. JGN acknowledges financial support from the Spanish CSIC for a JAE-DOC fellowship, co-funded by the European Social Fund. MN acknowledges final support from PRIN INAF 2012 project 'Looking into the dust-obscured phase of galaxy formation through cosmic zoom lenses in the Herschel Astrophysical Large Area Survey'. The Herschel-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/. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the SDSS 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, Herschel-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 paper has used data from the SDSS-III. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 73 TC 3 Z9 3 U1 0 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 AUG 11 PY 2014 VL 442 IS 3 BP 2680 EP 2690 DI 10.1093/mnras/stu1041 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5TU UT WOS:000339924300060 ER PT J AU Santiago, CN Becker, MH Belden, LK Gratwicke, B Minbiole, KPC AF Santiago, Celina N. Becker, Matthew H. Belden, Lisa K. Gratwicke, Brian Minbiole, Kevin P. C. TI Antifungal defenses of the Panamanian golden frog: Bacterial augmentation and chemical analysis SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 248th National Meeting of the American-Chemical-Society (ACS) CY AUG 10-14, 2014 CL San Francisco, CA SP Amer Chem Soc C1 [Santiago, Celina N.; Minbiole, Kevin P. C.] Villanova Univ, Dept Chem, Villanova, PA 19085 USA. [Becker, Matthew H.; Belden, Lisa K.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. [Gratwicke, Brian] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. EM csantia3@villanova.edu NR 0 TC 0 Z9 0 U1 2 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD AUG 10 PY 2014 VL 248 MA 197-CHED PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA CA8JN UT WOS:000349165102843 ER PT J AU Naoz, S Narayan, R AF Naoz, Smadar Narayan, Ramesh TI GLOBULAR CLUSTERS AND DARK SATELLITE GALAXIES THROUGH THE STREAM VELOCITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE globular clusters: general ID BARYONIC STRUCTURE FORMATION; YOUNG STAR-CLUSTERS; MATTER HALOS; 1ST STARS; ANTENNAE GALAXIES; TIDAL FIELD; NGC 2419; SIMULATIONS; ORIGIN; IMPACT AB The formation of purely baryonic globular clusters with no gravitationally bound dark matter is still a theoretical challenge. We show that these objects might form naturally whenever there is a relative stream velocity between baryons and dark matter. The stream velocity causes a phase shift between linear modes of baryonic and dark matter perturbations, which translates to a spatial offset between the two components when they collapse. For a 2 sigma (3 sigma) density fluctuation, baryonic clumps with masses in the range 10(5)-2.5 x 10(6) M-circle dot (10(5)-4 x 10(6) M-circle dot) collapse outside the virial radii of their counterpart dark matter halos. These objects could survive as long-lived, dark-matter-free objects and might conceivably become globular clusters. In addition, their dark matter counterparts, which were deprived of gas, might become dark satellite galaxies. C1 [Naoz, Smadar; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Naoz, Smadar] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. RP Naoz, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM snaoz@astro.ucla.edu OI Narayan, Ramesh/0000-0002-1919-2730; Naoz, Smadar/0000-0002-9802-9279 FU NASA; NSF [AST1312651]; Chandra X-ray Center FX S.N. was supported by NASA through an Einstein Post-doctoral Fellowship awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA, contract PF2-130096. R. N. was supported in part by NSF grant AST1312651. NR 45 TC 4 Z9 4 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 10 PY 2014 VL 791 IS 1 AR L8 DI 10.1088/2041-8205/791/1/L8 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4JB UT WOS:000341302200008 ER PT J AU Walsh, C Juhasz, A Pinilla, P Harsono, D Mathews, GS Dent, WRF Hogerheijde, MR Birnstiel, T Meeus, G Nomura, H Aikawa, Y Millar, TJ Sandell, G AF Walsh, Catherine Juhasz, Attila Pinilla, Paola Harsono, Daniel Mathews, Geoffrey S. Dent, William R. F. Hogerheijde, Michiel R. Birnstiel, T. Meeus, Gwendolyn Nomura, Hideko Aikawa, Yuri Millar, T. J. Sandell, Goeran TI ALMA HINTS AT THE PRESENCE OF TWO COMPANIONS IN THE DISK AROUND HD 100546 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE protoplanetary disks; stars: formation; stars: individual (HD 100546); stars: pre-main sequence; submillimeter: planetary systems ID HERBIG AE/BE STARS; NEAR-INFRARED SPECTROSCOPY; CO EMISSION-LINES; PROTOPLANETARY DISKS; DIGIT SURVEY; TW-HYDRAE; WARM GAS; DUST; HD-100546; PLANET AB HD 100546 is a well-studied Herbig Be star-disk system that likely hosts a close-in companion with compelling observational evidence for an embedded protoplanet at 68 AU. We present Atacama Large Millimeter/Submillimeter Array observations of the HD 100546 disk which resolve the gas and dust structure at (sub) millimeter wavelengths. The CO emission (at 345.795 GHz) originates from an extensive molecular disk (390 +/- 20 AU in radius) whereas the continuum emission is more compact (230 +/- 20 AU in radius), suggesting radial drift of the millimeter-sized grains. The CO emission is similar in extent to scattered light images indicating well-mixed gas and micrometer-sized grains in the disk atmosphere. Assuming azimuthal symmetry, a single-component power-law model cannot reproduce the continuum visibilities. The visibilities and images are better reproduced by a double-component model: a compact ring with a width of 21 AU centered at 26 AU and an outer ring with a width of 75 +/- 3 AU centered at 190 +/- 3 AU. The influence of a companion and protoplanet on the dust evolution is investigated. The companion at 10 AU facilitates the accumulation of millimeter-sized grains within a compact ring, approximate to 20-30 AU, by approximate to 10 Myr. The injection of a protoplanet at 1 Myr hastens the ring formation (approximate to 1.2 Myr) and also triggers the development of an outer ring (approximate to 100-200 AU). These observations provide additional evidence for the presence of a close-in companion and hint at dynamical clearing by a protoplanet in the outer disk. C1 [Walsh, Catherine; Juhasz, Attila; Pinilla, Paola; Harsono, Daniel; Mathews, Geoffrey S.; Hogerheijde, Michiel R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Harsono, Daniel] SRON Netherlands Inst Space Res, SRON, NL-9700 AV Groningen, Netherlands. [Mathews, Geoffrey S.] Univ Hawaii, Dept Phys & Astron, Honolulu, HI 96822 USA. [Dent, William R. F.] Joint ALMA Observ JAO, Santiago, Chile. [Dent, William R. F.] European So Observ, Santiago 19, Chile. [Birnstiel, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Meeus, Gwendolyn] Univ Autonoma Madrid, Fac Ciencias, Dept Fis Teor, E-28049 Madrid, Spain. [Nomura, Hideko] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Aikawa, Yuri] Kobe Univ, Dept Earth & Planetary Sci, Nada Ku, Kobe, Hyogo 6578501, Japan. [Millar, T. J.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Sandell, Goeran] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Walsh, C (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. OI Millar, Tom/0000-0001-5178-3656; Hogerheijde, Michiel/0000-0001-5217-537X; Birnstiel, Tilman/0000-0002-1899-8783 FU Netherlands Organisation for Scientific Research (NWO) [639.041.335]; EU A-ERC [291141]; KNAW; NASA Origins of Solar Systems [NNX12AJ04G]; STFC; Netherlands Organization for Scientific Research (NWO); European ALMA Regional Center node in the Netherlands FX This Letter 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. The authors thank E. F. van Dishoeck, C. P. Dullemond, N. van der Marel, and M. Schmalzl for useful discussions, and G. D. Mulders for sharing the results of his hydrodynamical simulations. C. W. acknowledges support from the Netherlands Organisation for Scientific Research (NWO, program number 639.041.335). This work was also supported by EU A-ERC grant 291141 CHEMPLAN and a KNAW prize. T. B. acknowledges support from NASA Origins of Solar Systems grant NNX12AJ04G. Astrophysics at QUB is supported by a grant from the STFC. M. R. H., A. J., and G. S. M. acknowledge support from the Netherlands Organization for Scientific Research (NWO) to Allegro, the European ALMA Regional Center node in the Netherlands. NR 44 TC 35 Z9 35 U1 1 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 AUG 10 PY 2014 VL 791 IS 1 AR L6 DI 10.1088/2041-8205/791/1/L6 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO4JB UT WOS:000341302200006 ER PT J AU Bai, XN AF Bai, Xue-Ning TI WIND-DRIVEN ACCRETION IN PROTOPLANETARY DISKS. II. RADIAL DEPENDENCE AND GLOBAL PICTURE (vol 772, pg 96, 2013) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 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 NR 2 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 2014 VL 791 IS 1 AR 73 DI 10.1088/0004-637X/791/1/73 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700073 ER PT J AU Bai, XN AF Bai, Xue-Ning TI MAGNETOROTATIONAL-INSTABILITY-DRIVEN ACCRETION IN PROTOPLANETARY DISKS (vol 739, pg 50, 2011) SO ASTROPHYSICAL JOURNAL LA English DT Correction ID WIND C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 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 NR 6 TC 2 Z9 2 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 2014 VL 791 IS 1 AR 72 DI 10.1088/0004-637X/791/1/72 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700072 ER PT J AU Barnard, R Garcia, MR Primini, F Murray, SS AF Barnard, R. Garcia, M. R. Primini, F. Murray, S. S. TI FIFTY M31 BLACK HOLE CANDIDATES IDENTIFIED BY CHANDRA AND XMM-NEWTON SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: black holes; X-rays: binaries; X-rays: general ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; GLOBULAR-CLUSTERS; NEUTRON-STAR; Z-TRACK; CXOM31 J004253.1+411422; SPECTRAL TRANSITIONS; EXTENDED CORONA; UPDATED SURVEY; XTE J1701-462 AB Over approximately the last five years, we have identified similar to 35 black hole candidates (BHCs) in M31 from their X-ray spectra. Our BHCs exhibited 0.3-10 keV spectra consistent with the X-ray binary (XB) hard state at luminosities that are above the upper limit for neutron star (NS) XBs. When our BHC spectra were modeled with a disk blackbody + blackbody model for comparison with bright NS XBs, we found that the BHCs inhabited a different parameter space than the NS XBs. However, BH XBs may also exhibit a thermally dominated (TD) state that has never been seen in NS XBs; this TD state is most often observed in X-ray transients. We examined the similar to 50 X-ray transients in our Chandra survey of M31 and found 13 with spectra suitable for analysis. We also examined two BHCs outside the field of view of our survey in the globular clusters B045 and B375. We have 42 strong BHCs and 8 plausible BHCs that may benefit from further observation. Of our 15 BHCs in globular clusters, 12 differ from NS spectra by >5 sigma. Due to improvements in our analysis, we have upgraded 10 previously identified plausible BHCs to strong BHCs. The mean maximum duty cycle of the 33 X-ray transients within 6 ' of M31* is 0.13; we estimate that >40% of the XBs in this region contain BH accretors. Remarkably, we estimate that BHCs contribute >90% of those XBs > 10(38) erg s(-1). C1 [Barnard, R.; Garcia, M. R.; Primini, F.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Baltimore, MA USA. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Primini, Francis/0000-0002-6077-0643 FU ESA member states; U.S. (NASA); Chandra grants [GO2-13106X, GO1-12109X]; HST [GO-11833, GO-12014] FX We thank the anonymous referee for useful suggestions that considerably improved this paper. This research has made use of data obtained from the Chandra satellite, and software provided by the Chandra X-Ray Center (CXC). We also include analysis of data from XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the U.S. (NASA). We are very grateful to Norbert Schartel and the XMM-Newton team for granting our TOO observation. R.B. is funded by Chandra grants GO2-13106X and GO1-12109X, along with HST grants GO-11833 and GO-12014. NR 41 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 AUG 10 PY 2014 VL 791 IS 1 AR 33 DI 10.1088/0004-637X/791/1/33 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700033 ER PT J AU Barro, G Faber, SM Perez-Gonzalez, PG Pacifici, C Trump, JR Koo, DC Wuyts, S Guo, Y Bell, E Dekel, A Porter, L Primack, J Ferguson, H Ashby, MLN Caputi, K Ceverino, D Croton, D Fazio, GG Giavalisco, M Hsu, L Kocevski, D Koekemoer, A Kurczynski, P Kollipara, P Lee, J McIntosh, DH McGrath, E Moody, C Somerville, R Papovich, C Salvato, M Santini, P Tal, T van der Wel, A Williams, CC Willner, SP Zolotov, A AF Barro, G. Faber, S. M. Perez-Gonzalez, P. G. Pacifici, C. Trump, J. R. Koo, D. C. Wuyts, S. Guo, Y. Bell, E. Dekel, A. Porter, L. Primack, J. Ferguson, H. Ashby, M. L. N. Caputi, K. Ceverino, D. Croton, D. Fazio, G. G. Giavalisco, M. Hsu, L. Kocevski, D. Koekemoer, A. Kurczynski, P. Kollipara, P. Lee, J. McIntosh, D. H. McGrath, E. Moody, C. Somerville, R. Papovich, C. Salvato, M. Santini, P. Tal, T. van der Wel, A. Williams, C. C. Willner, S. P. Zolotov, A. TI CANDELS+3D-HST: COMPACT SFGs AT z similar to 2-3, THE PROGENITORS OF THE FIRST QUIESCENT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: photometry; galaxies: starburst ID STAR-FORMING GALAXIES; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; ULTRA-DEEP-FIELD; LYMAN-BREAK GALAXIES; DIGITAL SKY SURVEY; GOODS-SOUTH FIELD; GREATER-THAN 1; SPECTRAL ENERGY-DISTRIBUTIONS; STELLAR POPULATION SYNTHESIS AB We analyze the star-forming and structural properties of 45 massive (log(M/M-circle dot) > 10) compact star-forming galaxies (SFGs) at 2 < z < 3 to explore whether they are progenitors of compact quiescent galaxies at z similar to 2. The optical/NIR and far-IR Spitzer/Herschel colors indicate that most compact SFGs are heavily obscured. Nearly half (47%) host an X-ray-bright active galactic nucleus (AGN). In contrast, only about 10% of other massive galaxies at that time host AGNs. Compact SFGs have centrally concentrated light profiles and spheroidal morphologies similar to quiescent galaxies and are thus strikingly different from other SFGs, which typically are disk-like and sometimes clumpy or irregular. Most compact SFGs lie either within the star formation rate (SFR)-mass main sequence (65%) or below it (30%), on the expected evolutionary path toward quiescent galaxies. These results show conclusively that galaxies become more compact before they lose their gas and dust, quenching star formation. Using extensive HST photometry from CANDELS and grism spectroscopy from the 3D-HST survey, we model their stellar populations with either exponentially declining (tau) star formation histories (SFHs) or physically motivated SFHs drawn from semianalytic models (SAMs). SAMs predict longer formation timescales and older ages similar to 2 Gyr, which are nearly twice as old as the estimates of the tau models. Both models yield good spectral energy distribution fits, indicating that the systematic uncertainty in the age due to degeneracies in the SFH is of that order of magnitude. However, SAM SFHs better match the observed slope and zero point of the SFR-mass main sequence. Contrary to expectations, some low-mass compact SFGs (log(M/M-circle dot) = 10-10.6) have younger ages but lower specific SFRs than that of more massive galaxies, suggesting that the low-mass galaxies reach the red sequence faster. If the progenitors of compact SFGs are extended SFGs, state-of-the-art SAMs show that mergers and disk instabilities (DIs) are both able to shrink galaxies, but DIs are more frequent (60% versus 40%) and form more concentrated galaxies. We confirm this result via high-resolution hydrodynamic simulations. C1 [Barro, G.; Faber, S. M.; Koo, D. C.; Guo, Y.; Tal, T.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Barro, G.; Faber, S. M.; Koo, D. C.; Guo, Y.; Tal, T.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Perez-Gonzalez, P. G.] Univ Complutense Madrid, F CC Fis, E-28040 Madrid, Spain. [Perez-Gonzalez, P. G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Perez-Gonzalez, P. G.; Lee, J.] Yonsei Univ, Yonsei Univ Observ, Seoul 120749, South Korea. [Trump, J. R.] Penn State Univ, University Pk, PA 16802 USA. [Wuyts, S.; Hsu, L.; Salvato, M.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Bell, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Dekel, A.; Zolotov, A.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [Porter, L.; Primack, J.; Kollipara, P.; Moody, C.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Ferguson, H.; Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ashby, M. L. N.; Fazio, G. G.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Caputi, K.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Ceverino, D.] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain. [Croton, D.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Giavalisco, M.; Williams, C. C.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kocevski, D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Kurczynski, P.; Somerville, R.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [McIntosh, D. H.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [McGrath, E.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [Papovich, C.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Santini, P.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [van der Wel, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Barro, G (reprint author), Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RI Perez-Gonzalez, Pablo/J-2871-2016; OI Perez-Gonzalez, Pablo/0000-0003-4528-5639; Santini, Paola/0000-0002-9334-8705; Koekemoer, Anton/0000-0002-6610-2048; Bell, Eric/0000-0002-5564-9873 FU NASA from the Space Telescope Science Institute [HST-GO-12060]; Association of Universities for Research in Astronomy, Incorporated, under NASA [NAS5-26555]; KASI-Yonsei Joint Research Program - Korea Astronomy and Space Science Institute; National Research Foundation of Korea through the SRC grant; Doyak grant [20090078756]; NSF [AST-08-08133]; [AYA2012-31277-E] FX We thank David Elbaz for very useful discussions. Support for Program number HST-GO-12060 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. G.B. acknowledges support from NSF grant AST-08-08133. P.G.P.-G. acknowledges support from grant AYA2012-31277-E. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). C.P. acknowledges the support by the KASI-Yonsei Joint Research Program for the Frontiers of Astronomy and Space Science funded by the Korea Astronomy and Space Science Institute. J.L. acknowledges the support by the National Research Foundation of Korea through the SRC grant to the Center for Galaxy Evolution Research and the Doyak grant (No. 20090078756). NR 201 TC 50 Z9 50 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 AUG 10 PY 2014 VL 791 IS 1 AR 52 DI 10.1088/0004-637X/791/1/52 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700052 ER PT J AU Betremieux, Y Kaltenegger, L AF Betremieux, Yan Kaltenegger, Lisa TI IMPACT OF ATMOSPHERIC REFRACTION: HOW DEEPLY CAN WE PROBE EXO-EARTH'S ATMOSPHERES DURING PRIMARY ECLIPSE OBSERVATIONS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; Earth; line: identification; methods: analytical; planets and satellites: atmospheres; radiative transfer ID TRANSMISSION SPECTRUM; LUNAR ECLIPSE; PLANETS; TRANSITS; SPECTROSCOPY; EXOPLANET; STARS AB Most models used to predict or fit exoplanet transmission spectra do not include all the effects of atmospheric refraction. Namely, the angular size of the star with respect to the planet can limit the lowest altitude, or highest density and pressure, probed during primary eclipses as no rays passing below this critical altitude can reach the observer. We discuss this geometrical effect of refraction for all exoplanets and tabulate the critical altitude, density, and pressure for an exoplanet identical to Earth with a 1 bar N-2/O-2 atmosphere as a function of both the incident stellar flux (Venus, Earth, and Mars-like) at the top of the atmosphere and the spectral type (O5-M9) of the host star. We show that such a habitable exo-Earth can be probed to a surface pressure of 1 bar only around the coolest stars. We present 0.4-5.0 mu m model transmission spectra of Earth's atmosphere viewed as a transiting exoplanet, and show how atmospheric refraction modifies the transmission spectrum depending on the spectral type of the host star. We demonstrate that refraction is another phenomenon that can potentially explain flat transmission spectra over some spectral regions. 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 [ENPKa3142/1-1]; Simons Foundation [290357] FX The authors acknowledge support from DFG funding ENPKa3142/1-1 and the Simons Foundation (290357, Kaltenegger). NR 24 TC 13 Z9 13 U1 0 U2 13 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 2014 VL 791 IS 1 AR 7 DI 10.1088/0004-637X/791/1/7 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700007 ER PT J AU Degenaar, N Medin, Z Cumming, A Wijnands, R Wolff, MT Cackett, EM Miller, JM Jonker, PG Homan, J Brown, EF AF Degenaar, N. Medin, Z. Cumming, A. Wijnands, R. Wolff, M. T. Cackett, E. M. Miller, J. M. Jonker, P. G. Homan, J. Brown, E. F. TI PROBING THE CRUST OF THE NEUTRON STAR IN EXO 0748-676 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: eclipsing; stars: individual (EXO 0748-676); stars: neutron; X-rays: binaries ID X-RAY TRANSIENT; PHOTON IMAGING CAMERA; COOLING LIGHT CURVES; BINARY MXB 1659-29; XMM-NEWTON; CEN X-4; QUIESCENT STATE; XTE J1701-462; KS 1731-260; TERZAN 5 AB X-ray observations of quiescent X-ray binaries have the potential to provide insight into the structure and the composition of neutron stars. EXO 0748-676 had been actively accreting for over 24 yr before its outburst ceased in late 2008. Subsequent X-ray monitoring revealed a gradual decay of the quiescent thermal emission that can be attributed to cooling of the accretion-heated neutron star crust. In this work, we report on new Chandra and Swift observations that extend the quiescent monitoring to similar or equal to 5 yr post-outburst. We find that the neutron star temperature remained at similar or equal to 117 eV between 2009 and 2011, but had decreased to similar or equal to 110 eV in 2013. This suggests that the crust has not fully cooled yet, which is supported by the lower temperature (similar or equal to 95 eV) measured similar or equal to 4 yr prior to the accretion phase in 1980. Comparing the data to thermal evolution simulations reveals that the apparent lack of cooling between 2009 and 2011 could possibly be a signature of convection driven by phase separation of light and heavy nuclei in the outer layers of the neutron star. C1 [Degenaar, N.; Miller, J. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Medin, Z.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Cumming, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Wolff, M. T.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Cackett, E. M.] Wayne State Univ, Dept Phys & Astron, Detroit, MI 48201 USA. [Jonker, P. G.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Homan, J.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Brown, E. F.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Degenaar, N (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM degenaar@umich.edu OI Brown, Edward/0000-0003-3806-5339 FU NASA through Hubble Postdoctoral Fellowship from the Space Telescope Science Institute (STScI) [HST-HF-51287.01-A]; NASA through Chandra award [GO3-14050X]; National Aeronautics and Space Administration (NASA) [NAS8-03060, NAS 5-26555]; NSERC Discovery Grant; Office of Naval Research FX N.D. is supported by NASA through Hubble Postdoctoral Fellowship grant number HST-HF-51287.01-A from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Incorporated, under the National Aeronautics and Space Administration (NASA) contract NAS 5-26555. Support for this work was provided by the NASA through Chandra award No. GO3-14050X 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. A.C. is supported by an NSERC Discovery Grant and is an Associate Member of the CIFAR Cosmology and Gravity program. M.T.W. is supported by the Office of Naval Research. The authors are grateful to Neil Gehrels and the Swift planning team for approving and scheduling the Swift TOO observations of EXO 0748-676. N.D., A.C., R.W., E.C., and E.B. acknowledge the hospitality of the International Space Science Institute in Bern, Switzerland, where part of this work was carried out. The authors are grateful to the anonymous referee and Joel Fridriksson for very useful comments. NR 78 TC 14 Z9 14 U1 1 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 AUG 10 PY 2014 VL 791 IS 1 AR 47 DI 10.1088/0004-637X/791/1/47 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700047 ER PT J AU Hung, CL Sanders, DB Casey, CM Koss, M Larson, KL Lee, N Li, YX Lockhart, K Shih, HY Barnes, JE Kartaltepe, JS Smith, HA AF Hung, Chao-Ling Sanders, D. B. Casey, Caitlin M. Koss, Michael Larson, Kirsten L. Lee, Nicholas Li, Yanxia Lockhart, Kelly Shih, Hsin-Yi Barnes, Joshua E. Kartaltepe, Jeyhan S. Smith, Howard A. TI A COMPARISON OF THE MORPHOLOGICAL PROPERTIES BETWEEN LOCAL AND z similar to 1 INFRARED LUMINOUS GALAXIES: ARE LOCAL AND HIGH-z (U) LIRGS DIFFERENT? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: structure; infrared: galaxies ID STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; HERSCHEL-SELECTED GALAXIES; ACTIVE GALACTIC NUCLEI; PASSIVE GALAXIES; REDSHIFT SURVEY; MAJOR MERGERS; DATA RELEASE; TIME-SCALES; SAMPLE AB Ultraluminous and luminous infrared galaxies (ULIRGs and LIRGs) are the most extreme star-forming galaxies in the universe and dominate the total star formation rate density atz > 1. In the local universe (z < 0.3), the majority of ULIRGs and a significant portion of LIRGs are triggered by interactions between gas-rich spiral galaxies, yet it is unclear if this is still the case at high z. To investigate the relative importance of galaxy interactions in infrared luminous galaxies, we carry out a comparison of optical morphological properties between local (U) LIRGs and (U) LIRGs at z = 0.5-1.5 based on the same sample selection, morphology classification scheme, and optical morphology at similar rest-frame wavelengths. In addition, we quantify the systematics in comparing local and high-z data sets by constructing a redshifted data set from local (U) LIRGs, in which its data quality mimics the high-z data set. Based on the Gini-M20 classification scheme, we find that the fraction of interacting systems decreases by similar to 8% from local to z less than or similar to 1, and it is consistent with the reduction between local and redshifted data sets (6(-6)(+14) %). Based on visual classifications, the merger fraction of local ULIRGs is found to be 20% lower compared to published results, and the reduction due to redshifting is 15+10 -8 %. Consequently, the differences of merger fractions between local and z less than or similar to 1 (U) LIRGs is only 17%. These results demonstrate that there is no strong evolution in the fraction of (U) LIRGs classified as mergers at least out to z 1. At z > 1, the morphology types of 30% of (U) LIRGs cannot be determined due to their faintness in the F814W band; thus, the merger fraction measured at z > 1 suffers from large uncertainties. C1 [Hung, Chao-Ling; Sanders, D. B.; Larson, Kirsten L.; Lee, Nicholas; Li, Yanxia; Lockhart, Kelly; Shih, Hsin-Yi; Barnes, Joshua E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Hung, Chao-Ling; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Casey, Caitlin M.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Koss, Michael] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Kartaltepe, Jeyhan S.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Hung, CL (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM clhung@ifa.hawaii.edu RI Koss, Michael/B-1585-2015; OI Koss, Michael/0000-0002-7998-9581; Casey, Caitlin/0000-0002-0930-6466 FU NASA [NNX11AB02G, NNX14AJ61G]; Smithsonian Astrophysical Observatory Predoctoral Fellowship; SAO [AR3-14011X] FX We thank the referee for constructive comments that have helped us to improve the quality of this paper. C.-L. H. acknowledges the funding support from NASA grants NNX11AB02G and NNX14AJ61G and the Smithsonian Astrophysical Observatory Predoctoral Fellowship. D. B. S. and K. L. L. gratefully acknowledge support from NASA grant NNX11AB02G, and N. L. acknowledges support from SAO grant AR3-14011X.; Part of the data presented in this paper has been made available by the COSMOS team (http://cosmos. astro. caltech. edu). COSMOS is based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA Inc., under NASA contract NAS 5-26555; also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; the XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation; the National Radio Astronomy Observatory, which is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.; and the CanadaFrance-Hawaii Telescope operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France and the University of Hawaii.; This paper has made use of the NASA/IPAC Extragalactic Database (NED) and IPAC Infrared Science Archive, which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with 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-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This work has also made use of data products from the Sloan Digital Sky Survey Data Release 7. 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 JapaneseMonbukagakusho, theMax Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www. sdss. org/. NR 61 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 AUG 10 PY 2014 VL 791 IS 1 AR 63 DI 10.1088/0004-637X/791/1/63 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700063 ER PT J AU Law, NM Morton, T Baranec, C Riddle, R Ravichandran, G Ziegler, C Johnson, JA Tendulkar, SP Bui, K Burse, MP Das, HK Dekany, RG Kulkarni, S Punnadi, S Ramaprakash, AN AF Law, Nicholas M. Morton, Tim Baranec, Christoph Riddle, Reed Ravichandran, Ganesh Ziegler, Carl Johnson, John Asher Tendulkar, Shriharsh P. Bui, Khanh Burse, Mahesh P. Das, H. K. Dekany, Richard G. Kulkarni, Shrinivas Punnadi, Sujit Ramaprakash, A. N. TI ROBOTIC LASER ADAPTIVE OPTICS IMAGING OF 715 KEPLER EXOPLANET CANDIDATES USING ROBO-AO SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; instrumentation: adaptive optics; instrumentation: high angular resolution; methods: data analysis; methods: observational; planetary systems; planets and satellites: detection; planets and satellites: fundamental parameters ID ASTROPHYSICAL FALSE POSITIVES; PLANET CANDIDATES; HOST STARS; TELESCOPE; MISSION; BINARY; LUCKY; ORBITS; MULTIPLICITY; OBJECTS AB The Robo-AO Kepler Planetary Candidate Survey is observing every Kepler planet candidate host star with laser adaptive optics imaging to search for blended nearby stars, which may be physically associated companions and/or responsible for transit false positives. In this paper, we present the results from the 2012 observing season, searching for stars close to 715 Kepler planet candidate hosts. We find 53 companions, 43 of which are new discoveries. We detail the Robo-AO survey data reduction methods including a method of using the large ensemble of target observations as mutual point-spread-function references, along with a new automated companion-detection algorithm designed for large adaptive optics surveys. Our survey is sensitive to objects from approximate to 0 ''.15 to 2 ''.5 separation, with magnitude differences up to Delta m approximate to 6. We measure an overall nearby-star probability for Kepler planet candidates of 7.4% +/- 1.0%, and calculate the effects of each detected nearby star on the Kepler-measured planetary radius. We discuss several Kepler Objects of Interest (KOIs) of particular interest, including KOI-191 and KOI-1151, which are both multi-planet systems with detected stellar companions whose unusual planetary system architecture might be best explained if they are "coincident multiple" systems, with several transiting planets shared between the two stars. Finally, we find 98% confidence evidence that short-period giant planets are two to three times more likely than longer-period planets to be found in wide stellar binaries. C1 [Law, Nicholas M.; Ziegler, Carl] Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. [Morton, Tim; Riddle, Reed; Tendulkar, Shriharsh P.; Bui, Khanh; Dekany, Richard G.; Kulkarni, Shrinivas; Punnadi, Sujit] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Baranec, Christoph] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Ravichandran, Ganesh] West Tresper Clarke High Sch, Westbury, NY 11590 USA. [Johnson, John Asher] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burse, Mahesh P.; Das, H. K.; Ramaprakash, A. N.] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. RP Law, NM (reprint author), Univ N Carolina, Dept Phys & Astron, Chapel Hill, NC 27599 USA. FU California Institute of Technology; Inter-University Centre for Astronomy and Astrophysics; National Science Foundation [AST-0906060, AST-0960343]; Mount Cuba Astronomical Foundation; Alfred P. Sloan Foundation; David and Lucile Packard Foundation FX We thank the anonymous referee for careful analysis and useful comments on the manuscript. The Robo-AO system is supported by collaborating partner institutions, the California Institute of Technology and the Inter-University Centre for Astronomy and Astrophysics, and by the National Science Foundation under grant Nos. AST-0906060 and AST-0960343, by the Mount Cuba Astronomical Foundation, by a gift from Samuel Oschin. We are grateful to the Palomar Observatory staff for their ongoing support of Robo-AO on the 60 inch telescope,particularly S. Kunsman, M. Doyle, J. Henning, R. Walters, G. Van Idsinga, B. Baker, K. Dunscombe and D. Roderick. 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. C.B. and J.A.J. acknowledge support from the Alfred P. Sloan Foundation. J.A.J. acknowledges support from the David and Lucile Packard Foundation. NR 45 TC 57 Z9 57 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 AUG 10 PY 2014 VL 791 IS 1 AR 35 DI 10.1088/0004-637X/791/1/35 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700035 ER PT J AU Medina, AA Raymond, JC Edgar, RJ Caldwell, N Fesen, RA Milisavljevic, D AF Medina, Amber A. Raymond, John C. Edgar, Richard J. Caldwell, Nelson Fesen, Robert A. Milisavljevic, Dan TI ELECTRON-ION EQUILIBRIUM AND SHOCK PRECURSORS IN THE NORTHEAST LIMB OF THE CYGNUS LOOP SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; ISM: individual objects (Cygnus Loop); ISM: supernova remnants; shock waves ID BALMER-DOMINATED SHOCKS; TYCHOS SUPERNOVA REMNANT; HIGH-RESOLUTION SPECTROSCOPY; NONRADIATIVE SHOCK; EMISSION; WAVES; TELESCOPE; SPECTRUM; SN-1006; RCW-86 AB We present an observational study using high-resolution echelle spectroscopy of collisionless shocks in the Cygnus Loop supernova remnant. Measured H alpha line profiles constrain pre-shock heating processes, shock speeds, and electron-ion equilibration (T-e/T-i). The shocks produce faint H alpha emission line profiles, which are characterized by narrow and broad components. The narrow component is representative of the pre-shock conditions, while the broad component is produced after charge transfer between neutrals entering the shock and protons in the post-shock gas, thus reflecting the properties of the post-shock gas. We observe a diffuse H alpha region extending about 2'.5 ahead of the shock with line width similar to 29 km s(-1), while the H alpha profile of the shock itself consists of broader than expected narrow (36 km s(-1)) and broad (250 km s(-1)) components. The observed diffuse emission arises in a photoionization precursor heated to about 18,000 K by He I and He II emission from the shock, with additional narrow component broadening originating from a thin cosmic-ray precursor. Broad to narrow component intensity ratios of similar to 1.0 imply full electron-ion temperature equilibration T-e similar or equal to T-i in the post-shock region. Broad component line widths indicate shock velocities of about 400 km s(-1). Combining the shock velocities with proper motions suggests that the distance to the Cygnus Loop is similar to 890 pc, significantly greater than the generally accepted upper limit of 637 pc. C1 [Medina, Amber A.; Raymond, John C.; Edgar, Richard J.; Caldwell, Nelson; Milisavljevic, Dan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Medina, Amber A.] New Mexico State Univ, Dept Phys, Las Cruces, NM 88003 USA. [Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. RP Medina, AA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amedina@cfa.harvard.edu; jraymond@cfa.harvard.edu; edgar@head.cfa.harvard.edu FU National Science Foundation REU; Department of Defense ASSURE programs under NSF [1262851]; Smithsonian Institution [HST-60-12885] FX This work is supported by the National Science Foundation REU and Department of Defense ASSURE programs under NSF Grant no. 1262851 and by the Smithsonian Institution. This work was partially supported by the grant HST-60-12885 to the Smithsonian Institution. NR 64 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 2014 VL 791 IS 1 AR 30 DI 10.1088/0004-637X/791/1/30 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700030 ER PT J AU Melendez, J Ramirez, I Karakas, AI Yong, D Monroe, TR Bedell, M Bergemann, M Asplund, M Maia, MT Bean, J do Nascimento, JD Bazot, M Alves-Brito, A Freitas, FC Castro, M AF Melendez, Jorge Ramirez, Ivan Karakas, Amanda I. Yong, David Monroe, TalaWanda R. Bedell, Megan Bergemann, Maria Asplund, Martin Maia, Marcelo Tucci Bean, Jacob do Nascimento, Jose-Dias, Jr. Bazot, Michael Alves-Brito, Alan Freitas, Fabricio C. Castro, Matthieu TI 18 Sco: A SOLAR TWIN RICH IN REFRACTORY AND NEUTRON-CAPTURE ELEMENTS. IMPLICATIONS FOR CHEMICAL TAGGING SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: abundances; stars: AGB and post-AGB; stars: fundamental parameters; Sun: abundances ID PLANET SEARCH PROGRAM; GIANT BRANCH MODELS; METAL-POOR STARS; SUN-LIKE STARS; OPEN CLUSTERS; Y-2 ISOCHRONES; S-PROCESS; R-PROCESS; LITHIUM ABUNDANCE; NLTE ABUNDANCES AB We study with unprecedented detail the chemical composition and stellar parameters of the solar twin 18 Sco in a strictly differential sense relative to the Sun. Our study is mainly based on high-resolution (R similar to 110,000), high signal-to-noise ratio (800-1,000) Very Large Telescope UVES spectra, which allow us to achieve a precision of about 0.005 dex in differential abundances. The effective temperature and surface gravity of 18 Sco are T-eff = 5823 +/- 6 K and log g = 4.45 +/- 0.02 dex, i.e., 18 Sco is 46 +/- 6 K hotter than the Sun and log g is 0.01 +/- 0.02 dex higher. Its metallicity is [Fe/H] = 0.054 +/- 0.005 dex, and its microturbulence velocity is +0.02 +/- 0.01 km s-1 higher than solar. Our precise stellar parameters and differential isochrone analysis show that 18 Sco has a mass of 1.04 +/- 0.02 M-circle dot and that it is similar to 1.6 Gyr younger than the Sun. We use precise High Accuracy Radial velocity Planet Searcher (HARPS) radial velocities to search for planets, but none are detected. The chemical abundance pattern of 18 Sco displays a clear trend with condensation temperature, thus showing higher abundances of refractories in 18 Sco than in the Sun. Intriguingly, there are enhancements in the neutron-capture elements relative to the Sun. Despite the small element-to-element abundance differences among nearby n-capture elements (similar to 0.02 dex), we successfully reproduce the r-process pattern in the Solar System. This is independent evidence for the universality of the r process. Our results have important implications for chemical tagging in our Galaxy and nucleosynthesis in general. C1 [Melendez, Jorge; Monroe, TalaWanda R.; Maia, Marcelo Tucci; Freitas, Fabricio C.] Univ Sao Paulo, Dept Astron, IAG USP, BR-05508900 Sao Paulo, Brazil. [Ramirez, Ivan] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Ramirez, Ivan] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Karakas, Amanda I.; Yong, David; Asplund, Martin] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Bedell, Megan; Bean, Jacob] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Bergemann, Maria] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [do Nascimento, Jose-Dias, Jr.] Univ Fed Rio Grande do Norte, Dept Fis Teor & Expt, BR-59072970 Natal, RN, Brazil. [do Nascimento, Jose-Dias, Jr.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bazot, Michael] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Alves-Brito, Alan] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil. RP Melendez, J (reprint author), Univ Sao Paulo, Dept Astron, IAG USP, Rua Matao 1226, BR-05508900 Sao Paulo, Brazil. EM jorge.melendez@iag.usp.br RI Castro, Matthieu/E-9247-2013; do Nascimento, Jose Dias/D-2416-2014; Melendez, Jorge/J-4002-2016 OI do Nascimento, Jose Dias/0000-0001-7804-2145; Melendez, Jorge/0000-0002-4933-2239 FU FAPESP [2012/24392-2, 2010/19810-4]; NSF [AST-1313119] FX and T. R. M. acknowledge support from FAPESP (2012/24392-2 and 2010/19810-4). M. B. and J. B. acknowledge support for this work from the NSF (grant No. AST-1313119) NR 83 TC 20 Z9 20 U1 2 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 2014 VL 791 IS 1 AR 14 DI 10.1088/0004-637X/791/1/14 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700014 ER PT J AU Pan, LB Padoan, P Scalo, J AF Pan, Liubin Padoan, Paolo Scalo, John TI TURBULENCE-INDUCED RELATIVE VELOCITY OF DUST PARTICLES. II. THE BIDISPERSE CASE SO ASTROPHYSICAL JOURNAL LA English DT Article DE minor planets, asteroids: general; planets and satellites: formation; protoplanetary disks; turbulence ID INERTIAL PARTICLES; ISOTROPIC TURBULENCE; PROTOPLANETARY DISKS; COLLISION RATES; GROWTH PEBBLES; PAIR DISPERSION; SOLAR NEBULA; GRAINS; PLANETESIMALS; BOULDERS AB We extend our earlier work on turbulence-induced relative velocity between equal-size particles ( Paper I, in this series) to particles of arbitrarily different sizes. The Pan & Padoan (PP10) model shows that the relative velocity between different particles has two contributions, named the generalized shear and acceleration terms, respectively. The generalized shear term represents the particles' memory of the spatial flow velocity difference across the particle distance in the past, while the acceleration term is associated with the temporal flow velocity difference on individual particle trajectories. Using the simulation of Paper I, we compute the root-mean-square relative velocity, < w(2)>(1/2), as a function of the friction times, tau(p1) and tau(p2), of the two particles and show that the PP10 prediction is in satisfactory agreement with the data, confirming its physical picture. For a given tau(p1) below the Lagrangian correlation time of the flow, T-L, < w(2)>(1/2) as a function of tau(p2) shows a dip at tau(p2) similar or equal to tau(p1), indicating tighter velocity correlation between similar particles. Defining a ratio f equivalent to tau(p,1)/tau(p,h), with tau(p,1) and tau(p,h) the friction times of the smaller and larger particles, we find that < w(2)>(1/2) increases with decreasing f due to the generalized acceleration contribution, which dominates at f less than or similar to 1/4. At a fixed f, our model predicts that < w(2)>(1/2) scales as tau(1/2)(p,h) tau(p,h) for in the inertial range of the flow, stays roughly constant for T-L less than or similar to tau(p,h) less than or similar to T-L/f, and finally decreases as tau(-1/2)(p,h) p, h for tau(p,h) >> T-L/f. The acceleration term is independent of the particle distance, r, and reduces the r dependence of < w(2)>(1/2) in the bidisperse case. C1 [Pan, Liubin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Padoan, Paolo] Univ Barcelona, ICREA, E-08028 Barcelona, Spain. [Padoan, Paolo] Univ Barcelona, ICC, E-08028 Barcelona, Spain. [Scalo, John] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Pan, LB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lpan@cfa.harvard.edu; ppadoan@icc.ub.edu; parrot@astro.as.utexas.edu OI Padoan, Paolo/0000-0002-5055-5800 FU Clay Fellowship at Harvard-Smithsonian Center for Astrophysics; FP7-PEOPLE-2010-RG [PIRG07-GA-2010-261359] FX Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center and by the Port d'Informacio Cientifica (PIC), Spain, maintained by a collaboration of the Institut de Fsica d'Altes Energies (IFAE) and the Centro de Investigaciones Energticas, Medioam-bientales y Tecnolgicas (CIEMAT). L.P. is supported by a Clay Fellowship at Harvard-Smithsonian Center for Astrophysics. P.P. acknowledges support by the FP7-PEOPLE-2010-RG grant PIRG07-GA-2010-261359. NR 43 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 AUG 10 PY 2014 VL 791 IS 1 AR 48 DI 10.1088/0004-637X/791/1/48 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700048 ER PT J AU Slater, CT Bell, EF Schlafly, EF Morganson, E Martin, NF Rix, HW Penarrubia, J Bernard, EJ Ferguson, AMN Martinez-Delgado, D Wyse, RFG Burgett, WS Chambers, KC Draper, PW Hodapp, KW Kaiser, N Magnier, EA Metcalfe, N Price, PA Tonry, JL Wainscoat, RJ Waters, C AF Slater, Colin T. Bell, Eric F. Schlafly, Edward F. Morganson, Eric Martin, Nicolas F. Rix, Hans-Walter Penarrubia, Jorge Bernard, Edouard J. Ferguson, Annette M. N. Martinez-Delgado, David Wyse, Rosemary F. G. Burgett, William S. Chambers, Kenneth C. Draper, Peter W. Hodapp, Klaus W. Kaiser, Nicholas Magnier, Eugene A. Metcalfe, Nigel Price, Paul A. Tonry, John L. Wainscoat, Richard J. Waters, Christopher TI THE COMPLEX STRUCTURE OF STARS IN THE OUTER GALACTIC DISK AS REVEALED BY PAN-STARRS1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: interactions; Galaxy: disk; Galaxy: structure ID MAJOR DWARF GALAXY; HIERARCHICAL SATELLITE ACCRETION; ANTICENTER STELLAR STRUCTURE; EXPLORING HALO SUBSTRUCTURE; DARK-MATTER SUBSTRUCTURE; RADIAL-VELOCITY SURVEY; MILKY-WAY; MONOCEROS RING; CANIS-MAJOR; LATITUDE STRUCTURES AB We present a panoptic view of the stellar structure in the Galactic disk's outer reaches commonly known as the Monoceros Ring, based on data from Pan-STARRS1. These observations clearly show the large extent of the stellar overdensities on both sides of the Galactic disk, extending between b = -25 degrees and b = +35 degrees and covering over 130 degrees in Galactic longitude. The structure exhibits a complex morphology with both stream-like features and a sharp edge to the structure in both the north and the south. We compare this map to mock observations of two published simulations aimed at explaining such structures in the outer stellar disk, one postulating an origin as a tidal stream and the other demonstrating a scenario where the disk is strongly distorted by the accretion of a satellite. These morphological comparisons of simulations can link formation scenarios to observed structures, such as demonstrating that the distorted-disk model can produce thin density features resembling tidal streams. Although neither model produces perfect agreement with the observations-the tidal stream predicts material at larger distances that is not detected while in the distorted disk model, the midplane is warped to an excessive degree-future tuning of the models to accommodate these latest data may yield better agreement. C1 [Slater, Colin T.; Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Schlafly, Edward F.; Martin, Nicolas F.; Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Morganson, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martin, Nicolas F.] Univ Strasbourg, CNRS, UMR 7550, Observ Astron Strasbourg, F-67000 Strasbourg, France. [Penarrubia, Jorge; Bernard, Edouard J.; Ferguson, Annette M. N.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Martinez-Delgado, David] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Wyse, Rosemary F. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Burgett, William S.; Chambers, Kenneth C.; Hodapp, Klaus W.; Kaiser, Nicholas; Magnier, Eugene A.; Tonry, John L.; Wainscoat, Richard J.; Waters, Christopher] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Draper, Peter W.; Metcalfe, Nigel] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Price, Paul A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Slater, CT (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM ctslater@umich.edu; ericbell@umich.edu OI Bernard, Edouard/0000-0002-8722-225X; Chambers, Kenneth /0000-0001-6965-7789; Metcalfe, Nigel/0000-0001-9034-4402; Bell, Eric/0000-0002-5564-9873; Schlafly, Edward Ford/0000-0002-3569-7421 FU NSF [AST 1008342]; DFG's "The Milky Way System" [SFB 881]; CNRS through PICS [PICS06183]; European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC [321035]; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G] FX We thank S. Kazantzidis for generously providing his simulation outputs. C. T. S. and E. F. B. were supported during this work by NSF grant AST 1008342. E. F. S., E. M., and N.F.M. acknowledge support from the DFG's SFB 881 grant "The Milky Way System" (sub-prdoject A3). N. F. M. gratefully acknowledges the CNRS for support through PICS project PICS06183. H. W. R. acknowledges support from the European Research Council under the European Union's Seventh Framework Programme (FP 7) ERC grant Agreement no. [321035]. The PS1 Survey has 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, Queens 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 49 TC 16 Z9 16 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 2014 VL 791 IS 1 AR 9 DI 10.1088/0004-637X/791/1/9 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700009 ER PT J AU Song, MM Finkelstein, SL Gebhardt, K Hill, GJ Drory, N Ashby, MLN Blanc, GA Bridge, J Chonis, T Ciardullo, R Fabricius, M Fazio, GG Gawiser, E Gronwall, C Hagen, A Huang, JS Jogee, S Livermore, R Salmon, B Schneider, DP Willner, SP Zeimann, GR AF Song, Mimi Finkelstein, Steven L. Gebhardt, Karl Hill, Gary J. Drory, Niv Ashby, Matthew L. N. Blanc, Guillermo A. Bridge, Joanna Chonis, Taylor Ciardullo, Robin Fabricius, Maximilian Fazio, Giovanni G. Gawiser, Eric Gronwall, Caryl Hagen, Alex Huang, Jia-Sheng Jogee, Shardha Livermore, Rachael Salmon, Brett Schneider, Donald P. Willner, S. P. Zeimann, Gregory R. TI THE HETDEX PILOT SURVEY. V. THE PHYSICAL ORIGIN OF Ly alpha EMITTERS PROBED BY NEAR-INFRARED SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: high-redshift; galaxies: ISM ID STAR-FORMING GALAXIES; LYMAN-BREAK GALAXIES; MASS-METALLICITY RELATION; EMISSION-LINE GALAXIES; SIMILAR-TO 2; HIGH-REDSHIFT GALAXIES; CONTINUUM-SELECTED GALAXIES; EXTRAGALACTIC LEGACY SURVEY; FRAME ULTRAVIOLET-SPECTRA; SPACE-TELESCOPE SEARCH AB We present the results from a Very Large Telescope/SINFONI and Keck/NIRSPEC near-infrared spectroscopic survey of 16 Ly alpha emitters (LAEs) at z = 2.1-2.5 in the COSMOS and GOODS-N fields discovered from the Hobby Eberly Telescope Dark Energy Experiment Pilot Survey. We detect rest-frame optical nebular lines (H alpha and/or [O III] lambda 5007) for 10 of the LAEs and measure physical properties, including the star formation rate (SFR), gas-phase metallicity, gas mass fraction, and Ly alpha velocity offset. We find that LAEs may lie below the mass-metallicity relation for continuum-selected star-forming galaxies at the same redshift. The LAEs all show velocity shifts of Ly alpha relative to the systemic redshift ranging between +85 and +296 km s(-1) with a mean of +180 km s(-1). This value is smaller than measured for continuum-selected star-forming galaxies at similar redshifts. The Ly alpha velocity offsets show a moderate correlation with the measured SFR (2.5 sigma), but no significant correlations are seen with the SFR surface density, specific SFR, stellar mass, or dynamical mass (less than or similar to 1.5 sigma). Exploring the role of dust, kinematics of the interstellar medium (ISM), and geometry on the escape of Ly alpha photons, we find no signature of selective quenching of resonantly scattered Ly alpha photons. However, we also find no evidence that a clumpy ISM is enhancing the Ly alpha equivalent width. Our results suggest that the low metallicity in LAEs may be responsible for yielding an environment with a low neutral hydrogen column density and less dust, easing the escape of Ly alpha photons over that in continuum-selected star-forming galaxies. C1 [Song, Mimi; Finkelstein, Steven L.; Gebhardt, Karl; Hill, Gary J.; Drory, Niv; Chonis, Taylor; Jogee, Shardha; Livermore, Rachael] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Ashby, Matthew L. N.; Fazio, Giovanni G.; Huang, Jia-Sheng; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blanc, Guillermo A.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Bridge, Joanna; Ciardullo, Robin; Gronwall, Caryl; Hagen, Alex; Schneider, Donald P.; Zeimann, Gregory R.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Bridge, Joanna; Ciardullo, Robin; Gronwall, Caryl; Hagen, Alex; Schneider, Donald P.; Zeimann, Gregory R.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Fabricius, Maximilian; Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Fazio, Giovanni G.; Salmon, Brett] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. RP Song, MM (reprint author), Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. EM mmsong@astro.as.utexas.edu RI Blanc, Guillermo/I-5260-2016 FU University of Texas at Austin; McDonald Observatory; NASA through a NASA Keck PI Data Award; W. M. Keck Foundation; National Science Foundation [AST-0926815] FX We thank Joshua J. Adams and E. Robinson for helpful discussions and comments that improved this paper. M.S. and S.L.F. acknowledge support from the University of Texas at Austin, the McDonald Observatory, and NASA through a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. This research is based on observations made with the European Southern Observatory Very Large Telescope, under program ID 086. A-0424(A) and 088. A-0154(A), and with the Keck Telescope from telescope time allocated to NASA through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the financial support of the W. M. Keck Foundation. We recognize and acknowledge the cultural role and reverence that the summit of Mauna Kea has within the indigenous Hawaiian community. This work is also based in part 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, as well as the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This research is supported by the National Science Foundation under grant AST-0926815. NR 161 TC 28 Z9 28 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 2014 VL 791 IS 1 AR 3 DI 10.1088/0004-637X/791/1/3 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM2CY UT WOS:000339657700003 ER PT J AU He, Q Bertness, MD Bruno, JF Li, B Chen, GQ Coverdale, TC Altieri, AH Bai, JH Sun, T Pennings, SC Liu, JG Ehrlich, PR Cui, BS AF He, Qiang Bertness, Mark D. Bruno, John F. Li, Bo Chen, Guoqian Coverdale, Tyler C. Altieri, Andrew H. Bai, Junhong Sun, Tao Pennings, Steven C. Liu, Jianguo Ehrlich, Paul R. Cui, Baoshan TI Economic development and coastal ecosystem change in China SO SCIENTIFIC REPORTS LA English DT Article ID ENVIRONMENTAL KUZNETS CURVE; CLIMATE-CHANGE; CO2 EMISSIONS; MARINE ECOSYSTEMS; HUMAN IMPACTS; SOUTH CHINA; GROWTH; SEA; DEFORESTATION; DEGRADATION AB Despite their value, coastal ecosystems are globally threatened by anthropogenic impacts, yet how these impacts are driven by economic development is not well understood. We compiled a multifaceted dataset to quantify coastal trends and examine the role of economic growth in China's coastal degradation since the 1950s. Although China's coastal population growth did not change following the 1978 economic reforms, its coastal economy increased by orders of magnitude. All 15 coastal human impacts examined increased over time, especially after the reforms. Econometric analysis revealed positive relationships between most impacts and GDP across temporal and spatial scales, often lacking dropping thresholds. These relationships generally held when influences of population growth were addressed by analyzing per capita impacts, and when population density was included as explanatory variables. Historical trends in physical and biotic indicators showed that China's coastal ecosystems changed little or slowly between the 1950s and 1978, but have degraded at accelerated rates since 1978. Thus economic growth has been the cause of accelerating human damage to China's coastal ecosystems. China's GDP per capita remains very low. Without strict conservation efforts, continuing economic growth will further degrade China's coastal ecosystems. C1 [He, Qiang; Bai, Junhong; Sun, Tao; Cui, Baoshan] Beijing Normal Univ, Sch Environm, State Key Lab Water Environm Simulat, Beijing 100875, Peoples R China. [Bertness, Mark D.; Coverdale, Tyler C.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Bruno, John F.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Li, Bo] Fudan Univ, Inst Biodivers Sci, Coastal Ecosyst Res Stn Yangtze River Estuary, Shanghai 200433, Peoples R China. [Chen, Guoqian] Peking Univ, Coll Engn, Div Climate Change Thermodynam & Syst Ecol, Beijing 100871, Peoples R China. [Chen, Guoqian] Beijing Normal Univ, Inst Environm Econ & Policy Res, Beijing 100875, Peoples R China. [Altieri, Andrew H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Pennings, Steven C.] Univ Houston, Dept Biol & Biochem, Houston, TX 77204 USA. [Liu, Jianguo] Michigan State Univ, Dept Fisheries & Wildlife, Ctr Syst Integrat & Sustainabil, E Lansing, MI 48823 USA. [Ehrlich, Paul R.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. RP Cui, BS (reprint author), Beijing Normal Univ, Sch Environm, State Key Lab Water Environm Simulat, Beijing 100875, Peoples R China. EM cuibs@bnu.edu.cn RI He, Qiang/G-2012-2011; Liu, Jianguo/G-5211-2015; Li, Bo/B-8016-2010; Pennings, Steven/A-8326-2013; Chen, G. Q./B-5407-2012; OI He, Qiang/0000-0001-6481-0924; Liu, Jianguo/0000-0001-6344-0087; Li, Bo/0000-0002-0439-5666; Pennings, Steven/0000-0003-4757-7125; Chen, G. Q./0000-0003-1173-6796; Coverdale, Tyler/0000-0003-0910-9187 FU National Key Basic Research Program of China [2013CB430406]; China National Funds for Distinguished Young Scientists [51125035]; National Science Foundation for Innovative Research Group [51121003]; National Science Foundation (USA) FX We thank D. F. Sax, C. B. Craft, S. Crotty and C. Brisson for comments/edits, and J. Huang for China's watershed map. This study was funded by National Key Basic Research Program of China (2013CB430406), China National Funds for Distinguished Young Scientists (51125035), National Science Foundation for Innovative Research Group (51121003) and the Biological Oceanography Program of the National Science Foundation (USA). NR 52 TC 20 Z9 24 U1 5 U2 83 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 8 PY 2014 VL 4 AR 5995 DI 10.1038/srep05995 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AN4XL UT WOS:000340593000007 PM 25104138 ER PT J AU McCully, C Jha, SW Foley, RJ Bildsten, L Fong, WF Kirshner, RP Marion, GH Riess, AG Stritzinger, MD AF McCully, Curtis Jha, Saurabh W. Foley, Ryan J. Bildsten, Lars Fong, Wen-fai Kirshner, Robert P. Marion, G. H. Riess, Adam G. Stritzinger, Maximilian D. TI A luminous, blue progenitor system for the type Iax supernova 2012Z SO NATURE LA English DT Article ID HUBBLE-SPACE-TELESCOPE; CORE-COLLAPSE SUPERNOVA; SN 2005HK; HELIUM NOVA; EXPLOSION; STARS; CONSTANT; MODELS; 2002CX AB Type Iax supernovae are stellar explosions that are spectroscopically similar to some type Ia supernovae at the time of maximum light emission, except with lower ejecta velocities(1,2). They are also distinguished by lower luminosities. At late times, their spectroscopic properties diverge from those of other supernovae(3-6), but their composition (dominated by iron-group and intermediate-mass elements(1,7)) suggests a physical connection to normal type Ia supernovae. Supernovae of type Iax are not rare; they occur at a rate between 5 and 30 per cent of the normal type Ia rate(1). The leading models for type Iax supernovae are thermonuclear explosions of accreting carbon-oxygen white dwarfs that do not completely unbind the star(8-10), implying that they are 'less successful' versions of normal type Ia supernovae, where complete stellar disruption is observed. Here we report the detection of the luminous, blue progenitor system of the type Iax SN 2012Z in deep pre-explosion imaging. The progenitor system's luminosity, colours, environment and similarity to the progenitor of the Galactic helium nova V445 Puppis(11-13) suggest that SN 2012Z was the explosion of a white dwarf accretingmaterial from a helium-star companion. Observations over the next few years, after SN 2012Z has faded, will either confirm this hypothesis or perhaps show that this super-nova was actually the explosive death of a massive star(14,15). C1 [McCully, Curtis; Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Foley, Ryan J.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Foley, Ryan J.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. [Bildsten, Lars] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bildsten, Lars] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Fong, Wen-fai; Kirshner, Robert P.; Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Riess, Adam G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Riess, Adam G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Stritzinger, Maximilian D.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Jha, SW (reprint author), Rutgers State Univ, Dept Phys & Astron, 136 Frelinghuysen Rd, Piscataway, NJ 08854 USA. EM saurabh@physics.rutgers.edu OI McCully, Curtis/0000-0001-5807-7893; stritzinger, maximilian/0000-0002-5571-1833 FU NASA/HST [GO-12913.01, GO-12999.01]; National Science Foundation (NSF) CAREER [AST-0847157]; NSF [PHY 11-25915, AST 11-09174]; Danish Agency for Science, Technology, and Innovation; NASA from the Space Telescope Science Institute [GO-12913, GO-12999]; NASA [NAS5-26555] FX We dedicate this paper to the memory of our friend and colleague Weidong Li, whose work on the Lick Observatory Supernova Search, SN 2002cx-like supernovae, and Hubble Space Telescope observations of supernova progenitors continues to inspire us. We thank the SH0ES team for assistance with data from HST programme GO-12880, E. Bertin for the development of the STIFF software to produce colour images, and A. Dolphin for software and guidance in photometry. This research at Rutgers University was supported through NASA/HST grant GO-12913.01 and National Science Foundation (NSF) CAREER award AST-0847157 to S.W.J.; NASA/HST grant GO-12999.01 to R.J.F. supported this work at the University of Illinois. At UC Santa Barbara, this work was supported by NSF grants PHY 11-25915 and AST 11-09174 to L.B. The Danish Agency for Science, Technology, and Innovation supported M.D.S. through a Sapere Aude Level 2 grant. Support for HST programmes GO-12913 and GO-12999 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 NAS5-26555. NR 34 TC 33 Z9 33 U1 0 U2 9 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 7 PY 2014 VL 512 IS 7512 BP 54 EP + DI 10.1038/nature13615 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM5NX UT WOS:000339908000029 PM 25100479 ER PT J AU Masiulionis, VE Rabeling, C Licht, HHD Schultz, T Bacci, M Bezerra, CMS Pagnocca, FC AF Masiulionis, Virginia E. Rabeling, Christian Licht, Henrik H. De Fine Schultz, Ted Bacci, Mauricio, Jr. Santos Bezerra, Cintia M. Pagnocca, Fernando C. TI A Brazilian Population of the Asexual Fungus-Growing Ant Mycocepurus smithii (Formicidae, Myrmicinae, Attini) Cultivates Fungal Symbionts with Gongylidia-Like Structures SO PLOS ONE LA English DT Article ID ACROMYRMEX-OCTOSPINOSUS REICH; MULTIPLE SEQUENCE ALIGNMENT; ATTA-CEPHALOTES L; HYMENOPTERA-FORMICIDAE; NEST ARCHITECTURE; FARMING ANTS; FOOD SOURCES; MUTUALISM; ORIGIN; AGRICULTURE AB Attine ants cultivate fungi as their most important food source and in turn the fungus is nourished, protected against harmful microorganisms, and dispersed by the ants. This symbiosis evolved approximately 50-60 million years ago in the late Paleocene or early Eocene, and since its origin attine ants have acquired a variety of fungal mutualists in the Leucocoprineae and the distantly related Pterulaceae. The most specialized symbiotic interaction is referred to as "higher agriculture'' and includes leafcutter ant agriculture in which the ants cultivate the single species Leucoagaricus gongylophorus. Higher agriculture fungal cultivars are characterized by specialized hyphal tip swellings, so-called gongylidia, which are considered a unique, derived morphological adaptation of higher attine fungi thought to be absent in lower attine fungi. Rare reports of gongylidia-like structures in fungus gardens of lower attines exist, but it was never tested whether these represent rare switches of lower attines to L. gonglyphorus cultivars or whether lower attine cultivars occasionally produce gongylidia. Here we describe the occurrence of gongylidia-like structures in fungus gardens of the asexual lower attine ant Mycocepurus smithii. To test whether M. smithii cultivates leafcutter ant fungi or whether lower attine cultivars produce gongylidia, we identified the M. smithii fungus utilizing molecular and morphological methods. Results shows that the gongylidia-like structures of M. smithii gardens are morphologically similar to gongylidia of higher attine fungus gardens and can only be distinguished by their slightly smaller size. A molecular phylogenetic analysis of the fungal ITS sequence indicates that the gongylidia-bearing M. smithii cultivar belongs to the so-called "Clade 1'' of lower Attini cultivars. Given that M. smithii is capable of cultivating a morphologically and genetically diverse array of fungal symbionts, we discuss whether asexuality of the ant host maybe correlated with low partner fidelity and active symbiont choice between fungus and ant mutualists. C1 [Masiulionis, Virginia E.; Bacci, Mauricio, Jr.; Santos Bezerra, Cintia M.; Pagnocca, Fernando C.] Sao Paulo State Univ, Inst Biociencias, Rio Claro, SP, Brazil. [Rabeling, Christian] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Rabeling, Christian; Schultz, Ted] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Licht, Henrik H. De Fine] Univ Copenhagen, Sect Organismal Biol, Dept Plant & Environm Sci, Copenhagen, Denmark. RP Masiulionis, VE (reprint author), Sao Paulo State Univ, Inst Biociencias, Rio Claro, SP, Brazil. EM vemasiulionis@gmail.com RI De Fine Licht, Henrik/G-3307-2014; Masiulionis, Virginia Elena/L-6800-2013 OI De Fine Licht, Henrik/0000-0003-3326-5729; Masiulionis, Virginia Elena/0000-0002-3619-5781 FU CNPq; Fapesp; CAPES/PEC-PG scholarship; Harvard Society of Fellows; HMS Milton Fund; U.S. National Science Foundation [DEB 0949689]; Smithsonian Institution Scholarly Studies Program; Smithsonian NMNH Small Grants Program; Danish Research Council; Carlsberg Foundation FX FCP and MB are grateful to CNPq and Fapesp for their financial support. VEM is a recipient of a CAPES/PEC-PG scholarship. CR was financially supported by a Junior Fellowship from the Harvard Society of Fellows and the HMS Milton Fund. TS was supported by the U.S. National Science Foundation grant DEB 0949689, the Smithsonian Institution Scholarly Studies Program, and the Smithsonian NMNH Small Grants Program. HHDFL was supported by grants from the Danish Research Council and the Carlsberg Foundation. 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 4 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 AUG 7 PY 2014 VL 9 IS 8 AR e103800 DI 10.1371/journal.pone.0103800 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM6SB UT WOS:000339993900024 PM 25101899 ER PT J AU Thomas, DB McGraw, KJ Butler, MW Carrano, MT Madden, O James, HF AF Thomas, Daniel B. McGraw, Kevin J. Butler, Michael W. Carrano, Matthew T. Madden, Odile James, Helen F. TI Ancient origins and multiple appearances of carotenoid-pigmented feathers in birds SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE ancestral state reconstruction; birds; coloration; pigmentation; plumage; supertree ID SR-BI; EVOLUTION; PLUMAGE; COLORATION; EXPRESSION; VERTEBRATES; CHARACTERS; SPECIATION; DIVERSITY; HISTORY AB The broad palette of feather colours displayed by birds serves diverse biological functions, including communication and camouflage. Fossil feathers provide evidence that some avian colours, like black and brown melanins, have existed for at least 160 million years (Myr), but no traces of bright carotenoid pigments in ancient feathers have been reported. Insight into the evolutionary history of plumage carotenoids may instead be gained from living species. We visually surveyed modern birds for carotenoid-consistent plumage colours (present in 2956 of 9993 species). We then used high-performance liquid chromatography and Raman spectroscopy to chemically assess the family-level distribution of plumage carotenoids, confirming their presence in 95 of 236 extant bird families (only 36 family-level occurrences had been confirmed previously). Using our data for all modern birds, we modelled the evolutionary history of carotenoid-consistent plumage colours on recent supertrees. Results support multiple independent origins of carotenoid plumage pigmentation in 13 orders, including six orders without previous reports of plumage carotenoids. Based on time calibrations from the supertree, the number of avian families displaying plumage carotenoids increased throughout the Cenozoic, and most plumage carotenoid originations occurred after the Miocene Epoch (23 Myr). The earliest origination of plumage carotenoids was reconstructed within Passeriformes, during the Palaeocene Epoch (66-56 Myr), and not at the base of crown-lineage birds. C1 [Thomas, Daniel B.; James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Carrano, Matthew T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Thomas, Daniel B.; Madden, Odile] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Thomas, Daniel B.] Massey Univ, Inst Nat & Math Sci, Auckland 0632, New Zealand. [McGraw, Kevin J.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Butler, Michael W.] Lafayette Coll, Dept Biol, Easton, PA 18042 USA. RP Thomas, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116, Washington, DC 20013 USA. EM d.b.thomas@massey.ac.nz RI Madden, Odile/N-9909-2015; Carrano, Matthew/C-7601-2011 OI Madden, Odile/0000-0003-2322-2522; Carrano, Matthew/0000-0003-2129-1612 FU National Museum of Natural History, Institution FX D.B.T. was funded by a Peter Buck Postdoctoral Fellowship from the National Museum of Natural History, Institution. NR 43 TC 11 Z9 13 U1 5 U2 79 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 2014 VL 281 IS 1788 AR 20140806 DI 10.1098/rspb.2014.0806 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AK7WE UT WOS:000338637600017 PM 24966316 ER PT J AU Malabarba, LR Jerep, FC AF Malabarba, Luiz R. Jerep, Fernando C. TI Review of the species of the genus Serrapinnus Malabarba, 1998 (Teleostei: Characidae: Cheirodontinae) from the rio Tocantins-Araguaia basin, with description of three new species SO ZOOTAXA LA English DT Article DE Cheirodontini; Ctenocheirodon; identification key; sexual dimorphism; taxonomy ID CHARACIFORMES CHARACIDAE; NORTHEASTERN BRAZIL; AMAZON BASIN; OSTARIOPHYSI; FISH; REDESCRIPTION; STATE AB Species of the genus Serrapinnus from the rio Tocantins-Araguaia basin are revised and three new species are described. Serrapinnus aster new species is diagnosed by the presence of scimitar-shaped ventral procurrent caudal-fin rays of mature males forming a semicircle and by the presence of 7-9 cusps on the premaxillary teeth; S. lucindai new species is distinguished from its congeners by the presence of a higher number of ventral procurrent caudal-fin rays (17 to 19); and S. tocantinensis new species differs from the remaining species of the genus by the elongation of the unbranched dorsal and pelvic-fin rays into filaments in mature males. Serrapinnus sterbai is recognized as broadly distributed in the Tocantins-Araguaia basin and is redescribed based on specimens from across its entire distribution. A key for the cheirodontines occurring in the Atlantic drainages of northeastern Brazil, from the rio Tocantins-Araguaia to the rio Paraguacu is provided. C1 [Malabarba, Luiz R.] Univ Fed Rio Grande do Sul, Dept Zool, BR-91501970 Porto Alegre, RS, Brazil. [Jerep, Fernando C.] Univ Estadual Londrina, Programa Posgrad Ciencias Biol, Dept Biol Anim & Vegetal, Ctr Ciencias Biol, BR-86057970 Londrina, PR, Brazil. [Jerep, Fernando C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20560 USA. RP Malabarba, LR (reprint author), Univ Fed Rio Grande do Sul, Dept Zool, Av Bento Goncalves 9500, BR-91501970 Porto Alegre, RS, Brazil. EM malabarb@ufrgs.br; fjerep@gmail.com RI Jerep, Fernando/F-5274-2015 FU CNPq [300705/2010-7, 477318/2012-6] FX Special thanks to Fernando R. Carvalho (IBSJRP) for the analysis of the type material of Serrapinnus sterbai and Richard P. Vari for his review of the manuscript. We are thankful to Carlos A. Lucena (MCP), Paulo H. F. Lucinda (UNT), Lucia Rapp Py-Daniel (INPA), Wilson Costa (UFRJ), Flavio C. T. Lima, Osvaldo Oyakawa (MZUSP), Paulo A. Buckup (MNRJ), Mary Anne Rogers, Kevin Swagel (FMNH), Richard Vari, Jerry Finan, Jeffrey Clayton (NMNH), John Lundberg, Mark Sabaj-Perez (ANSP), David Catania and Jon D. Fong (CAS) for the loan of specimens, and museum and technical support. We thank Jose L. Birindelli (UEL) and project SACI for photographs of S. sterbai. LRM research is supported by CNPq (300705/2010-7; 477318/2012-6). NR 20 TC 2 Z9 2 U1 0 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 6 PY 2014 VL 3847 IS 1 BP 57 EP 79 PG 23 WC Zoology SC Zoology GA AN6WW UT WOS:000340740100003 PM 25112325 ER PT J AU Thompson, FC Skevington, JH AF Thompson, F. Christian Skevington, Jeffrey H. TI Afrotropical flower flies (Diptera: Syrphidae). A new genus and species from Kenya, with a review of the melanostomine group of genera SO ZOOTAXA LA English DT Review DE Syrphinae key; Bacchini; Melanostomini ID DNA BARCODES; DIPTERA; PHYLOGENY; REVISION; LARVAL AB A new genus and species of flower flies (Diptera: Syrphidae: Syrphinae: Syrphini) are described from central Africa (Kenya & Uganda), Afrostoma quadripunctatum. A key to the Afrotropical genera of the subfamily Syrphinae is given. A review of the melanostomine [Bacchini] genera and subgenera is provided along with a key to them. Phylogenetic placement of Afrostoma is included based on mitochondrial cytochrome c oxidase subunit I (COI) data. C1 [Thompson, F. Christian] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Skevington, Jeffrey H.] Agr & Agri Food Canada, Canadian Natl Collect Insects Arachnids & Nematod, Ottawa, ON K1A 0C6, Canada. RP Skevington, JH (reprint author), Agr & Agri Food Canada, Canadian Natl Collect Insects Arachnids & Nematod, 960 Carling Ave, Ottawa, ON K1A 0C6, Canada. EM thompsonf@si.edu; jhskevington@gmail.com NR 102 TC 3 Z9 3 U1 0 U2 3 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 6 PY 2014 VL 3847 IS 1 BP 97 EP 114 PG 18 WC Zoology SC Zoology GA AN6WW UT WOS:000340740100005 PM 25112327 ER PT J AU Longino, JT Branstetter, MG Colwell, RK AF Longino, John T. Branstetter, Michael G. Colwell, Robert K. TI How Ants Drop Out: Ant Abundance on Tropical Mountains SO PLOS ONE LA English DT Article ID ELEVATIONAL DIVERSITY; SPECIES RICHNESS; ASSEMBLAGES; PRODUCTIVITY; TEMPERATURE; GRADIENTS; ENERGY AB In tropical wet forests, ants are a large proportion of the animal biomass, but the factors determining abundance are not well understood. We characterized ant abundance in the litter layer of 41 mature wet forest sites spread throughout Central America (Chiapas, Guatemala, Honduras, Nicaragua, and Costa Rica) and examined the impact of elevation (as a proxy for temperature) and community species richness. Sites were intentionally chosen to minimize variation in precipitation and seasonality. From sea level to 1500 m ant abundance very gradually declined, community richness declined more rapidly than abundance, and the local frequency of the locally most common species increased. These results suggest that within this elevational zone, density compensation is acting, maintaining high ant abundance as richness declines. In contrast, in sites above 1500 m, ant abundance dropped abruptly to much lower levels. Among these high montane sites, community richness explained much more of the variation in abundance than elevation, and there was no evidence of density compensation. The relative stability of abundance below 1500 m may be caused by opposing effects of temperature on productivity and metabolism. Lower temperatures may decrease productivity and thus the amount of food available for consumers, but slower metabolisms of consumers may allow maintenance of higher biomass at lower resource supply rates. Ant communities at these lower elevations may be highly interactive, the result of continuous habitat presence over geological time. High montane sites may be ephemeral in geological time, resulting in non-interactive communities dominated by historical and stochastic processes. Abundance in these sites may be determined by the number of species that manage to colonize and/or avoid extinction on mountaintops. C1 [Longino, John T.] Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. [Branstetter, Michael G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Colwell, Robert K.] Univ Connecticut, Dept Ecol & Evolutionary Biol, Storrs, CT USA. [Colwell, Robert K.] Univ Colorado, Museum Nat Hist, Boulder, CO 80309 USA. RP Longino, JT (reprint author), Univ Utah, Dept Biol, Salt Lake City, UT 84112 USA. EM jacklongino@gmail.com RI Colwell, Robert/C-7276-2015 FU National Science Foundation [DEB-0072702, DEB-0640015/DEB-1157383, DEB-1354739]; National Geographic Society [7331-02, 7751-04]; Conservation International; Smithsonian Institution FX This work was supported by National Science Foundation grants DEB-0072702 (Project ALAS), DEB-0640015/DEB-1157383 (Project LLAMA), DEB-1354739 (Project ADMAC), National Geographic Society grants 7331-02 and 7751-04, and Conservation International. MB was supported by a Buck Postdoctoral Fellowship from the Smithsonian Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 32 TC 11 Z9 11 U1 2 U2 33 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 6 PY 2014 VL 9 IS 8 AR e104030 DI 10.1371/journal.pone.0104030 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM6SM UT WOS:000339995100045 PM 25098722 ER PT J AU Leasi, F Norenburg, JL AF Leasi, Francesca Norenburg, Jon L. TI The Necessity of DNA Taxonomy to Reveal Cryptic Diversity and Spatial Distribution of Meiofauna, with a Focus on Nemertea SO PLOS ONE LA English DT Article ID MONOCELIS-LINEATA PROSERIATA; SPECIES COMPLEX; PELLIODITIS-MARINA; PHYLUM NEMERTEA; PHYLOGENETIC-RELATIONSHIPS; GENETIC-STRUCTURE; PHYLOGEOGRAPHY; OTOTYPHLONEMERTES; HOPLONEMERTEA; DELIMITATION AB Meiofauna represent one of the most abundant and diverse communities in marine benthic ecosystems. However, an accurate assessment of diversity at the level of species has been and remains challenging for these microscopic organisms. Therefore, for many taxa, especially the soft body forms such as nemerteans, which often lack clear diagnostic morphological traits, DNA taxonomy is an effective means to assess species diversity. Morphological taxonomy of Nemertea is well documented as complicated by scarcity of unambiguous character states and compromised by diagnoses of a majority of species (and higher clades) being inadequate or based on ambiguous characters and character states. Therefore, recent studies have advocated for the primacy of molecular tools to solve the taxonomy of this group. DNA taxonomy uncovers possible hidden cryptic species, provides a coherent means to systematize taxa in definite clades, and also reveals possible biogeographic patterns. Here, we analyze diversity of nemertean species by considering the barcode region of the mitochondrial gene Cytochrome Oxidase subunit I (COI) and different species delineation approaches in order to infer evolutionarily significant units. In the aim to uncover actual diversity of meiofaunal nemerteans across different sites in Central America, COI sequences were obtained for specimens assigned here to the genera Cephalothrix, Ototyphlonemertes, and Tetrastemma-like worms, each commonly encountered in our sampling. Additional genetic, taxonomic, and geographic data of other specimens belonging to these genera were added from GenBank. Results are consistent across different DNA taxonomy approaches, and revealed (i) the presence of several hidden cryptic species and (ii) numerous potential misidentifications due to traditional taxonomy. (iii) We additionally test a possible biogeographic pattern of taxonomic units revealed by this study, and, except for a few cases, the putative species seem not to be widely distributed, in contrast to what traditional taxonomy would suggest for the recognized morphotypes. C1 [Leasi, Francesca; Norenburg, Jon L.] Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Leasi, F (reprint author), Smithsonian Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM leasif@si.edu RI Norenburg, Jon/K-3481-2015; LEASI, FRANCESCA/E-4361-2017 OI Norenburg, Jon/0000-0001-7776-1527; FU Smithsonian Marine Networks grant; Encyclopedia of Life Synthesis award; LAB (Laboratory of Analytical Biology) (LAB, Smithsonian National Museum of Natural History) FX The workshops were partially funded by a Smithsonian Marine Networks grant, an Encyclopedia of Life Synthesis award and laboratory work was partially subsidized by LAB (Laboratory of Analytical Biology) (LAB, Smithsonian National Museum of Natural History). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 61 TC 18 Z9 19 U1 2 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 AUG 5 PY 2014 VL 9 IS 8 AR e104385 DI 10.1371/journal.pone.0104385 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO5BW UT WOS:000341357200108 PM 25093815 ER PT J AU Halfwerk, W Page, RA Taylor, RC Wilson, PS Ryan, MJ AF Halfwerk, Wouter Page, Rachel A. Taylor, Ryan C. Wilson, Preston S. Ryan, Michael J. TI Crossmodal Comparisons of Signal Components Allow for Relative-Distance Assessment SO CURRENT BIOLOGY LA English DT Article ID WATER-SURFACE-WAVES; FEMALE MATE CHOICE; NEOTROPICAL FROG; MATING SIGNALS; TUNGARA FROGS; COMMUNICATION; BEHAVIOR; PROXIMITY; RESPONSES; DISPLAY AB Animals have multiple senses through which they detect their surroundings and often integrate sensory information across different modalities to generate perceptions [1, 2]. Animal communication, likewise, often consists of signals containing stimuli processed by different senses [3-6]. Stimuli with different physical forms (i.e., from different sensory modalities) travel at different speeds [7]. As a consequence, multimodal stimuli simultaneously emitted at a source can arrive at a receiver at different times. Such differences in arrival time can provide unique information about the distance to the source [8, 9]. Male tungara frogs (Physalaemus pustulosus) call from ponds to attract females and to repel males. Production of the sound incidentally creates ripples on the water surface, providing a multimodal cue [10]. We tested whether male frogs attend to distance-dependent cues created by a calling rival and whether their response depends on crossmodal comparisons. In a first experiment, we showed distance-dependent changes in vocal behavior: males responded more strongly with decreasing distance to a mimicked rival. In a second experiment, we showed that males can discriminate between relatively near and far rivals by using a combination of unimodal cues, specifically amplitude changes of sound and water waves, as well as crossmodal differences in arrival time. Our data reveal that animals can compare the arrival time of simultaneously emitted multimodal cues to obtain information on relative distance to a source. We speculate that communicative benefits from crossmodal comparison may have been an important driver of the evolution of elaborate multimodal displays [11, 12]. C1 [Halfwerk, Wouter; Page, Rachel A.; Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Halfwerk, Wouter] Leiden Univ, Inst Biol, NL-2300 RA Leiden, Netherlands. [Taylor, Ryan C.] Salisbury Univ, Dept Biol, Salisbury, MD 21801 USA. [Wilson, Preston S.] Univ Texas Austin, Dept Mech Engn, Austin, TX 78712 USA. [Ryan, Michael J.] Univ Texas Austin, Dept Integrat Biol, Austin, TX 78712 USA. RP Halfwerk, W (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM wouter.halfwerk@gmail.com FU NWO [825.11.026]; KNAW [UPS/297 /Eco/1411J]; NSF [IBN 0517328] FX We are grateful to Jennifer Finley and Amanda Lea for valuable help during the experiments. Justin Touchon and Stuart Dennis provided statistical advice. We thank Barrett Klein and Paul Clements for fabricating the pneumatic robotic frog system. Comments from four reviewers greatly improved the paper. We thank the Smithsonian Tropical Research Institute for the infrastructure critical to conducting this work, as well as logistical and permitting support. The research was funded through an NWO grant (825.11.026) to W.H., an KNAW grant (UPS/297 /Eco/1411J) to W.H., and an NSF grant (IBN 0517328) to R.C.T., M.J.R., and R.A.P. NR 38 TC 9 Z9 9 U1 2 U2 15 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 4 PY 2014 VL 24 IS 15 BP 1751 EP 1755 DI 10.1016/j.cub.2014.05.068 PG 5 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA AM7UL UT WOS:000340074100023 PM 25042586 ER PT J AU Zeder, MA Bar-Oz, G AF Zeder, Melinda A. Bar-Oz, Guy TI A response to Betts (2014) SO QUATERNARY INTERNATIONAL LA English DT Editorial Material ID DESERT KITES; GAZELLE; NEGEV; LEVANT; WALLS AB In her critique of our 2013 article in Quaternary International (Zeder et al., 2013), Alison Betts defends the Neolithic temporal assignment of kite structures in the Harra and Hammad regions of eastern Jordan calling our attention to the final report on the survey and excavation project in this region (Betts, 1998). A review of this work, however, finds that this assignment remains open to question on several grounds. Although it is possible that the construction and use of these structures in this region may date back to the Neolithic, the case for this determination is far from incontrovertible, and there are alternative plausible arguments that can be made for a much more recent temporal placement. The open nature of the question of the dating of these structures does not, as Betts says in her critique, undermine the major substantive conclusions of our paper. Moreover, the unresolved temporal placement of these enigmatic structures speaks to the difficulty of dating kites, and not to the competency of this pioneering research. The Betts study stands as a landmark that has inspired all subsequent work on the function and dating of these structures across the Levant and beyond. (C) 2014 Elsevier Ltd and INQUA. All rights reserved. C1 [Zeder, Melinda A.] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Bar-Oz, Guy] Univ Haifa, Zinman Inst Archaeol, Haifa, Israel. RP Zeder, MA (reprint author), Smithsonian Inst, Anthropology 2227,Glasgow Rd, Alexandria, VA 22307 USA. EM Zederm@si.edu NR 21 TC 4 Z9 4 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 EI 1873-4553 J9 QUATERN INT JI Quat. Int. PD AUG 4 PY 2014 VL 338 BP 128 EP 131 DI 10.1016/j.quaint.2014.01.008 PG 4 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AM7BO UT WOS:000340019900015 ER PT J AU Knapp, LW Imamura, H AF Knapp, Leslie W. Imamura, Hisashi TI Grammoplites vittatus (Valenciennes), (Scorpaeniformes, Platycephalidae), removed from synonymy with Grammoplites scaber (Linnaeus) SO ZOOTAXA LA English DT Letter DE Grammoplites vittatus; Grammoplites scaber.; Platycephalidae AB Grammoplites vittatus (Valenciennes), often previously overlooked by authors or regarded as a junior synonym of G. scaber (Linnaeus), is shown here to be a valid species. It has more gill rakers (7-8) then G. scaber and G. knappi (usually 6) and a narrower interorbital width than G. scaber. A key to the species of Grammoplites Fowler is given. C1 [Knapp, Leslie W.] Natl Museum Nat Hist, Div Fishes, MRC Smithsonian Inst 534, Washington, DC 20013 USA. [Imamura, Hisashi] Hokkaido Univ, Lab Marine Biol & Div Systemat Ichthyol, Fac Fisheries Sci, Hakodate, Hokkaido 0418611, Japan. RP Knapp, LW (reprint author), Natl Museum Nat Hist, Div Fishes, MRC Smithsonian Inst 534, POB 37012, Washington, DC 20013 USA. EM knappl@si.edu; Imamura@fish.hokudai.ac.jp NR 10 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 AUG 4 PY 2014 VL 3846 IS 3 BP 447 EP 450 PG 4 WC Zoology SC Zoology GA AM2GO UT WOS:000339668200008 PM 25112262 ER PT J AU Kim, S Kim, Y Kim, Y Kim, K Wang, S Kang, H Yoo, B AF Kim, Sunghyun Kim, Yongkyu Kim, Youngjoo Kim, Kyeonghoon Wang, S. Kang, Hojeong Yoo, Byungho TI Effects of planting method and nitrogen addition on Sphagnum growth in microcosm wetlands SO PADDY AND WATER ENVIRONMENT LA English DT Article DE Bog; Sphagnum; Productivity; Decomposition rate ID CARBON ACCUMULATION; RAISED BOG; DEPOSITION; MOSSES; DECOMPOSITION; BRYOPHYTES; PEATLAND; MIRE; PHOSPHORUS; VEGETATION AB In this study, we propose a method to create a Sphagnum wetland in an urban ecosystem by collecting basic information about Sphagnum growth and decomposition. We constructed six groups of Sphagnum microcosms (1 m x 1 m) with three replicates. A factorial design with two planting methods (capitulum without stem and capitulum with stem) and three levels of nitrogen addition (0, 2, and 6 g N m(-2) year(-1)) were prepared. Changes in length, dry mass, and decomposition rates of Sphagnum were monitored over a growing season. The effect of N concentration on production varied for the different planting methods. Production of Sphagnum increased with N concentration in the capitulum without the stem treatment (-D) than in the with stem treatment (+D). Adding N affected the decomposition rate in both with and without stem treatments. Decomposition rate increased with added nitrogen. Planting without stems (-D) was an effective design for a high production and low decomposition of Sphagnum. Net primary production was 187-260 g m(-2) year(-1) for dry mass and 15.5-26.5 mm year(-1) for length, whereas decomposition rates were 10.9-14.7 % mass loss per year. These values are comparable to those from natural bogs. The overall results indicate that constructing Sphagnum wetlands can be successfully employed as a greening technology in urban ecosystems, even in mid-latitudes. C1 [Kim, Sunghyun] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Kim, Kyeonghoon] IlSong ERT Co LTD, Yongin, South Korea. Korea Inst Construct Technol, Ilsan, South Korea. [Wang, S.] Pukyong Natl Univ, Dept Energy Resource Engn, Pusan, South Korea. [Kang, Hojeong] Yonsei Univ, Sch Civil & Environm Engn, Seoul 120749, South Korea. [Yoo, Byungho] Kangwon Natl Univ, Korea Environm Ind & Technol Inst, Ctr Aquat Ecosyst Restorat, Chunchon 200701, Kangwon Do, South Korea. RP Kang, H (reprint author), Yonsei Univ, Sch Civil & Environm Engn, Seoul 120749, South Korea. EM hj_kang@yonsei.ac.kr RI Kang, Hojeong/C-7208-2011 FU Center for Aquatic Ecosystem Restoration (CAER) of the Ecostar project from the Ministry of Environment (MOE), Republic of Korea (MOE) [EW33-08-11]; Basic Science Research Program through the National Research Foundation of Korea (NRF) - Ministry of Education, Science and Technology [86457858] FX This study was supported by the Center for Aquatic Ecosystem Restoration (CAER) of the Ecostar project from the Ministry of Environment (MOE), Republic of Korea (MOE; EW33-08-11. S. Kim was supported by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (86457858). NR 48 TC 2 Z9 2 U1 5 U2 13 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1611-2490 EI 1611-2504 J9 PADDY WATER ENVIRON JI Paddy Water Environ. PD AUG PY 2014 VL 12 SU 1 SI SI BP S185 EP S192 DI 10.1007/s10333-014-0427-1 PG 8 WC Agricultural Engineering; Agronomy SC Agriculture GA CB9RX UT WOS:000349971200018 ER PT J AU Launius, RD AF Launius, Roger D. TI Dreams of Other Worlds: The Amazing Story of Unmanned Space Exploration. SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Launius, Roger D.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 2 U2 2 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0021-8286 EI 1753-8556 J9 J HIST ASTRON JI J. Hist. Astron. PD AUG PY 2014 VL 45 BP 377 EP 378 DI 10.1177/0021828614538381 PN 3 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA AR6DN UT WOS:000343673600005 ER PT J AU Green, WA Little, SA Price, CA Wing, SL Smith, SY Kotrc, B Doria, G AF Green, Walton A. Little, Stefan A. Price, Charles A. Wing, Scott L. Smith, Selena Y. Kotrc, Benjamin Doria, Gabriela TI READING THE LEAVES: A COMPARISON OF LEAF RANK AND AUTOMATED AREOLE MEASUREMENT FOR QUANTIFYING ASPECTS OF LEAF VENATION SO APPLICATIONS IN PLANT SCIENCES LA English DT Review DE automated image quantification; leaf architecture; leaf rank; leaf venation; repeatability ID VEIN DENSITY; EVOLUTION; ARCHITECTURE; ORGANIZATION; HYPOTHESIS; PATTERNS; ECOLOGY; IMAGE AB The reticulate venation that is characteristic of a dicot leaf has excited interest from systematists for more than a century, and from physiological and developmental botanists for decades. The tools of digital image acquisition and computer image analysis, however, are only now approaching the sophistication needed to quantify aspects of the venation network found in real leaves quickly, easily, accurately, and reliably enough to produce biologically meaningful data. In this paper, we examine 120 leaves distributed across vascular plants (representing 118 genera and 80 families) using two approaches: a semiquantitative scoring system called "leaf ranking," devised by the late Leo Hickey, and an automated image-analysis protocol. In the process of comparing these approaches, we review some methodological issues that arise in trying to quantify a vein network, and discuss the strengths and weaknesses of automatic data collection and human pattern recognition. We conclude that subjective leaf rank provides a relatively consistent, semiquantitative measure of areole size among other variables; that modal areole size is generally consistent across large sections of a leaf lamina; and that both approaches-semiquantitative, subjective scoring; and fully quantitative, automated measurement-have appropriate places in the study of leaf venation. C1 [Green, Walton A.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Little, Stefan A.] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. [Price, Charles A.] Univ Western Australia M084, Sch Plant Biol, Crawley, WA 6009, Australia. [Wing, Scott L.] Smithsonian Inst, Nat Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Smith, Selena Y.] Univ Michigan, Dept Earth & Environm Sci, Ann Arbor, MI 48109 USA. [Smith, Selena Y.] Univ Michigan, Museum Paleontol, Ann Arbor, MI 48109 USA. [Kotrc, Benjamin] MIT, Cambridge, MA 02139 USA. [Doria, Gabriela] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Green, WA (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, 26 Oxford St, Cambridge, MA 02138 USA. EM wagreen@bricol.net RI Price, Charles/B-1171-2011; Smith, Selena/I-6259-2012; OI Smith, Selena/0000-0002-5923-0404; Wing, Scott/0000-0002-2954-8905 FU Smithsonian Institution postdoctoral fellowship FX The late Leo J. Hickey does not appear as a co-author of this paper only because we feel that despite his contributions he would not have wanted to be credited as the author of a manuscript that he did not have a chance to edit. He contributed some of the data and many helpful ideas that are reported here. We deeply regret that he did not survive to see the outcome of this investigation, and we would not be comfortable publishing it without emphasizing his contribution. J. Weitz also made significant, practical contributions to the areole measurements discussed here. Part of the work was supported by a Smithsonian Institution postdoctoral fellowship to W. A. G. Thanks also to two anonymous reviewers for their input. NR 61 TC 5 Z9 5 U1 0 U2 5 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD AUG PY 2014 VL 2 IS 8 SI SI AR 1400006 DI 10.3732/apps.1400006 PG 14 WC Plant Sciences SC Plant Sciences GA AQ1SE UT WOS:000342560500003 ER PT J AU Han, JG Cao, HF Barb, A Punyasena, SW Jaramillo, C Shyu, CR AF Han, Jing Ginger Cao, Hongfei Barb, Adrian Punyasena, Surangi W. Jaramillo, Carlos Shyu, Chi-Ren TI A NEOTROPICAL MIOCENE POLLEN DATABASE EMPLOYING IMAGE-BASED SEARCH AND SEMANTIC MODELING SO APPLICATIONS IN PLANT SCIENCES LA English DT Article DE content-based image retrieval; database; Miocene; pollen morphology; semantics ID INFORMATION-RETRIEVAL; PALYNOLOGY; SEGMENTATION; SYSTEM AB Premise of the study: Digital microscopic pollen images are being generated with increasing speed and volume, producing opportunities to develop new computational methods that increase the consistency and efficiency of pollen analysis and provide the palynological community a computational framework for information sharing and knowledge transfer. Methods: Mathematical methods were used to assign trait semantics (abstract morphological representations) of the images of neotropical Miocene pollen and spores. Advanced database-indexing structures were built to compare and retrieve similar images based on their visual content. A Web-based system was developed to provide novel tools for automatic trait semantic annotation and image retrieval by trait semantics and visual content. Results: Mathematical models that map visual features to trait semantics can be used to annotate images with morphology semantics and to search image databases with improved reliability and productivity. Images can also be searched by visual content, providing users with customized emphases on traits such as color, shape, and texture. Discussion : Content-and semantic-based image searches provide a powerful computational platform for pollen and spore identification. The infrastructure outlined provides a framework for building a community-wide palynological resource, streamlining the process of manual identification, analysis, and species discovery. C1 [Han, Jing Ginger; Shyu, Chi-Ren] Univ Missouri, Inst Informat, Columbia, MO 65211 USA. [Cao, Hongfei; Shyu, Chi-Ren] Univ Missouri, Dept Comp Sci, Columbia, MO 65211 USA. [Barb, Adrian] Pennsylvania State Univ Great Valley, Dept Informat Sci, Malvern, PA 19355 USA. [Punyasena, Surangi W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa 03092, Ancon, Panama. RP Shyu, CR (reprint author), Univ Missouri, Inst Informat, Columbia, MO 65211 USA. EM shyuc@missouri.edu FU National Science Foundation [DBI-1053024, DBI-1052997, EAR-0957679] FX This research is supported by the National Science Foundation (grant numbers: DBI-1053024 to C. R. S., DBI-1052997 to S. W. P., and EAR-0957679 to C.J.). We thank Alejandra Restrepo, Ingrid Romero, and Carlos D'Apolito for their contributions to our pollen image database. Jacklyn Rodriguez assisted in organizing the sematic labels. NR 56 TC 3 Z9 3 U1 0 U2 3 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 2168-0450 J9 APPL PLANT SCI JI Appl. Plant Sci. PD AUG PY 2014 VL 2 IS 8 SI SI AR 1400030 DI 10.3732/apps.1400030 PG 17 WC Plant Sciences SC Plant Sciences GA AQ1SE UT WOS:000342560500005 ER PT J AU Clifford, SM Farmer, J Carr, MH Marais, DD Bibring, JP Craddock, R Newsom, H AF Clifford, Stephen M. Farmer, Jack Carr, Michael H. Marais, Dave Des Bibring, Jean-Pierre Craddock, Robert Newsom, Horton TI Introduction to the Early Mars III Special Section and Key Questions from the Third International Conference on Early Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID STRATIGRAPHY; EVENTS C1 [Clifford, Stephen M.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Farmer, Jack] Arizona State Univ, Dept Geol, Tempe, AZ 85287 USA. [Carr, Michael H.] US Geol Survey, Menlo Pk, CA 94025 USA. [Marais, Dave Des] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Bibring, Jean-Pierre] IAS, Orsay, France. [Craddock, Robert] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Sci, Washington, DC 20560 USA. [Newsom, Horton] Univ New Mexico, Inst Meteorit, Albuquerque, NM 87131 USA. RP Clifford, SM (reprint author), Lunar & Planetary Inst, 3303 NASA Rd 1, Houston, TX 77058 USA. EM clifford@lpi.usra.edu NR 15 TC 0 Z9 0 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1892 EP 1894 DI 10.1002/2014JE004643 PG 3 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000008 ER PT J AU Putzig, NE Phillips, RJ Campbell, BA Mellon, MT Holt, JW Brothers, TC AF Putzig, Nathaniel E. Phillips, Roger J. Campbell, Bruce A. Mellon, Michael T. Holt, John W. Brothers, T. Charles TI SHARAD soundings and surface roughness at past, present, and proposed landing sites on Mars: Reflections at Phoenix may be attributable to deep ground ice SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID POLAR LAYERED DEPOSITS; WATER; ACCUMULATION; STABILITY; BEHAVIOR; MODEL AB We use the Shallow Radar (SHARAD) on the Mars Reconnaissance Orbiter to search for subsurface interfaces and characterize surface roughness at the landing sites of Viking Landers 1 and 2, Mars Pathfinder, the Mars Exploration Rovers Spirit and Opportunity, the Phoenix Mars lander, the Mars Science Laboratory Curiosity rover, and three other sites proposed for Curiosity. Only at the Phoenix site do we find clear evidence of subsurface radar returns, mapping out an interface that may be the base of ground ice at depths of similar to 15-66 m across 2900 km(2) in the depression where the lander resides. At the Opportunity, Spirit, and candidate Curiosity sites, images and altimetry show layered materials tens to hundreds of meters thick extending tens to hundreds of kilometers laterally. These scales are well within SHARAD's resolution limits, so the lack of detections is attributable either to low density contrasts in layers of similar composition and internal structure or to signal attenuation within the shallowest layers. At each site, we use the radar return power to estimate surface roughness at scales of 10-100 m, a measure that is important for assessing physical properties, landing safety, and site trafficability. The strongest returns are found at the Opportunity site, indicating that Meridiani Planum is exceptionally smooth. Returns of moderate strength at the Spirit site reflect roughness more typical of Mars. Gale crater, Curiosity's ultimate destination, is the smoothest of the four proposed sites we examined, with Holden crater, Eberswalde crater, and Mawrth Vallis exhibiting progressively greater roughness. C1 [Putzig, Nathaniel E.; Mellon, Michael T.] SW Res Inst, Dept Space Studies, Space Sci & Engn Div, Boulder, CO 80302 USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Space Sci & Engn Div, Boulder, CO USA. [Phillips, Roger J.] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. [Campbell, Bruce A.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. [Holt, John W.; Brothers, T. Charles] Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX USA. [Holt, John W.; Brothers, T. Charles] Univ Texas Austin, Dept Geol Sci, Jackson Sch Geosci, Austin, TX USA. RP Putzig, NE (reprint author), SW Res Inst, Dept Space Studies, Space Sci & Engn Div, Boulder, CO 80302 USA. EM nathaniel@putzig.com RI Mellon, Michael/C-3456-2016; OI Brothers, Thomas/0000-0002-8043-7987 NR 40 TC 3 Z9 3 U1 1 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD AUG PY 2014 VL 119 IS 8 BP 1936 EP 1949 DI 10.1002/2014JE004646 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA AQ0ZA UT WOS:000342510000011 ER PT J AU Lima, SFB Christoffersen, ML Villacampa, Y AF Lima, Silvio F. B. Christoffersen, Martin L. Villacampa, Yolanda TI Record of Basilissopsis for the bathyal region of the South Atlantic (Brazil) based on the description of a new species and the designation of a lectotype for B. rhyssa SO SPIXIANA LA English DT Article ID GASTROPODA; VETIGASTROPODA; SEGUENZIOIDEA; SEGUENZIIDAE; MOLLUSCA; WATERS AB This paper records the genus Basilissopsis Dautzenberg & Fischer, 1897 for the South Atlantic Ocean. Basilissopsis bassa spec. nov. is described from deep waters off the state of Sao Paulo, Brazil. The new species is diagnosed by whorls with prominent shoulder angulation, a broadly flattened subsutural ramp, a strong spiral cord in the supramedian position and a greatly expanded peripheral keel. Basilissopsis bassa is compared with B. oxytropis (Watson, 1879), B. watsoni Dautzenberg & Fischer, 1897 and B. rhyssa (Dall, 1927). The type material of the last two species is also figured in this study. In addition, a lectotype for B. rhyssa is designated herein. C1 [Lima, Silvio F. B.; Christoffersen, Martin L.] Univ Fed Paraiba UFPB, Dept Sistemat & Ecol, BR-58051900 Joao Pessoa, Paraiba, Brazil. [Villacampa, Yolanda] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Lima, SFB (reprint author), Univ Fed Paraiba UFPB, Dept Sistemat & Ecol, Campus 1, BR-58051900 Joao Pessoa, Paraiba, Brazil. EM gergovia_lima@hotmail.com; mIchrist@dse.ufpb.br; villacay@si.edu RI Christoffersen, Martin /J-7794-2015 NR 21 TC 1 Z9 1 U1 0 U2 0 PU VERLAG DR FRIEDRICH PFEIL PI MUNICH PA WOLFRATSHAUSER STRASSE 27, MUNICH, D-81379, GERMANY SN 0341-8391 J9 SPIXIANA JI Spixiana PD AUG PY 2014 VL 37 IS 1 BP 27 EP 34 PG 8 WC Biology; Zoology SC Life Sciences & Biomedicine - Other Topics; Zoology GA AP9IX UT WOS:000342394600004 ER PT J AU Forbrich, J Oberg, K Lada, CJ Lombardi, M Hacar, A Alves, J Rathborne, JM AF Forbrich, Jan Oeberg, Karin Lada, Charles J. Lombardi, Marco Hacar, Alvaro Alves, Joao Rathborne, Jill M. TI Some like it cold: molecular emission and effective dust temperatures of dense cores in the Pipe Nebula SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; dust, extinction; radio lines: ISM; submillimeter: ISM ID STARLESS CORES; CLOUD CORES; DARK CLOUD; EXTINCTION MAPS; MASS FUNCTION; POPULATION; DEPLETION; BALANCE AB Aims. The Pipe Nebula is characterized by a low star-formation rate and is therefore an ideal environment to explore how initial conditions, including core characteristics, affect star-formation efficiencies. Methods. In a continued study of the molecular core population of the Pipe Nebula, we present a molecular-line survey of 52 cores. Previous research has shown a variety of different chemical evolutionary stages among the cores. Using the Mopra Radio Telescope, we observed the ground rotational transitions of HCO+, (HCO+)-C-13, HCN, (HCN)-C-13, HNC, and N2H+. These data are complemented with near-infrared extinction maps to constrain the column densities, effective dust temperatures derived from Herschel data, and NH3-based gas kinetic temperatures. Results. The target cores are located across the nebula, span visual extinctions between 5 and 67 mag, and effective dust temperatures (averaged along the lines of sight) between 13 and 19 K. The extinction-normalized integrated line intensities, a proxy for the abundance in constant excitation conditions of optically thin lines, vary within an order of magnitude for a given molecule. The effective dust temperatures and gas kinetic temperatures are correlated, but the effective dust temperatures are consistently higher than the gas kinetic temperatures. Combining the molecular line and temperature data, we find that N2H+ is only detected toward the coldest and densest cores, while other lines show no correlation with these core properties. Conclusions. Within this large sample, N2H+ is the only species to exclusively trace the coldest and densest cores, in agreement with chemical considerations. In contrast, the common high-density tracers HCN and HNC are present in a majority of the cores, demonstrating the utility of these molecules for characterizing cores over a wide range of extinctions. The correlation between the effective dust temperatures and the gas kinetic temperatures suggests that the former are dominated by dust that is both dense and thermodynamically coupled to the dense gas traced by NH3. A direct use of the effective dust temperatures in a determination of dust column densities from dust emission measurements would, however, result in an underestimate of the dust column densities. C1 [Forbrich, Jan; Hacar, Alvaro; Alves, Joao] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Forbrich, Jan; Oeberg, Karin; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Rathborne, Jill M.] CSIRO Astron & Space Sci, Sydney, NSW 1710, Australia. RP Forbrich, J (reprint author), Univ Vienna, Dept Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria. EM jan.forbrich@univie.ac.at OI Hacar, Alvaro/0000-0001-5397-6961; LOMBARDI, MARCO/0000-0002-3336-4965; Alves, Joao/0000-0002-4355-0921 FU Commonwealth of Australia; Australian Research Council; Austrian Science Fund (FWF) FX We would like to thank Ali Ahmad Khostovan, who worked with us on this project as a summer student in the SAO REU Summer Intern Program in 2011, an anonymous referee for comments that helped to improve the paper, and Malcolm Walmsley for a careful reading of the manuscript and additional constructive suggestions for improvement. The Mopra Radio Telescope 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. The University of New South Wales Digital Filter Bank used for the observations with the Mopra Telescope was provided with support from the Australian Research Council. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This publication is supported by the Austrian Science Fund (FWF). NR 25 TC 4 Z9 4 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 AUG PY 2014 VL 568 AR A27 DI 10.1051/0004-6361/201423913 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900079 ER PT J AU Jelic, V de Bruyn, AG Mevius, M Abdalla, FB Asad, KMB Bernardi, G Brentjens, MA Bus, S Chapman, E Ciardi, B Daiboo, S Fernandez, ER Ghosh, A Harker, G Jensen, H Kazemi, S Koopmans, LVE Labropoulos, P Martinez-Rubi, O Mellema, G Offringa, AR Pandey, VN Patil, AH Thomas, RM Vedantham, HK Veligatla, V Yatawatta, S Zaroubi, S Alexov, A Anderson, J Avruch, IM Beck, R Bell, ME Bentum, MJ Best, P Bonafede, A Bregman, J Breitling, F Broderick, J Brouw, WN Bruggen, M Butcher, HR Conway, JE de Gasperin, F de Geus, E Deller, A Dettmar, RJ Duscha, S Eisloffel, J Engels, D Faleke, H Fallows, RA Fender, R Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hamaker, JP Hassall, TE Haverkorn, M Heald, G Hessels, JWT Hoeft, M Horandel, J Horneffer, A van der Horst, A Iacobelli, M Juette, E Karastergiou, A Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G van Leeuwen, J Maat, P Mann, G McKay-Bakowski, D MeKean, JP Mank, H Nelles, A Morden, MJ Paas, H Pandey-Pornmier, M Pietka, G Pizzo, R Polatidis, AG Reich, W Rottgering, H Rowlinson, A Scaife, AMM Schwarz, D Serylak, M Smirnov, O Steinmetz, M Stewart, A Tagger, M Tang, Y Tasse, C ter Veen, S Thoudam, S Toribio, C Vermeulen, R Voeks, C van Weeren, RJ Wijers, RAMJ Wijnholds, SJ Wucknitz, O Zarka, P AF Jelic, V. de Bruyn, A. G. Mevius, M. Abdalla, F. B. Asad, K. M. B. Bernardi, G. Brentjens, M. A. Bus, S. Chapman, E. Ciardi, B. Daiboo, S. Fernandez, E. R. Ghosh, A. Harker, G. Jensen, H. Kazemi, S. Koopmans, L. V. E. Labropoulos, P. Martinez-Rubi, O. Mellema, G. Offringa, A. R. Pandey, V. N. Patil, A. H. Thomas, R. M. Vedantham, H. K. Veligatla, V. Yatawatta, S. Zaroubi, S. Alexov, A. Anderson, J. Avruch, I. M. Beck, R. Bell, M. E. Bentum, M. J. Best, P. Bonafede, A. Bregman, J. Breitling, F. Broderick, J. Brouw, W. N. Brueggen, M. Butcher, H. R. Conway, J. E. de Gasperin, F. de Geus, E. Deller, A. Dettmar, R. -J. Duscha, S. Eisloeffel, J. Engels, D. Faleke, H. Fallows, R. A. Fender, R. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hamaker, J. P. Hassall, T. E. Haverkorn, M. Heald, G. Hessels, J. W. T. Hoeft, M. Hoerandel, J. Horneffer, A. van der Horst, A. Iacobelli, M. Juette, E. Karastergiou, A. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. van Leeuwen, J. Maat, P. Mann, G. McKay-Bakowski, D. MeKean, J. P. Mank, H. Nelles, A. Morden, M. J. Paas, H. Pandey-Pornmier, M. Pietka, G. Pizzo, R. Polatidis, A. G. Reich, W. Roettgering, H. Rowlinson, A. Scaife, A. M. M. Schwarz, D. Serylak, M. Smirnov, O. Steinmetz, M. Stewart, A. Tagger, M. Tang, Y. Tasse, C. ter Veen, S. Thoudam, S. Toribio, C. Vermeulen, R. Voeks, C. van Weeren, R. J. Wijers, R. A. M. J. Wijnholds, S. J. Wucknitz, O. Zarka, P. TI Initial LOFAR observations of epoch of reionization windows II. Diffuse polarized emission in the ELAIS-N1 field SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radio continuum: ISM; techniques: interferometric; techniques: polarimetric; cosmology: observations; diffuse radiation; dark ages, reionization, first stars ID ROTATION MEASURE SYNTHESIS; NORTH CELESTIAL POLE; 350 MHZ; MULTIFREQUENCY POLARIMETRY; FOREGROUND REMOVAL; GALACTIC EMISSION; SELF-CALIBRATION; WIDE-FIELD; SKY SURVEY; RADIO AB Aims. This study aims to characterise the polarized foreground emission in the ELAIS-N1 field and to address its possible implications or extracting of the cosmological 21 cm signal from the LOw-Frequency ARray - Epoch of Reionization (LOFAR-EoR) data Methods. We used the high band antennas of LOFAR to image this region and RM-synthesis to unravel structures of polarized emission at high Galactic latitudes. Results. The brightness temperature of the detected Galactic emission is on average similar to 4 K in polarized intensity and covers the range from -10 to +13 rad m(-2) in Faraday depth, The total polarized intensity and polarization angle show a wide range of morphological features. We have also used the Westerbork Synthesis Radio Telescope (WSRT) at 350 MHz to image the same region. The LOFAR and WSRT images show a similar complex morphology at comparable brightness levels, but their spatial correlation is very low. The fractional polarization at 150 MHz, expressed as a percentage of the total intensity, amounts to approximate to 1.5%. There is no indication of diffuse emission in total intensity in the interferometric data. in line with results at higher frequencies Conclusions. The wide frequency range. high angular resolution, and high sensitivity make LOFAR an exquisite instrument for studying Galactic polarized emission at a resolution of similar to 1-2 rad m(-2) in Faraday depth. The different polarized patterns observed at 150 MHz and 350 MHz are consistent with different source distributions along the line of sight wring in a variety of Faraday thin regions of emission. The presence of polarized foregrounds is a serious complication for epoch of reionization experiments. To avoid the leakage of polarized emission into total intensity, which can depend on frequency, we need to calibrate the instrumental polarization across the field of view to a small fraction of 1%. C1 [Jelic, V.; de Bruyn, A. G.; Mevius, M.; Asad, K. M. B.; Bus, S.; Daiboo, S.; Fernandez, E. R.; Ghosh, A.; Kazemi, S.; Koopmans, L. V. E.; Labropoulos, P.; Martinez-Rubi, O.; Patil, A. H.; Thomas, R. M.; Vedantham, H. K.; Veligatla, V.; Zaroubi, S.; Avruch, I. M.; Brouw, W. N.; MeKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Jelic, V.; de Bruyn, A. G.; Brentjens, M. A.; Pandey, V. N.; Yatawatta, S.; Bentum, M. J.; Bregman, J.; Brouw, W. N.; de Geus, E.; Deller, A.; Duscha, S.; Faleke, H.; Fallows, R. A.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hamaker, J. P.; Heald, G.; Hessels, J. W. T.; Kondratiev, V. I.; Kuper, G.; van Leeuwen, J.; Maat, P.; MeKean, J. P.; Mank, H.; Morden, M. J.; Pizzo, R.; Polatidis, A. G.; Tang, Y.; Toribio, C.; Vermeulen, R.; Wijnholds, S. J.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Abdalla, F. B.; Chapman, E.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Bernardi, G.; Smirnov, O.] SKA SA, ZA-7405 Pinelands, South Africa. [Ciardi, B.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Harker, G.] 389 Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Jensen, H.; Mellema, G.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Jensen, H.; Mellema, G.] Stockholm Univ, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Offringa, A. R.; Butcher, H. R.] Australian Natl Univ, RSAA, Mt Stromlo Observ, Weston, ACT 2611, Australia. [Offringa, A. R.; Bell, M. E.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia. [Alexov, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Anderson, J.; Breitling, F.; Mann, G.; Steinmetz, M.; Voeks, C.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Avruch, I. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Beck, R.; Horneffer, A.; Kramer, M.; Kuniyoshi, M.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Broderick, J.; Hassall, T. E.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Conway, J. E.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Dettmar, R. -J.; Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessterwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Faleke, H.; Haverkorn, M.; Hoerandel, J.; Nelles, A.; ter Veen, S.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Fender, R.; Karastergiou, A.; Pietka, G.; Serylak, M.; Stewart, A.] Univ Oxford, Oxford OX1 3RH, England. [Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR7293, CNRS,Observ Cote Azur, F-06300 Nice, France. [Garrett, M. A.; Haverkorn, M.; Iacobelli, M.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmeier, J.; Tagger, M.] Univ Orleans, CNRS, LPC2E, Orleans, France. [Griessmeier, J.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS,INSU,USR 704,OSUC, F-18330 Nancay, France. [Hassall, T. E.; Kramer, M.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Hessels, J. W. T.; van der Horst, A.; van Leeuwen, J.; Rowlinson, A.; Wijers, R. A. M. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [McKay-Bakowski, D.] Univ Oulu, Sodankyla Geophys Observ, Sodankyla 99600, Finland. [McKay-Bakowski, D.] STFC Rutherford Appleton Lab, Didcot OX11 0QX, Oxon, England. [Paas, H.] Univ Groningen, Ctr Informat Technol, NL-9700 AB Groningen, Netherlands. [Pandey-Pornmier, 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. [Tasse, C.; Zarka, P.] Observ Paris, CNRS, LESIA, UMR 8109, F-92195 Meudon, France. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Jelic, V (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM vjelic@astro.rugnl RI Tagger, Michel/O-6615-2014; 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; Mellema, Garrelt/K-4962-2014; OI Tagger, Michel/0000-0003-2962-3220; de Gasperin, Francesco/0000-0003-4439-2627; Harker, Geraint/0000-0002-7894-4082; Kondratiev, Vladislav/0000-0001-8864-7471; Jelic, Vibor/0000-0002-6034-8610; Yatawatta, Sarod/0000-0001-5619-4017; Mellema, Garrelt/0000-0002-2512-6748; Wijers, Ralph/0000-0002-3101-1808; Abdalla, Filipe/0000-0003-2063-4345; Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660 FU VENT [639.041.336]; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] FX We thank an anonymous referee for useful comments that improved the manuscript. V.J. would like to thank the Netherlands Foundation for Scientific Research for financial support through VENT grant 639.041.336. C.F. acknowledges financial support by the Agence Nationale de la Recherche through grant ANR-09-JCJC-0001-01. The Low-Frequency Array (LOFAR) was designed and constructed by ASTRON, the Netherlands Institute for Radio Astronomy, and has facilities in several countries, which are owned by various parties (each with their own funding sources), and that are collectively operated by the International LOFAR Telescope (JET) foundation under a joint scientific policy. The WSRT is operated by ASTRON/NWO. NR 49 TC 23 Z9 23 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 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A101 DI 10.1051/0004-6361/201423998 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900093 ER PT J AU Lombardi, M Bouy, H Alves, J Lada, CJ AF Lombardi, Marco Bouy, Herve Alves, Joao Lada, Charles J. TI Herschel-Planck dust optical-depth and column-density maps I. Method description and results for Orion (vol 566, A45, 2014) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction C1 [Lombardi, Marco] Univ Milan, Dept Phys, I-20133 Milan, Italy. [Bouy, Herve] INTA CSIC, Ctr Astrobiol, Madrid, Spain. [Alves, Joao] Univ Vienna, A-1180 Vienna, Austria. [Lombardi, Marco; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lombardi, M (reprint author), Univ Milan, Dept Phys, Via Celoria 16, I-20133 Milan, Italy. EM marco.lombardi@unimi.it RI Bouy, Herve/H-2913-2012 OI Bouy, Herve/0000-0002-7084-487X NR 1 TC 1 Z9 1 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 DI 10.1051/0004-6361/201323293e PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900003 ER PT J AU Messias, H Dye, S Nagar, N Orellana, G Bussmann, RS Calanog, J Dannerbauer, H Fu, H Ibar, E Inohara, A Ivison, RJ Negrello, M Riechers, DA Sheen, YK Aguirre, JE Amber, S Birkinshaw, M Bourne, N Bradford, CM Clements, DL Cooray, A De Zotti, G Demarco, R Dunne, L Eales, S Fleuren, S Kamenetzky, J Lupu, RE Maddox, SJ Marrone, DP Michalowski, MJ Murphy, EJ Nguyen, HT Omont, A Rowlands, K Smith, D Smith, M Valiante, E Vieira, JD AF Messias, Hugo Dye, Simon Nagar, Neil Orellana, Gustavo Bussmann, R. Shane Calanog, Jae Dannerbauer, Helmut Fu, Hai Ibar, Edo Inohara, Andrew Ivison, R. J. Negrello, Mattia Riechers, Dominik A. Sheen, Yun-Kyeong Aguirre, James E. Amber, Simon Birkinshaw, Mark Bourne, Nathan Bradford, Charles M. Clements, Dave L. Cooray, Asantha De Zotti, Gianfranco Demarco, Ricardo Dunne, Loretta Eales, Stephen Fleuren, Simone Kamenetzky, Julia Lupu, Roxana E. Maddox, Steve J. Marrone, Daniel P. Michalowski, Michal J. Murphy, Eric J. Nguyen, Hien T. Omont, Alain Rowlands, Kate Smith, Dan Smith, Matt Valiante, Elisabetta Vieira, Joaquin D. TI Herschel-ATLAS and ALMA HATLAS J142935.3-002836, a lensed major merger at redshift 1.027 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong; galaxies: ISM; galaxies: kinematics and dynamics ID STAR-FORMING GALAXIES; SCIENCE DEMONSTRATION PHASE; DEGREE EXTRAGALACTIC SURVEY; SPITZER-SPACE-TELESCOPE; 1200-MU-M MAMBO SURVEY; DIGITAL SKY SURVEY; DEEP FIELD-SOUTH; SUBMILLIMETER GALAXIES; MOLECULAR GAS; INTERSTELLAR-MEDIUM AB Context. The submillimetre-bright galaxy population is believed to comprise, aside from local galaxies and radio-loud sources, intrinsically active star-forming galaxies, the brightest of which are lensed gravitationally. The latter enable studies at a level of detail beyond what is usually possible by the observation facility. Aims. This work focuses on one of these lensed systems, HATLAS J142935.3-002836 (H1429-0028), selected in the Herschel-ATLAS field. Gathering a rich, multi-wavelength dataset, we aim to confirm the lensing hypothesis and model the background source's morphology and dynamics, as well as to provide a full physical characterisation. Methods. Multi-wavelength high-resolution data is utilised to assess the nature of the system. A lensing-analysis algorithm that simultaneously fits different wavebands is adopted to characterise the lens. The background galaxy dynamical information is studied by reconstructing the 3D source plane of the ALMA CO (J: 4 -> 3) transition. Near-IR imaging from HST and Keck-AO allows to constrain rest-frame optical photometry independently for the foreground and background systems. Physical parameters (such as stellar and dust masses) are estimated via modelling of the spectral energy distribution taking source blending, foreground obscuration, and differential magnification into account. Results. The system comprises a foreground edge-on disk galaxy (at z(sp) = 0.218) with an almost complete Einstein ring around it. The background source (at z(sp) = 1.027) is magnified by a factor of p = 8-10 depending on wavelength. It is comprised of two components and a tens-of-kpc-long tidal tail resembling the Antenna merger. As a whole, the background source is a massive stellar system (1.32(0.41)(+0.63) x 10(11) M.) forming stars at a rate of 394 +/- 90 Mo yr(-1), and it has a significant gas reservoir M-ISM = 4.6 + 1.7 x 10(10) M-circle dot. Its depletion time due to star formation alone is thus expected to be T-sF = M-ISM/SFR = 117 +/- 51 Myr. The dynamical mass of one of the components is estimated to be 5.8 +/- 1.7 x 10(10) M., and, together with the photometric total mass estimate, it implies that H1429-0028 is a major merger system (1: 2.8+ 1). C1 [Messias, Hugo; Nagar, Neil; Orellana, Gustavo; Sheen, Yun-Kyeong; Demarco, Ricardo] Univ Concepcion, Barrio Univ, Concepcion, Chile. [Messias, Hugo] Univ Lisbon, Ctr Astron & Astrofis, Observatorio Astron Lisboa, P-1349018 Lisbon, Portugal. [Dye, Simon; Bourne, Nathan] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Bussmann, R. Shane] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Calanog, Jae; Inohara, Andrew; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dannerbauer, Helmut] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Fu, Hai] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Ibar, Edo] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile. [Ivison, R. J.; Dunne, Loretta; Maddox, Steve J.; Michalowski, Michal J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] European So Observ, Garching, Germany. [Negrello, Mattia; De Zotti, Gianfranco] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Riechers, Dominik A.; Cooray, Asantha] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Riechers, Dominik A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Aguirre, James E.; Lupu, Roxana E.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Amber, Simon] Open Univ, Milton Keynes MK7 6BJ, Bucks, England. [Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Birkinshaw, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bradford, Charles M.; Nguyen, Hien T.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Clements, Dave L.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Dunne, Loretta; Maddox, Steve J.] Univ Canterbury, Dept Phys & Astron, Christchurch 8140, New Zealand. [Eales, Stephen; Smith, Matt; Valiante, Elisabetta] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Fleuren, Simone] Univ London, Sch Math Sci, London E1 4NS, England. [Kamenetzky, Julia] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Marrone, Daniel P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Murphy, Eric J.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Omont, Alain] Univ Paris 06, Inst Astrophys Paris, UNIR 7095, CNRS, F-75014 Paris, France. [Rowlands, Kate] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Smith, Dan] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Vieira, Joaquin D.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Vieira, Joaquin D.] Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP Messias, H (reprint author), Univ Concepcion, Barrio Univ, Concepcion, Chile. EM hmessias@oal.ul.pt RI Lupu, Roxana/P-9060-2014; Ivison, R./G-4450-2011; OI Lupu, Roxana/0000-0003-3444-5908; Ivison, R./0000-0001-5118-1313; Marrone, Daniel/0000-0002-2367-1080; De Zotti, Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X; Dye, Simon/0000-0002-1318-8343 FU CONYCIT-ALMA [31100008]; FCT [SFRH/BPD/97986/2013, PTDC/FIS-AST/2194/2012, PEst-OE/FIS/UI2751/2014]; NSF [AST-1313319]; CONICYT/FONDECYT [3130504]; FONDECYT [3130470]; BASAL centre for Astrophysics and Associated Technologies (CATA) and by FONDECYT [1130528] FX H.M. acknowledges the support by CONYCIT-ALMA through a post-doc scholarship under the project 31100008. HM acknowledges support by FCT via the post-doctoral fellowship SFRH/BPD/97986/2013 and the programs PTDC/FIS-AST/2194/2012 and PEst-OE/FIS/UI2751/2014. N.N. and R.D. acknowledge support from BASAL PFB-06/2007, Fondecyt 1100540 and Anillo ACT1101. J.A.C. and A. C. acknowledge support from NSF AST-1313319. E.I. acknowledges funding from CONICYT/FONDECYT postdoctoral project No: 3130504. R.J.I., S.J.M. and L.D. ackowledge support from the European Research Council in the form of Advanced Investigator grant, COSMICISM. Y.K.S. acknowledges support by FONDECYT Grant No. 3130470. R.D. acknowledges the support provided by the BASAL centre for Astrophysics and Associated Technologies (CATA) and by FONDECYT N. 1130528. K.R. acknowledges support from the European Research Council Starting Grant SEDmorph (P.I. Wild). This paper makes use of the following ALMA data: ADS/JAO. ALMA#2011.0.00476. 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. This publication is based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. We are grateful to the competent staff at the APEX base-camp in Sequitor, Chile and the Z-Spec instrument team. 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. Based in part on observations obtained at the Gemini Observatory (include additional acknowledgement here, see Sect. 1.2), 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 Inovagao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). The Herschel-ATLAS is a project with Herschel, 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/. Based in part on observations carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). 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 recognise and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This 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 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. The authors thank the ALMA contact scientist Adam Leroy for the help throughout scheduling block preparation and quality assurance, and the help provided by Alexander J. Conley and Elisabete da Cunha handling, respectively, the MBBEMCEE and MAGPHYS codes. NR 143 TC 13 Z9 13 U1 1 U2 4 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 2014 VL 568 AR A92 DI 10.1051/0004-6361/201424410 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900134 ER PT J AU Morosan, DE Gallagher, PT Zucca, P Fallows, R Carley, EP Mann, G Bisi, MM Kerdraon, A Konovalenko, AA MacKinnon, AL Rucker, HO Thide, B Magdalenic, J Vocks, C Reid, H Anderson, J Asgekar, A Avruch, OM Bentum, MJ Bernardi, G Best, P Bonafede, A Bregman, I Breitling, F Broderick, J Bruggen, M Butcher, HR Ciardi, B Conway, JE de Gasperin, F de Geus, E Deller, A Duscha, S Eisloffel, J Engels, D Falcke, H Ferrari, C Frieswijk, W Garrett, MA Griessmeier, J Gunst, AW Hassall, TE Hessels, JWT Hoeft, M Horandel, J Horneffer, A Iacobelli, M Juette, E Karastergiou, A Kondratiev, VI Kramer, M Kuniyoshi, M Kuper, G Maat, P Markoff, S 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 Reich, W Rottgering, H Scaife, AMM Schwarz, D Serylak, M Smirnov, O Stappers, BW Stewart, A Tagger, M Tang, Y Tasse, C Thoudam, S Toribio, C Vermeulen, R van Weeren, RJ Wucknitz, O Yatawatta, S Zarka, P AF Morosan, D. E. Gallagher, P. T. Zucca, P. Fallows, R. Carley, E. P. Mann, G. Bisi, M. M. Kerdraon, A. Konovalenko, A. A. MacKinnon, A. L. Rucker, H. O. Thide, B. Magdalenic, J. Vocks, C. Reid, H. Anderson, J. Asgekar, A. Avruch, O. M. Bentum, M. J. Bernardi, G. Best, P. Bonafede, A. Bregman, I. Breitling, F. Broderick, J. Brueggen, M. Butcher, H. R. Ciardi, B. Conway, J. E. de Gasperin, F. de Geus, E. Deller, A. Duscha, S. Eisloeffel, J. Engels, D. Falcke, H. Ferrari, C. Frieswijk, W. Garrett, M. A. Griessmeier, J. Gunst, A. W. Hassall, T. E. Hessels, J. W. T. Hoeft, M. Hoerandel, J. Horneffer, A. Iacobelli, M. Juette, E. Karastergiou, A. Kondratiev, V. I. Kramer, M. Kuniyoshi, M. Kuper, G. Maat, P. Markoff, S. 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. Reich, W. Roettgering, H. Scaife, A. M. M. Schwarz, D. Serylak, M. Smirnov, O. Stappers, B. W. Stewart, A. Tagger, M. Tang, Y. Tasse, C. Thoudam, S. Toribio, C. Vermeulen, R. van Weeren, R. J. Wucknitz, O. Yatawatta, S. Zarka, P. TI LOFAR tied-array imaging of Type III solar radio bursts SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; Sun: radio radiation; Sun: particle emission; Sun: coronal mass ejections (CMEs) ID PLASMA EMISSION; ELECTRONS; WAVES; SHOCK; RADIOHELIOGRAPH; ACCELERATION; SPACECRAFT; DENSITY; CORONA AB Context. The Sun is an active source of radio emission which is often associated with energetic phenomena such as solar flares and coronal mass ejections (CMEs). At low radio frequencies (< 100 MHz), the Sun has not been imaged extensively because of the instrumental limitations of previous radio telescopes. Aims. Here, the combined high spatial, spectral, and temporal resolution of the LOw Frequency ARray (LOFAR) was used to study solar Type III radio bursts at 30-90 MHz and their association with CMEs. Methods. The Sun was imaged with 126 simultaneous tied-array beams within <= 5 R-circle dot of the solar centre. This method offers benefits over standard interferometric imaging since each beam produces high temporal (similar to 83 ms) and spectral resolution (12.5 kHz) dynamic spectra at an array of spatial locations centred on the Sun. LOFAR's standard interferometric output is currently limited to one image per second. Results. Over a period of 30 min, multiple Type III radio bursts were observed, a number of which were found to be located at high altitudes (similar to 4 R-circle dot from the solar center at 30 MHz) and to have non-radial trajectories. These bursts occurred at altitudes in excess of values predicted by 1D radial electron density models. The non-radial high altitude Type III bursts were found to be associated with the expanding flank of a CME. Conclusions. The CME may have compressed neighbouring streamer plasma producing larger electron densities at high altitudes, while the non-radial burst trajectories can be explained by the deflection of radial magnetic fields as the CME expanded in the low corona. C1 [Morosan, D. E.; Gallagher, P. T.; Zucca, P.; Carley, E. P.] Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. [Fallows, R.; Asgekar, A.; Bentum, M. J.; Bregman, I.; de Geus, E.; Deller, A.; Duscha, S.; Falcke, H.; Frieswijk, W.; Garrett, M. A.; Gunst, A. W.; Hessels, J. W. T.; Kondratiev, V. I.; Kuper, G.; Maat, P.; McKean, J. P.; Munk, H.; Norden, M. J.; Orru, E.; Pandey, V. N.; Pizzo, R.; Polatidis, A. G.; Tang, Y.; Toribio, C.; Vermeulen, R.; Yatawatta, S.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Mann, G.; Vocks, C.; Anderson, J.; Breitling, F.] Leibniz Inst Astrophys Potsdam AIP, D-14482 Potsdam, Germany. [Bisi, M. M.] Rutherford Appleton Lab, RAL Space Sci & Technol Facil Council, Didcot OX11 0QX, Oxon, England. [Kerdraon, A.; Tasse, C.; Zarka, P.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [Konovalenko, A. A.] Inst Radio Astron, UA-61002 Kharkov, Ukraine. [MacKinnon, A. L.; Reid, H.] Univ Glasgow, SUPA, Sch Phys & Astron, Glasgow G12 8QQ, Lanark, Scotland. [Rucker, H. O.] Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. [Thide, B.] Swedish Inst Space Phys, S-75121 Uppsala, Sweden. [Magdalenic, J.] Royal Observ Belgium, SIDC, Solar Terr Ctr Excellence, B-1180 Brussels, Belgium. [Asgekar, A.] Shell Technol Ctr, Bangalore 560099, Karnataka, India. [Avruch, O. M.] SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Avruch, O. M.; McKean, J. P.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bernardi, G.; van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Best, P.] Univ Edinburgh, Inst Astron, Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland. [Bonafede, A.; Brueggen, M.; de Gasperin, F.] Univ Hamburg, D-21029 Hamburg, Germany. [Broderick, J.; Hassall, T. E.; Scaife, A. M. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Butcher, H. R.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ciardi, B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Conway, J. E.] Chalmers, Dept Earth & Space Sci, Onsala Space Observ, S-43992 Onsala, Sweden. [Eisloeffel, J.; Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. [Engels, D.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Falcke, H.; Hoerandel, J.; Nelles, A.; Thoudam, S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Ferrari, C.] Univ Nice Sophia Antipolis, Lab Lagrange, UMR7293, CNRS,Observ Cote Azur, F-06300 Nice, France. [Garrett, M. A.; Iacobelli, M.; Roettgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Griessmeier, J.; Tagger, M.] Univ Orleans, LPC2E, CNRS, F-45071 Orleans, France. [Griessmeier, J.] Univ Orleans, Stn Radioastron Nancay, Observ Paris, CNRS,INSU,USR 704,OSUC, F-18330 Nancay, France. [Hassall, T. E.; Kramer, M.; Stappers, B. W.] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Hessels, J. W. T.; Markoff, S.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Horneffer, A.; Kramer, M.; Kuniyoshi, M.; Mulcahy, D. D.; Reich, W.; Wucknitz, O.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Juette, E.] Ruhr Univ Bochum, Astron Inst, D-44780 Bochum, Germany. [Karastergiou, A.; Pietka, G.; Serylak, M.; Stewart, A.] Univ Oxford, Oxford OX1 3RH, England. [Kondratiev, V. I.] Lebedev Phys Inst, Ctr Astro Space, Moscow 117997, Russia. [Paas, H.] Univ Groningen, Ctr Informat Technol, NL-9700 AB 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 Afric, ZA-7405 Pinelands, South Africa. [Wucknitz, O.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. RP Morosan, DE (reprint author), Univ Dublin Trinity Coll, Sch Phys, Dublin 2, Ireland. EM morosand@tcd.ie RI Tagger, Michel/O-6615-2014; Ciardi, Benedetta/N-7625-2015; Gallagher, Peter/C-7717-2011; Kondratiev, Vladislav/N-1105-2015; Yatawatta, Sarod/E-6037-2013; OI Tagger, Michel/0000-0003-2962-3220; Gallagher, Peter/0000-0001-9745-0400; Kondratiev, Vladislav/0000-0001-8864-7471; Yatawatta, Sarod/0000-0001-5619-4017; de Gasperin, Francesco/0000-0003-4439-2627; Deller, Adam/0000-0001-9434-3837; van Weeren, Reinout/0000-0002-0587-1660 FU Government of Ireland studentship from the Irish Research Council (IRC); Non-Foundation Scholarship - Trinity College Dublin; Innovation Academy; IRC New Frontiers; Agence Nationale de la Recherche [ANR-09-JCJC-0001-01] 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 and the Innovation Academy. We would also like to acknowledge the IRC New Frontiers Funding for supporting LOFAR related travel. Chiara Ferrari acknowledges financial support by the "Agence Nationale de la Recherche" through grant ANR-09-JCJC-0001-01. We would finally like to acknowledge the LOFAR telescope which is made possible by the hard work of dozens of engineers, technicians, developers, observers and support scientists. 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 45 TC 12 Z9 12 U1 0 U2 8 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2014 VL 568 AR A67 DI 10.1051/0004-6361/201423936 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900083 ER PT J AU Santangelo, G Nisini, B Codella, C Lorenzani, A Yildiz, UA Antoniucci, S Bjerkeli, P Cabrit, S Giannini, T Kristensen, LE Liseau, R Mottram, JC Tafalla, M van Dishoeck, EF AF Santangelo, G. Nisini, B. Codella, C. Lorenzani, A. Yildiz, U. A. Antoniucci, S. Bjerkeli, P. Cabrit, S. Giannini, T. Kristensen, L. E. Liseau, R. Mottram, J. C. Tafalla, M. van Dishoeck, E. F. TI Water distribution in shocked regions of the NGC 1333-IRAS 4A protostellar outflow SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: low mass; ISM: jets and outflows; ISM: molecules; ISM: individual objects: NGC 1333-IRAS 4A; stars: formation ID STAR-FORMING REGIONS; LOW-MASS PROTOSTARS; YOUNG STELLAR OBJECTS; HERSCHEL-HIFI; MOLECULAR OUTFLOW; NGC-1333 IRAS-4; KEY PROGRAM; CO EMISSION; L1157; PACS AB Context. Water is a key molecule in protostellar environments because its line emission is very sensitive to both the chemistry and the physical conditions of the gas. Observations of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observatory have highlighted the complexity of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ line profiles, in which different kinematic components can be distinguished. Aims. The goal is to study the spatial distribution of H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ, in particular of the different kinematic components detected in H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emission, at two bright shocked regions along IRAS 4A, one of the strongest H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emitters among the Class 0 outflows. Methods. We obtained Herschel-PACS maps of the IRAS 4A outflow and HIFI observations of two shocked positions. The largest HIFI beam of 38'' at 557 GHz was mapped in several key water lines with different upper energy levels, to reveal possible spatial variations of the line profiles. A large velocity gradient (LVG) analysis was performed to determine the excitation conditions of the gas. Results. We detect four H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ lines and CO (16-15) at the two selected shocked positions. In addition, transitions from related outflow and envelope tracers are detected. Different gas components associated with the shock are identified in the H2O emission. In particular, at the head of the red lobe of the outflow, two distinct gas components with different excitation conditions are distinguished in the HIFI emission maps: a compact component, detected in the ground-state water lines, and a more extended one. Assuming that these two components correspond to two different temperature components observed in previous H2O and CO studies, the LVG analysis of the H2O line emission from low-mass protostars and their associated outflows performed with HIFI onboard the Herschel Space Observ emission suggests that the compact (about 32, corresponding to about 700 AU) component is associated with a hot (T similar to 1000 K) gas with densities n(H2) similar to (1-4) x 10(5) cm(-3), whereas the extended (10 ''-17 '', corresponding to 2400-4000 AU) one traces a warm (T similar to 300-500 K) and dense gas (n(H2) similar to (3-5) x 10(7) cm(-3)). Finally, using the CO (16-15) emission observed at R2 and assuming a typical CO/H-2 abundance of 10(-4), we estimate the H2O/H-2 abundance of the warm and hot components to be (7-10) x 10(-7) and (3-7) x 10(-5). Conclusions. Our data allowed us, for the first time, to resolve spatially the two temperature components previously observed with HIFI and PACS. We propose that the compact hot component may be associated with the jet that impacts the surrounding material, whereas the warm, dense, and extended component originates from the compression of the ambient gas by the propagating flow. C1 [Santangelo, G.; Codella, C.; Lorenzani, A.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Santangelo, G.; Nisini, B.; Antoniucci, S.; Giannini, T.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Yildiz, U. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bjerkeli, P.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Bjerkeli, P.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Bjerkeli, P.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Bjerkeli, P.; Liseau, R.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Cabrit, S.] CNRS, Observ Paris, UMR 8112, LERMA, F-75014 Paris, France. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mottram, J. C.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys MPE, D-85748 Garching, Germany. RP Santangelo, G (reprint author), Osserv Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM gina@arcetri.astro.it RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; OI Giannini, Teresa/0000-0002-0224-096X; , Brunella Nisini/0000-0002-9190-0113; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Lorenzani, Andrea/0000-0002-4685-3434; Bjerkeli, Per/0000-0002-7993-4118; Antoniucci, Simone/0000-0002-0666-3847; Codella, Claudio/0000-0003-1514-3074 FU ASI project [01/005/11/0] FX Herschel activities at INAF are financially supported by the ASI project 01/005/11/0. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research. Groningen, The Netherlands and with major contributions from Germany, France and the US, Consortium members are Canada: CSA, U.Waterloo; France; CESR. LAB, LERMA, IRAM: Germany: ROSMA. MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetti- INAF; The Netherlands; SRON, TUD; Poland: CAMK, CHK: Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA): Sweden: Chalmers University of Technology - MC2. RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich. FHNW: USA; Caltech, JPL NHSC. NR 42 TC 8 Z9 8 U1 1 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 2014 VL 568 DI 10.1051/0004-6361/201424034 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900099 ER PT J AU Sodor, A Chene, AN De Cat, P Bognar, Z Wright, DJ Marois, C Walker, GAH Matthews, JM Kallinger, T Rowe, JF Kuschnig, R Guenther, DB Moffat, AFJ Rucinski, SM Sasselov, D Weiss, WW AF Sodor, A. Chene, A. -N. De Cat, P. Bognar, Zs. Wright, D. J. Marois, C. Walker, G. A. H. Matthews, J. M. Kallinger, T. Rowe, J. F. Kuschnig, R. Guenther, D. B. Moffat, A. F. J. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI MOST light-curve analysis of the gamma Doradus pulsator HR 8799, showing resonances and amplitude variations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: photometric; stars: individual: HR 8799; stars: oscillations ID RR LYRAE STARS; 1ST DETECTION; DEBRIS DISK; VEGA-LIKE; ASTEROSEISMOLOGY; FREQUENCIES; MODULATION; PHOTOMETRY; MULTISITE; PLANETS AB Context-The central star of the HR 8799 system is a gamma Dorados-type pulsator. The system harbours four planetary mass companions detected by direct imaging. and is a good solar system analogue. The masses of the companions are not accurately known because the estimation depends greatly on the age of the system, which is also not known with sufficient accuracy. Asteroseisrnic studies of the star might help to better constrain the age of HR 8799. We organized an extensive photometric and multi site spectroscopic observing campaign to study the pulsations of the central star. Aims. The aim of the present study is to investigate the pulsation properties of HR 8799 in detail via the ultra-precise 47 d nearly continuous photometry obtained with the Microvariability and Oscillations in STars (MOST) space telescope, and to find as many independent pulsation modes as possible, which is the prerequisite for an asteroseismic age determination. Methods. We carried out Fourier analysis of the wide band photometric time series. Results. We find that resonance and sudden amplitude changes characterize the pulsation of HR 8799. The dominant frequency is always at f(1) = 1.978 d(-1). Many multiples of one-ninth of the dominant frequency appear in the Fourier spectrum of the MOST data: n/9 f(1). where n =[1, 2, 3, 4. 5, 6,7, 8, 9, 10, 13, 14, 17, 18]. Our analysis also reveals that many of these peaks show strong amplitude decrease and phase variations even on the 47 d time scale. The dependencies between the pulsation frequencies of HR 8799 make the planned subsequent asteroseismic analysis rather difficult We point out some resemblance between the light curve of HR 8799 and the modulated pulsation light curves of Blazhko RR Lyrae stars. C1 [Sodor, A.; De Cat, P.; Wright, D. J.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Sodor, A.; Bognar, Zs.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Chene, A. -N.] Northern Operat Ctr, Gemini Observ, Hilo, HI 96720 USA. [Wright, D. J.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. [Marois, C.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kallinger, T.; Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron IfA, A-1180 Vienna, Austria. [Rowe, J. F.] NASA Ames Res Pk, Moffett Field, CA 94035 USA. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Rucinski, S. M.] Univ Toronto, David Dunlap Observ, Dept Astron & Astrophys, Richmond Hill, ON L4C 4Y6, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sodor, A (reprint author), Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium. EM adam.sodor@oma.be OI Kallinger, Thomas/0000-0003-3627-2561 FU Belgian Federal Science Policy [M0/33/029]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; Austrian Science Fonds (EWE) [P22691-N16] FX A.S. acknowledges support by the Belgian Federal Science Policy (project M0/33/029, PI: P.D.C.) and by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. WM. acknowledges support by the Austrian Science Fonds (EWE) P22691-N16. NR 26 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 2014 VL 568 AR A106 DI 10.1051/0004-6361/201423976 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO2VZ UT WOS:000341185900090 ER PT J AU Grandfield, K Chattah, NLT Djomehri, S Eidelmann, N Eichmiller, FC Webb, S Schuck, PJ Nweeia, M Ho, SP AF Grandfield, Kathryn Chattah, Netta Lev-Tov Djomehri, Sabra Eidelmann, Naomi Eichmiller, Frederick C. Webb, Samuel Schuck, P. James Nweeia, Martin Ho, Sunita P. TI The narwhal (Monodon monoceros) cementum-dentin junction: A functionally graded biointerphase SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART H-JOURNAL OF ENGINEERING IN MEDICINE LA English DT Article DE Monodon monoceros; narwhal; cementum-dentin junction; biomechanics; functional interface ID AGGRESSIVE TUSK USE; MECHANICAL-PROPERTIES; SPECKLE INTERFEROMETRY; CHEMICAL-COMPOSITION; BIOLOGICAL-MATERIALS; MINERALIZED TISSUES; TOOTH; COLLAGEN; ENAMEL; DEFORMATION AB In nature, an interface between dissimilar tissues is often bridged by a graded zone, and provides functional properties at a whole organ level. A perfect example is a biological interphase between stratified cementum and dentin of a narwhal tooth. This study highlights the graded structural, mechanical, and chemical natural characteristics of a biological interphase known as the cementum-dentin junction layer and their effect in resisting mechanical loads. From a structural perspective, light and electron microscopy techniques illustrated the layer as a wide 1000-2000m graded zone consisting of higher density continuous collagen fiber bundles from the surface of cementum to dentin, that parallels hygroscopic 50-100m wide collagenous region in human teeth. The role of collagen fibers was evident under compression testing during which the layer deformed more compared to cementum and dentin. This behavior is reflected through site-specific nanoindentation indicating a lower elastic modulus of 2.2 +/- 0.5 GPa for collagen fiber bundle compared to 3 +/- 0.4 GPa for mineralized regions in the layer. Similarly, microindentation technique illustrated lower hardness values of 0.36 +/- 0.05 GPa, 0.33 +/- 0.03 GPa, and 0.3 +/- 0.07 GPa for cementum, dentin, and cementum-dentin layer, respectively. Biochemical analyses including Raman spectroscopy and synchrotron-source microprobe X-ray fluorescence demonstrated a graded composition across the interface, including a decrease in mineral-to-matrix and phosphate-to-carbonate ratios, as well as the presence of tidemark-like bands with Zn. Understanding the structure-function relationships of wider tissue interfaces can provide insights into natural tissue and organ function. C1 [Grandfield, Kathryn; Djomehri, Sabra; Ho, Sunita P.] Univ Calif San Francisco, Dept Prevent & Restorat Dent Sci, Div Biomat & Bioengn, San Francisco, CA 94143 USA. [Chattah, Netta Lev-Tov] Israel Natl Police, Div Identificat & Forens Sci, Jerusalem, Israel. [Eidelmann, Naomi] NIST, Paffenbarger Res Ctr, Amer Dent Assoc Fdn, Gaithersburg, MD 20899 USA. [Eichmiller, Frederick C.] Delta Dent Wisconsin, Stevens Point, WI USA. [Webb, Samuel] SLAC Natl Accelerator Lab, Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA USA. [Schuck, P. James] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Mat Sci, Mol Foundry, Berkeley, CA 94720 USA. [Nweeia, Martin] Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Ho, SP (reprint author), Univ Calif San Francisco, Dept Prevent & Restorat Dent Sci, Div Biomat & Bioengn, San Francisco, CA 94143 USA. EM sunita.ho@ucsf.edu RI Foundry, Molecular/G-9968-2014 FU NIH/NIDCR [R00DE018212]; NIH/NCRR [S10RR026645]; Department of Preventive and Restorative Dental Sciences, UCSF; Department of Orofacial Sciences, UCSF; Faculty of Engineering, McMaster University, Canada; Office of Science, Office of Basic Energy Sciences, Division of Materials Sciences and Engineering, of the U.S. Department of Energy [DE-AC02-05CH11231]; [NIH/NIDCR-R01DE022032] FX The authors acknowledge funding support from NIH/NIDCR R00DE018212 (SPH), NIH/NIDCR-R01DE022032 (SPH), NIH/NCRR S10RR026645 (SPH) and Departments of Preventive and Restorative Dental Sciences and Orofacial Sciences, UCSF. K. G. acknowledges financial support from the Faculty of Engineering, McMaster University, Canada. Work at the Molecular Foundry was supported by the Director, Office of Science, Office of Basic Energy Sciences, Division of Materials Sciences and Engineering, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 44 TC 2 Z9 2 U1 8 U2 35 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-4119 EI 2041-3033 J9 P I MECH ENG H JI Proc. Inst. Mech. Eng. Part H-J. Eng. Med. PD AUG PY 2014 VL 228 IS 8 BP 754 EP 767 DI 10.1177/0954411914547553 PG 14 WC Engineering, Biomedical SC Engineering GA AP4PA UT WOS:000342058800002 PM 25205746 ER PT J AU Bianco, FB Modjaz, M Hicken, M Friedman, A Kirshner, RP Bloom, JS Challis, P Marion, GH Wood-Vasey, WM Rest, A AF Bianco, F. B. Modjaz, M. Hicken, M. Friedman, A. Kirshner, R. P. Bloom, J. S. Challis, P. Marion, G. H. Wood-Vasey, W. M. Rest, A. TI MULTI-COLOR OPTICAL AND NEAR-INFRARED LIGHT CURVES OF 64 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE supernovae: general ID RICH CIRCUMSTELLAR MEDIUM; GAMMA-RAY BURST; DIGITAL SKY SURVEY; IA SUPERNOVAE; IC SUPERNOVA; ABSOLUTE MAGNITUDE; IMAGE SUBTRACTION; NEUTRON-STAR; SN 2006JC; PHOTOMETRY AB We present a densely sampled, homogeneous set of light curves of 64 low-redshift (z less than or similar to 0.05) stripped-envelope supernovae (SNe of Type IIb, Ib, Ic, and Ic-BL). These data were obtained between 2001 and 2009 at the Fred L. Whipple Observatory (FLWO) on Mount Hopkins in Arizona, with the optical FLWO 1.2 m and the near-infrared (NIR) Peters Automated Infrared 1.3 m telescopes. Our data set consists of 4543 optical photometric measurements on 61 SNe, including a combination of UBVRI, UBVr'i', and u'BVr'i', and 1919 JHK(s) NIR measurements on 25 SNe. This sample constitutes the most extensive multi-color data set of stripped-envelope SNe to date. Our photometry is based on template-subtracted images to eliminate any potential host-galaxy light contamination. This work presents these photometric data, compares them with data in the literature, and estimates basic statistical quantities: date of maximum, color, and photometric properties. We identify promising color trends that may permit the identification of stripped-envelope SN subtypes from their photometry alone. Many of these SNe were observed spectroscopically by the Harvard-Smithsonian Center for Astrophysics (CfA) SN group, and the spectra are presented in a companion paper. A thorough exploration that combines the CfA photometry and spectroscopy of stripped-envelope core-collapse SNe will be presented in a follow-up paper. C1 [Bianco, F. B.; Modjaz, M.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Hicken, M.; Friedman, A.; Kirshner, R. P.; Challis, P.; Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Friedman, A.] MIT, Ctr Theoret Phys, Cambridge, MA 02139 USA. [Friedman, A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bloom, J. S.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marion, G. H.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Wood-Vasey, W. M.] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Bianco, FB (reprint author), NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA. EM fb55@nyu.edu RI Friedman, Andrew/I-4691-2013 OI Friedman, Andrew/0000-0003-1334-039X FU James Arthur fellowship at the Center for Cosmology and Particle Physics at NYU; NSF CAREER [AST-1352405]; National Science Foundation [AST06-06772]; NSF [AST09-07903, AST12-11196]; Kavli Institute for Theoretical Physics NSF [PHY99-07949]; Harvard University Milton Fund; University of Virginia; SAO; UC Berkeley; University of Massachusetts; Infrared Processing and Analysis Center/California Institute of Technology; NASA FX F.B.B. is supported by a James Arthur fellowship at the Center for Cosmology and Particle Physics at NYU. M.M. is supported in part by NSF CAREER award AST-1352405. Supernova research at Harvard University has been supported in part by the National Science Foundation grant AST06-06772 and R.P.K. in part by the NSF grants AST09-07903 and AST12-11196, and in part by the Kavli Institute for Theoretical Physics NSF grant PHY99-07949. Observations reported here were obtained at the F.L. Whipple Observatory, which is operated by the Smithsonian Astrophysical Observatory (SAO). PAIRITEL is operated by the Smithsonian Astrophysical Observatory and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and UC Berkeley. The data analysis in this paper has made use of the Hydra computer cluster run by the Computation Facility at the Harvard-Smithsonian Center for Astrophysics.; This research has made use of NASA's Astrophysics Data System Bibliographic Services (ADS), the HyperLEDA database, 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. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and NSF. NR 95 TC 29 Z9 29 U1 2 U2 10 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 2014 VL 213 IS 2 AR 19 DI 10.1088/0067-0049/213/2/19 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TM UT WOS:000341777400001 ER PT J AU Geller, MJ Hwang, HS Fabricant, DG Kurtz, MJ Dell'Antonio, IP Zahid, HJ AF Geller, Margaret J. Hwang, Ho Seong Fabricant, Daniel G. Kurtz, Michael J. Dell'Antonio, Ian P. Zahid, Harus Jabran TI SHELS: A COMPLETE GALAXY REDSHIFT SURVEY WITH R <= 20.6 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: abundances; galaxies: distances and redshifts; galaxies: evolution; large-scale structure of universe; surveys ID DIGITAL SKY SURVEY; FIBER-FED SPECTROGRAPH; 10K-BRIGHT SPECTROSCOPIC SAMPLE; DATA REDUCTION TECHNIQUES; STAR-FORMATION HISTORIES; MASS ASSEMBLY HISTORY; FIELD GALAXIES; LUMINOSITY FUNCTION; SPECTRAL PROPERTIES; EVOLUTION AB The SHELS (Smithsonian Hectospec Lensing Survey) is a complete redshift survey covering two well-separated fields (F1 and F2) of the Deep Lens Survey to a limiting R = 20.6. Here we describe the redshift survey of the F2 field (R.A.(2000) = 09(h)19(m)32(s).4 s and decl.(2000) = +30 degrees 00'00 '' ). The survey includes 16,294 new redshifts measured with the Hectospec on the MMT. The resulting survey of the 4 deg(2) F2 field is 95% complete to R = 20.6, currently the densest survey to this magnitude limit. The median survey redshift is z = 0.3; the survey provides a view of structure in the range 0.1 less than or similar to z less than or similar to 0.6 . A movie displays the large-scale structure in the survey region. We provide a redshift, spectral index D(n)4000, and stellar mass for each galaxy in the survey. We also provide a metallicity for each galaxy in the range 0.2 < z < 0.38 . To demonstrate potential applications of the survey, we examine the behavior of the index D(n)4000 as a function of galaxy luminosity, stellar mass, and redshift. The known evolutionary and stellar mass dependent properties of the galaxy population are cleanly evident in the data. We also show that the mass-metallicity relation previously determined from these data is robust to the analysis approach. C1 [Geller, Margaret J.; Hwang, Ho Seong; Fabricant, Daniel G.; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. [Zahid, Harus Jabran] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. RP Geller, MJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mgeller@cfa.harvard.edu; hhwang@cfa.harvard.edu; dfabricant@cfa.harvard.edu; mkurtz@cfa.harvard.edu; ian@het.brown.edu; jabran@ifa.hawaii.edu OI Geller, Margaret/0000-0002-9146-4876 FU Smithsonian Institution FX We thank the referee for comments that helped us to clarify points in this paper. We thank Perry Berlind and Michael Calkins who masterfully operated the Hectospec on the MMT and Susan Tokarz who efficiently reduced the data. Sean Moran contributed to the construction of the catalogs contained here. We thank Sangwoo Lee for helping us to make the animation using IDL. The Smithsonian Institution supports the research of M.J.G., H.S.H., D.G.F. and M.J.K. NR 65 TC 14 Z9 14 U1 0 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 AUG PY 2014 VL 213 IS 2 AR 35 DI 10.1088/0067-0049/213/2/35 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AP0TM UT WOS:000341777400017 ER PT J AU Bucher, KE Ballantine, DL Lozada-Troche, C Norris, JN AF Bucher, Katina E. Ballantine, David L. Lozada-Troche, Chad Norris, James N. TI Wrangelia gordoniae, a new species of Rhodophyta (Ceramiales, Wrangeliaceae) from the tropical western Atlantic SO BOTANICA MARINA LA English DT Article DE new species; Rhodophyta; western Atlantic; Wrangelia gordoniae; Wrangeliaceae ID RIBOSOMAL-RNA GENE; RDNA SEQUENCE DATA; MARINE RED ALGAE; SP-NOV; PROPOSAL; SEA AB On the basis of comparative morphological and molecular analyses, a new red algal species in the genus Wrangelia (Wrangeliaceae, Ceramiales) is described from the tropical western Atlantic. Distinctive characteristics of the proposed new species, W. gordoniae, include: overall habit; built up pseudoparenchymatous cortex that is composed of 2, and in localized sites up to 3, layers of cortical cells, with the outermost layer incomplete, composed of smaller, irregular-shaped cells; and spermatangial heads with 5-6 (-7) involucres, each consisting of a single elongate cell. Analyses of SSU sequences of specimens of Wrangelia from Puerto Rico further support the presence of four genetically distinct entities. In addition to numerous recent collections, a number of herbarium specimens from different Caribbean locales previously identified as "W. penicillata" are now recognized to be W. gordoniae. The new species is compared morphologically with other Wrangelia species that also have 5 whorl branchlets per segment and a cortex that partially or wholly covers their axes. A key to the tropical western Atlantic species of Wrangelia is provided. C1 [Bucher, Katina E.; Ballantine, David L.; Norris, James N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Ballantine, David L.] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA. [Lozada-Troche, Chad] Univ Puerto Rico, Dept Biol, Cayey, PR 00737 USA. RP Bucher, KE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, NHB166, Washington, DC 20560 USA. EM katinanorris@gmail.com FU NOAA (National Oceanographic and Atmospheric Administration) Coastal Ocean Programs [NA17OP2919, NA06NOS4780190]; NSF [SI-DSG-642041, SI-DSG- 642079] FX JNN thanks Steve M. Blair and Dominic Liberatore (HBOI sub pilot) for the opportunity to collect from the DSV Johnson-sea-Link I operating from the HBOI OR/V Seaward Johnson; our submersible and SCUBA dives during our expeditions to the Bahamas were made possible by support from Smithsonian Marine Station, Fort Pierce (SMSFP), and Harbor Branch Oceanographic Institute (HBOI), Florida Atlantic University. We thank Dr. Hector Ruiz for some of the Puerto Rican collections as well as for the in situ habit photographs and the macro digital images of the female gametophyte and tetrasporophyte, and Barrett Brooks, Diane Littler, Mark Littler, Valerie Paul, Ed Luedke, and Sherry Reed for sharing their collections. The participation of JNN and KEB on the NSF Bahamas expeditions enabled us to make SCUBA collections off the OR/V Columbus Islen (William Fenical, Chief Scientist, Scripps Institution Oceanography). Collections from the Belizean Barrier Reef were facilitated by the Smithsonian Carrie Bow Cay Marine Station-Caribbean Coral Reef Ecosystem program ( K. Ruetzler, Director). We also acknowledge C. Fred Gurgel, Suzanne Fredericq, R. Sims and Chip Clark for their diving and collecting assistance in Belize, and Mark Hay and Suzanne Fredericq for the Haiti collections made from the Smithsonian's R/V Marsys Resolute expeditions in the Caribbean (W.H. Adey, Captain and Chief Scientist). We thank Stanley Yankowski for digital photomicrograph assistance and Alice Tangerini for preparation and assembly of the figures. DLB gratefully acknowledges partial support for the research by NOAA (National Oceanographic and Atmospheric Administration) Coastal Ocean Programs under awards #NA17OP2919 and #NA06NOS4780190 to the University of Puerto Rico, Mayaguez. JNN acknowledges partial support for this study from NSF grants (SI-DSG-642041 and SI-DSG- 642079). This study represents Smithsonian Carrie Bow Cay-CCRE contribution no. 959, Smithsonian Marine Station, Fort Pierce, Florida contribution no. 951, and Ocean Heritage Foundation/Curacao Sea Aquarium/Substation Curacao no. 7. NR 71 TC 1 Z9 1 U1 1 U2 3 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0006-8055 EI 1437-4323 J9 BOT MAR JI Bot. Marina PD AUG PY 2014 VL 57 IS 4 BP 265 EP 280 DI 10.1515/bot-2014-0012 PG 16 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA AO5CD UT WOS:000341358300004 ER PT J AU Wilke, RHT Johnson-Wilke, RL Cotroneo, V McMuldroch, S Reid, PB Schwartz, DA Trolier-McKinstry, S AF Wilke, Rudeger H. T. Johnson-Wilke, Raegan L. Cotroneo, Vincenzo McMuldroch, Stuart Reid, Paul B. Schwartz, Daniel A. Trolier-McKinstry, Susan TI Fabrication of Adjustable Cylindrical Mirror Segments for the SMART-X Telescope SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article ID CHEMICAL SOLUTION DEPOSITION; ULTRATHIN-FILM CAPACITORS; PIEZOELECTRIC MEMS; THIN; PZT AB The adaptive optics system for the SMART-X telescope consists of piezoelectric PbZr0.52Ti0.48O3 (PZT) thin films deposited on the backside of the mirror. To achieve sufficient strain response from the piezoelectric films, the substrates chosen are thin, flexible glass pieces that can be slumped into the desired curvature. Preliminary testing has been performed using flat pieces and parts that were slumped into a cylindrical geometry. Commercially available boro-aluminosilicate glass segments (100 x 100 mm) were slumped along one axis to a radius of curvature of 220 mm. 2-mu m-thick PZT films were deposited via RF magnetron sputtering on flat glass substrates to demonstrate the viability of the processing approach. The deposited PZT showed high yield (>95%) on 1-cm(2) electrodes. The films exhibited relative permittivity values near 1500 and loss tangents below 0.05. In addition, the remanent polarization was 20 mu C/cm(2) with coercive fields near 30 kV/cm. 1-mu m-thick films with comparable electrical parameters were then deposited onto the slumped substrates. To understand the piezoelectric response of the films and characterize the device performance, influence function measurements were performed. The typical cell response using a 4 V (1.3V(c)) drive voltage corresponded to a 0.5 mu m out-of-plane displacement, which relates to an in-plane strain value larger than 150 ppm. Both of these parameters meet benchmark requirements for reaching the targeted 0.5 arcsecond resolution goal of the SMART-X telescope. These results demonstrate a viable route to fabricate highly functional mirror segments for the SMART-X telescope. C1 [Wilke, Rudeger H. T.; Johnson-Wilke, Raegan L.; Trolier-McKinstry, Susan] Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. [Cotroneo, Vincenzo; McMuldroch, Stuart; Reid, Paul B.; Schwartz, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wilke, RHT (reprint author), Penn State Univ, Mat Res Inst, University Pk, PA 16802 USA. EM rhw11@psu.edu OI Trolier-McKinstry, Susan/0000-0002-7267-9281 FU Gordon and Betty Moore Foundation; National Aeronautics and Space Administration (NASA) Astronomy and Physics Research and Analysis (APRA) contract [NNX09AE87G] FX This work was supported by grants from the Gordon and Betty Moore Foundation and from the National Aeronautics and Space Administration (NASA) Astronomy and Physics Research and Analysis (APRA) contract NNX09AE87G. NR 26 TC 1 Z9 1 U1 2 U2 15 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-3010 EI 1525-8955 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD AUG PY 2014 VL 61 IS 8 BP 1386 EP 1392 DI 10.1109/TUFFC.2014.3047 PG 7 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA AO8GJ UT WOS:000341591400017 ER PT J AU Lapinski, W Tschapka, M AF Lapinski, Witold Tschapka, Marco TI Desiccation resistance reflects patterns of microhabitat choice in a Central American assemblage of wandering spiders SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE Ecology; Physiology; Rainforest; Ctenidae; Trechaleidae; Canopy ID EVAPORATIVE WATER-LOSS; SKIN RESISTANCE; INSECTS; ARANEAE; FROGS; CUPIENNIUS; HABITATS; ARBOREAL; CTENIDAE AB The lowland rainforest of northeastern Costa Rica harbours an assemblage of large wandering spider species belonging to three habitat subguilds: (1) semi-aquatic, (2) forest ground dwelling and (3) vegetation dwelling. We hypothesized that desiccation resistance should differ among species preferring different microhabitats and the associated microclimate. Desiccation resistance was assessed by: (1) measuring water loss rates of the spiders under relatively dry experimental conditions, and (2) recording desiccation susceptibility, i.e. the reactions of the spiders to a relatively dry environment. High water loss rates and desiccation susceptibility of the semi-aquatic and forest-ground-dwelling subguilds clearly mirrored the relatively humid microclimate of the understory. Significantly lower water loss rates and desiccation susceptibility of the vegetation-dwelling species reflected the highly variable, often dry and hot conditions of the rainforest canopy and forest edge habitats. Vegetation-dwelling wandering spiders are therefore physiologically better adapted to dry conditions than the semi-aquatic and forest-ground-dwelling species. The results illustrate the significance of physiological characteristics for explaining both species-specific habitat use and, in a larger context, niche partitioning within a community. C1 [Lapinski, Witold] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Lapinski, W (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM Witold.Lapinski@uni-ulm.de; Marco.Tschapka@uni-ulm.de FU University of Ulm; German Academic Exchange Service (DAAD) in Costa Rica [332 4 04 101, 332 4 04 102] FX The German Academic Exchange Service (DAAD) supported the fieldwork of W.L. in Costa Rica [grant nos 332 4 04 101 and 332 4 04 102]; additional funding came from the University of Ulm. NR 43 TC 3 Z9 3 U1 4 U2 20 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 AUG PY 2014 VL 217 IS 15 BP 2789 EP 2795 DI 10.1242/jeb.102533 PG 7 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AO2XA UT WOS:000341189200029 PM 24855682 ER PT J AU Brescia, M Cavuoti, S Longo, G Nocella, A Garofalo, M Manna, F Esposito, F Albano, G Guglielmo, M D'Angelo, G Di Guido, A Djorgovski, SG Donalek, C Mahabal, AA Graham, MJ Fiore, M D'Abrusco, R AF Brescia, Massimo Cavuoti, Stefano Longo, Giuseppe Nocella, Alfonso Garofalo, Mauro Manna, Francesco Esposito, Francesco Albano, Giovanni Guglielmo, Marisa D'Angelo, Giovanni Di Guido, Alessandro Djorgovski, S. George Donalek, Ciro Mahabal, Ashish A. Graham, Matthew J. Fiore, Michelangelo D'Abrusco, Raffaele TI DAMEWARE: A Web Cyberinfrastructure for Astrophysical Data Mining SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GOODS-NORTH FIELD; PHOTOMETRIC REDSHIFTS; GALAXIES; SAMPLE AB Astronomy is undergoing a methodological revolution triggered by an unprecedented wealth of complex and accurate data. The new panchromatic, synoptic sky surveys require advanced tools for discovering patterns and trends hidden behind data which are both complex and of high dimensionality. We present DAMEWARE (DAta Mining & Exploration Web Application REsource): a general purpose, web-based, distributed data mining environment developed for the exploration of large data sets, and finely tuned for astronomical applications. By means of graphical user interfaces, it allows the user to perform classification, regression, or clustering tasks with machine learning methods. Salient features of DAMEWARE include its ability to work on large datasets with minimal human intervention, and to deal with a wide variety of real problems such as the classification of globular clusters in the galaxy NGC1399; the evaluation of photometric redshifts; and, finally, the identification of candidate Active Galactic Nuclei in multiband photometric surveys. In all these applications, DAMEWARE allowed us to achieve better results than those attained with more traditional methods. With the aim of providing potential users with all needed information, in this paper we briefly describe the technological background of DAMEWARE, give a short introduction to some relevant aspects of data mining, followed by a summary of some science cases and, finally, provide a detailed description of a template use case. C1 [Brescia, Massimo; Cavuoti, Stefano] INAF, Astron Observ Capodimonte, Naples, Italy. [Longo, Giuseppe] Univ Naples Federico II, Dept Phys, Naples, Italy. [Nocella, Alfonso; Garofalo, Mauro; Manna, Francesco; Esposito, Francesco; Albano, Giovanni; Guglielmo, Marisa; D'Angelo, Giovanni; Di Guido, Alessandro] Univ Naples Federico II, Dept Comp Sci & Engn, Naples, Italy. [Djorgovski, S. George; Donalek, Ciro; Mahabal, Ashish A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Graham, Matthew J.] CALTECH, Ctr Adv Res Comp, Pasadena, CA 91125 USA. [Fiore, Michelangelo] LAAS CNRS Toulouse, Toulouse, France. [D'Abrusco, Raffaele] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Brescia, M (reprint author), INAF, Astron Observ Capodimonte, Naples, Italy. RI D'Abrusco, Raffaele/L-2767-2016; Cavuoti, Stefano/B-4650-2017; OI D'Abrusco, Raffaele/0000-0003-3073-0605; Cavuoti, Stefano/0000-0002-3787-4196; Brescia, Massimo/0000-0001-9506-5680 FU Italian Ministry of Foreign Affairs; Department of Physics; Polo della Scienza e Della Tecnologia of the University Federico II in Napoli; University Federico II of Naples; PRIN-MIUR; Cosmology with the Euclid space mission; NSF [AST-0834235, IIS-1118041]; NASA [08-AISR08-0085] FX DAMEWARE has been a multiyear project funded by many sponsors. The Italian Ministry of Foreign Affairs through a bilateral Great Relevance Italy-USA project; the European funded VO-Tech (Virtual Observatory Technological Infrastructure) 6-th European FW project; the Department of Physics and the Polo della Scienza e Della Tecnologia of the University Federico II in Napoli. GL, MB and SC acknowledge financial support by the Project F.A.R.O., 3rd call by the University Federico II of Naples. GL wish also to thank the financial support by the PRIN-MIUR 2011, Cosmology with the Euclid space mission. SGD, CD, AAM, and MJG acknowledge a partial support from the NSF grants AST-0834235 and IIS-1118041, and the NASA grant 08-AISR08-0085. NR 56 TC 7 Z9 7 U1 0 U2 5 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 AUG PY 2014 VL 126 IS 942 BP 783 EP 797 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AO3KH UT WOS:000341227600006 ER PT J AU Evangelista, D Cam, S Huynh, T Krivitskiy, I Dudley, R AF Evangelista, Dennis Cam, Sharlene Huynh, Tony Krivitskiy, Igor Dudley, Robert TI Ontogeny of aerial righting and wing flapping in juvenile birds SO BIOLOGY LETTERS LA English DT Article DE aerodynamics; control; development; flight origins; manoeuvrability; wing ID FLIGHT; ORIGINS; DINOSAURS; EVOLUTION; BEHAVIOR AB Mechanisms of aerial righting in juvenile chukar partridge (Alectoris chukar) were studied from hatching to 14 days-post-hatching (dph). Asymmetric movements of the wings were used from 1 to 8 dph to effect progressively more successful righting behaviour via body roll. Following 8 dph, wing motions transitioned to bilaterally symmetric flapping that yielded aerial righting via nose-down pitch, along with substantial increases in vertical force production during descent. Ontogenetically, the use of such wing motions to effect aerial righting precedes both symmetric flapping and a previously documented behaviour in chukar (i.e. wing-assisted incline running) hypothesized to be relevant to incipient flight evolution in birds. These findings highlight the importance of asymmetric wing activation and controlled aerial manoeuvres during bird development and are potentially relevant to understanding the origins of avian flight. C1 [Evangelista, Dennis; Cam, Sharlene; Huynh, Tony; Krivitskiy, Igor; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Evangelista, Dennis] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Evangelista, D (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM devangel77b@gmail.com OI Evangelista, Dennis/0000-0002-6565-8300 FU NSF Integrative Graduate Education and Research Traineeship (IGERT) [DGE-0903711]; Berkeley Sigma Xi chapter; national Sigma Xi FX D.E. was supported by NSF Integrative Graduate Education and Research Traineeship (IGERT) #DGE-0903711 and by grants from the Berkeley Sigma Xi chapter and the national Sigma Xi. NR 17 TC 5 Z9 5 U1 2 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 PY 2014 VL 10 IS 8 AR 20140497 DI 10.1098/rsbl.2014.0497 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA AO4RO UT WOS:000341329100010 ER PT J AU Oberg, KI Fayolle, EC Reiter, JB Cyganowski, C AF Oeberg, Karin I. Fayolle, Edith C. Reiter, John B. Cyganowski, Claudia TI Complex molecule formation around massive young stellar objects SO FARADAY DISCUSSIONS LA English DT Article ID GRAIN-SURFACE-CHEMISTRY; STAR-FORMING REGIONS; HOT CORES; PROTOSTAR IRAS-16293-2422; ORGANIC-MOLECULES; HIGH-RESOLUTION; CHEMICAL-MODEL; W3 IRS5; GAS; SUBMILLIMETER AB Interstellar complex organic molecules were first identified in the hot inner regions of massive young stellar objects (MYSOs), but have more recently been found in many colder sources, indicating that complex molecules can form at a range of temperatures. However, individually these observations provide limited constraints on how complex molecules form, and whether the same formation pathways dominate in cold, warm and hot environments. To address these questions, we use spatially resolved observations from the Submillimeter Array of three MYSOs together with mostly unresolved literature data to explore how molecular ratios depend on environmental parameters, especially temperature. Towards the three MYSOs, we find multiple complex organic emission peaks characterized by different molecular compositions and temperatures. In particular, CH3CCH and CH3CN seem to always trace a lukewarm (T approximate to 60 K) and a hot (T > 100 K) complex chemistry, respectively. These spatial trends are consistent with abundance-temperature correlations of four representative complex organics - CH3CCH, CH3CN, CH3OCH3 and CH3CHO - in a large sample of complex molecule hosts mined from the literature. Together, these results indicate a general chemical evolution with temperature, i.e. that new complex molecule formation pathways are activated as a MYSO heats up. This is qualitatively consistent with model predictions. Furthermore, these results suggest that ratios of complex molecules may be developed into a powerful probe of the evolutionary stage of a MYSO, and may provide information about its formation history. C1 [Oeberg, Karin I.; Fayolle, Edith C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reiter, John B.] Univ Virginia, Charlottesville, VA USA. [Cyganowski, Claudia] Univ St Andrews, St Andrews KY16 9AJ, Fife, Scotland. RP Oberg, KI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 16, Cambridge, MA 02138 USA. EM koberg@cfa.harvard.edu OI Fayolle, Edith/0000-0001-8109-5256 NR 44 TC 4 Z9 4 U1 1 U2 5 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PD AUG 1 PY 2014 VL 168 BP 81 EP 101 DI 10.1039/c3fd00146f PG 21 WC Chemistry, Physical SC Chemistry GA AN7FA UT WOS:000340763200004 PM 25302375 ER PT J AU Fillion, JH Fayolle, EC Michaut, X Doronin, M Philippe, L Rakovsky, J Romanzin, C Champion, N Oberg, KI Linnartz, H Bertin, M AF Fillion, J. -H. Fayolle, E. C. Michaut, X. Doronin, M. Philippe, L. Rakovsky, J. Romanzin, C. Champion, N. Oeberg, K. I. Linnartz, H. Bertin, M. TI Wavelength resolved UV photodesorption and photochemistry of CO2 ice SO FARADAY DISCUSSIONS LA English DT Article ID ELECTRONIC ENERGY-TRANSFER; SOLID CARBON-DIOXIDE; ULTRAVIOLET PHOTODESORPTION; PROTOPLANETARY DISKS; HIGH-RESOLUTION; CROSS-SECTIONS; WATER ICE; SPECTROSCOPY; SURFACE; SPECTRUM AB Over the last four years we have illustrated the potential of a novel wavelength-dependent approach in determining molecular processes at work in the photodesorption of interstellar ice analogs. This method, utilizing the unique beam characteristics of the vacuum UV beamline DESIRS at the French synchrotron facility SOLEIL, has revealed an efficient indirect desorption mechanism that scales with the electronic excitations in molecular solids. This process, known as DIET - desorption induced by electronic transition - occurs efficiently in ices composed of very volatile species (CO, N-2), for which photochemical processes can be neglected. In the present study, we investigate the photodesorption energy dependence of pure and pre-irradiated CO2 ices at 10-40 K and between 7 and 14 eV. The photodesorption from pure CO2 is limited to photon energies above 10.5 eV and is clearly initiated by CO2 excitation and by the contribution of dissociative and recombination channels. The photodesorption from "pre-irradiated" ices is shown to present an efficient additional desorption pathway below 10 eV, dominating the desorption depending on the UV-processing history of the ice film. This effect is identified as an indirect DIET process mediated by photoproduced CO, observed for the first time in the case of less volatile species. The results presented here pinpoint the importance of the interconnection between photodesorption and photochemical processes in interstellar ices driven by UV photons having different energies. C1 [Fillion, J. -H.; Michaut, X.; Doronin, M.; Philippe, L.; Rakovsky, J.; Bertin, M.] Univ Paris 06, CNRS, UMR 7092, LPMAA, F-75252 Paris, France. [Fayolle, E. C.; Linnartz, H.] Leiden Univ, Sackler Lab Astrophys, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Romanzin, C.] Univ Paris 11, CNRS, UMR 8000, LCP, F-91400 Orsay, France. [Champion, N.] CNRS, UMR 8112, LERMA, F-92195 Meudon, France. [Champion, N.] Observ Paris, F-92195 Meudon, France. [Oeberg, K. I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Fillion, JH (reprint author), Univ Paris 06, CNRS, UMR 7092, LPMAA, F-75252 Paris, France. RI Bertin, Mathieu/C-7134-2012; Rakovsky, Jozef/F-5149-2014; OI Bertin, Mathieu/0000-0002-9021-2415; Rakovsky, Jozef/0000-0003-0149-0382; Fayolle, Edith/0000-0001-8109-5256 FU SOLEIL [20120834]; French CNRS national program Physique et Chimie du Milieu Interstellaire; UPMC platform for Astrophysics "ASTROLAB"; Dutch program Nederlandse Onderzoekschool voor Astronomie; Hubert Curien Partnership Van Gogh [25055YK]; NWO through VICI FX We acknowledge SOLEIL for providing of synchrotron radiation under project 20120834, and we thank Gustavo Garcia for assistance on the beamline DESIRS. Financial support from the French CNRS national program Physique et Chimie du Milieu Interstellaire, the UPMC platform for Astrophysics "ASTROLAB", the Dutch program Nederlandse Onderzoekschool voor Astronomie, and the Hubert Curien Partnership Van Gogh (25055YK) is gratefully acknowledged. The Leiden group acknowledges NWO support through a VICI grant. The authors are grateful to Guillermo Munoz-Caro and Gustavo Adolfo Cruz-Diaz for sending VUV absorption cross sections prior to publication. J.-H. F. thanks Dr. M. Gudipati for fruitful discussions. NR 55 TC 11 Z9 11 U1 4 U2 22 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK, MILTON RD, CAMBRIDGE CB4 0WF, CAMBS, ENGLAND SN 1359-6640 EI 1364-5498 J9 FARADAY DISCUSS JI Faraday Discuss. PD AUG 1 PY 2014 VL 168 BP 533 EP 552 DI 10.1039/c3fd00129f PG 20 WC Chemistry, Physical SC Chemistry GA AN7FA UT WOS:000340763200026 PM 25302397 ER PT J AU Hoberg, EP Phillips, AJ AF Hoberg, Eric P. Phillips, Anna J. TI Transfer of the US-National Parasite Collection SO FOLIA PARASITOLOGICA LA English DT Editorial Material C1 [Hoberg, Eric P.] ARS, US Natl Parasite Collect, USDA, Beltsville, MD USA. [Phillips, Anna J.] Smithsonians Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC USA. RP Phillips, AJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM phillipsaj@si.edu NR 4 TC 0 Z9 0 U1 0 U2 0 PU FOLIA PARASITOLOGICA PI CESKE BUDEJOVICE PA BRANISOVSKA 31,, CESKE BUDEJOVICE 370 05, CZECH REPUBLIC SN 0015-5683 EI 1803-6465 J9 FOLIA PARASIT JI Folia Parasitol. PD AUG PY 2014 VL 61 IS 4 BP 370 EP 370 PG 1 WC Parasitology SC Parasitology GA AN4SC UT WOS:000340577800009 PM 25185407 ER PT J AU Lohbeck, M Poorter, L Martinez-Ramos, M Rodriguez-Velazquez, J van Breugel, M Bongers, F AF Lohbeck, Madelon Poorter, Lourens Martinez-Ramos, Miguel Rodriguez-Velazquez, Jorge van Breugel, Michiel Bongers, Frans TI Changing drivers of species dominance during tropical forest succession SO FUNCTIONAL ECOLOGY LA English DT Article DE Chiapas; environmental filtering; functional convergence/divergence; functional traits; kurtosis; light gradient partitioning; Mexico; secondary succession ID PHYLOGENETIC COMMUNITY STRUCTURE; PLANT FUNCTIONAL TRAITS; LEAF LIFE-SPAN; RAIN-FOREST; COMPETITIVE-EXCLUSION; SECONDARY SUCCESSION; RELATIVE IMPORTANCE; COASTAL CALIFORNIA; ASSEMBLY RULES; DIVERSITY AB 1. Deterministic theories predict that local communities assemble from a regional species pool based on niche differences, thus by plant functional adaptations. We tested whether functional traits can also explain patterns in species dominance among the suite of co-occurring species. 2. We predicted that along a gradient of secondary succession, the main driver of species dominance changes from environmental filtering in the relatively harsh (dry and hot) early successional conditions, towards increased competitive interactions and limiting similarity in later successional conditions (when light is limited). 3. We used the Kurtosis (K) (a measure of peakedness) of the functional trait distribution of secondary forest communities in high-diversity tropical rain forest in Chiapas, Mexico. The forests ranged 1-25 years in age, and we used eight functional leaf traits related to a plants' carbon, water and heat balance. We calculated the functional trait distribution based on species dominance, where trait values were weighted by species' relative basal area, as well as based on species presence, all species counting once. 'K-ratio' was subsequently computed by dividing kurtosis based on species dominance by kurtosis based on species presence. If the K-ratio is high, the dominant species are functionally similar and we interpreted this as environmentally driven functional convergence allowing species to become dominant. If the K-ratio is small, dominant species are a functionally dissimilar subset of the species present and we interpreted this as competitively driven functional divergence allowing species to become dominant. 4. We found that in early succession, dominant species represent a functionally narrow subset of species with similar traits, and in late succession, dominant species increasingly represent a wide subset of the species present. This trend was found for traits that reflect photosynthetic performance and light capture, and indicates increased competition for light with succession. No trend was found for traits that indicate defence against herbivory, suggesting no successional changes in herbivore pressure. 5. Synthesis. This is one of the first studies showing that drivers of species dominance change along a gradient of secondary succession. During the early successional time window we evaluated, the importance of environmental filtering as a driving force fades away rapidly, and the importance of niche partitioning for species dominance starts to emerge. C1 [Lohbeck, Madelon; Poorter, Lourens; Bongers, Frans] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Lohbeck, Madelon; Martinez-Ramos, Miguel; Rodriguez-Velazquez, Jorge] Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58190, Michoacan, Mexico. [van Breugel, Michiel] Smithsonian Trop Res Inst, Balboa, Panama. RP Lohbeck, M (reprint author), Wageningen Univ, Forest Ecol & Forest Management Grp, POB 47, NL-6700 AA Wageningen, Netherlands. EM madelon.lohbeck@wur.nl RI Lohbeck, Madelon/M-6390-2014; OI Lohbeck, Madelon/0000-0002-3959-1800; van Breugel, Michiel/0000-0003-2778-7803 FU NSF-LTREB; Wageningen University and Research centre; NWO-WOTRO (Netherlands Organisation for Scientific Research - Science for Global Development) [W85-326]; MABOTRO project SEMARNAT-CONACYT [2002-C01-0597]; MABOTRO project SEP-CONACYT [CB-2005-01-51043]; DiverSus project through Inter-American Institute for Global Change Research (IAI) CRN - US National Science Foundation [GEO-0452325] FX We are indebted to the people of Loma Bonita, Chiapas, for their hospitality and assistance during field work, especially G. Jamangape for species identification. We thank J. Westveer for help with data collection, G. Carreno-Rocabado, M. Jansen, H. Paz, L. Pla for valuable advice and the NeoSelvas network (coordinated by R. Chazdon) for fruitful discussions. We thank Natalia Norden and an anonymous referee for constructive comments that greatly improved the manuscript. Fieldwork was partly supported by NSF-LTREB. ML and FB were supported by a research grant from Wageningen University and Research centre. MvB and FB were supported by NWO-WOTRO (Netherlands Organisation for Scientific Research - Science for Global Development) Grant W85-326. MMR was supported by MABOTRO projects SEMARNAT-CONACYT 2002-C01-0597 and SEP-CONACYT CB-2005-01-51043. LP was partly funded by the DiverSus project through Inter-American Institute for Global Change Research (IAI) CRN 2015, which is supported by the US National Science Foundation (Grant GEO-0452325). NR 62 TC 21 Z9 23 U1 12 U2 94 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD AUG PY 2014 VL 28 IS 4 BP 1052 EP 1058 DI 10.1111/1365-2435.12240 PG 7 WC Ecology SC Environmental Sciences & Ecology GA AN5ZY UT WOS:000340673900028 ER PT J AU Ros, M Ashton, GV Lacerda, MB Carlton, JT Vazquez-Luis, M Guerra-Garcia, JM Ruiz, GM AF Ros, Macarena Ashton, Gail V. Lacerda, Mariana B. Carlton, James T. Vazquez-Luis, Maite Guerra-Garcia, Jose M. Ruiz, Gregory M. TI The Panama Canal and the transoceanic dispersal of marine invertebrates: Evaluation of the introduced amphipod Paracaprella pusilla Mayer, 1890 in the Pacific Ocean SO MARINE ENVIRONMENTAL RESEARCH LA English DT Article DE Invasive species; Ballast water; Salinity; Tolerance; Fouling organisms; First record; Panama Canal; Paracaprella ID CAPRELLIDEA CRUSTACEA; PARANAGUA BAY; SPECIES IDENTIFICATION; MEDITERRANEAN SEA; INVASION DYNAMICS; ATLANTIC; ORGANISMS; TRANSPORT; COAST; WATER AB Although the Panama Canal is one of the major corridors for shipping and potential dispersal of marine invaders in the tropics, little is known about the effect that the Canal has had on the distribution of marine biota. In this study, we (a) document the existence of established populations of the Western Atlantic caprellid amphipod Paracaprella pusilla, Mayer, 1890 for the first time at the Pacific entrance to the Canal, (b) review its distribution in the Pacific Ocean, and (c) evaluate possible mechanisms of introduction. The confirmed distribution of P. pusilla in the Pacific Ocean is limited to Australia, Hawaii, and Panama, despite earlier published reports from Chile and China. Laboratory experiments demonstrated intolerance of P. pusilla to freshwater, causing 100% mortality, and suggest invasion of the Pacific coast of Panama occurred through the Canal via ships' ballast water or by secondary spread via ships (ballast water or hull fouling) from another Pacific region. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Ros, Macarena; Guerra-Garcia, Jose M.] Univ Seville, Fac Biol, Dept Zool, Lab Biol Marina, E-41012 Seville, Spain. [Ashton, Gail V.] Romberg Tiburon Ctr, Smithsonian Environm Res Ctr, Tiburon, CA 94920 USA. [Lacerda, Mariana B.] Univ Fed Parana, Dept Zool, BR-80060000 Curitiba, Parana, Brazil. [Carlton, James T.] Williams Coll Myst Seaport, Maritime Studies Program, Mystic, CT 06355 USA. [Vazquez-Luis, Maite] Inst Espanol Oceanog, Ctr Oceanog Balears, Palma de Mallorca 07015, Spain. [Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Ros, M (reprint author), Univ Seville, Fac Biol, Dept Zool, Lab Biol Marina, Avda Reina Mercedes 6, E-41012 Seville, Spain. EM mros@us.es RI Guerra-Garcia, Jose Manuel /P-1700-2014; OI Guerra-Garcia, Jose Manuel /0000-0001-6050-4997; Ruiz, Gregory/0000-0003-2499-441X FU Ministerio de Educacion de Espana [AP-2009-3380]; Smithsonian Institution FX We express our gratitude to the SERC (Smithsonian Environmental Research Center) staff who were involved with sample collection in Panama, and to K. Larson, M. Repetto and S. Havard for their technical support. We thank all those who kindly provided material for us to study: E. Baeza-Rojano from the Gulf of Mexico, L. Montelli from Australia, and M. Thiel and J.C. Astudillo from Chile. We gratefully thank P. Fofonoff for his support during the stay of the first author at SERC and S. Massunari for her advice and support during the experiments. Three referees provided useful comments that improved the manuscript. This work was funded by a predoctoral grant from the Ministerio de Educacion de Espana (Reference AP-2009-3380), and by the Smithsonian Institution. NR 60 TC 4 Z9 5 U1 5 U2 39 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0141-1136 EI 1879-0291 J9 MAR ENVIRON RES JI Mar. Environ. Res. PD AUG PY 2014 VL 99 BP 204 EP 211 DI 10.1016/j.marenvres.2014.07.001 PG 8 WC Environmental Sciences; Marine & Freshwater Biology; Toxicology SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Toxicology GA AN6JA UT WOS:000340699600023 PM 25060067 ER PT J AU Athanasiadis, A Ballantine, DL AF Athanasiadis, Athanasios Ballantine, David L. TI The genera Melyvonnea gen. nov and Mesophyllum s.s. (Melobesioideae, Corallinales, Rhodophyta) particularly from the central Atlantic Ocean SO NORDIC JOURNAL OF BOTANY LA English DT Article ID FOSLIE COMB-NOV; SOUTH-AFRICA; ALGAE RHODOPHYTA; PACIFIC COAST; NORTH-AMERICA; NEW-ZEALAND; RED ALGAE; SEA; SYNARTHROPHYTON; LEPTOPHYTUM AB We propose the new genus Melyvonnea to accommodate species previously included in Mesophyllum having: a) perithallial protuberances that may branch and dominate over the encrusting base, b) monoecious gametophytes with gametangial conceptacles occasionally developed in superimposition, c) spheroid carposporangial chambers (lacking a central pedestal), and d) filaments lining canals of multiporate roofs composed of 3 to 5 cells with distinctively elongate basal cells. The new genus shares with Mesophyllum the development of a predominantly coaxial hypothallium. Melyvonnea presently accommodates three species in the Central Atlantic, viz. the generitype Melyvonnea canariensis (Foslie) comb. nov. from the Canary Islands, Melyvonnea erubescens (Foslie) comb. nov. (= Mesophyllum incertum; type locality : Bermuda) from the western Atlantic, Melyvonnea aemulans (Foslie & Howe) comb. nov. from Puerto Rico, and one Indo-Pacific species, Melyvonnea madagascariensis (Foslie) comb. nov. We also emend Mesophyllum Lemoine to encompass Northern Hemisphere species that lack the above apomorphies of Melyvonnea and in addition develop a central pedestal in carposporangial conceptacles (via dissolution of the surrounding cells) with gonimoblasts bending down to fill the empty space. Mesophyllum sensu stricto currently includes six species in the northeast Pacific (M. aleuticum, M. conchatum, M. crassiusculum, M. lamellatum, M. megagastri, M. vancouveriense), two species in the western Atlantic (M. mesomorphum and M. syntrophicum), and three species in the northeast Atlantic and the Mediterranean Sea (M. expansum, M. lichenoides, M. philippii). Gametophytic species of each genus show a mainly disjunct distribution being restricted to the tropics-subtropics (Melyvonnea) and the temperate waters of the Northern Hemisphere (Mesophyllum s.s.). This classification is supported by a consensus of studies of all well-known species of Mesophyllum sensu Adey (1970), and is based on a phylogenetic analysis of morphological and anatomical characters in addition to molecular evidence. C1 [Athanasiadis, Athanasios] Univ Gothenburg, SE-40530 Gothenburg, Sweden. [Ballantine, David L.] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA. [Ballantine, David L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Athanasiadis, A (reprint author), Univ Gothenburg, POB 461, SE-40530 Gothenburg, Sweden. EM athanasios.athanasiadis@bioenv.gu.se FU Captain Stenholms Foundation; Royal Society of Arts and Sciences in Goteborg; National Oceanographic and Atmospheric Administration Coastal Ocean Program [NA17OP2919] FX We thank the keepers of the herbaria BM, C, DUKE, FH, L, MICH, MEL (LTB), MSM, NY, PC, TFC, TRH, UC, US, and WELT for information and/or generous loans of collections, including type specimens. Athanasios Athanasiadis acknowledges financial support for field and laboratory work through grants from the Captain Stenholms Foundation and The Royal Society of Arts and Sciences in Goteborg. David L. Ballantine acknowledges funding by the National Oceanographic and Atmospheric Administration Coastal Ocean Program under award no. NA17OP2919 to the University of Puerto Rico-Mayaguez. We also thank several reviewers for their helpful comments. NR 139 TC 8 Z9 8 U1 2 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0107-055X EI 1756-1051 J9 NORD J BOT JI Nord. J. Bot. PD AUG PY 2014 VL 32 IS 4 BP 385 EP 436 DI 10.1111/njb.00265 PG 52 WC Plant Sciences SC Plant Sciences GA AN4RD UT WOS:000340574500001 ER PT J AU Lin, F Comita, LS Wang, XG Bai, XJ Yuan, ZQ Xing, DL Hao, ZQ AF Lin, Fei Comita, Liza S. Wang, Xugao Bai, Xuejiao Yuan, Zuoqiang Xing, Dingliang Hao, Zhanqing TI The contribution of understory light availability and biotic neighborhood to seedling survival in secondary versus old-growth temperate forest SO PLANT ECOLOGY LA English DT Article DE Canopy openness; Density dependence; Shade tolerance; Species coexistence; Temperate forests ID TROPICAL TREE SEEDLINGS; LOWLAND RAIN-FOREST; POPLAR-BIRCH FOREST; SHADE TOLERANCE; DENSITY-DEPENDENCE; SPECIES COEXISTENCE; CANOPY GAPS; SPATIAL HETEROGENEITY; COMMUNITY STRUCTURE; LOCAL NEIGHBORHOOD AB Seedling survival plays an important role in the maintenance of species diversity and forest dynamics. Although substantial gains have been made in understanding the factors driving patterns of seedling survival in forests, few studies have considered the simultaneous contribution of understory light availability and the local biotic neighborhood to seedling survival in temperate forests at different successional stages. Here, we used generalized linear mixed models to assess the relative importance of understory light availability and biotic neighborhood variables on seedling survival in secondary and old-growth temperate forest in north eastern China at two levels (community and guild). At the community level, biotic neighborhood effects on seedling survival were more important than understory light availability in both forests. In both the old-growth and secondary forests, conspecific basal area had a negative effect on seedling survival, consistent with negative conspecific density dependence. At guild levels, the relative importance of light and biotic neighborhood on seedling survival showed considerable variation among guilds in both forests. Available understory light tended to have positive effects on seedling survival for shrub and light-demanding species in the old-growth forest, but negative effects on survival of shade-tolerant seedlings in the secondary forest. For tree species and shade-tolerant species, the best fit models included neighborhood variables, but that was not the case for shrubs, light-demanding, or mid shade-tolerant species. Overall, our results demonstrate that the relative importance of understory light availability and biotic factors on seedling survival vary with species life-history strategy and forest successional stage. C1 [Lin, Fei; Wang, Xugao; Yuan, Zuoqiang; Xing, Dingliang; Hao, Zhanqing] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China. [Lin, Fei; Xing, Dingliang] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Comita, Liza S.] Ohio State Univ, Dept Evolut Ecol & Organismal Biol, Columbus, OH 43210 USA. [Comita, Liza S.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Bai, Xuejiao] Shenyang Agr Univ, Coll Forestry, Shenyang 110866, Peoples R China. RP Hao, ZQ (reprint author), Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China. EM hzq@iae.ac.cn RI wang, xugao/B-1111-2015 OI wang, xugao/0000-0003-1207-8852 FU National Natural Science and Foundation of China [41101188, 31370444, 41301057]; State Key Laboratory of Forest and Soil Ecology [LFSE2013-11] FX This work was supported by the National Natural Science and Foundation of China (41101188, 31370444, and 41301057) and State Key Laboratory of Forest and Soil Ecology (LFSE2013-11). We thank Dr. Jiaojun Zhu for his valuable suggestions for methods. We thank Dr. Simon Queenborough for assistance with the figures. We also thank Liwei Wang, Ji Ye, Buhang Li, Zhaochen Zhang, Xu Kuang, Houjuan Song, Guodong Liu, Baizhang Song and Zhenshan Li for their assistance with the data collection. NR 83 TC 5 Z9 8 U1 8 U2 81 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 EI 1573-5052 J9 PLANT ECOL JI Plant Ecol. PD AUG PY 2014 VL 215 IS 8 BP 795 EP 807 DI 10.1007/s11258-014-0332-0 PG 13 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA AO1RP UT WOS:000341091600001 ER PT J AU Funk, VA Sancho, G Roque, N Kelloff, CL Ventosa-Rodriguez, I Diazgranados, M Bonifacino, JM Chan, R AF Funk, Vicki A. Sancho, Gisela Roque, Nadia Kelloff, Carol L. Ventosa-Rodriguez, Iralys Diazgranados, Mauricio Bonifacino, J. Mauricio Chan, Raymund TI A phylogeny of the Gochnatieae: Understanding a critically placed tribe in the Compositae SO TAXON LA English DT Article DE Anastraphia; Asteraceae; biogeography; character evolution; Gochnatia; Gochnatieae; molecular phylogenetics; Moquiniastrum; Neotropics; Pentaphorus; Richterago; systematics; taxon age ID SANTA-CRUZ PROVINCE; MUTISIEAE ASTERACEAE; POLLEN MORPHOLOGY; CHLOROPLAST DNA; SEQUENCES; RICHTERAGO; MATK; CICHORIOIDEAE; AMPLIFICATION; BIOGEOGRAPHY AB Subfamily Gochnatioideae is the sister group of similar to 96% of the species in Compositae (Asteraceae). It is of particular interest not only because of its position in the phylogeny, but also because, in recent molecular studies, the node it occupies is not strongly supported making difficult any inferences on the direction of character evolution in the family. The recognition of tribe Gochnatieae was one of the results of a comprehensive molecular analysis of the family that showed the traditional circumscription of the Mutisieae to be non-monophyletic. The four genera of Gochnatieae (Cnicothamnus, Cyclolepis, Gochnatia, Richterago) were defined by the presence of apiculate anther appendages and dorsally smooth style branches. Gochnatia, which contained about 70 species, was the largest and most complex genus and in the last decade some of its sections have been moved (or returned) to the rank of genus. This study includes a large selection of potential outgroups and over 60% of all species in the tribe, including all the genera and all but one of the sections of Gochnatia, to examine evolutionary relationships among the taxa. Both cpDNA and nrDNA were used in a phylogenetic analysis using parsimony, likelihood, and Bayesian approaches. The results suggest a non-monophyletic Gochnatia that is here resolved by the recognition of segregate genera. Morphological characters support these new genera and allow the adoption of a new classification for the Gochnatieae. A biogeographic analysis shows a possible southern South American/Andean origin followed by movement in three directions: into the Central Andes, into central and northern Brazil, and into Mexico and the Caribbean. The dating analysis gives an age of the split of the core Gochnatieae from the Wunderlichieae-Cyclolepis clade, and hence the age of the tribe, of 36-45 Ma and an age of 23-25 Ma for the first split within the core Gochnatieae (Andean vs. Brazil-Mexico-Caribbean). Cnicothamnus remains in Gochnatieae but Cyclolepis is designated incertae sedis. C1 [Funk, Vicki A.; Kelloff, Carol L.; Diazgranados, Mauricio; Chan, Raymund] Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, Washington, DC 20560 USA. [Sancho, Gisela] Museo La Plata, La Plata, BA, Argentina. [Roque, Nadia] Univ Fed Bahia, Inst Biol, BR-40170110 Salvador, BA, Brazil. [Ventosa-Rodriguez, Iralys] Inst Ecol & Sistemat, Havana, Cuba. [Bonifacino, J. Mauricio] Univ Republica, Fac Agron, Lab Bot, Montevideo, Uruguay. RP Funk, VA (reprint author), Smithsonian Inst NMNH, US Natl Herbarium, Dept Bot, MRC 166, Washington, DC 20560 USA. EM funkv@si.edu FU office of the Associate Director for Science, Department of Botany; Laboratory of Analytical Biology, National Museum of Natural History, Smithsonian Institution; ANPCyT (Agencia Nacional de Promocion Cientifica y Tecnologica); CONICET (Comision Nacional de Investigaciones Cientificas y Tecnicas); CNPq/PQ, REFLORA; CNPq/PQ, PRONEM FX The authors thank Gabriel Johnson (US) for his help with designing the alternative Cuban matK primer and the fungal blocker primer idea and reference. Also, thanks to Thomas F. Patterson (TEX) who made several trips to obtain vouchers, leaf material preserved on silica, and photos of Gochnatia hypoleuca in southern Texas; Tom Wendt (TEX) for his help with the voucher table; and Ken Wurdack (US) for his help with editing the Materials and Methods. We thank the following individuals for supplying leaf samples: Walter Judd (FLAS), Pedro Acevedo-R. (US), Charles Zartman (INPA), Susana Freire (SI), and Jun Wen (US). We thank G.A. Parada (MO) and TROPICOS (http://www.tropicos.org/Name/2706326) for permission to use the photograph of Gochnatia curvifolia and M. Mercadante (Brazil) for permission to use his photograph of Wunderlichia. Funding for this research was supplied by several agencies and institutions: the office of the Associate Director for Science, Department of Botany, and the Laboratory of Analytical Biology, National Museum of Natural History, Smithsonian Institution (to V.A.F.); ANPCyT (Agencia Nacional de Promocion Cientifica y Tecnologica) and CONICET (Comision Nacional de Investigaciones Cientificas y Tecnicas) to G.S.; and CNPq/PQ, REFLORA and PRONEM (to N.R.). Two reviewers and the Editors (Editor-in-Chief, Managing Editor, Production Editor) provided helpful comments and we appreciate their assistance. NR 83 TC 4 Z9 5 U1 0 U2 15 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 AUG PY 2014 VL 63 IS 4 BP 859 EP 882 PG 24 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AO0EU UT WOS:000340982700011 ER PT J AU Cleef, AM Diazgranados, M Funk, VA AF Cleef, Antoine M. Diazgranados, Mauricio Funk, Vicki A. TI SANTIAGO DIAZ PIEDRAHITA (1944-2014), COLOMBIAN SYNANTHEROLOGIST AND HISTORIAN SO TAXON LA English DT Biographical-Item C1 [Cleef, Antoine M.] Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, NL-1098 XH Amsterdam, Netherlands. [Diazgranados, Mauricio; Funk, Vicki A.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Diazgranados, Mauricio] Jardin Bot Jose Celestino Mutis, Bogota 111071, Colombia. RP Cleef, AM (reprint author), Univ Amsterdam, Inst Biodivers & Ecosyst Dynam, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. NR 1 TC 0 Z9 0 U1 0 U2 0 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD AUG PY 2014 VL 63 IS 4 BP 957 EP 958 PG 2 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AO0EU UT WOS:000340982700039 ER PT J AU Novotny, V Miller, SE AF Novotny, Vojtech Miller, Scott E. TI Mapping and understanding the diversity of insects in the tropics: past achievements and future directions SO AUSTRAL ENTOMOLOGY LA English DT Article DE alpha diversity; beta diversity; DNA barcoding; food web; latitudinal gradient; trophic interaction ID GLOBAL SPECIES RICHNESS; LOWLAND RAIN-FOREST; HOST-SPECIFICITY; HERBIVOROUS INSECTS; BETA-DIVERSITY; FOOD WEBS; HABITAT SPECIALIZATION; PARASITOID COMMUNITY; PLANT DIVERSITY; LARGE-SCALE AB We still do not know how many insect species there are in tropical forests. The rate of species description peaked a century ago. Unfortunately, taxonomy ceased to be fashionable before it had completed cataloguing insect diversity. Molecular information combined with web-based data dissemination promises to shorten the 20 years it takes on average for insect specimens to be described as new species. Our inability to enumerate tropical species has made estimates of their diversity popular. Plant-based estimates, multiplying the number of plant species by the number of insect species effectively specialized to them, have been used for the past 150 years for global insect diversity estimates and recently also for the first local rainforest diversity estimate of arthropods, at 25 000 species. Why are there so many insect species in tropical forests? Insect diversity may be driven by latitudinal trends in vegetation. The near impossibility of conducting a complete census of complex plant-insect food webs in tropical forests should focus our attention upon the most common species and interactions. Recent studies of trees in Amazonia and herbivores in New Guinea suggest that such reduced food webs may be surprisingly simple and, thus, amenable to study, while still including more than 50% of all plant and insect individuals and their interactions. A pan-tropical network of plots, modelled on the existing network of forest dynamics plots, and potentially utilizing the existing, but rather poorly used, network of canopy cranes, could provide spatially resolved data on plant-insect food webs. The study of food web dynamics requires experimental manipulation, which can range from exclusion or addition of single species to ecosystem-wide manipulation of species composition and habitat fragmentation. Recent progress in molecular taxonomy, proliferation of community phylogenies, improved food web census techniques and an increasing focus on experiments promise an exciting time for tropical entomology. C1 [Novotny, Vojtech] Univ South Bohemia, Acad Sci Czech Republ, Fac Sci, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech] New Guinea Binatang Res Ctr, Madang 604, Papua N Guinea. [Miller, Scott E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Novotny, V (reprint author), Univ South Bohemia, Acad Sci Czech Republ, Fac Sci, Ctr Biol, Ceske Budejovice 37005, Czech Republic. EM novotny@entu.cas.cz RI Novotny, Vojtech/G-9434-2014; OI Novotny, Vojtech/0000-0001-7918-8023; Miller, Scott/0000-0002-4138-1378 FU Czech Science Foundation [13-10486S]; Czech Ministry of Education; EU Funds [CZ.1.07/2.3.00/20.0064]; US National Science Foundation [DEB 0515678]; Darwin Initiative for the Survival of Species (UK); Christensen Fund FX This study was supported by Czech Science Foundation (13-10486S), Czech Ministry of Education and EU Funds (CZ.1.07/2.3.00/20.0064), US National Science Foundation (DEB 0515678), Darwin Initiative for the Survival of Species (UK) and the Christensen Fund. We thank Tom Fayle, Yves Basset, Simon Segar and Jan Hrcek for comments on the manuscript as well as to many other colleagues who have contributed to our ideas over the years. NR 105 TC 13 Z9 13 U1 9 U2 85 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2052-1758 EI 2052-174X J9 AUSTRAL ENTOMOL JI Austral Entomol. PD AUG PY 2014 VL 53 IS 3 BP 259 EP 267 DI 10.1111/aen.12111 PG 9 WC Entomology SC Entomology GA AN3PU UT WOS:000340501300003 ER PT J AU Gutierrez, EE Boria, RA Anderson, RP AF Gutierrez, Eliecer E. Boria, Robert A. Anderson, Robert P. TI Can biotic interactions cause allopatry? Niche models, competition, and distributions of South American mouse opossums SO ECOGRAPHY LA English DT Article ID SPECIES GEOGRAPHIC DISTRIBUTIONS; PLANT-POLLINATOR INTERACTIONS; CLIMATE-CHANGE; LIMITING SIMILARITY; SAMPLING BIAS; ISLAND BIOGEOGRAPHY; MUTUALISMS MATTER; BIODIVERSITY DATA; RANGE LIMITS; POCKET MICE AB Based on our own empirical data and a literature review, we explore the possibility that biotic interactions, specifically competition, might be responsible for creating, and/or maintaining, geographic isolation. Ecological niche modeling was first used to test whether the distributions of 2 species of Neotropical marsupials (Marmosa robinsoni and M. xerophila) fit the predicted geographic pattern of competitive exclusion: one species predominates in areas environmentally suitable for both species along real contact zones. Secondly, we examined the connectivity among populations of each species, interpreted in the light of the niche models. The results show predominance of M. xerophila along its contact zone with M. robinsoni in the Peninsula de Paraguana in northwestern Venezuela. There, M. robinsoni has an extremely restricted distribution despite climatic conditions suitable for both species across the peninsula and its isthmus. The latter two results suggest that M. xerophila may be responsible for the geographic isolation of the peninsular populations of M. robinsoni with respect to other populations of the latter species in northwestern Venezuela. These results may represent an example of allopatry caused, or at least maintained, by competition. Our results and a review of numerous studies in which biotic interactions restrict species distributions (including at the continental scale) support a previously overlooked phenomenon: biotic interactions can isolate populations of a species. We propose 2 general mechanisms, intrusion and contraction, to classify allopatric conditions caused by various classes of biotic interactions. We present a necessary modification of the concept of ecological vicariance to include biotic interactions as possible vicariant agents regardless of whether genetic differentiation occurs or not. C1 [Gutierrez, Eliecer E.; Boria, Robert A.; Anderson, Robert P.] CUNY City Coll, Dept Biol, New York, NY 10031 USA. [Gutierrez, Eliecer E.; Anderson, Robert P.] CUNY, Grad Ctr, New York, NY 10016 USA. [Gutierrez, Eliecer E.] Smithsonian Inst, Div Mammals, Natl Museum Nat Hist, MRC 108, Washington, DC 20013 USA. [Gutierrez, Eliecer E.] Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [Anderson, Robert P.] Amer Museum Nat Hist, Div Vertebrate Zool Mammal, New York, NY 10024 USA. RP Gutierrez, EE (reprint author), CUNY City Coll, Dept Biol, 526 Marshak Sci Bldg,160 Convent Ave, New York, NY 10031 USA. EM GutierrezE@si.edu RI Gutierrez, Eliecer/D-5703-2014 OI Gutierrez, Eliecer/0000-0001-6790-8185 FU American Museum of Natural History (Theodore Roosevelt Memorial Fund); City College of City Univ. of New York (Graduate Student Award); American Society of Mammalogists; National Science Foundation [DEB-0717357, DEB-1119915, DEB-743062, DEB-743039]; Graduate Center of the City Univ. of New York; Luis Stokes Alliance for Minority Participation; City College Academy for Professional Preparation FX We thank the curators and support staffs of institutions that allowed access to voucher material, especially Nancy Simmons, Robert Voss, Patricia Brunauer, and Eileen Westwig (AMNH); Pascual Soriano (CVULA); Francisco Bisbal-E. and Javier Sanchez-H. (EBRG); Carmen Ferreira, Sandra Giner, and Mercedes Salazar (MBUCV); Belkis Rivas (MHNLS); and Michael Carleton, Alfred Gardner, Linda Gordon, and Kristofer Helgen (USNM). Amy Berkov, Corentin Bohl, Sharon Jansa, Jason Munshi-South, Aleksandar Radosavljevic, Ali Raza, Mariano Soley-Guardia, and Robert Voss read one or more versions of this manuscript and made helpful comments. Similarly, Sara Varela, and our subject matter editor, Douglas Kelt, who remained anonymous during the review process, provided comments that improved the quality of the manuscript. Jesus Molinari and Pascual Soriano provided habitat photographs. Franziska Bauer provided critically relevant literature and assisted with Fig. 3. This work was funded, in part, by awards provided to EEG from the American Museum of Natural History (Theodore Roosevelt Memorial Fund), the City College of City Univ. of New York (Graduate Student Award), and the American Society of Mammalogists (Grants in Aid of Research), as well as by National Science Foundation grants DEB-0717357 and DEB-1119915 (both to RPA), DEB-743062 (to Sharon Jansa), and DEB-743039 (to Robert Voss). Additional support to EEG was provided by the Graduate Center of the City Univ. of New York (Science Fellowship, University Fellowship, Tuition Fellowship, and Sue Rosenberg Zalk Student Travel and Research Fund), and the Smithsonian Inst. (Buck Postdoctoral Fellowship Program and the Division of Mammals). Support from the Luis Stokes Alliance for Minority Participation and the City College Academy for Professional Preparation was provided to RAB (Bridge to Doctorate Fellowship). NR 127 TC 18 Z9 18 U1 4 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0906-7590 EI 1600-0587 J9 ECOGRAPHY JI Ecography PD AUG PY 2014 VL 37 IS 8 BP 741 EP 753 DI 10.1111/ecog.00620 PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AN2HQ UT WOS:000340405600004 ER PT J AU Arias, CF Salazar, C Rosales, C Kronforst, MR Linares, M Bermingham, E Mcmillan, WO AF Arias, Carlos F. Salazar, Camilo Rosales, Claudia Kronforst, Marcus R. Linares, Mauricio Bermingham, Eldredge Mcmillan, W. Owen TI Phylogeography of Heliconius cydno and its closest relatives: disentangling their origin and diversification SO MOLECULAR ECOLOGY LA English DT Article DE adaptive radiation; amplified fragment length polymorphisms; gene flow; genetic drift; Heliconius cydno; mtDNA; phylogeography; Pliocene-Pleistocene boundary ID MITOCHONDRIAL-DNA SEQUENCES; MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; GENE FLOW; LEPIDOPTERA-NYMPHALIDAE; BUTTERFLIES LEPIDOPTERA; EASTERN CORDILLERA; SHIFTING BALANCE; DIVERGENCE TIMES; SPECIES BOUNDARY AB The origins of the extraordinary diversity within the Neotropics have long fascinated biologists and naturalists. Yet, the underlying factors that have given rise to this diversity remain controversial. To test the relative importance of Quaternary climatic change and Neogene tectonic and paleogeographic reorganizations in the generation of biodiversity, we examine intraspecific variation across the Heliconius cydno radiation and compare this variation to that within the closely related Heliconius melpomene and Heliconius timareta radiations. Our data, which consist of both mtDNA and genome-scan data from nearly 2250 amplified fragment length polymorphism (AFLP) loci, reveal a complex history of differentiation and admixture at different geographic scales. Both mtDNA and AFLP phylogenies suggest that H.timareta and H.cydno are probably geographic extremes of the same radiation that probably diverged from H.melpomene prior to the Pliocene-Pleistocene boundary, consistent with hypotheses of diversification that rely on geological events in the Pliocene. The mtDNA suggests that this radiation originated in Central America or the northwestern region of South America, with a subsequent colonization of the eastern and western slopes of the Andes. Our genome-scan data indicate significant admixture among sympatric H.cydno/H.timareta and H.melpomene populations across the extensive geographic ranges of the two radiations. Within H.cydno, both mtDNA and AFLP data indicate significant population structure at local scales, with strong genetic differences even among adjacent H.cydno colour pattern races. These genetic patterns highlight the importance of past geoclimatic events, intraspecific gene flow, and local population differentiation in the origin and establishment of new adaptive forms. C1 [Arias, Carlos F.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Arias, Carlos F.; Salazar, Camilo; Rosales, Claudia; Bermingham, Eldredge; Mcmillan, W. Owen] Smithsonian Trop Res Inst, Panama City, Panama. [Salazar, Camilo; Linares, Mauricio] Univ Rosario, Fac Nat Sci & Math, Biol Program, Bogota 111221, Colombia. [Kronforst, Marcus R.] Univ Chicago, Dept Ecol & Evolut, Chicago, IL 60637 USA. [Bermingham, Eldredge] Patricia & Phillip Frost Museum Sci, Miami, FL USA. RP Arias, CF (reprint author), McGill Univ, Dept Biol, 1205 Ave Dr Penfield, Montreal, PQ H3A 1B1, Canada. EM solracarias@gmail.com RI Salazar, camilo/A-1647-2010; Arias, Carlos/G-2881-2016; Linares, Mauricio/I-3509-2016 OI Salazar, camilo/0000-0001-9217-6588; Arias, Carlos/0000-0001-5925-0985; Linares, Mauricio/0000-0002-1021-0226 FU Smithsonian Tropical Research Institute (STRI); NSF [DEB- 640279, DEB-1316 037]; IOS [1052541]; Colfuturo; Levinson Family; Max Binz Family; NEO-STRI; McGill University; Universidad del Rosario; Fondo FIUR from Universidad del Rosario FX We thank C. Jiggins and members of the McMillan and Bermingham Laboratory for useful comments on early versions of the manuscript. We are grateful to R. Gillespie and three anonymous reviewers for valuable comments on the manuscript. We acknowledge the Smithsonian Tropical Research Institute (STRI), where the laboratory work was carried out and funded. This project was also funded by NSF grant (DEB- 640279) and IOS (1052541) to WOM. C. F. Arias was supported by fellowships from Colfuturo, the Levinson Family, Max Binz Family, NEO-STRI and McGill University. C. Salazar received support from Universidad del Rosario. M. Linares was funded by Fondo FIUR from Universidad del Rosario. M. Kronforst was funded by NSF grant (DEB-1316 037). For the genetic access permit number RGE0027-LAM 3483, we thank the Ministerio de Ambiente, Vivienda y Desarrollo Territorial (Colombia). NR 99 TC 3 Z9 3 U1 3 U2 59 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD AUG PY 2014 VL 23 IS 16 BP 4137 EP 4152 DI 10.1111/mec.12844 PG 16 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA AN2MO UT WOS:000340419800016 PM 24962067 ER PT J AU Pennell, MW Eastman, JM Slater, GJ Brown, JW Uyeda, JC FitzJohn, RG Alfaro, ME Harmon, LJ AF Pennell, Matthew W. Eastman, Jonathan M. Slater, Graham J. Brown, Joseph W. Uyeda, Josef C. FitzJohn, Richard G. Alfaro, Michael E. Harmon, Luke J. TI geiger v2.0: an expanded suite of methods for fitting macroevolutionary models to phylogenetic trees SO BIOINFORMATICS LA English DT Article ID TRAIT EVOLUTION; TIME; COMPUTATION; RADIATIONS; CHARACTERS; DIVERSITY AB Phylogenetic comparative methods are essential for addressing evolutionary hypotheses with interspecific data. The scale and scope of such data have increased dramatically in the past few years. Many existing approaches are either computationally infeasible or inappropriate for data of this size. To address both of these problems, we present geiger v2.0, a complete overhaul of the popular R package geiger. We have reimplemented existing methods with more efficient algorithms and have developed several new approaches for accomodating heterogeneous models and data types. C1 [Pennell, Matthew W.; Eastman, Jonathan M.; Brown, Joseph W.; Uyeda, Josef C.; Harmon, Luke J.] Univ Idaho, Dept Biol Sci, Moscow, ID 83844 USA. [Pennell, Matthew W.; Eastman, Jonathan M.; Brown, Joseph W.; Uyeda, Josef C.; Harmon, Luke J.] Univ Idaho, Inst Bioinformat & Evolutionary Studies, Moscow, ID 83844 USA. [Slater, Graham J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [FitzJohn, Richard G.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [FitzJohn, Richard G.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Alfaro, Michael E.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. RP Pennell, MW (reprint author), Univ Idaho, Dept Biol Sci, Moscow, ID 83844 USA. RI Brown, Joseph/A-7713-2009 OI Brown, Joseph/0000-0002-3835-8062 FU Bioinformatics and Computational Biology Graduate Fellowship from the University of Idaho; National Science and Engineering Research Council PGS-D Fellowship; National Science Foundation [DEB 0919499, 1208912, 0918748] FX M.W.P. was supported by a Bioinformatics and Computational Biology Graduate Fellowship from the University of Idaho and a National Science and Engineering Research Council PGS-D Fellowship. This work was also supported by the National Science Foundation (DEB 0919499, 1208912 and 0918748). NR 19 TC 35 Z9 35 U1 4 U2 21 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 AUG 1 PY 2014 VL 30 IS 15 BP 2216 EP 2218 DI 10.1093/bioinformatics/btu181 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 AM7LQ UT WOS:000340049100021 PM 24728855 ER PT J AU Becker, MH Richards-Zawacki, CL Gratwicke, B Belden, LK AF Becker, Matthew H. Richards-Zawacki, Corinne L. Gratwicke, Brian Belden, Lisa K. TI The effect of captivity on the cutaneous bacterial community of the critically endangered Panamanian golden frog (Atelopus zeteki) SO BIOLOGICAL CONSERVATION LA English DT Article DE Amphibians; Captive management; Batrachochytrium dendrobatidis; Probiotic; Microbiome; Symbiosis ID PATHOGEN BATRACHOCHYTRIUM-DENDROBATIDIS; CAPERCAILLIE TETRAO-UROGALLUS; GUT MICROBIOTA; POPULATION DECLINES; HIGH-THROUGHPUT; HUMAN-SKIN; WILD; DIVERSITY; CONSERVATION; AMPHIBIANS AB For many threatened vertebrates, captivity may be the only option for species survival. Maintaining species in captivity prior to reintroduction presents many challenges, including the need to preserve genetic diversity and mitigation of disease risks. Recent studies suggest that captivity can alter the suite of symbiotic microbes that play important roles in host health. The Panamanian golden frog (Atelopus zeteki) has not been seen in its native habitat in Panama since 2009. Along with habitat loss and illegal collecting, the lethal disease chytridiomycosis, caused by the fungal pathogen Batrachochytrium dendrobatidis (Bd), is responsible for the severe decline of this species. Prior to the spread of Bd into golden frog habitat, conservation organizations collected golden frogs and placed them in captive survival assurance colonies. The skin of amphibians is host to a diverse resident bacterial community, which acts as a defense mechanism in some amphibians to inhibit pathogens. We characterized the cutaneous bacterial community from wild and F1 captive golden frogs originating from the same population with Illumina sequencing to assess how long-term captivity has affected this community. We found that species richness, phylogenetic diversity, and community structure of the skin microbiota was significantly different between wild and captive golden frogs. However, after approximately eight years of living in captivity, the offspring of the original captive golden frogs still shared 70% of their microbial community with wild frogs. These results demonstrate that host-associated microbial communities can be significantly altered by captive management, but most of the community composition can be preserved. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Becker, Matthew H.; Belden, Lisa K.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. [Richards-Zawacki, Corinne L.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Gratwicke, Brian] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. RP Becker, MH (reprint author), Virginia Tech, Dept Biol Sci, 2119 Derring Hall, Blacksburg, VA 24061 USA. EM beckermh@vt.edu; cori@tulane.edu; gratwickeb@si.edu; belden@vt.edu FU National Science Foundation [DEB-1136640, DEB-0608147]; Helen O. Brower Foundation; University of Michigan's Rackham Graduate School; University of Michigan Museum of Zoology; Society for the Study of Amphibians and Reptiles FX We would like to thank J. Becker, R. Harris, and J. Walke for insightful comments and review of the manuscript. This research was funded by the National Science Foundation (DEB-1136640 to L.K.B. and DEB-0608147 to C.L.R.-Z.), the Helen O. Brower Foundation (C.L.R.-Z.), the University of Michigan's Rackham Graduate School (C.L.R.-Z.), the University of Michigan Museum of Zoology (C.L.R.-Z.), and the Society for the Study of Amphibians and Reptiles (C.L.R.-Z.). Permission to study A. zeteki, as well as to collect, export, and import swab samples, was provided by the Panamanian environmental authority (ANAM) and the United States Fish and Wildlife Service. This study's methods were also approved by the Smithsonian National Zoological Park's and the University of Michigan's Animal Care and Use Committees. The captive population of A. zeteki in the United States is owned by the Maryland Zoo in Baltimore and is managed by the American Zoo and Aquarium Association's Panamanian golden frog species survival plan. We are grateful for their support for this investigation and for access to animals. NR 68 TC 17 Z9 17 U1 13 U2 91 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 2014 VL 176 BP 199 EP 206 DI 10.1016/j.biocon.2014.05.029 PG 8 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA AM9TI UT WOS:000340223500022 ER PT J AU Rick, TC Sillett, TS Ghalambor, CK Hofman, CA Ralls, K Anderson, RS Boser, CL Braje, TJ Cayan, DR Chesser, RT Collins, PW Erlandson, JM Faulkner, KR Fleischer, R Funk, WC Galipeau, R Huston, A King, J Laughrin, L Maldonado, J McEachern, K Muhs, DR Newsome, SD Reeder-Myers, L Still, C Morrison, SA AF Rick, Torben C. Sillett, T. Scott Ghalambor, Cameron K. Hofman, Courtney A. Ralls, Katherine Anderson, R. Scott Boser, Christina L. Braje, Todd J. Cayan, Daniel R. Chesser, R. Terry Collins, Paul W. Erlandson, Jon M. Faulkner, Kate R. Fleischer, Robert Funk, W. Chris Galipeau, Russell Huston, Ann King, Julie Laughrin, Lyndal Maldonado, Jesus McEachern, Kathryn Muhs, Daniel R. Newsome, Seth D. Reeder-Myers, Leslie Still, Christopher Morrison, Scott A. TI Ecological Change on California's Channel Islands from the Pleistocene to the Anthropocene SO BIOSCIENCE LA English DT Article DE conservation; historical ecology; novel ecosystems; restoration ID SANTA-CRUZ ISLAND; CLIMATE-CHANGE SCENARIOS; SEA-LEVEL RISE; ENVIRONMENTAL-CHANGE; SOUTHERN CALIFORNIA; COASTAL CALIFORNIA; ROSA ISLAND; CONSERVATION; ARCHAEOLOGY; ECOSYSTEMS AB Historical ecology is becoming an important focus in conservation biology and offers a promising tool to help guide ecosystem management. Here, we integrate data from multiple disciplines to illuminate the past, present, and future of biodiversity on California's Channel Islands, an archipelago that has undergone a wide range of land-use and ecological changes. Our analysis spans approximately 20,000 years, from before human occupation and through Native American hunter-gatherers, commercial ranchers and fishers, the US military, and other land managers. We demonstrate how long-term, interdisciplinary research provides insight into conservation decisions, such as setting ecosystem restoration goals, preserving rare and endemic taxa, and reducing the impacts of climate change on natural and cultural resources. We illustrate the importance of historical perspectives for understanding modern patterns and ecological change and present an approach that can be applied generally in conservation management planning. C1 [Rick, Torben C.; Hofman, Courtney A.; Reeder-Myers, Leslie] Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Hofman, Courtney A.] Univ Maryland, Dept Anthropol, College Pk, MD 20742 USA. [Hofman, Courtney A.; Ralls, Katherine; Fleischer, Robert; Maldonado, Jesus] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC USA. [Maldonado, Jesus] NMNH, Dept Vertebrate Zool, Washington, DC USA. [Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Front Royal, VA USA. [Ghalambor, Cameron K.; Funk, W. Chris] Colorado State Univ, Dept Biol, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Anderson, R. Scott] No Arizona Univ, Sch Earth Sci & Environm Sustainabil, Flagstaff, AZ 86011 USA. [Boser, Christina L.; Morrison, Scott A.] Nature Conservancy, San Francisco, CA USA. [Braje, Todd J.] San Diego State Univ, Dept Anthropol, San Diego, CA 92182 USA. [Cayan, Daniel R.] Univ Calif San Diego, Scripps Inst Oceanog, San Diego, CA 92103 USA. [Cayan, Daniel R.] US Geol Survey, La Jolla, CA USA. [Chesser, R. Terry] NMNH, USGS Patuxent Wildlife Res Ctr, Washington, DC USA. [Collins, Paul W.] Santa Barbara Museum Nat Hist, Dept Vertebrate Zool, Santa Barbara, CA USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. [Faulkner, Kate R.; Galipeau, Russell; Huston, Ann] Channel Islands Natl Pk, Ventura, CA USA. [King, Julie] Catalina Isl Conservancy, Avalon, CA USA. [Laughrin, Lyndal] Univ Calif Santa Barbara, Santa Cruz Island Reserve, Santa Barbara, CA 93106 USA. [McEachern, Kathryn] USGS Western Ecol Res Ctr, Channel Islands Field Stn, Ventura, CA USA. [Muhs, Daniel R.] USGS Fed Ctr, Denver, CO USA. [Newsome, Seth D.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Still, Christopher] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. RP Rick, TC (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. EM rickt@si.edu OI Erlandson, Jon/0000-0002-4705-4319 NR 70 TC 13 Z9 13 U1 32 U2 173 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 2014 VL 64 IS 8 BP 680 EP 692 DI 10.1093/biosci/biu094 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AM6PV UT WOS:000339988000006 ER PT J AU Hershler, R Liu, HP Howard, J AF Hershler, Robert Liu, Hsiu-Ping Howard, Jeanette TI Springsnails: A New Conservation Focus in Western North America SO BIOSCIENCE LA English DT Article DE biodiversity; conservation; groundwater; western North America; gastropods ID WATER BIODIVERSITY CONSERVATION; PYRGULOPSIS-BRUNEAUENSIS; UNITED-STATES; LIFE-HISTORY; RIVER-BASIN; HYDROBIIDAE; GASTROPODS; ECOLOGY; POPULATIONS; SYSTEMATICS AB Springsnails (genus Pyrgulopsis) are one of the most abundant and diverse members of the endemic western North American aquatic biota. These tiny gastropods are imperiled by threats ranging from groundwater pumping to livestock grazing. During the past 25 years, this long-neglected element of biodiversity has emerged as a new focus of conservation-related activities, including protection of several species under the Endangered Species Act and monitoring and habitat restoration efforts. Molecular investigations have helped sharpen springsnail taxonomy and suggest that these animals cannot be managed using a priori assumptions of population structure. Despite this progress, there is an urgent need for additional studies of springsnail natural history, taxonomy, and genetics. The prospects for improving the protection and restoration of springsnail habitats are promising but are clouded by the overarching threat of groundwater mining, which may be addressed best by broader conservation efforts focused on regional groundwater-dependent ecosystems. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. [Liu, Hsiu-Ping] Metropolitan State Univ Denver, Dept Biol, Denver, CO USA. [Howard, Jeanette] Nature Conservancy, Calif Chapter, San Francisco, CA USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. EM hershlerr@si.edu FU Nature Conservancy [06132013-1651] FX We thank Cristi Baldino, from the USFWS; Daniel Gustafson; Janel Johnson and Eric Miskow, from the Nevada Natural Heritage Program; John Karges, from the Texas Natural History Survey; Jerry Landye; Mike Martinez, also from the USFWS; and Kathie Taylor, from Argenta Ecological Consultants, for sharing information or color slides of habitats. Mike Martinez provided helpful comments on a draft version of the manuscript. The preparation of the manuscript was supported in part by contract no. 06132013-1651 from The Nature Conservancy to RH. NR 63 TC 8 Z9 8 U1 2 U2 19 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0006-3568 EI 1525-3244 J9 BIOSCIENCE JI Bioscience PD AUG PY 2014 VL 64 IS 8 BP 693 EP 700 DI 10.1093/biosci/biu100 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AM6PV UT WOS:000339988000007 ER PT J AU Marquet, PA Allen, AP Brown, JH Dunne, JA Enquist, BJ Gillooly, JF Gowaty, PA Green, JL Harte, J Hubbell, SP O'Dwyer, J Okie, JG Ostling, A Ritchie, M Storch, D West, GB AF Marquet, Pablo A. Allen, Andrew P. Brown, James H. Dunne, Jennifer A. Enquist, Brian J. Gillooly, James F. Gowaty, Patricia A. Green, Jessica L. Harte, John Hubbell, Steve P. O'Dwyer, James Okie, Jordan G. Ostling, Annette Ritchie, Mark Storch, David West, Geoffrey B. TI On Theory in Ecology SO BIOSCIENCE LA English DT Article DE theory unification; metabolic theory; neutral theory biodiversity; maximum entropy theory of ecology; big data ID ALLOMETRIC SCALING LAWS; MARGINAL VALUE THEOREM; RESOURCE-RATIO THEORY; BODY-SIZE; METABOLIC THEORY; PATCHY ENVIRONMENT; COMMUNITY ECOLOGY; SPECIES ABUNDANCE; MAXIMUM-ENTROPY; NEUTRAL THEORY AB We argue for expanding the role of theory in ecology to accelerate scientific progress, enhance the ability to address environmental challenges, foster the development of synthesis and unification, and improve the design of experiments and large-scale environmental-monitoring programs. To achieve these goals, it is essential to foster the development of what we call efficient theories, which have several key attributes. Efficient theories are grounded in first principles, are usually expressed in the language of mathematics, make few assumptions and generate a large number of predictions per free parameter, are approximate, and entail predictions that provide well-understood standards for comparison with empirical data. We contend that the development and successive refinement of efficient theories provide a solid foundation for advancing environmental science in the era of big data. C1 [Marquet, Pablo A.] Pontificia Univ Catolica Chile, Sch Biol Sci, Dept Ecol, Santiago, Chile. [Marquet, Pablo A.] Inst Ecol & Biodivers, Santiago, Chile. [Marquet, Pablo A.; Dunne, Jennifer A.; Enquist, Brian J.; West, Geoffrey B.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Marquet, Pablo A.] Inst Sistemas Complejos Valparaiso, Valparaiso, Chile. [Allen, Andrew P.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Brown, James H.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Dunne, Jennifer A.] Pacific Ecoinformat & Computat Ecol Lab, Berkeley, CA USA. [Enquist, Brian J.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Gillooly, James F.] Univ Florida, Dept Biol, Gainesville, FL USA. [Gowaty, Patricia A.; Hubbell, Steve P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA USA. [Gowaty, Patricia A.; Hubbell, Steve P.] Univ Calif Los Angeles, Inst Environm & Sustainabil, Los Angeles, CA USA. [Gowaty, Patricia A.; Hubbell, Steve P.] Smithsonian Trop Res Inst, Panama City, Panama. [Green, Jessica L.] Univ Oregon, Inst Ecol & Evolutionary Biol, Eugene, OR 97403 USA. [Harte, John] Univ Calif Berkeley, Energy & Resources Grp, Berkeley, CA 94720 USA. [Harte, John] Univ Calif Berkeley, Environm Sci Policy & Management Dept, Berkeley, CA 94720 USA. [O'Dwyer, James] Univ Illinois, Dept Plant Biol, Urbana, IL USA. [Okie, Jordan G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Ostling, Annette] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Ritchie, Mark] Syracuse Univ, Dept Biol, Syracuse, NY 13244 USA. [Storch, David] Charles Univ Prague, Fac Sci, Ctr Theoret Study, Prague, Czech Republic. [Storch, David] Charles Univ Prague, Fac Sci, Dept Ecol, Prague, Czech Republic. RP Marquet, PA (reprint author), Pontificia Univ Catolica Chile, Sch Biol Sci, Dept Ecol, Santiago, Chile. EM pmarquet@bio.puc.cl RI Marquet, Pablo /B-7732-2009; Storch, David/C-3339-2017; OI Marquet, Pablo /0000-0001-6369-9339; Storch, David/0000-0001-5967-1544; Enquist, Brian/0000-0002-6124-7096 FU National Center for Ecological Analysis and Synthesis; National Science Foundation (NSF) [DEB-0072909]; University of California, Santa Barbara; Santa Fe Institute, through NSF [DEB-0628281, ICM P05-002, PFB-23, FONDAP 1501-0001] FX This research was supported by the National Center for Ecological Analysis and Synthesis, a center funded by National Science Foundation (NSF) grant no. DEB-0072909, the University of California, Santa Barbara. We also acknowledge support from the Santa Fe Institute, through NSF grant no. DEB-0628281 and projects no. ICM P05-002, no. PFB-23, and no. FONDAP 1501-0001. This article resulted from a meeting in Valparaiso, Chile, in 2006. The first draft of the manuscript came into being in early 2007 as a manifesto for ecology, which we decided to make public, with the understanding that what we say may contribute to the advancement of the field. We thank many individuals who have provided valuable 'comments and criticisms and attended some of the meetings in which we discussed these ideas. In particular, we thank Jayanth Banavar, John Damuth, Aurora Gaxiola, Amos Maritan, and Igor Volkov. Finally, we thank three anonymous reviewers for their insights, comments, and helpful criticisms in some key conceptual and philosophical issues, which helped us to temper and refine our thoughts about theory in ecology. NR 78 TC 21 Z9 21 U1 19 U2 204 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 2014 VL 64 IS 8 BP 701 EP 710 DI 10.1093/biosci/biu098 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA AM6PV UT WOS:000339988000008 ER PT J AU Schreeg, LA Santiago, LS Wright, SJ Turner, BL AF Schreeg, L. A. Santiago, L. S. Wright, S. J. Turner, B. L. TI Stem, root, and older leaf N:P ratios are more responsive indicators of soil nutrient availability than new foliage SO ECOLOGY LA English DT Article DE Barro Colorado Nature Monument, Panama; forests; nitrogen; N:P ratios; phosphorus; soil nutrient availability; stoichiometry; woody plants ID LOWLAND TROPICAL FOREST; RAIN-FORESTS; P RATIOS; NITROGEN; PHOSPHORUS; PLANTS; TREE; STOICHIOMETRY; GROWTH; DETERMINANT AB Foliar nitrogen to phosphorus (N:P) ratios are widely used to indicate soil nutrient availability and limitation, but the foliar ratios of woody plants have proven more complicated to interpret than ratios from whole biomass of herbaceous species. This may be related to tissues in woody species acting as nutrient reservoirs during active growth, allowing maintenance of optimal N:P ratios in recently produced, fully expanded leaves (i.e., "new" leaves, the most commonly sampled tissue). Here we address the hypothesis that N:P ratios of newly expanded leaves are less sensitive indicators of soil nutrient availability than are other tissue types in woody plants. Seedlings of five naturally established tree species were harvested from plots receiving two years of fertilizer treatments in a lowland tropical forest in the Republic of Panama. Nutrient concentrations were determined in new leaves, old leaves, stems, and roots. For stems and roots, N:P ratios increased after N addition and decreased after P addition, and trends were consistent across all five species. Older leaves also showed strong responses to N and P addition, and trends were consistent for four of five species. In comparison, overall N:P ratio responses in new leaves were more variable across species. These results indicate that the N:P ratios of stems, roots, and older leaves are more responsive indicators of soil nutrient availability than are those of new leaves. Testing the generality of this result could improve the use of tissue nutrient ratios as indices of soil nutrient availability in woody plants. C1 [Schreeg, L. A.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Schreeg, L. A.] Marine Biol Lab, Ctr Ecosyst, Woods Hole, MA 02543 USA. [Santiago, L. S.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Santiago, L. S.; Wright, S. J.; Turner, B. L.] Smithsonian Trop Res Inst, Panama City, Panama. RP Schreeg, LA (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. EM schreeg@gmail.com RI Turner, Benjamin/E-5940-2011; Wright, Stuart/M-3311-2013; Santiago, Louis/E-3185-2016 OI Turner, Benjamin/0000-0002-6585-0722; Wright, Stuart/0000-0003-4260-5676; Santiago, Louis/0000-0001-5994-6122 FU Andrew W. Mellon Foundation; Smithsonian Institute Scholarly Studies grant; University of California Regent's Faculty Fellowship; Marine Biological Laboratory-Brown University SEED grant FX Data are from Santiago et al. (2012), which was supported by a grant from the Andrew W. Mellon Foundation to S. J. Wright, a Smithsonian Institute Scholarly Studies grant to S. J. Wright and J. B. Yavitt, and a University of California Regent's Faculty Fellowship to L. S. Santiago. We thank Omar Hernandez and Rufino Gonzalez for their field support. L. A. Schreeg was partially supported through a Marine Biological Laboratory-Brown University SEED grant to Z. Cardon, S. Porder, and L. A. Schreeg. NR 37 TC 17 Z9 22 U1 8 U2 105 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 2014 VL 95 IS 8 BP 2062 EP 2068 PG 7 WC Ecology SC Environmental Sciences & Ecology GA AM9QK UT WOS:000340215900005 PM 25230458 ER PT J AU Ledo, A Schnitzer, SA AF Ledo, Alicia Schnitzer, Stefan A. TI Disturbance and clonal reproduction determine liana distribution and maintain liana diversity in a tropical forest SO ECOLOGY LA English DT Article DE density dependence; disturbance; habitat specialization; point pattern analysis; spatial pattern; species coexistence ID NEGATIVE DENSITY-DEPENDENCE; SPATIAL POINT PATTERNS; BARRO-COLORADO ISLAND; HABITAT ASSOCIATIONS; SPECIES-DIVERSITY; NEOTROPICAL FOREST; TREE DIVERSITY; BASAL AREA; ABUNDANCE; MAINTENANCE AB Negative density dependence (NDD) and habitat specialization have received strong empirical support as mechanisms that explain tree species diversity maintenance and distribution in tropical forests. In contrast, disturbance appears to play only a minor role. Previous studies have rarely examined the relative strengths of these diversity maintenance mechanisms concurrently, and few studies have included plant groups other than trees. Here we used a large, spatially explicit data set from Barro Colorado Island, Panama (BCI) to test whether liana and tree species distribution patterns are most consistent with NDD, habitat specialization, or disturbance. We found compelling evidence that trees responded to habitat specialization and NDD; however, only disturbance explained the distribution of the majority of liana species and maintained liana diversity. Lianas appear to respond to disturbance with high vegetative (clonal) reproduction, and liana species' ability to produce clonal stems following disturbance results in a clumped spatial distribution. Thus, clonal reproduction following disturbance explains local liana spatial distribution and diversity maintenance on BCI, whereas negative density dependence and habitat specialization, two prominent mechanisms contributing to tree species diversity and distribution, do not. C1 [Ledo, Alicia; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53210 USA. [Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Miami, FL 34002 USA. RP Ledo, A (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53210 USA. EM alicialedo@gmail.com OI Schnitzer, Stefan/0000-0002-2715-9455 FU NSF-DEB [0613666, 0845071, 1019436]; Research Growth Initiative grant for the University of Wisconsin-Milwaukee FX We thank the dedicated field technicians who worked on the BCI liana census. We also thank Robyn Burnham, Scott Mangan, and three anonymous reviewers for helpful comments on the manuscript, and Adrian Baddeley and Rolf Turner for their help with the code in the spatstats package. Financial support was provided by NSF-DEB 0613666, NSF-DEB 0845071, and NSF-DEB 1019436, as well as a Research Growth Initiative grant for the University of Wisconsin-Milwaukee. Logistical support was provided by the Smithsonian Tropical Research Institute. NR 64 TC 26 Z9 27 U1 4 U2 30 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 2014 VL 95 IS 8 BP 2169 EP 2178 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AM9QK UT WOS:000340215900015 PM 25230468 ER PT J AU Hadley, AS Frey, SJK Robinson, WD Kress, WJ Betts, MG AF Hadley, Adam S. Frey, Sarah J. K. Robinson, W. Douglas Kress, W. John Betts, Matthew G. TI Tropical forest fragmentation limits pollination of a keystone under story herb SO ECOLOGY LA English DT Article DE habitat fragmentation; habitat loss; Heliconia; hummingbird; patch size; Phaethornis; pollination; tropical forest ID HABITAT FRAGMENTATION; COSTA-RICA; LANDSCAPE STRUCTURE; POLLEN-LIMITATION; PLANT; ECOLOGY; HELICONIA; DEFORESTATION; CONNECTIVITY; COMPETITION AB Loss of native vegetation cover is thought to be a major driver of declines in pollination success worldwide. However, it is not well known whether reducing the fragmentation of remaining vegetation can ameliorate these negative effects. We tested the independent effects of composition vs. configuration on the reproductive success of a keystone tropical forest herb (Heliconia tortuosa). To do this we designed a large-scale mensurative experiment that independently varied connected forest-patch size (configuration) and surrounding amount of forest (composition). In each patch, we tested whether pollen tubes, fruit, and seed set were associated with these landscape variables. We also captured hummingbirds as an indication of pollinator availability in a subset of patches according to the same design. We found evidence for an effect of configuration on seed set of H. tortuosa, but not on other aspects of plant reproduction; proportion of seeds produced increased 40% across the gradient in patch size we observed (0.64 to >1300 ha), independent of the amount of forest in the surrounding landscape at both local and landscape scales. We also found that the availability of pollinators was dependent upon forest configuration; hummingbird capture rates increased three and one-half times across the patch size gradient, independent of forest amount. Finally, pollinator availability was strongly positively correlated with seed set. We hypothesize that the effects of configuration on plant fitness that we observed are due to reduced pollen quality resulting from altered hummingbird availability and/or movement behavior. Our results suggest that prioritizing larger patches of tropical forest may be particularly important for conservation of this species. C1 [Hadley, Adam S.; Frey, Sarah J. K.; Betts, Matthew G.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. [Robinson, W. Douglas] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Hadley, AS (reprint author), Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. EM hadley.adam@gmail.com RI Hadley, Adam/G-8391-2012 OI Hadley, Adam/0000-0002-8344-3354 FU NSF [DEB-1050954]; NSERC, PGS-D FX M. Paniagua, J. Chacon, and E. Sandi helped with data collection. T. Bertwelt, A. Chozinski, and E. Jackson assisted with lab analysis. The manuscript was greatly improved by comments from two anonymous reviewers. This research was funded by NSF-DEB-1050954 to M. G. Betts and W. D. Robinson, and NSERC, PGS-D to A. S. Hadley. NR 54 TC 10 Z9 12 U1 9 U2 103 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 2014 VL 95 IS 8 BP 2202 EP 2212 PG 11 WC Ecology SC Environmental Sciences & Ecology GA AM9QK UT WOS:000340215900018 PM 25230471 ER PT J AU Souther, S Tingley, MW Popescu, VD Hayman, DTS Ryan, ME Graves, TA Hartl, B Terrell, K AF Souther, Sara Tingley, Morgan W. Popescu, Viorel D. Hayman, David T. S. Ryan, Maureen E. Graves, Tabitha A. Hartl, Brett Terrell, Kimberly TI Biotic impacts of energy development from shale: research priorities and knowledge gaps SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID CHRONIC ANTHROPOGENIC NOISE; GREATER SAGE-GROUSE; GAS DEVELOPMENT; NATURAL-GAS; HABITAT FRAGMENTATION; METHANE CONTAMINATION; WATER MANAGEMENT; FOREST; BIODIVERSITY; PENNSYLVANIA AB Although shale drilling operations for oil and natural gas have increased greatly in the past decade, few studies directly quantify the impacts of shale development on plants and wildlife. We evaluate knowledge gaps related to shale development and prioritize research needs using a quantitative framework that includes spatial and temporal extent, mitigation difficulty, and current level of understanding. Identified threats to biota from shale development include: surface and groundwater contamination; diminished stream flow; stream siltation; habitat loss and fragmentation; localized air, noise, and light pollution; climate change; and cumulative impacts. We find the highest research priorities to be probabilistic threats (underground chemical migration; contaminant release during storage, during disposal, or from accidents; and cumulative impacts), the study of which will require major scientific coordination among researchers, industry, and government decision makers. Taken together, our research prioritization outlines a way forward to better understand how energy development affects the natural world. C1 [Souther, Sara] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Tingley, Morgan W.] Princeton Univ, Woodrow Wilson Sch, Princeton, NJ 08544 USA. [Popescu, Viorel D.; Ryan, Maureen E.] Simon Fraser Univ, Dept Biol Sci, Earth Ocean Res Grp, Burnaby, BC V5A 1S6, Canada. [Popescu, Viorel D.] Univ Bucharest, Environm Res Ctr, Bucharest, Romania. [Hayman, David T. S.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Hayman, David T. S.] Univ Florida, Dept Biol, Gainesville, FL USA. [Hayman, David T. S.] Massey Univ, MEpiLab, Palmerston North, New Zealand. [Ryan, Maureen E.] Univ Washington, Sch Environm & Forest Sci, Seattle, WA USA. [Graves, Tabitha A.] Colorado State Univ, Dept Fish Wildlife & Conservat Biol, Ft Collins, CO 80523 USA. [Hartl, Brett] Soc Conservat Biol, Washington, DC USA. [Terrell, Kimberly] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. RP Souther, S (reprint author), Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. EM ssouther@wisc.edu RI Popescu, Viorel/O-3792-2014; OI Tingley, Morgan/0000-0002-1477-2218 FU David H Smith Fellowship program; Cedar Tree Foundation; Policy Fellowship from the Wilburforce Foundation FX We received support from the David H Smith Fellowship program, administered by the Society for Conservation Biology and funded by the Cedar Tree Foundation. BH was supported by a Policy Fellowship from the Wilburforce Foundation to the Society for Conservation Biology. An early version of this manuscript was sent as a letter to the US Geological Survey, the Environmental Protection Agency, and the US Department of the Interior; we thank these agencies for their review and assistance in improving the manuscript. We also thank M Bohm and B Collen for providing the freshwater species richness data, and S Friedrich for graphic design of Figure 2. NR 59 TC 23 Z9 24 U1 4 U2 80 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD AUG PY 2014 VL 12 IS 6 BP 330 EP 338 DI 10.1890/130324 PG 9 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA AM7XY UT WOS:000340083200015 ER PT J AU Velez, MI Escobar, J Brenner, M Rangel, O Betancourt, A Jaramillo, AJ Curtis, JH Moreno, JL AF Velez, Maria I. Escobar, Jaime Brenner, Mark Rangel, Orlando Betancourt, Alejandra Jaramillo, Alexis J. Curtis, Jason H. Moreno, Jessica L. TI Middle to late Holocene relative sea level rise, climate variability and environmental change along the Colombian Caribbean coast SO HOLOCENE LA English DT Article DE Caribbean; climate variability; diatoms; isotopes; middle-late Holocene; relative sea level change ID LAST GLACIAL MAXIMUM; ORGANIC-MATTER; HISTORY; RIVER; MANGROVE; WETLANDS; RATIOS; RECORD; CARBON; PLANTS AB We analyzed diatoms, lithology, and stable isotopes in a sediment core from the Cienaga Grande de Santa Marta lagoon to reveal the history of late Holocene relative sea level rise and the ontogeny of the lagoon on the Caribbean coast of Colombia. At similar to 5300 cal. yr BP, the area was characterized by shallow, freshwater ponds that were prone to seasonal flooding. From similar to 4250 to similar to 2060 cal. yr BP, these ponds became brackish as relative sea level began to rise, and since similar to 2060 cal. yr BP, marine conditions have prevailed. In addition to tracking relative sea level rise, we also investigated periods of greater and lesser precipitation during times of brackish and marine conditions, respectively, as indicated by diatom-inferred changes in water salinity and shifts in the source of sediment organic matter. Comparisons with other regional paleoenvironmental records suggest that humid climate conditions prevailed in the Caribbean until about 4000 cal. yr BP. After that time, climate became more variable, with drier conditions registered from similar to 4000 to 2000 cal. yr BP. Wetter conditions returned after similar to 2000 cal. yr BP. C1 [Velez, Maria I.] Univ Regina, Regina, SK S4S 0A2, Canada. [Escobar, Jaime] Uninorte, Barranquilla, Atlantico, Colombia. [Escobar, Jaime] Smithsonian Trop Res Inst, Balboa, Panama. [Brenner, Mark; Curtis, Jason H.] Univ Florida, Gainesville, FL 32611 USA. [Rangel, Orlando; Betancourt, Alejandra; Jaramillo, Alexis J.] Univ Nacl Colombia, Bogota, Colombia. [Moreno, Jessica L.] Univ Bogota Jorge Tadeo Lozano, Bogota, Colombia. RP Velez, MI (reprint author), Univ Regina, Dept Geol, Regina, SK S4S 0A2, Canada. EM Maria.Velez@uregina.ca FU Inter-American Institute for Global Change Research (IAI) [CRN3038]; US National Science Foundation [GEO-1128040]; Research Office at the Universidad del Norte; Vice President's office of the Universidad Nacional de Colombia (Vice-Rector de Investigacion y Extensin) FX This work was funded by a grant from the Inter-American Institute for Global Change Research (IAI) CRN3038, which is supported by the US National Science Foundation (Grant GEO-1128040). We thank the Vice President's office of the Universidad Nacional de Colombia (Vice-Rector de Investigacion y Extensin) for support of the project 'Biodiversity Assessment of Colombian Caribbean Region: Synthesis of Knowledge and Environmental Services'. We thank the Research Office at the Universidad del Norte for funding the geochemical analyses. NR 53 TC 2 Z9 2 U1 5 U2 21 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0959-6836 EI 1477-0911 J9 HOLOCENE JI Holocene PD AUG PY 2014 VL 24 IS 8 BP 898 EP 907 DI 10.1177/0959683614534740 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA AM8NE UT WOS:000340131800002 ER PT J AU Andrews, BJ AF Andrews, Benjamin J. TI Magmatic storage conditions, decompression rate, and incipient caldera collapse of the 1902 eruption of Santa Maria Volcano, Guatemala SO JOURNAL OF VOLCANOLOGY AND GEOTHERMAL RESEARCH LA English DT Article DE Magma storage conditions; Experimental petrology; Caldera formation; Magma decompression ID MOUNT-ST-HELENS; FORMING ERUPTION; SOUTHERN PERU; IGNIMBRITE ERUPTIONS; RHYOLITIC GLASSES; LITHIC FRAGMENTS; ASCENT; EVOLUTION; MODEL; WATER AB Phase equilibria experiments and analysis of natural pumice and phenocryst compositions indicate the 1902 Santa Maria dacite was stored at similar to 140-170 MPa and 840-850 degrees C prior to eruption. H2O-saturated, cold-seal experiments conducted in vessels with an intrinsic log f(O2) of NNO + 1 +/- 0.5 show that the natural phase assemblage (melt + plagioclase + amphibole + orthopyroxene + Fe-Ti oxides + apatite) is stable from approximately 115-140 MPa at temperatures below similar to 825 degrees C, to similar to 840-860 degrees C at 150 MPa, to >850 and <875 degrees C at 200 MPa. Natural plagioclase phenocrysts have rim compositions that range from An(40)-An(45); this range of compositions defines a similar to 20 degrees C band that intersects the stable phase assemblage at similar to 150 MPa and 850 degrees C. Plagioclase hosted melt inclusions were analyzed using FTIR and commonly contain <5 wt.% H2O, which corresponds to a pressure of similar to 170 MPa at 850 degrees C, under pure H2O saturated conditions. Amphibole geothermobarometry (Ridolfi et al., 2010) applied to experimental samples suggest two populations of amphiboles, phenocrysts grown during the experiments and inherited xenocrysts, but the pressure-temperature conditions returned by the geothermobarometer are routinely >50 MPa and >50 degrees C greater than experimental run conditions; precise estimates of magmatic conditions based solely upon amphibole composition are likely inaccurate. The experimental results and analysis of natural crystals suggest that although the natural amphiboles likely record a broad range of magmatic conditions, only the lower bounds of that range reflect pre-eruptive storage conditions. Comparison of Santa Maria microlite abundances with decompression experiments examining other silicic systems from the literature suggests that the 1902 dacite decompressed at the rate of similar to 0.005 to 0.01 MPa/s during the eruption. Applying the decompression rate with the previously described eruption rate of approximately 2-3 x 10(8) kg/s (Williams and Self, 1983; Carey and Sparks, 1986) to the conduit model CONFLOW reveals that the eruption conduit was dike-like with an along-strike length >1 km. Despite depositing similar to 20 km(3) of dacite tephra (equivalent to similar to 8.5 km(3) magma), the 1902 eruption did not form an obvious caldera. This work suggests that collapse of the dike-like conduit terminated the eruption, preventing full caldera collapse. Published by Elsevier B.V. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Andrews, BJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. NR 42 TC 2 Z9 2 U1 3 U2 21 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-0273 EI 1872-6097 J9 J VOLCANOL GEOTH RES JI J. Volcanol. Geotherm. Res. PD AUG 1 PY 2014 VL 282 BP 103 EP 114 DI 10.1016/j.jvolgeores.2014.06.009 PG 12 WC Geosciences, Multidisciplinary SC Geology GA AN0YH UT WOS:000340309400009 ER PT J AU Hong, T AF Hong, Terry TI I Am China SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC 20013 USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC 20013 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2014 VL 139 IS 13 BP 85 EP 86 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA AM7DM UT WOS:000340024900141 ER PT J AU Liu, G Xu, CQ Cao, Q Zimmermann, W Songer, M Zhao, SS Li, K Hu, DF AF Liu, Gang Xu, Chao-Qun Cao, Qing Zimmermann, Waltraut Songer, Mellisa Zhao, Sha-Sha Li, Kai Hu, De-Fu TI Mitochondrial and pedigree analysis in Przewalski's horse populations: implications for genetic management and reintroductions SO MITOCHONDRIAL DNA LA English DT Article DE Fecal sampling; genetic diversity; mitochondrial DNA; pedigree; Przewalski's horse; reintroduction ID FECAL DNA AMPLIFICATION; URSUS-ARCTOS; PRESERVATION METHODS; SEX IDENTIFICATION; SEQUENCE VARIATION; EQUUS-PRZEWALSKII; DOMESTIC HORSE; GENUS EQUUS; WILD HORSE; CONSERVATION AB Background and Aims: Przewalski's horses have been imported from the western zoos to China since 1985. Yet the genetic diversity in China's populations has not been studied, thus lacking of such knowledge inevitably affects this population's management. The aim of this study was to assess genetic diversity in Chinese population of Przewalski's horses via mitochondrial DNA (mtDNA) control region and pedigree analysis. Materials and methods: Two captive and one reintroduced populations were examined based on mitochondrial DNA control region variation via fecal sampling from 2010 to 2012, together with pedigree analysis. Results: Amplification success rates of fecal mtDNA were as high as 96.2% (93.8%-100%), and were higher for sample in winter than in summer and autumn. Two haplotypes were identified and shared among three populations, but the proportion of individuals with each haplotype varied among the three populations (F-ST = 0.10874, p = 0.00978). Haplotype diversity in the released population (0.153) was much lower than that in the two captive populations (0.4011 and 0.4966), in accordance with the direction of increase in probability of identity at the dam lines. Conclusion: Future concerns in Przewalski's horse population management should emphasize on strict reproduction control to minimize inbreeding in captivity, followed by long-term genetic diversity guidelines and non-invasive monitoring in the reintroduction programmes. C1 [Liu, Gang; Xu, Chao-Qun; Zhao, Sha-Sha; Li, Kai; Hu, De-Fu] Beijing Forestry Univ, Coll Biol Sci & Technol, Lab Noninvas Res Technol Endangered Species, Beijing 100083, Peoples R China. [Cao, Qing] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Zimmermann, Waltraut] Cologne Zool Garden, Cologne, Germany. [Songer, Mellisa] Smithsonian Natl Zool Pk, Conservat & Res Ctr, Front Royal, VA USA. RP Hu, DF (reprint author), Beijing Forestry Univ, Coll Biol Sci & Technol, Beijing 100083, Peoples R China. EM hudf@bjfu.edu.cn FU Special Fund for Forestry Scientific Research in the Public Interest; China's Ministry of Science and Technology [201004054]; National Natural Science Foundation [31000257] FX This work was financed by Special Fund for Forestry Scientific Research in the Public Interest, China's Ministry of Science and Technology (No. 201004054), and the National Natural Science Foundation (No. 31000257). The authors report no conflicts of interest. The authors alone are responsible for the content and writing of the paper. NR 56 TC 0 Z9 0 U1 4 U2 37 PU INFORMA HEALTHCARE PI LONDON PA TELEPHONE HOUSE, 69-77 PAUL STREET, LONDON EC2A 4LQ, ENGLAND SN 1940-1736 EI 1940-1744 J9 MITOCHONDR DNA JI Mitochondrial DNA PD AUG PY 2014 VL 25 IS 4 BP 313 EP 318 DI 10.3109/19401736.2013.800487 PG 6 WC Genetics & Heredity SC Genetics & Heredity GA AM8OV UT WOS:000340136500029 PM 23808923 ER PT J AU Komar, P Kessler, EM Bishof, M Jiang, L Sorensen, AS Ye, J Lukin, D AF Komar, P. Kessler, E. M. Bishof, M. Jiang, L. Sorensen, A. S. Ye, J. Lukin, D. TI A quantum network of clocks SO NATURE PHYSICS LA English DT Article ID TRAPPED ATOMIC IONS; ENTANGLEMENT DISTRIBUTION; FREQUENCY STANDARDS; TELEPORTATION; QUBITS; STABILITY; PHOTON; STATES; MATTER; NODES AB The development of precise atomic clocks plays an increasingly important role in modern society. Shared timing information constitutes a key resource for navigation with a direct correspondence between timing accuracy and precision in applications such as the Global Positioning System. By combining precision metrology and quantum networks, we propose a quantum, cooperative protocol for operating a network of geographically remote optical atomic clocks. Using nonlocal entangled states, we demonstrate an optimal utilization of global resources, and show that such a network can be operated near the fundamental precision limit set by quantum theory. Furthermore, the internal structure of the network, combined with quantum communication techniques, guarantees security both from internal and external threats. Realization of such a global quantum network of clocks may allow construction of a real-time single international time scale (world clock) with unprecedented stability and accuracy. C1 [Komar, P.; Kessler, E. M.; Lukin, D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kessler, E. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Bishof, M.; Ye, J.] Univ Colorado, Dept Phys, NIST, JILA, Boulder, CO 80309 USA. [Jiang, L.] Yale Univ, Dept Appl Phys, New Haven, CT 06511 USA. [Sorensen, A. S.] Danish Natl Res Fdn Ctr Quantum Opt, Niels Bohr Inst, QUANTOP, DK-2100 Copenhagen, Denmark. RP Lukin, D (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM lukin@physics.harvard.edu RI Ye, Jun/C-3312-2011; Sorensen, Anders/L-1868-2013; Kessler, Eric Matthias/E-6981-2012; Jiang, Liang/A-9847-2008 OI Sorensen, Anders/0000-0003-1337-9163; Kessler, Eric Matthias/0000-0001-9959-538X; Jiang, Liang/0000-0002-0000-9342 FU NSF; CUA; ITAMP; HQOC; JILA PFC; NIST; DARPA QuASAR; Quiness programs; Alfred P. Sloan Foundation; Packard Foundation; ARO MURI; ERC [306576]; NDSEG; NSF GRFP FX We are grateful to T. Rosenband, V. Vuletic J. Borregaard and T. Nicholson for enlightening discussions. This work was supported by NSF, CUA, ITAMP, HQOC, JILA PFC, NIST, DARPA QuASAR and Quiness programs, the Alfred P. Sloan Foundation, the Packard Foundation, ARO MURI, and the ERC grant QIOS (grant no. 306576); M.B. acknowledges support from NDSEG and NSF GRFP. It is dedicated to R. Blatt and P. Zoller on the occasion of their 60th birthday, when initial ideas for this work were formed. NR 43 TC 51 Z9 51 U1 4 U2 40 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 2014 VL 10 IS 8 BP 582 EP 587 DI 10.1038/NPHYS3000 PG 6 WC Physics, Multidisciplinary SC Physics GA AM8PU UT WOS:000340140300015 ER PT J AU Muletz, C Caruso, NM Fleischer, RC McDiarmid, RW Lips, KR AF Muletz, Carly Caruso, Nicholas M. Fleischer, Robert C. McDiarmid, Roy W. Lips, Karen R. TI Unexpected Rarity of the Pathogen Batrachochytrium dendrobatidis in Appalachian Plethodon Salamanders: 1957-2011 SO PLOS ONE LA English DT Article ID AMPHIBIAN CHYTRID FUNGUS; PARASITE VIRULENCE; KILLING FUNGUS; NORTH-CAROLINA; LOW-PREVALENCE; CLIMATE-CHANGE; USA; WIDESPREAD; DECLINES; DISEASE AB Widespread population declines in terrestrial Plethodon salamanders occurred by the 1980s throughout the Appalachian Mountains, the center of global salamander diversity, with no evident recovery. We tested the hypothesis that the historic introduction and spread of the pathogenic fungus Batrachochytrium dendrobatidis (Bd) Plethodon population declines. We expected to detect elevated prevalence of Bd prior to population declines as observed for Central American plethodontids. We tested 1,498 Plethodon salamanders of 12 species (892 museum specimens, 606 wild individuals) for the presence of Bd, and tested 94 of those for Batrachochytrium salamandrivorans (Bs) and for ranavirus. Field samples were collected in 2011 from 48 field sites across a 767 km transect. Historic samples from museum specimens ere collected at five sites with the greatest number and longest duration of collection (1957-987), four of which were sampled in the field in 2011. None of the museum specimens were positive for Bd, but four P. cinereus from field surveys positive The overall Bd prevalence from 1957-2011 for 12 Plethodon species sampled across a 757 km transect was 0.2% (95% CI 0.1-0.7%). All 94 samples were negative for Bs and ranavirus. We conclude that known amphibian pathogens are unlikely causes for declines in these Plethodon populations. Furthermore, these exceptionally low levels of Bd, in a region known to harbor Bd, may indicate that Plethodon specific traits limit Bd infection. C1 [Muletz, Carly; Caruso, Nicholas M.; Lips, Karen R.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Caruso, Nicholas M.] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL USA. [Muletz, Carly; Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC USA. [McDiarmid, Roy W.] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Muletz, C (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM cmuletz@umd.edu OI Lips, Karen/0000-0002-2719-1551 FU National Science Foundation [DEB 0917653, 0213851, 0234386]; University of Maryland; Smithsonian Seed Grant Program FX The National Science Foundation (http://www.nsf.gov/) provided support to KRL (DEB 0917653, 0213851, 0234386). Funding for this project was provided by the University of Maryland and Smithsonian Seed Grant Program (http://www.sgsi.umd.edu/) to KRL, RCF and RWM. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 46 TC 11 Z9 11 U1 4 U2 65 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 1 PY 2014 VL 9 IS 8 AR e103728 DI 10.1371/journal.pone.0103728 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM4JL UT WOS:000339819800074 PM 25084159 ER PT J AU do Nascimento, JD Garcia, RA Mathur, S Anthony, F Barnes, SA Meibom, S da Costa, JS Castro, M Salabert, D Ceillier, T AF do Nascimento, J. -D., Jr. Garcia, R. A. Mathur, S. Anthony, F. Barnes, S. A. Meibom, S. da Costa, J. S. Castro, M. Salabert, D. Ceillier, T. TI ROTATION PERIODS AND AGES OF SOLAR ANALOGS AND SOLAR TWINS REVEALED BY THE KEPLER MISSION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: evolution; stars: fundamental parameters; stars: rotation; stars: solar-type; Sun: fundamental parameters ID MAIN-SEQUENCE STARS; STELLAR ROTATION; LITHIUM ABUNDANCE; SUN; DEPLETION; GYROCHRONOLOGY; EMISSION; PLANETS; MASS AB A new sample of solar analogs and twin candidates has been constructed and studied, paying particular attention to their light curves from NASA's Kepler mission. This Letter aims to assess their evolutionary status, derive their rotation and ages, and identify those which are solar analogs or solar twin candidates. We separate out the subgiants that compose a large fraction of the asteroseismic sample, and which show an increase in the average rotation period as the stars ascend the subgiant branch. The rotation periods of the dwarfs, ranging from 6 to 30 days and averaging 19 days, allow us to assess their individual evolutionary states on the main sequence and to derive their ages using gyrochronology. These ages are found to be in agreement with a correlation coefficient of r = 0.79 with independent asteroseismic ages, where available. As a result of this investigation, we are able to identify 34 stars as solar analogs and 22 of them as solar twin candidates. C1 [do Nascimento, J. -D., Jr.; Meibom, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [do Nascimento, J. -D., Jr.; Anthony, F.; da Costa, J. S.; Castro, M.] Univ Fed Rio Grande do Norte, UFRN, Dep Fis Teor & Expt, DFTE, BR-59072970 Natal, RN, Brazil. [Garcia, R. A.; Salabert, D.; Ceillier, T.] Univ Paris Diderot IRFU SAp, Ctr Saclay, CNRS, Lab AIM,CEA DSM, F-91191 Gif Sur Yvette, France. [Mathur, S.] Space Sci Inst, Boulder, CO 80301 USA. [Barnes, S. A.] Leibniz Inst Astrophys, D-14467 Potsdam, Germany. RP do Nascimento, JD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jdonascimento@cfa.harvard.edu RI Castro, Matthieu/E-9247-2013; do Nascimento, Jose Dias/D-2416-2014; OI do Nascimento, Jose Dias/0000-0001-7804-2145; Garcia, Rafael/0000-0002-8854-3776 FU CNPq [Universal-B 485880/2012-1, PDE 237139/2012]; European Community [269194 (IRSES/ASK)]; CNES/CoRoT grant; NASA [NNX12AE17G] FX The authors thank the Kepler team. J.D.N. acknowledges CNPq Universal-B 485880/2012-1 and PDE 237139/2012. R. A. G. acknowledges the European Community Seventh Framework Program (FP7/2007-2013) No. 269194 (IRSES/ASK) and a CNES/CoRoT grant. S. M. was supported by NASA grant NNX12AE17G. J.D.N. is grateful to B. Chaplin for discussions and suggestions. This is a part of KASC Workpackage PE11.5 leader by J.D.N. This paper is in memoriam of Giusa Cayrel de Strobel, astronomer and pioneer in research on solar twins. NR 50 TC 15 Z9 15 U1 0 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 1 PY 2014 VL 790 IS 2 AR L23 DI 10.1088/2041-8205/790/2/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5KO UT WOS:000339897100009 ER PT J AU Fisher, DB Glazebrook, K Bolatto, A Obreschkow, D Cooper, EM Wisnioski, E Bassett, R Abraham, RG Damjanov, I Green, A McGregor, P AF Fisher, David B. Glazebrook, Karl Bolatto, Alberto Obreschkow, Danail Cooper, Erin Mentuch Wisnioski, Emily Bassett, Robert Abraham, Roberto G. Damjanov, Ivana Green, Andy McGregor, Peter TI EXTREME GAS FRACTIONS IN CLUMPY, TURBULENT DISK GALAXIES AT z similar to 0.1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: evolution; galaxies: ISM; galaxies: starburst; galaxies: star formation ID STAR-FORMING GALAXIES; HIGH-REDSHIFT GALAXIES; IRAM LEGACY SURVEY; MOLECULAR GAS; MASSIVE GALAXIES; FORMATION EFFICIENCY; FORMATION HISTORY; SCALING RELATIONS; DEPLETION TIME; SINS SURVEY AB In this Letter, we report the discovery of CO fluxes, suggesting very high gas fractions in three disk galaxies seen in the nearby universe (z similar to 0.1). These galaxies were investigated as part of the DYnamics of Newly Assembled Massive Objects (DYNAMO) survey. High-resolution Hubble Space Telescope imaging of these objects reveals the presence of large star forming clumps in the bodies of the galaxies, while spatially resolved spectroscopy of redshifted II alpha reveals the presence of high dispersion rotating disks. The internal dynamical state of these galaxies resembles that of disk systems seen at much higher redshifts (1 < z < 3). Using CO(1-0) observations made with the Plateau de Bure Interferometer, we find gas fractions of 20%-30% and depletion times of t(dep) similar to 0.5 Gyr (assuming aMilky-Way-like alpha(CO)). These properties are unlike those expected for low-redshift galaxies of comparable specific star formation rate, but they are normal for their high-z counterparts. DYNAMO galaxies break the degeneracy between gas fraction and redshift, and we show that the depletion time per specific star formation rate for galaxies is closely tied to gas fraction, independent of redshift. We also show that the gas dynamics of two of our local targets corresponds to those expected from unstable disks, again resembling the dynamics of high-z disks. These results provide evidence that DYNAMO galaxies are local analogs to the clumpy, turbulent disks, which are often found at high redshift. C1 [Fisher, David B.; Glazebrook, Karl; Bassett, Robert] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Glazebrook, Karl; Obreschkow, Danail] ARC Ctr Excellence All Sky Astrophys CAASTRO, Redfern, NSW 2016, Australia. [Bolatto, Alberto] Univ Maryland, Lab Millimeter Astron, College Pk, MD 20742 USA. [Obreschkow, Danail] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Cooper, Erin Mentuch] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Wisnioski, Emily] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Abraham, Roberto G.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada. [Damjanov, Ivana] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Green, Andy] Australian Astron Observ, N Ryde, NSW 1670, Australia. [McGregor, Peter] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Fisher, DB (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia. EM dfisher@swin.edu.au RI Glazebrook, Karl/N-3488-2015; OI Glazebrook, Karl/0000-0002-3254-9044; Green, Andrew/0000-0003-3052-0819 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Australian Research Council (ARC) Discovery Program (DP) [DP130101460]; CAREER [AST 08-38178, AST 09-55836]; Research Corporation for Science Advancement FX We thank the referee for helpful comments. We are very grateful to Sabine Konig for observational support and help calibrating the data. This work is based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain).; D. B. F. acknowledges support from Australian Research Council (ARC) Discovery Program (DP) grant DP130101460. Support for this project is provided in part by the Victorian Department of State Development, Business and Innovation through the Victorian International Research Scholarship (VIRS). A. B. acknowledges partial support form AST 08-38178, CAREER award AST 09-55836, and a Cottrell Scholar award from the Research Corporation for Science Advancement. NR 40 TC 12 Z9 12 U1 0 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 1 PY 2014 VL 790 IS 2 AR L30 DI 10.1088/2041-8205/790/2/L30 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5KO UT WOS:000339897100016 ER PT J AU Tian, H Kleint, L Peter, H Weber, M Testa, P DeLuca, E Golub, L Schanche, N AF Tian, H. Kleint, L. Peter, H. Weber, M. Testa, P. DeLuca, E. Golub, L. Schanche, N. TI OBSERVATIONS OF SUBARCSECOND BRIGHT DOTS IN THE TRANSITION REGION ABOVE SUNSPOTS WITH THE INTERFACE REGION IMAGING SPECTROGRAPH SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: chromosphere; sunspots; Sun: transition region; Sun: UV radiation ID HI-C; OSCILLATIONS; SIMULATIONS; DIAGNOSTICS; EMISSION; SPECTROMETER; PENUMBRAE; CORONA; LINES; MOSS AB Observations with the Interface Region Imaging Spectrograph (IRIS) have revealed numerous sub-arcsecond bright dots in the transition region above sunspots. These bright dots are seen in the 1400 and 1330 slit-jaw images. They are clearly present in all sunspots we investigated, mostly in the penumbrae, but also occasionally in some umbrae and light bridges. The bright dots in the penumbrae typically appear slightly elongated, with the two dimensions being 300-600 km and 250-450 km, respectively. The long sides of these dots are often nearly parallel to the bright filamentary structures in the penumbrae but sometimes clearly deviate from the radial direction. Their lifetimes are mostly less than one minute, although some dots last for a few minutes or even longer. Their intensities are often a few times stronger than the intensities of the surrounding environment in the slit-jaw images. About half of the bright dots show apparent movement with speeds of similar to 10-40 km s(-1) in the radial direction. Spectra of a few bright dots were obtained and the Si IV 1402.77 angstrom line profiles in these dots are significantly broadened. The line intensity can be enhanced by one to two orders of magnitude. Some relatively bright and long-lasting dots are also observed in several passbands of the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, and they appear to be located at the bases of loop-like structures. Many of these bright dots are likely associated with small-scale energy release events at the transition region footpoints of magnetic loops. C1 [Tian, H.; Weber, M.; Testa, P.; DeLuca, E.; Golub, L.; Schanche, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kleint, L.] Univ Appl Sci & Arts Northwestern Switzerland, CH-5210 Windisch, Switzerland. [Peter, H.] Max Planck Inst Solar Syst Res, D-37077 Gottingen, Germany. RP Tian, H (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hui.tian@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013 OI DeLuca, Edward/0000-0001-7416-2895 FU Lockheed-Martin [8100002705, SP02H1701R]; Norwegian Space Center (NSC, Norway) FX 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. This work is supported by contracts 8100002705 and SP02H1701R from Lockheed-Martin to SAO. We thank I. Hannah, J. Dudik, A. Lagg, and L. Rouppe van der Voort for helpful discussions. NR 33 TC 19 Z9 19 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 AUG 1 PY 2014 VL 790 IS 2 AR L29 DI 10.1088/2041-8205/790/2/L29 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5KO UT WOS:000339897100015 ER PT J AU Tremblay, GR Gladders, MD Baum, SA O'Dea, CP Bayliss, MB Cooke, KC Dahle, H Davis, TA Florian, M Rigby, JR Sharon, K Soto, E Wuyts, E AF Tremblay, Grant R. Gladders, Michael D. Baum, Stefi A. O'Dea, Christopher P. Bayliss, Matthew B. Cooke, Kevin C. Dahle, Hakon Davis, Timothy A. Florian, Michael Rigby, Jane R. Sharon, Keren Soto, Emmaris Wuyts, Eva TI A 30 kpc CHAIN OF "BEADS ON A STRING" STAR FORMATION BETWEEN TWO MERGING EARLY TYPE GALAXIES IN THE CORE OF A STRONG-LENSING GALAXY CLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (SDSS J1531+3414); galaxies; interactions; galaxies: star formation; gravitational lensing: strong ID COLOR-MAGNITUDE RELATIONS; GIANT ARCS; PROJECT; CONSTRAINTS; EVOLUTION; ORIGIN; SCALES; GAS; LAW AB New Hubble Space Telescope ultraviolet and optical imaging of the strong-lensing galaxy cluster SDSS J1531+3414 (z = 0.335) reveals two centrally dominant elliptical galaxies participating in an ongoing major merger. The interaction is at least somewhat rich in cool gas, as the merger is associated with a complex network of 19 massive superclusters of young stars (or small tidal dwarf galaxies) separated by similar to 1 kpc in projection from one another, combining to an estimated total star formation rate of similar to 5 M-circle dot yr(-1). The resolved young stellar superclusters are threaded by narrow Ha, [O-II], and blue excess filaments arranged in a network spanning similar to 27 kpc across the two merging galaxies. This morphology is strongly reminiscent of the well-known " beads on a string" mode of star formation observed on kiloparsecscales in the arms of spiral galaxies, resonance rings, and in tidal tails between interacting galaxies. Nevertheless, the arrangement of this star formation relative to the nuclei of the two galaxies is difficult to interpret in a dynamical sense, as no known " beads on a string" systems associated with kiloparsec-scale tidal interactions exhibit such lopsided morphology relative to the merger participants. In this Letter, we present the images and follow-up spectroscopy and discuss possible physical interpretations for the unique arrangement of the young stellar clusters. While we suggest that this morphology is likely to be dynamically short-lived, a more quantitative understanding awaits necessary multiwavelength follow-up, including optical integral field spectroscopy, ALMA submillimeter interferometry, and Chandra X-ray imaging. C1 [Tremblay, Grant R.; Davis, Timothy A.] European So Observ, D-85748 Garching, Germany. [Gladders, Michael D.; Florian, Michael] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, Michael D.; Florian, Michael] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Baum, Stefi A.; O'Dea, Christopher P.; Cooke, Kevin C.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Baum, Stefi A.; O'Dea, Christopher P.; Cooke, Kevin C.] Rochester Inst Technol, Sch Phys & Astron, Rochester, NY 14623 USA. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Sharon, Keren] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Soto, Emmaris] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Tremblay, GR (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM grant.tremblay@eso.org RI Rigby, Jane/D-4588-2012; OI Rigby, Jane/0000-0002-7627-6551; Davis, Timothy/0000-0003-4932-9379; Cooke, Kevin/0000-0002-2200-9845; Tremblay, Grant/0000-0002-5445-5401; Florian, Michael/0000-0001-5097-6755 FU European Community [229517]; NASA [HST-GO-13003]; Association of Universities for Research in Astronomy, Inc., under NASA [NAS5-26555]; Alfred P. Sloan Foundation; SDSS; Participating Institutions; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank Professors Francoise Combes, Eric Emsellem, and Tim de Zeeuw for thoughtful discussions. We also thank the anonymous referee whose feedback improved this work. G. R. T. and T. A. D. acknowledge support from a European Southern Observatory (ESO) Fellowship partially funded by the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517. Support for program number HST-GO-13003 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 NAS5-26555. This Letter is based on observations by the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute. We also present results from the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. 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/. NR 35 TC 5 Z9 5 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 2014 VL 790 IS 2 AR L26 DI 10.1088/2041-8205/790/2/L26 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AM5KO UT WOS:000339897100012 ER PT J AU O'Mara, MT Hickey, CM AF O'Mara, M. Teague Hickey, Cathriona M. TI The development of sex differences in ring-tailed lemur feeding ecology SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article DE Behavioral development; Diet; Juvenile; Female dominance; Reproduction; Resource partitioning; Lemur catta ID CAPUCHINS CEBUS-APELLA; FEMALE DOMINANCE; FORAGING BEHAVIOR; PAPIO-CYNOCEPHALUS; SOCIAL INFLUENCES; NICHE SEPARATION; TIME BUDGETS; SOUTHWESTERN MADAGASCAR; STREPSIRHINE PRIMATES; VARECIA-VARIEGATA AB Sex differences in feeding ecology may develop in response to fluctuations in physiological costs to females over their reproductive cycles, or to sexual size dimorphism, or function to minimize feeding competition within a group via resource partitioning. For most mammal species, it is unknown how these factors contribute to sex differences in feeding, or how the development of males and females reflects these intraspecific feeding differences. We show changes in dietary composition, diversity, overlap, and foraging behavior throughout development in ring-tailed lemurs (Lemur catta) and test how the development of sex differences in feeding is related to female costs of reproduction and year-round resource partitioning. Sex differences in dietary composition were only present when females were lactating, but sex differences in other aspects of feeding, including dietary diversity, and relative time spent feeding and foraging, developed at or near the time of weaning. Sex difference in juveniles and subadults, when present, were similar to the differences found in adults. The low year-round dietary overlap and early differences in dietary diversity indicate that some resource partitioning may begin with young individuals and fluctuate throughout development. The major differences between males and females in dietary composition suggest that these larger changes in diet are closely tied to female reproductive state when females must shift their diet to meet energetic and nutritional requirements. C1 [O'Mara, M. Teague] Smithsonian Trop Res Inst, Panama City, Panama. [O'Mara, M. Teague] Arizona State Univ, Sch Human Evolut & Social Change, Phoenix, AZ USA. [O'Mara, M. Teague] Univ Konstanz, Zukunftskolleg, Constance, Germany. [O'Mara, M. Teague] Univ Konstanz, Dept Biol, Constance, Germany. [O'Mara, M. Teague] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, D-78315 Radolfzell am Bodensee, Germany. [Hickey, Cathriona M.] Univ York, Dept Environm, CIRCLE, York YO10 5DD, N Yorkshire, England. RP O'Mara, MT (reprint author), Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Obstberg 1, D-78315 Radolfzell am Bodensee, Germany. EM tomara@orn.mpg.de OI O'Mara, M. Teague/0000-0002-6951-1648 FU National Science Foundation DDIG [BCS 0851761]; J. William Fulbright Foundation; Sigma Xi; ASU chapter; ASU Graduate and Professional Students Association; ASU School of Human Evolution and Social Change FX The authors would like to thank Ayden Sherritt, Paul Stephen, and Andy Fogel for their help with data collection. The authors thank Madagascar National Parks, the Ministere des Eaux et Foret, and ESSA-Foret Universite d'Antananarivo for research permission, and to the staff at Beza Mahafaly and MICET for facilitating logistics. Michelle Sauther, Frank Cuozzo, Jacky Antho, Stephanie Meredith, Andry Randrianandrasana, Jeannin Ranaivonasy, Benjamin Andriamihaja, and the members of the Beza Mahafaly Ecological Monitoring Team were all supportive of the fieldwork, as were Alison Richard and Robert Dewar. Leanne Nash, Kate Ihle, Meg Crofoot, Stephanie Meredith, and two anonymous reviewers greatly improved this manuscript. This work was supported by the National Science Foundation DDIG (BCS 0851761), the J. William Fulbright Foundation, Sigma Xi and its ASU chapter, the ASU Graduate and Professional Students Association, and the ASU School of Human Evolution and Social Change. NR 123 TC 1 Z9 1 U1 9 U2 85 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 2014 VL 68 IS 8 BP 1273 EP 1286 DI 10.1007/s00265-014-1738-3 PG 14 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA AM3CE UT WOS:000339728500006 ER PT J AU Nadeau, NJ Ruiz, M Salazar, P Counterman, B Medina, JA Ortiz-Zuazaga, H Morrison, A McMillan, WO Jiggins, CD Papa, R AF Nadeau, Nicola J. Ruiz, Mayte Salazar, Patricio Counterman, Brian Medina, Jose Alejandro Ortiz-Zuazaga, Humberto Morrison, Anna McMillan, W. Owen Jiggins, Chris D. Papa, Riccardo TI Population genomics of parallel hybrid zones in the mimetic butterflies, H. melpomene and H. erato SO GENOME RESEARCH LA English DT Article ID HELICONIUS-BUTTERFLIES; MULLERIAN MIMICRY; GENE-FLOW; WARNING-COLOR; REPRODUCTIVE ISOLATION; ECOLOGICAL SPECIATION; CONVERGENT EVOLUTION; NATURAL-SELECTION; WIDE ASSOCIATION; DIVERGENCE AB Hybrid zones can be valuable tools for studying evolution and identifying genomic regions responsible for adaptive divergence and underlying phenotypic variation. Hybrid zones between subspecies of Helliconius butterflies can be very narrow and are maintained by strong selection acting on color pattern. The comimetic species, H. erato and H. melpomene, have parallel hybrid zones in which both species undergo a change from one color pattern form to another. We use restriction-associated DNA sequencing to obtain several thousand genome-wide sequence markers and use these to analyze patterns of population divergence across two pairs of parallel hybrid zones in Peru and Ecuador. We compare two approaches for analysis of this type of data alignment to a reference genome and de novo assembly and find that alignment gives the best results for species both closely (H. melpomene) and distantly (H. erato, similar to 15% divergent) related to the reference sequence. Our results confirm that the color pattern controlling loci account for the majority of divergent regions across the genome, but we also detect other divergent regions apparently unlinked to color pattern differences. We also use association mapping to identify previously unmapped color pattern loci, in particular the Ro locus. Finally, we identify a new cryptic population of H. timareta in Ecuador, which occurs at relatively low altitude and is mimetic with H. melpomene malleti. C1 [Nadeau, Nicola J.; Salazar, Patricio; Morrison, Anna; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Nadeau, Nicola J.] Univ Sheffield, Dept Anim & Plant Sci, Sheffield S10 2TN, S Yorkshire, England. [Ruiz, Mayte; Papa, Riccardo] Univ Puerto Rico, Dept Biol, San Juan, PR 00921 USA. [Ruiz, Mayte; Papa, Riccardo] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, San Juan, PR 00921 USA. [Salazar, Patricio] Univ Tecnol Indoamer, Ctr Invest Biodiversidad & Cambio Climat BioCamb, Quito, Ecuador. [Counterman, Brian] Mississippi State Univ, Dept Biol, Mississippi State, MS 39762 USA. [Medina, Jose Alejandro; Ortiz-Zuazaga, Humberto] Univ Puerto Rico, High Performance Comp Facil, San Juan, PR 00927 USA. [Ortiz-Zuazaga, Humberto] Univ Puerto Rico, Dept Comp Sci, San Juan, PR 00921 USA. [McMillan, W. Owen; Jiggins, Chris D.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Jiggins, CD (reprint author), Univ Cambridge, Dept Zool, Downing St, Cambridge CB2 3EJ, England. EM c.jiggins@zoo.cam.ac.uk RI Nadeau, Nicola/E-1149-2011; Jiggins, Chris/B-9960-2008; OI Nadeau, Nicola/0000-0002-9319-921X; Jiggins, Chris/0000-0002-7809-062X; Ortiz-Zuazaga, Humberto/0000-0002-4667-8357 FU BBSRC [H01439X/1]; NSF-CREST [0206200]; Leverhulme Trust; Ford Foundation; NIH-NIGMS INBRE [P20GM103475]; NSF-EPSCoR [1002410]; [NSF-DEB-1257839]; [NSF-IOS 1305686] FX We thank Simon Baxter, Doug Turnbull, and William Cresko for their help and advice with RAD library preparation and sequencing. Sequencing was performed at the University of Oregon, Genomics Core Facility and The Gene Pool genomics facility in the University of Edinburgh. We would also like to thank Julian Catchen for his help with Stacks. We thank the governments of Peru and Ecuador for their permission to collect and export specimens. Santiago Villamarin from the Museo Ecuatoriano de Ciencias Naturales provided institutional support in Ecuador. We also thank Ismael Aldas, Carlos Robalino, and Patricia Salazar for their assistance with fieldwork. Joanna Riley assisted with DNA extractions. John Davey gave us access to his unpublished mapping results. We thank three anonymous reviewers for their comments. This project was supported by research grants BBSRC H01439X/1, NSF-CREST #0206200, NSF-DEB-1257839, and NSF-IOS 1305686. N.J.N. was funded by a Leverhulme Trust award to C.D.J.; M.R. was funded through the Ford Foundation Postdoctoral Fellowship Program administered by the National Academies; H.O.Z. and J.A.M. were partially supported by NIH-NIGMS INBRE award P20GM103475 and NSF-EPSCoR award 1002410. NR 80 TC 20 Z9 20 U1 11 U2 81 PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT PI COLD SPRING HARBOR PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA SN 1088-9051 EI 1549-5469 J9 GENOME RES JI Genome Res. PD AUG PY 2014 VL 24 IS 8 BP 1316 EP 1333 DI 10.1101/gr.169292.113 PG 18 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity GA AM4XT UT WOS:000339860200007 PM 24823669 ER PT J AU Picq, S Alda, F Krahe, R Bermingham, E AF Picq, Sophie Alda, Fernando Krahe, Ruediger Bermingham, Eldredge TI Miocene and Pliocene colonization of the Central American Isthmus by the weakly electric fish Brachyhypopomus occidentalis (Hypopomidae, Gymnotiformes) SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Central America; diversification; electric fishes; freshwater fishes; historical biogeography; ichthyological provinces; Isthmus of Panama; knifefishes; molecular clock; multiple colonization ID FRESH-WATER FISHES; SOUTH-AMERICA; EVOLUTIONARY HISTORY; MOLECULAR PHYLOGENY; BIOTIC INTERCHANGE; CLIMATE-CHANGE; BIOGEOGRAPHY; PANAMA; PHYLOGEOGRAPHY; TELEOSTEI AB Aim We present a molecular phylogenetic and biogeographical analysis of Brachyhypopomus occidentalis, one of the few gymnotiform electric fish in Central America, to further understand the colonization and diversification processes of primary freshwater fishes over the Central American Isthmus. Location Lower Central America. Methods We used Bayesian and maximum-likelihood phylogenetic reconstructions using mitochondrial [cytochrome c oxidase subunit I (COI) and ATP synthase 6 and 8 (ATPase 8/6)] and nuclear (RAG1 and rhodopsin) genes and extensive geographical sampling, together with molecular clock analyses and tests of biogeographical scenarios to assess the timing and mode of dispersal and diversification. Results We identified high levels of phylogeographical structure, with a highly divergent lineage composed of individuals from western Atlantic Panama (Bocas), sister to all trans-Andean South American and Central American lineages. The Pacific slope of Panama showed surprisingly little genetic structure compared with the Atlantic slope. Molecular-clock and biogeographical analyses support two waves of colonization originating from South America: a first dispersal event in the late Miocene with the Bocas lineage as the only relict, and a second major colonization in the late Pliocene leading to the establishment of B. occidentalis in all central and eastern Panama drainages. Main conclusions The genetic structure of B. occidentalis over the Isthmian landscape reflects the progressive, complex and dynamic geological evolution of the region. Our results support multiple colonization events, with an ancient Miocene dispersal event followed by a recent rapid expansion in the late Pliocene, probably facilitated by the final closure of the Isthmus, which provided an important corridor. Keywords Central America, diversification, electric fishes, freshwater fishes, historical biogeography, ichthyological provinces, Isthmus of Panama, knifefishes, molecular clock, multiple colonization. C1 [Picq, Sophie; Alda, Fernando; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Picq, Sophie; Krahe, Ruediger; Bermingham, Eldredge] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. RP Picq, S (reprint author), McGill Univ, Dept Biol, 1205 Docteur Penfield, Montreal, PQ H3A 1B1, Canada. EM sophiepicq@gmail.com FU McGill-Smithsonian Tropical Research Institute Neotropical Environment Program; NSERC (Natural Sciences and Engineering Research Council of Canada); Smithsonian Institution FX We wish to thank all the people who helped in the collection of specimens, especially Andrew Martin, Rigoberto Gonzalez and Ruth G. Reina. We are also very grateful to Rigoberto Gonzalez for curatorial assistance and to Ruth G. Reina for laboratory assistance. We thank Vielka Salazar for insightful comments while preparing this manuscript as well as two anonymous reviewers and the editor for helpful suggestions that significantly improved this manuscript. Financial and logistical support was provided by grants from the McGill-Smithsonian Tropical Research Institute Neotropical Environment Program to S.P., from NSERC (Natural Sciences and Engineering Research Council of Canada) to R.K., and from the Smithsonian Institution to E.B. NR 67 TC 7 Z9 9 U1 3 U2 28 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 AUG PY 2014 VL 41 IS 8 BP 1520 EP 1532 DI 10.1111/jbi.12309 PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA AM2FT UT WOS:000339665900008 ER PT J AU Mori, S Itoh, A Nanami, S Tan, S Chong, L Yamakura, T AF Mori, Sanae Itoh, Akira Nanami, Satoshi Tan, Sylvester Chong, Lucy Yamakura, Takuo TI Effect of wood density and water permeability on wood decomposition rates of 32 Bornean rainforest trees SO JOURNAL OF PLANT ECOLOGY LA English DT Article DE Sarawak; carbon dynamics; fine wood litter; wood density; tropical rain forest ID LOCALLY WEIGHTED REGRESSION; LEAF-LITTER DECOMPOSITION; SMOOTHING SCATTERPLOTS; DECAY; DEBRIS; DURABILITY; ECOSYSTEMS; CHEMISTRY; WORLDWIDE; DYNAMICS AB A better understanding of wood litter decomposition is essential for predicting responses of forest ecosystems to global climate change. Recent studies suggest that chemical properties of wood litters, rather than physical ones such as wood density, are more important for interspecific differences in wood decomposition rates. However, empirical data are still limited, especially for tropical trees. In addition, decomposition rate of wood litter often varies with time, which makes interspecific comparison difficult. We studied the wood decomposition of 32 rainforest trees to elucidate (i) the degree of interspecific variation in wood decomposition rate of a given size and configuration and (ii) if initial wood density and water permeability are consistent predictors of the overall decomposition rate and its pattern over time. A common garden decomposition experiment was conducted in a tropical rainforest in Malaysian Borneo for 32 native tree species. Small wood sticks were set on the forest floor and the weight loss was monitored monthly for 2.7 years. We found large variation in the wood decomposition rate (a 49-fold range), suggesting that we need to consider this variation when calculating community-level carbon dynamics of tropical rain forests. The physical traits of wood, i.e. wood density and water permeability, were related to wood decomposition rate and its pattern over time. Decomposition half-time related positively and negatively to initial wood density and water permeability, respectively. The time-dependent-rate model fitted better for 18 species (56% of the study species) that had higher water permeabilities than the others, suggesting that micelle porosity in wood relates to temporal changes in decomposition rate. C1 [Mori, Sanae; Itoh, Akira; Nanami, Satoshi; Yamakura, Takuo] Osaka City Univ, Grad Sch Sci, Plant Ecol Lab, Sumiyoshi Ku, Osaka 5588585, Japan. [Tan, Sylvester] Harvard Univ, Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Cambridge, MA 02138 USA. [Tan, Sylvester] Harvard Univ, Arnold Arboretum, Cambridge, MA 02138 USA. [Tan, Sylvester; Chong, Lucy] Sarawak Forestry Corp, Appl Forest Sci & Ind Dev, Kuching 93250, Sarawak, Malaysia. RP Itoh, A (reprint author), Osaka City Univ, Grad Sch Sci, Plant Ecol Lab, Sumiyoshi Ku, Sugimoto 3-3-138, Osaka 5588585, Japan. EM itoha@sci.osaka-cu.ac.jp FU Japan Society for the Promotion of Science [20405011] FX Grants-in-Aid for Scientific Research from Japan Society for the Promotion of Science (20405011). NR 38 TC 1 Z9 1 U1 1 U2 28 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1752-9921 EI 1752-993X J9 J PLANT ECOL JI J. Plant Ecol. PD AUG PY 2014 VL 7 IS 4 BP 356 EP 363 DI 10.1093/jpe/rtt041 PG 8 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA AM5RL UT WOS:000339917700005 ER PT J AU Heida, M Jonker, PG Torres, MAP Kool, E Servillat, M Roberts, TP Groot, PJ Walton, DJ Moon, DS Harrison, FA AF Heida, M. Jonker, P. G. Torres, M. A. P. Kool, E. Servillat, M. Roberts, T. P. Groot, P. J. Walton, D. J. Moon, D. -S. Harrison, F. A. TI Near-infrared counterparts of ultraluminous X-ray sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: black holes; infrared: stars ID NGC 5408 X-1; EXTRAGALACTIC DISTANCE DATABASE; SKY SURVEY 2MASS; MASS BLACK-HOLE; XMM-NEWTON; OPTICAL COUNTERPARTS; CHANDRA OBSERVATIONS; SOURCE POPULATION; HOLMBERG-II; EXTERNAL GALAXIES AB In this paper, we present the results of the first systematic search for counterparts to nearby ultraluminous X-ray sources (ULXs) in the near-infrared (NIR). We observed 62 ULXs in 37 galaxies within 10 Mpc and discovered 17 candidate NIR counterparts. The detection of 17 out of 62 ULX candidates points to intrinsic differences between systems that show and those that do not show infrared emission. For six counterparts, we conclude from the absolute magnitudes and - in some cases - additional information such as morphology and previously reported photometric or spectroscopic observations, that they are likely background active galactic nuclei or ULXs residing in star clusters. 11 counterparts have absolute magnitudes consistent with them being single red supergiant stars. Alternatively, these systems may have larger accretion discs that emit more NIR light than the systems that we do not detect. Other scenarios such as emission from a surrounding nebula or from a compact radio jet are also possible, although for Holmberg II X-1 the NIR luminosity far exceeds the expected jet contribution. The 11 possible red supergiant counterparts are excellent candidates for spectroscopic follow-up observations. This may enable us to measure the mass function in these systems if they are indeed red supergiant donor stars where we can observe absorption lines. C1 [Heida, M.; Jonker, P. G.; Torres, M. A. P.; Kool, E.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Heida, M.; Jonker, P. G.; Groot, P. J.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.; Servillat, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Servillat, M.] Univ Paris Diderot, CEA Saclay, CNRS INSU, Lab AIM,CEA Irfu SAp, F-91191 Gif Sur Yvette, France. [Roberts, T. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Walton, D. J.; Harrison, F. A.] CALTECH, Space Radiat Lab, Pasadena, CA 91125 USA. [Moon, D. -S.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Heida, M (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM m.heida@astro.ru.nl RI Groot, Paul/K-4391-2016 OI Groot, Paul/0000-0002-4488-726X FU STFC consolidated grant [ST/K000861/1]; European Southern Observatory, Chile [089.D-0663(A), 090.D-0417(A)] FX EK thanks Mischa Schirmer for his help with the data-reduction software THELI. We thank the anonymous referee for their comments that helped improve the paper. TPR's contribution to this paper was funded as part of STFC consolidated grant ST/K000861/1. Based on observations collected at the European Southern Observatory, Chile, programmes 089.D-0663(A) and 090.D-0417(A). The William Hershel Telescope is 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. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. NR 103 TC 7 Z9 7 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 2014 VL 442 IS 2 BP 1054 EP 1067 DI 10.1093/mnras/stu928 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8XM UT WOS:000339423100009 ER PT J AU Madej, OK Garcia, J Jonker, PG Parker, ML Ross, R Fabian, AC Chenevez, J AF Madej, O. K. Garcia, J. Jonker, P. G. Parker, M. L. Ross, R. Fabian, A. C. Chenevez, J. TI X-ray reflection in oxygen-rich accretion discs of ultracompact X-ray binaries SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; X-rays: binaries ID SOLAR-SYSTEM ABUNDANCES; 4U 0614+091; BLACK-HOLE; INTERSTELLAR-MEDIUM; SPECTRA; 4U-1543-624; ELEMENTS; STAR; SPECTROSCOPY; LINES AB We present spectroscopic X-ray data of two candidate ultracompact X-ray binaries (UCXBs): 4U 0614+091 and 4U 1543-624. We confirm the presence of a broad O viii Ly alpha reflection line (at a parts per thousand 18 angstrom) using XMM-Newton and Chandra observations obtained in 2012 and 2013. The donor star in these sources is a carbon-oxygen or oxygen-neon-magnesium white dwarf. Hence, the accretion disc is enriched with oxygen which makes the O viii Ly alpha line particularly strong. Modelling the X-ray reflection off a carbon- and oxygen-enriched, hydrogen- and helium-poor disc with models assuming solar composition likely biases several of the best-fitting parameters. In order to describe the X-ray reflection spectra self-consistently, we modify the currently available xillver reflection model. We present initial grids that can be used to model X-ray reflection spectra in UCXBs with carbon-oxygen-rich (and hydrogen- and helium-poor) accretion disc. We find that the new reflection model provides a better overall description of the reflection spectra of 4U 0614+091 and 4U 1543-624 than the reflection models that assume solar abundances. C1 [Madej, O. K.; Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Madej, O. K.; Jonker, P. G.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Garcia, J.; Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parker, M. L.; Fabian, A. C.] Inst Astron, Cambridge CB3 OHA, England. [Ross, R.] Coll Holy Cross, Dept Phys, Worcester, MA 01610 USA. [Chenevez, J.] Tech Univ Denmark, Natl Space Inst, DK-2800 Lyngby, Denmark. RP Madej, OK (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM oliwiamadej@gmail.com FU NASA [NNX11AD08G] FX OKM thanks John Raymond and Ciro Pinto for useful discussions and comments on the paper. JG acknowledges the support of NASA grant NNX11AD08G. NR 32 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 AUG 1 PY 2014 VL 442 IS 2 BP 1157 EP 1165 DI 10.1093/mnras/stu884 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8XM UT WOS:000339423100019 ER PT J AU Wang, WT Sales, LV Henriques, BMB White, SDM AF Wang, Wenting Sales, Laura V. Henriques, Bruno M. B. White, Simon D. M. TI Satellite abundances around bright isolated galaxies - II. Radial distribution and environmental effects SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: haloes; dark matter ID DIGITAL SKY SURVEY; NUMBER DENSITY PROFILES; DARK-MATTER HALOES; QUENCHING TIME-SCALES; STAR-FORMATION; SPATIAL-DISTRIBUTION; REDSHIFT SURVEY; GALACTIC SATELLITES; PHYSICAL-PROPERTIES; INTRACLUSTER LIGHT AB We use the Eighth Data Release of the Sloan Digital Sky Survey (SDSS/DR8) galaxy sample to study the radial distribution of satellite galaxies around isolated primaries, comparing to semi-analytic models of galaxy formation based on the Millennium and Millennium-II simulations. SDSS satellites behave differently around high- and low-mass primaries: those orbiting objects with M-* > 10(11) M-aS (TM) are mostly red and are less concentrated towards their host than the inferred dark matter halo, an effect that is very pronounced for the few blue satellites. On the other hand, less massive primaries have steeper satellite profiles that agree quite well with the expected dark matter distribution and are dominated by blue satellites, even in the inner regions where strong environmental effects are expected. In fact, such effects appear to be strong only for primaries with M-* > 10(11) M-aS (TM). This behaviour is not reproduced by current semi-analytic simulations, where satellite profiles always parallel those of the dark matter and satellite populations are predominantly red for primaries of all masses. The disagreement with SDSS suggests that environmental effects are too efficient in the models. Modifying the treatment of environmental and star formation processes can substantially increase the fraction of blue satellites, but their radial distribution remains significantly shallower than observed. It seems that most satellites of low-mass primaries can continue to form stars even after orbiting within their joint halo for 5 Gyr or more. C1 [Wang, Wenting; Sales, Laura V.; Henriques, Bruno M. B.; White, Simon D. M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Wang, Wenting] Chinese Acad Sci, Max Panck Inst Partner Grp, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Wang, Wenting] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Sales, Laura V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wang, WT (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM bilinxing.wenting@gmail.com RI he, shuyi/K-2082-2014; OI Henriques, Bruno/0000-0002-1392-489X FU NSFC [11121062, 10878001, 11033006, 11003035]; CAS/SAFEA International Partnership Program for Creative Research Teams [KJCX2-YW-T23]; Science and Technology Facilities Council [ST/F001166/1]; Marie Curie RTN CosmoComp; ERC [246797 GALFORMOD] FX WW is partially supported by NSFC (11121062, 10878001, 11033006, 11003035), and by the CAS/SAFEA International Partnership Program for Creative Research Teams (KJCX2-YW-T23) and by the Science and Technology Facilities Council (ST/F001166/1). LS was supported in part by the Marie Curie RTN CosmoComp. BH and SW were supported by ERC Advanced Grant 246797 GALFORMOD. WW is grateful for useful discussions with Yipeng Jing about the underlying methodology, sample selection and survey geometry. NR 81 TC 35 Z9 35 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 2014 VL 442 IS 2 BP 1363 EP 1378 DI 10.1093/mnras/stu988 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL8XM UT WOS:000339423100034 ER PT J AU Ostrom, PH Wiley, AE Rossman, S Stricker, CA James, HF AF Ostrom, Peggy H. Wiley, Anne E. Rossman, Sam Stricker, Craig A. James, Helen F. TI Unexpected hydrogen isotope variation in oceanic pelagic seabirds SO OECOLOGIA LA English DT Article DE Hydrogen isotope; Seabird; Salt gland; Salt load; Diet analysis ID COMPLEX ORGANIC MATERIALS; STABLE-ISOTOPES; FOOD WEBS; NONEXCHANGEABLE HYDROGEN; DELTA-D; COMPARATIVE EQUILIBRATION; TROPHIC RELATIONSHIPS; MASS-SPECTROMETRY; MIGRATORY BIRDS; ANIMAL-TISSUES AB Hydrogen isotopes have significantly enhanced our understanding of the biogeography of migratory animals. The basis for this methodology lies in predictable, continental patterns of precipitation delta D values that are often reflected in an organism's tissues. delta D variation is not expected for oceanic pelagic organisms whose dietary hydrogen (water and organic hydrogen in prey) is transferred up the food web from an isotopically homogeneous water source. We report a 142 aEuro degrees range in the delta D values of flight feathers from the Hawaiian petrel (Pterodroma sandwichensis), an oceanic pelagic North Pacific species, and inquire about the source of that variation. We show delta D variation between and within four other oceanic pelagic species: Newell's shearwater (Puffinus auricularis newellii), Black-footed albatross (Phoebastria nigripes), Laysan albatross (Phoebastria immutabilis) and Buller's shearwater (Puffinus bulleri). The similarity between muscle delta D values of hatch-year Hawaiian petrels and their prey suggests that trophic fractionation does not influence delta D values of muscle. We hypothesize that isotopic discrimination is associated with water loss during salt excretion through salt glands. Salt load differs between seabirds that consume isosmotic squid and crustaceans and those that feed on hyposmotic teleost fish. In support of the salt gland hypothesis, we show an inverse relationship between delta D and percent teleost fish in diet for three seabird species. Our results demonstrate the utility of delta D in the study of oceanic consumers, while also contributing to a better understanding of delta D systematics, the basis for one of the most commonly utilized isotope tools in avian ecology. C1 [Ostrom, Peggy H.; Wiley, Anne E.; Rossman, Sam] Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. [Wiley, Anne E.; James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Wiley, Anne E.] Univ Akron, Dept Biol, Akron, OH 44325 USA. [Stricker, Craig A.] US Geol Survey, Ft Collins Sci Ctr, Denver, CO 80225 USA. RP Ostrom, PH (reprint author), Michigan State Univ, Dept Zool, 203 Nat Sci Bldg, E Lansing, MI 48824 USA. EM ostrom@msu.edu FU National Science Foundation [DEB-0745604, DEB-0940338]; Graduate School of Michigan State University; Department of Zoology of Michigan State University FX We thank Robert Faucett of the Burke Museum for supplying feather samples of Buller's shearwater and Black-footed albatross. We also thank Cayce Gulbransen of the US Geological Survey for making hydrogen isotope measurements. Funding for this work was generously provided by the National Science Foundation (DEB-0745604 and DEB-0940338). Graduate student travel (A. Wiley) was supported, in part, by the Graduate School and Department of Zoology of Michigan State University. The use of any trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the US government. NR 58 TC 3 Z9 3 U1 4 U2 44 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD AUG PY 2014 VL 175 IS 4 BP 1227 EP 1235 DI 10.1007/s00442-014-2985-8 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AM5JM UT WOS:000339893600017 PM 24989118 ER PT J AU Wojdak, JM Touchon, JC Hite, JL Meyer, B Vonesh, JR AF Wojdak, Jeremy M. Touchon, Justin C. Hite, Jessica L. Meyer, Beth Vonesh, James R. TI Consequences of induced hatching plasticity depend on predator community SO OECOLOGIA LA English DT Article DE Predator diversity; Hatching; Complex life cycles; Agalychnis callidryas; Life history plasticity ID RED-EYED TREEFROG; CATCH-UP GROWTH; COMPENSATORY GROWTH; TRADE-OFFS; AMPHIBIAN METAMORPHOSIS; ADAPTIVE PLASTICITY; FUNCTIONAL-RESPONSE; TIME CONSTRAINTS; TROPHIC CASCADES; SIZE AB Many prey species face trade-offs in the timing of life history switch points like hatching and metamorphosis. Costs associated with transitioning early depend on the biotic and abiotic conditions found in the subsequent life stage. The red-eyed treefrog, Agalychnis callidryas, faces risks from predators in multiple, successive life stages, and can hatch early in response to mortality threats at the egg stage. Here we tested how the consequences of life history plasticity, specifically early hatching in response to terrestrial egg predators, depend on the assemblage of aquatic larval predators. We predicted that diverse predator assemblages would impose lower total predation pressure than the most effective single predator species and might thereby reduce the costs of hatching early. We then conducted a mesocosm experiment where we crossed hatchling phenotype (early vs. normal hatching) with five larval-predator environments (no predators, either waterbugs, dragonflies, or mosquitofish singly, or all three predator species together). The consequences of hatching early varied across predator treatments, and tended to disappear through time in some predation treatments, notably the waterbug and diverse predator assemblages. We demonstrate that the fitness costs of life history plasticity in an early life stage depend critically on the predator community composition in the next stage. C1 [Wojdak, Jeremy M.; Meyer, Beth] Radford Univ, Dept Biol, Radford, VA 24142 USA. [Touchon, Justin C.; Hite, Jessica L.; Vonesh, James R.] Smithsonian Trop Res Inst, Unit 9100, Miami, FL 34002 USA. [Hite, Jessica L.; Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [Hite, Jessica L.] Indiana Univ, Dept Biol, Bloomington, IN 47405 USA. RP Wojdak, JM (reprint author), Radford Univ, Dept Biol, POB 6931, Radford, VA 24142 USA. EM jmwojdak@radford.edu RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU Research Opportunity Award from the National Science Foundation, stemming from NSF [0717220]; NSF [IIA-1064566]; Virginia Commonwealth University; Radford University; Smithsonian Tropical Research Institute FX We thank the Autoridad Nacional del Ambiente de Panama for permission to conduct this research (permit SC/A-73-09). We would like to thank M. Hughey, K. Warkentin, and M. McCoy for their advice and assistance. L. Belden, as well as the reviewers and editors, made helpful suggestions to improve the manuscript. J. M. W. and B. M. were supported by a Research Opportunity Award from the National Science Foundation, stemming from NSF grant 0717220 to J. R. V; J. C. T. was supported by NSF grant IIA-1064566. Virginia Commonwealth University, Radford University, and the Smithsonian Tropical Research Institute also provided funding or support. NR 66 TC 2 Z9 2 U1 2 U2 32 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD AUG PY 2014 VL 175 IS 4 BP 1267 EP 1276 DI 10.1007/s00442-014-2962-2 PG 10 WC Ecology SC Environmental Sciences & Ecology GA AM5JM UT WOS:000339893600021 PM 24844644 ER PT J AU Shen, Y Santiago, LS Shen, H Ma, L Lian, JY Cao, HL Lu, HP Ye, WH AF Shen, Yong Santiago, Louis S. Shen, Hao Ma, Lei Lian, Juyu Cao, Honglin Lu, Huanping Ye, Wanhui TI Determinants of change in subtropical tree diameter growth with ontogenetic stage SO OECOLOGIA LA English DT Article DE Relative growth rate; Soil nutrient availability; Specific leaf area; Topography; Wood density ID LOWLAND TROPICAL FOREST; FUNCTIONAL DIVERSITY PATTERNS; BORNEAN RAIN-FOREST; HABITAT ASSOCIATIONS; PRECIPITATION GRADIENT; DEMOGRAPHIC RATES; NEOTROPICAL TREE; CANOPY TREES; TRAITS; MORTALITY AB We evaluated the degree to which relative growth rate (RGR) of saplings and large trees is related to seven functional traits that describe physiological behavior and soil environmental factors related to topography and fertility for 57 subtropical tree species in Dinghushan, China. The mean values of functional traits and soil environmental factors for each species that were related to RGR varied with ontogenetic stage. Sapling RGR showed greater relationships with functional traits than large-tree RGR, whereas large-tree RGR was more associated with soil environment than was sapling RGR. The strongest single predictors of RGR were wood density for saplings and slope aspect for large trees. The stepwise regression model for large trees accounted for a larger proportion of variability (R (2) = 0.95) in RGR than the model for saplings (R (2) = 0.55). Functional diversity analysis revealed that the process of habitat filtering likely contributes to the substantial changes in regulation of RGR as communities transition from saplings to large trees. C1 [Shen, Yong; Shen, Hao; Ma, Lei; Lian, Juyu; Cao, Honglin; Lu, Huanping; Ye, Wanhui] Chinese Acad Sci, South China Bot Garden, Key Lab Vegetat Restorat & Management Degraded Ec, Guangzhou 510650, Guangdong, Peoples R China. [Shen, Yong; Ma, Lei; Lu, Huanping] Univ Chinese Acad Sci, Beijing 10049, Peoples R China. [Santiago, Louis S.] Univ Calif Riverside, Bot & Plant Sci Dept, Riverside, CA 92521 USA. [Santiago, Louis S.] Smithsonian Trop Res Inst Balboa, Panama City, Panama. RP Ye, WH (reprint author), Chinese Acad Sci, South China Bot Garden, Key Lab Vegetat Restorat & Management Degraded Ec, Guangzhou 510650, Guangdong, Peoples R China. EM why@scib.ac.cn RI Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 FU National Natural Science Foundation of China [31370446, 31100312]; Knowledge Innovation Project of The Chinese Academy of Sciences [KSCX2-EW-Z]; Foreign Exchange Program National Founder [31011120470]; Chinese Forest Biodiversity Monitoring Network; China Scholarship Council FX We thank Prof. Bai-lian Li for establishing collaborations between the University of California Riverside and the South China Botanical Garden; numerous individuals in South China Botanical Garden who contributed to the field survey of Dinghushan plot; and the Santiago Lab for comments that improved the manuscript. The study was funded by the National Natural Science Foundation of China (31370446, 31100312), the Knowledge Innovation Project of The Chinese Academy of Sciences (KSCX2-EW-Z), the Foreign Exchange Program National Founder (31011120470), the Chinese Forest Biodiversity Monitoring Network and the China Scholarship Council. NR 66 TC 5 Z9 5 U1 5 U2 31 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD AUG PY 2014 VL 175 IS 4 BP 1315 EP 1324 DI 10.1007/s00442-014-2981-z PG 10 WC Ecology SC Environmental Sciences & Ecology GA AM5JM UT WOS:000339893600025 PM 24938832 ER PT J AU Zwintz, K Fossati, L Ryabchikova, T Guenther, D Aerts, C Barnes, TG Themessl, N Lorenz, D Cameron, C Kuschnig, R Pollack-Drs, S Moravveji, E Baglin, A Matthews, JM Moffat, AFJ Poretti, E Rainer, M Rucinski, SM Sasselov, D Weiss, WW AF Zwintz, K. Fossati, L. Ryabchikova, T. Guenther, D. Aerts, C. Barnes, T. G. Themessl, N. Lorenz, D. Cameron, C. Kuschnig, R. Pollack-Drs, S. Moravveji, E. Baglin, A. Matthews, J. M. Moffat, A. F. J. Poretti, E. Rainer, M. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI Echography of young stars reveals their evolution SO SCIENCE LA English DT Article ID MAIN-SEQUENCE STARS; INSTABILITY STRIP; MASS STARS; BIRTHLINE; NGC-2264 AB We demonstrate that a seismic analysis of stars in their earliest evolutionary phases is a powerful method with which to identify young stars and distinguish their evolutionary states. The early star that is born from the gravitational collapse of a molecular cloud reaches at some point sufficient temperature, mass, and luminosity to be detected. Accretion stops, and the pre-main sequence star that emerges is nearly fully convective and chemically homogeneous. It will continue to contract gravitationally until the density and temperature in the core are high enough to start nuclear burning of hydrogen. We show that there is a relationship for a sample of young stars between detected pulsation properties and their evolutionary status, illustrating the potential of asteroseismology for the early evolutionary phases. C1 [Zwintz, K.; Aerts, C.; Moravveji, E.] KU, Inst Sterrenkunde, B-3001 Leuven, Belgium. [Fossati, L.] Bond Univ, Argelander Inst Astron, D-53121 Bonn, Germany. [Ryabchikova, T.] Russian Acad Sci, Inst Astron, Moscow 109017, Russia. [Guenther, D.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Aerts, C.] Radboud Univ Nijmegen, Dept Astrophys, Inst Math Astrophys & Particle Phys, NL-6500 GL Nijmegen, Netherlands. [Barnes, T. G.] Univ Texas Austin, McDonald Observ, Mcdonald Observ, TX 79734 USA. [Themessl, N.; Lorenz, D.; Kuschnig, R.; Pollack-Drs, S.; Weiss, W. W.] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Cameron, C.] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Canada. [Baglin, A.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophy, F-92195 Meudon, France. [Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Poretti, E.; Rainer, M.] Osserv Astron Brera, Ist Nazl Astrofis, I-23807 Merate, Italy. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zwintz, K (reprint author), KU, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Leuven, Belgium. EM konstanze.zwintz@ster.kuleuven.be OI Zwintz, Konstanze/0000-0001-9229-8315; Poretti, Ennio/0000-0003-1200-0473 FU European Research Council (ERC) under the European Community/ERC [227224]; Research Council of the KU Leuven [GOA/2013/012]; Fund for Scientific Research of Flanders (FWO), Belgium [G.0B69.13]; Presidium RAS Program "Nonstationary Phenomena in Objects of the Universe"; Natural Sciences and Engineering Research Council (NSERC) of Canada; Austrian Fonds zur Forderung der wissenschaftlichen Forschung [P22691-N16]; Austrian Research Promotion Agency-ALR; FP7 project "SPACEINN: Exploitation of Space Data for Innovative Helio-and Asteroseismology"; Belgian Federal Science Policy Office by the Marie Curie Actions from the European Commission [246540]; Canadian Space Agency; Funds for Scientific Research of Flanders (FWO), Belgium; Research Council of KU Leuven, Belgium; Fonds National Recherches Scientific (FNRS), Belgium; Royal Observatory of Belgium; Observatoire de Geneve, Switzerland; Thuringer Landessternwarte Tautenburg, Germany; ESO Large Programme [LP185.D-0056] FX Data obtained with the MOST satellite are available through the MOST Public Data Archive (http://most.astro.ubc.ca//archive.html), and data from CoRoT are available in the CoRoT Archive (http://idoc-corot.ias.u-psud.fr/index.jsp). Spectroscopic data can be obtained at the European Southern Observatory (ESO) archive (http://archive.eso.org) and the Canada-France-Hawaii Telescope (CFHT) archive (http://www3.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/en/cfht). Data are also available from the public Web site: www.ster.kuleuven.be/similar to konstanze/science. We are grateful to the MOST and CoRoT teams for making this work possible. We thank N. Piskunov for his advice on the best usage of the SME software. The research leading to these results has received funding from the European Research Council (ERC) under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement 227224 (PROSPERITY), from the Research Council of the KU Leuven under grant agreement GOA/2013/012, and from the Fund for Scientific Research of Flanders (FWO), Belgium, under grant agreement G.0B69.13. T. R. acknowledges partial financial support from the Presidium RAS Program "Nonstationary Phenomena in Objects of the Universe." D. G., J.M.M., A. F. J.M., and S. M. R. acknowledge the funding support of the Natural Sciences and Engineering Research Council (NSERC) of Canada. R. K. and W. W. W. are supported by the Austrian Fonds zur Forderung der wissenschaftlichen Forschung (P22691-N16) and by the Austrian Research Promotion Agency-ALR. E. P. and M. R. acknowledge financial support from the FP7 project "SPACEINN: Exploitation of Space Data for Innovative Helio-and Asteroseismology." E. M. is beneficiary of a postdoctoral grant from the Belgian Federal Science Policy Office cofunded by the Marie Curie Actions FP7-PEOPLE-COFUND2008 n246540 Mobility Grant from the European Commission. C. C. was supported by the Canadian Space Agency. E. M. is the beneficiary of a postdoctoral grant from the Belgian Federal Science Policy Office cofunded by the Marie Curie Actions FP7-PEOPLE-COFUND2008 n246540 Mobility Grant from the European Commission. Spectroscopic data were obtained with the 2.7-m telescope at McDonald Observatory, Texas; the 3.6m-telescope at La Silla Observatory under the ESO Large Programme LP185.D-0056; the CFHT (proposal CFHT2012AC003); the Cerro Tololo Inter-American Observatory 1.5-m telescope; and the Mercator Telescope (operated on the island of La Palma by the Flemish Community, at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias) with the HERMES spectrograph, which is supported by the Funds for Scientific Research of Flanders (FWO), Belgium; the Research Council of KU Leuven, Belgium; the Fonds National Recherches Scientific (FNRS), Belgium; the Royal Observatory of Belgium, the Observatoire de Geneve, Switzerland; and the Thuringer Landessternwarte Tautenburg, Germany. NR 20 TC 12 Z9 12 U1 0 U2 10 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 1 PY 2014 VL 345 IS 6196 BP 550 EP 553 DI 10.1126/science.1253645 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM2AU UT WOS:000339651300042 PM 24993346 ER PT J AU Baskin, A Sadeghpour, HR Kral, P AF Baskin, Artem Sadeghpour, Hossein R. Kral, Petr TI Correlated Diskoid-like Electronic States SO SCIENTIFIC REPORTS LA English DT Article ID IMAGE-POTENTIAL STATES; 2 INTERACTING ELECTRONS; CONFINED HYDROGEN-ATOM; RYDBERG BLOCKADE; CONDUCTING DISK; HELIUM; MOLECULES; COLLAPSE; PHOTON; CAVITY AB We study highly excited diskoid-like electronic states formed in the vicinity of charged and strongly polarizable diskotic nanostructures, such as circular graphene flakes. First, we study the nature of such extended states in a simple two-electron model. The two electrons are attached to a point-like nucleus with a charge 2+, where the material electron is forced to move within a 2D disk area centered at the nucleus, while the extended electron is free to move in 3D. Pronounced and complex correlations are revealed in the diskoid-like states. We also develop semiclassical one-electron models of such diskotic systems and explain how the one-electron and many-electron solutions are related. C1 [Baskin, Artem; Kral, Petr] Univ Illinois, Dept Chem, Chicago, IL 60607 USA. [Sadeghpour, Hossein R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Kral, Petr] Univ Illinois, Dept Phys, Chicago, IL 60607 USA. RP Kral, P (reprint author), Univ Illinois, Dept Chem, Chicago, IL 60607 USA. EM pkral@uic.edu FU ACS PRF [53062-ND6]; Herbert E. Paaren Graduate Fellowship; ITAMP, Harvard-Smythsonian Astrophysical Laboratory; University of Illinois at Chicago FX This work was supported by the ACS PRF grant #53062-ND6. A.B. acknowledges the generous support obtained from the Herbert E. Paaren Graduate Fellowship and ITAMP, Harvard-Smythsonian Astrophysical Laboratory. The publication was supported by the Research Open Access Article Publishing (ROAAP) Fund of the University of Illinois at Chicago. NR 43 TC 1 Z9 1 U1 2 U2 12 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 1 PY 2014 VL 4 AR 5913 DI 10.1038/srep05913 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM5ZV UT WOS:000339940900007 PM 25081595 ER PT J AU Jordan, A Brahm, R Bakos, GA Bayliss, D Penev, K Hartman, JD Zhou, G Mancini, L Mohler-Fischer, M Ciceri, S Sato, B Csubry, Z Rabus, M Suc, V Espinoza, N Bhatti, W Borro, MD Buchhave, L Csak, B Henning, T Schmidt, B Tan, TG Noyes, RW Beky, B Butler, RP Shectman, S Crane, J Thompson, I Williams, A Martin, R Contreras, C Lazar, J Papp, I Sari, P AF Jordan, Andres Brahm, Rafael Bakos, G. A. Bayliss, D. Penev, K. Hartman, J. D. Zhou, G. Mancini, L. Mohler-Fischer, M. Ciceri, S. Sato, B. Csubry, Z. Rabus, M. Suc, V. Espinoza, N. Bhatti, W. Borro, M. de Val Buchhave, L. Csak, B. Henning, T. Schmidt, B. Tan, T. G. Noyes, R. W. Beky, B. Butler, R. P. Shectman, S. Crane, J. Thompson, I. Williams, A. Martin, R. Contreras, C. Lazar, J. Papp, I. Sari, P. TI HATS-4b: A DENSE HOT JUPITER TRANSITING A SUPER METAL-RICH G STAR SO ASTRONOMICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HATS-4, GSC 6505-00217); techniques: photometric; techniques: spectroscopic ID RADIAL-VELOCITY MEASUREMENTS; HATSOUTH SURVEY; EXTRASOLAR PLANETS; GIANT PLANETS; LIGHT CURVES; MASS STARS; STELLAR; SPECTROGRAPH; SATURN; SOLAR AB We report the discovery by the HATSouth survey of HATS-4b, an extrasolar planet transiting a V = 13.46 mag G star. HATS-4b has a period of P approximate to 2.5167 days, mass of M-p approximate to 1.32 M-Jup, radius of R-p approximate to 1.02 R-Jup, and density of rho(p) = 1.55 +/- 0.16 g cm(-3) approximate to 1.24 rho(Jup). The host star has a mass of 1.00 M-circle dot, a radius of 0.92 R-circle dot, and a very high metallicity [Fe/H]= 0.43 +/- 0.08. HATS-4b is among the densest known planets with masses between 1 and 2 M-J and is thus likely to have a significant content of heavy elements of the order of 75 M-circle plus. In this paper we present the data reduction, radial velocity measurements, and stellar classification techniques adopted by the HATSouth survey for the CORALIE spectrograph. We also detail a technique for simultaneously estimating nu sin i and macroturbulence using high resolution spectra. C1 [Jordan, Andres; Brahm, Rafael; Rabus, M.; Suc, V.; Espinoza, N.] Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Santiago 7820436, Chile. [Jordan, Andres; Brahm, Rafael; Espinoza, N.] Millennium Inst Astrophys, Santiago 7820436, Chile. [Bakos, G. A.; Penev, K.; Hartman, J. D.; Csubry, Z.; Bhatti, W.; Borro, M. de Val] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bayliss, D.; Zhou, G.; Schmidt, B.] Australian Natl Univ, Canberra, ACT, Australia. [Mancini, L.; Mohler-Fischer, M.; Ciceri, S.; Csak, B.; Henning, T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Sato, B.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Buchhave, L.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Buchhave, L.; Noyes, R. W.; Beky, B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tan, T. G.] Perth Exoplanet Survey Telescope, Perth, WA, Australia. [Butler, R. 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. [Williams, A.; Martin, R.] Perth Observ, Perth, WA 6076, Australia. [Contreras, C.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Lazar, J.; Papp, I.; Sari, P.] Hungarian Astron Assoc, Budapest, Hungary. RP Jordan, A (reprint author), Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago 7820436, Chile. RI Butler, Robert/B-1125-2009; Williams, Andrew/K-2931-2013; OI Williams, Andrew/0000-0001-9080-0105; Penev, Kaloyan/0000-0003-4464-1371; Schmidt, Brian/0000-0001-6589-1287; Buchhave, Lars A./0000-0003-1605-5666; Tan, Thiam-Guan/0000-0001-5603-6895; Hartman, Joel/0000-0001-8732-6166 FU NSF MRI [NSF/AST-0723074]; NASA [NNX09AB29G, NNX12AH91H]; FONDECYT [1130857, 3120097]; BASAL CATA [PFB-06]; Millennium Institute of Astrophysics (MAS) [IC120009]; Millennium Science Initiative, Chilean Ministry of Economy [P10-022-F]; CONICYT-PCHA/Doctorado Nacional; National Collaborative Research Infrastructure Strategy of the Australian Federal Government; CNTAC [CN2012A-62]; Swope telescope in Las Campanas Observatory [CN2013A-171]; ARC Laureate Fellowship [FL0992131]; Robert Martin Ayers Sciences Fund; NASA's Astrophysics Data System Bibliographic Services; SIMBAD; [NSF/AST-1108686] FX A.J. thanks Didier Queloz for discussions that provided important insights on the measurement of precision radial velocities with CORALIE. A.J. also enjoyed many useful discussions on the topic of radial velocity measurements with James Jenkins. 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 projects IC120009 "Millennium Institute of Astrophysics(MAS)" and P10-022-F of the Millennium Science Initiative, Chilean Ministry of Economy. R.B. and N.E. are supported by CONICYT-PCHA/Doctorado Nacional. R.B. acknowledges additional support from Nucleus P10-022-F of the Millennium Science Initiative, Chilean Ministry of Economy. V.S. acknowledges support form BASAL CATA PFB-06. M. R. acknowledges support from FONDECYT postdoctoral fellowship 3120097. This work is based on observations made with ESO telescopes at the La Silla Observatory under program IDs 089.C-0440(A), 090.D-0061(A), and 090.A-9012(A). Australian access to the Magellan Telescopes was supported through the National Collaborative Research Infrastructure Strategy of the Australian Federal Government. This paper also uses observations obtained with facilities of the Las Cumbres Observatory Global Telescope, with the Euler telescope in La Silla through time awarded by the CNTAC under program CN2012A-62 and with the Swope telescope in Las Campanas Observatory through time awarded under program CN2013A-171. 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, NASA's Astrophysics Data System Bibliographic Services, and the SIMBAD database, 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. We thank Timo Anguita and Regis Lachaume for their technical assistance during the observations at the MPG/ESO 2.2 m Telescope. NR 50 TC 24 Z9 24 U1 2 U2 8 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 2014 VL 148 IS 2 AR 29 DI 10.1088/0004-6256/148/2/29 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL7OQ UT WOS:000339324400005 ER PT J AU Milliman, KE Mathieu, RD Geller, AM Gosnell, NM Meibom, S Platais, I AF Milliman, Katelyn E. Mathieu, Robert D. Geller, Aaron M. Gosnell, Natalie M. Meibom, Soren Platais, Imants TI WIYN OPEN CLUSTER STUDY. LX. SPECTROSCOPIC BINARY ORBITS IN NGC 6819 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: spectroscopic; blue stragglers; open clusters and associations: individual (NGC 6819) ID STELLAR RADIAL-VELOCITIES; ECLIPSING BINARY; BLUE STRAGGLERS; KEPLER PHOTOMETRY; VARIABLE-STARS; CCD PHOTOMETRY; MASS-TRANSFER; RED GIANT; FIELD; POPULATIONS AB We present the current state of the WOCS radial-velocity (RV) survey for the rich open cluster NGC 6819 (2.5 Gyr) including 93 spectroscopic binary orbits with periods ranging from 1.5 to 8000 days. These results are the product of our ongoing RV survey of NGC 6819 using the Hydra Multi-Object Spectrograph on the WIYN 3.5 m telescope. We also include a detailed analysis of multiple prior sets of optical photometry for NGC 6819. Within a 1 degrees field of view, our stellar sample includes the giant branch, the red clump, and blue straggler candidates, and extends to almost 2 mag below the main sequence (MS) turnoff. For each star observed in our survey we present all RV measurements, the average RV, and velocity variability information. Additionally, we discuss notable binaries from our sample, including eclipsing binaries (WOCS 23009, WOCS 24009, and WOCS 40007), stars noted in Kepler asteroseismology studies (WOCS 4008, WOCS 7009, and WOCS 8007), and potential descendants of past blue stragglers (WOCS 1006 and WOCS 6002). We find the incompleteness-corrected binary fraction for all MS binaries with periods less than 10(4) days to be 22% +/- 3% and a tidal circularization period of 6.2(-1.1)(+1.1) days for NGC 6819. C1 [Milliman, Katelyn E.; Mathieu, Robert D.; Gosnell, Natalie M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Geller, Aaron M.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Geller, Aaron M.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Geller, Aaron M.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Platais, Imants] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Milliman, KE (reprint author), Univ Wisconsin, Dept Astron, 475 North Charter St, Madison, WI 53706 USA. EM milliman@astro.wisc.edu FU National Science Foundation [AST-0908082]; National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302765]; National Space Grant College and Fellowship Program; Wisconsin Space Grant Consortium FX The authors express their gratitude to the WIYN Observatory staff for the many long nights and excellent spectra. Also, we would like to thank the many undergraduate and graduate students who helped obtain and reduce the many hours of WIYN data that underlie this paper, including E. Braden, T. Hole, E. Leiner, and B. Tofflemire. This work was funded by the National Science Foundation grant AST-0908082 to the University of Wisconsin-Madison. A.M.G. is funded by a National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under Award No. AST-1302765. K.E.M. is supported in part by the National Space Grant College and Fellowship Program and the Wisconsin Space Grant Consortium. NR 43 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD AUG PY 2014 VL 148 IS 2 AR 38 DI 10.1088/0004-6256/148/2/38 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL7OQ UT WOS:000339324400014 ER PT J AU Archer, A Barnacka, A Beilicke, M Benbow, W Berger, K Bird, R Biteau, J Buckley, JH Bugaev, V Byrum, K Cardenzana, JV Cerruti, M Chen, W Chen, X Ciupik, L Connolly, MP Cui, W Dickinson, HJ Dumm, J Eisch, JD Falcone, A Federici, S Feng, Q Finley, JP Fleischhack, H Fortson, L Furniss, A Galante, N Griffin, S Griffiths, ST Grube, J Gyuk, G Hakansson, N Hanna, D Holder, J Hughes, G Johnson, CA Kaaret, P Kar, P Kertzman, M Khassen, Y Kieda, D Krawczynski, H Kumar, S Lang, MJ Maier, G McArthur, S McCann, A Meagher, K Moriarty, P Mukherjee, R Nieto, D de Bhroithe, AO Ong, RA Otte, AN Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Pueschel, E Quinn, J Ragan, K Rajotte, J Reyes, LC Reynolds, PT Richards, GT Roache, E 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 Zajczyk, A Zitzer, B AF Archer, A. Barnacka, A. Beilicke, M. Benbow, W. Berger, K. Bird, R. Biteau, J. Buckley, J. H. Bugaev, V. Byrum, K. Cardenzana, J. V. Cerruti, M. Chen, W. Chen, X. Ciupik, L. Connolly, M. P. Cui, W. Dickinson, H. J. Dumm, J. Eisch, J. D. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Fleischhack, H. Fortson, L. Furniss, A. Galante, N. Griffin, S. Griffiths, S. T. Grube, J. Gyuk, G. Hakansson, N. Hanna, D. Holder, J. Hughes, G. Johnson, C. A. Kaaret, P. Kar, P. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Kumar, S. Lang, M. J. Maier, G. McArthur, S. McCann, A. Meagher, K. Moriarty, P. Mukherjee, R. Nieto, D. de Bhroithe, A. O'Faolain Ong, R. A. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Pueschel, E. Quinn, J. Ragan, K. Rajotte, J. Reyes, L. C. Reynolds, P. T. Richards, G. T. Roache, E. 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. Zajczyk, A. Zitzer, B. TI VERY-HIGH ENERGY OBSERVATIONS OF THE GALACTIC CENTER REGION BY VERITAS IN 2010-2012 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astroparticle physics; black hole physics; Galaxy: center; gamma rays: galaxies; methods: data analysis; radiation mechanisms: non-thermal ID SGR-A-ASTERISK; GAMMA-RAY SOURCE; MOLECULAR CLOUDS; MAGIC TELESCOPE; SOURCE CATALOG; DARK-MATTER; CRAB-NEBULA; EMISSION; VARIABILITY; DISCOVERY AB The Galactic center is an interesting region for high-energy (0.1-100 GeV) and very-high-energy (E > 100 GeV) gamma-ray observations. Potential sources of GeV/TeV gamma-ray emission have been suggested, e.g., the accretion of matter onto the supermassive black hole, cosmic rays from a nearby supernova remnant (e.g., Sgr A East), particle acceleration in a plerion, or the annihilation of dark matter particles. The Galactic center has been detected by EGRET and by Fermi/LAT in the MeV/GeV energy band. At TeV energies, the Galactic center was detected with moderate significance by the CANGAROO and Whipple 10 m telescopes and with high significance by H.E.S.S., MAGIC, and VERITAS. We present the results from three years of VERITAS observations conducted at large zenith angles resulting in a detection of the Galactic center on the level of 18 standard deviations at energies above similar to 2.5 TeV. The energy spectrum is derived and is found to be compatible with hadronic, leptonic, and hybrid emission models discussed in the literature. Future, more detailed measurements of the high-energy cutoff and better constraints on the high-energy flux variability will help to refine and/or disentangle the individual models. C1 [Archer, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Chen, W.; Krawczynski, H.; Zajczyk, A.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Barnacka, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Benbow, W.; Cerruti, M.; Galante, N.; Roache, E.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Berger, K.; Holder, J.; Kumar, S.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bird, R.; Khassen, Y.; Pueschel, E.; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin, 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. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cardenzana, J. V.; Dickinson, H. J.; Eisch, J. D.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Chen, X.; Federici, S.; Hakansson, N.; Pohl, M.; Telezhinsky, I.; Wilhelm, A.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Chen, X.; Federici, S.; Fleischhack, H.; Hughes, G.; 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.; 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. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Griffin, S.; Hanna, D.; Ragan, K.; Rajotte, J.; Staszak, D.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Griffiths, S. T.; Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 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. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Nieto, D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Ong, R. A.; Popkow, A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 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 Phys & Instrumentat, Bishopstown, Cork, Ireland. RP Archer, A (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. EM beilicke@physics.wustl.edu RI Khassen, Yerbol/I-3806-2015; Nieto, Daniel/J-7250-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Nieto, Daniel/0000-0003-3343-0755; Pueschel, Elisa/0000-0002-0529-1973; Cui, Wei/0000-0002-6324-5772; Barnacka, Anna/0000-0001-5655-4158; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 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 UK FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, 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. NR 61 TC 6 Z9 6 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 AUG 1 PY 2014 VL 790 IS 2 AR 149 DI 10.1088/0004-637X/790/2/149 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800066 ER PT J AU Barnacka, A Bottcher, M Sushch, I AF Barnacka, Anna Boettcher, Markus Sushch, Iurii TI HOW GRAVITATIONAL LENSING HELPS gamma-RAY PHOTONS AVOID gamma-gamma ABSORPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gravitational lensing: micro; gravitational lensing: strong ID EXTRAGALACTIC BACKGROUND LIGHT; INDUCED PAIR CASCADES; RADIATION-FIELDS; OPTICAL DEPTH; BLAZARS; UNIVERSE; SPECTRA; OPACITY; SYSTEM; DUST AB We investigate potential gamma - gamma absorption of gamma-ray emission from blazars arising from inhomogeneities along the line of sight, beyond the diffuse Extragalactic Background Light (EBL). As plausible sources of excess gamma - gamma opacity, we consider (1) foreground galaxies, including cases in which this configuration leads to strong gravitational lensing, (2) individual stars within these foreground galaxies, and (3) individual stars within our own galaxy, which may act as lenses for microlensing events. We found that intervening galaxies close to the line of sight are unlikely to lead to significant excess gamma - gamma absorption. This opens up the prospect of detecting lensed gamma-ray blazars at energies above 10 GeV with their gamma-ray spectra effectively only affected by the EBL. The most luminous stars located either in intervening galaxies or in our galaxy provide an environment in which these gamma-rays could, in principle, be significantly absorbed. However, despite a large microlensing probability due to stars located in intervening galaxies, gamma-rays avoid absorption by being deflected by the gravitational potentials of such intervening stars to projected distances ("impact parameters") where the resulting gamma - gamma opacities are negligible. Thus, neither of the intervening excess photon fields considered here, provide a substantial source of excess gamma - gamma opacity beyond the EBL, even in the case of very close alignments between the background blazar and a foreground star or galaxy. C1 [Barnacka, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barnacka, Anna] Jagiellonian Univ, Astron Observ, Krakow, Poland. [Boettcher, Markus; Sushch, Iurii] North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa. [Boettcher, Markus] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Sushch, Iurii] Ivan Franko Natl Univ Lviv, Astron Observ, UA-79005 Lvov, Ukraine. RP Barnacka, A (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM abarnacka@cfa.harvard.edu; Markus.Bottcher@nwu.ac.za OI Barnacka, Anna/0000-0001-5655-4158 FU Department of Energy Office of Science, NASA; Smithsonian Astrophysical Observatory; NCN [DEC-2011/01/M/ST9/01891]; South African Research Chair Initiative (SARChI) by the National Research Foundation; Department of Science and Technology of South Africa, under SARChI Chair [64789] FX The work of A.B. is supported by the Department of Energy Office of Science, NASA, and the Smithsonian Astrophysical Observatory, and financial support by the NCN grant DEC-2011/01/M/ST9/01891 is acknowledged. The work of M. B. is supported through the South African Research Chair Initiative (SARChI) by the National Research Foundation and the Department of Science and Technology of South Africa, under SARChI Chair grant No. 64789. NR 33 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2014 VL 790 IS 2 AR 147 DI 10.1088/0004-637X/790/2/147 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800064 ER PT J AU Bayliss, MB Rigby, JR Sharon, K Wuyts, E Florian, M Gladders, MD Johnson, T Oguri, M AF Bayliss, Matthew B. Rigby, Jane R. Sharon, Keren Wuyts, Eva Florian, Michael Gladders, Michael D. Johnson, Traci Oguri, Masamune TI THE PHYSICAL CONDITIONS, METALLICITY AND METAL ABUNDANCE RATIOS IN A HIGHLY MAGNIFIED GALAXY AT z=3.6252 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: star formation; gravitational lensing: strong ID STAR-FORMING GALAXIES; GRAVITATIONALLY LENSED GALAXY; STELLAR POPULATION SYNTHESIS; LYMAN-BREAK GALAXY; GIANT ARCS SURVEY; SIMILAR-TO 2; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; H-II REGIONS; ULTRAVIOLET-SPECTRUM AB We present optical and near-IR imaging and spectroscopy of SGAS J105039.6+001730, a strongly lensed galaxy at z = 3.6252 magnified by >30x, and derive its physical properties. We measure a stellar mass of log(M-*/M-circle dot) = 9.5 +/- 0.35, star formation rates from [O II] lambda lambda 3727 and H beta of 55 +/- 25 and 84 +/- 24 M-circle dot yr(-1), respectively, an electron density of n(e) <= 10(3) cm(-2), an electron temperature of T-e <= 14,000 K, and a metallicity of 12 + log(O/H) = 8.3 +/- 0.1. The strong C III] lambda lambda 1907,1909 emission and abundance ratios of C, N, O, and Si are consistent with well-studied starbursts at z similar to 0 with similar metallicities. Strong P Cygni lines and He II lambda 1640 emission indicate a significant population of Wolf-Rayet stars, but synthetic spectra of individual populations of young, hot stars do not reproduce the observed integrated P Cygni absorption features. The rest-frame UV spectral features are indicative of a young starburst with high ionization, implying either (1) an ionization parameter significantly higher than suggested by rest-frame optical nebular lines, or (2) differences in one or both of the initial mass function and the properties of ionizing spectra of massive stars. We argue that the observed features are likely the result of a superposition of star forming regions with different physical properties. These results demonstrate the complexity of star formation on scales smaller than individual galaxies, and highlight the importance of systematic effects that result from smearing together the signatures of individual star forming regions within galaxies. C1 [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Sharon, Keren; Johnson, Traci] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wuyts, Eva] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Florian, Michael; Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Florian, Michael; Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Oguri, Masamune] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan. [Oguri, Masamune] Univ Tokyo, Kavli Inst Phys & Math Universe Kavli IPMU WPI, Chiba 2778583, Japan. RP Bayliss, MB (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. EM mbayliss@cfa.harvard.edu RI Rigby, Jane/D-4588-2012; Oguri, Masamune/C-6230-2011 OI Rigby, Jane/0000-0002-7627-6551; FU National Science Foundation [AST-1009012]; NASA from the Space Telescope Science Institute [HST-GO-13003.01]; NASA [NAS5-26555]; JSPS [23740161]; FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan FX We thank Sally Heap and Dan Stark for interesting and helpful discussions that improved this paper, as well as the anonymous referee who provided very thoughtful and constructive feedback. This work was supported by the National Science Foundation through grant AST-1009012, by NASA through grant HST-GO-13003.01 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and also by the FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and Grant-in-Aid for Scientific Research from the JSPS (23740161). NR 103 TC 22 Z9 22 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 2014 VL 790 IS 2 AR 144 DI 10.1088/0004-637X/790/2/144 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800061 ER PT J AU Chen, JC Wang, XF Ganeshalingam, M Silverman, JM Filippenko, AV Li, WD Chornock, R Li, JZ Steele, T AF Chen, Juncheng Wang, Xiaofeng Ganeshalingam, Mohan Silverman, Jeffrey M. Filippenko, Alexei V. Li, Weidong Chornock, Ryan Li, Junzheng Steele, Thea TI OPTICAL OBSERVATIONS OF THE TYPE Ic SUPERNOVA 2007gr IN NGC 1058 SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN 2007gr) ID CORE-COLLAPSE SUPERNOVAE; IA SUPERNOVAE; LIGHT CURVES; SN 2007GR; X-RAY; SPECTRAL EVOLUTION; UBVRI PHOTOMETRY; TRANSIENT 080109; LINE-PROFILES; SPECTROSCOPY AB We present extensive optical observations of the normal Type Ic supernova (SN) 2007gr, spanning from about one week before maximum light to more than one year thereafter. The optical light and color curves of SN 2007gr are very similar to those of the broad-lined Type Ic SN 2002ap, but the spectra show remarkable differences. The optical spectra of SN 2007gr are characterized by unusually narrow lines, prominent carbon lines, and slow evolution of the line velocity after maximum light. The earliest spectrum (taken at t = -8 days) shows a possible signature of helium (He I lambda 5876 at a velocity of similar to 19,000 km s(-1)). Moreover, the larger intensity ratio of the [O I] lambda 6300 and lambda 6364 lines inferred from the early nebular spectra implies a lower opacity of the ejecta shortly after the explosion. These results indicate that SN 2007gr perhaps underwent a less energetic explosion of a smaller-mass Wolf-Rayet star (similar to 8-9 M-circle dot) in a binary system, as favored by an analysis of the progenitor environment through pre-explosion and post-explosion Hubble Space Telescope images. In the nebular spectra, asymmetric double-peaked profiles can be seen in the [O I] lambda 6300 and Mg I] lambda 4571 lines. We suggest that the two peaks are contributed by the blueshifted and rest-frame components. The similarity in velocity structure and the different evolution of the strength of the two components favor an aspherical explosion with the ejecta distributed in a torus or disk-like geometry, but inside the ejecta the O and Mg have different distributions. C1 [Chen, Juncheng; Wang, Xiaofeng; Li, Junzheng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Chen, Juncheng; Wang, Xiaofeng; Li, Junzheng] Tsinghua Univ, Tsinghua Ctr Astrophys THCA, Beijing 100084, Peoples R China. [Ganeshalingam, Mohan; Silverman, Jeffrey M.; Filippenko, Alexei V.; Li, Weidong; Chornock, Ryan; Steele, Thea] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Ganeshalingam, Mohan] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Environm Energy Technol Div, Berkeley, CA 94720 USA. [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Chornock, Ryan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, JC (reprint author), Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. EM cjc09@mails.tsinghua.edu.cn; wang_xf@mail.tsinghua.edu.cn RI Wang, Xiaofeng/J-5390-2015 FU Major State Basic Research Development Program [2013CB834903]; National Natural Science Foundation of China (NSFC) [11073013, 11178003, 11325313]; Foundation of Tsinghua University [2011Z02170]; NSF [AST-1211916]; TABASGO Foundation; Christopher R. Redlich Fund; NASA through Space Telescope Science Institute [GO-10877, AR-12623]; NASA [NAS 5-26555]; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; W. M. Keck Foundation FX We are grateful to the anonymous referee for constructive suggestions that helped improve the paper. We thank the NAOC, Lick, and Keck Observatory staffs, as well as Maryam Modjaz and Ryan Foley for their assistance with the observations. 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. This work is supported by the Major State Basic Research Development Program (2013CB834903), National Natural Science Foundation of China (NSFC grants 11073013, 11178003, 11325313), and the Foundation of Tsinghua University (2011Z02170). A. V.F.'s group at UC Berkeley is grateful for financial assistance from NSF grant AST-1211916, the TABASGO Foundation, and the Christopher R. Redlich Fund. This work was also supported by NASA through grants GO-10877 and AR-12623 from the Space Telescope Science Institute, which is operated by the Associated Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. J. M. Silverman is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. NR 75 TC 6 Z9 6 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 2014 VL 790 IS 2 AR 120 DI 10.1088/0004-637X/790/2/120 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800037 ER PT J AU Chitsazzadeh, S Di Francesco, J Schnee, S Friesen, RK Shimajiri, Y Langston, GI Sadavoy, SI Bourke, TL Keto, ER Pineda, JE Takakuwa, S Tatematsu, K AF Chitsazzadeh, S. Di Francesco, J. Schnee, S. Friesen, R. K. Shimajiri, Y. Langston, G. I. Sadavoy, S. I. Bourke, T. L. Keto, E. R. Pineda, J. E. Takakuwa, S. Tatematsu, K. TI PHYSICAL AND CHEMICAL CHARACTERISTICS OF L1689-SMM16, AN OSCILLATING PRESTELLAR CORE IN OPHIUCHUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: kinematics and dynamics; ISM: molecules; ISM: structure; radio lines: ISM; stars: formation ID PRE-PROTOSTELLAR CORES; MASSIVE STAR-FORMATION; NRO 45-M TELESCOPE; GOULD BELT CLOUDS; DENSE CORES; MOLECULAR CLOUDS; DARK CLOUD; ENVELOPE EXPANSION; INITIAL CONDITIONS; INFALL MOTIONS AB We present single-dish observations of the L1689-SMM16 core in the Ophiuchus molecular cloud in NH3 (1, 1) and (2, 2) emission using the Green Bank Telescope, in N2H+ (1-0) emission using the Nobeyama Radio Observatory, and in NH2D (1(1,1)(a)-1(0,1)(s)), HCN (1-0), HNC (1-0), (HCO+)-C-13 (1-0), and HCO+ (1-0) emission using the Mopra telescope. The morphologies of the integrated NH3 (1, 1) and N2H+ (1-0) emission well match that of 250 mu m continuum emission. Line widths of NH3 (1, 1) and N2H+ (1-0) show the presence of transonic turbulence across the core. Jeans and virial analyses made using updated measurements of core mass and size confirm that L1689-SMM16 is prestellar, i.e., gravitationally bound. It also has accumulated more mass compared to its corresponding Jeans mass in the absence of magnetic fields and therefore is a "super-Jeans" core. The high levels of X(NH3)/X(N2H+) and deuterium fractionation reinforce the idea that the core has not yet formed a protostar. Comparing the physical parameters of the core with those of a Bonnor-Ebert sphere reveals the advanced evolutionary stage of L1689-SMM16 and shows that it might be unstable to collapse. We do not detect any evidence of infall motions toward the core. Instead, red asymmetry in the line profiles of HCN (1-0) and HNC (1-0) indicates the expansion of the outer layers of the core at a speed of similar to 0.2 km s(-1) to 0.3 km s(-1). For a gravitationally bound core, expansion in the outer layers might indicate that the core is experiencing oscillations. C1 [Chitsazzadeh, S.; Di Francesco, J.; Sadavoy, S. I.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Chitsazzadeh, S.; Di Francesco, J.; Sadavoy, S. I.] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. [Schnee, S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Friesen, R. K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Shimajiri, Y.] CEA DSM CNRS Univ Paris Diderot, Lab AIM, IRFU Serv Astrophys, CEA Saclay, F-91191 Gif Sur Yvette, France. [Langston, G. I.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Bourke, T. L.; Keto, E. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bourke, T. L.] Jodrell Bank Observ, SKA Org, Macclesfield SH11 9DL, Cheshire, England. [Pineda, J. E.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Takakuwa, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Tatematsu, K.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tatematsu, K.] Grad Univ Adv Studies Sokendai, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. RP Chitsazzadeh, S (reprint author), Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. EM schitsaz@uvic.ca OI Di Francesco, James/0000-0002-9289-2450; Pineda, Jaime/0000-0002-3972-1978 FU Natural Sciences and Engineering Research Council of Canada (NSERC); Commonwealth of Australia; Australian Research Council FX The authors thank the anonymous referee for comments that greatly improved the quality of this paper. We also thank the scientific editor, E. Feigelson, for his helpful suggestions toward this paper. We thank the observatory staff at the GBT, NRO, and Mopra telescopes for assistance with the observations. We also thank M. Houde, H. Kirk, S. Mairs, K. Thanjavur, and A. J. Remijan for helpful discussions. This work was supported by the Discovery Grant from Natural Sciences and Engineering Research Council of Canada (NSERC). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NRO is a branch of the National Astronomical Observatory of Japan, National Institutes of Natural Sciences. The Mopra radio telescope 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. The University of New South Wales Digital Filter Bank used for the observations with the Mopra telescope was provided with support from the Australian Research Council. This research has made use of data from the Herschel Gould Belt Survey (HGBS) project (http://gouldbelt-herschel.cea.fr). The HGBS is a Herschel Key Programme jointly carried out by SPIRE Specialist Astronomy Group 3 (SAG 3), scientists of several institutes in the PACS Consortium (CEA Saclay, INAF-IFSI Rome and INAF-Arcetri, KU Leuven, MPIA Heidelberg), and scientists of the Herschel Science Center (HSC). NR 98 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 AUG 1 PY 2014 VL 790 IS 2 AR 129 DI 10.1088/0004-637X/790/2/129 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800046 ER PT J AU Choi, YK Hachisuka, K Reid, MJ Xu, Y Brunthaler, A Menten, KM Dame, TM AF Choi, Y. K. Hachisuka, K. Reid, M. J. Xu, Y. Brunthaler, A. Menten, K. M. Dame, T. M. TI TRIGONOMETRIC PARALLAXES OF STAR FORMING REGIONS IN THE PERSEUS SPIRAL ARM SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; Galaxy: kinematics and dynamics; Galaxy: structure; masers; stars: formation ID BASE-LINE INTERFEROMETRY; MILKY-WAY; FUNDAMENTAL PARAMETERS; DISTANCE; GALAXY; VERA; ASTROMETRY; KINEMATICS; MOTIONS; VLBA AB We report trigonometric parallaxes and proper motions of water masers for 12 massive star forming regions in the Perseus spiral arm of the Milky Way as part of the Bar and Spiral Structure Legacy (BeSSel) Survey. Combining our results with 14 parallax measurements in the literature, we estimate a pitch angle of 9 degrees.9 +/- 1 degrees.5 for a section of the Perseus arm. The three-dimensional Galactic peculiar motions of these sources indicate that on average they are moving toward the Galactic center and slower than the Galactic rotation. C1 [Choi, Y. K.; Brunthaler, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Choi, Y. K.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hachisuka, K.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Reid, M. J.; Dame, T. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Xu, Y.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Jiangsu, Peoples R China. RP Choi, YK (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM ykchoi@mpifr-bonn.mpg.de FU European Research Council for the ERC Advanced Grant GLOSTAR (ERC-AdG) [247078]; Chinese National Science Foundation [NSF 11133008]; Key Laboratory for Radio Astronomy, Chinese Academy of Sciences FX Financial support by the European Research Council for the ERC Advanced Grant GLOSTAR (ERC-2009-AdG, grant agreement No. 247078) is gratefully acknowledged. This work was supported in part by the Chinese National Science Foundation through grant NSF 11133008 and the Key Laboratory for Radio Astronomy, Chinese Academy of Sciences. NR 29 TC 33 Z9 33 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 2014 VL 790 IS 2 AR 99 DI 10.1088/0004-637X/790/2/99 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800016 ER PT J AU Dupuy, TJ Liu, MC Ireland, MJ AF Dupuy, Trent J. Liu, Michael C. Ireland, Michael J. TI NEW EVIDENCE FOR A SUBSTELLAR LUMINOSITY PROBLEM: DYNAMICAL MASS FOR THE BROWN DWARF BINARY Gl 417BC SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; binaries: close; brown dwarfs; infrared: stars; stars: fundamental parameters; stars: individual (Gl 417, HD 130948) ID STAR ADAPTIVE OPTICS; SOLAR-TYPE STARS; VERY-LOW MASS; EXTRASOLAR GIANT PLANETS; MAIN-SEQUENCE STARS; INFRARED FILTER SET; LITHIUM ABUNDANCES; L/T TRANSITION; T DWARF; EVOLUTIONARY MODELS AB We present new evidence for a problem with cooling rates predicted by substellar evolutionary models that implies that model-derived masses in the literature for brown dwarfs and directly imaged planets may be too high. Based on our dynamical mass for Gl 417BC (L4.5+L6) and a gyrochronology system age from its young, solar-type host star, commonly used models predict luminosities 0.2-0.4 dex lower than we observe. This corroborates a similar luminosity-age discrepancy identified in our previous work on the L4+L4 binary HD 130948BC, which coincidentally has nearly identical component masses (approximate to 50-55 M-Jup) and age (approximate to 800 Myr) as Gl 417BC. Such a luminosity offset would cause systematic errors of 15%-25% in model-derived masses at this age. After comparing different models, including cloudless models that should not be appropriate for mid-L dwarfs like Gl 417BC and HD 130948BC but actually match their luminosities better, we speculate the observed overluminosity could be caused by opacity holes (i.e., patchy clouds) in these objects. Moreover, from hybrid substellar evolutionary models that account for cloud disappearance, we infer the corresponding phase of overluminosity may extend from a few hundred million years up to a few gigayears and cause masses to be overestimated by up to 25%, even well after clouds disappear from view entirely. Thus, the range of ages and spectral types affected by this potential systematic shift in luminosity evolution would encompass most known directly imaged gas-giants and field brown dwarfs. C1 [Dupuy, Trent J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ireland, Michael J.] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia. [Ireland, Michael J.] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia. [Ireland, Michael J.] Australian Astron Observ, Epping, NSW 1710, Australia. RP Dupuy, TJ (reprint author), Univ Texas Austin, Dept Astron, 2515 Speedway C1400, Austin, TX 78712 USA. FU NASA Keck PI Data Award; Space Telescope Science Institute [HST-HF-51271.01-A]; NASA [NAS 5-26555]; NSF [AST09-09222] FX We are grateful to Josh Carter for discussions about MCMC methods; Didier Saumon and Isabelle Baraffe for providing expanded model grids and helpful discussions about substellar evolution; Joel Aycock, Randy Campbell, Al Conrad, Heather Hershley, Jim Lyke, Jason McIlroy, Eric Nielsen, Gary Punawai, Julie Riviera, Hien Tran, Cynthia Wilburn, and the Keck Observatory staff for assistance with the Keck LGS AO observing; the anonymous referee for a constructive report; and James R. A. Davenport for distributing his IDL implementation of the cubehelix color scheme. This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. T.J.D. acknowledges support from Hubble Fellowship grant HST-HF-51271.01-A awarded by the Space Telescope Science Institute, which is operated by AURA for NASA, under contract NAS 5-26555. M. C. L. acknowledges support from NSF grant AST09-09222. Our research has employed the 2MASS data products; NASA's Astrophysical Data System; the SIMBAD database operated at CDS, Strasbourg, France; and the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism. Finally, 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 74 TC 26 Z9 26 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 AUG 1 PY 2014 VL 790 IS 2 AR 133 DI 10.1088/0004-637X/790/2/133 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800050 ER PT J AU Fabrycky, DC Lissauer, JJ Ragozzine, D Rowe, JF Steffen, JH Agol, E Barclay, T Batalha, N Borucki, W Ciardi, DR Ford, EB Gautier, TN Geary, JC Holman, MJ Jenkins, JM Li, J Morehead, RC Morris, RL Shporer, A Smith, JC Still, M Van Cleve, J AF Fabrycky, Daniel C. Lissauer, Jack J. Ragozzine, Darin Rowe, Jason F. Steffen, Jason H. Agol, Eric Barclay, Thomas Batalha, Natalie Borucki, William Ciardi, David R. Ford, Eric B. Gautier, Thomas N. Geary, John C. Holman, Matthew J. Jenkins, Jon M. Li, Jie Morehead, Robert C. Morris, Robert L. Shporer, Avi Smith, Jeffrey C. Still, Martin Van Cleve, Jeffrey TI ARCHITECTURE OF KEPLER'S MULTI-TRANSITING SYSTEMS. II. NEW INVESTIGATIONS WITH TWICE AS MANY CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: statistical; planetary systems; planets and satellites: detection; planets and satellites: dynamical evolution and stability ID PLANET SYSTEMS; ORBITAL ECCENTRICITIES; MULTIPLANET SYSTEMS; TIMING OBSERVATIONS; SUPER-EARTH; DYNAMICS; CONFIRMATION; STABILITY; MIGRATION; HARPS AB We report on the orbital architectures of Kepler systems having multiple-planet candidates identified in the analysis of data from the first six quarters of Kepler data and reported by Batalha et al. (2013). These data show 899 transiting planet candidates in 365 multiple-planet systems and provide a powerful means to study the statistical properties of planetary systems. Using a generic mass-radius relationship, we find that only two pairs of planets in these candidate systems (out of 761 pairs total) appear to be on Hill-unstable orbits, indicating similar to 96% of the candidate planetary systems are correctly interpreted as true systems. We find that planet pairs show little statistical preference to be near mean-motion resonances. We identify an asymmetry in the distribution of period ratios near first-order resonances (e.g., 2:1, 3:2), with an excess of planet pairs lying wide of resonance and relatively few lying narrow of resonance. Finally, based upon the transit duration ratios of adjacent planets in each system, we find that the interior planet tends to have a smaller transit impact parameter than the exterior planet does. This finding suggests that the mode of the mutual inclinations of planetary orbital planes is in the range 1 degrees.0-2 degrees.2, for the packed systems of small planets probed by these observations. C1 [Fabrycky, Daniel C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lissauer, Jack J.; Rowe, Jason F.; Barclay, Thomas; Batalha, Natalie; Borucki, William; Jenkins, Jon M.; Li, Jie; Morris, Robert L.; Smith, Jeffrey C.; Van Cleve, Jeffrey] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ragozzine, Darin; Geary, John C.; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowe, Jason F.; Li, Jie; Morris, Robert L.; Smith, Jeffrey C.; Van Cleve, Jeffrey] SETI Inst, Mountain View, CA 94043 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Steffen, Jason H.] CIERA Northwestern Univ, Evanston, IL 60208 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Barclay, Thomas; Still, Martin] NASA, Ames Res Ctr, Bay Area Environm Res Inst, Moffett Field, CA 94035 USA. [Batalha, Natalie] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Ford, Eric B.; Morehead, Robert C.] Penn State Univ, Davey Lab 525, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Ford, Eric B.; Morehead, Robert C.] Penn State Univ, Davey Lab 525, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ford, Eric B.; Morehead, Robert C.] Univ Florida, Dept Astron, Gainesville, FL 32111 USA. [Gautier, Thomas N.; Shporer, Avi] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Shporer, Avi] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Fabrycky, DC (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM fabrycky@uchicago.edu OI /0000-0002-0802-9145; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA through Hubble Fellowship [HF-51272.01-A]; NASA [NAS 5-26555]; NSF [0645416]; National Aeronautics and Space Administration [NNX08AR04G]; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; National Science Foundation [0707203, DGE-0802270] FX Funding for this mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler team for the many years of work that is making the Kepler mission so successful. We thank Emily Fabrycky, Doug Lin, Man-Hoi Lee, Scott Tremaine, and Tsevi Mazeh for helpful conversations and insightful comments. D.C F. acknowledges support for this work was provided by NASA through Hubble Fellowship grant No. HF-51272.01-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. E.A. was supported by NSF Career grant 0645416. E.B.F acknowledges support by the National Aeronautics and Space Administration under grant NNX08AR04G issued through the Kepler Participating Scientist Program, and the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. This material is based upon work supported by the National Science Foundation under grant No. 0707203. R.C.M. was support by the National Science Foundation Graduate Research Fellowship under grant No. DGE-0802270. NR 40 TC 107 Z9 107 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 AUG 1 PY 2014 VL 790 IS 2 AR 146 DI 10.1088/0004-637X/790/2/146 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800063 ER PT J AU Gatuzz, E Garcia, J Mendoza, C Kallman, TR Bautista, MA Gorczyca, TW AF Gatuzz, E. Garcia, J. Mendoza, C. Kallman, T. R. Bautista, M. A. Gorczyca, T. W. TI PHYSICAL PROPERTIES OF THE INTERSTELLAR MEDIUM USING HIGH-RESOLUTION CHANDRA SPECTRA: O K-EDGE ABSORPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; ISM: abundances; ISM: atoms; X-rays: binaries; X-rays: ISM ID X-RAY SPECTROSCOPY; XMM-NEWTON OBSERVATION; NEUTRON-STAR; ATOMIC OXYGEN; SCORPIUS X-1; 4U 1820-30; CYG X-2; SHELL PHOTOABSORPTION; CROSS-SECTIONS; LOW/HARD STATE AB Chandra high-resolution spectra toward eight low-mass Galactic binaries have been analyzed with a photoionization model that is capable of determining the physical state of the interstellar medium. Particular attention is given to the accuracy of the atomic data. Hydrogen column densities are derived with a broadband fit that takes into account pileup effects, and in general are in good agreement with previous results. The dominant features in the oxygen-edge region are OI and OII K alpha absorption lines whose simultaneous fits lead to average values of the ionization parameter of log xi = -2.90 and oxygen abundance of A(O) = 0.70. The latter is given relative to the standard by Grevesse & Sauval, but rescaling with the revision by Asplund et al. would lead to an average abundance value fairly close to solar. The low average oxygen column density (N-O = 9.2 x 10(17) cm(-2)) suggests a correlation with the low ionization parameters, the latter also being in evidence in the column density ratios N(O II)/N(O I) and N(O III)/N(O I) that are estimated to be less than 0.1. We do not find conclusive evidence for absorption by any other compound but atomic oxygen in our oxygen-edge region analysis. C1 [Gatuzz, E.; Mendoza, C.] Inst Venezolano Invest Cient, Ctr Fis, Caracas 1020A, Venezuela. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mendoza, C.; Bautista, M. A.; Gorczyca, T. W.] Western Michigan Univ, Dept Phys, Kalamazoo, MI 49008 USA. [Kallman, T. R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gatuzz, E (reprint author), Inst Venezolano Invest Cient, Ctr Fis, POB 20632, Caracas 1020A, Venezuela. EM egatuzz@ivic.gob.ve; javier@head.cfa.harvard.edu; claudio@ivic.gob.ve; timothy.r.kallman@nasa.gov; manuel.bautista@wmich.edu; thomas.gorczyca@wmich.edu OI Mendoza, Claudio/0000-0002-2854-4806 FU National Science Foundation [AST-1313265] FX Part of this work was carried out by Efrain Gatuzz during a visit in 2014 January to the Laboratory of High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, Maryland, USA. Their hospitality and financial support are gratefully acknowledged. Manuel Bautista has received financial support from the National Science Foundation through grant AST-1313265. We would also like to thank Dr. Frits Paerels for comments at the refereeing stage that led to substantial improvements of the arguments presented and thus of the final quality of the paper. NR 51 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 AUG 1 PY 2014 VL 790 IS 2 AR 131 DI 10.1088/0004-637X/790/2/131 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800048 ER PT J AU Lewkow, NR Kharchenko, V AF Lewkow, N. R. Kharchenko, V. TI PRECIPITATION OF ENERGETIC NEUTRAL ATOMS AND INDUCED NON-THERMAL ESCAPE FLUXES FROM THE MARTIAN ATMOSPHERE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astronomical databases: miscellaneous; atmospheric effects; atomic processes; planets and satellites: atmospheres; scattering ID DIFFERENTIAL CROSS-SECTIONS; CHARGE-TRANSFER SCATTERING; STOCHASTIC-MODELS; SATELLITE CORONAS; HOT PLANETARY; HYDROGEN-ATOMS; SMALL ANGLES; KEV ENERGIES; ABSOLUTE; COLLISIONS AB The precipitation of energetic neutral atoms, produced through charge exchange collisions between solar wind ions and thermal atmospheric gases, is investigated for the Martian atmosphere. Connections between parameters of precipitating fast ions and resulting escape fluxes, altitude-dependent energy distributions of fast atoms and their coefficients of reflection from the Mars atmosphere, are established using accurate cross sections in Monte Carlo (MC) simulations. Distributions of secondary hot (SH) atoms and molecules, induced by precipitating particles, have been obtained and applied for computations of the non-thermal escape fluxes. A new collisional database on accurate energy-angular-dependent cross sections, required for description of the energy-momentum transfer in collisions of precipitating particles and production of non-thermal atmospheric atoms and molecules, is reported with analytic fitting equations. Three-dimensional MC simulations with accurate energy-angular-dependent cross sections have been carried out to track large ensembles of energetic atoms in a time-dependent manner as they propagate into the Martian atmosphere and transfer their energy to the ambient atoms and molecules. Results of the MC simulations on the energy-deposition altitude profiles, reflection coefficients, and time-dependent atmospheric heating, obtained for the isotropic hard sphere and anisotropic quantum cross sections, are compared. Atmospheric heating rates, thermalization depths, altitude profiles of production rates, energy distributions of SH atoms and molecules, and induced escape fluxes have been determined. C1 [Lewkow, N. R.; Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Lewkow, N. R.; Kharchenko, V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. RP Lewkow, NR (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. FU NASA [NNX10AB88G] FX N. Lewkow and V. Kharchenko are grateful to NASA for supporting our research via the grant NNX10AB88G. NR 43 TC 2 Z9 2 U1 1 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 AUG 1 PY 2014 VL 790 IS 2 AR 98 DI 10.1088/0004-637X/790/2/98 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800015 ER PT J AU Lu, X Zhang, QZ Liu, HYBB Wang, JZ Gu, QS AF Lu, Xing Zhang, Qizhou Liu, Hauyu Baobab Wang, Junzhi Gu, Qiusheng TI VERY LARGE ARRAY OBSERVATIONS OF AMMONIA IN HIGH-MASS STAR FORMATION REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; stars: formation ID H-II REGIONS; ULTRACOMPACT HII-REGIONS; INFRARED DARK CLOUD; SPITZER-SPACE-TELESCOPE; CLUSTER-FORMING REGION; MOLECULAR CLOUDS; DENSE CORES; METHANOL MASERS; IRAS SOURCES; PROTOSTELLAR CORES AB We report systematic mapping observations of the NH3 (1, 1) and (2, 2) inversion lines toward 62 high-mass star-forming regions using the Very Large Array (VLA) in its D and DnC array configurations. The VLA images cover a spatial dynamic range from 40'' to 3'', allowing us to trace gas kinematics from similar to 1 pc scales to less than or similar to 0.1 pc scales. Based on the NH3 morphology and the infrared nebulosity on 1 pc scales, we categorize three subclasses in the sample: filaments, hot cores, and NH3-dispersed sources. The ubiquitous gas filaments found on 1 pc scales have a typical width of similar to 0.1 pc and often contain regularly spaced fragments along the major axis. The spacing of the fragments and the column densities is consistent with the turbulent supported fragmentation of cylinders. Several sources show multiple filaments that converge toward a center where the velocity field in the filaments is consistent with gas flows. We derive rotational temperature maps for the entire sample. For the three hot core sources, we find a projected radial temperature distribution that is best fit by power-law indices from -0.18 to -0.35. We identify 174 velocity-coherent similar to 0.1 pc scale dense cores from the entire sample. The mean physical properties for these cores are 1.1 km s(-1) in intrinsic linewidth, 18 K in NH3 rotational temperature, 2.3 x 10(15) cm(-2) in NH3 gas column density, and 67M(circle dot) in molecular mass. The dense cores identified from the filamentary sources are closer to being virialized. Dense cores in the other two categories of sources appear to be dynamically unstable. 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, Nanjing 210093, Jiangsu, Peoples R China. [Liu, Hauyu Baobab] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Wang, Junzhi] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. RP Lu, X (reprint author), Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. OI Zhang, Qizhou/0000-0003-2384-6589 FU National Science Basic Research Program of China (973 program) [2012CB821805]; National Science Foundation of China [11273015, 11133001, 11328301]; NASA; Smithsonian predoctoral fellowship FX We are grateful to the anonymous referee for valuable suggestions. This work was partly supported by the National Science Basic Research Program of China (973 program) No. 2012CB821805, the National Science Foundation of China under grant 11273015, 11133001, 11328301, and has made use of NASA's Astrophysics Data System and the SIMBAD database operated at CDS, Strasbourg, France. This study used observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. X. L. acknowledges the support of a Smithsonian predoctoral fellowship. NR 103 TC 14 Z9 14 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 AUG 1 PY 2014 VL 790 IS 2 AR 84 DI 10.1088/0004-637X/790/2/84 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800001 ER PT J AU Williams, BJ Borkowski, KJ Reynolds, SP Ghavamian, P Raymond, JC Long, KS Blair, WP Sankrit, R Winkler, PF Hendrick, SP AF Williams, Brian J. Borkowski, Kazimierz J. Reynolds, Stephen P. Ghavamian, Parviz Raymond, John C. Long, Knox S. Blair, William P. Sankrit, Ravi Winkler, P. Frank Hendrick, Sean P. TI SPITZER OBSERVATIONS OF THE TYPE IA SUPERNOVA REMNANT N103B: KEPLER'S OLDER COUSIN? SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: supernova remnants ID LARGE-MAGELLANIC-CLOUD; RESOLUTION X-RAY; SN 1006; COSMIC SILICATES; DUST; PROGENITOR; EMISSION; STARS; SHOCK; IDENTIFICATION AB We report results from Spitzer observations of SNR 0509-68.7, also known as N103B, a young Type Ia supernova remnant (SNR) in the Large Magellanic Cloud (LMC) that shows interaction with a dense medium in its western hemisphere. Our images show that N103B has strong IR emission from warm dust in the post-shock environment. The post-shock gas density we derive, 45 cm(-3), is much higher than in other Type Ia remnants in the LMC, though a lack of spatial resolution may bias measurements toward regions of higher than average density. This density is similar to that in Kepler's SNR, a Type Ia interacting with a circumstellar medium (CSM). Optical images show Ha emission along the entire periphery of the western portion of the shock, with [O III] and [S II] lines emitted from a few dense clumps of material where the shock has become radiative. The dust is silicate in nature, though standard silicate dust models fail to reproduce the "18 mu m" silicate feature that peaks instead at 17.3 mu m. We propose that the dense material is circumstellar material lost from the progenitor system, as with Kepler. If the CSM interpretation is correct, this remnant would become the second member, along with Kepler, of a class of Type Ia remnants characterized by interaction with a dense CSM hundreds of years post-explosion. A lack of N enhancement eliminates symbiotic asymptotic giant branch progenitors. The white dwarf companion must have been relatively unevolved at the time of the explosion. C1 [Williams, Brian J.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. [Ghavamian, Parviz] Towson Univ, Dept Phys Chem & Geosci, Towson, MD 21252 USA. [Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Long, Knox S.] STScI, Baltimore, MD 21218 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Hendrick, Sean P.] Millersville Univ Pennsylvania, Dept Phys, Millersville, PA 17551 USA. RP Williams, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM brian.j.williams@nasa.gov FU Spitzer Guest Observer [RSA 1265236, RSA 1328682] FX We thank R. Chris Smith for providing the optical images from CTIO. This work was supported through Spitzer Guest Observer Grants RSA 1265236 and RSA 1328682. NR 54 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 AUG 1 PY 2014 VL 790 IS 2 AR 139 DI 10.1088/0004-637X/790/2/139 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800056 ER PT J AU Wong, TW Valsecchi, F Ansari, A Fragos, T Glebbeek, E Kalogera, V McClintock, J AF Wong, Tsing-Wai Valsecchi, Francesca Ansari, Asna Fragos, Tassos Glebbeek, Evert Kalogera, Vassiliki McClintock, Jeffrey TI UNDERSTANDING COMPACT OBJECT FORMATION AND NATAL KICKS. IV. THE CASE OF IC 10 X-1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; stars: evolution; X-rays: binaries; X-rays: individual (IC 10 X-1) ID COMMON ENVELOPE EVOLUTION; X-RAY BINARIES; NEUTRON-STAR ACCRETION; LARGE-MAGELLANIC-CLOUD; MASS BLACK-HOLE; WHITE-DWARF BINARIES; WOLF-RAYET; PROPER MOTIONS; IC-10 X-1; PHYSICAL-PROPERTIES AB The extragalactic X-ray binary IC 10 X-1 has attracted attention as it is possibly the host of the most massive stellar-mass black-hole (BH) known to date. Here we consider all available observational constraints and construct its evolutionary history up to the instant just before the formation of the BH. Our analysis accounts for the simplest possible history, which includes three evolutionary phases: binary orbital dynamics at core collapse, common envelope (CE) evolution, and evolution of the BH-helium star binary progenitor of the observed system. We derive the complete set of constraints on the progenitor system at various evolutionary stages. Specifically, right before the core collapse event, we find the mass of the BH immediate progenitor to be greater than or similar to 31 M-circle dot (at 95% of confidence, same hereafter). The magnitude of the natal kick imparted to the BH is constrained to be less than or similar to 130 km s(-1). Furthermore, we find that the "enthalpy" formalism recently suggested by Ivanova & Chaichenets is able to explain the existence of IC 10 X-1 without the need to invoke unreasonably high CE efficiencies. With this physically motivated formalism, we find that the CE efficiency required to explain the system is in the range of similar or equal to 0.6-1. C1 [Wong, Tsing-Wai; Valsecchi, Francesca; Ansari, Asna; Kalogera, Vassiliki] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Wong, Tsing-Wai; Valsecchi, Francesca; Ansari, Asna; Kalogera, Vassiliki] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Wong, Tsing-Wai; Fragos, Tassos; McClintock, Jeffrey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ansari, Asna] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Glebbeek, Evert] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Wong, TW (reprint author), Northwestern Univ, CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA. EM tsingwong2012@u.northwestern.edu; francesca@u.northwestern.edu; ansari@ldeo.columbia.edu; tfragos@cfa.harvard.edu; e.glebbeek@astro.ru.nl; jem@cfa.harvard.edu RI Fragos, Tassos/A-3581-2016 OI Fragos, Tassos/0000-0003-1474-1523 FU NSF [AST-0908930]; CIC/Smithsonian pre-doctoral fellowship program; CfA prize fellowship program; ITC prize fellowship program; NWO [639.041.129]; NSF MRI [PHY-0619274] FX This work has been primarily supported by the NSF Grant AST-0908930 awarded to V. K.; T. W. also acknowledges partial support through the CIC/Smithsonian pre-doctoral fellowship program and the hospitality of the CfA; T. F. acknowledges support from the CfA and the ITC prize fellowship programs. E. G. acknowledges support from the NWO under grant 639.041.129. The calculations for this work were performed on the Northwestern University Fugu cluster, which was partially funded by NSF MRI grant PHY-0619274, and on the Northwestern University Quest High Performance Computing cluster. NR 98 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 1 PY 2014 VL 790 IS 2 AR 119 DI 10.1088/0004-637X/790/2/119 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AL4PV UT WOS:000339115800036 ER PT J AU Zapico, SC Menendez, ST Nunez, P AF Zapico, Sara C. Menendez, Sofia T. Nunez, Paula TI Cell death proteins as markers of early postmortem interval SO CELLULAR AND MOLECULAR LIFE SCIENCES LA English DT Article DE Postmortem interval; Cell death markers; mRNA; PTEN; FasL ID TUMOR-SUPPRESSOR GENE; VITREOUS-HUMOR; MESSENGER-RNA; FAS LIGAND; RAT; PTEN; TIME; INJURY; AKT; PHOSPHORYLATION AB Estimation of time since death is one of the challenges in forensic science. There are many approaches to estimate the postmortem interval, including both physical and thanatochemistry methods. Decomposition is triggered by a process called autolysis, which induces destructive changes in the cell leading to cell death. Based on the process of cell death signaling, this study analyzed the early postmortem interval (2-8 h since death) using the study of the mRNA expression of Fas Ligand (FasL) and phosphatase and tensin homologue deleted on chromosome 10 (PTEN) by Quantitative-PCR. Results of the study indicate a time-dependent increase in the mRNA levels of both proteins up until 6 h after death. Using a regression analysis in these first 6 h, a positive linear correlation was found between the mRNA expression of these proteins and the time since death. Since PTEN and FasL are implicated in signaling pathways, both proteins are potential candidates to analyze the time since death in time intervals of 6 h or less. Further research is needed to find additional cell death markers and expand the time period for time since death estimation. C1 [Zapico, Sara C.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Menendez, Sofia T.] Univ Oviedo, IUOPA, HUCA, E-33006 Oviedo, Asturias, Spain. [Nunez, Paula] Univ Oviedo, Dept Biol Func, Fac Med, E-33006 Oviedo, Asturias, Spain. RP Zapico, SC (reprint author), Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, MRC 112,10th & Constitut Ave NW, Washington, DC 20560 USA. EM saiczapico@gmail.com FU Smithsonian Institution FX Sara C. Zapico is supported by a Peter Buck Postdoctoral Fellowship from the Smithsonian Institution. The authors gratefully acknowledge Keitlyn Alcantara-Russell for the language revision of this manuscript. NR 41 TC 3 Z9 3 U1 1 U2 16 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 1420-682X EI 1420-9071 J9 CELL MOL LIFE SCI JI Cell. Mol. Life Sci. PD AUG PY 2014 VL 71 IS 15 BP 2957 EP 2962 DI 10.1007/s00018-013-1531-x PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA AL7TG UT WOS:000339337800012 ER PT J AU O'Dwyer, JP Chisholm, R AF O'Dwyer, James P. Chisholm, Ryan TI A mean field model for competition: from neutral ecology to the Red Queen SO ECOLOGY LETTERS LA English DT Article DE Macroecology; neutral ecology; Red Queen hypothesis ID RELATIVE SPECIES ABUNDANCE; COMMUNITY ECOLOGY; TROPICAL FORESTS; BETA-DIVERSITY; BIODIVERSITY; POPULATIONS; MECHANISMS; PATTERNS; NICHE; DISTRIBUTIONS AB Individual species are distributed inhomogeneously over space and time, yet, within large communities of species, aggregated patterns of biodiversity seem to display nearly universal behaviour. Neutral models assume that an individual's demographic prospects are independent of its species identity. They have successfully predicted certain static, time-independent patterns. But they have generally failed to predict temporal patterns, such as species ages or population dynamics. We construct a new, multispecies framework incorporating competitive differences between species, and assess the impact of this competition on static and dynamic patterns of biodiversity. We solve this model exactly for the special case of a Red Queen hypothesis, where fitter species are continually arising. The model predicts more realistic species ages than neutral models, without greatly changing predictions for static species abundance distributions. Our modelling approach may allow users to incorporate a broad range of ecological mechanisms. C1 [O'Dwyer, James P.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Chisholm, Ryan] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Chisholm, Ryan] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP O'Dwyer, JP (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. EM jodwyer@illinois.edu RI Chisholm, Ryan/H-8033-2012 FU Templeton World Charity Foundation [TWCF0079/AB47]; National University of Singapore [WBS R-154-000-551-133] FX We thank Stephen Cornell, Stephen Pacala and Tim Newman for comments on earlier versions of this work. We also thank Egbert Leigh and an anonymous reviewer for extremely constructive and helpful comments. JOD acknowledges support from the Templeton World Charity Foundation grant TWCF0079/AB47. RAC acknowledges support from the National University of Singapore grant WBS R-154-000-551-133. NR 48 TC 7 Z9 7 U1 4 U2 59 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 2014 VL 17 IS 8 BP 961 EP 969 DI 10.1111/ele.12299 PG 9 WC Ecology SC Environmental Sciences & Ecology GA AL4KF UT WOS:000339101100008 PM 24924150 ER PT J AU Mitchard, ETA Feldpausch, TR Brienen, RJW Lopez-Gonzalez, G Monteagudo, A Baker, TR Lewis, SL Lloyd, J Quesada, CA Gloor, M ter Steege, H Meir, P Alvarez, E Araujo-Murakami, A Aragao, LEOC Arroyo, L Aymard, G Banki, O Bonal, D Brown, S Brown, FI Ceron, CE Moscoso, VC Chave, J Comiskey, JA Cornejo, F Medina, MC Da Costa, L Costa, FRC Di Fiore, A Domingues, TF Erwin, TL Frederickson, T Higuchi, N Coronado, ENH Killeen, TJ Laurance, WF Levis, C Magnusson, WE Marimon, BS Marimon, BH Polo, IM Mishra, P Nascimento, MT Neill, D Vargas, MPN Palacios, WA Parada, A Molina, GP Pena-Claros, M Pitman, N Peres, CA Poorter, L Prieto, A Ramirez-Angulo, H Correa, ZR Roopsind, A Roucoux, KH Rudas, A Salomao, RP Schietti, J Silveira, M de Souza, PF Steininger, MK Stropp, J Terborgh, J Thomas, R Toledo, M Torres-Lezama, A van Andel, TR van der Heijden, GMF Vieira, ICG Vieira, S Vilanova-Torre, E Vos, VA Wang, O Zartman, CE Malhi, Y Phillips, OL AF Mitchard, Edward T. A. Feldpausch, Ted R. Brienen, Roel J. W. Lopez-Gonzalez, Gabriela Monteagudo, Abel Baker, Timothy R. Lewis, Simon L. Lloyd, Jon Quesada, Carlos A. Gloor, Manuel ter Steege, Hans Meir, Patrick Alvarez, Esteban Araujo-Murakami, Alejandro Aragao, Luiz E. O. C. Arroyo, Luzmila Aymard, Gerardo Banki, Olaf Bonal, Damien Brown, Sandra Brown, Foster I. Ceron, Carlos E. Chama Moscoso, Victor Chave, Jerome Comiskey, James A. Cornejo, Fernando Corrales Medina, Massiel Da Costa, Lola Costa, Flavia R. C. Di Fiore, Anthony Domingues, Tomas F. Erwin, Terry L. Frederickson, Todd Higuchi, Niro Honorio Coronado, Euridice N. Killeen, Tim J. Laurance, William F. Levis, Carolina Magnusson, William E. Marimon, Beatriz S. Marimon Junior, Ben Hur Mendoza Polo, Irina Mishra, Piyush Nascimento, Marcelo T. Neill, David Nunez Vargas, Mario P. Palacios, Walter A. Parada, Alexander Pardo Molina, Guido Pena-Claros, Marielos Pitman, Nigel Peres, Carlos A. Poorter, Lourens Prieto, Adriana Ramirez-Angulo, Hirma Restrepo Correa, Zorayda Roopsind, Anand Roucoux, Katherine H. Rudas, Agustin Salomao, Rafael P. Schietti, Juliana Silveira, Marcos de Souza, Priscila F. Steininger, Marc K. Stropp, Juliana Terborgh, John Thomas, Raquel Toledo, Marisol Torres-Lezama, Armando van Andel, Tinde R. van der Heijden, Geertje M. F. Vieira, Ima C. G. Vieira, Simone Vilanova-Torre, Emilio Vos, Vincent A. Wang, Ophelia Zartman, Charles E. Malhi, Yadvinder Phillips, Oliver L. TI Markedly divergent estimates of Amazon forest carbon density from ground plots and satellites SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Above-ground biomass; allometry; carbon cycle; REDD; remote sensing; satellite mapping; wood density ID ABOVEGROUND LIVE BIOMASS; STOCKS; DEFORESTATION; EMISSIONS; ALLOMETRY; PATTERNS; BASIN; SOILS AB Aim The accurate mapping of forest carbon stocks is essential for understanding the global carbon cycle, for assessing emissions from deforestation, and for rational land-use planning. Remote sensing (RS) is currently the key tool for this purpose, but RS does not estimate vegetation biomass directly, and thus may miss significant spatial variations in forest structure. We test the stated accuracy of pantropical carbon maps using a large independent field dataset. Location Tropical forests of the Amazon basin. The permanent archive of the field plot data can be accessed at: http://dx.doi.org/10.5521/FORESTPLOTS.NET/2014_1 Methods Two recent pantropical RS maps of vegetation carbon are compared to a unique ground-plot dataset, involving tree measurements in 413 large inventory plots located in nine countries. The RS maps were compared directly to field plots, and kriging of the field data was used to allow area-based comparisons. Results The two RS carbon maps fail to capture the main gradient in Amazon forest carbon detected using 413 ground plots, from the densely wooded tall forests of the north-east, to the light-wooded, shorter forests of the south-west. The differences between plots and RS maps far exceed the uncertainties given in these studies, with whole regions over-or under-estimated by > 25%, whereas regional uncertainties for the maps were reported to be < 5%. Main conclusions Pantropical biomass maps are widely used by governments and by projects aiming to reduce deforestation using carbon offsets, but may have significant regional biases. Carbon-mapping techniques must be revised to account for the known ecological variation in tree wood density and allometry to create maps suitable for carbon accounting. The use of single relationships between tree canopy height and above-ground biomass inevitably yields large, spatially correlated errors. This presents a significant challenge to both the forest conservation and remote sensing communities, because neither wood density nor species assemblages can be reliably mapped from space. C1 [Mitchard, Edward T. A.; Meir, Patrick] Univ Edinburgh, Sch GeoSci, Edinburgh EH9 3JN, Midlothian, Scotland. [Feldpausch, Ted R.; Brienen, Roel J. W.; Lopez-Gonzalez, Gabriela; Baker, Timothy R.; Lewis, Simon L.; Gloor, Manuel; Honorio Coronado, Euridice N.; Roucoux, Katherine H.; de Souza, Priscila F.; Phillips, Oliver L.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Feldpausch, Ted R.; Aragao, Luiz E. O. C.] Univ Exeter, Coll Life & Environm Sci, Exeter EX4 4RJ, Devon, England. [Monteagudo, Abel; Chama Moscoso, Victor] Jardin Bot Missouri, Oxapampa, Peru. [Lewis, Simon L.] UCL, Dept Geog, London WC1E 6BT, England. [Lloyd, Jon] Univ London Imperial Coll Sci Technol & Med, Dept Life Sci, Fac Nat Sci, London, England. [Quesada, Carlos A.; Costa, Flavia R. C.; Higuchi, Niro; Levis, Carolina; Magnusson, William E.; Schietti, Juliana; Zartman, Charles E.] Inst Nacl de Pesquisas da Amazonia, Manaus, Amazonas, Brazil. [ter Steege, Hans; van Andel, Tinde R.] Nat Biodivers Ctr, Leiden, Netherlands. [ter Steege, Hans] Univ Utrecht, Inst Environm Biol, Utrecht, Netherlands. [Meir, Patrick] Australian Natl Univ, Res Sch Biol, Canberra, ACT 0200, Australia. [Araujo-Murakami, Alejandro; Arroyo, Luzmila; Parada, Alexander] Jardin Bot Medellin, Grp Invest Serv Ecosistem & Cambio Climat, Medellin, Colombia. [Araujo-Murakami, Alejandro; Arroyo, Luzmila; Parada, Alexander] Univ Autonoma Gabriel Rene Moreno, Museo Hist Nat Noel Kempff Mercado, Santa Cruz, Bolivia. [Aragao, Luiz E. O. C.] Natl Inst Space Res INPE, Remote Sensing Div, Sao Jose Dos Campos, SP, Brazil. [Aymard, Gerardo] UNELLEZ Guanare, Programa Ciencias Agro & Mar Herbario Univ PORT, Mesa De Cavacas 3350, Estado Portugue, Venezuela. [Banki, Olaf] Univ Amsterdam, IBED, NL-1090 GE Amsterdam, Netherlands. [Bonal, Damien] INRA, UMR EEF 1137, F-54280 Champenoux, France. [Brown, Sandra] Winrock Int Livestock Res & Training Ctr, Ecosystem Serv Unit, Arlington, VA 22202 USA. [Brown, Foster I.] Woods Hole Res Ctr, Falmouth, MA USA. [Brown, Foster I.; Silveira, Marcos] Univ Fed Acre, Ctr Ciencias Biol & Nat, BR-69910900 Rio Branco, AC, Brazil. [Ceron, Carlos E.] Univ Cent Ecuador, Herbario Alfredo Paredes QAP, Quito, Ecuador. [Chave, Jerome] Univ Toulouse 3, Lab EDB, F-31062 Toulouse, France. [Comiskey, James A.] Natl Pk Serv, Fredericksburg, VA USA. [Cornejo, Fernando] Univ Nacl Agr La Molina, Fac Ciencias Forest, Lima, Peru. [Corrales Medina, Massiel] Univ Nacl San Agustin de Arequipa, Arequipa, Peru. [Da Costa, Lola] Fed Univ Para, BR-66059 Belem, Para, Brazil. [Di Fiore, Anthony] Univ Texas Austin, Austin, TX 78712 USA. [Domingues, Tomas F.] Univ Sao Paulo, Dept Biol, FFCLRP USP, BR-05508090 Sao Paulo, Brazil. [Erwin, Terry L.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Frederickson, Todd] Ferrum Coll, Ferum, VA USA. [Honorio Coronado, Euridice N.] Inst Invest Amazonia Peruana, Iquitos, Peru. [Salomao, Rafael P.; Vieira, Ima C. G.] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [Killeen, Tim J.] World Wildlife Fund, Washington, DC 20037 USA. [Laurance, William F.] James Cook Univ, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld 4878, Australia. [Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. [Marimon, Beatriz S.; Marimon Junior, Ben Hur] Univ Estado Mato Grosso, BR-78690000 Nova Xavantina, MT, Brazil. [Mishra, Piyush] Indian Inst Technol, Dept Civil Engn, Roorkee 247667, Uttar Pradesh, India. [Nascimento, Marcelo T.] Univ Estadual Norte Fluminese, Ctr Biociencias & Biotecnol, Rio De Janeiro, Brazil. [Neill, David] Univ Estatal Amazon, Puyo, Pastaza, Ecuador. [Nunez Vargas, Mario P.] Univ Nacl San Antonio Abad Cusco, Cuzco, Peru. [Palacios, Walter A.; Vos, Vincent A.] Univ Tecn Norte, Escuela Ingn Forestal, Ibarra, Ecuador. [Pardo Molina, Guido] Univ Autonoma Beni, Riberalta, Beni, Bolivia. [Pena-Claros, Marielos; Poorter, Lourens] Wageningen Univ, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Pena-Claros, Marielos; Toledo, Marisol] Inst Boliviano Invest Forestal, Santa Cruz, Bolivia. [Pitman, Nigel] Duke Univ, Ctr Trop Conservat, Durham, NC 27708 USA. [Peres, Carlos A.] Univ E Anglia, Sch Environm Sci, Ctr Biodivers Res, Norwich NR4 7JT, Norfolk, England. [Prieto, Adriana] Univ Nacl Colombia, Inst Ciencias Nat, Bogota, Colombia. [Ramirez-Angulo, Hirma; Torres-Lezama, Armando; Vilanova-Torre, Emilio] Univ Los Andes, Merida, Venezuela. [Roopsind, Anand] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Rudas, Agustin] Univ Nacl Colombia, Leticia, Colombia. [Steininger, Marc K.] Conservat Int, Ctr Appl Biodivers Sci, Washington, DC USA. [Toledo, Marisol] Univ Autonoma Gabriel Rene Moreno, Santa Cruz, Bolivia. [van der Heijden, Geertje M. F.] Univ Wisconsin, Milwaukee, WI 53201 USA. [van der Heijden, Geertje M. F.] Smithsonian Trop Res Inst, Panama City, Panama. [Vieira, Simone] Univ Estadual Campinas, Nucleo Estudos & Pesquisas Ambientais, Campinas, SP, Brazil. [Wang, Ophelia] No Arizona Univ, Lab Landscape Ecol & Conservat Biol, Flagstaff, AZ 86011 USA. [Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Oxford, England. RP Mitchard, ETA (reprint author), Univ Edinburgh, Sch GeoSci, Crew Bldg,Kings Buildings, Edinburgh EH9 3JN, Midlothian, Scotland. EM edward.mitchard@ed.ac.uk RI Feldpausch, Ted/D-3436-2009; Peres, Carlos/B-1276-2013; Marimon, Beatriz/J-6389-2012; Brown, I. Foster/J-3766-2014; Domingues, Tomas/G-9707-2011; Lloyd, Jonathan/F-8893-2010; Phillips, Oliver/A-1523-2011; Magnusson, William/J-9408-2014; Marimon Junior, Ben Hur/E-7330-2013; James Cook University, TESS/B-8171-2012; Vieira, Simone/H-1225-2011; Research ID, CTBCC /O-3564-2014; Schietti, Juliana/B-8226-2015; icmol, icmol/I-5784-2015; Honorio Coronado, Euridice/K-3412-2015; ter Steege, Amaz/B-5866-2011 OI Nascimento, Marcelo/0000-0003-4492-3344; Feldpausch, Ted/0000-0002-6631-7962; Peres, Carlos/0000-0002-1588-8765; Brown, I. Foster/0000-0003-1877-0866; Mitchard, Edward/0000-0002-5690-4055; Vos, Vincent Antoine/0000-0002-0388-8530; Lewis, Simon/0000-0002-8066-6851; Domingues, Tomas/0000-0003-2857-9838; Lloyd, Jonathan/0000-0002-5458-9960; Phillips, Oliver/0000-0002-8993-6168; Vieira, Simone/0000-0002-0129-4181; Schietti, Juliana/0000-0002-1687-4373; Honorio Coronado, Euridice/0000-0003-2314-590X; ter Steege, Amaz/0000-0002-8738-2659 FU Gordon and Betty Moore Foundation; European Union [283080, 282664]; European Union (ERC); Natural Environment Research Council (NERC); NERC Consortium [NE/F005806/1, NE/D005590/1]; Tropical Ecology Assessment and Monitoring (TEAM) Network; Conservation International; Missouri Botanical Garden; Smithsonian Institution; Wildlife Conservation Society; PRONEX - FAPEAM/CNPq [1600/2006]; Hidroveg FAPESP/FAPEAM; Universal/CNPq [473308/2009-6]; INCT-CENBAM; Investissement d'Avenir grants of the French ANR [CEBA: ANR-10-LABX-0025, TULIP: ANR-10-LABX-0041]; CNPq/PELD [Proc. 558069/2009 -6]; NERC [NE/I021217/1, NE/I021160/1]; Royal Society; ERC; ARC [FT110100457 (FT3)] FX This paper is a product of the RAINFOR network, supported by a Gordon and Betty Moore Foundation grant, the European Union's Seventh Framework Programme (283080, 'GEOCARBON'; 282664, 'AMAZALERT'; ERC grant 'Tropical Forests in the Changing Earth System'), and Natural Environment Research Council (NERC) Urgency Grant and NERC Consortium Grants 'AMAZONICA' (NE/F005806/1) and 'TROBIT' (NE/D005590/1). Additional data were included from 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 partly funded by these institutions, the Gordon and Betty Moore Foundation, and other donors. The PPBio network was supported by PRONEX - FAPEAM/CNPq (1600/2006), Hidroveg FAPESP/FAPEAM, Universal/CNPq (473308/2009-6) and INCT-CENBAM. This work was partly supported by Investissement d'Avenir grants of the French ANR (CEBA: ANR-10-LABX-0025; TULIP: ANR-10-LABX-0041) and CNPq/PELD (Proc. 558069/2009 -6). E.M. and R.J.W.B. are funded independently by research fellowships from NERC (grant ref: NE/I021217/1 to E.M. and grant ref: NE/I021160/1 to R.J.W.B.). S.L.L. is funded by a Royal Society Fellowship. O.L.P. is supported by an ERC Advanced Grant and a Royal Society Wolfson Research Merit Award. P.M. is supported by ARC Future Fellowship FT110100457 (FT3). We thank Sassan Saatchi (NASA JPL) and Alessandro Baccini (Woods Hole Research Center) for providing their published carbon maps. This paper is 633 in the Technical Series of the Biological Dynamics of Forest Fragments Project (BDFFP-INPA/STRI). NR 38 TC 68 Z9 69 U1 11 U2 140 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X EI 1466-8238 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD AUG PY 2014 VL 23 IS 8 BP 935 EP 946 DI 10.1111/geb.12168 PG 12 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA AL4NT UT WOS:000339110400011 ER PT J AU Oftedal, OT Eisert, R Barrell, GK AF Oftedal, O. T. Eisert, R. Barrell, G. K. TI Comparison of analytical and predictive methods for water, protein, fat, sugar, and gross energy in marine mammal milk SO JOURNAL OF DAIRY SCIENCE LA English DT Article DE marine mammal milk; method validation; Dumas method; carbon stoichiometry ID BOTTLE-NOSED-DOLPHIN; PINNIPED LACTATION STRATEGIES; SEAL CYSTOPHORA-CRISTATA; ETHER EXTRACTION METHODS; PUSILLUS-DORIFERUS MILK; CAPE FUR SEALS; DAIRY-PRODUCTS; CHEMICAL-CHARACTERIZATION; KJELDAHL METHOD; TOTAL SOLIDS AB Mammalian milks may differ greatly in composition from cow milk, and these differences may affect the performance of analytical methods. High-fat, high-protein milks with a preponderance of oligosaccharides, such as those produced by many marine mammals, present a particular challenge. We compared the performance of several methods against reference procedures using Weddell seal (Leptonychotes weddellii) milk of highly varied composition (by reference methods: 27-63% water, 24-62% fat, 8-12% crude protein, 0.5-1.8% sugar). A microdrying step preparatory to carbon-hydrogen-nitrogen (CHN) gas analysis slightly underestimated water content and had a higher repeatability relative standard deviation (RSDr) than did reference oven drying at 100 C. Compared with a reference macro-Kjeldahl protein procedure, the CHN (or Dumas) combustion method had a somewhat higher RSDr (1.56 vs. 0.60%) but correlation between methods was high (0.992), means were not different (CHN: 17.2 +/- 0.46% dry matter basis; Kjeldahl 17.3 +/- 0.49% dry matter basis), there were no significant proportional or constant errors, and predictive performance was high. A carbon stoichiometric procedure based on CHN analysis failed to adequately predict fat (reference: Rose-Gottlieb method) or total sugar (reference: phenol-sulfuric acid method). Gross energy content, calculated from energetic factors and results from reference methods for fat, protein, and total sugar, 'accurately predicted gross energy as measured by bomb calorimetry. We conclude that the CHN (Dumas) combustion method and calculation of gross energy are acceptable analytical approaches for marine mammal milk, but fat and sugar require separate analysis by appropriate analytic methods and cannot be adequately estimated by carbon stoichiometry. Some other alternative methods low-temperature drying for water determination; Bradford, Lowry, and biuret methods for protein; the Folch and, the Bligh and Dyer methods for fat; and enzymatic and reducing sugar methods for total sugar appear likely to produce substantial error in marine mammal milks. It is important that alternative analytical methods be properly validated against a reference method before being used, especially for mammalian milks that differ greatly from cow milk in analyte characteristics and concentrations. C1 [Oftedal, O. T.; Eisert, R.] Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Eisert, R.] Univ Canterbury, Gateway Antarctica, Christchurch 8140, New Zealand. [Barrell, G. K.] Lincoln Univ, Fac Agr & Life Sci, Lincoln 7647, New Zealand. RP Oftedal, OT (reprint author), Smithsonian Inst, Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM oftedalo@si.edu FU Antarctica New Zealand; New Zealand Lotteries Science [AP52833]; Smithsonian Visiting Scholar grant; National Science Foundation-Office of Polar Programs grant [ANT-0538592] FX Field research on Weddell seal lactation was supported by Antarctica New Zealand (field logistics in 1998), New Zealand Lotteries Science Grants Board, a Science Research Grant no. AP52833 to G. K. Barre 11, a Smithsonian Visiting Scholar grant to R. Eisert, and a National Science Foundation-Office of Polar Programs grant ANT-0538592 to O. T. Oftedal, R. Eisert, and D. Boness. We thank our teams who assisted in the field in 1998 (J. Banks, D. Geddes, P. Isherwood, S. Leslie, B. Stewart, and H. Stoklosinski from Lincoln University, Lincoln New Zealand, and particularly S. Ramdohr from the Alfred-Wegener-Institute of Bremerhaven, Germany) and in 2006 (D. Boness, D. Boritt, R. Joss, B. Krafft, M. Lara, M. Riser, J. Robinson, and H. Routti from the Smithsonian Institution, Washington, DC). We also thank the staff at Scott Base and McMurdo Station for their support of our field efforts. We are grateful to laboratory manager M. Jakubasz for logistic and laboratory support at the Nutrition Laboratory of the Smithsonian National Zoological Park, and the interns and technicians who assisted with various aspects of milk analysis: J. Behler, D. Boen, S. Childs, M. Collins, R. Harley, D. Hellinga, K. Messerschmidt, L. Nelson, C. Petzinger, K. Roback, K. Smythe, M. Snyder, and S. Wong. We thank W. Hood, Auburn University (Auburn, AL) for her ideas about how best to estimate input factors for the stoichiometric procedure. NR 114 TC 2 Z9 3 U1 4 U2 62 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0022-0302 EI 1525-3198 J9 J DAIRY SCI JI J. Dairy Sci. PD AUG PY 2014 VL 97 IS 8 BP 4713 EP 4732 DI 10.3168/jds.2014-7895 PG 20 WC Agriculture, Dairy & Animal Science; Food Science & Technology SC Agriculture; Food Science & Technology GA AL1VB UT WOS:000338913300006 PM 24931527 ER PT J AU Flynn, CM Pickering, KE Crawford, JH Lamsal, L Krotkov, N Herman, J Weinheimer, A Chen, G Liu, X Szykman, J Tsay, SC Loughner, C Hains, J Lee, P Dickerson, RR Stehr, JW Brent, L AF Flynn, Clare M. Pickering, Kenneth E. Crawford, James H. Lamsal, Lok Krotkov, Nickolay Herman, Jay Weinheimer, Andrew Chen, Gao Liu, Xiong Szykman, James Tsay, Si-Chee Loughner, Christopher Hains, Jennifer Lee, Pius Dickerson, Russell R. Stehr, Jeffrey W. Brent, Lacey TI Relationship between column-density and surface mixing ratio: Statistical analysis of O-3 and NO2 data from the July 2011 Maryland DISCOVER-AQ mission SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Ozone; Nitrogen oxides; DISCOVER-AQ; Column-surface relationship; Aircraft measurement campaign; Measurement-model comparison ID TROPOSPHERIC OZONE; AIR-POLLUTANTS; UNITED-STATES; PART I; MODEL; SATELLITE; POLLUTION; LAYER; OMI AB To investigate the ability of column (or partial column) information to represent surface air quality, results of linear regression analyses between surface mixing ratio data and column abundances for O-3 and NO2 are presented for the July 2011 Maryland deployment of the DISCOVER-AQ mission. Data collected by the P-3B aircraft, ground-based Pandora spectrometers, Aura/OMI satellite instrument, and simulations for July 2011 from the CMAQ air quality model during this deployment provide a large and varied data set, allowing this problem to be approached from multiple perspectives. O-3 columns typically exhibited a statistically significant and high degree of correlation with surface data (R-2 > 0.64) in the P-3B data set, a moderate degree of correlation (0.16 < R-2 < 0.64) in the CMAQ data set, and a low degree of correlation (R-2 < 0.16) in the Pandora and OMI data sets. NO2 columns typically exhibited a low to moderate degree of correlation with surface data in each data set. The results of linear regression analyses for O-3 exhibited smaller errors relative to the observations than NO2 regressions. These results suggest that O-3 partial column observations from future satellite instruments with sufficient sensitivity to the lower troposphere can be meaningful for surface air quality analysis. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Flynn, Clare M.; Pickering, Kenneth E.; Dickerson, Russell R.; Stehr, Jeffrey W.; Brent, Lacey] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. [Pickering, Kenneth E.; Krotkov, Nickolay; Tsay, Si-Chee] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Crawford, James H.; Chen, Gao] NASA Langley Res Ctr, Hampton, VA USA. [Lamsal, Lok] NASA Goddard Space Flight Ctr, GESTAR, Greenbelt, MD USA. [Herman, Jay] NASA Goddard Space Flight Ctr, UMBC, Greenbelt, MD USA. [Weinheimer, Andrew] NCAR Atmospher Chem Div, Boulder, CO USA. [Liu, Xiong] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Szykman, James] EPA, Off Res & Dev, Washington, DC USA. [Loughner, Christopher] NASA Goddard Space Flight Ctr, ESSIC, Greenbelt, MD USA. [Hains, Jennifer] Maryland Dept Environm, Baltimore, MD 21224 USA. [Lee, Pius] NOAA Air Resources Lab, Silver Spring, MD USA. RP Flynn, CM (reprint author), Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. EM cflynn@atmos.umd.edu RI Liu, Xiong/P-7186-2014; Krotkov, Nickolay/E-1541-2012; Lee, Pius/D-5201-2016; Pickering, Kenneth/E-6274-2012; Dickerson, Russell/F-2857-2010; OI Liu, Xiong/0000-0003-2939-574X; Krotkov, Nickolay/0000-0001-6170-6750; Dickerson, Russell/0000-0003-0206-3083; Herman, Jay/0000-0002-9146-1632; Loughner, Christopher/0000-0002-3833-2014 FU NASA Earth Venture-1 DISCOVER-AQ project [NNX10AR39G] FX Funding for this work was provided by the NASA Earth Venture-1 DISCOVER-AQ project (NASA Grant NNX10AR39G). The authors thank Donald Lenschow for providing estimates of PBL height during the deployment. NR 34 TC 10 Z9 10 U1 4 U2 44 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD AUG PY 2014 VL 92 BP 429 EP 441 DI 10.1016/j.atmosenv.2014.04.041 PG 13 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA AL0IO UT WOS:000338810800045 ER PT J AU Soares, L Abad-Franch, F Ferraz, G AF Soares, Leticia Abad-Franch, Fernando Ferraz, Goncalo TI Epidemiology of cutaneous leishmaniasis in central Amazonia: a comparison of sex-biased incidence among rural settlers and field biologists SO TROPICAL MEDICINE & INTERNATIONAL HEALTH LA English DT Article DE Leishmania (Viannia) guyanensis; Phlebotominae; environmental exposure; Bayesian analysis ID VISCERAL LEISHMANIASIS; ECO-EPIDEMIOLOGY; IMMUNE-RESPONSE; BRAZIL; PROTECTION; INFECTION; HORMONES; DIPTERA; VIANNIA; ECUADOR AB OBJECTIVE Cutaneous leishmaniasis (CL) is more frequently reported in men than in women; this may be due to male-biased exposure to CL vectors, female-biased resistance against the disease or both. We sought to determine whether gender-specific exposure to vector habitats explains male-biased CL incidence in two human populations of central Amazonia. METHODS We compared the CL incidence in one population of field researchers (N = 166), with similar exposure for males and females, and one population of rural settlers (N = 646), where exposure is overall male-biased. We used a combination of questionnaires and clinical data to quantify CL cases, and modelled disease incidence in a Bayesian framework. RESULTS There was a moderately higher incidence of CL among men than among women in both populations, but male bias decreased as exposure time increased. Disease incidence was overall higher among field researchers, suggesting that they are an important but understudied CL risk group. CONCLUSION Our comparison of two contrasting populations provided epidemiological evidence that CL incidence can be male-biased even when exposure is comparable in both sexes. C1 [Soares, Leticia; Ferraz, Goncalo] Smithsonian Trop Res Inst, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [Soares, Leticia; Ferraz, Goncalo] Inst Nacl de Pesquisas da Amazonia, Manaus, Amazonas, Brazil. [Soares, Leticia; Ferraz, Goncalo] Inst Nacl de Pesquisas da Amazonia, Grad Program Ecol, Manaus, Amazonas, Brazil. [Soares, Leticia] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Abad-Franch, Fernando] Fiocruz Amazonia, Inst Leonidas & Maria Deane, Manaus, Amazonas, Brazil. [Ferraz, Goncalo] Univ Fed Rio Grande do Sul, Inst Biociencias, Dept Ecol, BR-90049 Porto Alegre, RS, Brazil. RP Soares, L (reprint author), Univ Missouri, Dept Biol, One Univ Blvd,Res Bldg, St Louis, MO 63121 USA. EM leticiassoares@gmail.com FU IDRC (Canada); CNPq (Brazil); FAPEAM (Brazil); Research Program on Infectious Disease Ecology in the Amazon of the Instituto Leonidas e Maria Deane (RP-IDEA, ILMD - Fiocruz (Brazil); Brazilian Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Research Program on Infectious Disease Ecology in the Amazon (RP-IDEA) of the Instituto Leonidas e Maria Deane [20]; Biological Dynamics of Forest Fragments Project (BDFFP) [642] FX Special thanks are due to Rio Pardo settlers and BDFFP field researchers who contributed to our CL epidemiological survey. Fieldwork was supported by grants from IDRC (Canada), CNPq (Brazil), FAPEAM (Brazil) and the Research Program on Infectious Disease Ecology in the Amazon of the Instituto Leonidas e Maria Deane (RP-IDEA, ILMD - Fiocruz (Brazil). Leticia Soares received a fellowship from the Brazilian Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) for MSc studies at the graduate program in Ecology of the Instituto Nacional de Pesquisas da Amazonia (INPA). We are very thankful to Eduardo Venticinque and Toby V Barrett, who provided fundamental ideas for this study. We are also grateful to Felipe AC Pessoa, Luis Fernando Chaves, Jacob Koella, Richard Reithinger, Aloisio Falqueto and Ana Rabello who kindly read and commented on the written version of LS's MSc project. This is contribution number 20 of the Research Program on Infectious Disease Ecology in the Amazon (RP-IDEA) of the Instituto Leonidas e Maria Deane, and contribution number 642 of the Biological Dynamics of Forest Fragments Project (BDFFP). NR 36 TC 1 Z9 2 U1 0 U2 4 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1360-2276 EI 1365-3156 J9 TROP MED INT HEALTH JI Trop. Med. Int. Health PD AUG PY 2014 VL 19 IS 8 BP 988 EP 995 DI 10.1111/tmi.12337 PG 8 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA AL2DR UT WOS:000338936600010 PM 24862350 ER PT J AU Clay, NA Yanoviak, SP Kaspari, M AF Clay, Natalie A. Yanoviak, Stephen P. Kaspari, Michael TI Short-term sodium inputs attract microbi-detritivores and their predators SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Nutritional ecology; Invertebrates; Tropical rainforest; Trophic ecology; Nutrient subsidies; Stable isotopes ID TROPICAL RAIN-FOREST; FOOD-WEB; LITTER DECOMPOSITION; SPECIES RICHNESS; ANT COMMUNITY; SELECTION; POPULATION; LIMITATION; AMAZON; CARBON AB Understanding individual nutritional requirements can generate good predictions for how communities should be structured over gradients of nutrient availability. Sodium (Na) bioaccumulates from plants to predators: it is relatively unimportant for plants, which concentrate very little Na in their tissues, but critical for consumers, which concentrate Na well above plant levels. Thus, plant consumers are likely Na-limited but their predators, which consume salty prey, are likely not. From this framework, we can make predictions about how an entire community should respond to Na subsidies in Na-poor environments. We tested these predictions in an interior Amazonian brown (detrital) food web. Specifically, we quantified the responses of microbi-detritivores and their predators to experimental pulses of Na by adding 250 ml 0.5% NaCl solution that mimicked patchy urine deposition, or river water as controls, to 55 paired 0.25 m(2) plots every other day. We regularly harvested plots over a 19 day period. Consistent with the hypothesis of Na-limitation among plant consumers, the response (effect size) to Na addition by microbi-detritivores like termites was >6 times that of predators. Moreover, consistent with the bioaccumulation of Na, fewer predatory invertebrates increased on +NaCI plots, thus trophic position alone was a good predictor of response. Our results support the Na bioaccumulation hypothesis and suggest that patchy, short-term Na inputs (like urine) facilitate heterogeneity in these leaf litter communities. Further, this study demonstrates that combining principles from nutritional and community ecology can generate predictions about how communities should be structured over gradients of nutrient availability with good accuracy. (C) 2014 Elsevier Ltd. All rights reserved. C1 [Clay, Natalie A.; Kaspari, Michael] Univ Oklahoma, Dept Biol, Grad Program Ecol & Evolutionary Biol, Norman, OK 73019 USA. [Yanoviak, Stephen P.] Univ Arkansas, Dept Biol, Little Rock, AR 72204 USA. [Kaspari, Michael] Smithsonian Trop Res Inst, Balboa, Panama. RP Clay, NA (reprint author), Univ Oklahoma, Dept Biol, 730 Van Vleet Oval, Norman, OK 73019 USA. EM naclay@ou.edu; Steve.Yanoviak@louisville.edu; mkaspari@ou.edu OI Kaspari, Michael/0000-0002-9717-5768 FU National Geographic Society; NSF [DEB-0948762] FX We thank the Amazon Conservatory for Tropical Studies, Pam Bucur, and Steve Madigosky for facilitating fieldwork and the Peruvian Instituto Nacional de Recursos Naturales for permits. Special thanks to Kendra Tholt, Michael O'Brien, and Deana Flat for assistance in the lab. Thanks to Don Shepard and Zoology Ecology and Evolutionary Biology Discussion Group for valuable discussions of this manuscript. Additionally, special thanks to Rick Maynard and the University of Oklahoma stable isotope facility, J. Kelly and E. Marsh-Matthews for the use of equipment. This project was funded by grants from the National Geographic Society and NSF DEB-0948762 to MEK. NR 60 TC 6 Z9 6 U1 7 U2 35 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD AUG PY 2014 VL 75 BP 248 EP 253 DI 10.1016/j.soilbio.2014.04.021 PG 6 WC Soil Science SC Agriculture GA AK7PG UT WOS:000338619600027 ER PT J AU Anker, A Baeza, A AF Anker, Arthur Baeza, Antonio TI Molecular and morphological phylogeny of hooded shrimps, genera Betaeus and Betaeopsis (Decapoda, Alpheidae): Testing the Center of Origin biogeographic model and evolution of life history traits (vol 64, pg 401, 2012) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Correction C1 [Anker, Arthur] Univ Fed Ceara, Inst Ciencias Mar Labomar, Fortaleza, Ceara, Brazil. [Baeza, Antonio] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Baeza, Antonio] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, Antonio] Univ Catalica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. RP Baeza, A (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. EM arthuranker7@yahoo.com; baezaa@si.edu NR 1 TC 0 Z9 0 U1 0 U2 8 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 2014 VL 77 BP 23 EP 24 DI 10.1016/j.ympev.2014.04.001 PG 2 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AJ8CH UT WOS:000337929800003 ER PT J AU Almeida, FC Giannini, NP Simmons, NB Helgen, KM AF Almeida, Francisca C. Giannini, Norberto P. Simmons, Nancy B. Helgen, Kristofer M. TI Each flying fox on its own branch: A phylogenetic tree for Pteropus and related genera (Chiroptera: Pteropodidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Pteropus; Pteropodidae; Chiroptera; Sequencing of museum specimens; Island taxa; Molecular phylogeny ID MAXIMUM-LIKELIHOOD; CYTOCHROME-B; CAROLINE ISLANDS; BATS CHIROPTERA; GENUS-PTEROPUS; SPECIES TREES; INDIAN-OCEAN; MIXED MODELS; VESPERTILIONIDAE; SYSTEMATICS AB Pteropodidae is a diverse Old World family of non-echolocating, frugivorous and nectarivorous bats that includes the flying foxes (genus Pteropus) and allied genera. The subfamily Pteropodinae includes the largest living bats and is distributed across an immense geographic range from islands in East Africa to the Cook Islands of Polynesia. These bats are keystone species in their ecosystems and some carry zoonotic diseases that are increasingly a focus of interest in biomedical research. Here we present a comprehensive phylogeny for pteropodines focused on Pteropus. The analyses included 50 of the similar to 63 species of Pteropus and 11 species from 7 related genera. We obtained sequences of the cytochrome b and the 12S rRNA mitochondrial genes for all species and sequences of the nuclear RAG1, vWF, and BRCA1 genes for a subsample of taxa. Some of the sequences of Pteropus were obtained from skin biopsies of museum specimens including that of an extinct species, P. tokudae. The resulting trees recovered Pteropus as monophyletic, although further work is needed to determine whether P. personatus belongs in the genus. Monophyly of the majority of traditionally-recognized Pteropus species groups was rejected, but statistical support was strong for several clades on which we based a new classification of the Pteropus species into 13 species groups. Other noteworthy results emerged regarding species status of several problematic taxa, including recognition of P. capistratus and P. ennisae as distinct species, paraphyly of the P. hypomelanus complex, and conspecific status of P. pelewensis pelewensis and P. p. yapensis. Relationships among the pteropodine genera were not completely resolved with the current dataset. Divergence time analysis suggests that Pteropus originated in the Miocene and that two independent bursts of diversification occurred in the Pleistocene in different regions of the Indo-Pacific realm. (C) 2014 The Authors. Published by Elsevier Inc. C1 [Almeida, Francisca C.; Giannini, Norberto P.; Simmons, Nancy B.] Amer Museum Nat Hist, Div Vertebrate Zool, Dept Mammal, New York, NY 10024 USA. [Almeida, Francisca C.; Giannini, Norberto P.] Univ Nacl Tucuman, Fac Ciencias Nat, CONICET, Consejo Nacl Invest Cient & Tecnol, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. [Giannini, Norberto P.] Inst Miguel Lillo, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. RP Almeida, FC (reprint author), Univ Nacl Tucuman, Fac Ciencias Nat, CONICET, Consejo Nacl Invest Cient & Tecnol, RA-4000 San Miguel De Tucuman, Tucuman, Argentina. EM falmeida@nyu.edu; ngiannini@amnh.org; simmons@amnh.org; helgenk@si.edu OI Simmons, Nancy B./0000-0001-8807-7499 FU National Science Foundation [DEB-9873663]; National Institute of Allergy and Infectious Diseases [1R21A/105050]; Vernay Postdoctoral Fellowship FX For access to specimens under their care, loan of tissues, and other assistance during museum visits we thank S. Ingleby, D. Lunde, D. Wilson, L. Emmons, L. Gordon, E. Westwig, N. Duncan, R. Voss, J. Wible, S. McLaren, P. Jenkins, R. Portela Miguez, J. Patton, C. Conroy, C. Smeenk, W. Bergmans, B. Stanley, L. Heaney, B. Patterson, P. Giere, R. Asher, I. Thomas, J. Chupasko, E. Gilmore, J. Dines, K. Lim, Maharadatunlcamsi, M. Sinaga, I. Maryanto, G. Doria, J. Eger, and B. Lim. We thank Simone Loss and Kara Kaminski for their invaluable help with the molecular protocols. For helpful discussion we thank T. Flannery, S. Donnellan, K. Aplin, S. Tsang, K. Olival, and L. Helgen. K. Olival kindly made available the photos we used in the graphical abstract. This contribution was based upon work supported in part by the National Science Foundation under Grant No. DEB-9873663 and by the National Institute of Allergy and Infectious Diseases under Grant No. 1R21A/105050 to N. Simmons, and a Vernay Postdoctoral Fellowship to F. Almeida (AMNH). Travel for museum specimen comparisons was funded in part by the Smithsonian Institution and the South Australian Museum. NR 70 TC 16 Z9 17 U1 11 U2 83 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 2014 VL 77 BP 83 EP 95 DI 10.1016/j.ympev.2014.03.009 PG 13 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AJ8CH UT WOS:000337929800010 PM 24662680 ER PT J AU Hultgren, KM Hurt, C Anker, A AF Hultgren, Kristin M. Hurt, Carla Anker, Arthur TI Phylogenetic relationships within the snapping shrimp genus Synalpheus (Decapoda: Alpheidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Synalpheus; Phylogeny; Alpheidae; Snapping shrimp; Cryptic species ID SPONGE-DWELLING SHRIMPS; CRYPTIC DIVERSITY; BIOLOGICAL IDENTIFICATIONS; SPECIES DELIMITATION; MOLECULAR PHYLOGENY; INDO-PACIFIC; DNA BARCODES; CRUSTACEA; RADIATION; PATTERNS AB The snapping shrimp genus Synalpheus (Alpheidae) is one of the most speciose decapod genera, with over 160 described species worldwide. Most species live in symbiotic relationships with other marine organisms, such as sponges, corals and crinoids, and some sponge-dwelling species have a highly organized, social structure. The present study is the first worldwide molecular phylogenetic analysis of Synalpheus, based on >2200 bp of sequence data from two mitochondrial (COI and 16S) and two nuclear (PEPCK and 18S) loci. Our molecular data show strong support for monophyly of three out of six traditionally recognized morphology-based species groups: the S. brevicarpus; S. comatularum and S. gambarelloides groups. The remaining three species groups (S. paulsoni, S. neomeris and S. coutierei groups) are non-monophyletic in their current composition and will need to be either abandoned or taxonomically redefined. We also identified potential cryptic species of Synalpheus in our dataset, using intraspecific and interspecific sequence variation in COI from the taxonomically well-studied S. gambarelloides group to establish a genetic divergence threshold. We then used both genetic divergence and tree-based criteria (reciprocal monophyly) to identify potential cryptic species in the remaining taxa of the genus. Our results suggest the presence of multiple cryptic lineages in Synalpheus, underlining the need for more integrative taxonomic studies including morphological, ecological, molecular, and color pattern data in this biologically interesting genus. (C) 2014 Elsevier Inc. All rights reserved. C1 [Hultgren, Kristin M.] Seattle Univ, Dept Biol, Seattle, WA 98122 USA. [Hultgren, Kristin M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hurt, Carla] Univ Miami, Dept Biol, Coral Gables, FL 33143 USA. [Anker, Arthur] Natl Univ Singapore, Trop Marine Sci Inst, Singapore 119227, Singapore. [Hurt, Carla] Tennessee Technol Univ, Dept Biol, Cookeville, TN 38505 USA. RP Hultgren, KM (reprint author), Seattle Univ, Dept Biol, Seattle, WA 98122 USA. EM hultgrenk@seattleu.edu FU Wolcott funds at the Smithsonian Institution; Smithsonian Tropical Research Institute (STRI) FX Funding for this study, including support of KH and CH, was provided by Wolcott funds at the Smithsonian Institution. This study could not have been done without the support of Nancy Knowlton (National Museum of Natural History, Smithsonian Institution). This study also benefited greatly from the taxonomic expertise and collections of J. Emmett Duffy (Virginia Institute of Marine Studies). Dr. Amy Driskell (Smithsonian Laboratory of Analytical Biology) provided assistance with barcoding and database management. Early drafts of the manuscript were improved by the comments of two anonymous reviewers. Most of the Indo-West Pacific material used in this study was collected during BIOTAS (Madagascar, Reunion Island) and BIOCODE (French Polynesia) expeditions co-organized by Gustav Paulay (Florida Museum of Natural History). The Panamanian material was collected with support from the Smithsonian Tropical Research Institute (STRI); collection permits were issued by the ANAM. The Sao Tomean material was collected with permits from the Fisheries Department (Direccao das Pescas) of Sao Tome and Principe. NR 77 TC 9 Z9 12 U1 0 U2 31 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 2014 VL 77 BP 116 EP 125 DI 10.1016/j.ympev.2014.03.008 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AJ8CH UT WOS:000337929800013 PM 24680914 ER PT J AU Zhang, JQ Meng, SY Allen, GA Wen, J Rao, GY AF Zhang, Jian-Qiang Meng, Shi-Yong Allen, Geraldine A. Wen, Jun Rao, Guang-Yuan TI Rapid radiation and dispersal out of the Qinghai-Tibetan Plateau of an alpine plant lineage Rhodiola (Crassulaceae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Rhodiola; Qinghai-Tibetan Plateau; Rapid radiation; Ancestral distribution; Divergence time; Reticulate evolution ID EASTERN NORTH-AMERICA; CHLOROPLAST DNA; PHYLOGENETIC-RELATIONSHIPS; MOLECULAR PHYLOGENY; MAXIMUM-LIKELIHOOD; NONCODING REGIONS; ADJACENT REGIONS; GEOGRAPHIC RANGE; PINUS-DENSATA; EVOLUTION AB Rhodiola L. (Crassulaceae) is a mid-sized plant genus consisting of about 70 species, with most species distributed on the Qinghai-Tibetan Plateau (QTP) and the adjacent areas, and several species in north-east Asia, Europe, and North America. This study explored the origin and diversification history of Rhodiola and tested the biogeographic relationships between the QTP and other regions of the Northern Hemisphere. We sequenced the nuclear ribosomal internal transcribed spacers and eight plastid DNA fragments representing 55 species of Rhodiola, and reconstructed phylogenetic relationships with maximum parsimony, maximum likelihood and Bayesian inference. Several instances of incongruence between the nuclear and the plastid data sets were revealed, which can best be explained by reticulate evolution. Species of Rhodiola and Pseudosedum form a well-supported clade sister to Phedimus. Dating analysis suggested that the origin and diversification times of this group are largely correlated with the extensive uplifts of the Qinghai-Tibetan Plateau. Ancestral state reconstruction supports the hypothesis that Rhodiola originated on the QTP, and then dispersed to other regions of the Northern Hemisphere. Our findings highlight the importance of the uplifts of the Qinghai-Tibetan Plateau in promoting species diversification and the possible role of reticulate evolution in the diversification process. Our results also suggest the biogeographic significance of QTP as the source area in alpine plant evolution in the Northern Hemisphere. (C) 2014 Elsevier Inc. All rights reserved. C1 [Zhang, Jian-Qiang; Meng, Shi-Yong; Rao, Guang-Yuan] Peking Univ, Coll Life Sci, Beijing 100871, Peoples R China. [Allen, Geraldine A.] Univ Victoria, Dept Biol, Victoria, BC V8W 3N5, Canada. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu; rao@pku.edu.cn RI Allen, Geraldine/D-9254-2013 OI Allen, Geraldine/0000-0001-7138-9090 FU State Key Laboratory of Systematic and Evolutionary Botany (LSEB) of China [LSEB2009-06]; Laboratory of Analytical Biology of the National Museum of Natural History; Smithsonian Institution; China Scholarship Council [201206010113] FX The authors thank Yiming An and Dongqing Zhang for field assistance, Gabriel Johnson and Matt Kweskin for assistance in the lab and in data analyses, and Ms. Margret (Magga) Hauksdottir for her kind assistance with the sample of Rhodiola semenovii. This study was supported by the Open Project Program of the State Key Laboratory of Systematic and Evolutionary Botany (LSEB) of China (Grant Number: LSEB2009-06), and the Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. Jianqiang Zhang has been supported by a scholarship for exchanging Ph.D. candidates from the China Scholarship Council (No. 201206010113) for his studies at the Smithsonian Institution. The study represents part of Jianqiang Zhang's dissertation research. NR 126 TC 22 Z9 23 U1 15 U2 90 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 2014 VL 77 BP 147 EP 158 DI 10.1016/j.ympev.2014.04.013 PG 12 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AJ8CH UT WOS:000337929800016 PM 24780751 ER PT J AU Wirshing, HH Baker, AC AF Wirshing, Herman H. Baker, Andrew C. TI Molecular evolution of calcification genes in morphologically similar but phylogenetically unrelated scleractinian corals SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Scleractinia; Biomineralization; Phylogenetics; Carbonic anhydrase; Bone morphogenic protein (BMP) ID REEF-BUILDING CORALS; CARBONIC-ANHYDRASE; MAXIMUM-LIKELIHOOD; ACROPORA-MILLEPORA; DIFFERENTIAL EXPRESSION; STYLOPHORA-PISTILLATA; DNA POLYMORPHISM; TREE SELECTION; ORGANIC MATRIX; SKELETONS AB Molecular phylogenies of scleractinian corals often fail to agree with traditional phylogenies derived from morphological characters. These discrepancies are generally attributed to non-homologous or morphologically plastic characters used in taxonomic descriptions. Consequently, morphological convergence of coral skeletons among phylogenetically unrelated groups is considered to be the major evolutionary process confounding molecular and morphological hypotheses. A strategy that may help identify cases of convergence and/or diversification in coral morphology is to compare phylogenies of existing "neutral" genetic markers used to estimate genealogic phylogenetic history with phylogenies generated from non-neutral genes involved in calcification (biomineralization). We tested the hypothesis that differences among calcification gene phylogenies with respect to the "neutral" trees may represent convergent or divergent functional strategies among calcification gene proteins that may correlate to aspects of coral skeletal morphology. Partial sequences of two nuclear genes previously determined to be involved in the calcification process in corals, "Cnidaria-III" membrane-bound/secreted alpha-carbonic anhydrase (CIII-MBS alpha-CA) and bone morphogenic protein (BMP) 2/4, were PCR-amplified, cloned and sequenced from 31 scleractinian coral species in 26 genera and 9 families. For comparison, "neutral" gene phylogenies were generated from sequences from two protein-coding "non-calcification" genes, one nuclear (beta-tubulin) and one mitochondrial (cytochrome b), from the same individuals. Cloned CIII-MBS alpha-CA sequences were found to be non-neutral, and phylogenetic analyses revealed CIII-MBS alpha-CAs to exhibit a complex evolutionary history with clones distributed between at least 2 putative gene copies. However, for several coral taxa only one gene copy was recovered. With CIII-MBSa-CA, several recovered clades grouped taxa that differed from the "non-calcification" loci. In some cases, these taxa shared aspects of their skeletal morphology (i.e., convergence or diversification relative to the "non-calcification" loci), but in other cases they did not. For example, the "non-calcification" loci recovered Atlantic and Pacific mussids as separate evolutionary lineages, whereas with CIII-MBSa-CA, clones of two species of Atlantic mussids (Isophyllia sinuosa and Mycetophyllia sp.) and two species of Pacific mussids (Acanthastrea echinata and Lobophyllia hemprichii) were united in a distinct clade (except for one individual of Mycetophyllia). However, this clade also contained other taxa which were not unambiguously correlated with morphological features. BMP2/4 also contained clones that likely represent different gene copies. However, many of the sequences showed no significant deviation from neutrality, and reconstructed phylogenies were similar to the "non-calcification" tree topologies with a few exceptions. Although individual calcification genes are unlikely to precisely explain the diverse morphological features exhibited by scleractinian corals, this study demonstrates an approach for identifying cases where morphological taxonomy may have been misled by convergent and/or divergent molecular evolutionary processes in corals. Studies such as this may help illuminate our understanding of the likely complex evolution of genes involved in the calcification process, and enhance our knowledge of the natural history and biodiversity within this central ecological group. Published by Elsevier Inc. C1 [Wirshing, Herman H.; Baker, Andrew C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. RP Wirshing, HH (reprint author), Smithsonian Inst, POB 37012,MRC 163, Washington, DC 20013 USA. EM wirshingh@si.edu FU Rowlands and Knight Graduate Fellowships at the University of Miami's Rosenstiel School of Marine and Atmospheric Science; U.S. National Science Foundation [OCE-0527184] FX We would like to thank D. Crawford and A. Wilson for their invaluable advice during the early stages of this project and on the development of the manuscript, C. Starger and R. Bahgooli for help collecting field samples, and two anonymous reviewers whose advice greatly improved the manuscript. This study was supported by funding from the Rowlands and Knight Graduate Fellowships at the University of Miami's Rosenstiel School of Marine and Atmospheric Science, and by a grant from the U.S. National Science Foundation (OCE-0527184 to A. Baker and C. Langdon). NR 82 TC 3 Z9 3 U1 4 U2 44 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 2014 VL 77 BP 281 EP 295 DI 10.1016/j.ympev.2014.04.015 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA AJ8CH UT WOS:000337929800028 PM 24780747 ER PT J AU Thomsen, O Collin, R Carrillo-Baltodano, A AF Thomsen, Olaf Collin, Rachel Carrillo-Baltodano, Allan TI The Effects of Experimentally Induced Adelphophagy in Gastropod Embryos SO PLOS ONE LA English DT Article ID NURSE EGGS; CALYPTRAEID GASTROPODS; MARINE-INVERTEBRATES; NORTHERN CHILE; HATCHING SIZE; VERMETID GASTROPOD; CREPIDULA-DILATATA; LARVAL DEVELOPMENT; SEX-CHANGE; REPRODUCTION AB Adelphophagy, development where embryos grow large by consuming morphologically distinct nutritive embryos or their own normal siblings is widespread but uncommon among animal phyla. Among invertebrates it is particularly common in some families of marine gastropods and segmented worms, but rare or unknown in other closely related families. In calyptraeid gastropods phylogenetic analysis indicates that adelphophagy has arisen at least 9 times from species with planktotrophic larval development. This pattern of frequent parallel evolution of adelphophagy suggests that the embryos of planktotrophic species might be predisposed to evolve adelphophagy. Here we used embryos of three species of planktotrophic calyptraeids, one from each of three major genera in the family (Bostrycapulus, Crucibulum, and Crepidula), to answer the following 3 questions: (1) Can embryos of species with planktotrophic development benefit, in terms of pre-hatching growth, from the ingestion of yolk and tissue from experimentally damaged siblings? (2) Does ingestion of this material from damaged siblings increase variation in pre-hatching size? and (3) Does this experimentally induced adelphophagy alter the allometry between the velum and the shell, increasing morphological similarity to embryos of normally adelphophagic species? We found an overall increase in shell length and velum diameter when embryos feed on damaged siblings within their capsules. There was no detectable increase in variation in shell length or velum diameter, or changes in allometry. The overall effect of our treatment was small compared to the embryonic growth observed in naturally adelphophagic development. However each embryo in our experiment probably consumed less than one sibling on average, whereas natural adelphophages often each consume 10-30 or more siblings. These results suggest that the ability to consume, assimilate, and benefit from yolk and tissue of their siblings is widespread across calyptraeids. C1 [Thomsen, Olaf; Collin, Rachel; Carrillo-Baltodano, Allan] Smithsonian Trop Res Inst, Balboa, Panama. [Thomsen, Olaf] Carl von Ossietzky Univ Oldenburg, D-26111 Oldenburg, Germany. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM collinr@si.edu OI Collin, Rachel/0000-0001-5103-4460 FU United States National Science Foundation [IOS 1019727]; Smithsonian Tropical Research Institute FX This research was supported by United States National Science Foundation grant IOS 1019727 to R. Collin and the Smithsonian Tropical Research Institute. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 41 TC 3 Z9 3 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 29 PY 2014 VL 9 IS 7 AR e103366 DI 10.1371/journal.pone.0103366 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO4KU UT WOS:000341307600043 PM 25072671 ER PT J AU Tang, LY Yan, ZC Shi, TY Babb, JF AF Tang, Li-Yan Yan, Zong-Chao Shi, Ting-Yun Babb, James F. TI High-precision nonadiabatic calculations of dynamic polarizabilities and hyperpolarizabilities for low-lying vibrational-rotational states of hydrogen molecular ions SO PHYSICAL REVIEW A LA English DT Article ID BORN-OPPENHEIMER APPROXIMATION; FUNDAMENTAL PHYSICAL CONSTANTS; INFRARED-LASER SPECTROSCOPY; CODATA RECOMMENDED VALUES; ANGULAR-MOMENTUM STATES; D2 RYDBERG STATES; DIPOLE POLARIZABILITIES; MICROWAVE SPECTROSCOPY; POLARIZATION MODEL; H-2 AB The static and dynamic electric multipolar polarizabilities and second hyperpolarizabilities of the H-2(+), D-2(+), and HD+ molecular ions in the ground and first excited states are calculated nonrelativistically using explicitly correlated Hylleraas basis sets. The calculations are fully nonadiabatic; the Born-Oppenheimer approximation is not used. Comparisons are made with published theoretical and experimental results, where available. In our approach, no derivatives of energy functions nor derivatives of response functions are needed. In particular, we make contact with earlier calculations in the Born-Oppenheimer calculation where polarizabilities were decomposed into electronic, vibrational, and rotational contributions and where hyperpolarizabilities were determined from derivatives of energy functions. We find that the static hyperpolarizability for the ground state of HD+ is seven orders of magnitude larger than the corresponding dipole polarizability. For the dipole polarizability of HD+ in the first excited state the high precision of the present method facilitates treatment of a near cancellation between two terms. For applications to laser spectroscopy of trapped ions we find tune-out and magic wavelengths for the HD+ ion in a laser field. In addition, we also calculate the first few leading terms for long-range interactions of a hydrogen molecular ion and a ground state H, He, or Li atom. C1 [Tang, Li-Yan; Yan, Zong-Chao; Shi, Ting-Yun] Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China. [Tang, Li-Yan; Yan, Zong-Chao; Shi, Ting-Yun] Chinese Acad Sci, Wuhan Inst Phys & Math, Ctr Cold Atom Phys, Wuhan 430071, Peoples R China. [Tang, Li-Yan; Yan, Zong-Chao; Babb, James F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Yan, Zong-Chao] Univ New Brunswick, Dept Phys, Fredericton, NB E3B 5A3, Canada. RP Tang, LY (reprint author), Chinese Acad Sci, Wuhan Inst Phys & Math, State Key Lab Magnet Resonance & Atom & Mol Phys, Wuhan 430071, Peoples R China. OI Babb, James/0000-0002-3883-9501 FU National Basic Research Program of China [2010CB832803, 2012CB821305]; NNSF of China [11104323, 11274348]; NSERC of Canada; CAS/SAFEA International Partnership Program for Creative Research Teams; NSF to the Smithsonian Astrophysical Observatory; Harvard University FX We are grateful to Prof. J. Mitroy for comments and to Prof. W.G. Sturrus for helpful correspondence. This work was supported by the National Basic Research Program of China under Grants No. 2010CB832803 and No. 2012CB821305 and by NNSF of China under Grants No. 11104323 and No. 11274348. Z.-C.Y. was supported by NSERC of Canada and by the computing facilities of ACEnet and SHARCnet, and in part by the CAS/SAFEA International Partnership Program for Creative Research Teams. ITAMP is supported in part by a grant from the NSF to the Smithsonian Astrophysical Observatory and Harvard University NR 59 TC 7 Z9 7 U1 1 U2 32 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 29 PY 2014 VL 90 IS 1 AR 012524 DI 10.1103/PhysRevA.90.012524 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA AO4LN UT WOS:000341309900005 ER PT J AU Kokkin, DL Reilly, NJ Fortenberry, RC Crawford, TD McCarthy, MC AF Kokkin, D. L. Reilly, N. J. Fortenberry, R. C. Crawford, T. D. McCarthy, M. C. TI Optical spectra of the silicon-terminated carbon chain radicals SiCnH (n=3,4,5) SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID COUPLED-CLUSTER METHODS; SHELL HARTREE-FOCK; CORRELATED MOLECULAR CALCULATIONS; GAUSSIAN-BASIS SETS; ELECTRONIC SPECTROSCOPY; EXCITED-STATES; INTERSTELLAR CHEMISTRY; EXCITATION-ENERGIES; TRIPLE EXCITATIONS; ROTATIONAL SPECTRA AB The gas-phase optical spectra of three silicon-terminated carbon chain radicals, SiCnH (n = 3 - 5), formed in a jet-cooled discharge of silane and acetylene, have been investigated by resonant two-color two-photon ionization and laser-induced fluorescence/dispersed fluorescence. Analysis of the spectra was facilitated by calculations performed using equation-of-motion coupled cluster methods. For SiC3H and SiC5H, the observed transitions are well-described as excitations from a (2)Pi ground state to a (2)Pi state, in which vibronic coupling, likely involving a higher-lying Pi state with a very large predicted f-value (close to unity), is persistent. The lowest (2)Sigma states of both species are characterized by a rare silicon triple bond, which was identified previously [T. C. Smith, H. Y. Li, D. J. Clouthier, C. T. Kingston, and A. J. Merer, J. Chem. Phys. 112, 3662 (2000)] in the lowest (2)Sigma state of SiCH. Although a strong Pi - Pi transition is predicted for SiC4H, the observed spectrum near 505 nm more likely corresponds to excitation to a relatively dark Sigma state which is vibronically coupled to a nearby Pi state. In contrast to the chains with an odd number of carbon atoms, which exhibit relatively sharp spectral features and lifetimes in the 10-100 ns range, SiC4H shows intrinsically broadened spectral features consistent with a similar to 100 fs lifetime, and a subsequent long-lived decay (>50 mu s) which we ascribe to mixing with a nearby quartet state arising from the same electronic configuration. The spin-orbit coupling constants for both SiC3H and SiC5H radicals were determined to be approximately 64 cm(-1), similar to that of SiCH (69.8 cm(-1)), suggesting that the unpaired electron in these species is localized on the silicon atom. Motivated by the new optical work, the rotational spectrum of linear SiC3H was detected by cavity Fourier-transform microwave spectroscopy in the 13-34 GHz range. Each rotational transition from the (2)Pi(3/2) ground state exhibits well-resolved Lambda-doubling and hyperfine structure; the derived rotational constant of B = 2.605 GHz is in excellent agreement with our calculations. (C) 2014 AIP Publishing LLC. C1 [Kokkin, D. L.; Reilly, N. J.; McCarthy, M. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kokkin, D. L.; Reilly, N. J.; McCarthy, M. C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Fortenberry, R. C.; Crawford, T. D.] Virginia Tech, Dept Chem, Blacksburg, VA 24061 USA. RP McCarthy, MC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mccarthy@cfa.harvard.edu RI Crawford, Thomas/A-9271-2017; OI Crawford, Thomas/0000-0002-7961-7016; McCarthy, Michael/0000-0001-9142-0008 FU NSF [CHE-1058063]; NASA [NNX13AE59G]; U.S. National Science Foundation [CHE-1058420, CHE-0741927]; Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU); Virginia Space Grant Consortium FX The work in Cambridge is supported by NSF Grant No. CHE-1058063 and NASA Grant No. NNX13AE59G. Support for T. D. C. and R. C. F. is provided by the U.S. National Science Foundation Award No. CHE-1058420 and by Award No. CHE-0741927 (T. D. C.): a Multi-User Chemistry Research Instrumentation and Facility (CRIF:MU). The molecular structures in Fig. 7 were generated with the JMOL program, and Fig. 8 was generated with the CheMVP program developed at the Center for Computational and Quantum Chemistry at the University of Georgia. R. C. F. also wishes to thank the Virginia Space Grant Consortium for a Graduate Research Fellowship part of which was allocated during the time of this research. The authors would like to thank John Stanton for helpful discussions of this work. NR 68 TC 8 Z9 8 U1 2 U2 16 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 JUL 28 PY 2014 VL 141 IS 4 AR 044310 DI 10.1063/1.4883521 PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA AN6NT UT WOS:000340712200047 PM 25084913 ER PT J AU Grayson, DK Meltzer, DJ Buikstra, JE Flannery, KV Fowler, CS Marcus, J O'Connell, JF Piperno, DR Sabloff, JA Smith, BD Thomas, DH Willerslev, E Zeder, MA AF Grayson, D. K. Meltzer, D. J. Buikstra, J. E. Flannery, K. V. Fowler, C. S. Marcus, J. O'Connell, J. F. Piperno, D. R. Sabloff, J. A. Smith, B. D. Thomas, D. H. Willerslev, E. Zeder, M. A. TI Early Americans: Respecting ancestors SO SCIENCE LA English DT Letter C1 [Grayson, D. K.] Univ Washington, Dept Anthropol, Seattle, WA 98185 USA. [Grayson, D. K.] Univ Washington, Quaternary Res Ctr, Seattle, WA 98185 USA. [Meltzer, D. J.] So Methodist Univ, Dept Anthropol, Dallas, TX 75275 USA. [Buikstra, J. E.] Arizona State Univ, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Flannery, K. V.; Marcus, J.] Univ Michigan, Museum Anthropol Archaeol, Ann Arbor, MI 48109 USA. [Fowler, C. S.] Univ Nevada, Dept Anthropol, Reno, NV 89557 USA. [O'Connell, J. F.] Univ Utah, Dept Anthropol, Salt Lake City, UT 84112 USA. [Piperno, D. R.; Smith, B. D.; Zeder, M. A.] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Piperno, D. R.] Smithsonian Inst, Natl Museum Nat Hist, Smithsonian Trop Res Inst Panama, Washington, DC 20560 USA. [Sabloff, J. A.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Thomas, D. H.] Amer Museum Nat Hist, Div Anthropol, New York, NY 10024 USA. [Willerslev, E.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr GeoGenet, DK-1350 Copenhagen K, Denmark. RP Grayson, DK (reprint author), Univ Washington, Dept Anthropol, Seattle, WA 98185 USA. EM grayson@uw.edu NR 0 TC 0 Z9 0 U1 2 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 25 PY 2014 VL 345 IS 6195 BP 390 EP 390 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM2CB UT WOS:000339655100026 PM 25061197 ER PT J AU Donovan, MP Wilf, P Labandeira, CC Johnson, KR Peppe, DJ AF Donovan, Michael P. Wilf, Peter Labandeira, Conrad C. Johnson, Kirk R. Peppe, Daniel J. TI Novel Insect Leaf-Mining after the End-Cretaceous Extinction and the Demise of Cretaceous Leaf Miners, Great Plains, USA SO PLOS ONE LA English DT Article ID CHICXULUB IMPACT EVENT; TERTIARY BOUNDARY; LATE PALEOCENE; EARLY EOCENE; NORTH-AMERICA; HYMENOPTERA TENTHREDINIDAE; HERBIVOROUS INSECTS; PALEOGENE BOUNDARY; TROPICAL FORESTS; THERMAL MAXIMUM AB Plant and associated insect-damage diversity in the western U. S. A. decreased significantly at the Cretaceous-Paleogene (K-Pg) boundary and remained low until the late Paleocene. However, the Mexican Hat locality (ca. 65 Ma) in southeastern Montana, with a typical, low-diversity flora, uniquely exhibits high damage diversity on nearly all its host plants, when compared to all known local and regional early Paleocene sites. The same plant species show minimal damage elsewhere during the early Paleocene. We asked whether the high insect damage diversity at Mexican Hat was more likely related to the survival of Cretaceous insects from refugia or to an influx of novel Paleocene taxa. We compared damage on 1073 leaf fossils from Mexican Hat to over 9000 terminal Cretaceous leaf fossils from the Hell Creek Formation of nearby southwestern North Dakota and to over 9000 Paleocene leaf fossils from the Fort Union Formation in North Dakota, Montana, and Wyoming. We described the entire insect-feeding ichnofauna at Mexican Hat and focused our analysis on leaf mines because they are typically host-specialized and preserve a number of diagnostic morphological characters. Nine mine damage types attributable to three of the four orders of leaf-mining insects are found at Mexican Hat, six of them so far unique to the site. We found no evidence linking any of the diverse Hell Creek mines with those found at Mexican Hat, nor for the survival of any Cretaceous leaf miners over the K-Pg boundary regionally, even on well-sampled, surviving plant families. Overall, our results strongly relate the high damage diversity on the depauperate Mexican Hat flora to an influx of novel insect herbivores during the early Paleocene, possibly caused by a transient warming event and range expansion, and indicate drastic extinction rather than survivorship of Cretaceous insect taxa from refugia. C1 [Donovan, Michael P.; Wilf, Peter] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. [Johnson, Kirk R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Peppe, Daniel J.] Baylor Univ, Dept Geol, Waco, TX 76798 USA. RP Donovan, MP (reprint author), Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. EM mpd187@psu.edu RI Peppe, Daniel/E-8449-2011 OI Peppe, Daniel/0000-0003-4263-133X FU Geological Society of America; Paleontological Society of America; P.D. Krynine Memorial Fund, Penn State Department of Geosciences; American Philosophical Society; David and Lucile Packard Fellowship; NSF [DEB-0919071] FX This study was supported by a Geological Society of America Student Research Grant, a Paleontological Society of America Student Research Grant, and the P.D. Krynine Memorial Fund, Penn State Department of Geosciences (MPD). Additional funding was provided by the American Philosophical Society, a David and Lucile Packard Fellowship, and NSF Grant DEB-0919071 (PW). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 121 TC 5 Z9 5 U1 1 U2 10 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 24 PY 2014 VL 9 IS 7 AR e103542 DI 10.1371/journal.pone.0103542 PG 35 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AO5BG UT WOS:000341354800105 PM 25058404 ER PT J AU Tadhunter, C Morganti, R Rose, M Oonk, JBR Oosterloo, T AF Tadhunter, C. Morganti, R. Rose, M. Oonk, J. B. R. Oosterloo, T. TI Jet acceleration of the fast molecular outflows in the Seyfert galaxy IC 5063 SO NATURE LA English DT Article ID RADIO GALAXIES; STAR-FORMATION; BLACK-HOLES; COLD GAS; FEEDBACK; EMISSION; QUASARS; NUCLEUS; GROWTH; WARM AB Massive outflows driven by active galactic nuclei are widely recognized to have a key role in the evolution of galaxies(1-4), by heating the ambient gas, expelling it from the nuclear regions, and thereby affecting the star-formation histories of the galaxy bulges. It has been proposed that the powerful jets of relativistic particles (such as electrons) launched by some active nuclei can both accelerate(5-7) and heat(8) the molecular gas, which often dominates the mass budgets of the outflows(5,9). Clear evidence for this mechanism, in the form of detailed associations between the molecular gas kinematics and features in the radio-emitting jets, has however been lacking. Here we report that the warm molecular hydrogen gas in the western radio lobe of the Seyfert galaxy IC 5063 is moving at high velocities-up to about 600 kilometres per second-relative to the galaxy disk. This suggests that the molecules have been accelerated by fast shocks driven into the interstellar medium by the expanding radio jets. These results demonstrate the general feasibility of accelerating molecular outflows in fast shocks driven by active nuclei. C1 [Tadhunter, C.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Morganti, R.; Oonk, J. B. R.; Oosterloo, T.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Morganti, R.; Oosterloo, T.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Rose, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tadhunter, C (reprint author), Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. EM c.tadhunter@sheffield.ac.uk FU European Southern Observatory, Chile [290.B-5162]; UK Science and Technology Research Council; European Research Council under the European Union [RADIOLIFE-320745] FX This work is based on observations collected at the European Southern Observatory, Chile (programme 290.B-5162). C.T. and M.R. acknowledge financial support from the UK Science and Technology Research Council. R.M. acknowledges support from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Advanced Grant RADIOLIFE-320745. NR 30 TC 34 Z9 34 U1 0 U2 8 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 JUL 24 PY 2014 VL 511 IS 7510 BP 440 EP 443 DI 10.1038/nature13520 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AL7SO UT WOS:000339335700040 PM 25043049 ER PT J AU Jacobs, B Johnson, NL Wahl, D Schall, M Maseko, BC Lewandowski, A Raghanti, MA Wicinski, B Butti, C Hopkins, WD Bertelsen, MF Walsh, T Roberts, JR Reep, RL Hof, PR Sherwood, CC Manger, PR AF Jacobs, Bob Johnson, Nicholas L. Wahl, Devin Schall, Matthew Maseko, Busisiwe C. Lewandowski, Albert Raghanti, Mary A. Wicinski, Bridget Butti, Camilla Hopkins, William D. Bertelsen, Mads F. Walsh, Timothy Roberts, John R. Reep, Roger L. Hof, Patrick R. Sherwood, Chet C. Manger, Paul R. TI Comparative neuronal morphology of the cerebellar cortex in afrotherians, carnivores, cetartiodactyls, and primates (vol 8, pg 24, 2014) SO FRONTIERS IN NEUROANATOMY LA English DT Correction C1 [Jacobs, Bob; Johnson, Nicholas L.; Wahl, Devin; Schall, Matthew] Colorado Coll, Lab Quantitat Neuromorphol, Colorado Springs, CO 80903 USA. [Maseko, Busisiwe C.; Manger, Paul R.] Univ Witwatersrand, Fac Hlth Sci, Sch Anat Sci, Johannesburg, South Africa. [Lewandowski, Albert] Cleveland Metropk Zoo, Cleveland, OH USA. [Raghanti, Mary A.] Kent State Univ, Dept Anthropol, Kent, OH 44242 USA. [Wicinski, Bridget; Butti, Camilla; Hof, Patrick R.] Icahn Sch Med Mt Sinai, Fishberg Dept Neurosci, New York, NY 10029 USA. [Wicinski, Bridget; Butti, Camilla; Hof, Patrick R.] Icahn Sch Med Mt Sinai, Friedman Brian Inst, New York, NY 10029 USA. [Hopkins, William D.] Yerkes Natl Primate Res Ctr, Div Dev & Cognit Neurosci, Atlanta, GA USA. [Bertelsen, Mads F.] Copenhagen Zoo, Ctr Zoo & Wild Anim Hlth, Frederiksberg, Denmark. [Walsh, Timothy; Roberts, John R.] Smithsonian Natl Zool Pk, Washington, DC USA. [Reep, Roger L.] Univ Florida, Dept Physiol Sci, Gainesville, FL 32610 USA. [Sherwood, Chet C.] George Washington Univ, Dept Anthropol, Washington, DC USA. RP Jacobs, B (reprint author), Colorado Coll, Lab Quantitat Neuromorphol, Colorado Springs, CO 80903 USA. EM bjacobs@coloradocollege.edu NR 1 TC 0 Z9 0 U1 1 U2 4 PU FRONTIERS RESEARCH FOUNDATION PI LAUSANNE PA PO BOX 110, LAUSANNE, 1015, SWITZERLAND SN 1662-5129 J9 FRONT NEUROANAT JI Front. Neuroanat. PD JUL 23 PY 2014 VL 8 AR 69 DI 10.3389/fnana.2014.00069 PG 4 WC Anatomy & Morphology; Neurosciences SC Anatomy & Morphology; Neurosciences & Neurology GA AM5AP UT WOS:000339867800001 ER PT J AU Robertson, DR Cramer, KL AF Ross Robertson, D. Cramer, Katie L. TI Defining and Dividing the Greater Caribbean: Insights from the Biogeography of Shorefishes SO PLOS ONE LA English DT Article ID GULF-OF-MEXICO; TROPICAL EASTERN PACIFIC; GENETIC-STRUCTURE; REEF FISHES; ATLANTIC; WESTERN; OCEAN; SEA; DISTRIBUTIONS; SPECIATION AB The Greater Caribbean biogeographic region is the high-diversity heart of the Tropical West Atlantic, one of four global centers of tropical marine biodiversity. The traditional view of the Greater Caribbean is that it is limited to the Caribbean, West Indies, southwest Gulf of Mexico and tip of Florida, and that, due to its faunal homogeneity, lacks major provincial subdivisions. In this scenario the northern 2/3 of the Gulf of Mexico and southeastern USA represent a separate temperate, "Carolinian'' biogeographic region. We completed a comprehensive re-assessment of the biogeography of the Greater Caribbean by comparing the distributions of 1,559 shorefish species within 45 sections of shelf waters of the Greater Caribbean and adjacent areas. This analysis shows that that the Greater Caribbean occupies a much larger area than usually thought, extending south to at least Guyana, and north to encompass the entire Carolinian area. Rather than being homogenous, the Greater Caribbean is divided into three major provinces, each with a distinctive, primarily tropical fauna: (1) a central, tropical province comprising the West Indies, Bermuda and Central America; (2) a southern, upwelling-affected province spanning the entire continental shelf of northern South America; and (iii) a northern, subtropical province that includes all of the Gulf of Mexico, Florida and southeastern USA. This three-province pattern holds for both reef-and soft bottom fishes, indicating a general response by demersal fishes to major variation in provincial shelf environments. Such environmental differences include latitudinal variation in sea temperature, availability of major habitats (coral reefs, soft bottom shorelines, and mangroves), and nutrient additions from upwelling areas and large rivers. The three-province arrangement of the Greater Caribbean broadly resembles and has a similar environmental basis to the provincial arrangement of its sister biogeographic region, the Tropical Eastern Pacific. C1 [Ross Robertson, D.; Cramer, Katie L.] Smithsonian Trop Res Inst, Balboa, Panama. RP Robertson, DR (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. EM drr@stri.org FU Smithsonian Tropical Research Institute FX Smithsonian Tropical Research Institute general research funds. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 73 TC 7 Z9 7 U1 2 U2 39 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 23 PY 2014 VL 9 IS 7 AR e102918 DI 10.1371/journal.pone.0102918 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA AM1NT UT WOS:000339614100065 PM 25054225 ER EF